@misc{bhatti_cdips-pipeline_2019,
  author       = {Waqas Bhatti and
                  Luke Bouma and
                  Samuel Yee},
  title        = {\texttt{cdips-pipeline v0.1.0}},
  month        = aug,
  year         = 2019,
  doi          = {10.5281/zenodo.3370324},
  url          = {https://doi.org/10.5281/zenodo.3370324},
  note 		 = {\url{https://doi.org/10.5281/zenodo.3370324}}
}


@misc{bhatti_astrobase_2018,
	author       = {Waqas Bhatti and
	Luke G. Bouma and
	Joshua Wallace},
	title        = {\texttt{astrobase}},
	month        = nov,
	year         = 2018,
	version      = {0.3.20},
	publisher    = {Zenodo},
	doi          = {10.5281/zenodo.1469822},
	url          = {https://doi.org/10.5281/zenodo.1469822},
	note      = {\url{https://doi.org/10.5281/zenodo.1469822}}
}

@article{zhan_complex_2019,
	title = {Complex {Rotational} {Modulation} of {Rapidly} {Rotating} {M} {Stars} {Observed} with \textit{{TESS}}},
	volume = {876},
	issn = {1538-4357},
	url = {https://iopscience.iop.org/article/10.3847/1538-4357/ab158c},
	doi = {10.3847/1538-4357/ab158c},
	number = {2},
	urldate = {2019-08-12},
	journal = {The Astrophysical Journal},
	author = {Zhan, Z. and G\"unther, M. N. and Rappaport, S. and Oláh, K. and Mann, A. and Levine, A. M. and Winn, J. and Dai, F. and Zhou, G. and Huang, Chelsea X. and Bouma, L. G. and Ireland, M. J. and Ricker, G. and Vanderspek, R. and Latham, D. and Seager, S. and Jenkins, J. and Caldwell, D. A. and Doty, J. P. and Essack, Z. and Furesz, G. and Leidos, M. E. R. and Rowden, P. and Smith, J. C. and Stassun, K. G. and Vezie, M.},
	month = may,
	year = {2019},
	pages = {127}
}

@article{libralato_psf-based_2016,
	title = {A {PSF}-based approach to {Kepler}/{K}2 data - {I}. {Variability} within the {K}2 {Campaign} 0 star clusters {M} 35 and {NGC} 2158},
	volume = {456},
	issn = {0035-8711},
	url = {http://adsabs.harvard.edu/abs/2016MNRAS.456.1137L},
	doi = {10.1093/mnras/stv2628},
	abstract = {Kepler and K2 data analysis reported in the literature is mostly based 
on aperture photometry. Because of Kepler's large, undersampled pixels
and the presence of nearby sources, aperture photometry is not always
the ideal way to obtain high-precision photometry, and, because of this,
the data set has not been fully exploited so far. We present a new
method that builds on our experience with undersampled HST images. The
method involves a point-spread function (PSF) neighbour-subtraction and
was specifically developed to exploit the huge potential offered by the
K2 `super-stamps' covering the core of dense star clusters. Our test-bed
targets were the NGC 2158 and M 35 regions observed during the K2
Campaign 0. We present our PSF modelling and demonstrate that, by using
a high-angular-resolution input star list from the Asiago Schmidt
telescope as the basis for PSF neighbour subtraction, we are able to
reach magnitudes as faint as KP ≃ 24 with a photometric
precision of 10 per cent over 6.5 h, even in the densest regions. At the
bright end, our photometric precision reaches ˜30 parts per
million. Our method leads to a considerable level of improvement at the
faint magnitudes (KP ≳ 15.5) with respect to the
classical aperture photometry. This improvement is more significant in
crowded regions. We also extracted raw light curves of ˜60 000
stars and detrended them for systematic effects induced by spacecraft
motion and other artefacts that harms K2 photometric precision. We
present a list of 2133 variables.},
	urldate = {2017-09-13},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Libralato, M. and Bedin, L. R. and Nardiello, D. and Piotto, G.},
	month = feb,
	year = {2016},
	keywords = {techniques: photometric, binaries: general, techniques: image processing, open clusters and associations: individual: M 35, open clusters and associations: individual: NGC 2158, stars: variables: general},
	pages = {1137--1162},
	file = {NASA/ADS Full Text PDF:/Users/luke/Zotero/storage/5UKUWFDA/Libralato et al. - 2016 - A PSF-based approach to KeplerK2 data - I. Variab.pdf:application/pdf}
}

@article{oelkers_light_2019,
	title = {Light {Curves} for {All} {Stars} {Observed} in {TESS} {Full}-frame {Images}: {Sector} 1 and {Beyond}},
	volume = {3},
	issn = {2515-5172},
	shorttitle = {Light {Curves} for {All} {Stars} {Observed} in {TESS} {Full}-frame {Images}},
	url = {http://stacks.iop.org/2515-5172/3/i=1/a=8},
	doi = {10.3847/2515-5172/aafc34},
	language = {en},
	number = {1},
	urldate = {2019-01-15},
	journal = {Research Notes of the AAS},
	author = {Oelkers, Ryan J. and Stassun, Keivan G.},
	year = {2019},
	pages = {8},
	file = {IOP Full Text PDF:/Users/luke/Zotero/storage/GSSHNW4J/Oelkers and Stassun - 2019 - Light Curves for All Stars Observed in TESS Full-f.pdf:application/pdf}
}

@misc{handberg_tess_2019,
	title = {{TESS} {Data} {For} {Asteroseismology} {Lightcurves} ("{TASOC}")},
	url = {http://archive.stsci.edu/doi/resolve/resolve.html?doi=10.17909/t9-4smn-dx89},
	abstract = {The TESS Asteroseismic Investigation is organized within the TESS Asteroseismic Science Consortium (TASC). The data platform for TASC is provided via the TESS Asteroseismic Science Operations Center (TASOC), hosted at the Stellar Astrophysics Centre (SAC) at Aarhus University, Denmark. TASOC provides long-term storage of all data products. TASC membership is open to the entire TESS community and any member of TASC can apply to become a member of a given working group within TASC. The TASC Coordinated Activity “TESS Data for Asteroseismology” (T’DA) is responsible for maintaining the TASOC portal and for providing data products for TASC.  Data provided with this release have been extracted using the TASOC Photometry pipeline. The TASOC pipeline used to generate the data is open source and available on GitHub.  Before using data prepared by T’DA, the team strongly recommends you read through the TESS data release notes for the Sectors you are interested in, and consult the TESS Instrument Handbook.  The initial release (TASOC-0004-01) includes raw aperture photometry light curves for {\textasciitilde}1.7 million stars observed in Sectors 1 and 2. No corrections have been applied to the raw light curves. The team is currently implementing a co-trending component of the TASOC pipeline that will be adopted for future releases.},
	urldate = {2019-08-12},
	publisher = {STScI/MAST},
	author = {Handberg, Rasmus and Lund, Mikkel and Huber, Daniel},
	year = {2019},
	doi = {10.17909/t9-4smn-dx89},
	note = {type: dataset}
}

@article{lund_k2p_2015,
	title = {K2P $^{\textrm{2}}$ —{A} {PHOTOMETRY} {PIPELINE} {FOR} {THE} {K}2 {MISSION}},
	volume = {806},
	issn = {1538-4357},
	url = {http://stacks.iop.org/0004-637X/806/i=1/a=30?key=crossref.1db1d6deb373e7d57743a6c25312df32},
	doi = {10.1088/0004-637X/806/1/30},
	number = {1},
	urldate = {2019-08-12},
	journal = {The Astrophysical Journal},
	author = {Lund, Mikkel N. and Handberg, Rasmus and Davies, Guy R. and Chaplin, William J. and Jones, Caitlin D.},
	month = jun,
	year = {2015},
	pages = {30},
	file = {Full Text:/Users/luke/Zotero/storage/332HMJHI/Lund et al. - 2015 - K2P sup2sup —A PHOTOMETRY PIPELINE FOR THE K2.pdf:application/pdf}
}

@article{wallace_search_2019,
	title = {A {Search} for {Variable} {Stars} in the {Globular} {Cluster} {M}4 with {K}2},
	url = {http://arxiv.org/abs/1908.02373},
	abstract = {We extract light curves for 4554 objects with \$9{\textless}G{\textless}19\$ in the K2 superstamp observations of the globular cluster M4, including 3784 cluster members, and search for variability. Among cluster member objects, we detect 66 variables, of which 52 are new discoveries. Among objects not belonging to the cluster, we detect 24 variables, of which 20 are new discoveries. We additionally discover 57 cluster-member suspected variables, 10 cluster-non-member suspected variables, and four variables with ambiguous cluster membership. Our light curves reach sub-millimagnitude precision for the cluster horizontal branch, permitting us to detect asteroseismic activity in six horizontal branch stars outside the instability strip and one inside the strip but with only {\textasciitilde}1 mmag amplitude variability. 19 additional stars along the red giant branch also have detected asteroseismic variability. Several eclipsing binaries are found in the cluster, including a 4.6-day detached eclipsing binary and an EW-class eclipsing binary, as well as an EW with uncertain cluster membership and three other candidate EWs. A 22-day detached eclipsing binary is also found outside the cluster. We identify a candidate X-ray binary that is a cluster member with quiescent and periodic {\textasciitilde}20 mmag optical variability. We also obtain high-precision light curves for ten of the previously known RR Lyrae variables in the cluster and identify one as a candidate Blazhko variable with a Blazhko period in excess of 78 days. We make our light curves publicly available.},
	urldate = {2019-08-08},
	journal = {arXiv:1908.02373 [astro-ph]},
	author = {Wallace, Joshua J. and Hartman, Joel D. and Bakos, Gaspar A. and Bhatti, Waqas},
	month = aug,
	year = {2019},
	note = {arXiv: 1908.02373},
	keywords = {Astrophysics - Solar and Stellar Astrophysics}
}

@article{cantat-gaudin_velaOB2_2019,
	title = {Expanding associations in the {Vela}-{Puppis} region: 3D structure and kinematics of the young population⋆},
	volume = {626},
	issn = {0004-6361, 1432-0746},
	shorttitle = {Expanding associations in the {Vela}-{Puppis} region},
	url = {https://www.aanda.org/10.1051/0004-6361/201834957},
	doi = {10.1051/0004-6361/201834957},
	urldate = {2019-08-03},
	journal = {Astronomy \& Astrophysics},
	author = {Cantat-Gaudin, T. and Jordi, C. and Wright, N. J. and Armstrong, J. J. and Vallenari, A. and Balaguer-Núñez, L. and Ramos, P. and Bossini, D. and Padoan, P. and Pelkonen, V. M. and Mapelli, M. and Jeffries, R. D.},
	month = jun,
	year = {2019},
	pages = {A17},
	file = {Accepted Version:/Users/luke/Zotero/storage/VQ49F4DM/Cantat-Gaudin et al. - 2019 - Expanding associations in the Vela-Puppis region .pdf:application/pdf}
}

@article{sim_open_2019,
	title = {Open cluster survey within 1 kpc by the {Gaia} {DR}2},
	url = {https://ui.adsabs.harvard.edu/abs/2019arXiv190706872S/abstract},
	abstract = {We conducted a survey of open clusters within 1 kpc from the Sun using the astrometric and photometric data of Gaia DR2. We found 664 cluster candidates by visual inspection of the stellar distributions in proper motion space and spatial distributions in l-b space. All of the 664 cluster candidates have a well defined main-sequence except for two candidates if we consider that the main sequence of very young clusters are somewhat broad due to differential extinctions. Cross-matching of 662 open clusters with known open clusters in various catalogs resulted in 209 new open clusters. We present the basic data of newly discovered open clusters along with a brief description of the property of the new clusters. The majority of newly discovered open clusters have young and intermediate ages and they are likely to have member stars less than {\textasciitilde}50.},
	language = {en},
	urldate = {2019-08-03},
	journal = {arXiv e-prints},
	author = {Sim, Gyuheon and Lee, Sang Hyun and Ann, Hong Bae and Kim, Seunghyeon},
	month = jul,
	year = {2019},
	pages = {arXiv:1907.06872},
	file = {Full Text PDF:/Users/luke/Zotero/storage/NF46WAS4/Sim et al. - 2019 - Open cluster survey within 1 kpc by the Gaia DR2.pdf:application/pdf;Snapshot:/Users/luke/Zotero/storage/MRSADQZT/abstract.html:text/html}
}

@article{kounkel_untangling_2019,
	title = {Untangling the {Galaxy} {I}: {Local} {Structure} and {Star} {Formation} {History} of the {Milky} {Way}},
	shorttitle = {Untangling the {Galaxy} {I}},
	url = {http://arxiv.org/abs/1907.07709},
	abstract = {Gaia DR2 provides unprecedented precision in measurements of the distance and kinematics of stars in the solar neighborhood. Through applying unsupervised machine learning on DR2's 5-dimensional dataset (3d position + 2d velocity), we identify a number of clusters, associations, and co-moving groups within 1 kpc and \${\textbar}b{\textbar}{\textless}30{\textasciicircum}{\textbackslash}circ\$ (many of which have not been previously known). We estimate their ages with the precision of \${\textbackslash}sim\$0.15 dex. Many of these groups appear to be filamentary or string-like, oriented in parallel to the Galactic plane, and some span hundreds of pc in length. Most of these string lack a central cluster, indicating that their filamentary structure is primordial, rather than the result of tidal stripping or dynamical processing. The youngest strings (\${\textless}\$100 Myr) are orthogonal to the Local Arm. The older ones appear to be remnants of several other arm-like structures that cannot be presently traced by dust and gas. The velocity dispersion measured from the ensemble of groups and strings increase with age, suggesting a timescale for dynamical heating of \${\textbackslash}sim\$300 Myr. This timescale is also consistent with the age at which the population of strings begins to decline, while the population in more compact groups continues to increase, suggesting that dynamical processes are disrupting the weakly bound string populations, leaving only individual clusters to be identified at the oldest ages. These data shed a new light on the local galactic structure and a large scale cloud collapse.},
	urldate = {2019-08-03},
	journal = {arXiv:1907.07709 [astro-ph]},
	author = {Kounkel, Marina and Covey, Kevin},
	month = jul,
	year = {2019},
	note = {arXiv: 1907.07709},
	keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics},
	annote = {Comment: 17 pages, 14 figures. Accepted to AJ Interactive figures are accessible through http://mkounkel.com/mw3d/ and they will be available in the published version},
	file = {arXiv\:1907.07709 PDF:/Users/luke/Zotero/storage/QYYPC52X/Kounkel and Covey - 2019 - Untangling the Galaxy I Local Structure and Star .pdf:application/pdf;arXiv.org Snapshot:/Users/luke/Zotero/storage/F3893I6X/1907.html:text/html}
}

@article{jones_proper_1988,
	title = {Proper motions and variabilities of stars near the {Orion} {Nebula}},
	volume = {95},
	issn = {0004-6256},
	url = {http://adsabs.harvard.edu/abs/1988AJ.....95.1755J},
	doi = {10.1086/114773},
	abstract = {Relative proper motions were measured and membership probabilities were determined for over 1000 stars within 15-arcmin of the center of the Orion Nebula, M42. About 900 of the stars are associated with the Orion complex. The motions are of sufficient precision to measure the internal velocity dispersions. These dispersions are nearly isotropic, and depend only weakly on magnitude and distance from the Trapezium. The
corresponding velocity dispersion in one coordinate is just over 2 km/s. The distribution of stars follows closely the distribution of gas as measured by CO-13. The stars appear to be, at most, only weakly bound to the molecular cloud. A search for variable stars has found that nearly half of the member stars are either known variables or showed variation on the plates.},
	urldate = {2019-07-24},
	journal = {The Astronomical Journal},
	author = {Jones, B. F. and Walker, Merle F.},
	month = jun,
	year = {1988},
	keywords = {Variable Stars, Velocity Distribution, Stellar Motions, Molecular Clouds, Carbon Monoxide, H Ii Regions, Infrared Sources (Astronomy), Orion Nebula, Star Formation},
	pages = {1755--1782}
}


@ARTICLE{Pollacco_2006,
   author = {{Pollacco}, D.~L. and {Skillen}, I. and {Collier Cameron}, A. and 
	{Christian}, D.~J. and {Hellier}, C. and {Irwin}, J. and {Lister}, T.~A. and 
	{Street}, R.~A. and {West}, R.~G. and {Anderson}, D.~R. and 
	{Clarkson}, W.~I. and {Deeg}, H. and {Enoch}, B. and {Evans}, A. and 
	{Fitzsimmons}, A. and {Haswell}, C.~A. and {Hodgkin}, S. and 
	{Horne}, K. and {Kane}, S.~R. and {Keenan}, F.~P. and {Maxted}, P.~F.~L. and 
	{Norton}, A.~J. and {Osborne}, J. and {Parley}, N.~R. and {Ryans}, R.~S.~I. and 
	{Smalley}, B. and {Wheatley}, P.~J. and {Wilson}, D.~M.},
    title = "{The WASP Project and the SuperWASP Cameras}",
  journal = {\pasp},
   eprint = {astro-ph/0608454},
 keywords = {Instrumentation: Photometers, Stars: Planetary Systems, Techniques: Photometric},
     year = 2006,
    month = oct,
   volume = 118,
    pages = {1407-1418},
      doi = {10.1086/508556},
   adsurl = {https://ui.adsabs.harvard.edu/abs/2006PASP..118.1407P},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{price-whelan_binary_2018,
	title = {Binary {Companions} of {Evolved} {Stars} in {APOGEE} {DR}14: {Orbital} {Circularization}},
	volume = {867},
	issn = {0004-637X},
	shorttitle = {Binary {Companions} of {Evolved} {Stars} in {APOGEE} {DR}14},
	url = {https://doi.org/10.3847%2F1538-4357%2Faae264},
	doi = {10.3847/1538-4357/aae264},
	abstract = {Short-period binary star systems dissipate orbital energy through tidal interactions that lead to tighter, more circular orbits. Using a sample of binaries with subgiant, giant, and red clump star members that is nearly an order of magnitude larger than that of Verbunt \& Phinney, we reexamine predictions for tidal circularization of binary stars with evolved members. We confirm that binary star systems in our sample predicted to have circular orbits (using equilibrium tide theory) generally have negligible measured eccentricities. At a fixed stellar mass, the transition period is correlated with the surface gravity (i.e., size) of the evolved member, indicating that the circularization timescale must be shorter than the evolutionary timescale along the giant branch. A few exceptions to the conclusions above are mentioned in the discussion. Some of these exceptions are likely systems in which the spectrum of the secondary biases the radial velocity measurements, but four appear to be genuine, short-period, moderate-eccentricity systems.},
	language = {en},
	number = {1},
	urldate = {2019-07-24},
	journal = {The Astrophysical Journal},
	author = {Price-Whelan, Adrian M. and Goodman, Jeremy},
	month = oct,
	year = {2018},
	pages = {5},
	file = {IOP Full Text PDF:/home/luke/local/Zotero/storage/LYNCZKB2/Price-Whelan and Goodman - 2018 - Binary Companions of Evolved Stars in APOGEE DR14.pdf:application/pdf}
}

@article{luhman_formation_2012,
	title = {The {Formation} and {Early} {Evolution} of {Low}-{Mass} {Stars} and {Brown} {Dwarfs}},
	volume = {50},
	issn = {0066-4146},
	url = {http://adsabs.harvard.edu/abs/2012ARA%26A..50...65L},
	doi = {10.1146/annurev-astro-081811-125528},
	abstract = {The discovery of large numbers of young low-mass stars and brown dwarfs over the past decade has made it possible to investigate star formation and early evolution in a previously unexplored mass regime. In this review, we begin by describing surveys for low-mass members of nearby associations, open clusters, star-forming regions, and the methods used to characterize their stellar properties. We then use observations of these populations to test theories of star formation and evolution at low masses. For comparison to the formation models, we consider the initial mass function, stellar multiplicity, circumstellar disks, protostellar characteristics, and kinematic and spatial distributions at birth for low-mass stars and brown dwarfs. To test the evolutionary models, we focus on measurements of dynamical masses and empirical Hertzsprung-Russell diagrams for young brown dwarfs and planetary companions.},
	urldate = {2019-07-24},
	journal = {Annual Review of Astronomy and Astrophysics},
	author = {Luhman, Kevin L.},
	month = sep,
	year = {2012},
	pages = {65--106},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/P5LYNLHT/Luhman - 2012 - The Formation and Early Evolution of Low-Mass Star.pdf:application/pdf}
}

@article{kraus_mass-radius_2015,
	title = {The {Mass}-{Radius} {Relation} of {Young} {Stars}. {I}. {USco} 5, an {M}4.5 {Eclipsing} {Binary} in {Upper} {Scorpius} {Observed} by {K}2},
	volume = {807},
	issn = {0004-637X},
	url = {http://adsabs.harvard.edu/abs/2015ApJ...807....3K},
	doi = {10.1088/0004-637X/807/1/3},
	abstract = {We present the discovery that UScoCTIO 5, a known spectroscopic binary 
in the Upper Scorpius star-forming region (P = 34 days,
\{M\}\{tot\}\{sin\}(i)=0.64 \{M\}⊙ ), is an eclipsing
system with both primary and secondary eclipses apparent in K2 light
curves obtained during Campaign 2. We have simultaneously fit the
eclipse profiles from the K2 light curves and the existing RV data to
demonstrate that UScoCTIO 5 consists of a pair of nearly identical M4.5
stars with \{M\}A=0.329+/- 0.002 \{M\}⊙ ,
\{R\}A=0.834+/- 0.006 \{R\}⊙ ,
\{M\}B=0.317+/- 0.002 \{M\}⊙ , and
\{R\}B=0.810+/- 0.006 \{R\}⊙ . The radii are
broadly consistent with pre-main-sequence ages predicted by stellar
evolutionary models, but none agree to within the uncertainties. All
models predict systematically incorrect masses at the 25\%-50\%
level for the HR diagram position of these mid-M dwarfs, suggesting
significant modifications to mass-dependent outcomes of star and planet
formation. The form of the discrepancy for most model sets is not that
they predict luminosities that are too low, but rather that they predict
temperatures that are too high, suggesting that the models do not fully
encompass the physics of energy transport (via convection and/or missing
opacities) and/or a miscalibration of the SpT-\{T\}\{eff\}
scale. The simplest modification to the models (changing
\{T\}\{eff\} to match observations) would yield an older age for
this system, in line with the recently proposed older age of Upper
Scorpius (τ ˜ 11 Myr).},
	urldate = {2019-07-24},
	journal = {The Astrophysical Journal},
	author = {Kraus, Adam L. and Cody, Ann Marie and Covey, Kevin R. and Rizzuto, Aaron C. and Mann, Andrew W. and Ireland, Michael J.},
	month = jul,
	year = {2015},
	keywords = {stars: evolution, binaries: eclipsing, stars: low-mass, stars: fundamental parameters, stars: pre-main sequence, stars: individual: UScoCTIO 5},
	pages = {3}
}

@article{stassun_review_2014,
	title = {Empirical tests of pre-main-sequence stellar evolution models with eclipsing binaries},
	volume = {60},
	issn = {1387-6473},
	url = {http://adsabs.harvard.edu/abs/2014NewAR..60....1S},
	doi = {10.1016/j.newar.2014.06.001},
	abstract = {We examine the performance of standard pre-main-sequence (PMS) stellar 
evolution models against the accurately measured properties of a
benchmark sample of 26 PMS stars in 13 eclipsing binary (EB) systems
having masses 0.04-4.0 M⊙ and nominal ages ≈1-20 Myr.
We provide a definitive compilation of all fundamental properties for
the EBs, with a careful and consistent reassessment of observational
uncertainties. We also provide a definitive compilation of the various
PMS model sets, including physical ingredients and limits of
applicability. No set of model isochrones is able to successfully
reproduce all of the measured properties of all of the EBs. In the H-R
diagram, the masses inferred for the individual stars by the models are
accurate to better than 10\% at ≳1 M⊙, but below 1
M⊙ they are discrepant by 50-100\%. Adjusting the observed
radii and temperatures using empirical relations for the effects of
magnetic activity helps to resolve the discrepancies in a few cases, but
fails as a general solution. We find evidence that the failure of the
models to match the data is linked to the triples in the EB sample; at
least half of the EBs possess tertiary companions. Excluding the
triples, the models reproduce the stellar masses to better than ∼10\%
in the H-R diagram, down to 0.5 M⊙, below which the
current sample is fully contaminated by tertiaries. We consider several
mechanisms by which a tertiary might cause changes in the EB properties
and thus corrupt the agreement with stellar model predictions. We show
that the energies of the tertiary orbits are comparable to that needed
to potentially explain the scatter in the EB properties through
injection of heat, perhaps involving tidal interaction. It seems from
the evidence at hand that this mechanism, however it operates in detail,
has more influence on the surface properties of the stars than on their
internal structure, as the lithium abundances are broadly in good
agreement with model predictions. The EBs that are members of young
clusters appear individually coeval to within 20\%, but collectively show
an apparent age spread of ∼50\%, suggesting true age spreads in young
clusters. However, this apparent spread in the EB ages may also be the
result of scatter in the EB properties induced by tertiaries.},
	urldate = {2019-07-24},
	journal = {New Astronomy Reviews},
	author = {Stassun, Keivan G. and Feiden, Gregory A. and Torres, Guillermo},
	month = jun,
	year = {2014},
	pages = {1--28},
	file = {Submitted Version:/home/luke/local/Zotero/storage/LW2JZJPA/Stassun et al. - 2014 - Empirical tests of pre-main-sequence stellar evolu.pdf:application/pdf}
}

@article{milliman_wiyn_2014,
	title = {{WIYN} {Open} {Cluster} {Study}. {LX}. {Spectroscopic} {Binary} {Orbits} in {NGC} 6819},
	volume = {148},
	url = {https://ui.adsabs.harvard.edu//#abs/2014AJ....148...38M/abstract},
	doi = {10.1088/0004-6256/148/2/38},
	abstract = {We present the current state of the WOCS radial-velocity (RV) survey for the rich open cluster NGC 6819 (2.5 Gyr) including 93 spectroscopic binary orbits with periods ranging from 1.5 to 8000 days. These results are the product of our ongoing RV survey of NGC 6819 using the Hydra Multi-Object Spectrograph on the WIYN 3.5 m telescope. We also include a detailed analysis of multiple prior sets of optical photometry for NGC 6819. Within a 1° field of view, our stellar sample includes the giant branch, the red clump, and blue straggler candidates, and extends to almost 2 mag below the main sequence (MS) turnoff. For each star observed in our survey we present all RV measurements, the average RV, and velocity variability information. Additionally, we discuss notable binaries from our sample, including eclipsing binaries (WOCS 23009, WOCS 24009, and WOCS 40007), stars noted in Kepler asteroseismology studies (WOCS 4008, WOCS 7009, and WOCS 8007), and potential descendants of past blue stragglers (WOCS 1006 and WOCS 6002). We find the incompleteness-corrected binary fraction for all MS binaries with periods less than 10{\textless}SUP{\textgreater}4{\textless}/SUP{\textgreater} days to be 22\% ± 3\% and a tidal circularization period of 6.2{\textasciicircum}\{+1.1\}\_\{-1.1\} days for NGC 6819.},
	language = {en},
	number = {2},
	urldate = {2018-11-24},
	journal = {The Astronomical Journal},
	author = {Milliman, Katelyn E. and Mathieu, Robert D. and Geller, Aaron M. and Gosnell, Natalie M. and Meibom, Søren and Platais, Imants},
	month = aug,
	year = {2014},
	keywords = {binaries: spectroscopic, open clusters and associations: individual: NGC 6819, blue stragglers},
	pages = {38},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/KYLRJCUT/Milliman et al. - 2014 - WIYN Open Cluster Study. LX. Spectroscopic Binary .pdf:application/pdf;NASA/ADS Full Text PDF:/home/luke/local/Zotero/storage/RH6RENFX/Milliman et al. - 2014 - WIYN Open Cluster Study. LX. Spectroscopic Binary .pdf:application/pdf;Snapshot:/home/luke/local/Zotero/storage/8XPXE3CK/ui.adsabs.harvard.edu.html:text/html}
}

@article{meibom_robust_2005,
	title = {A {Robust} {Measure} of {Tidal} {Circularization} in {Coeval} {Binary} {Populations}: {The} {Solar}-{Type} {Spectroscopic} {Binary} {Population} in the {Open} {Cluster} {M}35},
	volume = {620},
	shorttitle = {A {Robust} {Measure} of {Tidal} {Circularization} in {Coeval} {Binary} {Populations}},
	url = {https://ui.adsabs.harvard.edu//#abs/2005ApJ...620..970M/abstract},
	doi = {10.1086/427082},
	abstract = {We present a new homogeneous sample of 32 spectroscopic binary orbits in the young ({\textasciitilde}150 Myr) main-sequence open cluster M35. The distribution of orbital eccentricity versus orbital period (e-logP) displays a distinct transition from eccentric to circular orbits at an orbital period of {\textasciitilde}10 days. The transition is due to tidal circularization of the closest binaries. The population of binary orbits in M35 provide a significantly improved constraint on the rate of tidal circularization at an age of 150 Myr. We propose a new and more robust diagnostic of the degree of tidal circularization in a binary population based on a functional fit to the e-logP distribution. We call this new measure the ``tidal circularization period.'' The tidal circularization period of a binary population represents the orbital period at which a binary orbit with the most frequent initial orbital eccentricity circularizes (defined as e=0.01) at the age of the population. We determine the tidal circularization period for M35, as well as for seven additional binary populations spanning ages from the pre-main sequence ({\textasciitilde}3 Myr) to the late main sequence ({\textasciitilde}10 Gyr), and use Monte Carlo error analysis to determine the uncertainties on the derived circularization periods. We conclude that current theories of tidal circularization cannot account for the distribution of tidal circularization periods with population age. WIYN Open Cluster Study XXII.},
	language = {en},
	number = {2},
	urldate = {2018-11-24},
	journal = {The Astrophysical Journal},
	author = {Meibom, Søren and Mathieu, Robert D.},
	month = feb,
	year = {2005},
	pages = {970},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/K5F66TUN/Meibom and Mathieu - 2005 - A Robust Measure of Tidal Circularization in Coeva.pdf:application/pdf;Snapshot:/home/luke/local/Zotero/storage/C2RWS4DM/ui.adsabs.harvard.edu.html:text/html}
}

@article{skumanich_time_1972,
	title = {Time {Scales} for {CA} {II} {Emission} {Decay}, {Rotational} {Braking}, and {Lithium} {Depletion}},
	volume = {171},
	issn = {0004-637X},
	url = {http://adsabs.harvard.edu/abs/1972ApJ...171..565S},
	doi = {10.1086/151310},
	abstract = {Abstract image available at: 
http://adsabs.harvard.edu/abs/1972ApJ...171..565S},
	urldate = {2016-10-06},
	journal = {The Astrophysical Journal},
	author = {Skumanich, A.},
	month = feb,
	year = {1972},
	pages = {565}
}

@article{fischer_planet-metallicity_2005,
	title = {The {Planet}-{Metallicity} {Correlation}},
	volume = {622},
	issn = {0004-637X},
	url = {http://adsabs.harvard.edu/abs/2005ApJ...622.1102F},
	doi = {10.1086/428383},
	abstract = {We have recently carried out spectral synthesis modeling to determine Teff, logg, vsini, and [Fe/H] for 1040 FGK-type stars on the Keck, Lick, and Anglo-Australian Telescope planet search programs. This is the first time that a single, uniform spectroscopic analysis has been made for every star on a large Doppler planet search survey. We identify a subset of 850 stars that have Doppler observations sufficient to detect uniformly all planets with radial velocity semiamplitudes K{\textgreater}30 m s-1 and orbital periods shorter than 4 yr. From this subset of stars, we determine that fewer than 3\% of stars with
-0.5{\textless}[Fe/H]{\textless}0.0 have Doppler-detected planets. Above solar
metallicity, there is a smooth and rapid rise in the fraction of stars with planets. At [Fe/H]{\textgreater}+0.3 dex, 25\% of observed stars have detected gas giant planets. A power-law fit to these data relates the formation probability for gas giant planets to the square of the number of metal atoms. High stellar metallicity also appears to be correlated with the presence of multiple-planet systems and with the total detected planet mass. This data set was examined to better understand the origin of high metallicity in stars with planets. None of the expected fossil
signatures of accretion are observed in stars with planets relative to the general sample: (1) metallicity does not appear to increase as the mass of the convective envelopes decreases, (2) subgiants with planets do not show dilution of metallicity, (3) no abundance variations for Na, Si, Ti, or Ni are found as a function of condensation temperature, and (4) no correlations between metallicity and orbital period or
eccentricity could be identified. We conclude that stars with extrasolar planets do not have an accretion signature that distinguishes them from other stars; more likely, they are simply born in higher metallicity molecular clouds.

