Spectroscopy of New High Proper Motion Stars in the Northern Sky. I. New Nearby Stars, New High-Velocity Stars, and an Enhanced Classification Scheme for M Dwarfs

By S. Lépine, R. Rich, M. Shara. 2002

136 citations recorded by the source corpus.

We define an enhanced spectral classification scheme for M dwarf stars and use it to derive spectral classification of 104 northern stars with proper motions larger than 0.″5 yr-1 that we discovered in a survey of high proper motion stars at low Galactic latitudes. The final tally is as follows: 54 M dwarfs, 25 sdK and sdM subdwarfs, 14 esdK and esdM extreme subdwarfs, and 11 DA and DC white dwarfs. Among the most interesting cases, we find one star to be the coolest subdwarf ever reported (LSR 2036+5059, with spectral type sdM7.5), a new M9.0 dwarf only about 6 pc distant (LSR 1835+3259), and a new M6.5 dwarf only 7 pc from the Sun (LSR 2124+4003). Spectroscopic distances suggests that 27 of the M dwarfs, three of the white dwarfs, and one of the subdwarfs (LSR 2036+5059) are within 25 pc of the Sun, making them excellent candidates for inclusion in the solar neighborhood census. Estimated sky-projected velocities suggest that most of our subdwarfs and extreme subdwarfs have halo kinematics. We find that several white dwarfs and non–metal-poor M dwarfs also have kinematics consistent with the halo, and we briefly discuss their possible origin.

Subfields: Astronomy and Astrophysics, Education, Instrumentation

View Paper: https://www.semanticscholar.org/paper/25bbb38695f7d6ba59275a29d060b4201239c9ef

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Citations in the corpus

Meeting the Cool Neighbors. V. A 2MASS-Selected Sample of Ultracool Dwarfs (2003, unknown): “…al. 2003a; (4) Kendall et al. 2003; (5) Schneider et al. 2002; (6) Geballe et al. 2002; (7) Hawley et al. 2002; (8) McCaughrean et al. 2002; (9) Phan-Bao et al. 2003; (10) Gizis 2002; (11) Ruiz et al. 2001; (12) Fan et al. 2000; (13) Paper IV; (14) Lépine et al. 2003; (15) Kirkpatrick et al. 2001.”
ERRATUM: “THE LUMINOSITY AND MASS FUNCTIONS OF LOW-MASS STARS IN THE GALACTIC DISK. II. THE FIELD” (2010, AJ, 139, 2679) (2010, methodology): “…measurements of metallicity-sensitive molecular band heads (CaH and TiO) are used to estimate the metallicity of M dwarfs at the ∼1 dex level (see Gizis 1997; Lépine et al. 2003; Burgasser & Kirkpatrick 2006; West et al. 2008), but detailed measurements are only available for a few stars.”
Low-Mass Dwarf Template Spectra from the Sloan Digital Sky Survey (2006, methodology): “…et al. 1997), have been employed in a variety of Galactic studies: tracing Galactic disk kinematics (Hawley et al. 1996; Gizis et al. 2002; Lépine et al. 2003; Bochanski et al. 2005), describing age-velocity dispersion relations (West et al. 2006), and studying Galactic structure…”
HOW TO CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, AND RADIUS (2015, background): “We 5 The Astrophysical Journal, 804:64 (38pp), 2015 May 1 Mann et al. calculated CaH2, CaH3, TiO5, TiO6, VO1, and VO2 band indices for each of the optical spectra following the definitions given in Reid et al. (1995) and Lépine et al. (2003).”
KNOW YOUR NEIGHBORHOOD: A DETAILED MODEL ATMOSPHERE ANALYSIS OF NEARBY WHITE DWARFS (2012, unknown): “And from other studies: LSR 1817+1328 (1814+134) from Lépine et al. (2003); PM J13420−3415 (1339−340) from Lépine et al. (2005); SSPM J2231−7514 (2226−754) and SSPM J2231−7515 (2226−755) from Scholz et al. (2002); LEHPM 1-4466 (2211−392) from Oppenheimer et al. (2001); LHS 1008 (0000−345) from…”
Meeting the Cool Neighbors. IX. The Luminosity Function of M7-L8 Ultracool Dwarfs in the Field (2006, background): “The redder 10LSR 1610-0040 was identified as an L subdwarf by Lépine et al. (2003a) but recent work has concluded that it is more likely to be a metal-poor M6 dwarf (Cushing & Vacca 2006; Reiners & Basri 2006) or a peculiar binary (A. Burgasser 2006, private communication).”
THE HAWAII INFRARED PARALLAX PROGRAM. I. ULTRACOOL BINARIES AND THE L/T TRANSITION, (2012, unknown): “…(2002b); (95) Leggett et al. (2007); (96) Leggett et al. (2009); (97) Leggett et al. (2010); (98) Leggett et al. (2012); (99) Leinert et al. (2000); (100) Lépine et al. (2003a); (101) Lépine et al. (2003b); (102) Lépine et al. (2009); (103) Liu et al. (2002); (104) Liu & Leggett (2005); (105)…”
CARMENES input catalogue of M dwarfs. I. Low-resolution spectroscopy with CAFOS (2015, background): “…et al. (2007): ζ = 1− TIO 5 1− [TiO 5]Z⊙ , (1) where [TiO 5]Z⊙ = 0.571−1.697CaH+1.841CaH 2−0.454CaH3 is a third-order fit of CaH= CaH 2+CaH 3 for our standard stars, and TiO 5, CaH 2, and CaH 3 are the spectral indices of Reid et al. (1995) (see also Gizis & Reid 1997 and Lépine et al. 2003).”
METALLICITY AND TEMPERATURE INDICATORS IN M DWARF K-BAND SPECTRA: TESTING NEW AND UPDATED CALIBRATIONS WITH OBSERVATIONS OF 133 SOLAR NEIGHBORHOOD M DWARFS (2011, methodology): “Bochanski et al. (2007) measured the (CaH2+CaH3)/TiO5 ratio, previously shown by Lépine et al. (2003) to roughly discriminate between solar-metallicity ([M/H]∼0), subdwarf ([M/H]∼-1.2) and extremesubdwarf ([M/H]∼-2.0) M dwarfs, for 6577 M dwarfs with Sloan Digital Sky Survey (SDSS) spectra.”