J/A+A/640/A22 Jellyfish galaxy JO201 JVLA datacube (Ramatsoku+, 2020)
GASP XXVI. HI gas in jellyfish galaxies. The case of JO201 and JO206.
Ramatsoku M., Serra P., Poggianti B.M., Moretti A., Gullieuszik M.,
Bettoni D., Deb T., Franchetto A., van Gorkom J.H., Jaffe Y., Tonnesen S.,
Verheijen M.A.W., Vulcani B., Andati L.A.L., de Blok E., Jozsa G.I.G.,
Kamphuis P., Kleiner D., Maccagni F.M., Makhathini S., Molnar D.Cs.,
Ramaila A.J.T., Smirnov O., Thorat K.
<Astron. Astrophys. 640, A22 (2020)>
=2020A&A...640A..22R 2020A&A...640A..22R (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Radio lines
Keywords: galaxies: star formation - galaxies: clusters: intracluster medium -
radio lines: galaxies
Abstract:
We present HI observations of the jellyfish galaxy, JO201, a massive
galaxy falling along the line-of-sight towards the centre of a rich
cluster, A85 at a high velocity. Its Hα emission shows a ∼40kpc
tail confined closely to its stellar disc and a ∼100kpc tail
extending further out. We find HI emission coinciding only with the
shorter clumpy Hα tail while no HI emission is detected along
the ∼100kpc Ha tail. In total, we measure an HI mass of
MHI=1.65x10+9M☉, which is about 60% lower than expected
based on its stellar mass and stellar surface density. We compared
JO201 to another jellyfish in the GASP sample, JO206, and find that
they are similarly HI-deficient. The global star formation rate (SFR)
analysis of JO201 suggests that its observed SFR would be expected if
it had 10x its current HI mass. The disc is the main contributor of
the high star formation efficiency at a given HI gas density for both
galaxies, but their tails also show higher star formation efficiencies
compared to the outer regions of field galaxies. Generally, we find
that JO201 and JO206 are similar based on their HI content, stellar
mass and star formation rate. This finding is unexpected considering
their different environments. A toy model comparing the ram pressure
of the ICM versus the restoring forces of these galaxies suggests that
the ram pressure strength exerted on them could be comparable if we
consider their 3D orbital velocities and radial distances relative to
the clusters.
Description:
The HI data were obtained from observations with the JVLA,
project code VLA/17A-293 (PI: B. Poggianti). JO201 was observed in
July 2017 for a total of 16 hours on source and 4 hours on
calibrators. The observations were conducted in the C-configuration
resulting in an angular resolution of 1500. They covered a total
bandwidth of 32MHz, centred at 1360.2103MHz, which was divided into
1024 channels of width 31.25kHz each (6.56km/s for HI at z=0).
Objects:
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RA (2000) DE Designation(s)
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00 41 30.30 -09 15 45.98 JO201 = [PFO2016] JO201
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 121 1 Information on fits datacube
fits/* . 1 Fits datacube
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 21 I2 --- Nx Number of pixels along X-axis
23- 24 I2 --- Ny Number of pixels along Y-axis
26- 27 I2 --- Nz Number of slices
29- 49 A21 "datime" Obs.date Observation date
51- 61 E11.6 m/s bVELO-HEL Lower value of VELO-HEL interval
63- 73 E11.6 m/s BVELO-HEL Upper value of VELO-HEL interval
75- 81 F7.2 m/s dVELO-HEL VELO-HEL resolution
83- 85 I3 Kibyte size Size of FITS file
87-103 A17 --- FileName Name of FITS file, in subdirectory fits
105-121 A17 --- Title Title of the FITS file
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Acknowledgements:
Mpati Ramatsoku, mpati.ramatsoku(at)inaf.it
(End) Patricia Vannier [CDS] 21-Jul-2020