2010MNRAS.403.1175S


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.18CET06:34:05

2010MNRAS.403.1175S - Mon. Not. R. Astron. Soc., 403, 1175-1192 (2010/April-2)

Probing evolutionary mechanisms in galaxy clusters: neutral atomic hydrogen in Abell1367.

SCOTT T.C., BRAVO-ALFARO H., BRINKS E., CARETTA C.A., CORTESE L., BOSELLI A., HARDCASTLE M.J., CROSTON J.H. and PLAUCHU I.

Abstract (from CDS):

We present Very Large Array Hi imaging data for a field in the NW of the galaxy cluster Abell 1367 (z =0.02) in an attempt to probe the effect environment has on the interstellar medium of late-type spiral galaxies. Several galaxies, like CGCG 097-087, show pronounced tails and asymmetries, and seven out of 10 show significant, several kpc offsets between the Hi centroid and the optical. We compare our results against a sample of optically bright, late-type galaxies (spirals) across the central 1.5 Mpc of the cluster taken from the Arecibo Galaxy Environment Survey. We find that these late-type spirals are predominantly found in the northern half of the cluster, especially those that are relatively gas rich. We calculate the Hi deficiency and find that the expected global trend for the Hi deficiency of these spirals to increase with projected proximity to the cluster core, seen in clusters like Coma and Virgo, is not observed. We classified the spirals into four evolutionary states, with the galaxies in each state sharing a similar degree of Hi deficiency and optical colour. The common characteristics of the spirals in each evolutionary state suggest they have been subject to similar environmental processes. Many of the spirals in the most common evolutionary state (moderate Hi deficiency and blue colour) have an Hi intensity maximum which is displaced relative to its optical counterpart. The orientation of these offsets and magnitude of their Hi deficiencies together with data from other wavelengths provide observational evidence in support of varying degrees of ram pressure stripping and tidal interaction. In general, our results indicate that the Hi discs of bright late-type galaxies in the central part of the cluster are subject to both gas loss and morphological disturbance as a result of their interaction with the cluster environment. This provides further observational evidence of a more complex environment in Abell 1367 as compared to Virgo and Coma.

Abstract Copyright: © 2010 The Authors. Journal compilation © 2010 RAS

Journal keyword(s): galaxies: clusters: individual: Abell1367 - galaxies: evolution - galaxies: ISM

