Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I.

By R. O. Gray, C. Corbally, R. Garrison, M. McFadden, P. Robinson. 2003

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We have embarked on a project, under the aegis of the Nearby Stars (NStars)/Space Interferometry Mission Preparatory Science Program, to obtain spectra, spectral types, and, where feasible, basic physical parameters for the 3600 dwarf and giant stars earlier than M0 within 40 pc of the Sun. In this paper, we report on the results of this project for the first 664 stars in the northern hemisphere. These results include precise, homogeneous spectral types, basic physical parameters (including the effective temperature, surface gravity, and overall metallicity [M/H]), and measures of the chromospheric activity of our program stars. Observed and derived data presented in this paper are also available on the project's Web site.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/73534a8a40cbcd6b3da409a2eb4665bea0116c9d

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Citations in the corpus

The angular sizes of dwarf stars and subgiants Surface brightness relations calibrated by interferometry (2004, background): “On the one hand, Gray et al. (2003) have recently published an extensive survey of the spectral properties of nearby stars within 40 pc, including estimates of their effective temperatures.”
FURTHER DEFINING SPECTRAL TYPE “Y” AND EXPLORING THE LOW-MASS END OF THE FIELD BROWN DWARF MASS FUNCTION (2012, background): “Other updates in Table 4 include better characterization of previously known or newly identified multiple systems and consistent, MK-based spectral types for stars earlier than late-K (see Gray et al. 2003 and Gray et al. 2006).”
Accurate fundamental parameters for lower main‐sequence stars (2006, background): “The bulk of the targets has been selected from the sample of nearby stars in the Northern hemisphere provided by Gray et al. (2003).”
Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, background): “Procyon, Eri, and 61 Cyg A were classified as active stars by Gray et al. (2003) based on Ca II H and K line emission, while µ Cas, 18 Sco, Gmb 1830, and 61 Cyg B were found to be inactive.”
AN EMPIRICAL UBV RI JHK COLOR–TEMPERATURE CALIBRATION FOR STARS (2006, background): “To try to fill in the “K dwarf desert” (see below) we also scoured Gray et al. (2003, 2006) and Casagrande et al. (2006) for photometry and abundance information.”
STELLAR DIAMETERS AND TEMPERATURES. I. MAIN-SEQUENCE A, F, AND G STARS (2011, neutral): “For stars without metallicity estimates from Holmberg et al. (2007), the [M/H] values from Gray et al. (2003, 2006) (HD 82885, HD 97603, HD 118098, HD 131156, HD 177724, HD 210418), and Takeda et al. (2005) (HD 182572) are used.”
Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics (2008, background): “…Duncan et al. (1991), Baliunas et al. (1996), Wright et al. (2004), and Hall et al. (2007), the large single-epoch surveys of Henry et al. (1996), Gray et al. (2003), and Gray et al. (2006), the smaller, focused surveys of Soderblom et al. (1993), Soderblom et al. (1998), Paulson et al. (2002),…”
DISCOVERY OF A FAINT COMPANION TO ALCOR USING MMT/AO 5 μm IMAGING (2009, background): “…inverse of parallax, (2) Gontcharov (2006), (3) Kidger & Mart́ın-Luis (2003), (4) mean value from Blackwell & Lynas-Gray (1998), Cenarro et al. (2001), Gray et al. (2003), and Le Borgne et al. (2003), (5) Gray & Garrison (1989), (6) from adopted Teff and tables of Flower (1996), (7) from adopted V…”
Two Suns in The Sky: Stellar Multiplicity in Exoplanet Systems (2006, background): “The ninth column lists the spectral type from Gray et al. (2003), the planet discovery paper, or other references for the primary, and from our spectroscopic observations or other references for the companion.”
BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc (2018, neutral): “…Lépine et al. 2013; (22) Wilson 1953; (23) White et al. 2007; (24) Griffin et al. 1988; (25) Cayrel de Strobel et al. 2001; (26) Stephenson 1986b; (27) Gray et al. 2003; (28) Nesterov et al. 1995; (29) Stephenson & Sanwal 1969; (30) Stephenson 1986a; (31) Evans 1967; (32) Royer et al. 2007;…”