Meeting the Cool Neighbors. VIII. A Preliminary 20 Parsec Census from the NLTT Catalogue

By I. Neill Reid, Kelle Cruz, Peter K. Allen, Finlay S. Mungall, D. Kilkenny, James W. Liebert, S. Hawley, O. Fraser, K. Covey, P. Lowrance and 2 more. 2004

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Continuing our census of late-type dwarfs in the solar neighborhood, we present BVRI photometry and optical spectroscopy of 800 mid-type M dwarfs drawn from the NLTT proper-motion catalog. The targets are taken both from our own cross-referencing of the NLTT Catalogue and the 2MASS Second Incremental Data Release, and from the revised NLTT compiled recently by Salim & Gould. All are identified as nearby-star candidates based on their location in the (mr, mr-Ks) diagram. Three hundred stars discussed here have previous astrometric, photometric, or spectroscopic observations. We present new BVRI photometry for 101 stars, together with low-resolution spectroscopy of a further 400 dwarfs. In total, we find that 241 stars are within 20 pc of the Sun, while a further 70 lie within 1 σ of our distance limit. Combining the present results with previous analyses, we have quantitative observations for 1910 of the 1913 candidates in our NLTT nearby-star samples. Eight hundred fifteen of those stars have distance estimates of 20 pc or less, including 312 additions to the local census. With our NLTT follow-up observations essentially complete, we have searched the literature for K and early-type M dwarfs within the sampling volume covered by the 2MASS second release. Comparing the resultant 20 pc census against predicted numbers, derived from the 8 pc luminosity function, shows an overall deficit of ∼20% for stellar systems and ∼35% for individual stars. Almost all are likely to be fainter than MJ = 7, and at least half are probably as yet undiscovered companions of known nearby stars. Our results suggest that there are relatively few missing systems at the lowest luminosities, MJ > 8.5. We discuss possible means of identifying the missing stars.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c0ecfa1ac639df9cd8e0267587aee32b761a9175