Based on observations obtained at Lick and Keck Observatories, operated by the University of California, and the Anglo-Australian Observatories.},
	urldate = {2016-09-04},
	journal = {The Astrophysical Journal},
	author = {Fischer, Debra A. and Valenti, Jeff},
	month = apr,
	year = {2005},
	keywords = {stars: fundamental parameters, stars: planetary systems, Stars: abundances, Stars: fundamental parameters},
	pages = {1102--1117},
	annote = {First uniform spectroscopic analysis (Teff, logg, vsini, Z) and thus uniform sample of metallicities ({\textasciitilde}850 stars, both with and without planets) from the California group. Enabled a careful study of how much giant planet occurrence (they claim within P{\textless}2yr, Msini{\textgreater}0.5Mj, give or take... really K{\textgreater}30m/s) varies with stellar metallicity.
They find: \% of stars with giant planets {\textasciitilde} (number of metal atoms){\textasciicircum}2 = (10*(Z)){\textasciicircum}2=10*(2*Z). E.g. while it's {\textasciitilde}2.5\% of solar-metallicity stars, it's {\textasciitilde}25\% of Z=0.5 stars that have jupiter mass companions. Rule is valid for -0.5{\textless}[Fe/H]{\textless}0.5.
Metallicity is probably the strongest predictor of any stellar parameter of the occurrence of giant planets.
It's also correlated with the presence of multiple planet systems (more strongly? weakly?) as well as total detected planet mass.
They also look for accretion signatures: the idea being that the star should accrete a lot of the gas from the protoplanetary disk, and planets may even fall in, perhaps enriching certain elements. You would expect the strengths of these signatures to scale with the mass (size) of the convective envelope, which increases (relative to the star) with decreasing stellar mass. They look for these signatures and don't find them [personally, not sure about how large these signatures are expected to be].
Specifically, you don't know a priori whether you're seeing more giants around metal rich stars as a consequence of formation, or as a consequence of pollution (accretion). If formation, you expect stars to have similar metallicities throughout (for most elements). If accretion, you only expect it in the convective zone. The CZ mass should then matter. Also, when stars hit the subgiant branch, they should have DECREASED metallicities compared to what they had before (since the CZ grows, they'd mix the accreted metals further down and dilute them). You might also expect there to be variations in the stars as a function of condensation temperature.
They don't see any of these, and conclude that the giant planet occurrence - metallicity correlation is a result of initial formation conditions rather than accretion/pollution of the stellar atmospheres. (this is hard to do, given the trickiness of getting a uniform sample of Teffs, loggs, vsinis, and Zs)},
	file = {NASA/ADS Full Text PDF:/home/luke/local/Zotero/storage/38PQGMKM/Fischer and Valenti - 2005 - The Planet-Metallicity Correlation.pdf:application/pdf}
}

@article{ivezic_statistics_2014,
	title = {Statistics, {Data} {Mining}, and {Machine} {Learning} in {Astronomy}},
	url = {https://ui.adsabs.harvard.edu/abs/2014sdmm.book.....I/abstract},
	abstract = {A powerful, streamlined new Astrophysics Data System},
	language = {en},
	urldate = {2019-07-20},
	journal = {Statistics},
	author = {Ivezi\'c, Zeljko and Connelly, Andrew J. and VanderPlas, Jacob T. and Gray, Alexander},
	year = {2014},
	file = {Snapshot:/Users/luke/Zotero/storage/X64DZYUX/abstract.html:text/html}
}

@article{sklearn_2011,
 title={Scikit-learn: Machine Learning in {P}ython},
 author={Pedregosa, F. and Varoquaux, G. and Gramfort, A. and Michel, V.
         and Thirion, B. and Grisel, O. and Blondel, M. and Prettenhofer, P.
         and Weiss, R. and Dubourg, V. and Vanderplas, J. and Passos, A. and
         Cournapeau, D. and Brucher, M. and Perrot, M. and Duchesnay, E.},
 journal={Journal of Machine Learning Research},
 volume={12},
 pages={2825--2830},
 year={2011}
}

@article{froebrich_FSR_2007,
	title = {A systematic survey for infrared star clusters with {\textbar}b{\textbar} \&lt;20° using 2MASS},
	volume = {374},
	url = {https://ui.adsabs.harvard.edu/abs/2007MNRAS.374..399F/abstract},
	doi = {10.1111/j.1365-2966.2006.11148.x},
	abstract = {We used star density maps obtained from the Two-Micron All-Sky Survey (2MASS) to obtain a sample of star clusters in the entire Galactic Plane with {\textbar}b{\textbar} \&lt; 20°. A total of 1788 star cluster candidates are identified in this survey. Among those are 681 previously known open clusters and 86 globular clusters. A statistical analysis indicates that our sample of 1021 new cluster candidates has a contamination of about 50per cent. Star cluster parameters are obtained by fitting a King profile to the star density. These parameters are used to statistically identify probable new globular cluster candidates in our sample. A detailed investigation of the projected distribution of star clusters in the Galaxy demonstrates that they show a clear tendency to cluster on spatial scales in the order of 12-25pc, a typical size for molecular clouds.},
	language = {en},
	number = {2},
	urldate = {2019-06-30},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Froebrich, D. and Scholz, A. and Raftery, C. L.},
	month = jan,
	year = {2007},
	pages = {399},
	file = {Full Text PDF:/Users/luke/Zotero/storage/ZRS2RX8G/Froebrich et al. - 2007 - A systematic survey for infrared star clusters wit.pdf:application/pdf;Snapshot:/Users/luke/Zotero/storage/PAUMBJVH/abstract.html:text/html}
}

@article{tamuz_correcting_2005,
	title = {Correcting systematic effects in a large set of photometric light curves},
	volume = {356},
	issn = {0035-8711},
	url = {https://academic.oup.com/mnras/article/356/4/1466/1014047},
	doi = {10.1111/j.1365-2966.2004.08585.x},
	abstract = {Abstract.  We suggest a new algorithm to remove systematic effects in a large set of light curves obtained by a photometric survey. The algorithm can remove sys},
	language = {en},
	number = {4},
	urldate = {2019-07-12},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Tamuz, O. and Mazeh, T. and Zucker, S.},
	month = feb,
	year = {2005},
	pages = {1466--1470}
}

@article{krone-martins_upmask_2014,
	title = {{UPMASK}: unsupervised photometric membership assignment in stellar clusters},
	volume = {561},
	issn = {0004-6361, 1432-0746},
	shorttitle = {{UPMASK}},
	url = {http://www.aanda.org/10.1051/0004-6361/201321143},
	doi = {10.1051/0004-6361/201321143},
	urldate = {2019-07-11},
	journal = {Astronomy \& Astrophysics},
	author = {Krone-Martins, A. and Moitinho, A.},
	month = jan,
	year = {2014},
	pages = {A57},
	file = {Full Text:/Users/luke/Zotero/storage/X3Y3ABNA/Krone-Martins and Moitinho - 2014 - UPMASK unsupervised photometric membership assign.pdf:application/pdf}
}

@article{mayor_harps_2011,
	title = {The {HARPS} search for southern extra-solar planets {XXXIV}. {Occurrence}, mass distribution and orbital properties of super-{Earths} and {Neptune}-mass planets},
	volume = {1109},
	url = {http://adsabs.harvard.edu/abs/2011arXiv1109.2497M},
	abstract = {We report on the results of an 8-year survey carried out at the La Silla 
Observatory with the HARPS spectrograph to detect and characterize
planets in the super-Earth and Neptune mass regime. The size of our star
sample and the precision achieved with HARPS have allowed the detection
of a sufficiently large number of low-mass planets to study the
statistical properties of their orbital elements, the correlation of the
host-star metallicity with the planet masses, as well as the occurrence
rate of planetary systems around solar-type stars. A robust estimate of
the frequency of systems shows that more than 50\% of solar-type stars
harbor at least one planet of any mass and with period up to 100 days.
Different properties are observed for the population of planets less
massive than about 30M-Earth compared to the population of gaseous giant
planets. The mass distribution of Super-Earths and Neptune-mass planets
(SEN) is strongly increasing between 30 and 15M-Earth. The SEN occurence
rate does not exhibit a preference for metal rich stars. Most of the SEN
planets belong to multi-planetary systems. The orbital eccentricities of
the SEN planets seems limited to 0.45. At the opposite, the occurence
rate of gaseous giant planets is growing with the logarithm of the
period, and is strongly increasing with the host-star metallicity. About
14\% of solar-type stars have a planetary companion more massive than
50M-Earth? on an orbit with a period shorter than 10 years. Orbital
eccentricities of giant planets are observed up to 0.9 and beyond. The
precision of HARPS-type spectrographs opens the possibility to detect
planets in the habitable zone of solar-type stars. Identification of a
significant number of super-Earths orbiting solar-type of the Sun
vicinity is achieved by Doppler spectroscopy. 37 newly discovered
planets are announced in the Appendix of this paper, among which 15
Super-Earths.},
	urldate = {2017-11-15},
	journal = {ArXiv e-prints},
	author = {Mayor, M. and Marmier, M. and Lovis, C. and Udry, S. and Ségransan, D. and Pepe, F. and Benz, W. and Bertaux, J. -L. and Bouchy, F. and Dumusque, X. and Lo Curto, G. and Mordasini, C. and Queloz, D. and Santos, N. C.},
	month = sep,
	year = {2011},
	keywords = {Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics},
	pages = {arXiv:1109.2497}
}

@article{wright_frequency_2012,
	title = {{THE} {FREQUENCY} {OF} {HOT} {JUPITERS} {ORBITING} {NEARBY} {SOLAR}-{TYPE} {STARS}},
	volume = {753},
	issn = {0004-637X, 1538-4357},
	url = {http://stacks.iop.org/0004-637X/753/i=2/a=160?key=crossref.d90356a2590e9f68bd46bf55ea77705b},
	doi = {10.1088/0004-637X/753/2/160},
	number = {2},
	urldate = {2016-09-04},
	journal = {The Astrophysical Journal},
	author = {Wright, J. T. and Marcy, G. W. and Howard, A. W. and Johnson, John Asher and Morton, T. D. and Fischer, D. A.},
	month = jul,
	year = {2012},
	pages = {160}
}

@article{howard_planet_2012,
	title = {Planet {Occurrence} within 0.25 {AU} of {Solar}-type {Stars} from {Kepler}},
	volume = {201},
	issn = {0067-0049},
	url = {http://adsabs.harvard.edu/abs/2012ApJS..201...15H},
	doi = {10.1088/0067-0049/201/2/15},
	abstract = {We report the distribution of planets as a function of planet radius, orbital period, and stellar effective temperature for orbital periods less than 50 days around solar-type (GK) stars. These results are based on the 1235 planets (formally "planet candidates") from the Kepler mission that include a nearly complete set of detected planets as small as 2 R ⊕. For each of the 156,000 target stars, we
assess the detectability of planets as a function of planet radius, R p, and orbital period, P, using a measure of the detection efficiency for each star. We also correct for the geometric probability of transit, R sstarf/a. We consider first Kepler target stars within the "solar subset" having T eff = 4100-6100 K, log g = 4.0-4.9, and Kepler magnitude Kp {\textless} 15 mag, i.e., bright,
main-sequence GK stars. We include only those stars having photometric noise low enough to permit detection of planets down to 2 R
⊕. We count planets in small domains of R p and P and divide by the included target stars to calculate planet occurrence in each domain. The resulting occurrence of planets varies by more than three orders of magnitude in the radius-orbital period plane and increases substantially down to the smallest radius (2 R
⊕) and out to the longest orbital period (50 days,
{\textasciitilde}0.25 AU) in our study. For P {\textless} 50 days, the distribution of planet radii is given by a power law, df/dlog R = kRR
α with kR = 2.9+0.5 -
0.4, α = -1.92 ± 0.11, and R ≡ R p/R
⊕. This rapid increase in planet occurrence with
decreasing planet size agrees with the prediction of core-accretion formation but disagrees with population synthesis models that predict a desert at super-Earth and Neptune sizes for close-in orbits. Planets with orbital periods shorter than 2 days are extremely rare; for R p {\textgreater} 2 R ⊕ we measure an occurrence of
less than 0.001 planets per star. For all planets with orbital periods less than 50 days, we measure occurrence of 0.130 ± 0.008, 0.023 ± 0.003, and 0.013 ± 0.002 planets per star for planets
with radii 2-4, 4-8, and 8-32 R ⊕, in agreement with
Doppler surveys. We fit occurrence as a function of P to a power-law model with an exponential cutoff below a critical period P 0. For smaller planets, P 0 has larger values, suggesting that the "parking distance" for migrating planets moves outward with
decreasing planet size. We also measured planet occurrence over a broader stellar T eff range of 3600-7100 K, spanning M0 to F2 dwarfs. Over this range, the occurrence of 2-4 R ⊕
planets in the Kepler field increases with decreasing T eff, with these small planets being seven times more abundant around cool stars (3600-4100 K) than the hottest stars in our sample (6600-7100 K).

Based in part on observations obtained at the W. M. Keck Observatory, which is operated by the University of California and the California Institute of Technology.},
	urldate = {2018-06-13},
	journal = {The Astrophysical Journal Supplement Series},
	author = {Howard, Andrew W. and Marcy, Geoffrey W. and Bryson, Stephen T. and Jenkins, Jon M. and Rowe, Jason F. and Batalha, Natalie M. and Borucki, William J. and Koch, David G. and Dunham, Edward W. and Gautier, III, Thomas N. and Van Cleve, Jeffrey and Cochran, William D. and Latham, David W. and Lissauer, Jack J. and Torres, Guillermo and Brown, Timothy M. and Gilliland, Ronald L. and Buchhave, Lars A. and Caldwell, Douglas A. and Christensen-Dalsgaard, Jørgen and Ciardi, David and Fressin, Francois and Haas, Michael R. and Howell, Steve B. and Kjeldsen, Hans and Seager, Sara and Rogers, Leslie and Sasselov, Dimitar D. and Steffen, Jason H. and Basri, Gibor S. and Charbonneau, David and Christiansen, Jessie and Clarke, Bruce and Dupree, Andrea and Fabrycky, Daniel C. and Fischer, Debra A. and Ford, Eric B. and Fortney, Jonathan J. and Tarter, Jill and Girouard, Forrest R. and Holman, Matthew J. and Johnson, John Asher and Klaus, Todd C. and Machalek, Pavel and Moorhead, Althea V. and Morehead, Robert C. and Ragozzine, Darin and Tenenbaum, Peter and Twicken, Joseph D. and Quinn, Samuel N. and Isaacson, Howard and Shporer, Avi and Lucas, Philip W. and Walkowicz, Lucianne M. and Welsh, William F. and Boss, Alan and Devore, Edna and Gould, Alan and Smith, Jeffrey C. and Morris, Robert L. and Prsa, Andrej and Morton, Timothy D. and Still, Martin and Thompson, Susan E. and Mullally, Fergal and Endl, Michael and MacQueen, Phillip J.},
	month = aug,
	year = {2012},
	keywords = {planetary systems, techniques: photometric, stars: statistics},
	pages = {15},
	annote = {One of the first major occurrence rate papers. Good (now old) plots of N planets per star at short periods vs say, stellar effective temperature.},
	file = {Full Text PDF:/Users/luke/Zotero/storage/ANLJ73ZA/Howard et al. - 2012 - Planet Occurrence within 0.25 AU of Solar-type Sta.pdf:application/pdf}
}


@article{petigura_metallicity_2018,
	title = {The {California}- \textit{{Kepler}} {Survey}. {IV}. {Metal}-rich {Stars} {Host} a {Greater} {Diversity} of {Planets}},
	volume = {155},
	issn = {1538-3881},
	url = {http://stacks.iop.org/1538-3881/155/i=2/a=89?key=crossref.3c016d97df21d2057deac77796f9d1c9},
	doi = {10.3847/1538-3881/aaa54c},
	number = {2},
	urldate = {2019-07-11},
	journal = {The Astronomical Journal},
	author = {Petigura, Erik A. and Marcy, Geoffrey W. and Winn, Joshua N. and Weiss, Lauren M. and Fulton, Benjamin J. and Howard, Andrew W. and Sinukoff, Evan and Isaacson, Howard and Morton, Timothy D. and Johnson, John Asher},
	month = jan,
	year = {2018},
	pages = {89},
	file = {Full Text:/Users/luke/Zotero/storage/J962663Q/Petigura et al. - 2018 - The California- iKepleri Survey. IV. Metal-ri.pdf:application/pdf}
}

@article{pepper_photometric_2008,
	title = {A {PHOTOMETRIC} {SURVEY} {FOR} {VARIABLES} {AND} {TRANSITS} {IN} {THE} {FIELD} {OF} {PRAESEPE} {WITH} {THE} {KILODEGREE} {EXTREMELY} {LITTLE} {TELESCOPE}},
	volume = {135},
	issn = {0004-6256, 1538-3881},
	url = {http://stacks.iop.org/1538-3881/135/i=3/a=907?key=crossref.8586d77baff5e30516c2c25095c386c5},
	doi = {10.1088/0004-6256/135/3/907},
	number = {3},
	urldate = {2019-07-11},
	journal = {The Astronomical Journal},
	author = {Pepper, Joshua and Stanek, K. Z. and Pogge, Richard W. and Latham, David W. and DePoy, D. L. and Siverd, Robert and Poindexter, Shawn and Sivakoff, Gregory R.},
	month = mar,
	year = {2008},
	pages = {907--921},
	file = {Full Text:/Users/luke/Zotero/storage/DZ97T79C/Pepper et al. - 2008 - A PHOTOMETRIC SURVEY FOR VARIABLES AND TRANSITS IN.pdf:application/pdf}
}

@article{burke_survey_2006,
	title = {Survey for {Transiting} {Extrasolar} {Planets} in {Stellar} {Systems}. {III}. {A} {Limit} on the {Fraction} of {Stars} with {Planets} in the {Open} {Cluster} {NGC} 1245},
	volume = {132},
	issn = {0004-6256, 1538-3881},
	url = {http://stacks.iop.org/1538-3881/132/i=1/a=210},
	doi = {10.1086/504468},
	language = {en},
	number = {1},
	urldate = {2019-07-11},
	journal = {The Astronomical Journal},
	author = {Burke, Christopher J. and Gaudi, B. Scott and DePoy, D. L. and Pogge, Richard W.},
	month = jul,
	year = {2006},
	pages = {210--230},
	file = {Full Text:/Users/luke/Zotero/storage/CSU9FUER/Burke et al. - 2006 - Survey for Transiting Extrasolar Planets in Stella.pdf:application/pdf}
}

@article{mochejska_planets_2005,
	title = {Planets in {Stellar} {Clusters} {Extensive} {Search}. {III}. {A} {Search} for {Transiting} {Planets} in the {Metal}-rich {Open} {Cluster} {NGC} 6791},
	volume = {129},
	issn = {0004-6256, 1538-3881},
	url = {http://stacks.iop.org/1538-3881/129/i=6/a=2856},
	doi = {10.1086/430219},
	language = {en},
	number = {6},
	urldate = {2019-07-11},
	journal = {The Astronomical Journal},
	author = {Mochejska, B. J. and Stanek, K. Z. and Sasselov, D. D. and Szentgyorgyi, A. H. and Bakos, G. Á. and Hradecky, V., J. Devor and Marrone, D. P. and Winn, J. N. and Zaldarriaga, M.},
	month = jun,
	year = {2005},
	pages = {2856--2868},
	file = {Full Text:/Users/luke/Zotero/storage/TL8MDQYP/Mochejska et al. - 2005 - Planets in Stellar Clusters Extensive Search. III..pdf:application/pdf}
}

@article{mochejska_planets_2006,
	title = {Planets in {Stellar} {Clusters} {Extensive} {Search}. {IV}. {A} {Detection} of a {Possible} {Transiting} {Planet} {Candidate} in the {Open} {Cluster} {NGC} 2158},
	volume = {131},
	issn = {0004-6256, 1538-3881},
	url = {http://stacks.iop.org/1538-3881/131/i=2/a=1090},
	doi = {10.1086/499208},
	language = {en},
	number = {2},
	urldate = {2019-07-11},
	journal = {The Astronomical Journal},
	author = {Mochejska, B. J. and Stanek, K. Z. and Sasselov, D. D. and Szentgyorgyi, A. H. and Adams, E. and Cooper, R. L. and Foster, J. B. and Hartman, J. D. and Hickox, R. C. and Lai, K. and Westover, M. and Winn, J. N.},
	month = feb,
	year = {2006},
	pages = {1090--1105},
	file = {Full Text:/Users/luke/Zotero/storage/3ANJLIDV/Mochejska et al. - 2006 - Planets in Stellar Clusters Extensive Search. IV. .pdf:application/pdf}
}

@article{bailer-jones_distances_2018,
	title = {Estimating distances from parallaxes {IV}: {Distances} to 1.33 billion stars in {Gaia} {Data} {Release} 2},
	shorttitle = {Estimating distances from parallaxes {IV}},
	url = {http://arxiv.org/abs/1804.10121},
	abstract = {For the vast majority of stars in the second Gaia data release, reliable distances cannot be obtained by inverting the parallax. A correct inference procedure must instead be used to account for the nonlinearity of the transformation and the asymmetry of the resulting probability distribution. Here we infer distances to essentially all 1.33 billion stars with parallaxes published in the second Gaia data release. This is done using a weak distance prior that varies smoothly as a function of Galactic longitude and latitude according to a Galaxy model. The irreducible uncertainty in the distance estimate is characterized by the lower and upper bounds of an asymmetric confidence interval. Although more precise distances can be estimated for a subset of the stars using additional data (such as photometry), our goal is to provide purely geometric distance estimates, independent of assumptions about the physical properties of, or interstellar extinction towards, individual stars. We analyse the characteristics of the catalogue and validate it using clusters. The catalogue can be queried using ADQL at http://gaia.ari.uni-heidelberg.de/tap.html (which also hosts the Gaia catalogue) as the table geometric\_distance in the schema gaiadr2\_complements. The catalogue will go live on or before 30 April. Before that you can access it as a set of CSV files from http://www.mpia.de/{\textasciitilde}calj/gdr2\_distances.html .},
	urldate = {2018-04-28},
	journal = {arXiv:1804.10121 [astro-ph]},
	author = {Bailer-Jones, C. A. L. and Rybizki, J. and Fouesneau, M. and Mantelet, G. and Andrae, R.},
	month = apr,
	year = {2018},
	note = {arXiv: 1804.10121},
	keywords = {Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics}
}

@article{zacharias_fourth_2013,
	title = {The {Fourth} {US} {Naval} {Observatory} {CCD} {Astrograph} {Catalog} ({UCAC}4)},
	volume = {145},
	url = {https://ui.adsabs.harvard.edu/abs/2013AJ....145...44Z/abstract},
	doi = {10.1088/0004-6256/145/2/44},
	abstract = {The fourth United States Naval Observatory (USNO) CCD Astrograph Catalog, UCAC4, was released in 2012 August (double-sided DVD and CDS data center Vizier catalog I/322). It is the final release in this series and contains over 113 million objects; over 105 million of them with proper motions (PMs). UCAC4 is an updated version of UCAC3 with about the same number of stars also covering all-sky. Bugs were fixed, Schmidt plate survey data were avoided, and precise five-band photometry was added for about half the stars. Astrograph observations have been supplemented for bright stars by FK6, Hipparcos, and Tycho-2 data to compile a UCAC4 star catalog complete from the brightest stars to about magnitude R = 16. Epoch 1998-2004 positions are obtained from observations with the 20 cm aperture USNO Astrograph's "red lens," equipped with a 4k by 4k CCD. Mean positions and PMs are derived by combining these observations with over 140 ground- and space-based catalogs, including Hipparcos/Tycho and the AC2000.2, as well as unpublished measures of over 5000 plates from other astrographs. For most of the faint stars in the southern hemisphere, the first epoch plates from the Southern Proper Motion program form the basis for PMs, while the Northern Proper Motion first epoch plates serve the same purpose for the rest of the sky. These data are supplemented by 2MASS near-IR photometry for about 110 million stars and five-band (B, V, g, r, i) APASS data for over 51 million stars. Thus the published UCAC4, as were UCAC3 and UCAC2, is a compiled catalog with the UCAC observational program being a major component. The positional accuracy of stars in UCAC4 at mean epoch is about 15-100 mas per coordinate, depending on magnitude, while the formal errors in PMs range from about 1 to 10 mas yr{\textless}SUP{\textgreater}-1{\textless}/SUP{\textgreater} depending on magnitude and observing history. Systematic errors in PMs are estimated to be about 1-4 mas yr{\textless}SUP{\textgreater}-1{\textless}/SUP{\textgreater}.},
	language = {en},
	number = {2},
	urldate = {2019-07-04},
	journal = {The Astronomical Journal},
	author = {Zacharias, N. and Finch, C. T. and Girard, T. M. and Henden, A. and Bartlett, J. L. and Monet, D. G. and Zacharias, M. I.},
	month = feb,
	year = {2013},
	pages = {44},
	file = {Full Text PDF:/Users/luke/Zotero/storage/VEU3F4AK/Zacharias et al. - 2013 - The Fourth US Naval Observatory CCD Astrograph Cat.pdf:application/pdf;Snapshot:/Users/luke/Zotero/storage/H682ZVEF/abstract.html:text/html}
}

@article{aigrain_robust_2017,
	title = {Robust, open-source removal of systematics in {Kepler} data},
	volume = {471},
	issn = {0035-8711},
	url = {https://academic.oup.com/mnras/article/471/1/759/3865959},
	doi = {10.1093/mnras/stx1422},
	abstract = {Abstract.  We present ARC2 (Astrophysically Robust Correction 2), an open-source python-based systematics-correction pipeline, to correct for the Kepler prime m},
	language = {en},
	number = {1},
	urldate = {2019-07-03},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Aigrain, S. and Parviainen, H. and Roberts, S. and Reece, S. and Evans, T.},
	month = oct,
	year = {2017},
	pages = {759--769},
	file = {Full Text PDF:/Users/luke/Zotero/storage/HARBPFTM/Aigrain et al. - 2017 - Robust, open-source removal of systematics in Kepl.pdf:application/pdf;Snapshot:/Users/luke/Zotero/storage/3GXHUIS8/3865959.html:text/html}
}

@article{smith_pdc_2012,
	title = {Kepler {Presearch} {Data} {Conditioning} {II} - {A} {Bayesian} {Approach} to {Systematic} {Error} {Correction}},
	volume = {124},
	issn = {1538-3873},
	url = {https://iopscience.iop.org/article/10.1086/667697/meta},
	doi = {10.1086/667697},
	language = {en},
	number = {919},
	urldate = {2019-05-02},
	journal = {Publications of the Astronomical Society of the Pacific},
	author = {Smith, Jeffrey C. and Stumpe, Martin C. and Cleve, Jeffrey E. Van and Jenkins, Jon M. and Barclay, Thomas S. and Fanelli, Michael N. and Girouard, Forrest R. and Kolodziejczak, Jeffery J. and McCauliff, Sean D. and Morris, Robert L. and Twicken, Joseph D.},
	month = sep,
	year = {2012},
	pages = {1000}
}


@article{vanderburg_hr858_2019,
	title = {{TESS} {Spots} a {Compact} {System} of {Super}-{Earths} around the {Naked}-{Eye} {Star} {HR} 858},
	url = {http://arxiv.org/abs/1905.05193},
	abstract = {Transiting Exoplanet Survey Satellite (TESS) observations have revealed a compact multi-planet system around the sixth-magnitude star HR 858 (TIC 178155732), located 32 parsecs away. Three planets, each about twice the size of Earth, transit this slightly-evolved, late F-type star, which is also a member of a visual binary. Two of the planets may be in mean motion resonance. We analyze the TESS observations, using novel methods to model and remove instrumental systematic errors, and combine these data with follow-up observations taken from a suite of ground-based telescopes to characterize the planetary system. The HR 858 planets are enticing targets for precise radial velocity observations, secondary eclipse spectroscopy, and measurements of the Rossiter-McLaughlin effect.},
	urldate = {2019-05-15},
	journal = {arXiv:1905.05193 [astro-ph]},
	author = {Vanderburg, Andrew and Huang, Chelsea X. and Rodriguez, Joseph E. and Becker, Juliette C. and Ricker, George R. and Vanderspek, Roland K. and Latham, David W. and Seager, Sara and Jenkins, Jon M. and Addison, Brett and Bieryla, Allyson and Briceño, Cesar and Bowler, Brendan P. and Burke, Christopher J. and Burt, Jennifer A. and Caldwell, Douglas A. and Clark, Jake T. and Crossfield, Ian and Dittmann, Jason A. and Dynes, Scott and Guerrero, Natalia and Horner, Jonathan and Kane, Stephen R. and Kielkopf, John and Kraus, Adam L. and Law, Nicolas and Mann, Andrew W. and Mengel, Matthew W. and Morton, Timothy D. and Okumura, Jack and Pearce, Logan A. and Plavchan, Peter and Rose, Mark E. and Rowden, Pam and Smith, Jeffrey C. and Stassun, Keivan and Tinney, C. G. and Wittenmyer, Rob and Wright, Duncan J. and Zhang, Hui and Zhou, George and Ziegler, Carl A.},
	month = may,
	year = {2019},
	note = {arXiv: 1905.05193},
	keywords = {Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics}
}

@incollection{bakos_hat_review_2018,
	title = {The {HATNet} and {HATSouth} {Exoplanet} {Surveys}},
	isbn = {978-3-319-30648-3},
	url = {https://doi.org/10.1007/978-3-319-30648-3_111-1},
	abstract = {The Hungarian-made Automated Telescope Network (HATNet) has been in operation since 2003, with the key science goal being the discovery and accurate characterization of transiting extrasolar planets (TEPs) around bright stars. Using six small, 11 cm aperture, fully automated telescopes in Arizona and Hawaii, as of March 2017, it has discovered and accurately characterized 67 such objects. The HATSouth network of telescopes has been in operation since 2009, using slightly larger, 18 cm diameter optical tubes. It was the first global network of telescopes using identical instrumentation. With three premier sites spread out in longitude (Chile, Namibia, Australia), the HATSouth network permits round-the-clock observations of a 128 square arcdegree swath of the sky at any given time, weather permitting. As of this writing, HATSouth has discovered 36 transiting exoplanets. Many of the altogether ∼100 HAT and HATSouth exoplanets were the first of their kind. They have been important contributors to the rapidly developing field of exoplanets, motivating and influencing observational techniques and theoretical studies and also actively shaping future instrumentation for the detection and characterization of such objects.},
	language = {en},
	urldate = {2018-11-24},
	booktitle = {Handbook of {Exoplanets}},
	publisher = {Springer International Publishing},
	author = {Bakos, G. A.},
	editor = {Deeg, Hans J. and Belmonte, Juan Antonio},
	year = {2018},
	doi = {10.1007/978-3-319-30648-3_111-1},
	pages = {1--11},
	file = {Springer Full Text PDF:/Users/luke/Zotero/storage/HIC8YWKZ/Á. Bakos - 2018 - The HATNet and HATSouth Exoplanet Surveys.pdf:application/pdf}
}


@article{andrae_apsis_2018,
	title = {Gaia {Data} {Release} 2. {First} stellar parameters from {Apsis}},
	volume = {616},
	url = {https://ui.adsabs.harvard.edu/abs/2018A%26A...616A...8A/abstract},
	doi = {10.1051/0004-6361/201732516},
	abstract = {The second Gaia data release (Gaia DR2) contains, beyond the astrometry, three-band photometry for 1.38 billion sources. One band is the G band, the other two were obtained by integrating the Gaia prism spectra (BP and RP). We have used these three broad photometric bands to infer stellar effective temperatures, T{\textless}SUB{\textgreater}eff{\textless}/SUB{\textgreater}, for all sources brighter than G = 17 mag with T{\textless}SUB{\textgreater}eff{\textless}/SUB{\textgreater} in the range 3000-10 000 K (some 161 million sources). Using in addition the parallaxes, we infer the line-of-sight extinction, A{\textless}SUB{\textgreater}G{\textless}/SUB{\textgreater}, and the reddening, E(BP - RP), for 88 million sources. Together with a bolometric correction we derive luminosity and radius for 77 million sources. These quantities as well as their estimated uncertainties are part of Gaia DR2. Here we describe the procedures by which these quantities were obtained, including the underlying assumptions, comparison with literature estimates, and the limitations of our results. Typical accuracies are of order 324 K (T{\textless}SUB{\textgreater}eff{\textless}/SUB{\textgreater}), 0.46 mag (A{\textless}SUB{\textgreater}G{\textless}/SUB{\textgreater}), 0.23 mag (E(BP - RP)), 15\% (luminosity), and 10\% (radius). Being based on only a small number of observable quantities and limited training data, our results are necessarily subject to some extreme assumptions that can lead to strong systematics in some cases (not included in the aforementioned accuracy estimates). One aspect is the non-negativity contraint of our estimates, in particular extinction, which we discuss. Yet in several regions of parameter space our results show very good performance, for example for red clump stars and solar analogues. Large uncertainties render the extinctions less useful at the individual star level, but they show good performance for ensemble estimates. We identify regimes in which our parameters should and should not be used and we define a "clean" sample. Despite the limitations, this is the largest catalogue of uniformly-inferred stellar parameters to date. More precise and detailed astrophysical parameters based on the full BP/RP spectrophotometry are planned as part of the third Gaia data release.},
	language = {en},
	urldate = {2019-07-02},
	journal = {Astronomy and Astrophysics},
	author = {Andrae, René and Fouesneau, Morgan and Creevey, Orlagh and Ordenovic, Christophe and Mary, Nicolas and Burlacu, Alexandru and Chaoul, Laurence and Jean-Antoine-Piccolo, Anne and Kordopatis, Georges and Korn, Andreas and Lebreton, Yveline and Panem, Chantal and Pichon, Bernard and Thévenin, Frédéric and Walmsley, Gavin and Bailer-Jones, Coryn A. L.},
	month = aug,
	year = {2018},
	pages = {A8}
}


@article{wenger_simbad_2000,
	title = {The {SIMBAD} astronomical database: {The} {CDS} reference database for astronomical objects},
	volume = {143},
	issn = {0365-0138, 1286-4846},
	shorttitle = {The {SIMBAD} astronomical database},
	url = {http://aas.aanda.org/10.1051/aas:2000332},
	doi = {10.1051/aas:2000332},
	number = {1},
	urldate = {2019-07-01},
	journal = {Astronomy and Astrophysics Supplement Series},
	author = {Wenger, M. and Ochsenbein, F. and Egret, D. and Dubois, P. and Bonnarel, F. and Borde, S. and Genova, F. and Jasniewicz, G. and Laloë, S. and Lesteven, S. and Monier, R.},
	month = apr,
	year = {2000},
	pages = {9--22},
	file = {Full Text:/Users/luke/Zotero/storage/YHI7KFPK/Wenger et al. - 2000 - The SIMBAD astronomical database The CDS referenc.pdf:application/pdf}
}

@article{saurin_isolating_2015,
	title = {Isolating the pre-main sequence in {Collinder} 34, {NGC} 3293, {NGC} 3766 and {NGC} 6231},
	volume = {448},
	url = {https://ui.adsabs.harvard.edu/abs/2015MNRAS.448.1687S/abstract},
	doi = {10.1093/mnras/stv026},
	abstract = {We employed field star decontaminated Two Micron All Sky Survey photometry to study four nearby optical embedded clusters - Collinder 34, NGC 3293, NGC 3766 and NGC 6231 - obtaining deep colour-magnitude diagrams and stellar radial density profiles. We found what seem to be pre-main sequences detached in different amounts from main sequences in these diagrams. The structural analysis of each cluster revealed different radial distributions for these two sequences. We argued that the detached evolutionary sequences in our sample may be evidence of sequential star formation. Finally, we compared the sample cluster parameters with those of other young clusters in the literature and point out evidence that NGC 3766 and NGC 6231 might be evolving to OB associations.},
	language = {en},
	number = {2},
	urldate = {2019-07-01},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Saurin, T. A. and Bica, E. and Bonatto, C.},
	month = apr,
	year = {2015},
	pages = {1687}
}

@article{majaess_discovering_2013,
	title = {Discovering protostars and their host clusters via {WISE}},
	volume = {344},
	issn = {0004-640X, 1572-946X},
	doi = {10.1007/s10509-012-1308-y},
	language = {en},
	number = {1},
	urldate = {2019-06-30},
	journal = {Astrophysics and Space Science},
	author = {Majaess, D.},
	month = mar,
	year = {2013},
	pages = {175--186}
}

@article{roser_nine_RSG_2016,
	title = {Nine new open clusters within 500 pc from the {Sun}},
	volume = {595},
	copyright = {© ESO 2016},
	issn = {0004-6361, 1432-0746},
	url = {https://www.aanda.org/articles/aa/abs/2016/11/aa29158-16/aa29158-16.html},
	doi = {10.1051/0004-6361/201629158},
	abstract = {{\textless}i{\textgreater}Aims. {\textless}i/{\textgreater}One of the results of the Milky Way Star Clusters (MWSC) survey was the detection of a slight under-density of old (ca. 1 Gyr) clusters within the nearest kilo-parsec from the Sun. This under-density may be due to an ineffectiveness in the detection of larger structures with lower surface brightness. We report on our attempts to reveal such clusters. {\textless}i{\textgreater}Methods. {\textless}i/{\textgreater}We derived proper motions from a combination of Tycho-2 with URAT1, and obtained a mean precision of about 1.4 mas/yr per co-ordinate for 1.3 million stars north of −20° declination. We cut the sky into narrow proper motion slices and searched for spatial over-densities of stars in each slice. We then examined stars from over-densities in optical and near-infrared colour-magnitude diagrams to determine if they are compatible with isochrones of a cluster. We estimated the field star contamination using our data and the Besançon Galactic model.{\textless}i{\textgreater}Results. {\textless}i/{\textgreater}We detected nine hitherto unknown open clusters in the vicinity of the Sun with ages between 70 Myr and 1 Gyr, and distances between 200 and 500 pc.},
	language = {en},
	urldate = {2019-06-30},
	journal = {Astronomy \& Astrophysics},
	author = {R\"oser, Siegfried and Schilbach, Elena and Goldman, Bertrand},
	month = nov,
	year = {2016},
	pages = {A22},
	file = {Full Text PDF:/Users/luke/Zotero/storage/EI5R85LK/Röser et al. - 2016 - Nine new open clusters within 500 pc from the Sun.pdf:application/pdf;Snapshot:/Users/luke/Zotero/storage/H4GZXFAW/aa29158-16.html:text/html}
}

@article{baumgardt_asterisms_1998,
	title = {The nature of some doubtful open clusters as revealed by {HIPPARCOS}},
	volume = {340},
	url = {https://ui.adsabs.harvard.edu/abs/1998A%26A...340..402B/abstract},
	abstract = {We discuss the nature of some galactic open clusters by using proper motions and parallaxes from the Hipparcos and ACT catalogues. We show that the clusters Collinder 399, Upgren 1, NGC 1252 and Melotte 227 do not exist. Collinder 132 is found to be mainly composed out of members of an OB association, but there may be a star cluster present in this area too. Roeser \&amp; Bastian (1994) proposed that NGC 2451 consists of two star clusters. We show that NGC 2451 A definitively does exist, NGC 2451 B may exist. A star cluster may also be present in the area of Roslund 5. The Hipparcos data finally confirm the reality of Collinder 135.},
	language = {en},
	urldate = {2019-06-30},
	journal = {Astronomy and Astrophysics},
	author = {Baumgardt, H.},
	month = dec,
	year = {1998},
	pages = {402},
	file = {Full Text PDF:/Users/luke/Zotero/storage/WJCWJMIN/Baumgardt - 1998 - The nature of some doubtful open clusters as revea.pdf:application/pdf;Snapshot:/Users/luke/Zotero/storage/VJEAGYS4/abstract.html:text/html}
}

@article{newton_dstuc_2019,
	title = {{TESS} {Hunt} for {Young} and {Maturing} {Exoplanets} ({THYME}): {A} planet in the 45 {Myr} {Tucana}-{Horologium} association},
	shorttitle = {{TESS} {Hunt} for {Young} and {Maturing} {Exoplanets} ({THYME})},
	url = {http://arxiv.org/abs/1906.10703},
	abstract = {Young exoplanets are snapshots of the planetary evolution process. Planets that orbit stars in young associations are particularly important because the age of the planetary system is well constrained. We present the discovery of a transiting planet larger than Neptune but smaller than Saturn in the 45 Myr Tucana-Horologium young moving group. The host star is a visual binary, and our follow-up observations demonstrate that the planet orbits the G6V primary component, DS Tuc A (HD 222259A, TIC 410214986). We first identified transits using photometry from the Transiting Exoplanet Survey Satellite (TESS; alerted as TOI 200.01). We validated the planet and improved the stellar parameters using a suite of new and archival data, including spectra from SOAR/Goodman, SALT/HRS and LCO/NRES; transit photometry from Spitzer; and deep adaptive optics imaging from Gemini/GPI. No additional stellar or planetary signals are seen in the data. We measured the planetary parameters by simultaneously modeling the photometry with a transit model and a Gaussian process to account for stellar variability. We determined that the planetary radius is \$5.70{\textbackslash}pm0.17\$ Earth radii and that the orbital period is 8.1 days. The inclination angles of the host star's spin axis, the planet's orbital axis, and the visual binary's orbital axis are aligned within 15 degrees to within the uncertainties of the relevant data. DS Tuc Ab is bright enough (V=8.5) for detailed characterization using radial velocities and transmission spectroscopy.},
	urldate = {2019-06-27},
	journal = {arXiv:1906.10703 [astro-ph]},
	author = {Newton, Elisabeth R. and Mann, Andrew W. and Tofflemire, Benjamin M. and Pearce, Logan and Rizzuto, Aaron C. and Vanderburg, Andrew and Martinez, Raquel A. and Wang, Jason J. and Ruffio, Jean-Baptiste and Kraus, Adam L. and Johnson, Marshall C. and Thao, Pa Chia and Wood, Mackenna L. and Rampalli, Rayna and Nielsen, Eric L. and Collins, Karen A. and Dragomir, Diana and Hellier, Coel and Anderson, D. R. and Barclay, Thomas and Brown, Carolyn and Feiden, Gregory and Hart, Rhodes and Isopi, Giovanni and Kielkopf, John F. and Mallia, Franco and Nelson, Peter and Rodriguez, Joseph E. and Stockdale, Chris and Waite, Ian A. and Wright, Duncan J. and Lissauer, Jack and Ricker, George R. and Vanderspek, Roland and Latham, David W. and Seager, S. and Winn, Joshua N. and Jenkins, Jon M. and Bouma, Luke G. and Burke, Christopher J. and Davies, Misty and Fausnaugh, Michael and Li, Jie and Morris, Robert L. and Mukai, Koji and Villaseñor, Joel and Villeneuva, Steven and De Rosa, Robert J. and Macintosh, Bruce and Mengel, Matthew W. and Okumura, Jack and Wittenmyer, Robert A.},
	month = jun,
	year = {2019},
	note = {arXiv: 1906.10703},
	keywords = {Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics}
}

