Computer Science – Numerical Analysis
Scientific paper
Mar 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aj....107.1003c&link_type=abstract
Astronomical Journal (ISSN 0004-6256), vol. 107, no. 3, p. 1003-1017
Computer Science
Numerical Analysis
220
Astrophysics, Density Distribution, Gas Flow, Hydrodynamic Ram Effect, Hydrogen, Images, Morphology, Radial Distribution, Spiral Galaxies, Stripping (Distillation), Virgo Galactic Cluster, Viscous Flow, Angular Resolution, Estimates, Numerical Analysis, Quantitative Analysis, Very Large Array (Vla)
Scientific paper
In this paper we analyze the radial profiles of the neutral hydrogen surface density distribution of 17 bright spirals in the Virgo Cluster. The profiles were derived from images, which were obtained with the Very Large Array (VLA) and which have been presented in a previous paper (Cayatte et al., (1990)). Although the sample is still small, we can for the first time show, that different galaxies are affected differently by the cluster environment. We make a quantitative estimate of the importance of the different gas removal mechanisms for selected individual galaxies and compare these estimates with the observed H I morphology. In some galaxies ram-pressure stripping has done serious damage to the H I disks, while in other galaxies turbulent viscous stripping and thermal conductivity have caused a mild, but global H I deficiency across the entire disk. For our analysis we divide the galaxies into three groups according to the ration of H I to optical diameter, a fourth group contains the anemic galaxies. As it turns out a classification according to relative H I diameter helps to elucidate which gas removal processes play a role. Galaxies in different groups have many other properties in common, most importantly the projected distance from the cluster center. A comparison of the radial H I surface density profiles with those of field spirals of the same morphological type shows, that spirals in different groups are affected very differently by the environment. Galaxies with the smallest H I sizes have normal central surface densities and we suggest that these are the galaxies that are currently undergoing ram-pressure sweeping. The galaxies with only slightly smaller than usual H I diameters have a depressed H I surface density across the entire face of the galaxy. This is quite likely due to viscous stripping. One group is only very mildly affected, this could be caused by gravitational effects due to distant encounters.
Balkowski Ch.
Cayatte Veronique
Kotanyi C.
van Gorkom Jacqueline H.
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