THE SLOAN DIGITAL SKY SURVEY DATA RELEASE 7 SPECTROSCOPIC M DWARF CATALOG. I. DATA

By Andrew A. West, D. Morgan, J. Bochanski, J. Andersen, K. Bell, A. Kowalski, James R. A. Davenport, S. Hawley, S. Schmidt, D. Bernat and 10 more. 2011

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We present a spectroscopic catalog of 70,841 visually inspected M dwarfs from the seventh data release of the Sloan Digital Sky Survey. For each spectrum, we provide measurements of the spectral type, a number of molecular band heads, and the Hα, Hβ, Hγ, Hδ, and Ca ii K emission lines. In addition, we calculate the metallicity-sensitive parameter ζ and identify a relationship between ζ and the g − r and r − z colors of M dwarfs. We assess the precision of our spectral types (which were assigned by individual examination), review the bulk attributes of the sample, and examine the magnetic activity properties of M dwarfs, in particular those traced by the higher order Balmer transitions. Our catalog is cross-matched to Two Micron All Sky Survey infrared data, and contains photometric distances for each star. Finally, we identify eight new late-type M dwarfs that are possibly within 25 pc of the Sun. Future studies will use these data to thoroughly examine magnetic activity and kinematics in late-type M dwarfs and examine the chemical and dynamical history of the local Milky Way.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/de41a9e8b35c29339c29b3bb94b9acaddb8981a4

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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): “Sloan Digital Sky Survey also has ' 70, 000 visible wavelength spectra of M dwarfs (West et al. 2011; Bochanski et al. 2011) with similar resolution to our own, which could be used in conjunction with our calibrations to map out the metallicity distribution of the sample.”
Measuring the vertical age structure of the Galactic disc using asteroseismology and SAGA (2015, background): “…dispersion relation (e.g. von Hoerner 1960; Mayor 1974; Wielen 1977; Holmberg et al. 2007), the chemistry in red giants (Masseron & Gilmore 2015) and the change in fraction of active M dwarfs of similar spectral type at increasing Galactic latitudes (e.g. West et al. 2011, and references therein).”
THE Hα EMISSION OF NEARBY M DWARFS AND ITS RELATION TO STELLAR ROTATION (2016, methodology): “Hα EWs We measure Hα EWs using the definition of West et al. (2011).”
WEATHER ON OTHER WORLDS. II. SURVEY RESULTS: SPOTS ARE UBIQUITOUS ON L AND T DWARFS (2014, background): “Notably, M and early-L dwarfs are known to have elevated magnetospheric activity (Schmidt et al. 2007; Hallinan et al. 2008; Berger et al. 2010; West et al. 2011).”
LAMOST Experiment for Galactic Understanding and Exploration (LEGUE) — The survey's science plan (2012, methodology): “Most M dwarfs identified in SDSS lie at high Galactic latitudes, and thus probe mainlythe Galactic old/thick disk (West et al. 2011).”
AN ALL-SKY CATALOG OF BRIGHT M DWARFS (2011, background): “Color and magnitude cuts for bright M stars Figure 3 shows the distribution of optical-to-infraredV − J colors for a subset of M dwarfs with spectral classification from the Sloan Digital Sky Survey database (West et al. 2011).”
THE BARYON OSCILLATION SPECTROSCOPIC SURVEY OF SDSS-III (2012, background): “SDSS I and II yielded a wealth of spectroscopic data of these ultracool dwarfs (Schmidt et al. 2010c; West et al. 2011), but were limited by the small number of spectra observed for stars with spectral types later than M7.”
The SDSS–2MASS–WISE 10-dimensional stellar colour locus (2014, background): “The position along the narrow locus in the (i − J, g − i) diagram of Figure 2 is parameterized by effective temperature over a wide range of stellar mass, as shown by Bochanski et al. (2007) and West et al. (2011) for red stars, and Ivezić et al. (2008) for blue stars.”
A NEARBY M STAR WITH THREE TRANSITING SUPER-EARTHS DISCOVERED BY K2 (2015, result): “We therefore measure the Hα equivalent width (EW) as defined by West et al. (2011) and Lépine et al. (2013) and find consistent results using both approaches.”
THE PAN-STARRS1 DISTANT z > 5.6 QUASAR SURVEY: MORE THAN 100 QUASARS WITHIN THE FIRST GYR OF THE UNIVERSE (2016, methodology): “In order to visualize the PS1 colors of brown dwarfs, we cross-matched the M-dwarf catalog of West et al. (2011) to the PS1 PV3 catalog.”
A NEAR-INFRARED SPECTROSCOPIC STUDY OF YOUNG FIELD ULTRACOOL DWARFS (2013, background): “A great deal of current work relies on the use of spectral templates for determination of spectral types, particularly for optical spectroscopy (e.g. West et al. 2011).”
How to Characterize Habitable Worlds and Signs of Life (2017, background): “M stars also remain active for longer periods of time than the Sun (e.g., West et al. 2011), making the surface of planets around an active M star a potentially highly irradiated environment, depending on the atmospheric composition.”
A STELLAR CENSUS OF THE TUCANA–HOROLOGIUM MOVING GROUP (2014, background): “• Hα emission: Old main sequence stars exhibit a wide range of activity levels (e.g., Kafka & Honeycutt 2006; West et al. 2011), and hence the presence of strong Hα emission can not be used as a positive criterion for determining membership.”
A SPECTROSCOPIC CATALOG OF THE BRIGHTEST (J < 9) M DWARFS IN THE NORTHERN SKY, (2012, methodology): “(Bochanski et al. 2005, 2010; West et al. 2011), and do not overlap with our present census.”