J/A+A/665/A155 AGES HI sources in Abell 1367 field (Deshev+, 2022)
The Arecibo Galaxy Environment Survey (AGES).
XI. The expanded Abell 1367 field: Data catalogue and HI census over the
surveyed volume.
Deshev B., Taylor R., Minchin R., Scott T.C., Brinks E.
<Astron. Astrophys. 665, A155 (2022)>
=2022A&A...665A.155D 2022A&A...665A.155D (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; H I data
Keywords: surveys - ISM: atoms - galaxies: evolution -
galaxies: clusters: individual: Abell 1367
Abstract:
Many galaxy properties are known to correlate with the environment in
which the galaxies are embedded. Their cold, neutral gas content,
usually assessed through 21cm HI observations, is related to many
other galaxy properties as it is the underlying fuel for star
formation. With its high sensitivity and broad sky coverage the blind
Arecibo Galaxy Environment Survey (AGES) survey brings significant
improvement to the census of HI properties of galaxies in a wide range
of environments, from voids to the core of a massive cluster. Here we
present an HI census over a volume of ∼44000Mpc3 towards the merging
cluster Abell 1367 and extending well beyond. Our aim is to measure
the effects different environments have on the HI content of their
constituent galaxies. We use AGES- a deep, blind, HI survey, with the
Arecibo radio telescope, 20 square degrees on the sky, centred on the
merging cluster Abell 1367 mapping the large-scale structure (LSS)
surrounding the cluster out to cz=20000km/s. The survey is sensitive
down to a column density of NHI=1.5x1017cm-2 for emission
filling the beam and a line width of 10km/s. As an approximate mass
sensitivity limit, a member of A1367 (at a distance of 92Mpc),
containing MHI=2.7x108M☉ distributed over a top-hat profile
of 50km/s width would be detected at 4σ. The results are
analysed in combination with optical spectroscopy data from SDSS which
we use to estimate the local galaxy density based on the
Voronoi-Delaunay method. We present the results of the complete AGES
survey of the A1367 field. In total we detect 457 HI sources, 213 of
which are detected for the first time by the AGES survey, 134 of which
are presented in this article for the first time. 225 of the
detections are in the cluster and 232 in the remaining volume
surveyed. Here we present the full catalogue of HI detections and
their basic properties, including optical ones. In this article we
concentrate on the difference between the cluster and the foreground
and background LSS. We reveal a lack of correlation of HI detected
fraction with local galaxy density when the cluster and the rest of
the surveyed volume are analysed separately. On the other hand the HI
detected fraction in the cluster is approximately half that found
outside the cluster.
Description:
The AGES used the seven-beam Arecibo L-Band Feed Array (ALFA)
instrument which has a hexagonal footprint on the sky. The FWHM of the
central beam is ∼3.3x3.8'.
Observations for the A1367 field were taken in April-May 2006, April
2007, November 2011, January-February 2012, May-June 2012, April-May
2013, December 2013, February-March 2015, May-June 2015, December 2016
- February 2017, June 2017, January-June 2018, and December 2018 -
February 2019. Observations were prioritised to begin with a central
5x1 degree strip centred on the main body of the Abell 1367 cluster.
These initial results were fully described in Cortese et al.
(2008MNRAS.383.1519C 2008MNRAS.383.1519C, Cat. J/MNRAS/383/1519).
