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Cool White Dwarfs Revisited: New Spectroscopy and Photometry

Salim, Samir and Rich, R. Michael and Hansen, Brad M. and Koopmans, L. V. E. and Oppenheimer, Ben R. and Blandford, Roger D. (2004) Cool White Dwarfs Revisited: New Spectroscopy and Photometry. Astrophysical Journal, 601 (2). pp. 1075-1087. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20170408-172900790

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Abstract

In this paper we present new and improved data on 38 cool white dwarfs identified in 2001 by Oppenheimer and coworkers as candidate dark-halo objects. Using the high-resolution spectra obtained with LRIS on Keck I, we measure precise radial velocities for 13 white dwarfs that show an Hα absorption line. We show that accounting for radial velocities on average decreases the U-V plane velocities by only 6%. In two cases, accounting for the radial velocities put original halo candidates below the Oppenheimer and coworkers velocity cut. The radial velocity sample has a velocity dispersion in the direction perpendicular to the Galactic plane of σ_W = 59 km s^(-1), between the values typically associated with the thick-disk and stellar-halo populations. We also see indications of the presence of two populations by analyzing the velocities in the U-V plane. In addition, we present CCD photometry for half of the sample, and with it recalibrate the photographic photometry of the remaining white dwarfs. Using the new photometry in standard bands and applying the appropriate color-magnitude relations for hydrogen and helium atmospheres, we obtain new distance estimates. By recalibrating the distances of the white dwarfs that were not originally selected as halo candidates, we obtain 13 new candidates (and lose two original ones). On average, the new distances produce velocities in the U-V plane that are larger by 10%, with already fast objects gaining more. Using the new data while applying the same U-V plane velocity cut (94 km s^(-1)) and methods of analysis as did Oppenheimer and coworkers, we find a density of cool white dwarfs of 1.7 × 10^(-4) pc^(-3), confirming their value. In addition, we derive the density as a function of the U-V plane velocity cutoff. The density (corrected for losses due to higher U-V plane velocity cuts) starts to flatten out at 150 km s-1 (0.4 × 10^(-4) pc^(-3)) and is minimized (thus minimizing the possible nonhalo contamination) at 190 km s-1 (0.3 × 10^(-4) pc^(-3)). These densities are in rough agreement with the estimates for the stellar-halo white dwarfs, corresponding to values a factor of 1.9 and 1.4 higher.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/380581DOIArticle
http://arxiv.org/abs/astro-ph/0308126arXivDiscussion Paper
Additional Information:© 2004. The American Astronomical Society. Received 2003 August 7; accepted 2003 October 7. We thank Didier Saumon for valuable discussions and the referee Hugh Harris for sharing some unpublished measurements. We are indebted to Nigel Hambly and Andrew Digby for their work in constructing the SuperCOSMOS sample. This publication makes use of the VizieR and SIMBAD Catalogue Services of CDS in Strasbourg, France, and data products from 2MASS, which is a joint project of the University of Massachusetts and IPAC/Caltech, funded by NASA and the National Science Foundation.
Group:TAPIR
Funders:
Funding AgencyGrant Number
NASA/JPL/CaltechUNSPECIFIED
NSFUNSPECIFIED
Subject Keywords:dark matter; Galaxy: halo; stars: kinematics; white dwarfs
Record Number:CaltechAUTHORS:20170408-172900790
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20170408-172900790
Official Citation:Samir Salim et al 2004 ApJ 601 1075
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:76356
Collection:CaltechAUTHORS
Deposited By: 1Science Import
Deposited On:29 Mar 2018 23:12
Last Modified:29 Mar 2018 23:12

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