M Dwarfs from Hubble Space Telescope Star Counts. IV.

Please use this identifier to cite or link to this item: http://hdl.handle.net/1811/48165

Show full item record

Files Size Format View
fac_ZhengZheng_ ... alJournal_2001_555_393.pdf 288.9Kb PDF View/Open

Title: M Dwarfs from Hubble Space Telescope Star Counts. IV.
Creators: Zheng, Zheng; Flynn, Chris; Gould, Andrew; Bahcall, John N.; Salim, Samir
Keywords: stars: late-type
stars: low-mass, brown dwarfs
stars: luminosity function, mass function
stars: statistics
Issue Date: 2001-07-01
Publisher: American Astronomical Society
Citation: Zheng Zheng et al, "M Dwarfs from Hubble Space Telescope Star Counts. IV.," The Astrophysical Journal 555, no. 1 (2001), doi:10.1086/321485
DOI: 10.1086/321485
Abstract: We study a sample of about 1400 disk M dwarfs that are found in 148 fields observed with the Wide Field Camera 2 (WFC2) on the Hubble Space Telescope and 162 fields observed with pre-repair Planetary Camera 1 (PC1), of which 95 of the WFC2 fields are newly analyzed. The method of maximum likelihood is applied to derive the luminosity function and the Galactic disk parameters. At first, we use a local color-magnitude relation and a locally determined mass-luminosity relation in our analysis. The results are consistent with those of previous work but with considerably reduced statistical errors. These small statistical errors motivate us to investigate the systematic uncertainties. Considering the metallicity gradient above the Galactic plane, we introduce a modified color-magnitude relation that is a function of Galactic height. The resultant M dwarf luminosity function has a shape similar to that derived using the local color-magnitude relation but with a higher peak value. The peak occurs at M_V ~ 12, and the luminosity function drops sharply toward M_V ~ 14. We then apply a height-dependent mass-luminosity function interpolated from theoretical models with different metallicities to calculate the mass function. Unlike the mass function obtained using local relations, which has a power-law index α = 0.47, the one derived from the height-dependent relations tends to be flat (α = -0.10). The resultant local surface density of disk M dwarfs (12.2 ± 1.6 Msun pc^-2) is somewhat smaller than the one obtained using local relations (14.3 ± 1.3 Msun pc^-2). Our measurement favors a short disk scale length, H = 2.75 ± 0.16 (statistical) ± 0.25 (systematic) kpc.
ISSN: 1538-4357
URI: http://hdl.handle.net/1811/48165
Bookmark and Share