Characterization of M, L, and T Dwarfs in the Sloan Digital Sky Survey

By S. Hawley, K. Covey, G. Knapp, D. Golimowski, Xiaohui Fan, S. Anderson, James E. Gunn, H. Harris, Željko Ivezic´, G. M. Long and 22 more. 2002

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An extensive sample of M, L, and T dwarfs identified in the Sloan Digital Sky Survey (SDSS) has been compiled. The sample of 718 dwarfs includes 677 new objects (629 M dwarfs and 48 L dwarfs), together with 41 that have been previously published. All new objects and some of the previously published ones have new optical spectra obtained either with the SDSS spectrographs or with the Apache Point Observatory 3.5 m ARC telescope. Spectral types and SDSS colors are available for all objects; approximately 35% also have near-infrared magnitudes measured by 2MASS (Two Micron All Sky Survey) or on the Mauna Kea system. We use this sample to characterize the color–spectral type and color-color relations of late-type dwarfs in the SDSS filters and to derive spectroscopic and photometric parallax relations for use in future studies of the luminosity and mass functions based on SDSS data. We find that the i* - z* and i* - J colors provide good spectral type and absolute magnitude (Mi*) estimates for M and L dwarfs. Our distance estimates for the current sample indicate that SDSS is finding early M dwarfs out to ∼1.5 kpc, L dwarfs to ∼100 pc, and T dwarfs to ∼20 pc. The T dwarf photometric data show large scatter and are therefore less reliable for spectral type and distance estimation.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c6ca57070da8bd0344cd6035155521f21d919d57

