The Palomar/MSU Nearby Star Spectroscopic Survey. IV. The Luminosity Function in the Solar Neighborhood and M Dwarf Kinematics

By I. Neill Reid, J. Gizis, S. Hawley. 2002

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Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f6af622da6a86e8a75f84635dc0aae71d835ca05

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Citations in the corpus

Galactic Stellar and Substellar Initial Mass Function (2003, unknown): “The MF derived from the new V-band LF or Reid et al. (2002), not displayed in the figure, closely resembles the one derived from the Henry & McCarthy (1990) K-band LF.”
The Variation of Integrated Star Initial Mass Functions among Galaxies (2005, background): “The Canonical IMF and the Maximal Stellar Mass in a Cluster The universal or canonical stellar IMF is conveniently written (Kroupa 2001; Reid et al. 2002) as a multi–power law, (m) / m i , with exponents 0 ¼ þ0:30 (0:01 m/M < 0:08), 1 ¼þ1:30 (0:08 m/M < 0:50), 2 ¼þ2:35 (0:50 m/M < 1:00), and 3 ¼…”
Star formation and feedback in smoothed particle hydrodynamic simulations – I. Isolated galaxies (2006, background): “Our IMF starts at 0.1 M⊙ because Reid et al. (2002) report that the stellar luminosity function appears to turn over at a luminosity corresponding to that mass, so that stars with a mass < 0.1 M⊙ do not make a large contribution to the total stellar mass.”
Evolution of low-mass star and brown dwarf eclipsing binaries (2007, background): “The EBs and, more generally, active LMS are fast rotators with rotation periods of P <∼ 3 days and rotation velocities of vrot >∼ 10 kms −1 (Delfosse et al. 1998; Reid et al. 2002, Mohanty & Basri 2003).”
The Mass Distribution and Lifetime of Prestellar Cores in Perseus, Serpens, and Ophiuchus (2008, result): “This result is consistent with recent measurements of the stellar initial mass function (α = −2.3 to −2.8; e.g. Reid et al. 2002; Kroupa 2002), providing further evidence that the final masses of stars are directly linked to the core formation process.”
Meeting the Cool Neighbors. IX. The Luminosity Function of M7-L8 Ultracool Dwarfs in the Field (2006, background): “We also note that ∼5% of the sources in our sample may prove to be unrecognized spectroscopic (∆ < 2 AU) binaries (Reid et al. 2002c; Basri & Reiners 2006).”
Comparing Star Formation on Large Scales in the c2d Legacy Clouds: Bolocam 1.1 mm Dust Continuum Surveys of Serpens, Perseus, and Ophiuchus (2007, unknown): “For example, Reid et al. (2002) find α = 2.5 above 0.6 M⊙, and α = 2.8 above 1 M⊙.”
The Milky Way Tomography with SDSS. I. Stellar Number Density Distribution (2005, unknown): “For example, assuming that the luminosity function of the overdensity is similar to that of the solar neighborhood (Reid et al. 2002, Table 4) and that our sample of overdensity stars is incomplete for g r > 0:5 (see bottom left panel of Fig.”
The Palomar/MSU Nearby Star Spectroscopic Survey. III. Chromospheric Activity, M Dwarf Ages, and the Local Star Formation History (2002, background): “As will be discussed in Paper IV of this series (Reid et al. 2002), the addition of the new astrometric data affects the inclusion/ omission of only 15% of the stars in the Paper I sample.”
Meeting the Cool Neighbors. V. A 2MASS-Selected Sample of Ultracool Dwarfs (2003, unknown): “12 of Reid et al. 2002a).”
Meeting the Cool Neighbors. VIII. A Preliminary 20 Parsec Census from the NLTT Catalogue (2004, background): “The results from this thread of our project are published as follows: • Paper IV ( Reid et al., 2002) presents the initial result from the ultracool survey, the identi- fication of an M8 dwarf within 6 parsecs of the Sun.”