Here we present the full 5x4 degree field, spanning
RA (11:33:32-11:54:39) and Dec (17:45:00-21:54:00).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 190 457 Full catalogue of HI detections and their
basic properties
--------------------------------------------------------------------------------
See also:
J/MNRAS/383/1519 : Abell 1367 HI sources from AGES (Cortese+, 2008)
J/AJ/140/1093 : AGES NGC7332/7339 & NGC 1156 HI sources (Minchin+, 2010)
J/MNRAS/415/1883 : AGES HI sources in NGC 7448 (Davies+, 2011)
J/MNRAS/423/787 : AGES sources in Virgo cluster (Taylor+, 2012)
J/MNRAS/443/2634 : AGES HI sources in NGC 7448 field (Taylor+, 2014)
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Jname HI object id (JHHMMSS+DDMMSS)
16- 17 I2 h RAh HI object central right ascension (J2000)
19- 20 I2 min RAm HI object central right ascension (J2000)
22- 26 F5.2 s RAs HI object central right ascension (J2000)
28- 30 F3.1 s e_RAs Uncertainty on right ascension
31 A1 --- DE- HI object declination sign (J2000)
32- 33 I2 deg DEd HI object declination (J2000)
35- 36 I2 arcmin DEm HI object declination (J2000)
38- 42 F5.2 arcsec DEs HI object declination (J2000)
44- 45 I2 arcsec e_DEs Uncertainty on Declination
47- 51 I5 km/s VHI Central velocity of HI source
53- 54 I2 km/s e_VHI Uncertainty on Vel_HI
56- 58 I3 km/s W50 HI profile width at 50% of peak
60- 61 I2 km/s e_W50 Uncertainty on W50
63- 65 I3 km/s W20 HI profile width at 10% of peak
67- 68 I2 km/s e_W20 Uncertainty on W20
70- 73 F4.1 mJy Fpeak Peak flux
75- 77 F3.1 mJy e_Fpeak Uncertainty on Peak Flux
79- 84 F6.3 Jy.km/s Ftot Total HI Flux
86- 90 F5.3 Jy.km/s e_Ftot Uncertainty on TotFlux
92- 96 F5.2 [Msun] logMHI Logarithm of total HI mass
98-101 F4.2 [Msun] e_logMHI Uncertainty on logMHI
103-108 F6.2 --- AASNR Signal-to-noise ratio
110-112 A3 --- flagHI HI detection flag (1)
114-132 I19 --- specObjID ?=-1 ID of primary optical counterpart
134-152 I19 --- specObjID2 ?=-1 ID of the second optical counterpart
154-163 F10.5 deg RAOdeg ?=-1 Right ascension of primary optical
counterpart (J2000)
165-174 F10.6 deg DEOdeg ?=-1 Declination of primary optical
counterpart (J2000)
176-180 I5 km/s VOpt ?=-1 Central velocity of primary optical
counterpart
182-190 A9 --- OCflag OCflag (potential or spectrosc)
--------------------------------------------------------------------------------
Note (1): HI detection flag as follows:
0 = certain
1 = uncertain
2 = multiple optical counterparts
3 = source at the edge of the cube
4 = resolved source
--------------------------------------------------------------------------------
Acknowledgements:
Boris Deshev, deshev(at)asu.cas.cz
References:
Auld et al., Paper I 2006MNRAS.371.1617A 2006MNRAS.371.1617A
Cortese et al., Paper II 2008MNRAS.383.1519C 2008MNRAS.383.1519C, Cat. J/MNRAS/383/1519
Minchin et al., Paper III 2010AJ....140.1093M 2010AJ....140.1093M, Cat. J/AJ/140/1093
Davies et al., Paper IV 2011MNRAS.415.1883D 2011MNRAS.415.1883D, Cat. J/MNRAS/415/1883
Taylor et al., Paper V 2012MNRAS.423..787T 2012MNRAS.423..787T, Cat. J/MNRAS/423/787
Taylor et al., Paper VI 2013MNRAS.428..459T 2013MNRAS.428..459T
Taylor et al., Paper VII 2014MNRAS.443.2634T 2014MNRAS.443.2634T, Cat. J/MNRAS/443/2634
Taylor et al., Paper VIII 2014MNRAS.442L..46T 2014MNRAS.442L..46T
Minchin et al., Paper IX 2016MNRAS.455.3430M 2016MNRAS.455.3430M
Keenan et al., Paper X 2016MNRAS.456..951K 2016MNRAS.456..951K
(End) Patricia Vannier [CDS] 22-Jun-2022