|
| | | | |
| | | |
| Stat |
Members: 3645
Articles: 2'501'711
Articles rated: 2609
19 April 2024 |
|
| | | | |
|
Article overview
| |
|
|
The Atlas3D project - XX. Mass-size and Mass-sigma projections of the Virial Plane of early-type galaxies: variation of morphology, kinematics, mass-to-light ratio and stellar initial mass function | | Michele Cappellari
; Richard M. McDermid
; Katherine Alatalo
; Leo Blitz
; Maxime Bois
; Frederic Bournaud
; M. Bureau
; Alison F. Crocker
; Roger L. Davies
; Timothy A. Davis
; P. T. de Zeeuw
; Pierre-Alain Duc
; Sadegh Khochfar
; Davor Krajnovic
; Harald Kuntschner
; Raffaella Morganti
; Thorsten Naab
; Tom Oosterloo
; Marc Sarzi
; Nicholas Scott
; Paolo Serra
; Anne-Marie Weijmans
; Lisa M. Young
; | | Date: |
17 Aug 2012 | | Abstract: | In the companion Paper XIX we derive accurate total (M/L)_JAM within a sphere
of radius r=Re, as well as stellar (M/L)_stars for the volume-limited Atlas3D
sample of 260 early-type galaxies. Here we study the two projections
(M_JAM,sigma_e) and (M_JAM,R_e^max) of the thin Virial Plane
(VP)(M_JAM,sigma_e,R_e^max) which describes the distribution of the galaxy
population. The distribution of galaxy properties on both projections of the VP
is characterized by (i) a boundary in the galaxy distribution, described by two
power-laws, joined by a break at a characteristic mass M_JAM ~ 3*10^10 Msun,
which corresponds to the minimum Re and maximum stellar density, and (ii) a
characteristic mass M_JAM ~ 2*10^11 Msun which separates a population dominated
by fast rotator with disks at lower masses, from one dominated by quite round
slow rotators at larger masses. The distribution of ETGs properties on the two
projections of the VP tends to be constant along lines of constant sigma_e, and
forms a continuous and parallel sequence with the distribution of spiral
galaxies. This applies to the dynamical (M/L)_JAM and to other indicators of
the (M/L)_pop of the stellar population, like Hbeta and colour, as well as to
galaxy concentration, which we show is tracing the bulge mass. A similar
variation along contours of sigma_e is also observed for the stellar Initial
Mass Function (IMF), which was recently shown to vary systematically within the
ETGs galaxy population. Our preferred relation has the form log
[(M/L)_stars/(M/L)_Salp] = a + b*log (sigma_e/130kms) with a=-0.11+/-0.01 and
b=0.36+/-0.06. This trend implies a transition of the mean IMF from Kroupa to
Salpeter in the interval log(sigma_e) ~ 1.9-2.4, with a smooth variation in
between. [Abridged] | | Source: | arXiv, 1208.3523 | | Services: | Forum | Review | PDF | Favorites | |
|
|
No review found.
Did you like this article?
Note: answers to reviews or questions about the article must be posted in the forum section.
Authors are not allowed to review their own article. They can use the forum section.
browser Mozilla/5.0 AppleWebKit/537.36 (KHTML, like Gecko; compatible; ClaudeBot/1.0; +claudebot@anthropic.com)
|
| |
|
|
|
|
News, job offers and information for researchers and scientists:
| |
REGISTER