TY - JOUR
T1 - The influence of the cluster environment on the large-scale radio continuum emission of 8 Virgo cluster spirals
AU - Vollmer, B.
AU - Soida, M.
AU - Chung, A.
AU - Beck, R.
AU - Urbanik, M.
AU - Chyz̊y, K. T.
AU - Otmianowska-Mazur, K.
AU - Van Gorkom, J. H.
PY - 2010
Y1 - 2010
N2 - The influence of the environment on the polarized and total power radio continuum emission of cluster spiral galaxies is investigated. We present deep scaled array VLA 20 and 6 cm observations including polarization of 8 Virgo spiral galaxies. These data are combined with existing optical, Hi, and Hα data. Ram pressure compression leads to sharp edges of the total power distribution at one side of the galactic disk. These edges coincide with Hi edges. In edge-on galaxies the extraplanar radio emission can extend further than the Hi emission. In the same galaxies asymmetric gradients in the degree of polarization give additional information on the ram pressure wind direction. The local total power emission is not sensitive to the effects of ram pressure. The radio continuum spectrum might flatten in the compressed region only for very strong ram pressure. This implies that neither the local star formation rate nor the turbulent small-scale magnetic field are significantly affected by ram pressure. Ram pressure compression occurs mainly on large scales ($\ga$1 kpc) and is primarily detectable in polarized radio continuum emission.
AB - The influence of the environment on the polarized and total power radio continuum emission of cluster spiral galaxies is investigated. We present deep scaled array VLA 20 and 6 cm observations including polarization of 8 Virgo spiral galaxies. These data are combined with existing optical, Hi, and Hα data. Ram pressure compression leads to sharp edges of the total power distribution at one side of the galactic disk. These edges coincide with Hi edges. In edge-on galaxies the extraplanar radio emission can extend further than the Hi emission. In the same galaxies asymmetric gradients in the degree of polarization give additional information on the ram pressure wind direction. The local total power emission is not sensitive to the effects of ram pressure. The radio continuum spectrum might flatten in the compressed region only for very strong ram pressure. This implies that neither the local star formation rate nor the turbulent small-scale magnetic field are significantly affected by ram pressure. Ram pressure compression occurs mainly on large scales ($\ga$1 kpc) and is primarily detectable in polarized radio continuum emission.
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U2 - 10.1051/0004-6361/200913591
DO - 10.1051/0004-6361/200913591
M3 - Article
AN - SCOPUS:77950441861
SN - 0004-6361
VL - 512
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
IS - 5
M1 - A36
ER -