2000MNRAS.315..184K


C.D.S. - SIMBAD4 rel 1.7 - 2020.02.27CET22:14:29

2000MNRAS.315..184K - Mon. Not. R. Astron. Soc., 315, 184-208 (2000/June-2)

The stellar populations of early-type galaxies in the Fornax cluster.

KUNTSCHNER H.

Abstract (from CDS):

We have measured central line strengths for a magnitude-limited sample of early-type galaxies in the Fornax cluster, comprising 11 elliptical (E) and 11 lenticular (S0) galaxies, more luminous than MB=-17. When compared with single-burst stellar population models we find that the centres of Fornax ellipticals follow a locus of fixed age and have metallicities varying roughly from half solar to twice solar. The centres of (lower luminosity) lenticular galaxies, however, exhibit a substantial spread to younger luminosity-weighted ages, indicating a more extended star formation history.

Galaxies with old stellar populations show tight scaling relations between metal-line indices and the central velocity dispersion. Remarkably also, the Fe lines are well correlated with σ0. Our detailed analysis of the stellar populations suggests that these scaling relations are driven mostly by metallicity. Galaxies with a young stellar component do generally deviate from the main relation. In particular, the lower luminosity S0s show a large spread.

Our conclusions are based on several age/metallicity diagnostic diagrams in the Lick/IDS system comprising established indices such as Mg2 and Hβ as well as new and more sensitive indices such as HγA and Fe3, a combination of three prominent Fe lines. The inferred difference in the age distribution between lenticular and elliptical galaxies is a robust conclusion, as the models generate consistent relative ages using different age and metallicity indicators, even though the absolute ages remain uncertain. The absolute age uncertainty is mainly caused by the effects of non-solar abundance ratios which are not yet accounted for by the stellar population models. Furthermore, we find that elliptical galaxies and the bulge of one bright S0 are overabundant in magnesium, where the most luminous galaxies show the strongest overabundances. The stellar populations of young and faint S0s are consistent with solar abundance ratios or a weak Mg underabundance. Two of the faintest lenticular galaxies in our sample have blue continua and extremely strong Balmer-line absorption, suggesting star formation <2Gyr ago.


Abstract Copyright: 2000, Royal Astronomical Society

Journal keyword(s): galaxies: abundances - galaxies: clusters: individual: Fornax - galaxies: elliptical and lenticular, cD - galaxies: formation - galaxies: kinematics and dynamics