@article{bryson_identification_2013,
	title = {Identification of {Background} {False} {Positives} from {Kepler} {Data}},
	volume = {125},
	issn = {0004-6280},
	url = {http://adsabs.harvard.edu/abs/2013PASP..125..889B},
	doi = {10.1086/671767},
	abstract = {The Kepler Mission was launched on 2009 March 6 to perform a photometric survey of more than 100,000 dwarf stars to search for Earth-size planets with the transit technique. The reliability of the resulting planetary candidate list relies on the ability to identify and remove false positives. Major sources of astrophysical false positives are planetary transits and stellar eclipses on background stars. We describe several new techniques for the identification of background transit sources that are separated from their target stars, indicating an astrophysical false positive. These techniques use only Kepler photometric data. We describe the concepts and construction of these techniques in detail as well as their performance and relative merits.},
	urldate = {2017-04-24},
	journal = {Publications of the Astronomical Society of the Pacific},
	author = {Bryson, Stephen T. and Jenkins, Jon M. and Gilliland, Ronald L. and Twicken, Joseph D. and Clarke, Bruce and Rowe, Jason and Caldwell, Douglas and Batalha, Natalie and Mullally, Fergal and Haas, Michael R. and Tenenbaum, Peter},
	month = aug,
	year = {2013},
	pages = {889},
	file = {NASA/ADS Full Text PDF:/Users/luke/Zotero/storage/FBJST2V7/Bryson et al. - 2013 - Identification of Background False Positives from .pdf:application/pdf}
}

@article{kostov_l9859_2019,
	title = {The {L} 98-59 {System}: {Three} {Transiting}, {Terrestrial}-{Sized} {Planets} {Orbiting} a {Nearby} {M}-dwarf},
	shorttitle = {The {L} 98-59 {System}},
	url = {http://arxiv.org/abs/1903.08017},
	abstract = {We report the Transiting Exoplanet Survey Satellite (TESS) discovery of three terrestrial-sized planets transiting L 98-59 (TOI-175, TIC 307210830) -- a bright M dwarf at a distance of 10.6 pc. Using the Gaia-measured distance and broad-band photometry we find that the host star is an M3 dwarf. Combined with the TESS transits from one sector, the corresponding stellar parameters yield planet radii ranging from 0.7 REarth to 1.3 REarth. All three planets have short orbital periods, ranging from 2.25 to 7.45 days with the outer pair just wide of a 2:1 period resonance. Diagnostic tests produced by the TESS Data Validation and the vetting package DAVE rule out common false positive sources. These analyses, along with dedicated follow-up and the multiplicity of the system, lend confidence that the observed signals are caused by planets transiting L 98-59 and are not associated with other sources in the field. The L 98-59 system is interesting for a number of reasons: the host star is bright (V = 11.7 mag, K = 7.1 mag) and the planets are prime targets for further follow-up observations including precision radial-velocity mass measurements and future transit spectroscopy with the James Webb Space Telescope; the near resonant configuration makes the system a laboratory to study planetary system dynamical evolution; and three planets of relatively similar size in the same system present an opportunity to study terrestrial planets where other variables (age, metallicity, etc.) can be held constant. L 98-59 will be observed in 6 more TESS sectors, which will provide a wealth of information on the three currently known planets and have the potential to reveal additional planets in the system.},
	urldate = {2019-04-04},
	journal = {arXiv:1903.08017 [astro-ph]},
	author = {Kostov, Veselin B. and Schlieder, Joshua E. and Barclay, Thomas and Quintana, Elisa V. and Colon, Knicole D. and Brande, Jonathan and Collins, Karen A. and Hadden, Samuel and Kane, Stephen R. and Kreidberg, Laura and Kruse, Ethan and Lam, Christopher and Matthews, Elisabeth and Montet, Benjamin T. and Pozuelos, Francisco J. and Stassun, Keivan G. and Winters, Jennifer G. and Ricker, George and Vanderspek, Roland and Latham, David and Seager, Sara and Winn, Joshua and Jenkins, Jon M. and Afanasev, Dennis and Armstrong, James J. D. and Boyd, Patricia and Barentsen, Geert and Barkaoui, Khalid and Batalha, Natalie E. and Bayliss, Daniel and Burdanov, Artem and Cacciapuoti, Luca and Carson, Andrew and Charbonneau, David and Collins, Kevin I. and Conti, Dennis M. and Covone, Giovanni and Clampin, Mark and Delrez, Laetitia and Dressing, Courtney and Ducrot, Elsa and Essack, Zahra and Everett, Mark E. and Foreman-Mackey, Daniel and Gan, Tianjun and Gilbert, Emily and Gillon, Michael and Hamann, Aaron and Hedges, Christina and Horch, Elliott P. and Hocutt, Hannah and Horne, Keith and Hynes, Shane and Ireland, Michael and Irwin, Jonathan M. and Isopi, Giovanni and Jensen, Eric L. N. and Jehin, Emmanuel and Kielkopf, John F. and Lissauer, Jack J. and Mann, Andrew W. and Mallia, Franco and Matson, Rachel A. and Mazeh, Tsevi and Moran, Vickie and Morris, Brett and Muirhead, Philip and Mukai, Koji and Murray, Catriona and Narita, Norio and Palle, Enric and Quinn, David and Relles, Howard and Rinehart, Stephen and Ritsko, Matthew and Rodriguez, Joseph E. and Rowden, Pamela and Sebastian, Daniel and Sefako, Ramotholo and Shahaf, Sahar and Shporer, Avi and Tenenbaum, Peter and Ting, Eric B. and Twicken, Joseph D. and van Belle, Gerard T. and Vega, Laura and Volosin, Jeffrey and Youngblood, Allison},
	month = mar,
	year = {2019},
	note = {arXiv: 1903.08017},
	keywords = {Astrophysics - Earth and Planetary Astrophysics},
	annote = {Comment: 42 pages, 22 figures, submitted to AAS, comments welcome},
	file = {arXiv\:1903.08017 PDF:/Users/luke/Zotero/storage/G9TDG3MK/Kostov et al. - 2019 - The L 98-59 System Three Transiting, Terrestrial-.pdf:application/pdf;arXiv.org Snapshot:/Users/luke/Zotero/storage/V7842DKN/1903.html:text/html}
}


@article{pecaut_intrinsic_2013,
	title = {{INTRINSIC} {COLORS}, {TEMPERATURES}, {AND} {BOLOMETRIC} {CORRECTIONS} {OF} {PRE}-{MAIN}-{SEQUENCE} {STARS}},
	volume = {208},
	issn = {0067-0049, 1538-4365},
	url = {http://stacks.iop.org/0067-0049/208/i=1/a=9?key=crossref.40637725e05e58390e6b2c1741c9f4ac},
	doi = {10.1088/0067-0049/208/1/9},
	number = {1},
	urldate = {2016-05-22},
	journal = {The Astrophysical Journal Supplement Series},
	author = {Pecaut, Mark J. and Mamajek, Eric E.},
	month = sep,
	year = {2013},
	pages = {9}
}


@article{scargle_studies_1982,
	title = {Studies in astronomical time series analysis. {II} - {Statistical} aspects of spectral analysis of unevenly spaced data},
	volume = {263},
	issn = {0004-637X},
	url = {http://adsabs.harvard.edu/abs/1982ApJ...263..835S},
	doi = {10.1086/160554},
	abstract = {Detection of a periodic signal hidden in noise is frequently a goal in 
	astronomical data analysis. This paper does not introduce a new
	detection technique, but instead studies the reliability and efficiency
	of detection with the most commonly used technique, the periodogram, in
	the case where the observation times are unevenly spaced. This choice
	was made because, of the methods in current use, it appears to have the
	simplest statistical behavior. A modification of the classical
	definition of the periodogram is necessary in order to retain the simple
	statistical behavior of the evenly spaced case. With this modification,
	periodogram analysis and least-squares fitting of sine waves to the data
	are exactly equivalent. Certain difficulties with the use of the
	periodogram are less important than commonly believed in the case of
	detection of strictly periodic signals. In addition, the standard method
	for mitigating these difficulties (tapering) can be used just as well if
	the sampling is uneven. An analysis of the statistical significance of
	signal detections is presented, with examples},
	urldate = {2019-06-23},
	journal = {The Astrophysical Journal},
	author = {Scargle, J. D.},
	month = dec,
	year = {1982},
	keywords = {Astronomy, Fourier Transformation, Frequency Response, Power Spectra, Signal Detection, Signal To Noise Ratios, Spectrum Analysis, Statistical Distributions, Time Series Analysis},
	pages = {835--853},
	file = {Full Text PDF:/Users/luke/Zotero/storage/CJ5KDBZE/Scargle - 1982 - Studies in astronomical time series analysis. II -.pdf:application/pdf}
}

@article{lomb_1976,
	title = {Least-squares frequency analysis of unequally spaced data},
	volume = {39},
	issn = {0004-640X},
	url = {http://adsabs.harvard.edu/abs/1976Ap%26SS..39..447L},
	doi = {10.1007/BF00648343},
	abstract = {The statistical properties of least-squares frequency analysis of unequally spaced data are examined. It is shown that, in the
	least-squares spectrum of gaussian noise, the reduction in the sum of squares at a particular frequency is a chi2-squared variable. The reductions at different frequencies are not independent, as there is a correlation between the height of the spectrum at any two frequencies, f1 and f2, which is equal to the mean height of the spectrum due to a sinusoidal signal of frequency f1, at the frequency f2. These correlations reduce the distortion in the spectrum of a signal affected by noise. Some numerical illustrations of the properties of least-squares frequency spectra are given.},
	urldate = {2019-06-23},
	journal = {Astrophysics and Space Science},
	author = {Lomb, N. R.},
	month = feb,
	year = {1976},
	keywords = {Astronomy, Background Noise, Data Reduction, Least Squares Method, Power Spectra, Sine Waves, Spectrum Analysis, Statistical Analysis, Variable Stars},
	pages = {447--462},
	file = {Full Text PDF:/Users/luke/Zotero/storage/AEI8ICSG/Lomb - 1976 - Least-squares frequency analysis of unequally spac.pdf:application/pdf}
}

@article{vanderplas_periodograms_2015,
	title = {{PERIODOGRAMS} {FOR} {MULTIBAND} {ASTRONOMICAL} {TIME} {SERIES}},
	volume = {812},
	issn = {0004-637X},
	url = {https://doi.org/10.1088%2F0004-637x%2F812%2F1%2F18},
	doi = {10.1088/0004-637X/812/1/18},
	abstract = {This paper introduces the multiband periodogram, a general extension of the well-known Lomb–Scargle approach for detecting periodic signals in time-domain data. In addition to advantages of the Lomb–Scargle method such as treatment of non-uniform sampling and heteroscedastic errors, the multiband periodogram significantly improves period finding for randomly sampled multiband light curves (e.g., Pan-STARRS, DES, and LSST). The light curves in each band are modeled as arbitrary truncated Fourier series, with the period and phase shared across all bands. The key aspect is the use of Tikhonov regularization which drives most of the variability into the so-called base model common to all bands, while fits for individual bands describe residuals relative to the base model and typically require lower-order Fourier series. This decrease in the effective model complexity is the main reason for improved performance. After a pedagogical development of the formalism of least-squares spectral analysis, which motivates the essential features of the multiband model, we use simulated light curves and randomly subsampled SDSS Stripe 82 data to demonstrate the superiority of this method compared to other methods from the literature and find that this method will be able to efficiently determine the correct period in the majority of LSST’s bright RR Lyrae stars with as little as six months of LSST data, a vast improvement over the years of data reported to be required by previous studies. A Python implementation of this method, along with code to fully reproduce the results reported here, is available on GitHub.},
	language = {en},
	number = {1},
	urldate = {2019-06-23},
	journal = {The Astrophysical Journal},
	author = {VanderPlas, Jacob T. and Ivezi\'c, Željko},
	month = oct,
	year = {2015},
	pages = {18},
	file = {IOP Full Text PDF:/Users/luke/Zotero/storage/ZN9HDCVX/VanderPlas and Ivezic´ - 2015 - PERIODOGRAMS FOR MULTIBAND ASTRONOMICAL TIME SERIE.pdf:application/pdf}
}

@book{sulentic_revised_1973,
	title = {The revised new catalogue of nonstellar astronomical objects},
	url = {http://adsabs.harvard.edu/abs/1973rncn.book.....S},
	abstract = {Not Available},
	urldate = {2019-06-23},
	author = {Sulentic, Jack W. and Tifft, William G. and Dreyer, John Louis Emil},
	year = {1973},
	keywords = {CATALOGS, GALAXIES, NEBULAE, STAR CLUSTERS}
}

@article{kos_galah_2018,
	title = {The {GALAH} survey and {Gaia} {DR}2: (non-)existence of five sparse high-latitude open clusters},
	volume = {480},
	issn = {0035-8711},
	shorttitle = {The {GALAH} survey and {Gaia} {DR}2},
	url = {https://academic.oup.com/mnras/article/480/4/5242/5071959},
	doi = {10.1093/mnras/sty2171},
	abstract = {ABSTRACT.  Sparse open clusters can be found at high galactic latitudes where loosely populated clusters are more easily detected against the lower stellar back},
	language = {en},
	number = {4},
	urldate = {2018-12-31},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Kos, Janez and de Silva, Gayandhi and Buder, Sven and Bland-Hawthorn, Joss and Sharma, Sanjib and Asplund, Martin and D’Orazi, Valentina and Duong, Ly and Freeman, Ken and Lewis, Geraint F. and Lin, Jane and Lind, Karin and Martell, Sarah L. and Schlesinger, Katharine J. and Simpson, Jeffrey D. and Zucker, Daniel B. and Zwitter, Tomaž and Bedding, Timothy R. and Čotar, Klemen and Horner, Jonathan and Nordlander, Thomas and Stello, Denis and Ting, Yuan-Sen and Traven, Gregor},
	month = nov,
	year = {2018},
	pages = {5242--5259},
	file = {Full Text PDF:/Users/luke/Zotero/storage/V9TQJ3X9/Kos et al. - 2018 - The GALAH survey and Gaia DR2 (non-)existence of .pdf:application/pdf;Snapshot:/Users/luke/Zotero/storage/VK23A9DA/Kos et al. - 2018 - The GALAH survey and Gaia DR2 (non-)existence of .html:text/html}
}

@misc{serven_pygam_2018_1476122,
    author       = {Daniel Serv\'en and
    Charlie Brummitt and
    Hassan Abedi},
    title        = {dswah/pyGAM: v0.8.0},
    month        = oct,
    year         = 2018,
    doi          = {10.5281/zenodo.1476122},
    url          = {https://doi.org/10.5281/zenodo.1476122}
}


@article{eilers_flexible_1996,
    title = {Flexible smoothing with {B}-splines and penalties},
    volume = {11},
    issn = {0883-4237, 2168-8745},
    url = {https://projecteuclid.org/euclid.ss/1038425655},
    doi = {10.1214/ss/1038425655},
    abstract = {B-splines are attractive for nonparametric modelling, but 
    choosing the optimal number and positions of knots is a complex task. 
    Equidistant knots can be used, but their small and discrete number allows 
    only limited control over smoothness and fit. We propose to use a 
    relatively large number of knots and a difference penalty on coefficients 
    of adjacent B-splines. We show connections to the familiar spline penalty 
    on the integral of the squared second derivative. A short overview of 
    B-splines, of their construction and of penalized likelihood is presented. 
    We discuss properties of penalized B-splines and propose various criteria 
    for the choice of an optimal penalty parameter. Nonparametric logistic 
    regression, density estimation and scatterplot smoothing are used as 
    examples. Some details of the computations are presented.},
    language = {en},
    number = {2},
    urldate = {2019-06-11},
    journal = {Statistical Science},
    author = {Eilers, Paul H. C. and Marx, Brian D.},
    month = may,
    year = {1996},
    mrnumber = {MR1435485},
    zmnumber = {0955.62562},
    keywords = {splines, density estimation, Generalized linear models, 
    nonparametric models, smoothing},
    pages = {89--121}
}

@article{hippke_wotan_2019,
    title = {Wotan: {Comprehensive} time-series de-trending in {Python}},
    shorttitle = {Wotan},
    url = {http://arxiv.org/abs/1906.00966},
    abstract = {The detection of transiting exoplanets in time-series 
    photometry requires the removal or modeling of instrumental and stellar 
    noise. While instrumental systematics can be reduced using methods such as 
    pixel level decorrelation, removing stellar trends while preserving 
    transit signals proves challenging. Due to vast archives of light curves 
    from recent transit surveys, there is a strong need for accurate automatic 
    detrending, without human intervention. A large variety of detrending 
    algorithms are in active use, but their comparative performance for 
    transit discovery is unexplored. We benchmark all commonly used detrending 
    methods against hundreds of Kepler, K2, and TESS planets, selected to 
    represent the most difficult cases for systems with small planet-to-star 
    radius ratios. The full parameter range is explored for each method to 
    determine the best choices for planet discovery. We conclude that the 
    ideal method is a time-windowed slider with an iterative robust location 
    estimator based on Tukey's biweight. This method recovers 99\% and 94\% of 
    the shallowest Kepler and K2 planets, respectively. We include an 
    additional analysis for young stars with extreme variability and conclude 
    they are best treated using a spline-based method with a robust Huber 
    estimator. All stellar detrending methods explored are available for 
    public use in wotan, an open-source Python package on "GitHub 
    https://github.com/hippke/wotan".},
    urldate = {2019-06-05},
    journal = {arXiv:1906.00966 [astro-ph]},
    author = {Hippke, Michael and David, Trevor J. and Mulders, Gijs D. and 
    Heller, René},
    month = jun,
    year = {2019},
    note = {arXiv: 1906.00966},
    keywords = {Astrophysics - Earth and Planetary Astrophysics, Astrophysics 
    - Instrumentation and Methods for Astrophysics}
}

@misc{handberg_rasmus_2019_2579846,
    author       = {Handberg, Rasmus and
    Lund, Mikkel Nørup},
    title        = {{T'DA Data Release Notes - Data Release 4 for TESS 
    Sectors 1 + 2}},
    month        = feb,
    year         = 2019,
    doi          = {10.5281/zenodo.2579846},
    url          = {https://doi.org/10.5281/zenodo.2579846}
}


@article{robin_synthetic_2003,
    title = {A synthetic view on structure and evolution of the {Milky} {Way}},
    volume = {409},
    issn = {0004-6361},
    url = {http://adsabs.harvard.edu/abs/2003A%26A...409..523R},
    doi = {10.1051/0004-6361:20031117},
    abstract = {Since the Hipparcos mission and recent large scale surveys in 
    the optical and the near-infrared, new constraints have been obtained on 
    the structure and evolution history of the Milky Way. The population 
    synthesis approach is a useful tool to interpret such data sets and to 
    test scenarios of evolution of the Galaxy. We present here new
    constraints on evolution parameters obtained from the Besançon
    model of population synthesis and analysis of optical and near-infrared 
    star counts. The Galactic potential is computed self-consistently, in 
    agreement with Hipparcos results and the observed rotation curve. 
    Constraints are posed on the outer bulge structure, the warped and flared 
    disc, the thick disc and the spheroid populations. The model is tuned to 
    produce reliable predictions in the visible and the
    near-infrared in wide photometric bands from U to K. Finally, we describe 
    applications such as photometric and astrometric simulations and a new 
    classification tool based on a Bayesian probability estimator, which could 
    be used in the framework of Virtual Observatories. As examples, samples of 
    simulated star counts at different wavelengths and directions are also 
    given.},
    journal = {Astronomy and Astrophysics},
    author = {Robin, A. C. and Reyl\'e, C. and Derri\`ere, S. and Picaud, S.},
    month = oct,
    year = {2003},
    keywords = {Galaxy: kinematics and dynamics, Galaxy: stellar content, 
    Galaxy: evolution, Galaxy: structure, Galaxy: general},
    pages = {523--540},
    file = {NASA/ADS Full Text 
    PDF:/home/luke/local/Zotero/storage/C8C8AEW2/Robin et al. - 2003 - A 
    synthetic view on structure and evolution of the.pdf:application/pdf}
}


@article{leinert_1997_1998,
	title = {The 1997 reference of diffuse night sky brightness},
	volume = {127},
	url = {https://ui.adsabs.harvard.edu/abs/1998A%26AS..127....1L/abstract},
	doi = {10.1051/aas:1998105},
	abstract = {In the following we present material in tabular and graphical form, with the aim to allow the non-specialist to obtain a realistic estimate of the diffuse night sky brightness over a wide range of wavelengths from the far UV longward of Lyalpha to the far-infrared. At the same time the data are to provide a reference for cases in which background brightness has to be discussed, including the planning for space observations and the issue of protection of observatory sites. We try to give a critical presentation of the status at the beginning of 1997. Prepared by members of Commission 21 ``Light of the night sky'' of the IAU, including most of the recent (vice-)presidents.},
	language = {en},
	urldate = {2019-06-19},
	journal = {Astronomy and Astrophysics Supplement Series},
	author = {Leinert, Ch and Bowyer, S. and Haikala, L. K. and Hanner, M. S. and Hauser, M. G. and Levasseur-Regourd, A.-Ch and Mann, I. and Mattila, K. and Reach, W. T. and Schlosser, W. and Staude, H. J. and Toller, G. N. and Weiland, J. L. and Weinberg, J. L. and Witt, A. N.},
	month = jan,
	year = {1998},
	pages = {1},
	file = {Snapshot:/home/luke/local/Zotero/storage/UDF2CYUE/abstract.html:text/html;Submitted Version:/home/luke/local/Zotero/storage/QFU6B7XW/Leinert et al. - 1998 - The 1997 reference of diffuse night sky brightness.pdf:application/pdf}
}

@article{winn_background_2013,
	title = {Expected sky background in the {TESS} bandpass},
	journal = {TESS Science Memo No. 2, Version 1. Available upon request.},
	author = {Winn, Joshua N.},
	year = {2013}
}


@article{huang_tess_2018,
	title = {{TESS} {Discovery} of a {Transiting} {Super}-{Earth} in the pi {Mensae} {System}},
	volume = {868},
	issn = {2041-8205},
	url = {https://doi.org/10.3847%2F2041-8213%2Faaef91},
	doi = {10.3847/2041-8213/aaef91},
	abstract = {We report the detection of a transiting planet around π Men (HD 39091), using data from the Transiting Exoplanet Survey Satellite (TESS). The solar-type host star is unusually bright (V = 5.7) and was already known to host a Jovian planet on a highly eccentric, 5.7 yr orbit. The newly discovered planet has a size of 2.04 ± 0.05 R ⊕ and an orbital period of 6.27 days. Radial-velocity data from the High-Accuracy Radial-velocity Planet Searcher and Anglo-Australian Telescope/University College London Echelle Spectrograph archives also displays a 6.27 day periodicity, confirming the existence of the planet and leading to a mass determination of 4.82 ± 0.85 M ⊕. The star’s proximity and brightness will facilitate further investigations, such as atmospheric spectroscopy, asteroseismology, the Rossiter–McLaughlin effect, astrometry, and direct imaging.},
	language = {en},
	number = {2},
	urldate = {2019-06-19},
	journal = {The Astrophysical Journal},
	author = {Huang, Chelsea X. and Burt, Jennifer and Vanderburg, Andrew and Günther, Maximilian N. and Shporer, Avi and Dittmann, Jason A. and Winn, Joshua N. and Wittenmyer, Rob and Sha, Lizhou and Kane, Stephen R. and Ricker, George R. and Vanderspek, Roland K. and Latham, David W. and Seager, Sara and Jenkins, Jon M. and Caldwell, Douglas A. and Collins, Karen A. and Guerrero, Natalia and Smith, Jeffrey C. and Quinn, Samuel N. and Udry, Stéphane and Pepe, Francesco and Bouchy, François and Ségransan, Damien and Lovis, Christophe and Ehrenreich, David and Marmier, Maxime and Mayor, Michel and Wohler, Bill and Haworth, Kari and Morgan, Edward H. and Fausnaugh, Michael and Ciardi, David R. and Christiansen, Jessie and Charbonneau, David and Dragomir, Diana and Deming, Drake and Glidden, Ana and Levine, Alan M. and McCullough, P. R. and Yu, Liang and Narita, Norio and Nguyen, Tam and Morton, Tim and Pepper, Joshua and Pál, András and Rodriguez, Joseph E. and Stassun, Keivan G. and Torres, Guillermo and Sozzetti, Alessandro and Doty, John P. and Christensen-Dalsgaard, Jørgen and Laughlin, Gregory and Clampin, Mark and Bean, Jacob L. and Buchhave, Lars A. and Bakos, G. Á and Sato, Bun'ei and Ida, Shigeru and Kaltenegger, Lisa and Palle, Enric and Sasselov, Dimitar and Butler, R. P. and Lissauer, Jack and Ge, Jian and Rinehart, S. A.},
	month = nov,
	year = {2018},
	pages = {L39},
	file = {IOP Full Text PDF:/home/luke/local/Zotero/storage/9GUSHZXM/Huang et al. - 2018 - TESS Discovery of a Transiting Super-Earth in the .pdf:application/pdf}
}

@article{jenkins_spoc_2010,
	title = {Overview of the {Kepler} {Science} {Processing} {Pipeline}},
	volume = {713},
	issn = {0004-637X},
	url = {http://adsabs.harvard.edu/abs/2010ApJ...713L..87J},
	doi = {10.1088/2041-8205/713/2/L87},
	abstract = {The Kepler Mission Science Operations Center (SOC) performs several critical functions including managing the {\textasciitilde}156,000 target stars, associated target tables, science data compression tables and
parameters, as well as processing the raw photometric data downlinked from the spacecraft each month. The raw data are first calibrated at the pixel level to correct for bias, smear induced by a shutterless readout, and other detector and electronic effects. A background sky flux is estimated from {\textasciitilde}4500 pixels on each of the 84 CCD readout channels, and simple aperture photometry is performed on an optimal aperture for each star. Ancillary engineering data and diagnostic information extracted from the science data are used to remove systematic errors in the flux time series that are correlated with these data prior to searching for signatures of transiting planets with a wavelet-based, adaptive matched filter. Stars with signatures exceeding 7.1σ are subjected to a
suite of statistical tests including an examination of each star's centroid motion to reject false positives caused by background eclipsing binaries. Physical parameters for each planetary candidate are fitted to the transit signature, and signatures of additional transiting planets are sought in the residual light curve. The pipeline is operational, finding planetary signatures and providing robust eliminations of false positives.},
	urldate = {2019-06-19},
	journal = {The Astrophysical Journal Letters},
	author = {Jenkins, Jon M. and Caldwell, Douglas A. and Chandrasekaran, Hema and Twicken, Joseph D. and Bryson, Stephen T. and Quintana, Elisa V. and Clarke, Bruce D. and Li, Jie and Allen, Christopher and Tenenbaum, Peter and Wu, Hayley and Klaus, Todd C. and Middour, Christopher K. and Cote, Miles T. and McCauliff, Sean and Girouard, Forrest R. and Gunter, Jay P. and Wohler, Bill and Sommers, Jeneen and Hall, Jennifer R. and Uddin, AKM K. and Wu, Michael S. and Bhavsar, Paresh A. and Van Cleve, Jeffrey and Pletcher, David L. and Dotson, Jessie A. and Haas, Michael R. and Gilliland, Ronald L. and Koch, David G. and Borucki, William J.},
	month = apr,
	year = {2010},
	keywords = {methods: data analysis, techniques: photometric},
	pages = {L87--L91},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/HJSVFT63/Jenkins et al. - 2010 - Overview of the Kepler Science Processing Pipeline.pdf:application/pdf}
}

@article{feinstein_eleanor_2019,
	title = {eleanor: {An} open-source tool for extracting light curves from the {TESS} {Full}-{Frame} {Images}},
	shorttitle = {eleanor},
	url = {http://arxiv.org/abs/1903.09152},
	abstract = {During its two year prime mission the Transiting Exoplanet Survey Satellite (TESS) will perform a time-series photometric survey covering over 80\% of the sky. This survey comprises observations of 26 24 x 96 degree sectors that are each monitored continuously for approximately 27 days. The main goal of TESS is to find transiting planets around 200,000 pre-selected stars for which fixed aperture photometry is recorded every two minutes. However, TESS is also recording and delivering Full-Frame Images (FFIs) of each detector at a 30 minute cadence. We have created an open-source tool, eleanor, to produce light curves for objects in the TESS FFIs. Here, we describe the methods used in eleanor to produce light curves that are optimized for planet searches. The tool performs background subtraction, aperture and PSF photometry, decorrelation of instrument systematics, and cotrending using principal component analysis. We recover known transiting exoplanets in the FFIs to validate the pipeline and perform a limited search for new planet candidates in Sector 1. Our tests indicate that eleanor produces light curves with significantly less scatter than other tools that have been used in the literature. Cadence-stacked images, and raw and detrended eleanor light curves for each analyzed star will be hosted on MAST, with planet candidates on ExoFOP-TESS as Community TESS Objects of Interest (CTOIs). This work confirms the promise that the TESS FFIs will enable the detection of thousands of new exoplanets and a broad range of time domain astrophysics.},
	urldate = {2019-03-25},
	journal = {arXiv:1903.09152 [astro-ph]},
	author = {Feinstein, Adina D. and Montet, Benjamin T. and Foreman-Mackey, Daniel and Bedell, Megan E. and Saunders, Nicholas and Bean, Jacob L. and Christiansen, Jessie L. and Hedges, Christina and Luger, Rodrigo and Scolnic, Daniel and Cardoso, Jose Vinicius de Miranda},
	month = mar,
	year = {2019},
	note = {arXiv: 1903.09152},
	keywords = {Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics}
}

@article{benatti_dstuc_2019,
	title = {A possibly inflated planet around the bright, young star {DS} {Tuc} {A}},
	url = {http://arxiv.org/abs/1904.01591},
	abstract = {The origin of the observed diversity of planetary system architectures is one of the main topic of the exoplanetary research. The detection of a statistically significant sample of planets around young stars allows us to study the early stages of planet formation and evolution, but only a handful of them is known so far. In this regard, a considerable contribution is expected from the NASA TESS satellite, which is now performing a survey of \${\textbackslash}sim 85 {\textbackslash}\%\$ of the sky to search for short-period transiting planets In its first month of operations, TESS found a planet candidate with an orbital period of 8.14 days around a member of the Tuc-Hor young association (\${\textbackslash}sim\$ 40 Myr), the G6V main component of the binary system DS{\textbackslash},Tuc. If confirmed, it would be the first transiting planet around a young star suitable for radial velocity and/or atmospheric characterization. We aim to validate the planetary nature of this companion and to measure its orbital and physical parameters. We obtain accurate planet parameters by coupling an independent reprocessing of the TESS light curve with improved stellar parameters and the dilution caused by the binary companion; we analyse high precision archival radial velocities to impose an upper limit of 0.94 M\$\_\{{\textbackslash}rm Jup\}\$ on the planet mass; we finally rule out the presence of external companions beyond 40 au with adaptive optics images. We confirm the presence of a young, giant (\$\{{\textbackslash}rm R\} = 0.50\$ R\$\_\{{\textbackslash}rm Jup\}\$) and possibly inflated planet (having a theoretical mass lower than 20 M\$\_\{{\textbackslash}oplus\}\$) around DS{\textbackslash},Tuc A. We discuss the feasibility of mass determination, Rossiter-McLaughlin analysis and atmosphere characterization, allowed by the brightness of the star.},
	urldate = {2019-04-04},
	journal = {arXiv:1904.01591 [astro-ph]},
	author = {Benatti, S. and Nardiello, D. and Malavolta, L. and Desidera, S. and Borsato, L. and Nascimbeni, V. and Damasso, M. and D'Orazi, V. and Mesa, D. and Messina, S. and Esposito, M. and Bignamini, A. and Claudi, R. and Covino, E. and Lovis, C. and Sabotta, S.},
	month = apr,
	year = {2019},
	note = {arXiv: 1904.01591},
	keywords = {Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics},
	annote = {Comment: 10 pages, 7 figures. Submitted to A\&A},
	file = {arXiv\:1904.01591 PDF:/Users/luke/Zotero/storage/KPGWVZVX/Benatti et al. - 2019 - A possibly inflated planet around the bright, youn.pdf:application/pdf;arXiv.org Snapshot:/Users/luke/Zotero/storage/42I65WWA/1904.html:text/html}
}

@article{zuckerman_young_2004,
	title = {Young {Stars} {Near} the {Sun}},
	volume = {42},
	url = {https://ui.adsabs.harvard.edu/abs/2004ARA%26A..42..685Z/abstract},
	doi = {10.1146/annurev.astro.42.053102.134111},
	abstract = {Until the late 1990s the rich Hyades and the sparse UMa clusters were the only coeval, comoving concentrations of stars known within 60 pc of Earth. Both are hundreds of millions of years old. Then beginning in the late 1990s the TW Hydrae Association, the Tucana/Horologium Association, the Pictoris Moving Group, and the AB Doradus Moving Group were identified within 60 pc of Earth, and the Chamaeleontis cluster was found at 97 pc. These young groups (ages 8 50 Myr), along with other nearby, young stars, will enable imaging and spectroscopic studies of the origin and early evolution of planetary systems.},
	language = {en},
	number = {1},
	urldate = {2019-06-17},
	journal = {Annual Review of Astronomy and Astrophysics},
	author = {Zuckerman, B. and Song, Inseok},
	month = sep,
	year = {2004},
	pages = {685},
	file = {Full Text PDF:/Users/luke/Zotero/storage/AC9FIDJ2/Zuckerman and Song - 2004 - Young Stars Near the Sun.pdf:application/pdf;Snapshot:/Users/luke/Zotero/storage/YZ97WLXS/abstract.html:text/html}
}

@article{cantat-gaudin_newOCs_2019,
	title = {Gaia {DR}2 unravels incompleteness of nearby cluster population: new open clusters in the direction of {Perseus}},
	volume = {624},
	shorttitle = {Gaia {DR}2 unravels incompleteness of nearby cluster population},
	url = {https://ui.adsabs.harvard.edu/abs/2019A%26A...624A.126C/abstract},
	doi = {10.1051/0004-6361/201834453},
	abstract = {Context. Open clusters (OCs) are popular tracers of the structure and evolutionary history of the Galactic disc. The OC population is often considered to be complete within 1.8 kpc of the Sun. The recent Gaia Data Release 2 (DR2) allows the latter claim to be challenged. {\textless}BR /{\textgreater} Aims: We perform a systematic search for new OCs in the direction of Perseus using precise and accurate astrometry from Gaia DR2. {\textless}BR /{\textgreater} Methods: We implemented a coarse-to-fine search method. First, we exploited spatial proximity using a fast density-aware partitioning of the sky via a k-d tree in the spatial domain of Galactic coordinates, (l, b). Secondly, we employed a Gaussian mixture model in the proper motion space to tag fields quickly around OC candidates. Thirdly, we applied an unsupervised membership assignment method, UPMASK, to scrutinise the candidates. We visually inspected colour-magnitude diagrams to validate the detected objects. Finally, we performed a diagnostic to quantify the significance of each identified over-density in proper motion and in parallax space. {\textless}BR /{\textgreater} Results: We report the discovery of 41 new stellar clusters. This represents an increment of at least 20\% of the previously known OC population in this volume of the Milky Way. We also report on the clear identification of NGC 886, an object previously considered an asterism. This study challenges the previous claim of a near-complete sample of OCs up to 1.8 kpc. Our results reveal that this claim requires revision, and a complete census of nearby OCs is yet to be found. The list of members are only available at the CDS via anonymous ftp to {\textless}A href="http://cdsarc.u-strasbg.fr"{\textgreater}http://cdsarc.u-strasbg.fr{\textless}/A{\textgreater} (ftp://130.79.128.5) or via {\textless}A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/624/A126"{\textgreater}http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/624/A126{\textless}/A{\textgreater}},
	language = {en},
	urldate = {2019-06-18},
	journal = {Astronomy and Astrophysics},
	author = {Cantat-Gaudin, T. and Krone-Martins, A. and Sedaghat, N. and Farahi, A. and de Souza, R. S. and Skalidis, R. and Malz, A. I. and Macêdo, S. and Moews, B. and Jordi, C. and Moitinho, A. and Castro-Ginard, A. and Ishida, E. E. O. and Heneka, C. and Boucaud, A. and Trindade, A. M. M.},
	month = apr,
	year = {2019},
	pages = {A126}
}

