Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· On-line Data
· References in the article
· Citations to the Article (32) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (115)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Wide Binary Systems and the Nature of High-Velocity White Dwarfs
Authors:
Silvestri, Nicole M.; Oswalt, Terry D.; Hawley, Suzanne L.
Affiliation:
AA(Department of Physics and Space Sciences and the SARA Observatory, Florida Institute of Technology, 150 West University Boulvard, Melbourne, FL 32901-6975 , ), AB(Department of Physics and Space Sciences and the SARA Observatory, Florida Institute of Technology, 150 West University Boulvard, Melbourne, FL 32901-6975 , ), AC(Department of Astronomy, University of Washington, Seattle, WA 98195; )
Publication:
The Astronomical Journal, Volume 124, Issue 2, pp. 1118-1126. (AJ Homepage)
Publication Date:
08/2002
Origin:
UCP
AJ Keywords:
Stars: Binaries: General, Galaxy: disk, Galaxy: Kinematics and Dynamics, Stars: Fundamental Parameters, Stars: White Dwarfs
DOI:
10.1086/341382
Bibliographic Code:
2002AJ....124.1118S

Abstract

We present measured radial velocities and complete space motions for 116 white dwarf stars with M dwarf companions. Thirteen pairs have ``halo-like'' velocities. According to a recent study by Oppenheimer et al., all these high-velocity white dwarfs should be considered part of the dark matter heavy halo of the Galaxy, based on their kinematics. Based on the near-solar abundance levels of the M dwarf companions, we conclude that 12 of our 13 high-velocity white dwarfs are actually part of the high-velocity tail of the thick disk, rather than the dark matter halo of the Galaxy, in agreement with the results of a recent study of 514 M dwarfs performed by Reid, Sahu, & Hawley. We find only one potential stellar halo white dwarf (LP 164-52) in our sample. The M dwarf companion of LP 164-52 is a metal-poor, intermediate subdwarf with high-velocity UVW-space motions. In view of the similarity to our sample, we conclude that the majority of the dark matter halo white dwarfs identified by Oppenheimer et al. are most likely to be members of the thick disk, and hence their contribution to the dark matter content of the halo is very much overestimated. Our results suggest that the assignment of population membership solely on incomplete kinematical information is not definitive and that a more robust examination of suspected halo white dwarfs must be performed. Based on observations obtained with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium, and the SARA Observatory at Kitt Peak, which is owned and operated by the Southeastern Association for Research in Astronomy.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints