Mon. Not. R. Astron. Soc., 487, 4580-4591 (2019/August-3)
GASP - XVII. H I imaging of the jellyfish galaxy JO206: gas stripping and enhanced star formation.
RAMATSOKU M., SERRA P., POGGIANTI B.M., MORETTI A., GULLIEUSZIK M., BETTONI D., DEB T., FRITZ J., VAN GORKOM J.H., JAFFE Y.L., TONNESEN S., VERHEIJEN M.A.W., VULCANI B., HUGO B., JOZSA G.I.G., MACCAGNI F.M., MAKHATHINI S., RAMAILA A., SMIRNOV O. and THORAT K.
Abstract (from CDS):
We present VLA H I observations of JO206, a prototypical ram-pressure-stripped galaxy in the GASP sample. This massive galaxy (M* = 8.5 x 1010 M☉) is located at a redshift of z = 0.0513, near the centre of the low-mass galaxy cluster, IIZw108 (σ ∼ 575 km s–1). JO206 is characterized by a long tail (>=90 kpc) of ionized gas stripped away by ram pressure. We find a similarly long H I tail in the same direction as the ionized gas tail and measure a total H I mass of 3.2 x 109 M☉. This is about half the expected H I mass given the stellar mass and surface density of JO206. A total of 1.8 x 109 M☉ (60 per cent) of the detected H I is in the gas-stripped tail. An analysis of the star formation rate shows that the galaxy is forming more stars compared to galaxies with the same stellar and H I mass. On average we find an H I gas depletion time of ∼0.5 Gyr which is about four times shorter than that of 'normal' spiral galaxies. We performed a spatially resolved analysis of the relation between star formation rate density and gas density in the disc and tail of the galaxy at the resolution of our H I data. The star formation efficiency of the disc is about 10 times higher than that of the tail at fixed H I surface densities. Both the inner and outer parts of JO206 show an enhanced star formation compared to regions of similar H I surface density in field galaxies. The enhanced star formation is due to ram-pressure stripping during the galaxy's first infall into the cluster.
© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
galaxies: clusters: intracluster medium
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