2017A&A...604A..30N


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.17CET10:00:34

2017A&A...604A..30N - Astronomy and Astrophysics, volume 604A, 30-30 (2017/8-1)

A combined photometric and kinematic recipe for evaluating the nature of bulges using the CALIFA sample.

NEUMANN J., WISOTZKI L., CHOUDHURY O.S., GADOTTI D.A., WALCHER C.J., BLAND-HAWTHORN J., GARCIA-BENITO R., GONZALEZ DELGADO R.M., HUSEMANN B., MARINO R.A., MARQUEZ I., SANCHEZ S.F., ZIEGLER B. (The CALIFA collaboration)

Abstract (from CDS):

Understanding the nature of bulges in disc galaxies can provide important insights into the formation and evolution of galaxies. For instance, the presence of a classical bulge suggests a relatively violent history. In contrast, the presence of an inner disc instead (also referred to as a "pseudobulge") indicates the occurrence of secular evolution processes in the main disc. However, we still lack criteria to effectively categorise bulges, limiting our ability to study their impact on the evolution of the host galaxies. Here we present a recipe to separate inner discs from classical bulges by combining four different parameters from photometric and kinematic analyses: the bulge Sersic index nb, the concentration index C20,50, the Kormendy (1977ApJ...217..406K) relation and the inner slope of the radial velocity dispersion profile ∇σ. With that recipe we provide a detailed bulge classification for a sample of 45 galaxies from the integral-field spectroscopic survey CALIFA. To aid in categorising bulges within these galaxies, we perform 2D image decomposition to determine bulge Sersic index, bulge-to-total light ratio, surface brightness and effective radius of the bulge and use growth curve analysis to derive a new concentration index, C20,50. We further extract the stellar kinematics from CALIFA data cubes and analyse the radial velocity dispersion profile. The results of the different approaches are in good agreement and allow a safe classification for approximately 95% of the galaxies. In particular, we show that our new "inner" concentration index performs considerably better than the traditionally used C50,90 when yielding the nature of bulges. We also found that a combined use of this index and the Kormendy relation gives a very robust indication of the physical nature of the bulge.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: bulges - galaxies: photometry - galaxies: kinematics and dynamics - galaxies: structure - galaxies: structure

Simbad objects: 45

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Number of rows : 45

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 UGC 5 AGN 00 03 05.6525922410 -01 54 49.915893585   13.92 13.32 12.40 12.08 ~ 85 0
2 NGC 7819 GiG 00 04 24.495 +31 28 19.30   14.3       ~ 101 0
3 NGC 7824 GiP 00 05 06.2406522424 +06 55 12.490046538   14.5       ~ 45 0
4 NGC 1 GiP 00 07 15.8554856380 +27 42 29.024562244   13.4       ~ 94 0
5 NGC 160 G 00 36 04.0981265430 +23 57 28.510460638   13.7       ~ 75 0
6 NGC 234 EmG 00 43 32.3816212175 +14 20 33.389672451   13.5       ~ 97 0
7 NGC 257 GiG 00 48 01.5094425149 +08 17 49.506328654   13.7       ~ 70 0
8 IC 1683 GiG 01 22 38.867 +34 26 13.21   14.2       ~ 67 0
9 NGC 496 GiG 01 23 11.618 +33 31 45.29   14.3       ~ 88 0
10 NGC 517 GiG 01 24 43.806 +33 25 46.54   13.6       ~ 53 0
11 NGC 1167 LIN 03 01 42.358 +35 12 20.34   13.84 12.77     ~ 285 2
12 NGC 2253 G 06 43 14.6852097640 +65 40 38.949836611   15.0       ~ 41 0
13 NGC 2906 GiG 09 32 06.247 +08 26 30.86   13.1       ~ 123 0
14 NGC 2916 Sy2 09 34 57.5939750994 +21 42 18.947459809 12.81 12.74 12.05     ~ 122 1
15 NGC 3106 LIN 10 04 05.2521409689 +31 11 07.659449395   14.0       ~ 75 0
16 NGC 4047 G 12 02 50.6873307305 +48 38 10.343981636   12.8       ~ 73 0
17 NGC 4470 H2G 12 29 37.8070254595 +07 49 27.286182613   12.9       ~ 191 0
18 NGC 4711 GiC 12 48 45.8621672335 +35 19 57.883605425   14.4       ~ 50 0
19 UGC 8234 GiG 13 08 46.5066023172 +62 16 18.148378960   13.8       ~ 36 0
20 NGC 5016 AGN 13 12 06.6702084873 +24 05 41.970504488   13.180 12.558 12.093 11.547 ~ 128 0
21 NGC 5520 GiP 14 12 22.8052932999 +50 20 54.474015371   13.3       ~ 98 0
22 NGC 5633 EmG 14 27 28.3609163671 +46 08 47.523613534   13.176 12.932 12.449 11.575 ~ 147 0
23 NGC 5732 G 14 40 38.994 +38 38 15.70   14.4       ~ 54 0
24 UGC 9476 rG 14 41 31.959 +44 30 45.39   13.59 12.95     ~ 72 0
25 NGC 5784 GiG 14 54 16.458 +42 33 27.97   13.7       ~ 57 0
26 NGC 6060 GiG 16 05 51.980 +21 29 05.94   14.3       ~ 79 0
27 NGC 6063 G 16 07 13.0017702658 +07 58 44.436124734   14.1       ~ 121 0
28 NGC 6081 LIN 16 12 56.850 +09 52 01.63   14.4       ~ 42 0
29 NGC 6155 EmG 16 26 08.3334871725 +48 22 00.416360731   13.20       ~ 88 1
30 NGC 6301 GiG 17 08 32.739 +42 20 20.86   14.6       ~ 48 0
31 NGC 6314 LIN 17 12 38.6893448746 +23 16 12.247289041 16.04 15.56 14.62 14.02 13.33 ~ 84 0
32 IC 1256 G 17 23 47.322 +26 29 11.45   14.297 13.551 13.022 12.434 ~ 78 0
33 UGC 10905 LIN 17 34 06.4348342631 +25 20 38.248227609   14.6       ~ 31 0
34 NGC 7025 LIN 21 07 47.329 +16 20 09.09   14.10       ~ 54 0
35 UGC 11717 LIN 21 18 35.376 +19 43 07.15   15.1       ~ 32 0
36 NGC 7311 LIN 22 34 06.760 +05 34 13.11   13.4       ~ 84 0
37 NGC 7364 rG 22 44 24.3708304089 -00 09 43.648311705   13.8       ~ 76 0
38 UGC 12224 G 22 52 38.291 +06 05 37.21   15.30       ~ 65 0
39 NGC 7489 G 23 07 32.6805868048 +22 59 52.984149095   14.3       ~ 70 0
40 NGC 7623 GiG 23 20 30.0035556734 +08 23 44.807404006   13.9       ~ 69 0
41 NGC 7625 IG 23 20 30.132 +17 13 32.16 13.31 13.23 11.98 11.25   ~ 238 0
42 NGC 7653 LIN 23 24 49.3611914459 +15 16 32.141943276   12.06 11.91     ~ 76 1
43 NGC 7671 GiP 23 27 19.329 +12 28 02.60   14.3       ~ 50 0
44 NGC 7683 GiG 23 29 03.809 +11 26 42.37   14.60       ~ 41 0
45 NGC 7711 GiG 23 35 39.404 +15 18 07.74   14.0       ~ 60 0

    Equat.    Gal    SGal    Ecl

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2019.11.17-10:00:34

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