Query : 2012A&A...544A..99W

2012A&A...544A..99W - Astronomy and Astrophysics, volume 544A, 99-99 (2012/8-1)

Tidal interaction vs. ram pressure stripping effects as seen in X-rays. Hot gas in group and cluster galaxies.


Abstract (from CDS):

Cluster and group spiral galaxies are very often affected by their environment. The hot intracluster/intragroup medium (ICM/IGM) and a high galaxy density can lead to perturbations of the galactic interstellar medium (ISM) due to ram pressure and/or tidal interaction effects. In radio polarimetry observations, both phenomena may manifest similar features. X-ray data can help to determine the real origin of the perturbation. We analyse the distribution and physical properties of the hot gas in the Virgo cluster spiral galaxies NGC4254 and NGC4569, which indicate that the cluster environment has had a significant influence on their properties. By performing both spatial and spectral analyses of X-ray data, we try to distinguish between two major phenomena: tidal and ram pressure interactions. We compare our findings with the case of NGC2276, in which a shock was reported, by analysing XMM-Newton X-ray data for this galaxy. We use archival XMM-Newton observations of NGC4254, NGC4569, and NGC2276. Maps of the soft diffuse emission in the energy band 0.2-1keV are obtained. For the three galaxies, especially at the position of magnetic field enhancements we perform a spectral analysis to derive gas temperatures and thus to look for shock signatures. A shock is a signature of ram pressure resulting from supersonic velocities; weak tidal interactions are not expected to influence the temperature of the ionized gas. In NGC4254, we do not observe any temperature increase at the position of the bright polarized radio ridge. This suggests that the feature is formed by tidal interactions, and not by ram pressure stripping. NGC4569 shows a higher temperature at the position of the polarized features, which may be indicative of ram-pressure effects. For NGC2276, we do not find clear indications of a shock. Although ram-pressure effects seem to be visible, the main driver of the observed distortions is most likely tidal interaction. Determining gas temperatures via sensitive X-ray observations at the position of polarized radio ridges seems to be a good method for distinguishing between ram pressure and tidal interaction effects acting upon a galaxy.

Abstract Copyright:

Journal keyword(s): galaxies: groups: general - galaxies: clusters: individual: Virgo - galaxies: groups: individual: NGC 2300 - galaxies: clusters: general

Simbad objects: 8

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Number of rows : 8
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
1 NGC 2276 IG 07 27 14.485 +85 45 16.20   12.3       ~ 366 0
2 NGC 2300 IG 07 32 20.486 +85 42 31.90   12.2       ~ 331 0
3 NAME NGC 2300 Group GrG 07 32 22.84 +85 42 26.3           ~ 55 0
4 M 99 H2G 12 18 49.625 +14 24 59.36 10.45 10.44 9.87     ~ 887 2
5 NAME Virgo Cluster ClG 12 26 32.1 +12 43 24           ~ 6510 0
6 M 87 AGN 12 30 49.42338414 +12 23 28.0436859 10.16 9.59 8.63   7.49 ~ 7025 3
7 IC 3583 GiG 12 36 43.558 +13 15 32.93   13.31       ~ 173 1
8 M 90 Sy2 12 36 49.8009839880 +13 09 46.523813040 10.56 10.26 9.54     ~ 881 1

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