@article{david_k2-233_2018,
	title = {Three {Small} {Planets} {Transiting} the {Bright} {Young} {Field} {Star} {K}2-233},
	volume = {155},
	url = {https://ui.adsabs.harvard.edu//#abs/2018AJ....155..222D/abstract},
	doi = {10.3847/1538-3881/aabde8},
	abstract = {We report the detection of three small transiting planets around the young K3 dwarf K2-233 (2MASS J15215519-2013539) from observations during Campaign 15 of the K2 mission. The star is relatively nearby (d = 69 pc) and bright (V = 10.7 mag, K {\textless}SUB{\textgreater} s {\textless}/SUB{\textgreater} = 8.4 mag), making the planetary system an attractive target for radial velocity follow-up and atmospheric characterization with the James Webb Space Telescope. The inner two planets are hot super-Earths (R {\textless}SUB{\textgreater} b {\textless}/SUB{\textgreater} = 1.40 ± 0.06 \{R\}{\textless}SUB{\textgreater}{\textbackslash}oplus {\textless}/SUB{\textgreater}, R {\textless}SUB{\textgreater} c {\textless}/SUB{\textgreater} = 1.34 ± 0.08 \{R\}{\textless}SUB{\textgreater}{\textbackslash}oplus {\textless}/SUB{\textgreater}), while the outer planet is a warm sub-Neptune (R {\textless}SUB{\textgreater} d {\textless}/SUB{\textgreater} = 2.6 ± 0.1 \{R\}{\textless}SUB{\textgreater}{\textbackslash}oplus {\textless}/SUB{\textgreater}). We estimate the stellar age to be \{360\}{\textless}SUB{\textgreater}-140{\textless}/SUB{\textgreater}{\textless}SUP{\textgreater}+490{\textless}/SUP{\textgreater} Myr based on rotation, activity, and kinematic indicators. The K2-233 system is particularly interesting given recent evidence for inflated radii in planets around similarly aged stars, a trend potentially related to photo-evaporation, core cooling, or both mechanisms.},
	language = {en},
	number = {5},
	urldate = {2019-01-28},
	journal = {The Astronomical Journal},
	author = {David, Trevor J. and Crossfield, Ian J. M. and Benneke, Björn and Petigura, Erik A. and Gonzales, Erica J. and Schlieder, Joshua E. and Yu, Liang and Isaacson, Howard T. and Howard, Andrew W. and Ciardi, David R. and Mamajek, Eric E. and Hillenbrand, Lynne A. and Cody, Ann Marie and Riedel, Adric and Schwengeler, Hans Martin and Tanner, Christopher and Ende, Martin},
	month = may,
	year = {2018},
	pages = {222},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/BYQHGTFG/David et al. - 2018 - Three Small Planets Transiting the Bright Young Fi.pdf:application/pdf;Snapshot:/home/luke/local/Zotero/storage/STHR4QE2/ui.adsabs.harvard.edu.html:text/html}
}

@article{david_v1298_2019,
	title = {A warm {Jupiter}-sized planet transiting the pre-main sequence star {V}1298 {Tau}},
	url = {http://arxiv.org/abs/1902.09670},
	abstract = {We report the detection of V1298 Tau b, a warm Jupiter-sized planet (\$R\_P\$ = 0.91 \${\textbackslash}pm\$ 0.05{\textasciitilde} \$R\_{\textbackslash}mathrm\{Jup\}\$, \$P = 24.1\$ days) transiting a young solar analog with an estimated age of 23 million years. The star and its planet belong to Group 29, a young association in the foreground of the Taurus-Auriga star-forming region. While hot Jupiters have been previously reported around young stars, those planets are non-transiting and near-term atmospheric characterization is not feasible. The V1298 Tau system is a compelling target for follow-up study through transmission spectroscopy and Doppler tomography owing to the transit depth (0.5{\textbackslash}\%), host star brightness (\$K\_s\$ = 8.1 mag), and rapid stellar rotation (\$v{\textbackslash}sin\{i\}\$ = 23 {\textbackslash}kms). Although the planet is Jupiter-sized, its mass is presently unknown due to high-amplitude radial velocity jitter. Nevertheless, V1298 Tau b may help constrain formation scenarios for at least one class of close-in exoplanets, providing a window into the nascent evolution of planetary interiors and atmospheres.},
	urldate = {2019-06-13},
	journal = {arXiv:1902.09670 [astro-ph]},
	author = {David, Trevor J. and Cody, Ann Marie and Hedges, Christina L. and Mamajek, Eric E. and Hillenbrand, Lynne A. and Ciardi, David R. and Beichman, Charles A. and Petigura, Erik A. and Fulton, Benjamin J. and Isaacson, Howard T. and Howard, Andrew W. and Gagné, Jonathan and Saunders, Nicholas K. and Rebull, Luisa M. and Stauffer, John R. and Vasisht, Gautam and Hinkley, Sasha},
	month = feb,
	year = {2019},
	note = {arXiv: 1902.09670},
	keywords = {Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics},
	annote = {Comment: Accepted to AJ},
	file = {arXiv\:1902.09670 PDF:/home/luke/local/Zotero/storage/66F2QUEN/David et al. - 2019 - A warm Jupiter-sized planet transiting the pre-mai.pdf:application/pdf}
}

@article{rizzuto_zeitVIII_2018,
	title = {Zodiacal {Exoplanets} in {Time} ({ZEIT}) {VIII}: {A} {Two} {Planet} {System} in {Praesepe} from {K}2 {Campaign} 16},
	shorttitle = {Zodiacal {Exoplanets} in {Time} ({ZEIT}) {VIII}},
	url = {http://arxiv.org/abs/1808.07068},
	abstract = {Young planets offer a direct view of the the formation and evolution processes that produced the diverse population of mature exoplanet systems known today. The repurposed Kepler mission K2 is providing the first sample of young transiting planets by observing populations of stars in nearby, young clusters or stellar associations. We report the detection and confirmation of two planets transiting EPIC 211964830, an M2.5 dwarf in the 650 Myr old Praesepe open cluster. Using our notch-filter search method on the K2 lightcurve, we identify planets with periods of 5.84 d and 19.66 d. This is currently the second known multi-transit system in open clusters younger than 1 Gyr. The inner planet has a radius of 2.27\$\_\{-0.16\}{\textasciicircum}\{+0.20\}\$ R\$\_{\textbackslash}oplus\$ and the outer planet has a radius of 2.77\$\_\{-0.18\}{\textasciicircum}\{+0.20\}\$ R\$\_{\textbackslash}oplus\$. Both planets are likely mini-Neptunes. These planets are expected to produce radial velocity signals of 3.4 and 2.7 m/s respectively, which is smaller than the expected stellar variability in the optical (\${\textbackslash}simeq\$30{\textbackslash},m/s), making mass measurements unlikely in the optical, but possible with future near-infrared spectrographs. We use an injection-recovery test to place robust limits on additional planets in the system, and find that planets larger than 1-2 R\$\_{\textbackslash}oplus\$ with periods of 1-20 d are unlikely, while planets larger than 2 R\$\_{\textbackslash}oplus\$ are ruled out at periods of 20-30 d.},
	urldate = {2018-08-23},
	journal = {arXiv:1808.07068 [astro-ph]},
	author = {Rizzuto, Aaron C. and Vanderburg, Andrew and Mann, Andrew W. and Kraus, Adam L. and Dressing, Courtney D. and Agüeros, Marcel A. and Douglas, Stephanie T.},
	month = aug,
	year = {2018},
	note = {arXiv: 1808.07068},
	keywords = {Astrophysics - Earth and Planetary Astrophysics}
}

@article{mann_ZEITVI_2018,
	title = {Zodiacal {Exoplanets} in {Time} ({ZEIT}). {VI}. {A} {Three}-planet {System} in the {Hyades} {Cluster} {Including} an {Earth}-sized {Planet}},
	volume = {155},
	url = {https://ui.adsabs.harvard.edu/abs/2018AJ....155....4M/abstract},
	doi = {10.3847/1538-3881/aa9791},
	abstract = {Planets in young clusters are powerful probes of the evolution of planetary systems. Here we report the discovery of three planets transiting EPIC 247589423, a late-K dwarf in the Hyades (≃800 Myr) cluster, and robust detection limits for additional planets in the system. The planets were identified from their K2 light curves as part of our survey of young clusters and star-forming regions. The smallest planet has a radius comparable to Earth (\{0.99\}{\textless}SUB{\textgreater}-0.04{\textless}/SUB{\textgreater}{\textless}SUP{\textgreater}+0.06{\textless}/SUP{\textgreater}\{R\}{\textless}SUB{\textgreater}{\textbackslash}oplus {\textless}/SUB{\textgreater}), making it one of the few Earth-sized planets with a known, young age. The two larger planets are likely a mini-Neptune and a super-Earth, with radii of \{2.91\}{\textless}SUB{\textgreater}-0.10{\textless}/SUB{\textgreater}{\textless}SUP{\textgreater}+0.11{\textless}/SUP{\textgreater}\{R\}{\textless}SUB{\textgreater}{\textbackslash}oplus {\textless}/SUB{\textgreater} and \{1.45\}{\textless}SUB{\textgreater}-0.08{\textless}/SUB{\textgreater}{\textless}SUP{\textgreater}+0.11{\textless}/SUP{\textgreater}\{R\}{\textless}SUB{\textgreater}{\textbackslash}oplus {\textless}/SUB{\textgreater}, respectively. The predicted radial velocity signals from these planets are between 0.4 and 2 m s{\textless}SUP{\textgreater}-1{\textless}/SUP{\textgreater}, achievable with modern precision RV spectrographs. Because the target star is bright (V = 11.2) and has relatively low-amplitude stellar variability for a young star (2-6 mmag), EPIC 247589423 hosts the best known planets in a young open cluster for precise radial velocity follow-up, enabling a robust test of earlier claims that young planets are less dense than their older counterparts.},
	language = {en},
	number = {1},
	urldate = {2019-06-13},
	journal = {The Astronomical Journal},
	author = {Mann, Andrew W. and Vanderburg, Andrew and Rizzuto, Aaron C. and Kraus, Adam L. and Berlind, Perry and Bieryla, Allyson and Calkins, Michael L. and Esquerdo, Gilbert A. and Latham, David W. and Mace, Gregory N. and Morris, Nathan R. and Quinn, Samuel N. and Sokal, Kimberly R. and Stefanik, Robert P.},
	month = jan,
	year = {2018},
	pages = {4},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/8WTHFEBM/Mann et al. - 2018 - Zodiacal Exoplanets in Time (ZEIT). VI. A Three-pl.pdf:application/pdf;Snapshot:/home/luke/local/Zotero/storage/BX769L9X/abstract.html:text/html}
}

@article{livingston_k2-264_2019,
	title = {K2-264: a transiting multiplanet system in the {Praesepe} open cluster},
	volume = {484},
	issn = {0035-8711},
	shorttitle = {K2-264},
	url = {https://academic.oup.com/mnras/article/484/1/8/5255202},
	doi = {10.1093/mnras/sty3464},
	abstract = {ABSTRACT.  Planet host stars with well-constrained ages provide a rare window to the time domain of planet formation and evolution. The NASA K2 mission has enab},
	language = {en},
	number = {1},
	urldate = {2019-06-13},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Livingston, John H. and Dai, Fei and Hirano, Teruyuki and Gandolfi, Davide and Trani, Alessandro A. and Nowak, Grzegorz and Cochran, William D. and Endl, Michael and Albrecht, Simon and Barragan, Oscar and Cabrera, Juan and Csizmadia, Szilard and de Leon, Jerome P. and Deeg, Hans and Eigmüller, Philipp and Erikson, Anders and Fridlund, Malcolm and Fukui, Akihiko and Grziwa, Sascha and Guenther, Eike W. and Hatzes, Artie P. and Korth, Judith and Kuzuhara, Masayuki and Montañes, Pilar and Narita, Norio and Nespral, David and Palle, Enric and Pätzold, Martin and Persson, Carina M. and Prieto-Arranz, Jorge and Rauer, Heike and Tamura, Motohide and Van Eylen, Vincent and Winn, Joshua N.},
	month = mar,
	year = {2019},
	pages = {8--18},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/CGA4ISLF/Livingston et al. - 2019 - K2-264 a transiting multiplanet system in the Pra.pdf:application/pdf;Snapshot:/home/luke/local/Zotero/storage/YAENN2LG/5255202.html:text/html}
}

@article{livingston_three_2018,
	title = {Three {Small} {Planets} {Transiting} a {Hyades} {Star}},
	volume = {155},
	issn = {1538-3881},
	url = {https://doi.org/10.3847%2F1538-3881%2Faaa841},
	doi = {10.3847/1538-3881/aaa841},
	abstract = {We present the discovery of three small planets transiting K2-136 (LP 358 348, EPIC 247589423), a late K dwarf in the Hyades. The planets have orbital periods of 7.9757 ± 0.0011, , and , and radii of 1.05 ± 0.16, 3.14 ± 0.36, and , respectively. With an age of 600–800 Myr, these planets are some of the smallest and youngest transiting planets known. Due to the relatively bright (J = 9.1) host star, the planets are compelling targets for future characterization via radial velocity mass measurements and transmission spectroscopy. As the first known star with multiple transiting planets in a cluster, the system should be helpful for testing theories of planet formation and migration.},
	language = {en},
	number = {3},
	urldate = {2019-06-13},
	journal = {The Astronomical Journal},
	author = {Livingston, John H. and Dai, Fei and Hirano, Teruyuki and Gandolfi, Davide and Nowak, Grzegorz and Endl, Michael and Velasco, Sergio and Fukui, Akihiko and Narita, Norio and Prieto-Arranz, Jorge and Barragan, Oscar and Cusano, Felice and Albrecht, Simon and Cabrera, Juan and Cochran, William D. and Csizmadia, Szilard and Deeg, Hans J. and Eigmüller, Philipp and Erikson, Anders and Fridlund, Malcolm and Grziwa, Sascha and Guenther, Eike W. and Hatzes, Artie P. and Kawauchi, Kiyoe and Korth, Judith and Nespral, David and Palle, Enric and Pätzold, Martin and Persson, Carina M. and Rauer, Heike and Smith, Alexis M. S. and Tamura, Motohide and Tanaka, Yusuke and Eylen, Vincent Van and Watanabe, Noriharu and Winn, Joshua N.},
	month = feb,
	year = {2018},
	pages = {115},
	file = {IOP Full Text PDF:/home/luke/local/Zotero/storage/33DECSL4/Livingston et al. - 2018 - Three Small Planets Transiting a Hyades Star.pdf:application/pdf}
}


@article{ciardi_k2-136_2018,
	title = {K2-136: {A} {Binary} {System} in the {Hyades} {Cluster} {Hosting} a {Neptune}-sized {Planet}},
	volume = {155},
	issn = {1538-3881},
	shorttitle = {K2-136},
	url = {http://stacks.iop.org/1538-3881/155/i=1/a=10},
	doi = {10.3847/1538-3881/aa9921},
	abstract = {We report the discovery of a Neptune-size planet ( \#\#IMG\#\# [http://ej.iop.org/images/1538-3881/155/1/10/ajaa9921ieqn1.gif] \$R\_{\textbackslash}rmp=3.0{\textbackslash},R\_øplus \$ ) in the Hyades Cluster. The host star is in a binary system, comprising a K5V star and M7/8V star with a projected separation of 40 au. The planet orbits the primary star with an orbital period of 17.3 days and a transit duration of 3 hrs. The host star is bright ( V = 11.2, J = 9.1) and so may be a good target for precise radial velocity measurements. K2-136A c is the first Neptune-sized planet to be found orbiting in a binary system within an open cluster. The Hyades is the nearest star cluster to the Sun, has an age of 625–750 Myr, and forms one of the fundamental rungs in the distance ladder; understanding the planet population in such a well-studied cluster can help us understand and set constraints on the formation and evolution of planetary systems.},
	language = {en},
	number = {1},
	urldate = {2017-12-20},
	journal = {The Astronomical Journal},
	author = {Ciardi, David R. and Crossfield, Ian J. M. and Feinstein, Adina D. and Schlieder, Joshua E. and Petigura, Erik A. and David, Trevor J. and Bristow, Makennah and Patel, Rahul I. and Arnold, Lauren and Benneke, Björn and Christiansen, Jessie L. and Dressing, Courtney D. and Fulton, Benjamin J. and Howard, Andrew W. and Isaacson, Howard and Sinukoff, Evan and Thackeray, Beverly},
	year = {2018},
	keywords = {planets and satellites: detection, K2-136A c, K2-136AB, stars: individual: EPIC 247589423AB},
	pages = {10}
}

@article{vanderburg_zeitVII_2018,
	title = {Zodiacal {Exoplanets} in {Time} ({ZEIT}) {VII}: {A} {Temperate} {Candidate} {Super}-{Earth} in the {Hyades} {Cluster}},
	shorttitle = {Zodiacal {Exoplanets} in {Time} ({ZEIT}) {VII}},
	url = {http://arxiv.org/abs/1805.11117},
	abstract = {Transiting exoplanets in young open clusters present opportunities to study how exoplanets evolve over their lifetimes. Recently, significant progress detecting transiting planets in young open clusters has been made with the K2 mission, but so far all of these transiting cluster planets orbit close to their host stars, so planet evolution can only be studied in a high-irradiation regime. Here, we report the discovery of a long-period planet candidate, called HD 283869 b, orbiting a member of the Hyades cluster. Using data from the K2 mission, we detected a single transit of a super-Earth-sized (1.96 +/- 0.12 R\_earth) planet candidate orbiting the K-dwarf HD 283869 with a period longer than 72 days. Since we only detected a single transit event, we cannot validate HD 283869 b with high confidence, but our analysis of the K2 images, archival data, and follow-up observations suggests that the source of the event is indeed a transiting planet. We estimated the candidate's orbital parameters and find that if real, it has a period P{\textasciitilde}100 days and receives approximately Earth-like incident flux, giving the candidate a 71\% chance of falling within the circumstellar habitable zone. If confirmed, HD 283869 b would have the longest orbital period, lowest incident flux, and brightest host star of any known transiting planet in an open cluster, making it uniquely important to future studies of how stellar irradiation affects planetary evolution.},
	urldate = {2018-05-30},
	journal = {arXiv:1805.11117 [astro-ph]},
	author = {Vanderburg, Andrew and Mann, Andrew W. and Rizzuto, Aaron and Bieryla, Allyson and Kraus, Adam L. and Berlind, Perry and Calkins, Michael L. and Curtis, Jason L. and Douglas, Stephanie T. and Esquerdo, Gilbert A. and Everett, Mark E. and Horch, Elliott P. and Howell, Steve B. and Latham, David W. and Mayo, Andrew W. and Quinn, Samuel N. and Scott, Nicholas J. and Stefanik, Robert P.},
	month = may,
	year = {2018},
	note = {arXiv: 1805.11117},
	keywords = {Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics},
	annote = {Comment: 13 pages, 9 figures, 1 table. Accepted in AJ},
	file = {arXiv\:1805.11117 PDF:/home/luke/local/Zotero/storage/M9GF26VN/Vanderburg et al. - 2018 - Zodiacal Exoplanets in Time (ZEIT) VII A Temperat.pdf:application/pdf;arXiv.org Snapshot:/home/luke/local/Zotero/storage/QIENYX7L/1805.html:text/html}
}

@article{obermeier_k2_2016,
	title = {K2 {Discovers} a {Busy} {Bee}: {An} {Unusual} {Transiting} {Neptune} {Found} in the {Beehive} {Cluster}},
	volume = {152},
	issn = {0004-6256},
	shorttitle = {K2 {Discovers} a {Busy} {Bee}},
	url = {http://adsabs.harvard.edu/abs/2016AJ....152..223O},
	doi = {10.3847/1538-3881/152/6/223},
	abstract = {Open clusters have been the focus of several exoplanet surveys, but only 
a few planets have so far been discovered. The Kepler spacecraft
revealed an abundance of small planets around small cool stars,
therefore, such cluster members are prime targets for exoplanet transit
searches. Kepler's new mission, K2, is targeting several open clusters
and star-forming regions around the ecliptic to search for transiting
planets around their low-mass constituents. Here, we report the
discovery of the first transiting planet in the intermediate-age (800
Myr) Beehive cluster (Praesepe). K2-95 is a faint (K\{\{p\}\}=15.5 \{mag\})
\{\{M\}\}3.0+/- 0.5 dwarf from K2's Campaign 5 with an effective temperature
of 3471+/- 124 \{\{K\}\}, approximately solar metallicity and a radius of
0.402+/- 0.050 \{R\}⊙ . We detected a transiting planet
with a radius of \{3.47\}-0.53+0.78 \{R\}{\textbackslash}oplus
 and an orbital period of 10.134 days. We combined photometry,
medium/high-resolution spectroscopy, adaptive optics/speckle imaging,
and archival survey images to rule out any false-positive detection
scenarios, validate the planet, and further characterize the system. The
planet’s radius is very unusual as M-dwarf field stars rarely have
Neptune-sized transiting planets. The comparatively large radius of
K2-95b is consistent with the other recently discovered cluster planets
K2-25b (Hyades) and K2-33b (Upper Scorpius), indicating systematic
differences in their evolutionary states or formation. These discoveries
from K2 provide a snapshot of planet formation and evolution in cluster
environments and thus make excellent laboratories to test differences
between field-star and cluster planet populations.},
	journal = {The Astronomical Journal},
	author = {Obermeier, Christian and Henning, Thomas and Schlieder, Joshua E. and Crossfield, Ian J. M. and Petigura, Erik A. and Howard, Andrew W. and Sinukoff, Evan and Isaacson, Howard and Ciardi, David R. and David, Trevor J. and Hillenbrand, Lynne A. and Beichman, Charles A. and Howell, Steve B. and Horch, Elliott and Everett, Mark and Hirsch, Lea and Teske, Johanna and Christiansen, Jessie L. and Lépine, Sébastien and Aller, Kimberly M. and Liu, Michael C. and Saglia, Roberto P. and Livingston, John and Kluge, Matthias},
	month = dec,
	year = {2016},
	keywords = {techniques: photometric, techniques: spectroscopic, Stars: Low-Mass, eclipses, stars: individual: K2-95},
	pages = {223},
	file = {NASA/ADS Full Text PDF:/home/luke/local/Zotero/storage/F8WAPVHD/Obermeier et al. - 2016 - K2 Discovers a Busy Bee An Unusual Transiting Nep.pdf:application/pdf}
}

@article{brucalassi_search_2017,
	title = {Search for giant planets in {M} 67. {IV}. {Survey} results},
	volume = {603},
	url = {https://ui.adsabs.harvard.edu/abs/2017A%26A...603A..85B/abstract},
	doi = {10.1051/0004-6361/201527562},
	abstract = {Context. We present the results of a seven-year-long radial velocity survey of a sample of 88 main-sequence and evolved stars to reveal signatures of Jupiter-mass planets in the solar-age and solar-metallicity open cluster M 67. {\textless}BR /{\textgreater} Aims: We aim at studying the frequency of giant planets in this cluster with respect to the field stars. In addition, our sample is also ideal to perform a long-term study to compare the chemical composition of stars with and without giant planets in detail. {\textless}BR /{\textgreater} Methods: We analyzed precise radial velocity (RV) measurements obtained with the HARPS spectrograph at the European Southern Observatory (La Silla), the SOPHIE spectrograph at the Observatoire de Haute-Provence (France), the HRS spectrograph at the Hobby Eberly Telescope (Texas), and the HARPS-N spectrograph at the Telescopio Nazionale Galileo (La Palma). Additional RV data come from the CORALIE spectrograph at the Euler Swiss Telescope (La Silla). We conducted Monte Carlo simulations to estimate the occurrence rate of giant planets in our radial velocity survey. We considered orbital periods between 1.0 day and 1000 days and planet masses between 0.2 M{\textless}SUB{\textgreater}J{\textless}/SUB{\textgreater} and 10.0 M{\textless}SUB{\textgreater}J{\textless}/SUB{\textgreater}. We used a measure of the observational detection efficiency to determine the frequency of planets for each star. {\textless}BR /{\textgreater} Results: All the planets previously announced in this RV campaign with their properties are summarized here: 3 hot Jupiters around the main-sequence stars YBP1194, YBP1514, and YBP401, and 1 giant planet around the evolved star S364. Two additional planet candidates around the stars YBP778 and S978 are also analyzed in the present work. We discuss stars that exhibit large RV variability or trends individually. For 2 additional stars, long-term trends are compatible with new binary candidates or substellar objects, which increases the total number of binary candidates detected in our campaign to 14. Based on the Doppler-detected planets discovered in this survey, we find an occurrence of giant planets of 18.0{\textless}SUP{\textgreater}+12.0{\textless}/SUP{\textgreater}{\textless}SUB{\textgreater}-8.0{\textless}/SUB{\textgreater}\% in the selected period-mass range. This frequency is slightly higher but consistent within the errors with the estimate for the field stars, which leads to the general conclusion that open cluster and field statistics agree. However, we find that the rate of hot Jupiters in the cluster ( 5.7{\textless}SUP{\textgreater}+5.5{\textless}/SUP{\textgreater}{\textless}SUB{\textgreater}-3.0{\textless}/SUB{\textgreater}\%) is substantially higher than in the field. Based on observations collected at the ESO 3.6m telescope (La Silla), at the 1.93 m telescope of the Observatoire de Haute-Provence (OHP, France), at the Hobby Eberly Telescope (HET, Texas), at the Telescopio Nazionale Galileo (TNG, La Palma) and at the Euler Swiss Telescope (La Silla).Individual RV measurements are available at the CDS via anonymous ftp to {\textless}A href="http://cdsarc.u-strasbg.fr"{\textgreater}http://cdsarc.u-strasbg.fr{\textless}/A{\textgreater} ({\textless}A href="http://130.79.128.5"{\textgreater}http://130.79.128.5{\textless}/A{\textgreater}) or via {\textless}A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/603/A85"{\textgreater}http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/603/A85{\textless}/A{\textgreater}},
	language = {en},
	urldate = {2019-06-13},
	journal = {Astronomy and Astrophysics},
	author = {Brucalassi, A. and Koppenhoefer, J. and Saglia, R. and Pasquini, L. and Ruiz, M. T. and Bonifacio, P. and Bedin, L. R. and Libralato, M. and Biazzo, K. and Melo, C. and Lovis, C. and Randich, S.},
	month = jul,
	year = {2017},
	pages = {A85}
}

@article{flagg_co_2019,
	title = {{CO} {Detected} in {CI} {Tau} b: {Hot} {Start} {Implied} by {Planet} {Mass} and {M}\$\_K\$},
	shorttitle = {{CO} {Detected} in {CI} {Tau} b},
	url = {http://arxiv.org/abs/1906.02860},
	abstract = {We acquired high resolution IR spectra of CI Tau, the host star of one of the few young planet candidates amenable to direct spectroscopic detection. We confirm the planet's existence with a direct detection of CO in the planet's atmosphere. We also calculate a mass of 11.6 M\$\_J\$ based on the amplitude of its radial velocity variations. We estimate its flux contrast with its host star to get an absolute magnitude estimate for the planet of 8.17 in the K band. This magnitude implies the planet formed via a "hot start" formation mechanism. This makes CI Tau b the youngest confirmed exoplanet as well as the first exoplanet around a T Tauri star with a directly determined, model-independent, dynamical mass.},
	urldate = {2019-06-12},
	journal = {arXiv:1906.02860 [astro-ph]},
	author = {Flagg, Laura and Johns-Krull, Christopher M. and Nofi, Larissa and Llama, Joe and Prato, L. and Sullivan, Kendall and Jaffe, D. T. and Mace, Gregory},
	month = jun,
	year = {2019},
	note = {arXiv: 1906.02860},
	keywords = {Astrophysics - Earth and Planetary Astrophysics},
	annote = {Comment: accepted to ApJ Letters; 7 pages, 2 figures},
	file = {arXiv\:1906.02860 PDF:/Users/luke/Zotero/storage/DRMX4NS9/Flagg et al. - 2019 - CO Detected in CI Tau b Hot Start Implied by Plan.pdf:application/pdf;arXiv.org Snapshot:/Users/luke/Zotero/storage/EUSNVSC6/1906.html:text/html}
}

@article{johns-krull_candidate_2016,
	title = {A {CANDIDATE} {YOUNG} {MASSIVE} {PLANET} {IN} {ORBIT} {AROUND} {THE} {CLASSICAL} {T} {TAURI} {STAR} {CI} {TAU}},
	volume = {826},
	issn = {0004-637X},
	url = {https://doi.org/10.3847%2F0004-637x%2F826%2F2%2F206},
	doi = {10.3847/0004-637X/826/2/206},
	abstract = {The ∼2 Myr old classical T Tauri star CI Tau shows periodic variability in its radial velocity (RV) variations measured at infrared (IR) and optical wavelengths. We find that these observations are consistent with a massive planet in a ∼9 day period orbit. These results are based on 71 IR RV measurements of this system obtained over five years, and on 26 optical RV measurements obtained over nine years. CI Tau was also observed photometrically in the optical on 34 nights over ∼one month in 2012. The optical RV data alone are inadequate to identify an orbital period, likely the result of star spot and activity-induced noise for this relatively small data set. The infrared RV measurements reveal significant periodicity at ∼9 days. In addition, the full set of optical and IR RV measurements taken together phase coherently and with equal amplitudes to the ∼9 day period. Periodic RV signals can in principle be produced by cool spots, hotspots, and reflection of the stellar spectrum off the inner disk, in addition to resulting from a planetary companion. We have considered each of these and find the planet hypothesis most consistent with the data. The RV amplitude yields an of ∼8.1 M Jup; in conjunction with a 1.3 mm continuum emission measurement of the circumstellar disk inclination from the literature, we find a planet mass of ∼11.3 M Jup, assuming alignment of the planetary orbit with the disk.},
	language = {en},
	number = {2},
	urldate = {2019-06-13},
	journal = {The Astrophysical Journal},
	author = {Johns-Krull, Christopher M. and McLane, Jacob N. and Prato, L. and Crockett, Christopher J. and Jaffe, Daniel T. and Hartigan, Patrick M. and Beichman, Charles A. and Mahmud, Naved I. and Chen, Wei and Skiff, B. A. and Cauley, P. Wilson and Jones, Joshua A. and Mace, G. N.},
	month = aug,
	year = {2016},
	pages = {206},
	file = {IOP Full Text PDF:/Users/luke/Zotero/storage/LAJ7VWTZ/Johns-Krull et al. - 2016 - A CANDIDATE YOUNG MASSIVE PLANET IN ORBIT AROUND T.pdf:application/pdf}
}

@article{donati_hj_2016,
	title = {A hot {Jupiter} orbiting a 2-million-year-old solar-mass {T} {Tauri} star},
	volume = {advance online publication},
	copyright = {© 2016 Nature Publishing Group, a division of Macmillan Publishers Limited. All Rights Reserved.},
	issn = {0028-0836},
	url = {http://www.nature.com/nature/journal/vaop/ncurrent/full/nature18305.html},
	doi = {10.1038/nature18305},
	abstract = {Hot Jupiters are giant Jupiter-like exoplanets that orbit their host stars 100 times more closely than Jupiter orbits the Sun. These planets presumably form in the outer part of the primordial disk from which both the central star and surrounding planets are born, then migrate inwards and yet avoid falling into their host star. It is, however, unclear whether this occurs early in the lives of hot Jupiters, when they are still embedded within protoplanetary disks, or later, once multiple planets are formed and interact. Although numerous hot Jupiters have been detected around mature Sun-like stars, their existence has not yet been firmly demonstrated for young stars, whose magnetic activity is so intense that it overshadows the radial velocity signal that close-in giant planets can induce. Here we report that the radial velocities of the young star V830 Tau exhibit a sine wave of period 4.93 days and semi-amplitude 75 metres per second, detected with a false-alarm probability of less than 0.03 per cent, after filtering out the magnetic activity plaguing the spectra. We find that this signal is unrelated to the 2.741-day rotation period of V830 Tau and we attribute it to the presence of a planet of mass 0.77 times that of Jupiter, orbiting at a distance of 0.057 astronomical units from the host star. Our result demonstrates that hot Jupiters can migrate inwards in less than two million years, probably as a result of planet–disk interactions.},
	language = {en},
	urldate = {2016-06-28},
	journal = {Nature},
	author = {Donati, J. F. and Moutou, C. and Malo, L. and Baruteau, C. and Yu, L. and Hébrard, E. and Hussain, G. and Alencar, S. and Ménard, F. and Bouvier, J. and Petit, P. and Takami, M. and Doyon, R. and Cameron, A. Collier},
	month = jun,
	year = {2016},
	annote = {Hot Jupiters are giant Jupiter-like exoplanets that orbit their host stars 100 times more closely than Jupiter orbits the Sun. These planets presumably form in the outer part of the primordial disk from which both the central star and surrounding planets are born, then migrate inwards and yet avoid falling into their host star1. It is, however, unclear whether this occurs early in the lives of hot Jupiters, when they are still embedded within protoplanetary disks2, or later, once multiple planets are formed and interact3. Although numerous hot Jupiters have been detected around mature Sun-like stars, their existence has not yet been firmly demonstrated for young stars4, 5, 6, whose magnetic activity is so intense that it overshadows the radial velocity signal that close-in giant planets can induce. Here we report that the radial velocities of the young star V830 Tau exhibit a sine wave of period 4.93 days and semi-amplitude 75 metres per second, detected with a false-alarm probability of less than 0.03 per cent, after filtering out the magnetic activity plaguing the spectra. We find that this signal is unrelated to the 2.741-day rotation period of V830 Tau and we attribute it to the presence of a planet of mass 0.77 times that of Jupiter, orbiting at a distance of 0.057 astronomical units from the host star. Our result demonstrates that hot Jupiters can migrate inwards in less than two million years, probably as a result of planet–disk interactions2.
It seems like they were careful with their signal analysis, but if any of the 3 claims of planets around young stars from the past {\textasciitilde}month are wrong... seems likely to be the one where RV data is the only source.},
	file = {Full Text PDF:/Users/luke/Zotero/storage/XJK3X2Q9/Donati et al. - 2016 - A hot Jupiter orbiting a 2-million-year-old solar-.pdf:application/pdf;Snapshot:/Users/luke/Zotero/storage/WNS77MDA/nature18305.html:text/html}
}

@article{meibom_spin-down_2015,
	title = {A spin-down clock for cool stars from observations of a 2.5-billion-year-old cluster},
	volume = {517},
	copyright = {© 2015 Nature Publishing Group, a division of Macmillan Publishers Limited. All Rights Reserved.},
	issn = {0028-0836},
	url = {http://www.nature.com/nature/journal/v517/n7536/full/nature14118.html},
	doi = {10.1038/nature14118},
	abstract = {The ages of the most common stars—low-mass (cool) stars like the Sun, and smaller—are difficult to derive because traditional dating methods use stellar properties that either change little as the stars age or are hard to measure. The rotation rates of all cool stars decrease substantially with time as the stars steadily lose their angular momenta. If properly calibrated, rotation therefore can act as a reliable determinant of their ages based on the method of gyrochronology. To calibrate gyrochronology, the relationship between rotation period and age must be determined for cool stars of different masses, which is best accomplished with rotation period measurements for stars in clusters with well-known ages. Hitherto, such measurements have been possible only in clusters with ages of less than about one billion years, and gyrochronology ages for older stars have been inferred from model predictions. Here we report rotation period measurements for 30 cool stars in the 2.5-billion-year-old cluster NGC 6819. The periods reveal a well-defined relationship between rotation period and stellar mass at the cluster age, suggesting that ages with a precision of order 10 per cent can be derived for large numbers of cool Galactic field stars.},
	language = {en},
	number = {7536},
	urldate = {2016-10-08},
	journal = {Nature},
	author = {Meibom, Søren and Barnes, Sydney A. and Platais, Imants and Gilliland, Ronald L. and Latham, David W. and Mathieu, Robert D.},
	month = jan,
	year = {2015},
	keywords = {STARS},
	pages = {589--591},
	annote = {gyrochronology should work up to 10\% precision (i.e. you should be able to estimate ages to 10\% precision by measuring a star's rotation period, its mass, and to weaker order its metallicity).
Note difference from van Saders 2016, which says: ya, but not up to 4Gyr?! (kind of arbitrary)},
	file = {Snapshot:/Users/luke/Zotero/storage/M2WCJIKX/nature14118.html:text/html}
}

@article{barnes_color-period_2015,
	title = {A color-period diagram for the open cluster {M} 48 ({NGC} 2548), and its rotational age},
	volume = {583},
	issn = {0004-6361, 1432-0746},
	doi = {10.1051/0004-6361/201526129},
	abstract = {Rotation periods are increasingly being used to derive ages for cool single field stars. Such ages are based on an empirical understanding of how cool stars spin down, acquired by constructing color-period diagrams (CPDs) for a series of open clusters. Our main aims here are to construct a CPD for M 48, to compare this with other clusters of similar age to check for consistency, and to derive a rotational age for M 48 using gyrochronology. We monitored M 48 photometrically for over 2 months with AIP's STELLA I 1.2 m telescope and the WiFSIP 4K imager in Tenerife. Light curves with 3 mmag precision for bright (V{\textasciitilde}14 mag) stars were produced and then analysed to provide rotation periods. A cluster CPD has then been constructed. We report 62 rotation periods for cool stars in M 48. The CPD displays a clear slow/I-sequence of rotating stars, similar to those seen in the 625 Myr-old Hyades and 590 Myr-old Praesepe clusters, and below both, confirming that M 48 is younger. A similar comparison with the 250 Myr-old M 34 cluster shows that M 48 is older and does not possess any fast/C-sequence G or early K stars like those in M 34, although relatively fast rotators do seem to be present among the late-K and M stars. A more detailed comparison of the CPD with rotational evolution models shows that the cluster stars have a mean age of 450 Myr, and its (rotating) stars can be individually dated to +-117 Myr (26\%). Much of this uncertainty stems from intrinsic astrophysical spread in initial periods, and almost all stars are consistent with a single age of 450 Myr. The gyro-age of M 48 as a whole is 450+-50 Myr, in agreement with the previously determined isochrone age of 400+-100 Myr.},
	urldate = {2019-06-02},
	journal = {Astronomy \& Astrophysics},
	author = {Barnes, Sydney A. and Weingrill, Jörg and Granzer, Thomas and Spada, Federico and Strassmeier, Klaus G.},
	month = nov,
	year = {2015},
	keywords = {Astrophysics - Solar and Stellar Astrophysics},
	pages = {A73}
}