Simbad objects: 41

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Number of rows : 41

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 * del Psc PM* 00 48 40.94433 +07 35 06.2926 7.83 5.95 4.44 3.27 2.40 K5-III 176 0
2 NGC 1316 GiP 03 22 41.789 -37 12 29.52 9.81 9.15 8.53 7.66   ~ 1178 1
3 NGC 1336 GiG 03 26 32.199 -35 42 48.86   13.12   11.95   ~ 103 0
4 ESO 358-6 GiG 03 27 18.048 -34 31 35.15   14.15   12.95   ~ 77 0
5 NGC 1339 GiG 03 28 06.582 -32 17 10.16   12.63   11.18   ~ 150 0
6 NGC 1351 GiG 03 30 34.983 -34 51 14.22   12.30   10.85   ~ 152 0
7 NGC 1373 GiP 03 34 59.208 -35 10 16.25 14.44 14.03 13.26     ~ 99 1
8 NGC 1374 GiP 03 35 16.598 -35 13 34.50 12.46 11.97 11.08 10.59   ~ 250 1
9 NGC 1375 GiG 03 35 16.8019706983 -35 15 56.379169010 13.50 13.02 12.40 11.74   ~ 136 1
10 IC 1963 GiG 03 35 31.029 -34 26 49.55   12.90   11.71   ~ 102 0
11 ESO 358-25 GiG 03 35 33.134 -32 27 53.55   13.90       ~ 73 0
12 NGC 1379 GiP 03 36 03.940 -35 26 28.23 12.17 12.04 10.91 10.60   ~ 236 1
13 NGC 1380 GiP 03 36 27.590 -34 58 34.68 11.32 10.94 9.93 9.37   ~ 368 1
14 NGC 1381 GiP 03 36 31.6595958424 -35 17 42.745665386 12.90 12.47 11.50 11.02   ~ 208 1
15 ESO 358-33 GiG 03 36 47.5025610434 -34 44 22.780563798 13.63 13.36 12.41 12.00   ~ 104 1
16 NGC 1399 BiC 03 38 29.083 -35 27 02.67 11.05 9.74 9.59 8.12   ~ 1435 1
17 ACO S 373 ClG 03 38 30 -35 27.3           ~ 1510 0
18 NGC 1404 GiP 03 38 51.917 -35 35 39.81 11.53 10.69 10.00 9.03   ~ 655 1
19 NGC 1419 GiG 03 40 42.120 -37 30 39.09   13.56   12.07   ~ 109 0
20 ESO 358-50 GiG 03 41 03.608 -33 46 45.51   13.86   12.57   ~ 58 0
21 NGC 1427 GiG 03 42 19.4447168502 -35 23 33.193682690   11.89   10.44   ~ 245 0
22 NGC 1428 GiG 03 42 22.9 -35 09 12   13.77   12.49   ~ 82 0
23 ESO 358-59 GiG 03 45 03.554 -35 58 21.37   14.08   12.85   ~ 92 0
24 ESO 359-2 GiG 03 50 36.723 -35 54 33.51   14.48   13.49   ~ 64 0
25 IC 2006 EmG 03 54 28.427 -35 58 01.75   12.39   10.94 11.9 ~ 194 0
26 * phi02 Ori PM* 05 36 54.3881859 +09 17 26.409553 5.70 5.04 4.09 3.33 2.78 G9.5IIIbFe-2.5 336 0
27 HD 40657 PM* 06 00 03.3497895029 -03 04 27.334050744 6.95 5.74 4.52 3.59 2.92 K1.5III-IIIbCN-1 62 0
28 * nu.02 CMa PM* 06 36 41.0375756 -19 15 21.165905 5.96 5.011 3.91 3.13 2.61 K1.5III-IVFe1 237 1
29 * 20 Mon PM* 07 10 13.6817668816 -04 14 13.582860775 6.73 5.95 4.92 4.13 3.61 K0III 130 0
30 * gam CMi SB* 07 28 09.7930317295 +08 55 31.907956790 7.26 5.73 4.30 3.19 2.40 K3-IIIFe-0.5 95 0
31 LAWD 25 WD* 07 40 20.7887176053 -17 24 49.155097204   13.36 13.061 12.886 12.70 DAZ6 179 0
32 * alf Mon PM* 07 41 14.8325688 -09 33 04.071083 5.83 4.95 3.93 3.16 2.64 G9.5III-IIIbFe-0.5 183 0
33 HD 66141 PM* 08 02 15.9365899 +02 20 04.452198 6.91 5.63 4.38 3.39 2.72 K2IIIbFe-0.5: 169 1
34 HD 71597 * 08 28 14.5571373588 +00 14 38.191885908   8.47 7.29     K1IV 42 0
35 * iot Hya PM* 09 39 51.3614457 -01 08 34.113491 6.68 5.23 3.91 2.92 2.25 K2.5III 164 0
36 GD 108 HS* 10 00 47.2462037648 -07 33 30.777365253 12.406 13.349 13.563 13.662 13.781 sdB 129 1
37 * lam Hya SB* 10 10 35.2885811545 -12 21 14.858923765 5.53 4.61 3.61 2.84 2.36 K0IIIbCN0.5 194 0
38 M 105 LIN 10 47 49.600 +12 34 53.87   10.56 9.76 9.12 8.18 ~ 1371 0
39 * alf Crt PM* 10 59 46.4648602 -18 17 55.617244 6.14 5.16 4.07 3.27 2.72 K0IIIb 197 0
40 * psi01 Aqr PM* 23 15 53.4952540919 -09 05 15.841221338 6.37 5.36 4.25 3.46 2.90 K1-IIIFe-0.5 215 1
41 HD 221148 PM* 23 29 32.0811959294 -04 31 57.881823844   7.34 6.25     K3-IIIbFe2 128 0

    Equat.    Gal    SGal    Ecl

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2020.02.27-22:14:29

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