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Citations in the corpus

Hubble Space Telescope Observations of Binary Very Low Mass Stars and Brown Dwarfs (2003, methodology): “…snapshot WFPC2 imaging with HST were chosen from the list of 2MASS-selected late M dwarfs (Gizis et al. 2000) and L dwarfs (Kirkpatrick et al. 1999, 2000) and from late M and L dwarfs identified from the initial regions covered by SDSS (Fan et al. 2000; Schneider et al. 2002; Hawley et al. 2002).”
IDENTIFYING THE YOUNG LOW-MASS STARS WITHIN 25 PC. I. SPECTROSCOPIC OBSERVATIONS (2009, background): “The Two Micron All Sky Survey (2MASS) is optimal for finding low-mass stars, since the spectral energy distributions (SEDs) of cool stars peak in the near-IR (e.g., Hawley et al. 2002).”
Near-Infrared Photometry and Spectroscopy of L and T Dwarfs: The Effects of Temperature, Clouds, and Gravity (2004, background): “…TiO and VO, and the T dwarfs, characterized by methane-band absorption in the H and K spectral regions (Martı́n et al. 1997, 1999b; Kirkpatrick et al. 1999, 2000; Strauss et al. 1999; Leggett et al. 2000, 2002b; Geballe et al. 2002, hereafter G02; Burgasser et al. 2002a; Hawley et al. 2002).”
LOW-MASS TERTIARY COMPANIONS TO SPECTROSCOPIC BINARIES. I. COMMON PROPER MOTION SURVEY FOR WIDE COMPANIONS USING 2MASS (2009, methodology): “Using the MJ -SpT relationship from Hawley et al. (2002), we estimated the expected spectral type, given an absolute J magnitude of 6.9±0.04, as M1.”
Automatic determination of stellar atmospheric parameters and construction of stellar spectral templates of the Guoshoujing Telescope (LAMOST) (2011, neutral): “Methods in Singh et al. (1998), BailerJones (2002), Hawley et al. (2002), Covey et al. (2007), and Bazarghan & Gupta (2008) may be adopted if they could provide reliable results for GSJT observations (Wu et al. 2011b in preparation).”
Design Considerations for a Ground-Based Transit Search for Habitable Planets Orbiting M Dwarfs (2007, background): “The resulting fits, displayed in Figure 3, are: i J ¼ 1:09 1:46ðJ KsÞ þ 2:50ðJ KsÞ2 0:2 < J Ks < 0:9; (4) z J ¼ 0:56þ 0:73ðJ KsÞ 0:2 < J Ks < 0:9: (5) For the primary M dwarfs, J Ks is degenerate, so we rely instead on the MJ versus i J and MJ versus z J relations of Hawley et al. (2002).”
FUNDAMENTAL PARAMETERS AND SPECTRAL ENERGY DISTRIBUTIONS OF YOUNG AND FIELD AGE OBJECTS WITH MASSES SPANNING THE STELLAR TO PLANETARY REGIME (2015, neutral): “…(2005), (24) Burgasser et al. (2006b), (25) Burgasser (2007), (26) Luyten (1979a), (27) Dieterich et al. (2014), (28) Geballe et al. (2002), (29) Hawley et al. (2002), (30) Naud et al. (2014), (31) Reid et al. (2001), (32) Cruz et al. (2003), (33) Kirkpatrick et al. (2006), (34) K. Cruz et al.…”
Meeting the Cool Neighbors. V. A 2MASS-Selected Sample of Ultracool Dwarfs (2003, methodology): “The former method has yielded close to 200 L dwarfs and over 180 ultracool M dwarfs in the three surveys (notable for quantity are Phan-Bao et al. 2001, 2003; Schneider et al. 2002; Hawley et al. 2002; Gizis et al. 2000b; Kirkpatrick et al. 1999, 2000; Martı́n et al 1999b).”
BANYAN. VII. A NEW POPULATION OF YOUNG SUBSTELLAR CANDIDATE MEMBERS OF NEARBY MOVING GROUPS FROM THE BASS SURVEY (2015, neutral): “…Costa et al. (2005, 2006); Cushing et al. (2011); Deacon et al. (2014); Delorme et al. (2008a,b); Dieterich et al. (2014); Faherty et al. (2013); Hawley et al. (2002); Kendall et al. (2007b,a); Kirkpatrick et al. (2012); Leggett et al. (2000, 2002, 2009, 2010, 2013, 2015); Lodieu et al. (2005,…”
New spectral types L and T (2005, background): “17 + 024424.8, type T0) listed in the near-infrared spectroscopy paper by Knapp et al. (2004) appears in the optical spectroscopy paper by Hawley et al. (2002), where it is listed as an L8 dwarf.”
CONSTRAINING THE AGE–ACTIVITY RELATION FOR COOL STARS: THE SLOAN DIGITAL SKY SURVEY DATA RELEASE 5 LOW-MASS STAR SPECTROSCOPIC SAMPLE (2007, background): “…examine the statistical properties of M dwarfs in a variety of capacities, including analyses of mean M dwarf colors and spectroscopic properties (Hawley et al. 2002; West et al. 2004; hereafter W04; West, Walkowicz & Hawley 2005; Bochanski et al. 2007a; Covey et al. 2007), computing the…”
A SPECTROSCOPIC CATALOG OF THE BRIGHTEST (J < 9) M DWARFS IN THE NORTHERN SKY, (2012, methodology): “This corroborates the observation made previously by Hawley et al. (2002), as part of the PMSU survey.”
Preliminary Parallaxes of 40 L and T Dwarfs from the US Naval Observatory Infrared Astrometry Program (2004, methodology): “Column 7 of Table 1 gives the codes H, S, or IR indicating whether the Hawley et al. (2002), Siegel et al. (2002), and/or infrared calibrations were employed.”
Exploring the Variable Sky with the Sloan Digital Sky Survey (2007, background): “…and stars (Richards et al. 2002), spectral classification of stars to within one to two spectral subtypes (Lenz et al. 1998; Finlator et al. 2000; Hawley et al. 2002), and even remarkably efficient color selection of horizontal-branch and RR Lyrae stars (Yanny et al. 2000; Sirko et al. 2004;…”