@article{curtis_tess_2019,
	title = {{TESS} reveals that the nearby {Pisces}-{Eridanus} stellar stream is only 120 {Myr} old},
	url = {http://arxiv.org/abs/1905.10588},
	abstract = {Pisces-Eridanus (Psc-Eri), a nearby (\$d\$ \${\textbackslash}simeq\$ 80-226 pc) stellar stream stretching across \${\textbackslash}approx\$120 degrees of the sky, was recently discovered with Gaia data. The stream was claimed to be \${\textbackslash}approx\$1 Gyr old, which would make it an exceptional discovery for stellar astrophysics, as star clusters of that age are rare and tend to be distant, limiting their utility as benchmark samples. We test this old age for Psc-Eri in two ways. First, we compare the rotation periods for 101 low-mass members (measured using time series photometry from the Transiting Exoplanet Survey Satellite, TESS) to those of well-studied open clusters. Second, we identify 34 new high-mass candidate members, including the notable stars \${\textbackslash}lambda\$ Tauri (an Algol-type eclipsing binary) and HD 1160 (host to a directly imaged object near the hydrogen-burning limit). We conduct an isochronal analysis of the color--magnitude data for these highest-mass members, again comparing our results to those for open clusters. Both analyses show that the stream has an age consistent with that of the Pleiades, i.e., \${\textbackslash}approx\$120 Myr. This makes the Psc-Eri stream an exciting source of young benchmarkable stars and, potentially, exoplanets located in a more diffuse environment that is distinct from that of the Pleiades and of other dense star clusters.},
	urldate = {2019-05-28},
	journal = {arXiv:1905.10588 [astro-ph]},
	author = {Curtis, Jason Lee and Ag\"ueros, Marcel A. and Mamajek, Eric E. and Wright, Jason T. and Cummings, Jeffrey D.},
	month = may,
	year = {2019},
	note = {arXiv: 1905.10588},
	keywords = {Astrophysics - Solar and Stellar Astrophysics}
}


@article{weldrake_searching_2006,
	title = {Searching for {Planetary} {Transits} in {Globular} {Clusters} - 47 {Tucanae} and omega {Centauri}},
	url = {http://arxiv.org/abs/astro-ph/0612215},
	abstract = {We have performed a large ground-based search for transiting Hot Jupiter planets in the outer regions of the globular clusters 47 Tucanae and omega Centauri. The aim was to help understand the role that environmental effects play on Hot Jupiter formation and survivability in globular clusters. Using the ANU 1m telescope and a 52' X 52' field, a total of 54,000 solar-type stars were searched for transits in both clusters with fully tested transit-finding algorithms. Detailed Monte Carlo simulations were performed to model the datasets and calculate the expected planet yields. Seven planets were expected in 47 Tuc, and five in omega Cen. Despite a detailed search, no planet-like candidates were identified in either cluster. Combined with previous theoretical studies of planet survivability, and the HST null result in the core of 47 Tuc, the lack of detections in the uncrowded outer regions of both clusters indicates that stellar metallicity is the dominant factor inhibiting Hot Jupiter formation in the cluster environment.},
	urldate = {2016-09-13},
	journal = {arXiv:astro-ph/0612215},
	author = {Weldrake, David T. F. and Sackett, Penny D. and Bridges, Terry J.},
	month = dec,
	year = {2006},
	note = {arXiv: astro-ph/0612215},
	keywords = {Astrophysics},
	annote = {Comment: 6 pages, 2 figures. To appear in the PASP proceedings of "Transiting Extrasolar Planets Workshop" MPIA Heidelberg Germany, 25th-28th September 2006. Eds: Cristina Afonso, David Weldrake \& Thomas Henning},
	file = {arXiv\:astro-ph/0612215 PDF:/Users/luke/Zotero/storage/GPB2AMXG/Weldrake et al. - 2006 - Searching for Planetary Transits in Globular Clust.pdf:application/pdf;arXiv.org Snapshot:/Users/luke/Zotero/storage/FRP8XP73/0612215.html:text/html}
}

@article{gilliland_lack_2000,
	title = {A {Lack} of {Planets} in 47 {Tucanae} from a {Hubble} {Space} {Telescope} {Search}},
	volume = {545},
	issn = {1538-4357},
	url = {http://stacks.iop.org/1538-4357/545/i=1/a=L47},
	doi = {10.1086/317334},
	abstract = {We report results from a large Hubble Space Telescope project to observe a significant ( 34,000) ensemble of main-sequence stars in the globular cluster 47 Tucanae with a goal of defining the frequency of inner orbit, gas giant planets. Simulations based on the characteristics of the 8.3 days of time series data in the F555W and F814W Wide Field Planetary Camera 2 (WFPC2) filters show that 17 planets should be detected by photometric transit signals if the frequency of hot Jupiters found in the solar neighborhood is assumed to hold for 47 Tuc. The experiment provided high-quality data sufficient to detect planets. A full analysis of these WFPC2 data reveals 75 variables, but no light curves resulted for which a convincing interpretation as a planet could be made. The planet frequency in 47 Tuc is at least an order of magnitude below that for the solar neighborhood. The cause of the absence of close-in planets in 47 Tuc is not yet known; presumably the low metallicity and/or crowding of 47 Tuc interfered with planet formation, with orbital evolution to close-in positions, or with planet survival.},
	language = {en},
	number = {1},
	urldate = {2016-09-02},
	journal = {The Astrophysical Journal Letters},
	author = {Gilliland, Ronald L. and Brown, T. M. and Guhathakurta, P. and Sarajedini, A. and Milone, E. F. and Albrow, M. D. and Baliber, N. R. and Bruntt, H. and Burrows, A. and Charbonneau, D. and Choi, P. and Cochran, W. D. and Edmonds, P. D. and Frandsen, S. and Howell, J. H. and Lin, D. N. C. and Marcy, G. W. and Mayor, M. and Naef, D. and Sigurdsson, S. and Stagg, C. R. and Vandenberg, D. A. and Vogt, S. S. and Williams, M. D.},
	year = {2000},
	pages = {L47},
	file = {IOP Full Text PDF:/Users/luke/Zotero/storage/KAQN32IV/Gilliland et al. - 2000 - A Lack of Planets in 47 Tucanae from a Hubble Spac.pdf:application/pdf}
}

@article{howell_k2_2014,
	title = {The {K}2 {Mission}: {Characterization} and {Early} {Results}},
	volume = {126},
	issn = {1538-3873},
	shorttitle = {The {K}2 {Mission}},
	url = {http://stacks.iop.org/1538-3873/126/i=938/a=398},
	doi = {10.1086/676406},
	abstract = {The K2 mission will make use of the Kepler spacecraft and its assets to expand upon Kepler's groundbreaking discoveries in the fields of exoplanets and astrophysics through new and exciting observations. K2 will use an innovative way of operating the spacecraft to observe target fields along the ecliptic for the next 2-3 years. Early science commissioning observations have shown an estimated photometric precision near 400 ppm in a single 30 minute observation, and a 6-hr photometric precision of 80 ppm (both at V = 12). The K2 mission offers long-term, simultaneous optical observation of thousands of objects at a precision far better than is achievable from ground-based telescopes. Ecliptic fields will be observed for approximately 75 days enabling a unique exoplanet survey which fills the gaps in duration and sensitivity between the Kepler and TESS missions, and offers pre-launch exoplanet target identification for JWST transit spectroscopy. Astrophysics observations with K2 will include studies of young open clusters, bright stars, galaxies, supernovae, and asteroseismology.},
	language = {en},
	number = {938},
	urldate = {2016-08-21},
	journal = {Publications of the Astronomical Society of the Pacific},
	author = {Howell, Steve B. and Sobeck, Charlie and Haas, Michael and Still, Martin and Barclay, Thomas and Mullally, Fergal and {John Troeltzsch} and Aigrain, Suzanne and Bryson, Stephen T. and Caldwell, Doug and Chaplin, William J. and Cochran, William D. and Huber, Daniel and Marcy, Geoffrey W. and Miglio, Andrea and Najita, Joan R. and Smith, Marcie and Twicken, J. D. and Fortney, Jonathan J.},
	year = {2014},
	pages = {398},
	file = {IOP Full Text PDF:/Users/luke/Zotero/storage/GBX9D83U/Howell et al. - 2014 - The K2 Mission Characterization and Early Results.pdf:application/pdf}
}

@article{borucki_kepler_2010,
	title = {Kepler {Planet}-{Detection} {Mission}: {Introduction} and {First} {Results}},
	volume = {327},
	shorttitle = {Kepler {Planet}-{Detection} {Mission}},
	url = {https://ui.adsabs.harvard.edu/abs/2010Sci...327..977B/abstract},
	doi = {10.1126/science.1185402},
	abstract = {The Kepler mission was designed to determine the frequency of Earth-sized planets in and near the habitable zone of Sun-like stars. The habitable zone is the region where planetary temperatures are suitable for water to exist on a planet’s surface. During the first 6 weeks of observations, Kepler monitored 156,000 stars, and five new exoplanets with sizes between 0.37 and 1.6 Jupiter radii and orbital periods from 3.2 to 4.9 days were discovered. The density of the Neptune-sized Kepler-4b is similar to that of Neptune and GJ 436b, even though the irradiation level is 800,000 times higher. Kepler-7b is one of the lowest-density planets ({\textasciitilde}0.17 gram per cubic centimeter) yet detected. Kepler-5b, -6b, and -8b confirm the existence of planets with densities lower than those predicted for gas giant planets.},
	language = {en},
	number = {5968},
	urldate = {2019-06-12},
	journal = {Science},
	author = {Borucki, William J. and Koch, David and Basri, Gibor and Batalha, Natalie and Brown, Timothy and Caldwell, Douglas and Caldwell, John and Christensen-Dalsgaard, Jørgen and Cochran, William D. and DeVore, Edna and Dunham, Edward W. and Dupree, Andrea K. and Gautier, Thomas N. and Geary, John C. and Gilliland, Ronald and Gould, Alan and Howell, Steve B. and Jenkins, Jon M. and Kondo, Yoji and Latham, David W. and Marcy, Geoffrey W. and Meibom, Søren and Kjeldsen, Hans and Lissauer, Jack J. and Monet, David G. and Morrison, David and Sasselov, Dimitar and Tarter, Jill and Boss, Alan and Brownlee, Don and Owen, Toby and Buzasi, Derek and Charbonneau, David and Doyle, Laurance and Fortney, Jonathan and Ford, Eric B. and Holman, Matthew J. and Seager, Sara and Steffen, Jason H. and Welsh, William F. and Rowe, Jason and Anderson, Howard and Buchhave, Lars and Ciardi, David and Walkowicz, Lucianne and Sherry, William and Horch, Elliott and Isaacson, Howard and Everett, Mark E. and Fischer, Debra and Torres, Guillermo and Johnson, John Asher and Endl, Michael and MacQueen, Phillip and Bryson, Stephen T. and Dotson, Jessie and Haas, Michael and Kolodziejczak, Jeffrey and Van Cleve, Jeffrey and Chandrasekaran, Hema and Twicken, Joseph D. and Quintana, Elisa V. and Clarke, Bruce D. and Allen, Christopher and Li, Jie and Wu, Haley and Tenenbaum, Peter and Verner, Ekaterina and Bruhweiler, Frederick and Barnes, Jason and Prsa, Andrej},
	month = feb,
	year = {2010},
	pages = {977},
	file = {Snapshot:/Users/luke/Zotero/storage/DQ92XM2I/abstract.html:text/html;Submitted Version:/Users/luke/Zotero/storage/LLD7F93C/Borucki et al. - 2010 - Kepler Planet-Detection Mission Introduction and .pdf:application/pdf}
}

@article{hartman_rotation_2009,
	title = {Deep {MMT} {Transit} {Survey} of the {Open} {Cluster} {M}37. {III}. {Stellar} {Rotation} at 550 {Myr}},
	volume = {691},
	issn = {0004-637X},
	url = {http://adsabs.harvard.edu/abs/2009ApJ...691..342H},
	doi = {10.1088/0004-637X/691/1/342},
	abstract = {In the course of conducting a deep (14.5 lsim r lsim 23), 20 night 
survey for transiting planets in the rich {\textasciitilde}550 Myr old open cluster M37,
we have measured the rotation periods of 575 stars, which lie near the
cluster main sequence, with masses 0.2 M sun lsim M lsim 1.3
M sun. This is the largest sample of rotation periods for a
cluster older than 500 Myr. Using this rich sample we investigate a
number of relations between rotation period, color, and the amplitude of
photometric variability. Stars with M gsim 0.8 M sun show a
tight correlation between period and mass with heavier stars rotating
more rapidly. There is a group of four stars with P {\textgreater} 15 days that
fall well above this relation, which, if real, would present a
significant challenge to theories of stellar angular momentum evolution.
Below 0.8 M sun, the stars continue to follow the period-mass
correlation but with a broad tail of rapid rotators that expands to
shorter periods with decreasing mass. We combine these results with
observations of other open clusters to test the standard theory of lower
main-sequence stellar angular momentum evolution. We find that the model
reproduces the observations for solar-mass stars, but discrepancies are
apparent for stars with 0.6 lsim M lsim 1.0 M sun. We also
find that for late K through early M dwarf stars in this cluster, rapid
rotators tend to be bluer than slow rotators in B - V but redder than
slow rotators in V - IC . This result supports the hypothesis
that the significant discrepancy between the observed and predicted
temperatures and radii of low-mass main-sequence stars is due to stellar
activity.

Observations reported here were obtained at the MMT Observatory, a joint
facility of the Smithsonian Institution and the University of Arizona.},
	urldate = {2017-09-18},
	journal = {The Astrophysical Journal},
	author = {Hartman, J. D. and Gaudi, B. S. and Pinsonneault, M. H. and Stanek, K. Z. and Holman, M. J. and McLeod, B. A. and Meibom, S. and Barranco, J. A. and Kalirai, J. S.},
	month = jan,
	year = {2009},
	keywords = {stars: low-mass, brown dwarfs, stars: rotation, stars: variables: other, open clusters and associations: individual: M37, stars: spots},
	pages = {342--364},
	file = {NASA/ADS Full Text PDF:/Users/luke/Zotero/storage/HZDGUWZE/Hartman et al. - 2009 - Deep MMT Transit Survey of the Open Cluster M37. I.pdf:application/pdf}
}

@article{soderblom_ages_2010,
	title = {The {Ages} of {Stars}},
	volume = {48},
	issn = {0066-4146},
	url = {http://adsabs.harvard.edu/abs/2010ARA%26A..48..581S},
	doi = {10.1146/annurev-astro-081309-130806},
	abstract = {The age of an individual star cannot be measured, only estimated through mostly model-dependent or empirical methods, and no single method works well for a broad range of stellar types or for a full range in age. This review presents a summary of the available techniques for age-dating stars and ensembles of stars, their realms of applicability, and their strengths and weaknesses. My emphasis is on low-mass stars because they are present from all epochs of star formation in the Galaxy and because they present both special opportunities and problems. The ages of open clusters are important for understanding the limitations of stellar models and for calibrating empirical age indicators. For individual stars, a hierarchy of quality for the available age-dating methods is described. Although our present ability to determine the ages of even the nearest stars is mediocre, the next few years hold great promise as asteroseismology probes beyond stellar surfaces and starts to provide precise interior properties of stars and as models continue to improve when stressed by better observations.},
	urldate = {2017-09-13},
	journal = {Annual Review of Astronomy and Astrophysics},
	author = {Soderblom, David R.},
	month = sep,
	year = {2010},
	pages = {581--629},
	file = {Full Text PDF:/Users/luke/Zotero/storage/DMCCBENW/Soderblom - 2010 - The Ages of Stars.pdf:application/pdf;NASA/ADS Full Text PDF:/Users/luke/Zotero/storage/DE9XZ6XN/Soderblom - 2010 - The Ages of Stars.pdf:application/pdf}
}

@article{Irwin_NGC2516_2007,
    title = {The Monitor project: rotation of low-mass stars in the open 
    cluster {NGC}2516},
    volume = {377},
    pages = {741--758},
    journal = {MNRAS},
    author = {Irwin, Jonathan and Hodgkin, Simon and Aigrain, Suzanne and 
    Hebb, Leslie and Bouvier, Jerome and Clarke, Cathie and Moraux, Estelle 
    and Bramich, D. M.},
    year = {2007}
}


@article{miller_monitor_2008,
	title = {The {Monitor} project: the search for transits in the open cluster {NGC} 2362},
	volume = {387},
	issn = {0035-8711},
	shorttitle = {The {Monitor} project},
	url = {http://adsabs.harvard.edu/abs/2008MNRAS.387..349M},
	doi = {10.1111/j.1365-2966.2008.13236.x},
	urldate = {2017-09-18},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Miller, Adam A. and Irwin, Jonathan and Aigrain, Suzanne and Hodgkin, Simon and Hebb, Leslie},
	month = jun,
	year = {2008},
	keywords = {planetary systems, techniques: photometric, surveys, occultations, open clusters and associations: individual: NGC 2362},
	pages = {349--363},
	file = {NASA/ADS Full Text PDF:/Users/luke/Zotero/storage/MXNLLWQ7/Miller et al. - 2008 - The Monitor project the search for transits in th.pdf:application/pdf}
}

@article{irwin_monitor_PMSEB_2007,
	title = {The {Monitor} project: {JW} 380 - a 0.26-, 0.15-{Msolar}, pre-main-sequence eclipsing binary in the {Orion} nebula cluster},
	volume = {380},
	issn = {0035-8711},
	shorttitle = {The {Monitor} project},
	url = {http://adsabs.harvard.edu/abs/2007MNRAS.380..541I},
	doi = {10.1111/j.1365-2966.2007.12117.x},
	abstract = {We report the discovery of a low-mass (0.26 +/- 0.02, 0.15 +/- 
			0.01Msolar) pre-main-sequence (PMS) eclipsing binary (EB)
			with a 5.3d orbital period. JW 380 was detected as part of a
			high-cadence time-resolved photometric survey (the Monitor project)
			using the 2.5-m Isaac Newton Telescope and Wide Field Camera for a
			survey of a single field in the Orion nebula cluster (ONC) region in V
			and i bands. The star is assigned a 99 per cent membership probability
			from proper motion measurements, and radial velocity observations
			indicate a systemic velocity within 1σ of that of the ONC.
			Modelling of the combined light and radial velocity curves of the system
			gave stellar radii of 1.19+0.04-0.18 and
			0.90+0.17-0.03Rsolar for the primary
			and the secondary, with a significant third light contribution which is
			also visible as a third peak in the cross-correlation functions used to
			derive radial velocities. The masses and radii appear to be consistent
			with stellar models for 2-3Myr age from several authors, within the
			present observational errors. These observations probe an important
			region of mass-radius parameter space, where there are currently only a
			handful of known PMS EB systems with precise measurements available in
			the literature.},
	urldate = {2017-09-18},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Irwin, Jonathan and Aigrain, Suzanne and Hodgkin, Simon and Stassun, Keivan G. and Hebb, Leslie and Irwin, Mike and Moraux, Estelle and Bouvier, Jerome and Alapini, Aude and Alexander, Richard and Bramich, D. M. and Holtzman, Jon and Martín, Eduardo L. and McCaughrean, Mark J. and Pont, Frédéric and Verrier, P. E. and Zapatero Osorio, María Rosa},
	month = sep,
	year = {2007},
	keywords = {surveys, binaries: eclipsing, stars: pre-main-sequence, open clusters and associations: individual: Orion nebula cluster, stars: individual: JW 380},
	pages = {541--550},
	file = {NASA/ADS Full Text PDF:/Users/luke/Zotero/storage/SG82P3N5/Irwin et al. - 2007 - The Monitor project JW 380 - a 0.26-, 0.15-Msolar.pdf:application/pdf}
}

@article{irwin_monitordata_2007,
	title = {The {Monitor} project: data processing and light curve production},
	volume = {375},
	issn = {0035-8711},
	shorttitle = {The {Monitor} project},
	url = {http://adsabs.harvard.edu/abs/2007MNRAS.375.1449I},
	doi = {10.1111/j.1365-2966.2006.11408.x},
	abstract = {We have begun a large-scale photometric survey of nearby open clusters and star-forming regions, the Monitor project, aiming to measure time-series photometry for {\textgreater}10000 cluster members over {\textgreater}10
	deg2 of sky, to find low-mass eclipsing binary and planet systems. We describe the software pipeline we have developed for this project, showing that we can achieve peak rms accuracy over the entire data set of better than {\textasciitilde}2 mmag using aperture photometry, with rms {\textless}1 per cent over {\textasciitilde}4 mag, in data from 2- and 4-m class telescopes with wide-field mosaic cameras. We investigate the noise properties of our data, finding correlated `red' noise at the {\textasciitilde}1-1.5 mmag level in bright stars, over transit-like time-scales of 2.5h. An important source of correlated noise in aperture photometry is image blending, which produces variations correlated with the seeing. We present a simple blend index based on fitting polynomials to these variations, and find that subtracting the fit from the data provides a method to reduce their amplitude, in lieu of using techniques, such as point spread function fitting photometry, which tackle their cause. Finally, we use the SYSREM algorithm to search for any further systematic effects.},
	urldate = {2017-09-18},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Irwin, Jonathan and Irwin, Mike and Aigrain, Suzanne and Hodgkin, Simon and Hebb, Leslie and Moraux, Estelle},
	month = mar,
	year = {2007},
	keywords = {techniques: photometric, surveys, methods: data analysis},
	pages = {1449--1462},
	file = {NASA/ADS Full Text PDF:/Users/luke/Zotero/storage/I3DH65CH/Irwin et al. - 2007 - The Monitor project data processing and light cur.pdf:application/pdf}
}

@article{aigrain_monitor_2007,
	title = {The {Monitor} project: searching for occultations in young open clusters},
	volume = {375},
	issn = {0035-8711},
	shorttitle = {The {Monitor} project},
	url = {http://adsabs.harvard.edu/abs/2007MNRAS.375...29A},
	doi = {10.1111/j.1365-2966.2006.11303.x},
	abstract = {The Monitor project is a photometric monitoring survey of nine young (1-200Myr) clusters in the solar neighbourhood to search for eclipses by very low mass stars and brown dwarfs and for planetary transits in the light curves of cluster members. It began in the autumn of 2004 and uses several 2- to 4-m telescopes worldwide. We aim to calibrate the relation between age, mass, radius and where possible luminosity, from the K dwarf to the planet regime, in an age range where constraints on evolutionary models are currently very scarce. Any detection of an exoplanet in one of our youngest targets ({\textless}{\textasciitilde}10Myr) would also provide important constraints on planet formation and migration time-scales and their relation to protoplanetary disc lifetimes. Finally, we will use the light curves of cluster members to study rotation and flaring in low-mass pre-main-sequence stars.
	The present paper details the motivation, science goals and observing strategy of the survey. We present a method to estimate the sensitivity and number of detections expected in each cluster, using a simple semi-analytic approach which takes into account the characteristics of the cluster and photometric observations, using (tunable) best-guess assumptions for the incidence and parameter distribution of putative companions, and we incorporate the limits imposed by radial velocity follow-up from medium and large telescopes. We use these calculations to show that the survey as a whole can be expected to detect over 100 young low and very low mass eclipsing binaries, and {\textasciitilde}3 transiting planets with radial velocity signatures detectable with currently available
facilities.},
	urldate = {2017-09-18},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Aigrain, S. and Hodgkin, S. and Irwin, J. and Hebb, L. and Irwin, M. and Favata, F. and Moraux, E. and Pont, F.},
	month = feb,
	year = {2007},
	keywords = {planetary systems, stars: low-mass, binaries: eclipsing, brown dwarfs, stars: pre-main-sequence, occultations},
	pages = {29--52},
	file = {NASA/ADS Full Text PDF:/Users/luke/Zotero/storage/5PULZXWG/Aigrain et al. - 2007 - The Monitor project searching for occultations in.pdf:application/pdf}
}


@article{hartman_MMT_IV_2009,
	title = {Deep {MMT} {Transit} {Survey} of the {Open} {Cluster} {M}37 {IV}: {Limit} on the {Fraction} of {Stars} with {Planets} as {Small} as 0.3R{\textless}{SUB}{\textgreater}{J}{\textless}/{SUB}{\textgreater}},
	volume = {695},
	shorttitle = {Deep {MMT} {Transit} {Survey} of the {Open} {Cluster} {M}37 {IV}},
	url = {https://ui.adsabs.harvard.edu/abs/2009ApJ...695..336H/abstract},
	doi = {10.1088/0004-637X/695/1/336},
	abstract = {We present the results of a deep (15 lsim r lsim 23), 20 night survey for transiting planets in the intermediate-age open cluster M37 (NGC 2099) using the Megacam wide-field mosaic CCD camera on the 6.5 m MMT. We do not detect any transiting planets among the {\textasciitilde}1450 observed cluster members. We do, however, identify a {\textasciitilde}1R{\textless}SUB{\textgreater}J{\textless}/SUB{\textgreater} candidate planet transiting a {\textasciitilde}0.8 M {\textless}SUB{\textgreater}sun{\textless}/SUB{\textgreater} Galactic field star with a period of 0.77 days. The source is faint (V = 19.85 mag) and has an expected velocity semiamplitude of K {\textasciitilde} 220 m s{\textless}SUP{\textgreater}-1{\textless}/SUP{\textgreater}(M/M{\textless}SUB{\textgreater}J{\textless}/SUB{\textgreater} ). We conduct Monte Carlo transit injection and recovery simulations to calculate the 95\% confidence upper limit on the fraction of cluster members and field stars with planets as a function of planetary radius and orbital period. Assuming a uniform logarithmic distribution in the orbital period, we find that \&lt;1.1\%, \&lt;2.7\%, and \&lt;8.3\% of cluster members have 1.0R{\textless}SUB{\textgreater}J{\textless}/SUB{\textgreater} planets within extremely hot Jupiter (EHJ; 0.4 \&lt; P \&lt; 1.0 day), very hot Jupiter (VHJ; 1.0 \&lt; P \&lt; 3.0 day), and hot Jupiter (HJ; 3.0 \&lt; P \&lt; 5.0 day) period ranges, respectively. For 0.5R{\textless}SUB{\textgreater}J{\textless}/SUB{\textgreater} planets, the limits are less than 3.2\% and less than 21\% for EHJ and VHJ period ranges, respectively, while for 0.35R{\textless}SUB{\textgreater}J{\textless}/SUB{\textgreater} planets we can only place an upper limit of less than 25\% on the EHJ period range. For a sample of 7814 Galactic field stars, consisting primarily of FGKM dwarfs, we place 95\% upper limits of \&lt;0.3\%, \&lt;0.8\%, and \&lt;2.7\% on the fraction of stars with a 1.0R{\textless}SUB{\textgreater}J{\textless}/SUB{\textgreater} EHJ, VHJ, and HJ, respectively, assuming that the candidate planet is not genuine. If the candidate is genuine, the frequency of {\textasciitilde}1.0R{\textless}SUB{\textgreater}J{\textless}/SUB{\textgreater} planets in the EHJ period range is 0.002\% \&lt; f {\textless}SUB{\textgreater}EHJ{\textless}/SUB{\textgreater} \&lt; 0.5\% with 95\% confidence. We place limits of \&lt;1.4\%, \&lt;8.8\%, and \&lt;47\% for 0.5R{\textless}SUB{\textgreater}J{\textless}/SUB{\textgreater} planets, and a limit of \&lt;16\% on 0.3R{\textless}SUB{\textgreater}J{\textless}/SUB{\textgreater} planets in the EHJ period range. This is the first transit survey to place limits on the fraction of stars with planets as small as Neptune. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona.},
	language = {en},
	number = {1},
	urldate = {2019-06-12},
	journal = {The Astrophysical Journal},
	author = {Hartman, J. D. and Gaudi, B. S. and Holman, M. J. and McLeod, B. A. and Stanek, K. Z. and Barranco, J. A. and Pinsonneault, M. H. and Meibom, S. and Kalirai, J. S.},
	month = apr,
	year = {2009},
	pages = {336},
	file = {Full Text PDF:/Users/luke/Zotero/storage/JXABBCV8/Hartman et al. - 2009 - Deep MMT Transit Survey of the Open Cluster M37 IV.pdf:application/pdf;Snapshot:/Users/luke/Zotero/storage/HP9CP3X9/abstract.html:text/html}
}

@article{stassun_TIC_2018,
    title = {The {TESS} {Input} {Catalog} and {Candidate} {Target} {List}},
    volume = {156},
    issn = {1538-3881},
    url = {http://stacks.iop.org/1538-3881/156/i=3/a=102},
    doi = {10.3847/1538-3881/aad050},
    abstract = {The Transiting Exoplanet Survey Satellite ( TESS ) will be 
    conducting a nearly all-sky photometric survey over two years, with a core 
    mission goal to discover small transiting exoplanets orbiting nearby 
    bright stars. It will obtain 30 minute cadence observations of all objects 
    in the TESS fields of view, along with two-minute cadence observations of 
    200,000–400,000 selected stars. The choice of which stars to observe at 
    the two-minute cadence is driven by the need to detect small transiting 
    planets, which leads to the selection of primarily bright, cool dwarfs. We 
    describe the catalogs assembled and the algorithms used to populate the 
    TESS Input Catalog (TIC), including plans to update the TIC with the 
    incorporation of the Gaia second data release in the near future. We also 
    describe a ranking system for prioritizing stars according to the smallest 
    transiting planet detectable, and assemble a Candidate Target List (CTL) 
    using that ranking. We discuss additional factors that affect the ability 
    to photometrically detect and dynamically confirm small planets, and we 
    note additional stellar populations of interest that may be added to the 
    final target list. The TIC is available on the STScI MAST server, and an 
    enhanced CTL is available through the Filtergraph data visualization 
    portal system at the URL http://filtergraph.com/tess\_ctl 
    [http://filtergraph.com/tess\_ctl] .},
    language = {en},
    number = {3},
    urldate = {2018-11-09},
    journal = {The Astronomical Journal},
    author = {Stassun, Keivan G. and Oelkers, Ryan J. and Pepper, Joshua and 
    Paegert, Martin and Lee, Nathan De and Torres, Guillermo and Latham, David 
    W. and Charpinet, Stéphane and Dressing, Courtney D. and Huber, Daniel and 
    Kane, Stephen R. and {Sébastien Lépine} and Mann, Andrew and Muirhead, 
    Philip S. and Rojas-Ayala, Bárbara and Silvotti, Roberto and Fleming, 
    Scott W. and {Al Levine} and Plavchan, Peter},
    year = {2018},
    pages = {102},
    file = {Submitted Version:/home/luke/local/Zotero/storage/4BUX3WC9/Stassun 
    et al. - 2018 - The TESS Input Catalog and Candidate Target 
    List.pdf:application/pdf}
}

@article{stassun_TIC8_2019,
    title = {The {Revised} {TESS} {Input} {Catalog} and {Candidate} {Target} 
    {List}},
    url = {http://arxiv.org/abs/1905.10694},
    abstract = {We describe the catalogs assembled and the algorithms used to 
    populate the revised TESS Input Catalog (TIC), based on the incorporation 
    of the Gaia second data release. We also describe a revised ranking system 
    for prioritizing stars for 2-minute cadence observations, and assemble a 
    revised Candidate Target List (CTL) using that ranking. The TIC is 
    available on the Mikulski Archive for Space Telescopes (MAST) server, and 
    an enhanced CTL is available through the Filtergraph data visualization 
    portal system at the URL http://filtergraph.vanderbilt.edu/tess\_ctl.},
    urldate = {2019-05-28},
    journal = {arXiv:1905.10694 [astro-ph]},
    author = {Stassun, Keivan G. and Oelkers, Ryan J. and Paegert, Martin and 
    Torres, Guillermo and Pepper, Joshua and De Lee, Nathan and Collins, Kevin 
    and Latham, David W. and Muirhead, Philip S. and Chittidi, Jay and 
    Rojas-Ayala, Barbara and Fleming, Scott W. and Rose, Mark E. and 
    Tenenbaum, Peter and Ting, Eric B. and Kane, Stephen R. and Barclay, 
    Thomas and Bean, Jacob L. and Brassuer, C. E. and Charbonneau, David and 
    Lissauer, Jack J. and Mann, Andrew W. and McLean, Brian and Mulally, Susan 
    and Narita, Norio and Plavchan, Peter and Ricker, George R. and Sasselov, 
    Dimitar and Seager, S. and Sharma, Sanjib and Shiao, Bernie and Sozzetti, 
    Alessandro and Stello, Dennis and Vanderspek, Roland and Wallace, Geoff 
    and Winn, Joshua N.},
    month = may,
    year = {2019},
    note = {arXiv: 1905.10694},
    keywords = {Astrophysics - Solar and Stellar Astrophysics, Astrophysics - 
    Earth and Planetary Astrophysics}
}

@article{brasseur_astrocut_2019,
	title = {Astrocut: {Tools} for creating cutouts of {TESS} images},
	shorttitle = {Astrocut},
	url = {https://ui.adsabs.harvard.edu/abs/2019ascl.soft05007B/abstract},
	abstract = {The Transiting Exoplanet Survey Satellite (TESS) produces Full Frame Images (FFIs) at a half hour cadence and keeps the same pointing for 27 days at a time. Astrocut performs the same cutout across all FFIs that share a common pointing to create a time series of images on a small portion of the sky. The Astrocut package has two parts: the CubeFactory and the CutoutFactory. The CubeFactory class creates a large image cube from a list of FFI files, which allows the cutout operation to be performed efficiently. The CutoutFactory class performs the actual cutout and builds a target pixel file (TPF) that is compatible with TESS pipeline TPFs. Because this software operates on TESS mission-produced FFIs, the resulting TPFs are not background-subtracted. In addition to the Astrocut software itself, the Mikulski Archive for Space Telescopes (MAST) provides a cutout service, TESScut, which runs Astrocut on MAST servers, and allows users to simply request cutouts through a web form or direct HTTP API query.},
	language = {en},
	urldate = {2019-06-03},
	journal = {Astrophysics Source Code Library},
	author = {Brasseur, C. E. and Phillip, Carlita and Fleming, Scott W. and Mullally, S. E. and White, Richard L.},
	month = may,
	year = {2019},
	pages = {ascl:1905.007}
}

@article{stellingwerf_period_1978,
    title = {Period determination using phase dispersion minimization},
    volume = {224},
    issn = {0004-637X},
    url = {http://adsabs.harvard.edu/abs/1978ApJ...224..953S},
    doi = {10.1086/156444},
    abstract = {We derive a period determination technique that is well suited 
    to the case of nonsinusoidal time variation covered by only a few 
    irregularly spaced observations. A detailed statistical analysis allows 
    comparison with other techniques and indicates the optimum choice of 
    parameters for a given problem. Application to the double-mode Cepheid BK 
    Cen
    demonstrates the applicability of these methods to difficult cases. Using 
    49 photoelectric points, we obtain the two primary oscillatory components 
    as well as the principal mode-interaction term; the derived periods are in 
    agreement with previous estimates.},
    urldate = {2017-03-17},
    journal = {The Astrophysical Journal},
    author = {Stellingwerf, R. F.},
    month = sep,
    year = {1978},
    keywords = {Statistical Analysis, Periodic Variations, Variable Stars, 
    Cepheid Variables, Computer Techniques, Curve Fitting, Data Smoothing, 
    Least Squares Method, Light Curve, Run Time (Computers), Significance},
    pages = {953--960},
    file = {NASA/ADS Full Text 
    PDF:/home/luke/local/Zotero/storage/4KX9XM6D/Stellingwerf - 1978 - Period 
    determination using phase dispersion minimi.pdf:application/pdf}
}

@article{bouma_wasp-4b_2019,
    title = {{WASP}-4b {Arrived} {Early} for the {TESS} {Mission}},
    volume = {157},
    issn = {1538-3881},
    url = {https://iopscience.iop.org/article/10.3847/1538-3881/ab189f/meta},
    doi = {10.3847/1538-3881/ab189f},
    language = {en},
    number = {6},
    urldate = {2019-05-07},
    journal = {The Astronomical Journal},
    author = {Bouma, L. G. and Winn, J. N. and Baxter, C. and Bhatti, W. and 
    Dai, F. and Daylan, T. and Désert, J.-M. and Hill, M. L. and Kane, S. R. 
    and Stassun, K. G. and Villasenor, J. and Ricker, G. R. and Vanderspek, R. 
    and Latham, D. W. and Seager, S. and Jenkins, J. M. and Berta-Thompson, Z. 
    and Colón, K. and Fausnaugh, M. and Glidden, Ana and Guerrero, N. and 
    Rodriguez, J. E. and Twicken, J. D. and Wohler, B.},
    month = may,
    year = {2019},
    pages = {217}
}

