The luminosity function of white dwarfs and M dwarfs, using dark nebulae as opaque outer screens
| dc.creator | Festin, Leif | |
| dc.date | 1998-06-11 | |
| dc.date.accessioned | 2026-07-07T02:27:11Z | |
| dc.date.available | 2026-07-07T02:27:11Z | |
| dc.description | By using dark nebulae as opaque outer screens, the luminosity function of white dwarfs and M dwarfs has been studied. High-extinction areas towards the Orion A, Serpens and rho Oph cloud complexes were observed, covering a volume corresponding to 464 pc3 in the solar neighbourhood, complete to Mv=16.5. Foreground stars were selected by VRI photometry and photometric parallaxes. The resulting foreground sample consists of 21 M dwarfs and 7 white dwarfs. The derived M-dwarf luminosity function is consistent with previous studies, showing no substantial upturn beyond Mv=16. The 7 white dwarfs imply a local density of 0.013(+-0.005)Msun/pc3 (~15% of the dynamical mass in the solar neighbourhood) supporting other recent results but obtained with a completely different method. For the clouds, foreground-star data were used to derive independent cloud distances, while the background stars and a simple model of the Milky Way gave reliable cloud extinctions. | |
| dc.description | 12 pages, 15 figures, to be published in A&A | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9806166 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9806166 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/12583 | |
| dc.subject | Astrophysics | |
| dc.title | The luminosity function of white dwarfs and M dwarfs, using dark nebulae as opaque outer screens | |
| dc.type | text |