2000ApJ...541..126M


Query : 2000ApJ...541..126M

2000ApJ...541..126M - Astrophys. J., 541, 126-133 (2000/September-3)

Strong Balmer lines in old stellar populations: no need for young ages in ellipticals?

MARASTON C. and THOMAS D.

Abstract (from CDS):

Comparing models of Simple Stellar Populations (SSPs) with observed line strengths generally provides a tool for breaking the age-metallicity degeneracy in elliptical galaxies. Because of the wide range of Balmer line strengths observed, ellipticals have been interpreted as exhibiting an appreciable scatter in age. In this paper, we analyze Composite Stellar Population models with a simple mix of an old metal-rich and an old metal-poor component. We show that these models simultaneously produce strong Balmer lines and strong metallic lines without invoking a young population. The key to this result is that our models are based on SSPs that better match the steep increase of Hβ in metal-poor globular clusters than models in the literature. Hence, the scatter of Hβ observed in cluster and luminous field elliptical galaxies can be explained by a spread in the metallicity of old stellar populations. We check our model with respect to the so-called G-dwarf problem in ellipticals. For a galaxy subsample covering a large range in 1500-V colors, we demonstrate that the addition of an old metal-poor subcomponent does not invalidate other observational constraints like colors and the flux in the mid-UV.

Abstract Copyright:

Journal keyword(s): Galaxies: Abundances - Galaxies: Elliptical and Lenticular, cD - Galaxies: Formation - Galaxies: Fundamental Parameters - Galaxies: Stellar Content

Simbad objects: 22

goto Full paper

goto View the references in ADS

Number of rows : 22
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NGC 104 GlC 00 24 05.359 -72 04 53.20   5.78 4.09     ~ 3658 0
2 M 32 IG 00 42 41.825 +40 51 54.61 9.51 9.03 8.08     ~ 2049 2
3 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 11446 1
4 ACO S 373 ClG 03 38 30 -35 27.3           ~ 1632 0
5 NGC 1404 GiP 03 38 51.917 -35 35 39.81 11.53 10.69 10.00 9.03   ~ 687 1
6 NGC 1700 GiG 04 56 56.347 -04 51 56.64   12   11.14   ~ 333 1
7 NGC 3377 GiP 10 47 42.400 +13 59 08.30 11.55 11.24 10.38     ~ 736 1
8 M 105 LIN 10 47 49.600 +12 34 53.87   10.56 9.76 9.12 8.18 ~ 1400 0
9 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 6087 0
10 M 49 Sy2 12 29 46.798 +08 00 01.48   13.21 12.17     ~ 1994 2
11 NGC 4489 GiG 12 30 52.240 +16 45 31.31   13.2       ~ 242 0
12 M 60 GiP 12 43 40.008 +11 33 09.40   10.3       ~ 1278 0
13 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4388 2
14 M 53 GlC 13 12 55.25 +18 10 05.4   8.95 7.79     ~ 753 0
15 NAME Centaurus A Sy2 13 25 27.61509104 -43 01 08.8056025   8.18 6.84 6.66   ~ 4122 3
16 M 3 GlC 13 42 11.62 +28 22 38.2     6.39     ~ 2333 0
17 NGC 5831 GiG 15 04 07.024 +01 13 11.70   13.1   11.19   ~ 281 0
18 M 13 GlC 16 41 41.634 +36 27 40.75     5.8     ~ 2065 0
19 NGC 6388 GlC 17 36 17.461 -44 44 08.34   7.40       ~ 837 1
20 NGC 6441 GlC 17 50 13.06 -37 03 05.2   9.26 8.00     ~ 800 0
21 NGC 6702 G 18 46 57.5820964893 +45 42 20.301418496 15.30 14.73 13.05     ~ 133 0
22 NGC 7454 GiG 23 01 06.5111755176 +16 23 18.475417783   13.6       ~ 138 0

To bookmark this query, right click on this link: simbad:objects in 2000ApJ...541..126M and select 'bookmark this link' or equivalent in the popup menu


2021.09.23-23:07:26

© Université de Strasbourg/CNRS

    • Contact