J/A+A/659/A94 HI-detected Coma and field galaxies properties (Molnar+, 2022)
The Westerbork Coma Survey.
A blind, deep, high-resolution HI survey of the Coma cluster.
Molnar D.Cs., Serra P., van der Hulst T., Jarrett T.H., Boselli A.,
Cortese L., Healy J., de Blok E., Cappellari M., Hess K.M., Jozsa G.I.G.,
McDermid R.M., Oosterloo T.A., Verheijen M.A.W.
<Astron. Astrophys. 659, A94 (2022)>
=2022A&A...659A..94M 2022A&A...659A..94M (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies ; H I data
Keywords: galaxies: clusters: general - galaxies: interactions -
galaxies: evolution - radio lines: galaxies - galaxies: star formation
Abstract:
We present the blind Westerbork Coma Survey probing the HI content of
the Coma galaxy cluster with the Westerbork Synthesis Radio Telescope.
The survey covers the inner ∼1Mpc around the cluster centre,
extending out to 1.5Mpc towards the south-western NGC 4839 group. The
survey probes the atomic gas in the entire Coma volume down to a
sensitivity of ∼1019cm-2 and 108M☉.
Combining automated source finding with source extraction at optical
redshifts and visual verification, we obtained 40 HI detections of
which 24 are new. Over half of the sample displays perturbed HI
morphologies indicative of an ongoing interaction with the cluster
environment. With the use of ancillary UV and mid-IR, data we measured
their stellar masses and star formation rates and compared the HI
properties to a set of field galaxies spanning a similar stellar mass
and star formation rate range. We find that ∼75% of HI-selected Coma
galaxies have simultaneously enhanced star formation rates (by
∼0.2dex) and are HI deficient (by ∼0.5dex) compared to field galaxies
of the same stellar mass. According to our toy model, the simultaneous
HI deficiency and enhanced star formation activity can be attributed
to either HI stripping of already highly star forming galaxies on a
very short timescale, while their H2 content remains largely
unaffected, or to HI stripping coupled to a temporary boost of the
HI-to-H2 conversion, causing a brief starburst phase triggered by
ram pressure before eventually quenching the galaxy.
Description:
The survey consists of 24 individual WSRT pointings observed
throughout June 2012 using the Multi-Frequency-Frontends.
We use SoFiA (Serra et al., 2015MNRAS.448.1922S 2015MNRAS.448.1922S; Westmeier et al.,
2021MNRAS.506.3962W 2021MNRAS.506.3962W) to find HI sources in the two mosaic cubes.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
wcshidet.dat 182 40 Coma cluster galaxies with HI-detections in the
Westerbork Coma Survey
refsamp.dat 132 192 Reference sample of field galaxies
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Byte-by-byte Description of file: wcshidet.dat
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Bytes Format Units Label Explanations
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1- 22 A22 --- ID ID of optical counterpart
24- 41 F18.14 deg RAdeg Right Ascension (J2000)
43- 60 F18.15 deg DEdeg Declination (J2000)
62- 73 F12.9 arcsec off Angular offset between the
optical and HI source centres
75- 91 F17.11 km/s vHI line-of-sight velocity of
the HI detection
93- 98 F6.1 Mpc dc projected distance to the centre
of the Fornax cluster
100-103 F4.2 km/s voff difference between the optical and
HI line-of-sight velocities
105-110 F6.3 [Msun] logMstar stellar mass of the galaxy (1)
112-116 F5.3 [Msun] e_logMstar stellar mass uncertainty of the galaxy
118-136 F19.16 [Msun/yr] logSFR star formation rate of the galaxy (2)
138-156 F19.17 [Msun/yr] e_logSFR star formation rate uncertainty
of the galaxy
158-174 F17.15 [Msun] logMHI HI mass of the galaxy (3)
176 I1 --- HItype [0/3] HI morphological type (4)
178 I1 --- Tail [0/1] flag indicating a tail at UV
and/or Halpha wavelengths (5)
180 I1 --- AGN [0/1] flag indicating the presence of
an AGN (6)
182 I1 --- NewDet [0/1] flag to indicate whether the
source is a new HI detection (7)
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Note (1): calculated with the use of WISE 3.4 and 4.6 micron photometry
(extracted by T.H. Jarrett), with the method described in Cluver et al
(2014ApJ...782...90C 2014ApJ...782...90C). For details see Sect. 3.3 of the paper.
