Low-Mass Dwarf Template Spectra from the Sloan Digital Sky Survey

By J. Bochanski, Andrew A. West, S. Hawley, K. Covey. 2006

225 citations recorded by the source corpus.

We present template spectra of low-mass (M0-L0) dwarfs derived from over 4000 Sloan Digital Sky Survey spectra. These composite spectra are suitable for use as medium-resolution (R ∼ 1800) radial velocity standards. We report mean spectral properties (molecular band-head strengths, equivalent widths) and use the templates to investigate the effects of magnetic activity and metallicity on the spectroscopic and photometric properties of low-mass stars.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4915c536a94cea3995f88eb855f0519abfc514aa

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

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.”
THE Hα EMISSION OF NEARBY M DWARFS AND ITS RELATION TO STELLAR ROTATION (2016, methodology): “We adjust for the known 7.3 km/s offset in the SDSS absolute RV rest frame Yanny et al. (2009), which we note was not corrected for in West et al. (2015).”
THE MILKY WAY TOMOGRAPHY WITH SDSS. III. STELLAR KINEMATICS (2009, methodology): “A significant vertical age gradient for disk stars is also supported by an analysis of active M dwarfs presented in Bochanski et al. (2007b).”
SPECTRO-THERMOMETRY OF M DWARFS AND THEIR CANDIDATE PLANETS: TOO HOT, TOO COOL, OR JUST RIGHT? (2013, methodology): “…spectrum in wavelength to the rest frames of their source stars by cross-correlating each spectrum to a spectral template of similar spectral type from the Sloan Digital Sky Survey (Stoughton et al. 2002; Bochanski et al. 2007) using the IDL routine xcorl (Mohanty & Basri 2003; West & Basri 2009).”
On the Spectral Evolution of Hot White Dwarf Stars. I. A Detailed Model Atmosphere Analysis of Hot White Dwarfs from SDSS DR12 (2020, methodology): “Briefly, we combined our white dwarf synthetic spectra with the M dwarf spectral templates of Bochanski et al. (2007), and we fitted each observed spectrum with a function given by [ ( ) ( )] [ ]l l l = + ´ ´ + + + F F T g f F a a a a , log type . obs WD eff M 0 1 2 2 3 3 In this equation, the flux…”
THE SPITZER DEEP, WIDE-FIELD SURVEY (2009, background): “The SDSS colors of this object appear consistent with it being of spectral type M0 or perhaps M1 (Bochanski et al. 2007).”
ERRATUM: “THE LUMINOSITY AND MASS FUNCTIONS OF LOW-MASS STARS IN THE GALACTIC DISK. II. THE FIELD” (2010, AJ, 139, 2679) (2010, background): “The latter two cuts ensure that the stars have red colors typical of M dwarfs (Bochanski et al. 2007b; Covey et al. 2007; West et al. 2008).”
EARLY-TYPE GALAXY ARCHEOLOGY: AGES, ABUNDANCE RATIOS, AND EFFECTIVE TEMPERATURES FROM FULL-SPECTRUM FITTING (2013, methodology): “We have also supplemented the MILES empirical library with stacked SDSS M dwarf spectra from Bochanski et al. (2007).”
LSST: From Science Drivers to Reference Design and Anticipated Data Products (2008, methodology): “SEDs for M, L, and T dwarfs are generated from a combination of spectral models and by stacking spectra from the SDSS (e.g., Cushing et al. 2005, Bochanski et al. 2007, Burrows et al. 2006, Petterson & Hawley 1989, Kowalski et al. 2010).”
A SPECTROSCOPIC CATALOG OF THE BRIGHTEST (J < 9) M DWARFS IN THE NORTHERN SKY, (2012, methodology): “As with the MDM data, SNIFS spectra were shifted to the rest frames of their emitting stars by cross-correlation to SDSS templates (Bochanski et al. 2007) of the corresponding spectral subtype.”
Stellar SEDs from 0.3 to 2.5 μm: Tracing the Stellar Locus and Searching for Color Outliers in the SDSS and 2MASS (2007, methodology): “…FGKM dwarf stars; for those stars, Williams et al. (2002), Hawley et al. (2002), West et al. (2005), Bilir et al. (2005), Davenport et al. (2006), Bochanski et al. (2007) and Golimowski et al. (2007) present science-grade empirical measurements, while Girardi et al. (2004) and Dotter & Chaboyer…”
CONSTRAINING THE AGE–ACTIVITY RELATION FOR COOL STARS: THE SLOAN DIGITAL SKY SURVEY DATA RELEASE 5 LOW-MASS STAR SPECTROSCOPIC SAMPLE (2007, methodology): “We adapt the Lepine two-dimensional metallicity space to a single ratio, (CaH2+CaH3)/TiO5, and use this as a proxy for metallicity at a given spectral type (a similar technique was used in Bochanski et al. 2007b).”
The Stellar Populations of Praesepe and Coma Berenices (2007, methodology): “We combined these results with the r i, i z, and z J colors of West et al. (2005) and the u g and g r colors of Bochanski et al. (2007).”
Trumpeting M dwarfs with CONCH-SHELL: a catalogue of nearby cool host-stars for habitable exoplanets and life (2014, methodology): “We placed each of the remaining 1185 spectra in their rest frames by converting wavelengths to vacuum val- ues then cross-correlating each spectrum to SDSS templates (Bochanski et al. 2007) of the corresponding spectral subtype.”
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): “The most likely explanation for this is a small difference in the RV templates used for our SpeX and SNIFS data, taken from Rayner et al. (2009) and Bochanski et al. (2007) respectively.”
CARMENES input catalogue of M dwarfs. I. Low-resolution spectroscopy with CAFOS (2015, background): “Moreover, several authors have identified significat differences between colours and spectral indices of active andin ctive stars of similar properties that may affect the spectral typing of M dwarfs (Stauffer & Hartmann 1986; Hawley et al. 1996; Bochanski et al. 2007; Morales et al. 2008).”
A SPECTROSCOPIC SURVEY AND ANALYSIS OF BRIGHT, HYDROGEN-RICH WHITE DWARFS (2011, methodology): “Our fitting procedure for these systems combines the synthetic spectra computed from our pure hydrogen model atmospheres with the M dwarf spectral templates compiled and presented by Bochanski et al. (2007).”
THE SLOAN DIGITAL SKY SURVEY DATA RELEASE 7 SPECTROSCOPIC M DWARF CATALOG. I. DATA (2011, methodology): “This method has been shown to produce uncertainties ranging from 7 to 10 km s−1 (Bochanski et al. 2007b).”