ERRATUM: “THE LUMINOSITY AND MASS FUNCTIONS OF LOW-MASS STARS IN THE GALACTIC DISK. II. THE FIELD” (2010, AJ, 139, 2679)

By J. Bochanski, S. Hawley, K. Covey, Andrew A. West, I. Neill Reid, D. Golimowski, Željko Ivezic´. 2010

243 citations recorded by the source corpus.

We report on new measurements of the luminosity function (LF) and mass function (MF) of field low-mass dwarfs derived from Sloan Digital Sky Survey Data Release 6 photometry. The analysis incorporates ~15 million low-mass stars (0.1 ), spread over 8400 deg2. Stellar distances are estimated using new photometric parallax relations, constructed from ugriz photometry of nearby low-mass stars with trigonometric parallaxes. We use a technique that simultaneously measures Galactic structure and the stellar LF from 7 < Mr < 16. We compare the LF to previous studies and convert to an MF using the mass-luminosity relations of Delfosse et?al. The system MF, measured over ?1.0< log <?0.1, is well described by a lognormal distribution with = 0.25 . We stress that our results should not be extrapolated to other mass regimes. Our work generally agrees with prior low-mass stellar MFs and places strong constraints on future theoretical star formation studies.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/bf404133c4faf17ff4bbf174930723b44b73201d

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In Astronomy and Astrophysics

1. D. Charbonneau
2. Timothy Morton
3. J. Johnson
4. E. Gaidos
5. Jon Fortney
6. Michael C. Liu
7. A. Mann
8. K. Luhman

In Instrumentation

1. D. Charbonneau
2. Timothy Morton
3. J. Johnson
4. Michael C. Liu
5. K. Luhman
6. E. Gaidos
7. A. Mann
8. Jon Fortney

Citations in the corpus

• CHARACTERIZING THE COOL KOIs. IV. KEPLER-32 AS A PROTOTYPE FOR THE FORMATION OF COMPACT PLANETARY SYSTEMS THROUGHOUT THE GALAXY (2012, background): “Seventy percent of stars in the Galaxy are dwarfs of the M spectral class (“M dwarfs” or “red dwarfs,” Bochanski et al. 2010), with masses that are only ∼ 10− 50% the mass of the Sun, much cooler temperatures, and different evolutionary histories.”
• NEAR-INFRARED METALLICITIES, RADIAL VELOCITIES, AND SPECTRAL TYPES FOR 447 NEARBY M DWARFS (2013, methodology): “Bochanski et al. (2010), again exploiting SDSS, measured th M dwarf luminosity and mass functions.”
• THE SLOAN DIGITAL SKY SURVEY DATA RELEASE 7 SPECTROSCOPIC M DWARF CATALOG. I. DATA (2011, methodology): “…Kowalski et al. 2009; Kruse et al. 2010; Hilton et al. 2010), as well as the structure and kinematics of the local Milky Way thin and thick disks (Bochanski et al. 2007a, 2010; Jurić et al. 2008; Fuchs et al. 2009) and the lowmass initial mass and luminosity functions (Covey et al. 2008b;…”
• The effective temperature scale of M dwarfs (2013, background): “They constitute 70% of all stars (Reid & Gizis 1997, Bochanski et al. 2010) and 40% of the total stellar mass of the Galaxy (Chabrier 2003, 2005).”
• Debris disks as signposts of terrestrial planet formation (2011, methodology): “Our simulations are confined to Solar-mass stars, which are a small minority of all stars (Bochanski et al. 2010).”
• The Habitability of Planets Orbiting M-dwarf Stars (2016, background): “Since M dwarfs comprise ∼70% of all stars in the galaxy (Bochanski et al., 2010), they offer the best chance of finding habitable planets through sheer numbers and proximity to the Sun.”
• The Formation and Early Evolution of Low-Mass Stars and Brown Dwarfs (2012, methodology): “We also include mass functions for the Pleiades (Moraux, Kroupa & Bouvier 2004) and the field (Bochanski et al. 2010, see Section 3.2.1).”
• The stellar and sub-stellar IMF of simple and composite populations (2011, methodology): “The immense analysis by Bochanski et al. (2010) of the LF and MF of 15×106 field low-mass dwarfs (0.1<∼m/M⊙ <∼ 0.8) derived from Sloan Digital Sky Survey Data Release 6 photometry using the photometric parallax method again finds good consistency with the previous work on the stellar LF and MF.”
• KEPLER FLARES. I. ACTIVE AND INACTIVE M DWARFS (2014, methodology): “…stars in Table 1 were determined using published R− I colors transformed to SDSS r− i (Davenport et al. 2006) and then employing the Mr vs r − i photometric parallax relation given in Bochanski et al. (2010), with the updated values given in the erratum to that paper (Bochanski et al. 2012).”
• WHITE-LIGHT FLARES ON COOL STARS IN THE KEPLER QUARTER 1 DATA (2010, background): “All the stars in our flare sample have SDSS and 2MASS colors, for which there are existing photometric parallax relations (Bochanski et al. 2010; Covey et al. 2007).”
• PLANETS AROUND LOW-MASS STARS (PALMS). IV. THE OUTER ARCHITECTURE OF M DWARF PLANETARY SYSTEMS (2014, background): “…Japan. neighborhood they make up ≈75% of stars (Henry et al. 2006; Kirkpatrick et al. 2012), which is a good estimate for their galactic-wide rate (Bochanski et al. 2010), and there is some evidence that M dwarfs represent even larger fractions of stellar populations in evolved galaxies (van…”
• A CATALOG OF ROTATION AND ACTIVITY IN EARLY-M STARS (2012, methodology): “For each spectral bin, we derive its range in logM and determine the number of stars within a 12pc volume as expected from the mass function given in Bochanski et al. (2010).”
• The big problems in star formation: The star formation rate, stellar clustering, and the initial mass function (2014, background): “…the caveat about binaries aside, observations using the field star (Kroupa 2001, 2002; Chabrier 2003, 2005; Covey et al. 2008; Deacon et al. 2008; Bochanski et al. 2010; Parravano et al. 2011), young cluster (Muench et al. 2002; Chabrier 2003, 2005; Sabbi et al. 2008; Andersen et al. 2009; Sung…”