AN ALL-SKY CATALOG OF BRIGHT M DWARFS

By S. Lépine, E. Gaidos. 2011

198 citations recorded by the source corpus.

We present an all-sky catalog of M dwarf stars with apparent infrared magnitude J < 10. The 8889 stars are selected from the ongoing SUPERBLINK survey of stars with proper motion μ > 40 mas yr−1, supplemented on the bright end with the Tycho-2 catalog. Completeness tests which account for kinematic (proper motion) bias suggest that our catalog represents ≈75% of the estimated ∼11, 900 M dwarfs with J < 10 expected to populate the entire sky. Our catalog is, however, significantly more complete for the northern sky (≈90%) than it is for the south (≈60%). Stars are identified as cool, red M dwarfs from a combination of optical and infrared color cuts, and are distinguished from background M giants and highly reddened stars using either existing parallax measurements or, if such measurements are lacking, using their location in an optical-to-infrared reduced proper motion diagram. These bright M dwarfs are all prime targets for exoplanet surveys using the Doppler radial velocity or transit methods; the combination of low-mass and bright apparent magnitude should make possible the detection of Earth-size planets on short-period orbits using currently available techniques. Parallax measurements, when available, and photometric distance estimates are provided for all stars, and these place most systems within 60 pc of the Sun. Spectral type estimated from V − J color shows that most of the stars range from K7 to M4, with only a few late M dwarfs, all within 20 pc. Proximity to the Sun also makes these stars good targets for high-resolution exoplanet imaging searches, especially if younger objects can be identified on the basis of X-ray or UV excess. For that purpose, we include X-ray flux from ROSAT and FUV/NUV ultraviolet magnitudes from GALEX for all stars for which a counterpart can be identified in those catalogs. Additional photometric data include optical magnitudes from Digitized Sky Survey plates and infrared magnitudes from the Two Micron All Sky Survey.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/bda6408102f4d471644641a79cbe41ab1e7e19dc

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Citations in the corpus

PROSPECTING IN LATE-TYPE DWARFS: A CALIBRATION OF INFRARED AND VISIBLE SPECTROSCOPIC METALLICITIES OF LATE K AND M DWARFS SPANNING 1.5 dex (2012, methodology): “This cut will remove almost all stars earlier than K5 (Lépine & Gaidos 2011) where metallicities can be measured using modified spectral synthesis techniques (Valenti & Piskunov 1996; Valenti & Fischer 2005).”
They are small worlds after all: revised properties of Kepler M dwarf stars and their planets (2015, background): “TRILEGAL predicts about 0.11 M dwarf per sq. deg. with J < 10, somewhat less than the 0.14 found by Lépine & Gaidos (2011), and too few to calculate priors for the brightest stars.”
INTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS (2013, methodology): “We fit polynomial relations to V –KS versus KS–W1, KS–W2, KS–W3, and KS–W4 for stars within 75 pc from the Hipparcos catalog and the catalog of bright M dwarfs from Lépine & Gaidos (2011).”
HOW TO CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, AND RADIUS (2015, methodology): “8 18 T h e A stro ph y sica l Jo u rn a l, 804:64 (38pp), 2015 M ay 1 M a n n et a l. Table 5 (Continued) LG11/LSPM Name CNS3 R.A. Decl.”
A self-consistent, absolute isochronal age scale for young moving groups in the solar neighbourhood (2015, methodology): “…of these studies provide associated uncertainties on the V -band magnitude, stars for which we have adopted NOMAD and SPM4 photometry, as well as photometry taken from the studies of Zuckerman & Song (2004), Barrado y Navascués (2006), Chauvin et al. (2010), and Lépine & Gaidos (2011) do not.”
HAZMAT. I. THE EVOLUTION OF FAR-UV AND NEAR-UV EMISSION FROM EARLY M STARS (2014, unknown): “…et al. (2006), 20: Bowler et al. (2012), 21: Ammler-von Eiff & Guenther (2009), 22: Perryman et al. (1998), 23: Guenther et al. (2005), 24: Lépine & Gaidos (2011), 25: Poveda et al. (1994), 26: Riedel et al. (2014), 27: Pourbaix et al. (2004). d TWA 31 and TWA 30 B are both known to be…”
A SPECTROSCOPIC CATALOG OF THE BRIGHTEST (J < 9) M DWARFS IN THE NORTHERN SKY, (2012, methodology): “In order to assemble a comprehensive database of M dwarfs targets suitable for exoplanet survey programs, we are now conducting a spectroscopic follow-up survey of the brightest M dwarf candidates from (Lépine & Gaidos 2011).”
The habitable-zone planet finder: a stabilized fiber-fed NIR spectrograph for the Hobby-Eberly Telescope (2012, background): “The figure also shows in grey dots the larger sample of star identified as M dwarfs from proper motion catalogs.(15,16)”
HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: NEW ESTIMATES (2013, methodology): “We anticipate having this information for ∼ 650 M dwarfs drawn from the J 10 Lepine & Gaidos (2011)catalog, and have applied for time to observe ∼ 300 more.”
Trumpeting M dwarfs with CONCH-SHELL: a catalogue of nearby cool host-stars for habitable exoplanets and life (2014, background): “J color rather than spectral type, and some M0 stars with blue colors, e.g. metal-poor stars, are omitted (Lépine & Gaidos 2011).”
THE METALLICITY DISTRIBUTION FUNCTIONS OF SEGUE G AND K DWARFS: CONSTRAINTS FOR DISK CHEMICAL EVOLUTION AND FORMATION (2011, methodology): “Therefore, we identified stars from our sample that were very likely to be dwarfs using a reduced proper-motion criterion (Lépine & Gaidos 2011).”
THE ASTRALUX LARGE M-DWARF MULTIPLICITY SURVEY (2012, background): “However, recently a number of efforts have been made in identifying and characterizing nearby M-dwarfs (e.g., Riaz et al. 2006; Reid et al. 2007; Lépine & Gaidos 2011), which has mitigated this situation.”
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.”
The M-dwarfs in Multiples (MinMs) survey – I. Stellar multiplicity among low-mass stars within 15 pc (2015, background): “Among the nearest stars, the large majority are M-dwarfs (e.g. Reid & Gizis 1997), with a recent accounting indicating that Mdwarfs outnumber higher mass stars by a factor of ∼3 (Lépine & Gaidos 2011).”
A NEARBY M STAR WITH THREE TRANSITING SUPER-EARTHS DISCOVERED BY K2 (2015, background): “We identified the high proper motion star PMI112930127 as a target for our Campaign 1 proposal (GO103614, PI Crossfield) from the SUPERBLINK proper motion survey (Lépine & Shara 2005; Lépine & Gaidos 2011).”