@article{ofir_optimizing_2014,
    title = {Optimizing the search for transiting planets in long time series},
    volume = {561},
    url = {https://ui.adsabs.harvard.edu/abs/2014A%26A...561A.138O/abstract},
    doi = {10.1051/0004-6361/201220860},
    abstract = {Context. Transit surveys, both ground- and space-based, have 
    already accumulated a large number of light curves that span several 
    years. {\textless}BR /{\textgreater} Aims: The search for transiting 
    planets in these long time series is computationally intensive. We wish to 
    optimize the search for both detection and computational efficiencies. 
    {\textless}BR /{\textgreater} Methods: We assume that the searched systems 
    can be described well by Keplerian orbits. We then propagate the effects 
    of different system parameters to the detection parameters. {\textless}BR 
    /{\textgreater} Results: We show that the frequency information content of 
    the light curve is primarily determined by the duty cycle of the transit 
    signal, and thus the optimal frequency sampling is found to be cubic and 
    not linear. Further optimization is achieved by considering duty-cycle 
    dependent binning of the phased light curve. By using the (standard) BLS, 
    one is either fairly insensitive to long-period planets or less sensitive 
    to short-period planets and computationally slower by a significant factor 
    of {\textasciitilde}330 (for a 3 yr long dataset). We also show how the 
    physical system parameters, such as the host star's size and mass, 
    directly affect transit detection. This understanding can then be used to 
    optimize the search for every star individually. {\textless}BR 
    /{\textgreater} Conclusions: By considering Keplerian dynamics explicitly 
    rather than implicitly one can optimally search the BLS parameter space. 
    The presented Optimal BLS enhances the detectability of both very short 
    and very long period planets, while allowing such searches to be done with 
    much reduced resources and time. The Matlab/Octave source code for Optimal 
    BLS is made available. The MATLAB code is only available at the CDS via 
    anonymous ftp to {\textless}A 
    href="http://cdsarc.u-strasbg.fr"{\textgreater}http://cdsarc.u-strasbg.fr{\textless}/A{\textgreater}
     (ftp://130.79.128.5) or via {\textless}A 
    href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/561/A138"{\textgreater}http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/561/A138{\textless}/A{\textgreater}},
    language = {en},
    urldate = {2019-04-19},
    journal = {Astronomy and Astrophysics},
    author = {Ofir, Aviv},
    month = jan,
    year = {2014},
    pages = {A138},
    file = {Full Text PDF:/home/luke/local/Zotero/storage/Q4SREWZH/Ofir - 2014 
    - Optimizing the search for transiting planets in 
    lo.pdf:application/pdf;Snapshot:/home/luke/local/Zotero/storage/6HPDXSKX/abstract.html:text/html}
}

@article{hippke_TLS_2019,
    title = {Transit {Least} {Squares}: {An} optimized transit detection 
    algorithm to search for periodic transits of small planets},
    shorttitle = {Transit {Least} {Squares}},
    url = {http://arxiv.org/abs/1901.02015},
    abstract = {We present a new method to detect planetary transits from 
    time-series photometry, the Transit Least Squares (TLS) algorithm. TLS 
    searches for transit-like features while taking the stellar limb darkening 
    and planetary ingress and egress into account. We have optimized TLS for 
    both signal detection efficiency (SDE) of small planets and computational 
    speed. TLS analyses the entire, unbinned phase-folded light curve. We 
    compensate for the higher computational load by (i.) using algorithms like 
    "Mergesort" (for the trial orbital phases) and by (ii.) restricting the 
    trial transit durations to a smaller range that encompasses all known 
    planets, and using stellar density priors where available. A typical K2 
    light curve, including 80d of observations at a cadence of 30min, can be 
    searched with TLS in {\textasciitilde}10s real time on a standard laptop 
    computer, as fast as the widely used Box Least Squares (BLS) algorithm. We 
    perform a transit injection-retrieval experiment of Earth-sized planets 
    around sun-like stars using synthetic light curves with 110ppm white noise 
    per 30min cadence, corresponding to a photometrically quiet KP=12 star 
    observed with Kepler. We determine the SDE thresholds for both BLS and TLS 
    to reach a false positive rate of 1\% to be SDE{\textasciitilde}7 in both 
    cases. The resulting true positive (or recovery) rates are 
    {\textasciitilde}93\% for TLS and {\textasciitilde}76\% for BLS, implying 
    more reliable detections with TLS. We also test TLS with the K2 light 
    curve of the TRAPPIST-1 system and find six of seven Earth-sized planets 
    using an iterative search for increasingly lower signal detection 
    efficiency, the phase-folded transit of the seventh planet being affected 
    by a stellar flare. TLS is more reliable than BLS in finding any kind of 
    transiting planet but it is particularly suited for the detection of small 
    planets in long time series from Kepler, TESS, and PLATO. We make our 
    Python implementation of TLS publicly available.},
    urldate = {2019-01-09},
    journal = {arXiv:1901.02015 [astro-ph]},
    author = {Hippke, Michael and Heller, René},
    month = jan,
    year = {2019},
    note = {arXiv: 1901.02015},
    keywords = {Astrophysics - Earth and Planetary Astrophysics, Astrophysics 
    - Instrumentation and Methods for Astrophysics}
}

@article{eastman_achieving_2010,
	title = {Achieving better than 1 minute accuracy in the {Heliocentric} and {Barycentric} {Julian} {Dates}},
	volume = {122},
	issn = {0004-6280, 1538-3873},
	url = {http://arxiv.org/abs/1005.4415},
	doi = {10.1086/655938},
	abstract = {As the quality and quantity of astrophysical data continue to improve, the precision with which certain astrophysical events can be timed becomes limited not by the data themselves, but by the manner, standard, and uniformity with which time itself is referenced. While some areas of astronomy (most notably pulsar studies) have required absolute time stamps with precisions of considerably better than 1 minute for many decades, recently new areas have crossed into this regime. In particular, in the exoplanet community, we have found that the (typically unspecified) time standards adopted by various groups can differ by as much as a minute. Left uncorrected, this ambiguity may be mistaken for transit timing variations and bias eccentricity measurements. We argue that, since the commonly-used Julian Date, as well as its heliocentric and barycentric counterparts, can be specified in several time standards, it is imperative that their time standards always be reported when accuracies of 1 minute are required. We summarize the rationale behind our recommendation to quote the site arrival time, in addition to using BJD\_TDB, the Barycentric Julian Date in the Barycentric Dynamical Time standard for any astrophysical event. The BJD\_TDB is the most practical absolute time stamp for extra-terrestrial phenomena, and is ultimately limited by the properties of the target system. We compile a general summary of factors that must be considered in order to achieve timing precisions ranging from 15 minutes to 1 microsecond. Finally, we provide software tools that, in principal, allow one to calculate BJD\_TDB to a precision of 1 microsecond for any target from anywhere on Earth or from any spacecraft.},
	number = {894},
	urldate = {2018-08-26},
	journal = {Publications of the Astronomical Society of the Pacific},
	author = {Eastman, Jason and Siverd, Robert and Gaudi, B. Scott},
	month = aug,
	year = {2010},
	note = {arXiv: 1005.4415},
	keywords = {Astrophysics - Instrumentation and Methods for Astrophysics},
	pages = {935--946}
}

@article{wang_pixel-level_2017,
    title = {A pixel-level model for event discovery in time-domain imaging},
    url = {http://arxiv.org/abs/1710.02428},
    abstract = {Difference imaging or image subtraction is a method that 
    measures differential photometry by matching the pointing and point-spread 
    function (PSF) between image frames. It is used for the detection of 
    time-variable phenomena. Here we present a new category of method---CPM 
    Difference Imaging, in which differences are not measured between matched 
    images but instead between image frames and a data-driven predictive model 
    that has been designed only to predict the pointing, PSF, and detector 
    effects but not astronomical variability. In CPM Difference Imaging each 
    pixel is modelled by the Causal Pixel Model (CPM) originally built for 
    modeling Kepler data, in which pixel values are predicted by a linear 
    combination of other pixels at the same epoch but far enough away such 
    that these pixels are causally disconnected, astrophysically. It does not 
    require that the user have any explicit model or description of the 
    pointing or point-spread function of any of the images. Its principal 
    drawback is that---in its current form---it requires an imaging campaign 
    with many epochs and fairly stable telescope pointing. The method is 
    applied to simulated data and also the K2 Campaign 9 microlensing data. We 
    show that CPM Difference Imaging can detect variable objects and produce 
    precise differentiate photometry in a crowded field. CPM Difference 
    Imaging is capable of producing image differences at nearly photon-noise 
    precision.},
    urldate = {2017-10-09},
    journal = {arXiv:1710.02428 [astro-ph]},
    author = {Wang, Dun and Hogg, David W. and Foreman-Mackey, Daniel and 
    Schölkopf, Bernhard},
    month = oct,
    year = {2017},
    note = {arXiv: 1710.02428},
    keywords = {Astrophysics - Instrumentation and Methods for Astrophysics}
}

@article{bramich_new_2008,
	title = {A new algorithm for difference image analysis},
	volume = {386},
	issn = {0035-8711},
	url = {http://adsabs.harvard.edu/abs/2008MNRAS.386L..77B},
	doi = {10.1111/j.1745-3933.2008.00464.x},
	abstract = {In the context of difference image analysis (DIA), we present a new method for determining the convolution kernel matching a pair of images of the same field. Unlike the standard DIA technique which involves modelling the kernel as a linear combination of basis functions, we consider the kernel as a discrete pixel array and solve for the kernel pixel values directly using linear least squares. The removal of basis functions from the kernel model is advantageous for a number of
	compelling reasons. First, it removes the need for the user to specify such functions, which makes for a much simpler user application and avoids the risk of an inappropriate choice. Secondly, basis functions are constructed around the origin of the kernel coordinate system, which requires that the two images are perfectly aligned for an optimal result. The pixel kernel model is sufficiently flexible to correct for image misalignments, and in the case of a simple translation between images, image resampling becomes unnecessary. Our new algorithm can be extended to spatially varying kernels by solving for individual pixel kernels in a grid of image subregions and interpolating the solutions to obtain the kernel at any one pixel.},
	urldate = {2018-03-07},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Bramich, D. M.},
	month = may,
	year = {2008},
	keywords = {techniques: photometric, methods: statistical, techniques: image processing},
	pages = {L77--L81}
}

@article{zari_3d_2018,
	title = {3D mapping of young stars in the solar neighbourhood with {Gaia} {DR}2},
	volume = {620},
	url = {https://ui.adsabs.harvard.edu/abs/2018A%26A...620A.172Z/abstract},
	doi = {10.1051/0004-6361/201834150},
	abstract = {We study the three dimensional arrangement of young stars in the solar neighbourhood using the second release of the Gaia mission (Gaia DR2) and we provide a new, original view of the spatial configuration of the star-forming regions within 500 pc of the Sun. By smoothing the star distribution through a Gaussian filter, we construct three dimensional (3D) density maps for early-type stars (upper-main sequence, UMS) and pre-main sequence (PMS) sources. The PMS and the UMS samples are selected through a combination of photometric and astrometric criteria. A side product of the analysis is a 3D, G-band extinction map, which we use to correct our colour-magnitude diagram for extinction and reddening. Both density maps show three prominent structures, Scorpius-Centaurus, Orion, and Vela. The PMS map shows a plethora of lower-mass star-forming regions, such as Taurus, Perseus, Cepheus, Cassiopeia, and Lacerta, which are less visible in the UMS map due to the lack of large numbers of bright, early-type stars. We report the finding of a candidate new open cluster towards l, b ̃ 218.5° , - 2°, which could be related to the Orion star-forming complex. We estimate ages for the PMS sample and we study the distribution of PMS stars as a function of their age. We find that younger stars cluster in dense, compact clumps, and are surrounded by older sources, whose distribution is instead more diffuse. The youngest groups that we find are mainly located in Scorpius-Centaurus, Orion, Vela, and Taurus. Cepheus, Cassiopeia, and Lacerta are instead more evolved and less numerous. Finally, we find that the 3D density maps show no evidence for the existence of the ring-like structure which is usually referred to as the Gould Belt. The PMS and UMS catalogues are only available at the CDS via anonymous ftp to {\textless}A href="http://cdsarc.u-strasbg.fr/"{\textgreater}http://cdsarc.u-strasbg.fr{\textless}/A{\textgreater} (ftp://130.79.128.5) or via {\textless}A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/620/A172"{\textgreater}http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/620/A172{\textless}/A{\textgreater}},
	language = {en},
	urldate = {2019-05-07},
	journal = {Astronomy and Astrophysics},
	author = {Zari, E. and Hashemi, H. and Brown, A. G. A. and Jardine, K. and de Zeeuw, P. T.},
	month = dec,
	year = {2018},
	pages = {A172}
}

@article{marrese_gaia_2019,
	title = {Gaia {Data} {Release} 2 - {Cross}-match with external catalogues: algorithms and results},
	volume = {621},
	copyright = {© ESO 2019},
	issn = {0004-6361, 1432-0746},
	shorttitle = {Gaia {Data} {Release} 2 - {Cross}-match with external catalogues},
	url = {https:/articles/aa/abs/2019/01/aa34142-18/aa34142-18.html},
	doi = {10.1051/0004-6361/201834142},
	abstract = {{\textless}i{\textgreater}Context.{\textless}i/{\textgreater} Although the {\textless}i{\textgreater}Gaia{\textless}i/{\textgreater} catalogue on its own is a very powerful tool, it is the combination of this high-accuracy archive with other archives that will truly open up amazing possibilities for astronomical research. The advanced interoperation of archives is based on cross-matching, leaving the user with the feeling of working with one single data archive. The data retrieval should work not only across data archives but also across wavelength domains. The first step for a seamless access to the data is the computation of the cross-match between {\textless}i{\textgreater}Gaia{\textless}i/{\textgreater} and external surveys.{\textless}i{\textgreater}Aims.{\textless}i/{\textgreater} We describe the adopted algorithms and results of the pre-computed cross-match of the {\textless}i{\textgreater}Gaia{\textless}i/{\textgreater} Data Release 2 (DR2) catalogue with dense surveys (Pan-STARRS1 DR1, 2MASS, SDSS DR9, GSC 2.3, URAT-1, allWISE, PPMXL, and APASS DR9) and sparse catalogues (HIPPARCOS2, {\textless}i{\textgreater}Tycho{\textless}i/{\textgreater}-2, and RAVE 5).{\textless}i{\textgreater}Methods.{\textless}i/{\textgreater} A new algorithm is developed specifically for sparse catalogues. Improvements and changes with respect to the algorithm adopted for DR1 are described in detail.{\textless}i{\textgreater}Results.{\textless}i/{\textgreater} The outputs of the cross-match are part of the official {\textless}i{\textgreater}Gaia{\textless}i/{\textgreater} DR2 catalogue. The global analysis of the cross-match results is also presented.},
	language = {en},
	urldate = {2019-04-03},
	journal = {Astronomy \& Astrophysics},
	author = {Marrese, P. M. and Marinoni, S. and Fabrizio, M. and Altavilla, G.},
	month = jan,
	year = {2019},
	pages = {A144},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/FJ7PBZAC/Marrese et al. - 2019 - Gaia Data Release 2 - Cross-match with external ca.pdf:application/pdf;Snapshot:/home/luke/local/Zotero/storage/SK7KFHZ3/aa34142-18.html:text/html}
}

@article{roeser_ppmxl_2010,
	title = {The {PPMXL} {Catalog} of {Positions} and {Proper} {Motions} on the {ICRS}. {Combining} {USNO}-{B}1.0 and the {Two} {Micron} {All} {Sky} {Survey} (2MASS)},
	volume = {139},
	issn = {0004-6256},
	url = {http://ads.ari.uni-heidelberg.de/abs/2010AJ....139.2440R},
	doi = {10.1088/0004-6256/139/6/2440},
	language = {en},
	urldate = {2019-04-03},
	journal = {The Astronomical Journal},
	author = {R\"oser, S. and Demleitner, M. and Schilbach, E.},
	month = jun,
	year = {2010},
	pages = {2440--2447}
}

@article{skrutskie_tmass_2006,
	title = {The {Two} {Micron} {All} {Sky} {Survey} (2MASS)},
	volume = {131},
	issn = {0004-6256},
	url = {http://adsabs.harvard.edu/abs/2006AJ....131.1163S},
	doi = {10.1086/498708},
	abstract = {Between 1997 June and 2001 February the Two Micron All Sky Survey (2MASS) collected 25.4 Tbytes of raw imaging data covering 99.998\% of the celestial sphere in the near-infrared J (1.25 μm), H (1.65
μm), and Ks (2.16 μm) bandpasses. Observations were
conducted from two dedicated 1.3 m diameter telescopes located at Mount Hopkins, Arizona, and Cerro Tololo, Chile. The 7.8 s of integration time accumulated for each point on the sky and strict quality control yielded a 10 σ point-source detection level of better than 15.8, 15.1, and 14.3 mag at the J, H, and Ks bands, respectively, for virtually the entire sky. Bright source extractions have 1 σ
photometric uncertainty of {\textless}0.03 mag and astrometric accuracy of order 100 mas. Calibration offsets between any two points in the sky are {\textless}0.02 mag. The 2MASS All-Sky Data Release includes 4.1 million
compressed FITS images covering the entire sky, 471 million source extractions in a Point Source Catalog, and 1.6 million objects
identified as extended in an Extended Source Catalog.},
	urldate = {2019-04-03},
	journal = {The Astronomical Journal},
	author = {Skrutskie, M. F. and Cutri, R. M. and Stiening, R. and Weinberg, M. D. and Schneider, S. and Carpenter, J. M. and Beichman, C. and Capps, R. and Chester, T. and Elias, J. and Huchra, J. and Liebert, J. and Lonsdale, C. and Monet, D. G. and Price, S. and Seitzer, P. and Jarrett, T. and Kirkpatrick, J. D. and Gizis, J. E. and Howard, E. and Evans, T. and Fowler, J. and Fullmer, L. and Hurt, R. and Light, R. and Kopan, E. L. and Marsh, K. A. and McCallon, H. L. and Tam, R. and Van Dyk, S. and Wheelock, S.},
	month = feb,
	year = {2006},
	keywords = {Catalogs, Infrared: General, Surveys},
	pages = {1163--1183},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/CIKUFXWW/Skrutskie et al. - 2006 - The Two Micron All Sky Survey (2MASS).pdf:application/pdf}
}

@article{roser_deep_2011,
	title = {A deep all-sky census of the {Hyades}},
	volume = {531},
	copyright = {© ESO, 2011},
	issn = {0004-6361, 1432-0746},
	url = {https://www.aanda.org/articles/aa/abs/2011/07/aa16948-11/aa16948-11.html},
	doi = {10.1051/0004-6361/201116948},
	abstract = {{\textless}i{\textgreater}Aims.{\textless}i/{\textgreater} On the basis of the PPMXL catalogue we perform an all-sky census of the Hyades down to masses of about 0.2 {\textless}i{\textgreater}m{\textless}i/{\textgreater}{\textless}sub{\textgreater}⊙{\textless}sub/{\textgreater} in a region up to 30 pc from the cluster centre.{\textless}i{\textgreater}Methods.{\textless}i/{\textgreater} We use the proper motions from PPMXL in the convergent point method to determine probable kinematic members. From 2MASS photometry and CMC14 {\textless}i{\textgreater}r′{\textless}i/{\textgreater}-band photometry, we derive empirical colour-absolute magnitude diagrams and, finally, determine photometric membership for all kinematic candidates. {\textless}i{\textgreater}Results.{\textless}i/{\textgreater} This is the first deep ({\textless}i{\textgreater}r′{\textless}i/{\textgreater} ≤ 17) all-sky survey of the Hyades allowing a full three-dimensional analysis of the cluster. The survey is complete down to at least {\textless}i{\textgreater}M{\textless}i/{\textgreater}{\textless}sub{\textgreater}{\textless}i{\textgreater}K{\textless}i/{\textgreater}{\textless}sub{\textgreater}s{\textless}sub/{\textgreater}{\textless}sub/{\textgreater} = 7.3 or 0.25 {\textless}i{\textgreater}m{\textless}i/{\textgreater}{\textless}sub{\textgreater}⊙{\textless}sub/{\textgreater}. We find 724 stellar systems co-moving with the bulk Hyades space velocity, which represent a total mass of 435 {\textless}i{\textgreater}m{\textless}i/{\textgreater}{\textless}sub{\textgreater}⊙{\textless}sub/{\textgreater}. The tidal radius is about 9 pc, and 275 {\textless}i{\textgreater}m{\textless}i/{\textgreater}{\textless}sub{\textgreater}⊙{\textless}sub/{\textgreater} (364 systems) are gravitationally bound. This is the cluster proper. Its mass density profile is perfectly fitted by a Plummer model with a central density of 2.21 {\textless}i{\textgreater}m{\textless}i/{\textgreater}{\textless}sub{\textgreater}⊙{\textless}sub/{\textgreater} pc{\textless}sup{\textgreater}-3{\textless}sup/{\textgreater} and a core radius of {\textless}i{\textgreater}r{\textless}i/{\textgreater}{\textless}sub{\textgreater}co{\textless}sub/{\textgreater} = 3.10 pc, while the half-mass radius is {\textless}i{\textgreater}r{\textless}i/{\textgreater}{\textless}sub{\textgreater}h{\textless}sub/{\textgreater} = 4.1 pc. There are another 100 {\textless}i{\textgreater}m{\textless}i/{\textgreater}{\textless}sub{\textgreater}⊙{\textless}sub/{\textgreater} in a volume between one and two tidal radii (halo), and another 60 {\textless}i{\textgreater}m{\textless}i/{\textgreater}{\textless}sub{\textgreater}⊙{\textless}sub/{\textgreater} up to a distance of 30 pc from the centre. Strong mass segregation is inherent in the cluster. The present-day luminosity and mass functions are noticeably different in various parts of the cluster (core, corona, halo, and co-movers). They are strongly evolved compared to presently favoured initial mass functions. The analysis of the velocity dispersion of the cluster shows that about 20\% of its members must be binaries. As a by-product, we find that presently available theoretical isochrones are not able to adequately describe the near-infrared colour-absolute magnitude relation for those cluster stars that are less massive than about 0.6 {\textless}i{\textgreater}m{\textless}i/{\textgreater}{\textless}sub{\textgreater}⊙{\textless}sub/{\textgreater}.},
	language = {en},
	urldate = {2019-03-06},
	journal = {Astronomy \& Astrophysics},
	author = {R\"oser, S. and Schilbach, E. and Piskunov, A. E. and Kharchenko, N. V. and Scholz, R.-D.},
	month = jul,
	year = {2011},
	pages = {A92},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/7J9AB6QV/R\"oser et al. - 2011 - A deep all-sky census of the Hyades.pdf:application/pdf}
}

@article{rizzuto_multidimensional_2011,
	title = {Multidimensional {Bayesian} membership analysis of the {Sco} {OB}2 moving group},
	volume = {416},
	issn = {0035-8711},
	url = {http://adsabs.harvard.edu/abs/2011MNRAS.416.3108R},
	doi = {10.1111/j.1365-2966.2011.19256.x},
	abstract = {We present a new high-mass membership of the nearby Sco OB2 association based on Hipparcos positions, proper motions and parallaxes, and radial velocities taken from the 2nd Catalogue of Radial Velocities with Astrometric Data (CRVAD-2). The Bayesian membership selection method developed makes no distinction between subgroups of Sco OB2 and utilizes linear models in calculation of membership probabilities. We select 436 members, 88 of which are new members not included in previous membership selections. We include the classical non-members α-Cru and
β-Cru as new members as well as the pre-main-sequence stars HIP
79080 and 79081. We also show that the association is well mixed over distances of 8° on the sky, and hence no determination can be made as to the formation process of the entire association.},
	urldate = {2018-08-20},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Rizzuto, A. C. and Ireland, M. J. and Robertson, J. G.},
	month = oct,
	year = {2011},
	keywords = {stars: kinematics and dynamics, methods: statistical, stars: early-type, open clusters and associations: individual: Sco-Cen},
	pages = {3108--3117}
}

@article{bell_32ori_2017,
	title = {A stellar census of the nearby, young 32 {Orionis} group},
	volume = {468},
	issn = {0035-8711},
	url = {http://adsabs.harvard.edu/abs/2017MNRAS.468.1198B},
	doi = {10.1093/mnras/stx535},
	abstract = {The 32 Orionis group was discovered almost a decade ago and despite the fact that it represents the first northern, young (age ˜ 25 Myr) stellar aggregate within 100 pc of the Sun (d ≃ 93 pc), a
comprehensive survey for members and detailed characterization of the group has yet to be performed. We present the first large-scale
spectroscopic survey for new (predominantly M type) members of the group after combining kinematic and photometric data to select candidates with Galactic space motion and positions in colour-magnitude space consistent with membership. We identify 30 new members, increasing the number of known 32 Ori group members by a factor of 3 and bringing the total number of identified members to 46, spanning spectral types B5 to L1. We also identify the lithium depletion boundary (LDB) of the group, I.e. the luminosity at which lithium remains unburnt in a coeval population. We estimate the age of the 32 Ori group independently using both isochronal fitting and LDB analyses and find it is essentially coeval with the β Pictoris moving group, with an age of 24 ± 4 Myr.
Finally, we have also searched for circumstellar disc hosts utilizing the AllWISE catalogue. Although we find no evidence for warm, dusty discs, we identify several stars with excess emission in the WISE W4 band at 22 μm. Based on the limited number of W4 detections, we
estimate a debris disc fraction of 32{\textasciicircum}\{+12\}\_\{-8\} per cent for the 32 Ori group.},
	urldate = {2019-03-06},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Bell, Cameron P. M. and Murphy, Simon J. and Mamajek, Eric E.},
	month = jun,
	year = {2017},
	keywords = {stars: pre-main-sequence, stars: fundamental parameters, open clusters and associations: general, stars: kinematics and dynamics, solar neighbourhood},
	pages = {1198--1220}
}

@article{oh_comoving_2017,
	title = {Comoving {Stars} in {Gaia} {DR}1: {An} {Abundance} of {Very} {Wide} {Separation} {Comoving} {Pairs}},
	volume = {153},
	issn = {1538-3881},
	shorttitle = {Comoving {Stars} in {Gaia} {DR}1},
	url = {http://stacks.iop.org/1538-3881/153/i=6/a=257},
	doi = {10.3847/1538-3881/aa6ffd},
	abstract = {The primary sample of the Gaia Data Release 1 is the Tycho- Gaia Astrometric Solution (TGAS): ≈2 million Tycho-2 sources with improved parallaxes and proper motions relative to the initial catalog. This increased astrometric precision presents an opportunity to find new binary stars and moving groups. We search for high-confidence comoving pairs of stars in TGAS by identifying pairs of stars consistent with having the same 3D velocity using a marginalized likelihood ratio test to discriminate candidate comoving pairs from the field population. Although we perform some visualizations using (bias-corrected) inverse parallax as a point estimate of distance, the likelihood ratio is computed with a probabilistic model that includes the covariances of parallax and proper motions and marginalizes the (unknown) true distances and 3D velocities of the stars. We find 13,085 comoving star pairs among 10,606 unique stars with separations as large as 10 pc (our search limit). Some of these pairs form larger groups through mutual comoving neighbors: many of these pair networks correspond to known open clusters and OB associations, but we also report the discovery of several new comoving groups. Most surprisingly, we find a large number of very wide ( \#\#IMG\#\# [http://ej.iop.org/images/1538-3881/153/6/257/ajaa6ffdieqn1.gif] \${\textbackslash}gt 1\$ pc) separation comoving star pairs, the number of which increases with increasing separation and cannot be explained purely by false-positive contamination. Our key result is a catalog of high-confidence comoving pairs of stars in TGAS. We discuss the utility of this catalog for making dynamical inferences about the Galaxy, testing stellar atmosphere models, and validating chemical abundance measurements.},
	language = {en},
	number = {6},
	journal = {The Astronomical Journal},
	author = {Oh, Semyeong and Price-Whelan, Adrian M. and Hogg, David W. and Morton, Timothy D. and Spergel, David N.},
	year = {2017},
	pages = {257},
	file = {IOP Full Text PDF:/home/luke/local/Zotero/storage/E58MBUH7/Oh et al. - 2017 - Comoving Stars in Gaia DR1 An Abundance of Very W.pdf:application/pdf}
}

@article{kraus_tucanahor_2014,
	title = {A {Stellar} {Census} of the {Tucana}-{Horologium} {Moving} {Group}},
	volume = {147},
	issn = {0004-6256},
	url = {http://adsabs.harvard.edu/abs/2014AJ....147..146K},
	doi = {10.1088/0004-6256/147/6/146},
	abstract = {We report the selection and spectroscopic confirmation of 129 new late-type (SpT = K3-M6) members of the Tucana-Horologium moving group, a nearby (d {\textasciitilde} 40 pc), young (τ {\textasciitilde} 40 Myr) population of comoving stars. We also report observations for 13 of the 17 known Tuc-Hor members in this spectral type range, and that 62 additional candidates are likely to be unassociated field stars; the confirmation frequency for new candidates is therefore 129/191 = 67\%. We have used radial velocities, Hα emission, and Li6708 absorption to distinguish
between contaminants and bona fide members. Our expanded census of Tuc-Hor increases the known population by a factor of {\textasciitilde}3 in total and by a factor of {\textasciitilde}8 for members with SpT {\textgreater}= K3, but even so, the K-M dwarf population of Tuc-Hor is still markedly incomplete. Our expanded census allows for a much more detailed study of Tuc-Hor than was previously feasible. The spatial distribution of members appears to trace a two-dimensional sheet, with a broad distribution in X and Y, but a very narrow distribution (±5 pc) in Z. The corresponding velocity
distribution is very small, with a scatter of ±1.1 km
s-1 about the mean UVW velocity for stars spanning the entire 50 pc extent of Tuc-Hor. We also show that the isochronal age (τ {\textasciitilde} 20-30 Myr) and the lithium depletion boundary age (τ {\textasciitilde} 40 Myr)
disagree, following the trend in other pre-main-sequence populations for isochrones to yield systematically younger ages. The Hα emission line strength follows a trend of increasing equivalent width with later spectral type, as is seen for young clusters. We find that moving group members have been depleted of measurable lithium for spectral types of K7.0-M4.5. None of our targets have significant infrared excesses in the WISE W3 band, yielding an upper limit on warm debris disks of F {\textless} 0.7\%. Finally, our purely kinematic and color-magnitude selection procedure allows us to test the efficiency and completeness for
activity-based selection of young stars. We find that 60\% of K-M dwarfs in Tuc-Hor do not have ROSAT counterparts and would have been omitted in X-ray-selected samples. In contrast, GALEX UV-selected samples using a previously suggested criterion for youth achieve completeness of 77\% and purity of 78\%, and we suggest new SpT-dependent selection criteria that will yield {\textgreater}95\% completeness for τ {\textasciitilde} 40 Myr populations with
GALEX data available.},
	urldate = {2019-03-06},
	journal = {The Astronomical Journal},
	author = {Kraus, Adam L. and Shkolnik, Evgenya L. and Allers, Katelyn N. and Liu, Michael C.},
	month = jun,
	year = {2014},
	keywords = {binaries: spectroscopic, open clusters and associations: individual: Tucana-Horologium, stars: activity, stars: kinematics and dynamics, stars: low-mass, stars: pre-main sequence},
	pages = {146},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/FRQP5QIF/Kraus et al. - 2014 - A Stellar Census of the Tucana-Horologium Moving G.pdf:application/pdf}
}

@article{gagne_banyan_XII_2018,
	title = {{BANYAN}. {XII}. {New} {Members} of {Nearby} {Young} {Associations} from {GAIA}–{Tycho} {Data}},
	volume = {860},
	issn = {0004-637X},
	url = {http://adsabs.harvard.edu/abs/2018ApJ...860...43G},
	doi = {10.3847/1538-4357/aac2b8},
	abstract = {We present a search for stellar members of young associations within 150 pc of the Sun, based on TGAS and an updated version of the BANYAN Σ software to determine Bayesian membership probabilities that
includes Gaia–2MASS color-magnitude diagrams. We identify 32 new F0–M3-type bona fide members of the 10–200 Myr old Sco-Cen,
Carina, Tucana-Horologium, Columba, and Octans associations and the AB Doradus, β Pictoris, and Carina-Near moving groups. These new bona fide members have measurements of their full kinematics and literature data consistent with a young age. We also confirm the membership of 66 previously known candidate members using their Gaia–Tycho
trigonometric distances or new literature radial velocities, and identify 219 additional new candidate members, most of which do not yet have a radial velocity measurement. This work is the first step toward a completeness-corrected survey of young association members based on Gaia DR2 in the near future.},
	urldate = {2018-08-21},
	journal = {The Astrophysical Journal},
	author = {Gagn\'e, Jonathan and Roy-Loubier, Olivier and Faherty, Jacqueline K. and Doyon, Ren\'e and Malo, Lison},
	month = jun,
	year = {2018},
	keywords = {methods: data analysis, stars: kinematics and dynamics, proper motions},
	pages = {43}
}

@article{gagne_banyan_XI_2018,
	title = {{BANYAN}. {XI}. {The} {BANYAN} Σ {Multivariate} {Bayesian} {Algorithm} to {Identify} {Members} of {Young} {Associations} with 150 pc},
	volume = {856},
	issn = {0004-637X},
	url = {http://adsabs.harvard.edu/abs/2018ApJ...856...23G},
	doi = {10.3847/1538-4357/aaae09},
	abstract = {BANYAN Σ is a new Bayesian algorithm to identify members of young 
stellar associations within 150 pc of the Sun. It includes 27 young
associations with ages in the range ˜1-800 Myr, modeled with
multivariate Gaussians in six-dimensional (6D) XYZUVW space. It is the
first such multi-association classification tool to include the nearest
sub-groups of the Sco-Cen OB star-forming region, the IC 2602, IC 2391,
Pleiades and Platais 8 clusters, and the ρ Ophiuchi, Corona
Australis, and Taurus star formation regions. A model of field stars is
built from a mixture of multivariate Gaussians based on the
Besançon Galactic model. The algorithm can derive membership
probabilities for objects with only sky coordinates and proper motion,
but can also include parallax and radial velocity measurements, as well
as spectrophotometric distance constraints from sequences in
color-magnitude or spectral type-magnitude diagrams. BANYAN
Σ benefits from an analytical solution to the Bayesian
marginalization integrals over unknown radial velocities and distances
that makes it more accurate and significantly faster than its
predecessor BANYAN II. A contamination versus hit rate analysis is
presented and demonstrates that BANYAN Σ achieves a better
classification performance than other moving group tools available in
the literature, especially in terms of cross-contamination between young
associations. An updated list of bona fide members in the 27 young
associations, augmented by the Gaia-DR1 release, as well as all
parameters for the 6D multivariate Gaussian models for each association
and the Galactic field neighborhood within 300 pc are presented. This
new tool will make it possible to analyze large data sets such as the
upcoming Gaia-DR2 to identify new young stars. IDL and Python versions
of BANYAN Σ are made available with this publication, and a more
limited online web tool is available at http://www.exoplanetes.umontreal.ca/banyan/banyansigma.php.},
	urldate = {2019-03-06},
	journal = {The Astrophysical Journal},
	author = {Gagn\'e, Jonathan and Mamajek, Eric E. and Malo, Lison and Riedel, Adric and Rodriguez, David and Lafrenière, David and Faherty, Jacqueline K. and Roy-Loubier, Olivier and Pueyo, Laurent and Robin, Annie C. and Doyon, Ren\'e},
	month = mar,
	year = {2018},
	keywords = {brown dwarfs, methods: data analysis, proper motions, stars: kinematics and dynamics, stars: low-mass},
	pages = {23},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/HZB5D2XV/Gagn\'e et al. - 2018 - BANYAN. XI. The BANYAN Σ Multivariate Bayesian Alg.pdf:application/pdf}
}

@article{gagne_banyan_XIII_2018,
	title = {{BANYAN}. {XIII}. {A} {First} {Look} at {Nearby} {Young} {Associations} with {Gaia} {Data} {Release} 2},
	volume = {862},
	issn = {0004-637X},
	url = {https://doi.org/10.3847%2F1538-4357%2Faaca2e},
	doi = {10.3847/1538-4357/aaca2e},
	abstract = {In this paper, we examine the nearest 100 pc entries in Data Release 2 of Gaia to identify previously unrecognized candidate members in young associations. We analyze 695 952 stars with the BANYAN Σ Bayesian classification software and discover 898 new high-likelihood candidate members that span a wide range of properties, from spectral types B9 to L2, including 104 comoving systems, 111 brown dwarfs, and 31 new bona fide members. Our sample is mostly composed of highly active M dwarfs and will be crucial in examining the low-mass end of the initial mass function of young associations. Our sample includes new candidate members near the Galactic plane where previous surveys suffered from a high rate of contamination. This paper represents the first step toward a full reassessment of young associations in the solar neighborhood with the second data release of the Gaia mission.},
	language = {en},
	number = {2},
	urldate = {2019-03-06},
	journal = {The Astrophysical Journal},
	author = {Gagn\'e, Jonathan and Faherty, Jacqueline K.},
	month = jul,
	year = {2018},
	pages = {138},
	file = {IOP Full Text PDF:/home/luke/local/Zotero/storage/ETWXATEB/Gagn\'e and Faherty - 2018 - BANYAN. XIII. A First Look at Nearby Young Associa.pdf:application/pdf}
}

@article{dias_proper_2014,
	title = {Proper motions of the optically visible open clusters based on the {UCAC}4 catalog},
	volume = {564},
	issn = {0004-6361},
	url = {http://adsabs.harvard.edu/abs/2014A%26A...564A..79D},
	doi = {10.1051/0004-6361/201323226},
	abstract = {We present a catalog of mean proper motions and membership probabilities 
of individual stars for optically visible open clusters, which have been
determined using data from the UCAC4 catalog in a homogeneous way. The
mean proper motion of the cluster and the membership probabilities of
the stars in the region of each cluster were determined by applying the
statistical method in a modified fashion. In this study, we applied a
global optimization procedure to fit the observed distribution of proper
motions with two overlapping normal bivariate frequency functions, which
also take the individual proper motion errors into account. For 724
clusters, this is the first determination of proper motion, and for the
whole sample, we present results with a much larger number of identified
astrometric member stars. Furthermore, it was possible to estimate the
mean radial velocity of 364 clusters (102 unpublished so far) with the
stellar membership using published radial velocity catalogs. These
results provide an increase of 30\% and 19\% in the sample of open
clusters with a determined mean absolute proper motion and mean radial
velocity, respectively.

