Trumpeting M dwarfs with CONCH-SHELL: a catalogue of nearby cool host-stars for habitable exoplanets and life

By E. Gaidos, A. Mann, S. Lépine, A. Buccino, David J. James, M. Ansdell, R. Petrucci, P. Mauas, E. Hilton. 2014

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We present an all-sky catalog of 2970 nearby (d . 50 pc), bright (J < 9) M- or late Ktype dwarf stars, 86% of which have been confirmed by spectroscopy. This catalog will be useful for searches for Earth-size and possibly Earth-like planets by future spacebased transit missions and ground-based infrared Doppler radial velocity surveys. Stars were selected from the SUPERBLINK proper motion catalog according to absolute magnitudes, spectra, or a combination of reduced proper motions and photometric colors. From our spectra we determined gravity-sensitive indices, and identified and removed 0.2% of these as interloping hotter or evolved stars. Thirteen percent of the stars exhibit Hα emission, an indication of stellar magnetic activity and possible youth. The mean metallicity is [Fe/H] = -0.07 with a standard deviation of 0.22 dex, similar to nearby solar-type stars. We determined stellar effective temperatures by least-squares fitting of spectra to model predictions calibrated by fits to stars with established bolometric temperatures, and estimated radii, luminosities, and masses using empirical relations. Six percent of stars with images from integral field spectra are resolved doubles. We inferred the planet population around M dwarfs using Kepler data and applied this to our catalog to predict detections by future exoplanet surveys.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

STELLAR AND PLANETARY PROPERTIES OF K2 CAMPAIGN 1 CANDIDATES AND VALIDATION OF 17 PLANETS, INCLUDING A PLANET RECEIVING EARTH-LIKE INSOLATION (2015, methodology): “More details of this procedure are given in Mann et al. (2013b) and Gaidos et al. (2014).”
They are small worlds after all: revised properties of Kepler M dwarf stars and their planets (2015, methodology): “Our estimate within one standard deviation of previous estimates by DC13, Gaidos et al. (2014), Morton & Swift (2014), and DC15.”
How to Constrain Your M Dwarf. II. The Mass–Luminosity–Metallicity Relation from 0.075 to 0.70 Solar Masses (2018, methodology): “For these targets we recalculated KS magnitudes using available optical and NIR spectra, following the method of Mann & von Braun (2015) and Mann et al. (2015), using available optical spectra from Gaidos et al. (2014).”
ZODIACAL EXOPLANETS IN TIME (ZEIT). III. A SHORT-PERIOD PLANET ORBITING A PRE-MAIN-SEQUENCE STAR IN THE UPPER SCORPIUS OB ASSOCIATION (2016, methodology): “Comparison to the Gaidos et al. (2014) templates also give significantly higher χ2ν values than to those from Herczeg & Hillenbrand (2014), likely because of gravity-dependent differences in the spectrum.”
HOW TO CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, AND RADIUS (2015, methodology): “Our part of the reduction is described in some detail in Lépine et al. (2013) and Gaidos et al. (2014).”
THE Hα EMISSION OF NEARBY M DWARFS AND ITS RELATION TO STELLAR ROTATION (2016, methodology): “For 2MASS 7 12 10 8 6 4 2 0 FAST H EW ( ) 12 10 8 6 4 2 0 Li te ra tu re H E W w / lin e a r co rr e ct io n ( ) One-to-one match Alonso-Floriano et al. (2015) Gaidos et al. (2014) Gizis et al. (2002) 0.6 0.4 0.20.0 0.2 0.4 0.6 0.4 0.2 0.0 0.2 0.4 Figure 1.”
Target Selection for the SDSS-IV APOGEE-2 Survey (2017, methodology): “These M dwarfs were drawn from multiple catalogs (e.g., Reid & Gizis 2005; Lépine & Shara 2005; Lépine & Gaidos 2011; Gaidos et al. 2014), within a magnitude range of 7 < H < 12 and with a color requirement of (V −J) > 0.”