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Citations in the corpus

MEETING THE COOL NEIGHBORS. X. ULTRACOOL DWARFS FROM THE 2MASS ALL-SKY DATA RELEASE (2008, result): “The main results from our M-dwarf surveys are summarised in Papers VIII and XI of this series (Reid et al, 2004; 2007), which present preliminary J-band luminosity functions, Φ(MJ), for stars within 20-parsecs of the Sun.”
IDENTIFYING THE YOUNG LOW-MASS STARS WITHIN 25 PC. I. SPECTROSCOPIC OBSERVATIONS (2009, methodology): “Reid et al. (2003, 2004, 2007a) used a combination of photometric (i.e., (V − J ) 3 and (H − Ks) 0.23 to largely eliminate stars earlier than M0) and proper-motion methods to identify candidate cool objects, which were subsequently confirmed with follow-up moderate-resolution (R ∼ 1800) optical…”
A SPECTROSCOPIC CATALOG OF THE BRIGHTEST (J < 9) M DWARFS IN THE NORTHERN SKY, (2012, background): “Most notably, the “Meet the Cool Neighbours” program (hereafter MCN) has determined spectral subtypes for several hundred M dwarfs identified from the Luyten catalogs but not listed in the CNS3 (Cruz & Reid 2002; Cruz et al. 2003; Reid et al. 2003, 2004; Cruz et al. 2007; Reid, Cruz, & Allen 2007).”
FURTHER DEFINING SPECTRAL TYPE “Y” AND EXPLORING THE LOW-MASS END OF THE FIELD BROWN DWARF MASS FUNCTION (2012, methodology): “This list relies heavily on previous work, most notably the list compiled by Reid & Gizis (1997) with updates in Reid et al. (2004) and Reid (priv. comm.) and the list of the hundred nearest stars compiled by RECONS at their website.”
The Solar Neighborhood. XVII. Parallax Results from the CTIOPI 0.9 m Program: 20 New Members of the RECONS 10 Parsec Sample (2006, methodology): “More recently, large-scale work by Reid and collaborators (Reid & Cruz 2002; Reid et al. 2002, 2003a, 2003b, 2004; Cruz & Reid 2002; Cruz et al. 2003; Reid 2003) has identified additional new systems from proper-motion compendia, and has reidentified and confirmedmany of the systems noted by others.”
M dwarfs: effective temperatures, radii and metallicities (2008, methodology): “Another accurate source of Johnson–Cousins photometry for M dwarfs is Reid et al. (2002, 2003, 2004).”
SPECTRO-THERMOMETRY OF M DWARFS AND THEIR CANDIDATE PLANETS: TOO HOT, TOO COOL, OR JUST RIGHT? (2013, background): “Since over 70% of stars in the solar neighborhood are M dwarfs (Henry et al. 1994; Chabrier 2003; Reid et al. 2004) it is likely that the vast majority of potentially habitable planets near our Sun orbit around late K and M dwarfs.”
BAYESIAN ANALYSIS TO IDENTIFY NEW STAR CANDIDATES IN NEARBY YOUNG STELLAR KINEMATIC GROUPS (2012, methodology): “…2007; (o) thiswork; (p) Zuckerman et al. 2001c; (q) Reid et al. 2003; (r) Reid & Cruz 2002; (s) Koen et al. 2010; (t) Casagrande et al. 2008; (u) Reid et al. 2004; (v) SDSS-DR8; Adelman-McCarthy & et al. 2011; (w) Weis 1991; (x) Koen et al. 2002; (y) NOMAD; Zacharias et al. 2005; (z) PPMXL;…”
A STELLAR CENSUS OF THE TUCANA–HOROLOGIUM MOVING GROUP (2014, unknown): “…be robustly calibrated for the age of Tuc-Hor, then their measurement for stars unaffiliated with any moving group can distinguish analogs to stars in star-forming regions (τ = 1–20 Myr) from the young (τ = 50–300 Myr) field population (Shkolnik et al. 2012) and old field stars (Reid et al. 2004).”
The effective temperature scale of M dwarfs (2013, methodology): “It comes from the NOMAD catalogue (Zacharias et al. 2005), the Deep Near-Infrared Survey (DENIS, Epchtein 1997), the Two Micron All Sky Survey (2MASS, Skrutskie et al. 2006), Reid et al. (2004, 2007), Koen & Eyer (2002); Koen et al. (2010).”
Stellar Flares from the First TESS Data Release: Exploring a New Sample of M Dwarfs (2019, background): “%) of the stellar population (Dole 1964; Henry et al. 1994; Reid et al. 2004; Covey et al. 2008).”
CARMENES input catalogue of M dwarfs. I. Low-resolution spectroscopy with CAFOS (2015, unknown): “…al. 2000; CrRe02: Cruz & Reid 2002; Gray03: Gray et al. 2003; Lep03: Lépine et al. 2003; Reid03: Reid et al. 2003; Tee03: Teegarden et al. 2003; Reid04: Reid et al. 2004; Boc05: Bochanski et al. 2005; Scho05: Scholz et al. 2005; Gray06: Gray et al. 2006; Mon06: Montagnier et al. 2006; Riaz06:…”
Meeting the Cool Neighbors. IX. The Luminosity Function of M7-L8 Ultracool Dwarfs in the Field (2006, background): “As discussed in Reid et al. (2004), 95% of the 8-parsec stars have reliable trigonometric parallaxes; the J - band photometry is taken either from 2MASS or, for bright stars, drawn from the literature and transformed, if necessary, to the CIT system.”
THE HAWAII INFRARED PARALLAX PROGRAM. I. ULTRACOOL BINARIES AND THE L/T TRANSITION, (2012, unknown): “…et al. (2012); (131) Reid et al. (1995); (132) Reid & Cruz (2002a); (133) Reid & Cruz (2002b); (134) Reid et al. (2003a); (135) Reid et al. (2003b); (136) Reid et al. (2004); (137) Reid et al. (2008b); (138) Ruiz et al. (1991); (139) Schilbach et al. (2009); (140) Schneider et al. (2002); (141)…”
THE PALOMAR/KECK ADAPTIVE OPTICS SURVEY OF YOUNG SOLAR ANALOGS: EVIDENCE FOR A UNIVERSAL COMPANION MASS FUNCTION (2008, unknown): “T dwarfs (Leggett et al. 2002; Reid et al. 2004) with known parallaxes (from Dahn et al. 2002; Vrba et al. 2004).”
TIME-RESOLVED PROPERTIES AND GLOBAL TRENDS IN dMe FLARES FROM SIMULTANEOUS PHOTOMETRY AND SPECTRA (2013, methodology): “…Johnson B and V fluxes were compared to the accepted magnitudes (in Table 1, obtained from Reid & Hawley (2005) who compiled magnitude data from Bessell 1990; Koen et al. 2002; Leggett 1992, GJ 1243 measurements were obtained from Reid et al. (2004)), using the Johnson (1966) flux zeropoints.”