Tables 2 to 1809 are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr
(ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/564/A79},
	urldate = {2019-03-05},
	journal = {Astronomy and Astrophysics},
	author = {Dias, W. S. and Monteiro, H. and Caetano, T. C. and L\'epine, J. R. D. and Assafin, M. and Oliveira, A. F.},
	month = apr,
	year = {2014},
	keywords = {open clusters and associations: general},
	pages = {A79},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/APMM7HIB/Dias et al. - 2014 - Proper motions of the optically visible open clust.pdf:application/pdf}
}

@article{gaia_hr_2018,
	title = {Gaia {Data} {Release} 2. {Observational} {Hertzsprung}-{Russell} diagrams},
	volume = {616},
	url = {https://ui.adsabs.harvard.edu/?#abs/2018A%26A...616A..10G},
	doi = {10.1051/0004-6361/201832843},
	abstract = {Context. Gaia Data Release 2 provides high-precision astrometry and three-band photometry for about 1.3 billion sources over the full sky. The precision, accuracy, and homogeneity of both astrometry and photometry are unprecedented. {\textless}BR /{\textgreater} Aims: We highlight the power of the Gaia DR2 in studying many fine structures of the Hertzsprung-Russell diagram (HRD). Gaia allows us to present many different HRDs, depending in particular on stellar population selections. We do not aim here for completeness in terms of types of stars or stellar evolutionary aspects. Instead, we have chosen several illustrative examples. {\textless}BR /{\textgreater} Methods: We describe some of the selections that can be made in Gaia DR2 to highlight the main structures of the Gaia HRDs. We select both field and cluster (open and globular) stars, compare the observations with previous classifications and with stellar evolutionary tracks, and we present variations of the Gaia HRD with age, metallicity, and kinematics. Late stages of stellar evolution such as hot subdwarfs, post-AGB stars, planetary nebulae, and white dwarfs are also analysed, as well as low-mass brown dwarf objects. {\textless}BR /{\textgreater} Results: The Gaia HRDs are unprecedented in both precision and coverage of the various Milky Way stellar populations and stellar evolutionary phases. Many fine structures of the HRDs are presented. The clear split of the white dwarf sequence into hydrogen and helium white dwarfs is presented for the first time in an HRD. The relation between kinematics and the HRD is nicely illustrated. Two different populations in a classical kinematic selection of the halo are unambiguously identified in the HRD. Membership and mean parameters for a selected list of open clusters are provided. They allow drawing very detailed cluster sequences, highlighting fine structures, and providing extremely precise empirical isochrones that will lead to more insight in stellar physics. {\textless}BR /{\textgreater} Conclusions: Gaia DR2 demonstrates the potential of combining precise astrometry and photometry for large samples for studies in stellar evolution and stellar population and opens an entire new area for HRD-based studies. The full Table A.1 is only available at the CDS via anonymous ftp to {\textless}A href="http://cdsarc.u-strasbg.fr"{\textgreater}http://cdsarc.u-strasbg.fr{\textless}/A{\textgreater} ({\textless}A href="http://cdsarc.u-strasbg.fr"{\textgreater}http://130.79.128.5{\textless}/A{\textgreater}) or via {\textless}A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/616/A10"{\textgreater}http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/616/A10{\textless}/A{\textgreater}},
	language = {en},
	urldate = {2019-03-06},
	journal = {Astronomy and Astrophysics},
	author = {{Gaia Collaboration} and Babusiaux, C. and van Leeuwen, F. and Barstow, M. A. and Jordi, C. and Vallenari, A. and Bossini, D. and Bressan, A. and Cantat-Gaudin, T. and van Leeuwen, M. and Brown, A. G. A. and Prusti, T. and de Bruijne, J. H. J. and Bailer-Jones, C. a. L. and Biermann, M. and Evans, D. W. and Eyer, L. and Jansen, F. and Klioner, S. A. and Lammers, U. and Lindegren, L. and Luri, X. and Mignard, F. and Panem, C. and Pourbaix, D. and Randich, S. and Sartoretti, P. and Siddiqui, H. I. and Soubiran, C. and Walton, N. A. and Arenou, F. and Bastian, U. and Cropper, M. and Drimmel, R. and Katz, D. and Lattanzi, M. G. and Bakker, J. and Cacciari, C. and Castañeda, J. and Chaoul, L. and Cheek, N. and De Angeli, F. and Fabricius, C. and Guerra, R. and Holl, B. and Masana, E. and Messineo, R. and Mowlavi, N. and Nienartowicz, K. and Panuzzo, P. and Portell, J. and Riello, M. and Seabroke, G. M. and Tanga, P. and Th\'evenin, F. and Gracia-Abril, G. and Comoretto, G. and Garcia-Reinaldos, M. and Teyssier, D. and Altmann, M. and Andrae, R. and Audard, M. and Bellas-Velidis, I. and Benson, K. and Berthier, J. and Blomme, R. and Burgess, P. and Busso, G. and Carry, B. and Cellino, A. and Clementini, G. and Clotet, M. and Creevey, O. and Davidson, M. and De Ridder, J. and Delchambre, L. and Dell'Oro, A. and Ducourant, C. and Fernández-Hernández, J. and Fouesneau, M. and Fr\'emat, Y. and Galluccio, L. and García-Torres, M. and González-Núñez, J. and González-Vidal, J. J. and Gosset, E. and Guy, L. P. and Halbwachs, J.-L. and Hambly, N. C. and Harrison, D. L. and Hernández, J. and Hestroffer, D. and Hodgkin, S. T. and Hutton, A. and Jasniewicz, G. and Jean-Antoine-Piccolo, A. and Jordan, S. and Korn, A. J. and Krone-Martins, A. and Lanzafame, A. C. and Lebzelter, T. and L\"offler, W. and Manteiga, M. and Marrese, P. M. and Martín-Fleitas, J. M. and Moitinho, A. and Mora, A. and Muinonen, K. and Osinde, J. and Pancino, E. and Pauwels, T. and Petit, J.-M. and Recio-Blanco, A. and Richards, P. J. and Rimoldini, L. and Robin, A. C. and Sarro, L. M. and Siopis, C. and Smith, M. and Sozzetti, A. and Süveges, M. and Torra, J. and van Reeven, W. and Abbas, U. and Abreu Aramburu, A. and Accart, S. and Aerts, C. and Altavilla, G. and Álvarez, M. A. and Alvarez, R. and Alves, J. and Anderson, R. I. and Andrei, A. H. and Anglada Varela, E. and Antiche, E. and Antoja, T. and Arcay, B. and Astraatmadja, T. L. and Bach, N. and Baker, S. G. and Balaguer-Núñez, L. and Balm, P. and Barache, C. and Barata, C. and Barbato, D. and Barblan, F. and Barklem, P. S. and Barrado, D. and Barros, M. and Bartholom\'e Muñoz, L. and Bassilana, J.-L. and Becciani, U. and Bellazzini, M. and Berihuete, A. and Bertone, S. and Bianchi, L. and Bienaym\'e, O. and Blanco-Cuaresma, S. and Boch, T. and Boeche, C. and Bombrun, A. and Borrachero, R. and Bouquillon, S. and Bourda, G. and Bragaglia, A. and Bramante, L. and Breddels, M. A. and Brouillet, N. and Brüsemeister, T. and Brugaletta, E. and Bucciarelli, B. and Burlacu, A. and Busonero, D. and Butkevich, A. G. and Buzzi, R. and Caffau, E. and Cancelliere, R. and Cannizzaro, G. and Carballo, R. and Carlucci, T. and Carrasco, J. M. and Casamiquela, L. and Castellani, M. and Castro-Ginard, A. and Charlot, P. and Chemin, L. and Chiavassa, A. and Cocozza, G. and Costigan, G. and Cowell, S. and Crifo, F. and Crosta, M. and Crowley, C. and Cuypers, J. and Dafonte, C. and Damerdji, Y. and Dapergolas, A. and David, P. and David, M. and de Laverny, P. and De Luise, F. and De March, R. and de Martino, D. and de Souza, R. and de Torres, A. and Debosscher, J. and del Pozo, E. and Delbo, M. and Delgado, A. and Delgado, H. E. and Diakite, S. and Diener, C. and Distefano, E. and Dolding, C. and Drazinos, P. and Durán, J. and Edvardsson, B. and Enke, H. and Eriksson, K. and Esquej, P. and Eynard Bontemps, G. and Fabre, C. and Fabrizio, M. and Faigler, S. and Falcão, A. J. and Farràs Casas, M. and Federici, L. and Fedorets, G. and Fernique, P. and Figueras, F. and Filippi, F. and Findeisen, K. and Fonti, A. and Fraile, E. and Fraser, M. and Fr\'ezouls, B. and Gai, M. and Galleti, S. and Garabato, D. and García-Sedano, F. and Garofalo, A. and Garralda, N. and Gavel, A. and Gavras, P. and Gerssen, J. and Geyer, R. and Giacobbe, P. and Gilmore, G. and Girona, S. and Giuffrida, G. and Glass, F. and Gomes, M. and Granvik, M. and Gueguen, A. and Guerrier, A. and Guiraud, J. and Guti\'e, R. and Haigron, R. and Hatzidimitriou, D. and Hauser, M. and Haywood, M. and Heiter, U. and Helmi, A. and Heu, J. and Hilger, T. and Hobbs, D. and Hofmann, W. and Holland, G. and Huckle, H. E. and Hypki, A. and Icardi, V. and Janßen, K. and Jevardat de Fombelle, G. and Jonker, P. G. and Juhász, Á L. and Julbe, F. and Karampelas, A. and Kewley, A. and Klar, J. and Kochoska, A. and Kohley, R. and Kolenberg, K. and Kontizas, M. and Kontizas, E. and Koposov, S. E. and Kordopatis, G. and Kostrzewa-Rutkowska, Z. and Koubsky, P. and Lambert, S. and Lanza, A. F. and Lasne, Y. and Lavigne, J.-B. and Le Fustec, Y. and Le Poncin-Lafitte, C. and Lebreton, Y. and Leccia, S. and Leclerc, N. and Lecoeur-Taibi, I. and Lenhardt, H. and Leroux, F. and Liao, S. and Licata, E. and Lindstrøm, H. E. P. and Lister, T. A. and Livanou, E. and Lobel, A. and López, M. and Managau, S. and Mann, R. G. and Mantelet, G. and Marchal, O. and Marchant, J. M. and Marconi, M. and Marinoni, S. and Marschalkó, G. and Marshall, D. J. and Martino, M. and Marton, G. and Mary, N. and Massari, D. and Matijevič, G. and Mazeh, T. and McMillan, P. J. and Messina, S. and Michalik, D. and Millar, N. R. and Molina, D. and Molinaro, R. and Molnár, L. and Montegriffo, P. and Mor, R. and Morbidelli, R. and Morel, T. and Morris, D. and Mulone, A. F. and Muraveva, T. and Musella, I. and Nelemans, G. and Nicastro, L. and Noval, L. and O'Mullane, W. and Ord\'enovic, C. and Ordóñez-Blanco, D. and Osborne, P. and Pagani, C. and Pagano, I. and Pailler, F. and Palacin, H. and Palaversa, L. and Panahi, A. and Pawlak, M. and Piersimoni, A. M. and Pineau, F.-X. and Plachy, E. and Plum, G. and Poggio, E. and Poujoulet, E. and Prša, A. and Pulone, L. and Racero, E. and Ragaini, S. and Rambaux, N. and Ramos-Lerate, M. and Regibo, S. and Reyl\'e, C. and Riclet, F. and Ripepi, V. and Riva, A. and Rivard, A. and Rixon, G. and Roegiers, T. and Roelens, M. and Romero-Gómez, M. and Rowell, N. and Royer, F. and Ruiz-Dern, L. and Sadowski, G. and Sagristà Sell\'es, T. and Sahlmann, J. and Salgado, J. and Salguero, E. and Sanna, N. and Santana-Ros, T. and Sarasso, M. and Savietto, H. and Schultheis, M. and Sciacca, E. and Segol, M. and Segovia, J. C. and S\'egransan, D. and Shih, I.-C. and Siltala, L. and Silva, A. F. and Smart, R. L. and Smith, K. W. and Solano, E. and Solitro, F. and Sordo, R. and Soria Nieto, S. and Souchay, J. and Spagna, A. and Spoto, F. and Stampa, U. and Steele, I. A. and Steidelmüller, H. and Stephenson, C. A. and Stoev, H. and Suess, F. F. and Surdej, J. and Szabados, L. and Szegedi-Elek, E. and Tapiador, D. and Taris, F. and Tauran, G. and Taylor, M. B. and Teixeira, R. and Terrett, D. and Teyssandier, P. and Thuillot, W. and Titarenko, A. and Torra Clotet, F. and Turon, C. and Ulla, A. and Utrilla, E. and Uzzi, S. and Vaillant, M. and Valentini, G. and Valette, V. and van Elteren, A. and Van Hemelryck, E. and Vaschetto, M. and Vecchiato, A. and Veljanoski, J. and Viala, Y. and Vicente, D. and Vogt, S. and von Essen, C. and Voss, H. and Votruba, V. and Voutsinas, S. and Walmsley, G. and Weiler, M. and Wertz, O. and Wevers, T. and Wyrzykowski, Ł and Yoldas, A. and Žerjal, M. and Ziaeepour, H. and Zorec, J. and Zschocke, S. and Zucker, S. and Zurbach, C. and Zwitter, T.},
	month = aug,
	year = {2018},
	pages = {A10},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/SYQZZYUM/Collaboration et al. - 2018 - Gaia Data Release 2. Observational Hertzsprung-Rus.pdf:application/pdf;Snapshot:/home/luke/local/Zotero/storage/RLSXJ9IZ/ui.adsabs.harvard.edu.html:text/html}
}

@article{cantat-gaudin_gaia_2018,
	title = {A {Gaia} {DR}2 view of the open cluster population in the {Milky} {Way}},
	volume = {618},
	copyright = {© ESO 2018},
	issn = {0004-6361, 1432-0746},
	url = {https:/articles/aa/abs/2018/10/aa33476-18/aa33476-18.html},
	doi = {10.1051/0004-6361/201833476},
	abstract = {{\textless}i{\textgreater}Context.{\textless}i/{\textgreater} Open clusters are convenient probes of the structure and history of the Galactic disk. They are also fundamental to stellar evolution studies. The second {\textless}i{\textgreater}Gaia{\textless}i/{\textgreater} data release contains precise astrometry at the submilliarcsecond level and homogeneous photometry at the mmag level, that can be used to characterise a large number of clusters over the entire sky.{\textless}i{\textgreater}Aims.{\textless}i/{\textgreater} In this study we aim to establish a list of members and derive mean parameters, in particular distances, for as many clusters as possible, making use of {\textless}i{\textgreater}Gaia{\textless}i/{\textgreater} data alone.{\textless}i{\textgreater}Methods.{\textless}i/{\textgreater} We compiled a list of thousands of known or putative clusters from the literature. We then applied an unsupervised membership assignment code, UPMASK, to the {\textless}i{\textgreater}Gaia{\textless}i/{\textgreater} DR2 data contained within the fields of those clusters.{\textless}i{\textgreater}Results.{\textless}i/{\textgreater} We obtained a list of members and cluster parameters for 1229 clusters. As expected, the youngest clusters are seen to be tightly distributed near the Galactic plane and to trace the spiral arms of the Milky Way, while older objects are more uniformly distributed, deviate further from the plane, and tend to be located at larger Galactocentric distances. Thanks to the quality of {\textless}i{\textgreater}Gaia{\textless}i/{\textgreater} DR2 astrometry, the fully homogeneous parameters derived in this study are the most precise to date. Furthermore, we report on the serendipitous discovery of 60 new open clusters in the fields analysed during this study.},
	language = {en},
	urldate = {2019-03-06},
	journal = {Astronomy \& Astrophysics},
	author = {Cantat-Gaudin, T. and Jordi, C. and Vallenari, A. and Bragaglia, A. and Balaguer-Núñez, L. and Soubiran, C. and Bossini, D. and Moitinho, A. and Castro-Ginard, A. and Krone-Martins, A. and Casamiquela, L. and Sordo, R. and Carrera, R.},
	month = oct,
	year = {2018},
	pages = {A93},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/CA8ICTDD/Cantat-Gaudin et al. - 2018 - A Gaia DR2 view of the open cluster population in .pdf:application/pdf;Snapshot:/home/luke/local/Zotero/storage/EBECUSCK/aa33476-18.html:text/html}
}

@misc{kim_2018_gaia2read,
  title = {Querying Gaia for Wide Binary Companions to Exoplanet
    Hosts},
  author = {Kim, J.},
  year={2018},
  howpublished= {Princeton Junior Thesis (Unpublished)}
}


@book{dierckx_curve_1996,
	address = {Oxford},
	edition = {Repr},
	series = {Monographs on {Numerical} {Analysis}},
	title = {Curve and surface fitting with splines},
	isbn = {978-0-19-853440-2},
	language = {eng},
	publisher = {Clarendon Press},
	author = {Dierckx, Paul},
	year = {1996},
	note = {OCLC: 245719230},
	annote = {Includes bibliographical references and index},
	file = {Table of Contents PDF:/home/luke/local/Zotero/storage/9LCJ5WWV/Dierckx - 1996 - Curve and surface fitting with splines.pdf:application/pdf}
}

@article{huang_high-precision_2015,
	title = {High-precision photometry for {K}2 {Campaign} 1},
	volume = {454},
	issn = {0035-8711},
	url = {http://adsabs.harvard.edu/abs/2015MNRAS.454.4159H},
	doi = {10.1093/mnras/stv2257},
	abstract = {The two reaction wheel K2 mission promises and has delivered new discoveries in the stellar and exoplanet fields. However, due to the loss of accurate pointing, it also brings new challenges for the data reduction processes. In this paper, we describe a new reduction pipeline for extracting high-precision photometry from the K2 data set, and present public light curves for the K2 Campaign 1 target pixel data set. Key to our reduction is the derivation of global astrometric solutions from the target stamps, from which accurate centroids are passed on for high-precision photometry extraction. We extract target light curves for sources from a combined UCAC4 and EPIC catalogue - this includes not only primary targets of the K2 campaign 1, but also any other stars that happen to fall on the pixel stamps. We provide the raw light curves, and the products of various detrending processes aimed at removing different types of systematics. Our astrometric solutions achieve a median residual of ˜0.127 arcsec. For bright stars, our best 6.5 h
precision for raw light curves is ˜20 parts per million (ppm). For our detrended light curves, the best 6.5 h precision achieved is ˜15 ppm. We show that our detrended light curves have fewer
systematic effects (or trends, or red-noise) than light curves produced by other groups from the same observations. Example light curves of transiting planets and a Cepheid variable candidate, are also presented. We make all light curves public, including the raw and detrended photometry, at http://k2.hatsurveys.org.},
	urldate = {2018-10-28},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Huang, C. X. and Penev, K. and Hartman, J. D. and Bakos, G. Á. and Bhatti, W. and Domsa, I. and de Val-Borro, M.},
	month = dec,
	year = {2015},
	keywords = {surveys, techniques: photometric, methods: data analysis, METHODS: DATA ANALYSIS, astrometry},
	pages = {4159--4171},
	annote = {nb. this is the entire HATNET team. Huang on point, Hartman, Penev, de Val-Borro, Bhatti. No Melinda Soares.},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/9UWD9MCH/Huang et al. - 2015 - High-precision photometry for K2 Campaign 1.pdf:application/pdf;Snapshot:/home/luke/local/Zotero/storage/CIAVC9MD/4159.html:text/html}
}

@article{zhang_precision_2016,
	title = {Precision {Multiband} {Photometry} with a {DSLR} {Camera}},
	volume = {128},
	issn = {0004-6280},
	url = {http://adsabs.harvard.edu/abs/2016PASP..128c5001Z},
	doi = {10.1088/1538-3873/128/961/035001},
	abstract = {Ground-based exoplanet surveys such as SuperWASP, HAT Network of Telescopes (HATNet), and KELT have discovered close to two hundred transiting extrasolar planets in the past several years. The strategy of these surveys is to look at a large field of view and measure the brightnesses of its bright stars to around half a percent per point precision, which is adequate for detecting hot Jupiters. Typically, these surveys use CCD detectors to achieve high precision photometry. These CCDS, however, are expensive relative to other consumer-grade optical imaging devices, such as digital single-lens reflex cameras (DSLRs). We look at the possibility of using a DSLR camera for precision photometry. Specifically, we used a Canon EOS 60D camera that records light in three colors simultaneously. The DSLR was integrated into the HATNet survey and collected observations for a month, after which photometry was extracted for 6600 stars in a selected stellar field. We found that the DSLR achieves a best-case median absolute deviation of 4.6 mmag per 180 s exposure when the DSLR color channels are combined, and 1000 stars are measured to better than 10 mmag (1\%). Also, we achieve 10 mmag or better photometry in the individual colors. This is good enough to detect transiting hot Jupiters. We performed a candidate search on all stars and found four candidates, one of which is KELT-3b, the only known transiting hot Jupiter in our selected field. We conclude that the Canon 60D is a cheap, lightweight device capable of useful photometry in multiple colors.},
	urldate = {2018-03-26},
	journal = {Publications of the Astronomical Society of the Pacific},
	author = {Zhang, M. and Bakos, G. A. and Penev, K. and Csubry, Z. and Hartman, J. D. and Bhatti, W. and de Val-Borro, M.},
	month = mar,
	year = {2016},
	pages = {035001}
}

@article{gaia_collaboration_gaia_2016,
	title = {The {Gaia} mission},
	volume = {595},
	issn = {0004-6361},
	url = {http://adsabs.harvard.edu/abs/2016A%26A...595A...1G},
	doi = {10.1051/0004-6361/201629272},
	abstract = {Gaia is a cornerstone mission in the science programme of the EuropeanSpace Agency (ESA). The spacecraft construction was approved in 2006, following a study in which the original interferometric concept was changed to a direct-imaging approach. Both the spacecraft and the payload were built by European industry. The involvement of the
	scientific community focusses on data processing for which the
	international Gaia Data Processing and Analysis Consortium (DPAC) was selected in 2007. Gaia was launched on 19 December 2013 and arrived at its operating point, the second Lagrange point of the Sun-Earth-Moon system, a few weeks later. The commissioning of the spacecraft and payload was completed on 19 July 2014. The nominal five-year mission started with four weeks of special, ecliptic-pole scanning and
	subsequently transferred into full-sky scanning mode. We recall the scientific goals of Gaia and give a description of the as-built
	spacecraft that is currently (mid-2016) being operated to achieve these goals. We pay special attention to the payload module, the performance of which is closely related to the scientific performance of the mission. We provide a summary of the commissioning activities and findings, followed by a description of the routine operational mode. We summarise scientific performance estimates on the basis of in-orbit operations. Several intermediate Gaia data releases are planned and the data can be retrieved from the Gaia Archive, which is available through the Gaia home page.
	
	http://www.cosmos.esa.int/gaia},
	urldate = {2018-11-29},
	journal = {Astronomy and Astrophysics},
	author = {{Gaia Collaboration} and Prusti, T. and de Bruijne, J. H. J. and Brown, A. G. A. and Vallenari, A. and Babusiaux, C. and Bailer-Jones, C. A. L. and Bastian, U. and Biermann, M. and Evans, D. W. and Eyer, L. and Jansen, F. and Jordi, C. and Klioner, S. A. and Lammers, U. and Lindegren, L. and Luri, X. and Mignard, F. and Milligan, D. J. and Panem, C. and Poinsignon, V. and Pourbaix, D. and Randich, S. and Sarri, G. and Sartoretti, P. and Siddiqui, H. I. and Soubiran, C. and Valette, V. and van Leeuwen, F. and Walton, N. A. and Aerts, C. and Arenou, F. and Cropper, M. and Drimmel, R. and Høg, E. and Katz, D. and Lattanzi, M. G. and O'Mullane, W. and Grebel, E. K. and Holland, A. D. and Huc, C. and Passot, X. and Bramante, L. and Cacciari, C. and Castañeda, J. and Chaoul, L. and Cheek, N. and De Angeli, F. and Fabricius, C. and Guerra, R. and Hernández, J. and Jean-Antoine-Piccolo, A. and Masana, E. and Messineo, R. and Mowlavi, N. and Nienartowicz, K. and Ordóñez-Blanco, D. and Panuzzo, P. and Portell, J. and Richards, P. J. and Riello, M. and Seabroke, G. M. and Tanga, P. and Th\'evenin, F. and Torra, J. and Els, S. G. and Gracia-Abril, G. and Comoretto, G. and Garcia-Reinaldos, M. and Lock, T. and Mercier, E. and Altmann, M. and Andrae, R. and Astraatmadja, T. L. and Bellas-Velidis, I. and Benson, K. and Berthier, J. and Blomme, R. and Busso, G. and Carry, B. and Cellino, A. and Clementini, G. and Cowell, S. and Creevey, O. and Cuypers, J. and Davidson, M. and De Ridder, J. and de Torres, A. and Delchambre, L. and Dell'Oro, A. and Ducourant, C. and Fr\'emat, Y. and García-Torres, M. and Gosset, E. and Halbwachs, J.-L. and Hambly, N. C. and Harrison, D. L. and Hauser, M. and Hestroffer, D. and Hodgkin, S. T. and Huckle, H. E. and Hutton, A. and Jasniewicz, G. and Jordan, S. and Kontizas, M. and Korn, A. J. and Lanzafame, A. C. and Manteiga, M. and Moitinho, A. and Muinonen, K. and Osinde, J. and Pancino, E. and Pauwels, T. and Petit, J.-M. and Recio-Blanco, A. and Robin, A. C. and Sarro, L. M. and Siopis, C. and Smith, M. and Smith, K. W. and Sozzetti, A. and Thuillot, W. and van Reeven, W. and Viala, Y. and Abbas, U. and Abreu Aramburu, A. and Accart, S. and Aguado, J. J. and Allan, P. M. and Allasia, W. and Altavilla, G. and Álvarez, M. A. and Alves, J. and Anderson, R. I. and Andrei, A. H. and Anglada Varela, E. and Antiche, E. and Antoja, T. and Antón, S. and Arcay, B. and Atzei, A. and Ayache, L. and Bach, N. and Baker, S. G. and Balaguer-Núñez, L. and Barache, C. and Barata, C. and Barbier, A. and Barblan, F. and Baroni, M. and Barrado y Navascu\'es, D. and Barros, M. and Barstow, M. A. and Becciani, U. and Bellazzini, M. and Bellei, G. and Bello García, A. and Belokurov, V. and Bendjoya, P. and Berihuete, A. and Bianchi, L. and Bienaym\'e, O. and Billebaud, F. and Blagorodnova, N. and Blanco-Cuaresma, S. and Boch, T. and Bombrun, A. and Borrachero, R. and Bouquillon, S. and Bourda, G. and Bouy, H. and Bragaglia, A. and Breddels, M. A. and Brouillet, N. and Brüsemeister, T. and Bucciarelli, B. and Budnik, F. and Burgess, P. and Burgon, R. and Burlacu, A. and Busonero, D. and Buzzi, R. and Caffau, E. and Cambras, J. and Campbell, H. and Cancelliere, R. and Cantat-Gaudin, T. and Carlucci, T. and Carrasco, J. M. and Castellani, M. and Charlot, P. and Charnas, J. and Charvet, P. and Chassat, F. and Chiavassa, A. and Clotet, M. and Cocozza, G. and Collins, R. S. and Collins, P. and Costigan, G. and Crifo, F. and Cross, N. J. G. and Crosta, M. and Crowley, C. and Dafonte, C. and Damerdji, Y. and Dapergolas, A. and David, P. and David, M. and De Cat, P. and de Felice, F. and de Laverny, P. and De Luise, F. and De March, R. and de Martino, D. and de Souza, R. and Debosscher, J. and del Pozo, E. and Delbo, M. and Delgado, A. and Delgado, H. E. and di Marco, F. and Di Matteo, P. and Diakite, S. and Distefano, E. and Dolding, C. and Dos Anjos, S. and Drazinos, P. and Durán, J. and Dzigan, Y. and Ecale, E. and Edvardsson, B. and Enke, H. and Erdmann, M. and Escolar, D. and Espina, M. and Evans, N. W. and Eynard Bontemps, G. and Fabre, C. and Fabrizio, M. and Faigler, S. and Falcão, A. J. and Farràs Casas, M. and Faye, F. and Federici, L. and Fedorets, G. and Fernández-Hernández, J. and Fernique, P. and Fienga, A. and Figueras, F. and Filippi, F. and Findeisen, K. and Fonti, A. and Fouesneau, M. and Fraile, E. and Fraser, M. and Fuchs, J. and Furnell, R. and Gai, M. and Galleti, S. and Galluccio, L. and Garabato, D. and García-Sedano, F. and Gar\'e, P. and Garofalo, A. and Garralda, N. and Gavras, P. and Gerssen, J. and Geyer, R. and Gilmore, G. and Girona, S. and Giuffrida, G. and Gomes, M. and González-Marcos, A. and González-Núñez, J. and González-Vidal, J. J. and Granvik, M. and Guerrier, A. and Guillout, P. and Guiraud, J. and Gúrpide, A. and Guti\'errez-Sánchez, R. and Guy, L. P. and Haigron, R. and Hatzidimitriou, D. and Haywood, M. and Heiter, U. and Helmi, A. and Hobbs, D. and Hofmann, W. and Holl, B. and Holland, G. and Hunt, J. A. S. and Hypki, A. and Icardi, V. and Irwin, M. and Jevardat de Fombelle, G. and Jofr\'e, P. and Jonker, P. G. and Jorissen, A. and Julbe, F. and Karampelas, A. and Kochoska, A. and Kohley, R. and Kolenberg, K. and Kontizas, E. and Koposov, S. E. and Kordopatis, G. and Koubsky, P. and Kowalczyk, A. and Krone-Martins, A. and Kudryashova, M. and Kull, I. and Bachchan, R. K. and Lacoste-Seris, F. and Lanza, A. F. and Lavigne, J.-B. and Le Poncin-Lafitte, C. and Lebreton, Y. and Lebzelter, T. and Leccia, S. and Leclerc, N. and Lecoeur-Taibi, I. and Lemaitre, V. and Lenhardt, H. and Leroux, F. and Liao, S. and Licata, E. and Lindstrøm, H. E. P. and Lister, T. A. and Livanou, E. and Lobel, A. and L\"offler, W. and López, M. and Lopez-Lozano, A. and Lorenz, D. and Loureiro, T. and MacDonald, I. and Magalhães Fernandes, T. and Managau, S. and Mann, R. G. and Mantelet, G. and Marchal, O. and Marchant, J. M. and Marconi, M. and Marie, J. and Marinoni, S. and Marrese, P. M. and Marschalkó, G. and Marshall, D. J. and Martín-Fleitas, J. 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S. and Olias Sanz, A. and Ortiz, P. and Osorio, J. and Oszkiewicz, D. and Ouzounis, A. and Palmer, M. and Park, P. and Pasquato, E. and Peltzer, C. and Peralta, J. and P\'eturaud, F. and Pieniluoma, T. and Pigozzi, E. and Poels, J. and Prat, G. and Prod'homme, T. and Raison, F. and Rebordao, J. M. and Risquez, D. and Rocca-Volmerange, B. and Rosen, S. and Ruiz-Fuertes, M. I. and Russo, F. and Sembay, S. and Serraller Vizcaino, I. and Short, A. and Siebert, A. and Silva, H. and Sinachopoulos, D. and Slezak, E. and Soffel, M. and Sosnowska, D. and Straižys, V. and ter Linden, M. and Terrell, D. and Theil, S. and Tiede, C. and Troisi, L. and Tsalmantza, P. and Tur, D. and Vaccari, M. and Vachier, F. and Valles, P. and Van Hamme, W. and Veltz, L. and Virtanen, J. and Wallut, J.-M. and Wichmann, R. and Wilkinson, M. I. and Ziaeepour, H. and Zschocke, S.},
	month = nov,
	year = {2016},
	keywords = {astrometry, Galaxy: structure, parallaxes, proper motions, space vehicles: instruments, telescopes},
	pages = {A1},
	file = {Full Text PDF:/Users/luke/Zotero/storage/F496L4QC/Gaia Collaboration et al. - 2016 - The Gaia mission.pdf:application/pdf}
}



@article{gaia_collaboration_gaia_2018,
	title = {Gaia {Data} {Release} 2. {Summary} of the contents and survey properties},
	volume = {616},
	issn = {0004-6361},
	url = {http://adsabs.harvard.edu/abs/2018A%26A...616A...1G},
	doi = {10.1051/0004-6361/201833051},
	abstract = {Context. We present the second Gaia data release, Gaia DR2, consisting of astrometry, photometry, radial velocities, and information on astrophysical parameters and variability, for sources brighter than magnitude 21. In addition epoch astrometry and photometry are provided for a modest sample of minor planets in the solar system. Aims: A summary of the contents of Gaia DR2 is presented, accompanied by a discussion on the differences with respect to Gaia DR1 and an overview of the main limitations which are still present in the survey.
	Recommendations are made on the responsible use of Gaia DR2 results. Methods: The raw data collected with the Gaia instruments during the first 22 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium (DPAC) and turned into this second data release, which represents a major advance with respect to Gaia DR1 in terms of completeness, performance, and richness of the data
	products. Results: Gaia DR2 contains celestial positions and the apparent brightness in G for approximately 1.7 billion sources. For 1.3 billion of those sources, parallaxes and proper motions are in addition available. The sample of sources for which variability information is provided is expanded to 0.5 million stars. This data release contains four new elements: broad-band colour information in the form of the apparent brightness in the GBP (330-680 nm) and
	GRP (630-1050 nm) bands is available for 1.4 billion sources; median radial velocities for some 7 million sources are presented; for between 77 and 161 million sources estimates are provided of the stellar effective temperature, extinction, reddening, and radius and luminosity; and for a pre-selected list of 14 000 minor planets in the solar system epoch astrometry and photometry are presented. Finally, Gaia DR2 also represents a new materialisation of the celestial reference frame in the optical, the Gaia-CRF2, which is the first optical reference frame based solely on extragalactic sources. There are notable changes in the photometric system and the catalogue source list with respect to Gaia DR1, and we stress the need to consider the two data releases as independent. Conclusions: Gaia DR2 represents a major achievement for the Gaia mission, delivering on the long standing promise to provide parallaxes and proper motions for over 1 billion stars, and representing a first step in the availability of complementary radial velocity and source astrophysical information for a sample of stars in the Gaia survey which covers a very substantial fraction of the volume of our galaxy.},
	urldate = {2018-11-29},
	journal = {Astronomy and Astrophysics},
	author = {{Gaia Collaboration} and Brown, A. G. A. and Vallenari, A. and Prusti, T. and de Bruijne, J. H. J. and Babusiaux, C. and Bailer-Jones, C. A. L. and Biermann, M. and Evans, D. W. and Eyer, L. and Jansen, F. and Jordi, C. and Klioner, S. A. and Lammers, U. and Lindegren, L. and Luri, X. and Mignard, F. and Panem, C. and Pourbaix, D. and Randich, S. and Sartoretti, P. and Siddiqui, H. I. and Soubiran, C. and van Leeuwen, F. and Walton, N. A. and Arenou, F. and Bastian, U. and Cropper, M. and Drimmel, R. and Katz, D. and Lattanzi, M. G. and Bakker, J. and Cacciari, C. and Castañeda, J. and Chaoul, L. and Cheek, N. and De Angeli, F. and Fabricius, C. and Guerra, R. and Holl, B. and Masana, E. and Messineo, R. and Mowlavi, N. and Nienartowicz, K. and Panuzzo, P. and Portell, J. and Riello, M. and Seabroke, G. M. and Tanga, P. and Th\'evenin, F. and Gracia-Abril, G. and Comoretto, G. and Garcia-Reinaldos, M. and Teyssier, D. and Altmann, M. and Andrae, R. and Audard, M. and Bellas-Velidis, I. and Benson, K. and Berthier, J. and Blomme, R. and Burgess, P. and Busso, G. and Carry, B. and Cellino, A. and Clementini, G. and Clotet, M. and Creevey, O. and Davidson, M. and De Ridder, J. and Delchambre, L. and Dell'Oro, A. and Ducourant, C. and Fernández-Hernández, J. and Fouesneau, M. and Fr\'emat, Y. and Galluccio, L. and García-Torres, M. and González-Núñez, J. and González-Vidal, J. J. and Gosset, E. and Guy, L. P. and Halbwachs, J.-L. and Hambly, N. C. and Harrison, D. L. and Hernández, J. and Hestroffer, D. and Hodgkin, S. T. and Hutton, A. and Jasniewicz, G. and Jean-Antoine-Piccolo, A. and Jordan, S. and Korn, A. J. and Krone-Martins, A. and Lanzafame, A. C. and Lebzelter, T. and L\"offler, W. and Manteiga, M. and Marrese, P. M. and Martín-Fleitas, J. 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	month = aug,
	year = {2018},
	keywords = {asteroids: general, astrometry, catalogs, minor planets, stars: fundamental parameters, stars: variables: general, techniques: radial velocities},
	pages = {A1},
	file = {Full Text PDF:/Users/luke/Zotero/storage/NDSX7M3W/Gaia Collaboration et al. - 2018 - Gaia Data Release 2. Summary of the contents and s.pdf:application/pdf}
}


