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Mass distribution of hot stellar sys...

Princeton University.

Mass distribution of hot stellar systems.

紀錄類型:	書目-電子資源 : Monograph/item
正題名/作者:	Mass distribution of hot stellar systems.
作者:	Wu, Xiaoan.
面頁冊數:	110 p.
附註:	Adviser: Scott Tremaine.
附註:	Source: Dissertation Abstracts International, Volume: 68-03, Section: B, page: 1682.
Contained By:	Dissertation Abstracts International68-03B.
標題:	Physics, Astronomy and Astrophysics.
電子資源:	http://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=3255851

Mass distribution of hot stellar systems.
Wu, Xiaoan.

Mass distribution of hot stellar systems. - 110 p.

Adviser: Scott Tremaine.

Thesis (Ph.D.)--Princeton University, 2007.

The mass distribution of hot stellar systems is hard to measure because they do not contain gas or star disks, and because there is a degeneracy between the overall mass distribution and the distribution function of the observable particles. Assuming that the potential is spherical, we describe a maximum-likelihood nonparametric method to utilize to the full extent available kinematic data, which is applied to an elliptical galaxy (M87), three dwarf spheroidal galaxies (Draco, Ursa Minor and Fornax) and a globular cluster (o Centauri). For M87, the mass within 32 kpc is (2:4 +/- 0:6) x 1012 M &odot; , and the exponent of the density profile rho &prop; r -alpha in the range 10 - 100 kpc is alpha = 1:6 +/- 0:4. The energy distribution suggests a few kinematically distinct groups of globular clusters. For dwarf spheroidal galaxies, our models naturally produce the so-called "extra-tidal extensions", which had previously been suggested as evidence of tidal stripping. The average V-band mass-to-light ratio is 400 +/- 80M &odot; =LV, &odot; within 0:75 kpc for Draco, 580+140-100 M &odot; =V, &odot; within 1:1 kpc for Ursa Minor and 25+7-5 M &odot; =LV, &odot; within 2:5 kpc for Fornax. We do not find that anisotropy contributes substantially to the high mass-to-light ratios in these dSph galaxies. For o Centauri, we derive an averaged (V -band) mass-to-light ratio Gamma = 2:96 +/- 0:10 M &odot; /L &odot; . Moreover, we find no evidence that the even part of the DF is dependent on total angular momentum; that is, two-integral models in which the DF depends on energy and the z'-component of angular momentum are sufficient to fit the data.Subjects--Topical Terms:

227131
Physics, Astronomy and Astrophysics.

Mass distribution of hot stellar systems.
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