2008MNRAS.389..341M

Query : 2008MNRAS.389..341M

2008MNRAS.389..341M - Mon. Not. R. Astron. Soc., 389, 341-363 (2008/September-1)

Stellar populations of bulges in 14 cluster disc galaxies.

MORELLI L., POMPEI E., PIZZELLA A., MENDEZ-ABREU J., CORSINI E.M., COCCATO L., SAGLIA R.P., SARZI M. and BERTOLA F.

Abstract (from CDS):

Photometry and long-slit spectroscopy are presented for 14 S0 and spiral galaxies of the Fornax, Eridanus and Pegasus cluster, and NGC 7582 group. The structural parameters of the galaxies are derived from the R-band images by performing a two-dimensional photometric decomposition of the surface brightness distribution. This is assumed to be the sum of the contribution of a bulge and disc component characterized by elliptical and concentric isophotes with constant (but possibly different) ellipticity and position angles. The rotation curves and velocity dispersion profiles are measured from the spectra obtained along the major axis of galaxies. The radial profiles of the Hβ, Mg and Fe line-strength indices are presented too. Correlations between the central values of Mg2, <Fe>, Hβ and σ are found. The age, metallicity and α/Fe enhancement of the stellar population in the centre and at the radius where bulge and disc give the same contribution to the total surface brightness are obtained using stellar population models with variable element abundance ratios. Three classes of bulges are identified. The youngest bulges (∼2 Gyr) with ongoing star formation, intermediate-age bulges (4-8 Gyr) have solar metallicity, and old bulges (∼10 Gyr) have high metallicity. Most of the sample bulges display solar α/Fe enhancement, no gradient in age and a negative gradient of metallicity. The presence of negative gradient in the metallicity radial profile favours a scenario with bulge formation via dissipative collapse. This implies strong inside-out formation that should give rise to a negative gradient in the α/Fe enhancement too. But, no gradient is measured in the [α/Fe] radial profiles for all the galaxies, except for NGC 1366. In this galaxy there is a kinematically decoupled component, which is younger than the rest of host bulge. It possibly formed by enriched material probably acquired via interaction or minor merging. The bulge of NGC 1292 is the most reliable pseudo-bulge of our sample. The properties of its stellar population are consistent with a slow build-up within a scenario of secular evolution.

Abstract Copyright: © 2008 The Authors. Journal compilation © 2008 RAS

Journal keyword(s): galaxies: abundances - galaxies: bulges - galaxies: evolution - galaxies: formation - galaxies: kinematics and dynamics - galaxies: stellar content

Simbad objects: 35

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Number of rows : 35
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 * eps Psc PM* 01 02 56.6083833328 +07 53 24.479451631 5.95 5.24 4.28 3.50 2.98 G9IIIbFe-2 170 0
2 * 25 Cet PM* 01 03 02.5369500840 -04 50 11.757188544   6.517 5.408     K0/1III 77 0
3 * nu. Psc * 01 41 25.8941428289 +05 29 15.401884416 7.36 5.81 4.44 3.38 2.67 K3III 248 0
4 * omi Psc PM* 01 45 23.6252151720 +09 09 27.902640312 5.90 5.22 4.26 3.53 3.04 G8III 174 0
5 NGC 1292 EmG 03 18 14.894 -27 36 37.19   12.75   11.78 12.2 ~ 105 0
6 NGC 1351 GiG 03 30 34.9598617824 -34 51 14.242996620   12.30   10.85   ~ 190 0
7 NGC 1366 Sy2 03 33 53.6940996096 -31 11 38.966332632   12.94   11.49   ~ 102 0
8 MCG-03-10-010 GiG 03 34 19.2696369192 -19 25 27.406986744   14.26   12.98   ~ 40 0
9 ACO S 373 ClG 03 38 29.4 -35 27 08           ~ 2029 0
10 NAME Eridanus ClG GrG 03 38 32.00 -22 18 51.0           ~ 200 0
11 MCG-06-09-018 GiG 03 41 03.6078361560 -33 46 45.297655572   13.86   12.57   ~ 95 0
12 NGC 1425 EmG 03 42 11.4831633240 -29 53 36.186684252   11.61   11.6 10.9 ~ 209 0
13 IC 1993 GiG 03 47 04.8369103704 -33 42 35.877997728   12.50   11.16 11.7 ~ 93 0
14 * 39 Eri PM* 04 14 23.6878980552 -10 15 22.620462156 7.18 6.07 4.90 4.01 3.44 K2III 121 0
15 * del Lep PM* 05 51 19.2960278488 -20 52 44.730655825 5.54 4.83 3.85 2.99 2.43 K0IIIbFe-1.5CH0.5 222 0
16 * nu.02 CMa PM* 06 36 41.0376788353 -19 15 21.169452656 5.96 5.011 3.91 3.13 2.61 K1.5III-IVFe1 282 1
17 * 17 Mon * 06 47 19.8301708488 +08 02 14.122870224 7.82 6.17 4.77 3.74 3.04 K4III 125 0
18 * 20 Mon PM* 07 10 13.6815026472 -04 14 13.585055244 6.73 5.95 4.92 4.13 3.61 K0III 162 0
19 * alf Mon PM* 07 41 14.8319734511 -09 33 04.077766984 5.83 4.95 3.93 3.16 2.64 G9.5III-IIIbFe-0.5 214 0
20 * G CMi PM* 08 02 15.9369212008 +02 20 04.458846354 6.91 5.63 4.38 3.39 2.72 K2IIIbFe-0.5: 206 1
21 * sig Hya * 08 38 45.4374492452 +03 20 29.166677783 6.91 5.63 4.43 3.54 2.98 K1III 148 0
22 ACO 1656 ClG 12 59 44.40 +27 54 44.9           ~ 5141 2
23 NGC 5267 LIN 13 40 39.9765450720 +38 47 38.639158116   14.3       ~ 59 0
24 * eta Sct PM* 18 57 03.6701923416 -05 50 46.734335232   5.904 4.818     K1-III 106 0
25 HD 180928 PM* 19 19 00.0959552544 -15 32 11.647331124 9.06 7.49 6.06 4.94 4.11 K4III 101 0
26 * 37 Aql * 19 35 07.2578540184 -10 33 37.593599760   6.213 5.120     G8.5IIIa 81 0
27 IC 5267 Sy2 22 57 13.572 -43 23 46.11   11.18 10.47 9.83 10.4 ~ 151 0
28 NGC 7515 GiG 23 12 48.6739160184 +12 40 45.584218812   14.0       ~ 50 0
29 NGC 7531 GiG 23 14 48.4576363992 -43 35 59.465701536   11.99 11.26 12.1 11.7 ~ 156 0
30 NGC 7557 GiP 23 15 39.7623297912 +06 42 29.924345880   15.0       ~ 43 0
31 NAME NGC 7582 Group GrG 23 18 54.6 -42 18 28           ~ 11 0
32 IC 5309 GiG 23 19 11.638 +08 06 33.58   15.0       ~ 132 0
33 NAME Peg Cluster ClG 23 20 14.7 +08 12 23           ~ 131 0
34 NGC 7631 GiG 23 21 26.6685629592 +08 13 03.560510496   13.8       ~ 160 0
35 NGC 7643 GiG 23 22 50.3808345024 +11 59 19.843143756   14.8       ~ 53 0

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