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Photometric Properties of White Dwarf Dominated Halos

Published online by Cambridge University Press:  05 March 2013

Hyun-chul Lee
Affiliation:
Centre for Astrophysics and Supercomputing, Swinburne University, Melbourne VIC 3122, Australia
Brad K. Gibson
Affiliation:
Centre for Astrophysics and Supercomputing, Swinburne University, Melbourne VIC 3122, Australia
Yeshe Fenner
Affiliation:
Centre for Astrophysics and Supercomputing, Swinburne University, Melbourne VIC 3122, Australia
Chris B. Brook
Affiliation:
Centre for Astrophysics and Supercomputing, Swinburne University, Melbourne VIC 3122, Australia
Daisuke Kawata
Affiliation:
Centre for Astrophysics and Supercomputing, Swinburne University, Melbourne VIC 3122, Australia
Agostino Renda
Affiliation:
Centre for Astrophysics and Supercomputing, Swinburne University, Melbourne VIC 3122, Australia
Janne Holopainen
Affiliation:
Centre for Astrophysics and Supercomputing, Swinburne University, Melbourne VIC 3122, Australia Tuorla Observatory, Piikkiö FIN-21500, Finland
Chris Flynn
Affiliation:
Centre for Astrophysics and Supercomputing, Swinburne University, Melbourne VIC 3122, Australia Tuorla Observatory, Piikkiö FIN-21500, Finland
Corresponding
E-mail address:
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Abstract

Using stellar population synthesis techniques, we explore the photometric signatures of white dwarf progenitor dominated galactic halos, in order to constrain the fraction of halo mass that may be locked up in white dwarf stellar remnants. We first construct a 109 M stellar halo using the canonical Salpeter initial stellar mass distribution, and then allow for an additional component of low- and intermediate-mass stars, which ultimately give rise to white dwarf remnants. Microlensing observations towards the Large Magellanic Cloud, coupled with several ground-based proper motion surveys, have led to claims that in excess of 20% of the dynamical mass of the halo (1012 M) might be found in white dwarfs. Our results indicate that (1) even if only 1% of the dynamical mass of the dark halo today could be attributed to white dwarfs, their main sequence progenitors at high redshift (z ≈ 3) would have resulted in halos more than 100 times more luminous than those expected from conventional initial mass functions alone, and (2) any putative halo white dwarf progenitor dominated initial mass function component, regardless of its dynamical importance, would be virtually impossible to detect at the present day, due to its extremely faint surface brightness.

Type
Research Article
Copyright
Copyright © Astronomical Society of Australia 2004

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