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 - 2021
#notes
1 NAME COMA SUPERCL SCG 11 23 +23.9           ~ 239 0
2 NGC 3821 GiG 11 42 09.071 +20 18 56.79 13.93 13.70 12.88     ~ 62 1
3 MCG+03-30-048 GiG 11 42 14.6142734385 +20 05 52.123569522   14.7   14.52   ~ 39 0
4 2MASX J11421476+1958350 GiG 11 42 14.766 +19 58 35.07   15.5   14.67   ~ 66 0
5 2MASX J11421561+2002550 GiC 11 42 15.623 +20 02 55.22   15.7       ~ 42 0
6 NVSS J114224+200711 rG 11 42 24.491 +20 07 09.46 14.59 14.55 13.84 13.53   ~ 119 1
7 MCG+03-30-055 GiG 11 42 45.201 +20 01 55.88   15.0   13.74   ~ 64 0
8 LEDA 36382 GiC 11 42 56.450 +19 57 58.37 15.85 16.25   15.27   ~ 90 0
9 SDSS J114258.69+195612.9 G 11 42 58.724 +19 56 13.00 19.15 19.39   18.45   ~ 4 0
10 UGC 6680 GiC 11 43 02.1530762471 +19 38 59.017235744   15.5       ~ 42 0
11 SDSS J114313.05+193646.9 GiC 11 43 13.054 +19 36 46.97           ~ 9 0
12 2MFGC 9193 GiC 11 43 13.096 +20 00 17.52 15.91 16.52   15.56   ~ 94 0
13 UGC 6683 GiG 11 43 16.2251618207 +19 44 55.425505647   15.42       ~ 32 1
14 IC 2951 GiG 11 43 24.5561793672 +19 44 59.338304206 15.38 14.98 13.55 13.43   ~ 56 1
15 UGC 6697 GiG 11 43 49.078 +19 58 06.46 13.96 14.35 13.59 13.29   ~ 200 2
16 2MASX J11435819+2011073 H2G 11 43 58.2414926105 +20 11 07.446082202 15.80 15.92   14.79   ~ 49 0
17 NGC 3840 H2G 11 43 58.9643701127 +20 04 37.306253441 14.87 14.89 13.84 13.58   ~ 109 1
18 MCG+03-30-071 GiG 11 44 01.882 +19 47 04.35 15.77 16.04   15.10   ~ 61 0
19 MCG+04-28-043 GiG 11 44 16.4920491936 +20 13 00.678530952 16.35 15.93   14.24   ~ 47 0
20 2MASX J11442587+2006098 GiG 11 44 25.9314469971 +20 06 09.552440787 17.52 17.22   15.60   ~ 25 0
21 ACO 1367 ClG 11 44 44.6 +19 41 59           ~ 1002 1
22 UGC 6719 AGN 11 44 47.054 +20 07 29.98 14.90 14.68 13.59 13.12   ~ 80 1
23 MCG+03-30-087 H2G 11 44 47.791 +19 46 24.29 16.22 16.53   15.45   ~ 69 0
24 MCG+03-30-085 GiC 11 44 47.9451128094 +19 41 18.512914570 16.70 16.45   14.99   ~ 27 0
25 NGC 3860 AGN 11 44 49.1689905748 +19 47 42.142765911 14.81 14.61   13.12   ~ 104 0
26 [SKV2002] K2 b ? 11 44 49.61 +19 46 04.0           ~ 3 0
27 [SKV2002] K2 a ? 11 44 50.61 +19 46 02.4           ~ 3 0
28 [SKV2002] K2 ? 11 44 50.81 +19 46 05.1           ~ 6 0
29 [SKV2002] Dw 2 GiC 11 44 51.094 +19 47 18.15 20.11 18.72   19.93   ~ 12 0
30 NGC 3859 H2G 11 44 52.2238101997 +19 27 15.272776251   14.9   13.80   ~ 89 0
31 2MASX J11445486+1946349 GiG 11 44 54.849 +19 46 35.28   15.4   14.14   ~ 70 0
32 3C 264.0 QSO 11 45 05.0090520 +19 36 22.741257   14.98 13.97     ~ 542 2
33 2MASX J11450658+2009229 GiC 11 45 06.5732441309 +20 09 23.122016912           ~ 10 0
34 MCG+03-30-094 AGN 11 45 06.995 +19 58 00.97   14.0   14.59   ~ 28 2
35 2MASX J11454468+2001518 GiG 11 45 44.689 +20 01 51.83   15.5   15.00   ~ 42 0
36 2MASX J11455306+1936408 GiC 11 45 53.068 +19 36 40.85           ~ 7 0
37 M 99 H2G 12 18 49.625 +14 24 59.36 10.45 10.44 9.87     ~ 784 2
38 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5949 0
39 NGC 4438 LIN 12 27 45.652 +13 00 30.92 11.37 11.02 10.17     ~ 584 3
40 NGC 4522 GiG 12 33 39.657 +09 10 29.54   13.6       ~ 331 0
41 NGC 4568 GiP 12 36 34.292 +11 14 19.07   12.11 11.19     ~ 348 2
42 M 90 Sy2 12 36 49.816 +13 09 46.33 10.56 10.26 9.54     ~ 809 1
43 NGC 4654 GiP 12 43 56.638 +13 07 34.86   11.8       ~ 507 1
44 NGC 4848 AGN 12 58 05.5774186519 +28 14 33.264194270   14.2   13.53   ~ 175 0
45 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4298 2

    Equat.    Gal    SGal    Ecl

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2021.01.18-06:34:05

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