2005ApJ...632..217S


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.18CET06:25:56

2005ApJ...632..217S - Astrophys. J., 632, 217-226 (2005/October-2)

Secular evolution via bar-driven gas inflow: results from BIMA SONG.

SHETH K., VOGEL S.N., REGAN M.W., THORNLEY M.D. and TEUBEN P.J.

Abstract (from CDS):

We present an analysis of the molecular gas distributions in the 29 barred and 15 unbarred spirals in the BIMA CO (J=1-0) Survey of Nearby Galaxies (SONG). For galaxies that are bright in CO, we confirm the conclusion by Sakamoto et al. that barred spirals have higher molecular gas concentrations in the central kiloparsec. The SONG sample also includes 27 galaxies below the CO brightness limit used by Sakamoto et al. Even in these less CO-bright galaxies we show that high central gas concentrations are more common in barred galaxies, consistent with radial inflow driven by the bar. However, there is a significant population of early-type (Sa-Sbc) barred spirals (6 of 19) that have no molecular gas detected in the nuclear region and have very little out to the bar corotation radius. This suggests that in barred galaxies with gas-deficient nuclear regions, the bar has already driven most of the gas within the bar corotation radius to the nuclear region, where it has been consumed by star formation. The median mass of nuclear molecular gas is over 4 times higher in early-type bars than in late-type (Sc-Sdm) bars. Since previous work has shown that the gas consumption rate is an order of magnitude higher in early-type bars, this implies that the early types have significantly higher bar-driven inflows. The lower accretion rates in late-type bars can probably be attributed to the known differences in bar structure between early and late types. Despite the evidence for bar-driven inflows in both early and late Hubble-type spirals, the data indicate that it is highly unlikely for a late-type galaxy to evolve into an early type via bar-induced gas inflow. Nonetheless, secular evolutionary processes are undoubtedly present, and pseudobulges are inevitable; evidence for pseudobulges is likely to be clearest in early-type galaxies because of their high gas inflow rates and higher star formation activity.

Abstract Copyright:

Journal keyword(s): Galaxies: Evolution - Galaxies: Nuclei - Galaxies: Spiral - Galaxies: Starburst - Galaxies: Structure - ISM: Molecules

Simbad objects: 44

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Number of rows : 44

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 M 74 G 01 36 41.772 +15 47 00.46 10.52 10.00 9.46 9.16   ~ 1447 1
2 NGC 925 H2G 02 27 16.913 +33 34 43.97   10.69 10.12 9.55   ~ 704 1
3 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 4161 2
4 IC 342 SBG 03 46 48.514 +68 05 45.98   10.5       ~ 1399 1
5 NGC 2403 AGN 07 36 51.396 +65 36 09.17 9.31 8.84 8.38 8.19   ~ 1631 1
6 NGC 2841 LIN 09 22 02.655 +50 58 35.32 10.43 10.09 9.22     ~ 999 1
7 NGC 2905 H2G 09 32 10.111 +21 30 02.99 10.44 9.75 9.07 8.68   ~ 1002 3
8 NGC 2976 GiP 09 47 15.458 +67 54 58.97 11.77 11.03 10.16 9.51   ~ 594 1
9 M 81 Sy2 09 55 33.17306143 +69 03 55.0609270   7.89 6.94     ~ 4027 5
10 NGC 3180 GiG 10 18 16.985 +41 25 27.77   10.4       ~ 642 0
11 NGC 3344 EmG 10 43 31.150 +24 55 19.99 10.38 10.54 9.86 9.71   ~ 347 1
12 M 95 GiP 10 43 57.733 +11 42 13.00 10.71 10.51 9.73 9.48   ~ 959 2
13 M 96 GiP 10 46 45.744 +11 49 11.78 10.42 10.15 9.25 8.99   ~ 751 1
14 NGC 3521 LSB 11 05 48.5676206040 -00 02 09.228156576 10.06 9.83 9.02 10.1 9.6 ~ 717 2
15 M 66 GiP 11 20 15.026 +12 59 28.64 9.85 9.65 8.92     ~ 1185 4
16 NGC 3726 GiG 11 33 21.1357515876 +47 01 45.260627622   11.11   10.02   ~ 328 0
17 NGC 3938 GiG 11 52 49.453 +44 07 14.63 10.80 10.90 10.38     ~ 473 1
18 NGC 3953 GiG 11 53 49.0087614111 +52 19 36.473777126   11.08   9.71   ~ 319 0
19 M 109 GiG 11 57 35.984 +53 22 28.27   10.94   9.57   ~ 424 0
20 NGC 4051 Sy1 12 03 09.6098828919 +44 31 52.693714606   11.08 12.92 9.94   ~ 2021 1
21 M 106 Sy2 12 18 57.620 +47 18 13.39   9.14 8.41 8.11   ~ 2151 3
22 M 61 Sy2 12 21 54.9275149050 +04 28 25.588335799 10.07 10.18 9.65     ~ 888 2
23 M 100 AGN 12 22 54.9318850854 +15 49 20.294302163 10.04 10.05 9.35     ~ 1676 2
24 NGC 4414 GiG 12 26 27.089 +31 13 24.76 11.12 10.96 10.12     ~ 520 2
25 NGC 4450 LIN 12 28 29.634 +17 05 05.82   10.90 10.08     ~ 514 1
26 NGC 4490 GiP 12 30 36.368 +41 38 37.07 10.03 10.22 9.79     ~ 533 3
27 NGC 4535 H2G 12 34 20.310 +08 11 51.94   11.1       ~ 532 0
28 M 91 LIN 12 35 26.430 +14 29 46.75   14.63 13.57     ~ 533 0
29 NGC 4559 H2G 12 35 57.6399424116 +27 57 35.859639262   10.46 10.01     ~ 546 1
30 M 90 Sy2 12 36 49.816 +13 09 46.33 10.56 10.26 9.54     ~ 809 1
31 M 58 SyG 12 37 43.597 +11 49 05.12 10.80 10.48 9.66     ~ 982 2
32 NGC 4699 GiG 12 49 02.186 -08 39 51.49   10.8   10.01 10.3 ~ 191 0
33 NGC 4725 Sy2 12 50 26.5692916552 +25 30 02.737610391   13.45 12.44     ~ 630 2
34 M 94 SyG 12 50 53.148 +41 07 12.55 9.15 8.96 8.24 7.78   ~ 1239 3
35 M 64 SyG 12 56 43.696 +21 40 57.57   9.36 8.52     ~ 830 2
36 NGC 5005 GiP 13 10 56.312 +37 03 32.19   14.67 13.67     ~ 504 2
37 NGC 5033 Sy1 13 13 27.535 +36 35 37.14   11.01 12.03 9.73   ~ 806 3
38 M 63 LIN 13 15 49.2738527699 +42 01 45.726078017   9.34 8.59 8.35   ~ 1086 2
39 M 51 GiP 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 3867 4
40 NGC 5248 GiG 13 37 32.069 +08 53 06.22   11.4       ~ 451 0
41 NGC 5247 GiG 13 38 03.0179394007 -17 53 02.635368748   10.77   9.96 10.5 ~ 204 0
42 M 101 GiP 14 03 12.583 +54 20 55.50   8.46 7.86 7.76   ~ 2586 2
43 NGC 6946 H2G 20 34 52.332 +60 09 13.24   10.5       ~ 2281 2
44 NGC 7331 LIN 22 37 04.102 +34 24 57.31 10.65 10.35 9.48     ~ 1125 2

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2021.01.18-06:25:56

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