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


Query : 2017A&A...604A..30N

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 - 2023
#notes
1 UGC 5 AGN 00 03 05.6532278352 -01 54 49.909114908   13.92 13.32 12.40 12.08 ~ 98 0
2 NGC 7819 GiG 00 04 24.495 +31 28 19.30   14.3       ~ 116 0
3 NGC 7824 GiP 00 05 06.2405943024 +06 55 12.496933380   14.5       ~ 56 0
4 NGC 1 GiP 00 07 15.8562637560 +27 42 29.020113144   13.4       ~ 107 0
5 NGC 160 G 00 36 04.0982272704 +23 57 28.502827092   13.7       ~ 87 0
6 NGC 234 EmG 00 43 32.3817530400 +14 20 33.397671804   13.5       ~ 116 0
7 NGC 257 GiG 00 48 01.5091790304 +08 17 49.505819100   13.7       ~ 81 0
8 IC 1683 GiG 01 22 38.867 +34 26 13.21   14.2       ~ 82 0
9 NGC 496 GiG 01 23 11.5872831672 +33 31 45.417105984   14.3       ~ 103 0
10 NGC 517 GiG 01 24 43.806 +33 25 46.54   13.6       ~ 64 0
11 NGC 1167 LIN 03 01 42.3322774176 +35 12 20.300948892   13.84 12.77     ~ 334 2
12 NGC 2253 G 06 43 14.6846186952 +65 40 38.950679568   15.0       ~ 56 0
13 NGC 2906 GiG 09 32 06.2228278920 +08 26 30.486567516   13.1       ~ 154 0
14 NGC 2916 Sy2 09 34 57.5933209584 +21 42 18.960584796 12.81 12.74 12.05     ~ 140 1
15 NGC 3106 LIN 10 04 05.2518653088 +31 11 07.659854232   14.0       ~ 93 0
16 NGC 4047 G 12 02 50.6855747352 +48 38 10.300035480   12.8       ~ 90 0
17 NGC 4470 H2G 12 29 37.8066943368 +07 49 27.284422224   12.9       ~ 224 0
18 NGC 4711 GiC 12 48 45.8623156056 +35 19 57.881064972   14.4       ~ 67 0
19 UGC 8234 GiG 13 08 46.5057756192 +62 16 18.162586956   13.8       ~ 46 0
20 NGC 5016 AGN 13 12 06.6662685192 +24 05 41.945286156   13.180 12.558 12.093 11.547 ~ 153 0
21 NGC 5520 GiP 14 12 22.8055823616 +50 20 54.479575320   13.3       ~ 119 0
22 NGC 5633 EmG 14 27 28.3616823288 +46 08 47.521403916   13.176 12.932 12.449 11.575 ~ 172 0
23 NGC 5732 G 14 40 38.9756466216 +38 38 16.358563788   14.4       ~ 69 0
24 UGC 9476 rG 14 41 32.0219639160 +44 30 45.962947872   13.59       ~ 92 0
25 NGC 5784 GiG 14 54 16.4510371920 +42 33 28.382514552   13.7       ~ 74 0
26 NGC 6060 GiG 16 05 51.9982696320 +21 29 05.766126036   14.3       ~ 94 0
27 NGC 6063 G 16 07 13.0021003512 +07 58 44.434838856   14.1       ~ 142 0
28 NGC 6081 LIN 16 12 56.8487186784 +09 52 01.414323552   14.4       ~ 61 0
29 NGC 6155 EmG 16 26 08.3352615552 +48 22 00.410482092   13.20       ~ 100 1
30 NGC 6301 GiG 17 08 32.7448601544 +42 20 20.859983448   14.6       ~ 61 0
31 NGC 6314 LIN 17 12 38.6880420672 +23 16 12.229407012 16.04 15.56 14.62 14.02 13.33 ~ 97 0
32 IC 1256 G 17 23 47.2869698760 +26 29 11.470994700   14.297 13.551 13.022 12.434 ~ 89 0
33 UGC 10905 LIN 17 34 06.4351060416 +25 20 38.250057372   14.6       ~ 42 0
34 NGC 7025 LIN 21 07 47.3404766136 +16 20 09.224408688   14.10       ~ 69 0
35 UGC 11717 LIN 21 18 35.4033052152 +19 43 07.475332980   15.1       ~ 41 0
36 NGC 7311 LIN 22 34 06.7905936096 +05 34 13.172695392   13.4       ~ 103 0
37 NGC 7364 rG 22 44 24.3715638768 -00 09 43.659115272   13.8       ~ 93 0
38 UGC 12224 G 22 52 38.3367927576 +06 05 37.218158628   15.30       ~ 74 0
39 NGC 7489 G 23 07 32.6813971224 +22 59 52.998974304   14.3       ~ 80 0
40 NGC 7623 GiG 23 20 30.0039351816 +08 23 44.814596208   13.9       ~ 81 0
41 NGC 7625 IG 23 20 30.132 +17 13 32.16 13.31 13.23 11.98 11.25   ~ 258 0
42 NGC 7653 LIN 23 24 49.3605599784 +15 16 32.129440788   12.06 11.91     ~ 92 1
43 NGC 7671 GiP 23 27 19.3401587400 +12 28 02.728494624   14.3       ~ 64 0
44 NGC 7683 GiG 23 29 03.8180030520 +11 26 42.645888420   14.60       ~ 57 0
45 NGC 7711 GiG 23 35 39.3728741856 +15 18 07.098903144   14.0       ~ 71 0

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2023.01.27-22:14:52

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