A Catalog of Cool Dwarf Targets for the Transiting Exoplanet Survey Satellite
Philip S. Muirhead, Courtney Dressing, Andrew W. Mann, Bárbara Rojas-Ayala, Sebastien Lepine, Martin Paegert, Nathan De Lee, Ryan Oelkers
(Submitted on 30 Sep 2017)
We present a catalog of cool dwarf targets (V−J>2.7, TEff≲4000K) and their stellar properties for the upcoming Transiting Exoplanet Survey Satellite (TESS), for the purpose of determining which cool dwarfs should be observed using two-minute observations. TESS has the opportunity to search tens of thousands of nearby, cool, late K and M-type dwarfs for transiting exoplanets, an order of magnitude more than current or previous transiting exoplanet surveys, such as {\it Kepler}, K2 and ground-based programs. This necessitates a new approach to choosing cool dwarf targets. Cool dwarfs were chosen by collating parallax and proper motion catalogs from the literature and subjecting them to a variety of selection criteria. We calculate stellar parameters and TESS magnitudes using the best possible relations from the literature while maintaining uniformity of methods for the sake of reproducibility. We estimate the expected planet yield from TESS observations using statistical results from the {\it Kepler} Mission, and use these results to choose the best targets for two-minute observations, optimizing for small planets for which masses can conceivably be measured using follow up Doppler spectroscopy by current and future Doppler spectrometers. The catalog is incorporated into the TESS Input Catalog and TESS Candidate Target List until a more complete and accurate cool dwarf catalog identified by ESA’s Gaia Mission can be incorporated.
Comments: Submitted to AAS Journals
Subjects: Solar and Stellar Astrophysics (astro-ph.SR); Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:1710.00193 [astro-ph.SR] (or arXiv:1710.00193v1 [astro-ph.SR] for this version)
Submission history
From: Philip Muirhead
[v1] Sat, 30 Sep 2017 12:50:19 GMT (10646kb,D)
https://arxiv.org/abs/1710.00193
