The Kinematics of High Proper Motion Halo White Dwarfs

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dc.creatorKoopmans, L. V. E.
dc.creatorBlandford, R. D.
dc.date2001-07-18
dc.date.accessioned2026-07-07T01:59:22Z
dc.date.available2026-07-07T01:59:22Z
dc.descriptionWe analyse the kinematics of the entire spectroscopic sample of 99 recently discovered high proper-motion white dwarfs by Oppenheimer et al. using a maximum-likelihood analysis, and discuss the claim that the high-velocity white dwarfs are members of a halo population with a local density at least ten times greater than traditionally assumed. We argue that the observations, as reported, are consistent with the presence of an almost undetected thin disc plus a thick disc, with densities as conventionally assumed. In addition, there is a kinematically distinct, flattened, halo population at the more than 99% confidence level. Surprisingly, the thick disc and halo populations are indistinguishable in terms of luminosity, color and apparent age (1-10 Gyr). Adopting a bimodal, Schwarzschild model for the local velocity ellipsoid, with the ratios sigma_U:sigma_V:sigma_W=1:2/3:1/2, we infer radial velocity dispersions of sigma_U=62(+8/-10) km/s and 150(+80/-40) km/s (90% C.L.) for the local thick disc and halo populations, respectively. The thick disc result agrees with the empirical relation between asymmetric drift and radial velocity dispersion, inferred from local stellar populations. The local thick-disc plus halo density of white dwarfs is n^{td+h}=(1.9+-0.5)x10^-3 pc^-3 (90% C.L.), of which n^{h}=1.1(+2.1/-0.7)x10^-4 pc^-3 (90% C.L.) belongs to the halo, a density about five times higher than previously thought. (Abridged)
dc.description19 pages, 11 figures; submitted to MNRAS
dc.identifierhttps://arxiv.org/abs/astro-ph/0107358
dc.identifierhttp://arxiv.org/abs/astro-ph/0107358
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/3084
dc.subjectAstrophysics
dc.titleThe Kinematics of High Proper Motion Halo White Dwarfs
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