Note (2): calculated with the combination of GALEX NUV and WISE 22 micron
photometry with the coefficient of Boquien et al. (2016A&A...591A...6B 2016A&A...591A...6B).
For details see Sect. 3.3 of the paper.
Note (3): measured in our WSRT cubes. For details on the observations,
source detection, counterpart matching and verification, see Sect. 2
of the paper.
Note (4): HI morphological class of the galaxy. Details of the
classification method are described in Sect. 3.1 of the paper.
Classes as follows:
1 = settled
2 = one-sided asymmetry
3 = unsettled
Note (5): tailed sources from Smith et al. (2010MNRAS.408.1417S 2010MNRAS.408.1417S)
and Yagi et al. (2010AJ....140.1814Y 2010AJ....140.1814Y).
0 = no tail observed or was not covered by either studies
1 = has tail according to either surveys
Note (6): AGN hosts based on Mahajan et al. (2010MNRAS.404.1745M 2010MNRAS.404.1745M,
Cat. J/MNRAS/404/1745), Gavazzi et al. (2011A&A...534A..31G 2011A&A...534A..31G,
Cat. J/A+A/534/A31), or Toba et al. (2014ApJ...788...45T 2014ApJ...788...45T, Cat. J/ApJ/788/45)
0 = not identified as an AGN host
1 = found to harbour an AGN
Note (7): previously detected HI sources from Bravo-Alfaro et al.
(2000AJ....119..580B 2000AJ....119..580B), Bravo-Alfaro et al. (2001A&A...379..347B 2001A&A...379..347B),
or Gavazzi et al. (2006A&A...449..929G 2006A&A...449..929G, Cat. J/A+A/449/929)
0 = has been detected before
1 = newly detected source
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Byte-by-byte Description of file: refsamp.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- ID ID from the HRS or VGS (1)
8- 16 F9.5 deg RAdeg Right Ascension (J2000)
18- 26 F9.5 deg DEdeg Declination (J2000)
28- 45 F18.15 [Msun] logMstar Stellar mass of the galaxy (2)
47- 65 F19.17 [Msun] e_logMstar Stellar mass uncertainty of the galaxy
67- 79 F13.10 [Msun/yr] logSFR Star formation rate of the galaxy (3)
81- 91 F11.9 [Msun/yr] e_logSFR Star formation rate uncertainty of the
galaxy
93-110 F18.15 [Msun] logMHI HI mass of the galaxy (4)
112-132 F21.19 [Msun] e_logMHI HI mass uncertainty of the galaxy
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Note (1): adopted from Boselli et al. (2010PASP..122..261B 2010PASP..122..261B, Cat. J/PASP/122/261,
HRS) and Kreckel et al. (2011AJ....141....4K 2011AJ....141....4K, VGS)
Note (2): calculated with the use of WISE 3.4 and 4.6 micron photometry
(extracted by T.H. Jarrett), with the method described in Cluver et al.
(2014ApJ...782...90C 2014ApJ...782...90C). For details see Sect. 3.3 of the paper.
Note (3): calculated with the combination of GALEX NUV and WISE 22 micron
photometry with the coefficient of Boquien et al. (2016A&A...591A...6B 2016A&A...591A...6B).
For details see Sect. 3.3 of the paper.
Note (4): For HRS sources HI masses are from Boselli et al.
(2014A&A...564A..65B 2014A&A...564A..65B, Cat. J/A+A/564/A65).
For VGS HI observations are dominantly ALFALFA measurements from
Haynes et al. (2011AJ....142..170H 2011AJ....142..170H, Cat. J/AJ/142/170) and single-dish data
from Springob et al. (2005ApJS..160..149S 2005ApJS..160..149S, Cat. VIII/77).
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Acknowledgements:
Daniel Cs. Molnar, daniel.molnar(at)inaf.it
(End) Patricia Vannier [CDS] 28-Dec-2021