@article{carrasco_gaia_2016,
	title = {Gaia {Data} {Release} 1. {Principles} of the photometric calibration of the {G} band},
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	url = {https://ui.adsabs.harvard.edu//#abs/2016A&A...595A...7C/abstract},
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}


@Article{perez_2007,
  Author    = {P\'erez, Fernando and Granger, Brian E.},
  Title     = {{IP}ython: a System for Interactive Scientific Computing},
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  year      = 2007,
  url       = "http://ipython.org",
  ISSN      = "1521-9615",
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}

@misc{jones_scipy_2001,
	title={Open {source} {scientific} {tools} for {Python}},
	author={Jones, Eric and Oliphant, Travis and Peterson, P and others},
	year={2001},
	publisher={Scipy}
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@article{hunter_matplotlib_2007,
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@article{walt_numpy_2011,
	title = {The {NumPy} {Array}: {A} {Structure} for {Efficient} {Numerical} {Computation}},
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@InProceedings{ mckinney-proc-scipy-2010, 
    author    = { Wes McKinney }, 
    title     = { Data Structures for Statistical Computing in Python }, 
    booktitle = { Proceedings of the 9th Python in Science Conference }, 
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    editor    = { St\'efan van der Walt and Jarrod Millman } 
} 


@article{the_astropy_collaboration_astropy_2018,
	title = {The {Astropy} {Project}: {Building} an inclusive, open-science project and status of the v2.0 core package},
	shorttitle = {The {Astropy} {Project}},
	url = {http://arxiv.org/abs/1801.02634},
	abstract = {The Astropy project supports and fosters the development of open-source and openly-developed Python packages that provide commonly-needed functionality to the astronomical community. A key element of the Astropy project is the core package Astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of inter-operable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy project.},
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	journal = {arXiv:1801.02634 [astro-ph]},
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	month = jan,
	year = {2018},
	note = {arXiv: 1801.02634},
	keywords = {Astrophysics - Instrumentation and Methods for Astrophysics},
	annote = {Comment: Minor changes to author list and title. Comments and feedback welcome through the paper source repository: https://github.com/astropy/astropy-v2.0-paper For more information about Astropy, see http://www.astropy.org/},
	file = {arXiv\:1801.02634 PDF:/home/luke/local/Zotero/storage/FKLNPK5F/The Astropy Collaboration et al. - 2018 - The Astropy Project Building an inclusive, open-s.pdf:application/pdf;arXiv.org Snapshot:/home/luke/local/Zotero/storage/E4EYVZHN/1801.html:text/html}
}



@article{corner_2016,
    Author = {Daniel Foreman-Mackey},
    Doi = {10.21105/joss.00024},
    Title = {corner.py: Scatterplot matrices in Python},
    Journal = {The Journal of Open Source Software},
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    Volume = 24,
    Url = {http://dx.doi.org/10.5281/zenodo.45906}
}

@article{foreman-mackey_emcee_2013,
	title = {emcee: {The} {MCMC} {Hammer}},
	volume = {125},
	issn = {0004-6280},
	shorttitle = {emcee},
	url = {http://adsabs.harvard.edu/abs/2013PASP..125..306F},
	doi = {10.1086/670067},
	abstract = {We introduce a stable, well tested Python implementation of the affine-invariant ensemble sampler for Markov chain Monte Carlo (MCMC) proposed by Goodman \& Weare (2010). The code is open source and has already been used in several published projects in the astrophysics literature. The algorithm behind emcee has several advantages over traditional MCMC sampling methods and it has excellent performance as measured by the autocorrelation time (or function calls per independent sample). One major advantage of the algorithm is that it requires hand-tuning of only 1 or 2 parameters compared to ˜N2 for a traditional algorithm in an N-dimensional parameter space. In this document, we describe the algorithm and the details of our
implementation. Exploiting the parallelism of the ensemble method, emcee permits any user to take advantage of multiple CPU cores without extra effort. The code is available online at http://dan.iel.fm/emcee under the GNU General Public License v2.},
	urldate = {2018-09-10},
	journal = {Publications of the Astronomical Society of the Pacific},
	author = {Foreman-Mackey, Daniel and Hogg, David W. and Lang, Dustin and Goodman, Jonathan},
	month = mar,
	year = {2013},
	pages = {306}
}

@article{goodman_ensemble_2010,
	title = {Ensemble samplers with affine invariance},
	volume = {5},
	issn = {2157-5452, 1559-3940},
	url = {http://msp.org/camcos/2010/5-1/p04.xhtml},
	doi = {10.2140/camcos.2010.5.65},
	language = {en},
	number = {1},
	urldate = {2018-11-12},
	journal = {Communications in Applied Mathematics and Computational Science},
	author = {Goodman, Jonathan and Weare, Jonathan},
	month = jan,
	year = {2010},
	pages = {65--80},
	file = {Full Text:/Users/luke/Zotero/storage/78YPERD7/Goodman and Weare - 2010 - Ensemble samplers with affine invariance.pdf:application/pdf}
}

@article{kreidberg_batman_2015,
	title = {batman: {BAsic} {Transit} {Model} {cAlculatioN} in {Python}},
	volume = {127},
	issn = {1538-3873},
	shorttitle = {batman},
	url = {http://iopscience.iop.org/article/10.1086/683602/meta},
	doi = {10.1086/683602},
	language = {en},
	number = {957},
	urldate = {2017-05-06},
	journal = {Publications of the Astronomical Society of the Pacific},
	author = {Kreidberg, Laura},
	month = nov,
	year = {2015},
	pages = {1161},
	file = {Full Text PDF:/Users/luke/Zotero/storage/B9CVHGCX/Kreidberg - 2015 - batman BAsic Transit Model cAlculatioN in Python.pdf:application/pdf;Snapshot:/Users/luke/Zotero/storage/53TR46DT/683602.html:text/html}
}

@article{mandel_analytic_2002,
	title = {Analytic {Lightcurves} for {Planetary} {Transit} {Searches}},
	volume = {580},
	issn = {0004637X, 15384357},
	url = {http://arxiv.org/abs/astro-ph/0210099},
	doi = {10.1086/345520},
	abstract = {We present exact analytic formulae for the eclipse of a star described by quadratic or nonlinear limb darkening. In the limit that the planet radius is less than a tenth of the stellar radius, we show that the exact lightcurve can be well approximated by assuming the region of the star blocked by the planet has constant surface brightness. We apply these results to the HST observations of HD 209458, showing that the ratio of the planetary to stellar radii is 0.1207+-0.0003. These formulae give a fast and accurate means of computing lightcurves using limb-darkening coefficients from model atmospheres which should aid in the detection, simulation, and parameter fitting of planetary transits.},
	number = {2},
	urldate = {2016-07-20},
	journal = {The Astrophysical Journal},
	author = {Mandel, Kaisey and Agol, Eric},
	month = dec,
	year = {2002},
	note = {arXiv: astro-ph/0210099},
	keywords = {Astrophysics},
	pages = {L171--L175},
	annote = {Comment: 4 pages, 2 figures, emulateapj, accepted for publication in ApJ Letters, subroutines available at http://www.pha.jhu.edu/{\textasciitilde}agol},
	file = {arXiv\:astro-ph/0210099 PDF:/Users/luke/Zotero/storage/895U7XDP/Mandel and Agol - 2002 - Analytic Lightcurves for Planetary Transit Searche.pdf:application/pdf;arXiv.org Snapshot:/Users/luke/Zotero/storage/DV8JJ42V/0210099.html:text/html}
}




@misc{astroquery_2018,
	title = {Astropy/{Astroquery}: {V}0.3.7 {Release}},
	shorttitle = {Astropy/{Astroquery}},
	url = {https://zenodo.org/record/1160627},
	abstract = {Functions and classes to access online data resources. Maintainer: @keflavich and @bsipocz},
	urldate = {2018-11-27},
	publisher = {Zenodo},
	author = {Ginsburg, Adam and Sipocz, Brigitta and {Madhura Parikh} and Woillez, Julien and Groener, Austen and Liedtke, Simon and Robitaille, Thomas and Deil, Christoph and {Jcsegovia} and Norman, Henrik and Svoboda, Brian and {C. E. Brasseur} and Tollerud, Erik and Persson, Magnus Vilhelm and {Adamginsburg} and S\'eguin-Charbonneau, Loïc and Armstrong, Caden and Val-Borro, Miguel De and Morris, Brett M. and Mirocha, Jordan and {Ayush Yadav} and Seifert, Michael and Droettboom, Michael and Moolekamp, Fred and {James-Allen} and {Azalee Bostroem} and Egeland, Ricky and Singer, Leo and Rol, Evert and Grollier, Fr\'ed\'eric},
	month = jan,
	year = {2018},
	doi = {10.5281/zenodo.1160627}
}

@article{claret_limb_2017,
	title = {Limb and gravity-darkening coefficients for the {TESS} satellite at several metallicities, surface gravities, and microturbulent velocities},
	volume = {600},
	issn = {0004-6361, 1432-0746},
	url = {http://arxiv.org/abs/1804.10295},
	doi = {10.1051/0004-6361/201629705},
	abstract = {We present new gravity and limb-darkening coefficients for a wide range of effective temperatures, gravities, metallicities, and microturbulent velocities. These coefficients can be used in many different fields of stellar physics as synthetic light curves of eclipsing binaries and planetary transits, stellar diameters, line profiles in rotating stars, and others. The limb-darkening coefficients were computed specifically for the photometric system of the space mission TESS and were performed by adopting the least-square method. In addition, the linear and bi-parametric coefficients, by adopting the flux conservation method, are also available. On the other hand, to take into account the effects of tidal and rotational distortions, we computed the passband gravity-darkening coefficients \$y({\textbackslash}lambda)\$ using a general differential equation in which we consider the effects of convection and of the partial derivative \${\textbackslash}left({\textbackslash}partial\{{\textbackslash}ln I({\textbackslash}lambda)\}/\{{\textbackslash}partial\{{\textbackslash}ln g\}\}{\textbackslash}right)\_\{T\_\{{\textbackslash}rm eff\}\}\$. To generate the limb-darkening coefficients we adopt two stellar atmosphere models: ATLAS (plane-parallel) and PHOENIX (spherical, quasi-spherical, and \$r\$-method). The specific intensity distribution was fitted using five approaches: linear, quadratic, square root, logarithmic, and a more general one with four terms. These grids cover together 19 metallicities ranging from 10\${\textasciicircum}\{-5\}\$ up to 10\${\textasciicircum}\{+1\}\$ solar abundances, 0 \${\textbackslash}leq\$ log g \${\textbackslash}leq\$ 6.0 and 1500 K \${\textbackslash}leq\$ T\$\_\{{\textbackslash}rm eff\}\$ \${\textbackslash}leq\$ 50000 K. The calculations of the gravity-darkening coefficients were performed for all plane-parallel ATLAS models.},
	urldate = {2018-09-12},
	journal = {Astronomy \& Astrophysics},
	author = {Claret, Antonio},
	month = apr,
	year = {2017},
	note = {arXiv: 1804.10295},
	keywords = {Astrophysics - Solar and Stellar Astrophysics},
	pages = {A30}
}

@article{kovacs_box-fitting_2002,
	title = {A box-fitting algorithm in the search for periodic transits},
	volume = {391},
	url = {https://ui.adsabs.harvard.edu//#abs/2002A&A...391..369K/abstract},
	doi = {10.1051/0004-6361:20020802},
	abstract = {We study the statistical characteristics of a box-fitting algorithm to analyze stellar photometric time series in the search for periodic transits by extrasolar planets. The algorithm searches for signals characterized by a periodic alternation between two discrete levels, with much less time spent at the lower level. We present numerical as well as analytical results to predict the possible detection significance at various signal parameters. It is shown that the crucial parameter is the effective signal-to-noise ratio - the expected depth of the transit divided by the standard deviation of the measured photometric average within the transit. When this parameter exceeds the value of 6 we can expect a significant detection of the transit. We show that the box-fitting algorithm performs better than other methods available in the astronomical literature, especially for low signal-to-noise ratios.},
	language = {en},
	urldate = {2018-11-10},
	journal = {Astronomy and Astrophysics},
	author = {Kov\'acs, G. and Zucker, S. and Mazeh, T.},
	month = aug,
	year = {2002},
	pages = {369},
	file = {Full Text PDF:/Users/luke/Zotero/storage/TW7Z6XCJ/Kovács et al. - 2002 - A box-fitting algorithm in the search for periodic.pdf:application/pdf;Snapshot:/Users/luke/Zotero/storage/4JPVTP83/ui.adsabs.harvard.edu.html:text/html}
}


@article{miller_optimal_2008,
	title = {Optimal {Image} {Subtraction} {Method}: {Summary} {Derivations}, {Applications}, and {Publicly} {Shared} {Application} {Using} {IDL}},
	volume = {120},
	issn = {0004-6280},
	shorttitle = {Optimal {Image} {Subtraction} {Method}},
	url = {http://adsabs.harvard.edu/abs/2008PASP..120..449M},
	doi = {10.1086/588258},
	abstract = {To detect objects that vary in brightness or spatial coordinates over 
time, C. Alard and R. H. Lupton in 1998 proposed an “optimal image
subtraction” (OIS) method that constructs a convolution kernel
from a set of matching stars distributed across the two images to be
subtracted. Using multivariable least squares, the kernel is derived and
can be designed to vary by pixel coordinates across the convolved image.
Local effects in the optics, including aberrations or other spatially
sensitive perturbations to a perfect image, can be mitigated. This paper
presents the specific systems of equations that originate from the OIS
method. Also included is a complete description of the Gaussian
components basis vectors used by Alard \& Lupton to construct the
convolution kernel. An alternative set of basis vectors, called the
delta function basis, is also described. Important issues are addressed,
including the selection of the matching stars, differential background
correction, constant photometric flux, contaminated pixel masking, and
alignment at the subpixel level. Computer algorithms for the OIS method
were developed, written using the Interactive Data Language (IDL), and
applications demonstrating these algorithms are presented.},
	urldate = {2018-03-07},
	journal = {Publications of the Astronomical Society of the Pacific},
	author = {Miller, J. Patrick and Pennypacker, C. R. and White, Graeme L.},
	month = apr,
	year = {2008},
	pages = {449}
}

@article{pal_astrometry_2006,
	title = {Astrometry in {Wide}-{Field} {Surveys}},
	volume = {118},
	url = {https://ui.adsabs.harvard.edu//#abs/2006PASP..118.1474P/abstract},
	doi = {10.1086/508573},
	abstract = {We present a robust and fast algorithm for performing astrometry and source cross-identification on lists of two-dimensional points, such as between a catalog and an astronomical image, or between two images. The method is based on minimal assumptions: the lists can be rotated, magnified, and inverted with respect to each other in an arbitrary way. The algorithm is tailored to work efficiently on wide fields with a large number of sources and significant nonlinear distortions, as long as the distortions can be approximated with linear transformations locally over the scale length of the average distance between the points. The procedure is based on symmetric point matching in a newly defined continuous triangle space that consists of triangles generated by extended Delaunay triangulation. Our software implementation performed at the 99.995\% success rate on {\textasciitilde}260,000 frames taken by the HATNet project.},
	language = {en},
	number = {848},
	urldate = {2018-12-16},
	journal = {Publications of the Astronomical Society of the Pacific},
	author = {P\'al, Andr\'as and Bakos, G\'asp\'ar \'A},
	month = oct,
	year = {2006},
	pages = {1474},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/F94L46KE/Pál and Bakos - 2006 - Astrometry in Wide-Field Surveys.pdf:application/pdf;Snapshot:/home/luke/local/Zotero/storage/ZRVGLPX3/ui.adsabs.harvard.edu.html:text/html}
}

@article{oelkers_precision_2018,
	title = {Precision {Light} {Curves} from {TESS} {Full}-frame {Images}: {A} {Different} {Imaging} {Approach}},
	volume = {156},
	issn = {1538-3881},
	shorttitle = {Precision {Light} {Curves} from {TESS} {Full}-frame {Images}},
	url = {http://stacks.iop.org/1538-3881/156/i=3/a=132},
	doi = {10.3847/1538-3881/aad68e},
	abstract = {The Transiting Exoplanet Survey Satellite ( TESS ) will observe ∼150 million stars brighter than \#\#IMG\#\# [http://ej.iop.org/images/1538-3881/156/3/132/ajaad68eieqn1.gif] \$T\_{\textbackslash}mathrmmag{\textbackslash}approx 16\$ , with photometric precision from 60 ppm to 3\%, enabling an array of exoplanet and stellar astrophysics investigations. While light curves will be provided for ∼400,000 targets observed at 2 minute cadence, observations of most stars will only be provided as full-frame images (FFIs) at 30 minute cadence. The TESS image scale of ∼21″/pix is highly susceptible to crowding, blending, and source confusion, and the highly spatially variable point-spread function (PSF) will challenge traditional techniques, such as aperture and Gaussian-kernel PSF photometry. We use official “End-to-End 6” TESS simulated FFIs to demonstrate a difference image analysis pipeline, using a δ -function kernel, that achieves the mission specification noise floor of 60 ppm hr −1/2 . We show that the pipeline performance does not depend on position across the field, and only ∼2\% of stars appear to exhibit residual systematics at the level of ∼5 ppt. We also demonstrate recoverability of planet transits, eclipsing binaries, and other variables. We provide the pipeline as an open-source tool at https://github.com/ryanoelkers/DIA [http://https://github.com/ryanoelkers/DIA] in both IDL and PYTHON. We intend to extract light curves for all point sources in the TESS FFIs as soon as they become publicly available, and will provide the light curves through the Filtergraph data visualization service. An example data portal based on the simulated FFIs is available for inspection at https://filtergraph.com/tess\_ffi [http://https://filtergraph.com/tess\_ffi] .},
	language = {en},
	number = {3},
	urldate = {2018-09-05},
	journal = {The Astronomical Journal},
	author = {Oelkers, Ryan J. and Stassun, Keivan G.},
	year = {2018},
	pages = {132}
}

@article{soares-furtado_image_2017,
	title = {Image {Subtraction} {Reduction} of {Open} {Clusters} {M}35 \& {NGC} 2158 in the {K}2 {Campaign} 0 {Super} {Stamps}},
	volume = {129},
	issn = {0004-6280},
	url = {http://adsabs.harvard.edu/abs/2017PASP..129d4501S},
	doi = {10.1088/1538-3873/aa5c7c},
	abstract = {We observed the open clusters M35 and NGC 2158 during the initial K2 
campaign (C0). Reducing these data to high-precision photometric
timeseries is challenging due to the wide point-spread function (PSF)
and the blending of stellar light in such dense regions. We developed an
image-subtraction-based K2 reduction pipeline that is applicable to both
crowded and sparse stellar fields. We applied our pipeline to the
data-rich C0 K2 super stamp, containing the two open clusters, as well
as to the neighboring postage stamps. In this paper, we present our
image subtraction reduction pipeline and demonstrate that this technique
achieves ultra-high photometric precision for sources in the C0 super
stamp. We extract the raw light curves of 3960 stars taken from the
UCAC4 and EPIC catalogs and de-trend them for systematic effects. We
compare our photometric results with the prior reductions published in
the literature. For de-trended TFA-corrected sources in the
12-12.25 \{\{\{K\}\}\}\{\{p\}\} magnitude range, we achieve a
best 6.5-hour window running rms of 35 ppm, falling to 100 ppm for
fainter stars in the 14-14.25 \{\{\{K\}\}\}\{\{p\}\} magnitude
range. For stars with \{K\}p{\textgreater} 14, our de-trended and
6.5-hour binned light curves achieve the highest photometric precision.
Moreover, all our TFA-corrected sources have higher precision on all
timescales investigated. This work represents the first published image
subtraction analysis of a K2 super stamp. This method will be
particularly useful for analyzing the Galactic bulge observations
carried out during K2 campaign 9. The raw light curves and the final
results of our de-trending processes are publicly available at http://k2.hatsurveys.org/archive/.},
	urldate = {2017-09-13},
	journal = {Publications of the Astronomical Society of the Pacific},
	author = {Soares-Furtado, M. and Hartman, J. D. and Bakos, G. Á. and Huang, C. X. and Penev, K. and Bhatti, W.},
	month = apr,
	year = {2017},
	pages = {044501},
	file = {NASA/ADS Full Text PDF:/home/luke/local/Zotero/storage/CUGE9HBT/Soares-Furtado et al. - 2017 - Image Subtraction Reduction of Open Clusters M35 &.pdf:application/pdf}
}

@article{pence_fits_2010,
	title = {Definition of the {Flexible} {Image} {Transport} {System} ({FITS}), version 3.0},
	volume = {524},
	url = {https://ui.adsabs.harvard.edu//#abs/2010A&A...524A..42P/abstract},
	doi = {10.1051/0004-6361/201015362},
	abstract = {The Flexible Image Transport System (FITS) has been used by astronomers for over 30 years as a data interchange and archiving format; FITS files are now handled by a wide range of astronomical software packages. Since the FITS format definition document (the “standard”) was last printed in this journal in 2001, several new features have been developed and standardized, notably support for 64-bit integers in images and tables, variable-length arrays in tables, and new world coordinate system conventions which provide a mapping from an element in a data array to a physical coordinate on the sky or within a spectrum. The FITS Working Group of the International Astronomical Union has therefore produced this new version 3.0 of the FITS standard, which is provided here in its entirety. In addition to describing the new features in FITS, numerous editorial changes were made to the previous version to clarify and reorganize many of the sections. Also included are some appendices which are not formally part of the standard. The FITS standard is likely to undergo further evolution, in which case the latest version may be found on the FITS Support Office Web site at \&lt;ext-link ext-link-type="uri" xlink:href="http://fits.gsfc.nasa.gov/"\&gt;http://fits.gsfc.nasa.gov/\&lt;/ext-link\&gt;, which also provides many links to FITS-related resources.},
	language = {en},
	urldate = {2019-01-11},
	journal = {Astronomy and Astrophysics},
	author = {Pence, W. D. and Chiappetti, L. and Page, C. G. and Shaw, R. A. and Stobie, E.},
	month = dec,
	year = {2010},
	pages = {A42}
}

@article{lang_2010,
	title = {Astrometry.net: {Blind} {Astrometric} {Calibration} of {Arbitrary} {Astronomical} {Images}},
	volume = {139},
	shorttitle = {Astrometry.net},
	url = {https://ui.adsabs.harvard.edu//#abs/2010AJ....139.1782L/abstract},
	doi = {10.1088/0004-6256/139/5/1782},
	abstract = {We have built a reliable and robust system that takes as input an astronomical image, and returns as output the pointing, scale, and orientation of that image (the astrometric calibration or World Coordinate System information). The system requires no first guess, and works with the information in the image pixels alone; that is, the problem is a generalization of the "lost in space" problem in which nothing—not even the image scale—is known. After robust source detection is performed in the input image, asterisms (sets of four or five stars) are geometrically hashed and compared to pre-indexed hashes to generate hypotheses about the astrometric calibration. A hypothesis is only accepted as true if it passes a Bayesian decision theory test against a null hypothesis. With indices built from the USNO-B catalog and designed for uniformity of coverage and redundancy, the success rate is \&gt;99.9\% for contemporary near-ultraviolet and visual imaging survey data, with no false positives. The failure rate is consistent with the incompleteness of the USNO-B catalog; augmentation with indices built from the Two Micron All Sky Survey catalog brings the completeness to 100\% with no false positives. We are using this system to generate consistent and standards-compliant meta-data for digital and digitized imaging from plate repositories, automated observatories, individual scientific investigators, and hobbyists. This is the first step in a program of making it possible to trust calibration meta-data for astronomical data of arbitrary provenance.},
	language = {en},
	number = {5},
	urldate = {2019-01-11},
	journal = {The Astronomical Journal},
	author = {Lang, Dustin and Hogg, David W. and Mierle, Keir and Blanton, Michael and Roweis, Sam},
	month = may,
	year = {2010},
	pages = {1782},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/ENZCYYGE/Lang et al. - 2010 - Astrometry.net Blind Astrometric Calibration of A.pdf:application/pdf;Snapshot:/home/luke/local/Zotero/storage/KWDWVJN9/ui.adsabs.harvard.edu.html:text/html}
}

@misc{tess_data_product_description_2018,
author = {Tenenbaum, P. and Jenkins, J.},
year = {2018},
title = {TESS Science Data Products Description Document},
howpublished= {EXP-TESS-ARC-ICD-0014 Rev D,
  \url{https://archive.stsci.edu/missions/tess/doc/EXP-TESS-ARC-ICD-TM-0014.pdf}}
}

@misc{ricker_tess_alerts_2018,
author = {Ricker, George and Vanderspek, Roland},
year = {2018},
title = {Data Products From TESS Data Alerts},
doi = {10.17909/t9-wx1n-aw08},
howpublished= {\url{https://archive.stsci.edu/prepds/tess-data-alerts/index.html}} 
}


@article{vanderspek_2018,
	title = {{TESS} {Instrument} {Handbook}},
	url = {archive.stsci.edu/missions/tess/doc/TESS_Instrument_Handbook_v0.1.pdf},
	language = {en},
	urldate = {2018-01-11},
	journal = {TESS Science Document},
	author = {Vanderspek, Roland and Doty, John and Fausnaugh, Michael and others},
	month = dec,
	year = {2018},
	pages = {73}
}


@article{clarke_kepler_2017,
	title = {Kepler {Data} {Processing} {Handbook}: {Pixel} {Level} {Calibrations}},
	shorttitle = {Kepler {Data} {Processing} {Handbook}},
	url = {https://ui.adsabs.harvard.edu//#abs/2017ksci.rept....5C/abstract},
	abstract = {A powerful, streamlined new Astrophysics Data System},
	language = {en},
	urldate = {2018-11-24},
	journal = {Kepler Science Document},
	author = {Clarke, Bruce D. and Caldwell, Douglas A. and Quintana, Elisa V. and Chandrasekaran, Hema and Twicken, Joseph D. and Jenkins, Jon M. and Cote, Miles T. and McCauliff, Sean D. and Klaus, Todd C. and Allen, Christopher and Bryson, Stephen T.},
	month = jan,
	year = {2017},
	pages = {5},
	file = {Full Text PDF:/home/luke/local/Zotero/storage/5QYY9KBW/Clarke et al. - 2017 - Kepler Data Processing Handbook Pixel Level Calib.pdf:application/pdf;Snapshot:/home/luke/local/Zotero/storage/4KXTTPIW/ui.adsabs.harvard.edu.html:text/html}
}


@article{ricker_transiting_2015,
	title = {Transiting {Exoplanet} {Survey} {Satellite} ({TESS})},
	volume = {1},
	url = {https://ui.adsabs.harvard.edu//#abs/2015JATIS...1a4003R/abstract},
	doi = {10.1117/1.JATIS.1.1.014003},
	abstract = {The Transiting Exoplanet Survey Satellite (TESS) will search for planets transiting bright and nearby stars. TESS has been selected by NASA for launch in 2017 as an Astrophysics Explorer mission. The spacecraft will be placed into a highly elliptical 13.7-day orbit around the Earth. During its 2-year mission, TESS will employ four wide-field optical charge-coupled device cameras to monitor at least 200,000 main-sequence dwarf stars with I{\textless}SUB{\textgreater}C{\textless}/SUB{\textgreater}≈4-13 for temporary drops in brightness caused by planetary transits. Each star will be observed for an interval ranging from 1 month to 1 year, depending mainly on the star's ecliptic latitude. The longest observing intervals will be for stars near the ecliptic poles, which are the optimal locations for follow-up observations with the James Webb Space Telescope. Brightness measurements of preselected target stars will be recorded every 2 min, and full frame images will be recorded every 30 min. TESS stars will be 10 to 100 times brighter than those surveyed by the pioneering Kepler mission. This will make TESS planets easier to characterize with follow-up observations. TESS is expected to find more than a thousand planets smaller than Neptune, including dozens that are comparable in size to the Earth. Public data releases will occur every 4 months, inviting immediate community-wide efforts to study the new planets. The TESS legacy will be a catalog of the nearest and brightest stars hosting transiting planets, which will endure as highly favorable targets for detailed investigations.},
	language = {en},
	urldate = {2018-11-29},
	journal = {Journal of Astronomical Telescopes, Instruments, and Systems},
	author = {Ricker, George R. and Winn, Joshua N. and Vanderspek, Roland and Latham, David W. and Bakos, Gáspár Á and Bean, Jacob L. and Berta-Thompson, Zachory K. and Brown, Timothy M. and Buchhave, Lars and Butler, Nathaniel R. and Butler, R. Paul and Chaplin, William J. and Charbonneau, David and Christensen-Dalsgaard, Jørgen and Clampin, Mark and Deming, Drake and Doty, John and De Lee, Nathan and Dressing, Courtney and Dunham, Edward W. and Endl, Michael and Fressin, Francois and Ge, Jian and Henning, Thomas and Holman, Matthew J. and Howard, Andrew W. and Ida, Shigeru and Jenkins, Jon M. and Jernigan, Garrett and Johnson, John Asher and Kaltenegger, Lisa and Kawai, Nobuyuki and Kjeldsen, Hans and Laughlin, Gregory and Levine, Alan M. and Lin, Douglas and Lissauer, Jack J. and MacQueen, Phillip and Marcy, Geoffrey and McCullough, Peter R. and Morton, Timothy D. and Narita, Norio and Paegert, Martin and Palle, Enric and Pepe, Francesco and Pepper, Joshua and Quirrenbach, Andreas and Rinehart, Stephen A. and Sasselov, Dimitar and Sato, Bun'ei and Seager, Sara and Sozzetti, Alessandro and Stassun, Keivan G. and Sullivan, Peter and Szentgyorgyi, Andrew and Torres, Guillermo and Udry, Stephane and Villasenor, Joel},
	month = jan,
	year = {2015},
	pages = {014003},
	file = {Snapshot:/Users/luke/Zotero/storage/Y6L92CPU/ui.adsabs.harvard.edu.html:text/html}
}


@article{bakos_2010,
	title = {{HAT}-{P}-11b: {A} {Super}-{Neptune} {Planet} {Transiting} a {Bright} {K} {Star} in the {Kepler} {Field}},
	volume = {710},
	issn = {0004-637X},
	shorttitle = {{HAT}-{P}-11b},
	url = {http://adsabs.harvard.edu/abs/2010ApJ...710.1724B},
	doi = {10.1088/0004-637X/710/2/1724},
	urldate = {2017-09-14},
	journal = {The Astrophysical Journal},
	author = {Bakos, G. \'A. and Torres, G. and P\'al, A. and Hartman, J. and Kovács, G\'eza and Noyes, R. W. and Latham, D. W. and Sasselov, D. D. and Sipőcz, B. and Esquerdo, G. A. and Fischer, D. A. and Johnson, J. A. and Marcy, G. W. and Butler, R. P. and Isaacson, H. and Howard, A. and Vogt, S. and Kovács, Gábor and Fernandez, J. and Moór, A. and Stefanik, R. P. and Lázár, J. and Papp, I. and Sári, P.},
	month = feb,
	year = {2010},
	keywords = {techniques: photometric, planetary systems, stars: individual: HAT-P-11 GSC 03561-02092, techniques: spectroscopic},
	pages = {1724--1745},
	file = {NASA/ADS Full Text PDF:/home/luke/local/Zotero/storage/EZYA4VW2/Bakos et al. - 2010 - HAT-P-11b A Super-Neptune Planet Transiting a Bri.pdf:application/pdf}
}

@article{kovacs_trend_2005,
	title = {A trend filtering algorithm for wide-field variability surveys},
	volume = {356},
	issn = {0035-8711, 1365-2966},
	url = {http://mnras.oxfordjournals.org/content/356/2/557},
	doi = {10.1111/j.1365-2966.2004.08479.x},
	abstract = {We show that various systematics related to certain instrumental effects and data reduction anomalies in wide-field variability surveys can be efficiently corrected by a trend filtering algorithm (TFA) applied to the photometric time-series produced by standard data pipelines. Statistical tests, performed on the data base of the HAT Network project, show that by the application of this filtering method the cumulative detection probability of periodic transits increases by up to 0.4 for variables brighter than 11 mag, with a trend of increasing efficiency toward brighter magnitudes. We also show that the TFA can be used for the reconstruction of periodic signals by iteratively filtering out systematic distortions.},
	language = {en},
	number = {2},
	urldate = {2016-09-06},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Kov\'acs, G\'eza and Bakos, Gáspár and Noyes, Robert W.},
	month = jan,
	year = {2005},
	keywords = {surveys, planetary systems, stars: variables: other, METHODS: DATA ANALYSIS},
	pages = {557--567}
}

@article{David_et_al_2017,
	title = {A Neptune-sized transiting planet closely orbiting a 5-10 million year old star},
	volume = {534},
	journal = {Nature},
	author = {David, T. and Hillenbrand, L. and Petigura, E.},
	month = jun,
	year = {2016},
	pages = {658}
}

@article{Kharchenko_et_al_2013,
	title = {Global survey of star clusters in the {Milky} {Way}. 
	{II}. {The} catalogue of basic parameters},
	volume = {558},
	journal = {Astronomy and Astrophysics},
	author = {Kharchenko, N. V. and Piskunov, A. E. and Schilbach, 
	E. and R\"oser, S. and Scholz, R.-D.},
	month = oct,
	year = {2013},
	pages = {A53}
}


@article{kharchenko_global_2012,
	title = {Global survey of star clusters in the {Milky} {Way}. {I}. {The} pipeline and fundamental parameters in the second quadrant},
	volume = {543},
	issn = {0004-6361},
	url = {http://adsabs.harvard.edu/abs/2012A%26A...543A.156K},
	doi = {10.1051/0004-6361/201118708},
	urldate = {2017-09-10},
	journal = {Astronomy and Astrophysics},
	author = {Kharchenko, N. V. and Piskunov, A. E. and Schilbach, E. and R\"oser, S. and Scholz, R.-D.},
	month = jul,
	year = {2012},
	keywords = {open clusters and associations: general, catalogs, globular clusters: general},
	pages = {A156}
}

@article{Bouma_et_al_2017,
    title = {Planet {Detection} {Simulations} for {Several} 
    {Possible} {TESS} {Extended} {Missions}},
    journal = {arXiv:1705.08891},
    author = {Bouma, L. G. and Winn, Joshua N. and Kosiarek, Jacobi 
    and McCullough, P. R.},
    month = may,
    year = {2017}
}

@article{Sullivan_et_al_2015,
    title = {{THE} {TRANSITING} {EXOPLANET} {SURVEY} {SATELLITE}: 
    {SIMULATIONS} {OF} {PLANET} {DETECTIONS} {AND} {ASTROPHYSICAL} {FALSE} 
    {POSITIVES}},
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@phdthesis{Pal_2009,
	title = {Tools for discovering and characterizing extrasolar planets},
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	abstract = {Among the group of extrasolar planets, transiting planets provide a great opportunity to obtain direct measurements for the basic physical properties, such as mass and radius of these objects. These planets are therefore highly important in the understanding of the evolution and formation of planetary systems: from the observations of photometric transits, the interior structure of the planet and atmospheric properties can also be constrained. The most efficient way to search for transiting extrasolar planets is based on wide-field surveys by hunting for short and shallow periodic dips in light curves covering quite long time intervals. These surveys monitor fields with several degrees in diameter and tens or hundreds of thousands of objects simultaneously. In the practice of astronomical observations, surveys of large field-of-view are rather new and therefore require special methods for photometric data reduction that have not been used before. In this PhD thesis, I summarize my efforts related to the development of a complete software solution for high precision photometric reduction of astronomical images. I also demonstrate the role of this newly developed package and the related algorithms in the case of particular discoveries of the HATNet project. [abridged]},
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	author = {P\'al, Andr\'as},
	month = jun,
	year = {2009},
	note = {arXiv: 0906.3486},
	keywords = {Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics},
	annote = {Comment: PhD thesis, Eotvos Lorand University (June 18, 2009), 68 pages in journal style, 41 figures, 18 tables},
	file = {arXiv\:0906.3486 PDF:/Users/luke/Zotero/storage/9UZSMDK8/Pál - 2009 - Tools for discovering and characterizing extrasola.pdf:application/pdf;arXiv.org Snapshot:/Users/luke/Zotero/storage/G7KU6CKD/Pál - 2009 - Tools for discovering and characterizing extrasola.html:text/html}
}


@article{Pal_2012,
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