J/MNRAS/489/5723 ASKAP HI imaging of the Lyon Group of Galaxies 351 (For+, 2019)
WALLABY early science - V.
ASKAP H I imaging of the Lyon Group of Galaxies 351.
For B.-Q., Staveley-Smith L., Westmeier T., Whiting M., Oh S.-H.,
Koribalski B., Wang J., Wong O.I., Bekiaris G., Cortese L., Elagali A.,
Kleiner D., Lee-Waddell K., Madrid J.P., Popping A., Rhee J.,
Reynolds T.N., Collier J.D., Phillips C.J., Voronkov M.A., Muller O.,
Jerjen H.
<Mon. Not. R. Astron. Soc., 489, 5723-5741 (2019)>
=2019MNRAS.489.5723F 2019MNRAS.489.5723F (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, radio ; Interferometry ; H I data ; Redshifts ;
Rotational velocities ; Photometry, infrared ;
Photometry, ultraviolet
Keywords: instrumentation: interferometer - galaxies: distances and redshifts -
galaxies: groups: general - galaxies: interactions -
galaxies: star formation
Abstract:
We present an HI study of the galaxy group LGG 351 using Widefield
ASKAP L-band Legacy All-sky Blind Survey (WALLABY) early science data
observed with the Australian Square Kilometre Array Pathfinder
(ASKAP). LGG 351 resides behind the M 83 group at a velocity range
(cz) of ∼3500-4800km/s within the rich Hydra-Centaurus overdensity
region. We detect 40 sources with the discovery of a tidally
interacting galaxy pair and two new HI sources that are not presented
in previous optical catalogues. 23 out of 40 sources have new
redshifts derived from the new HI data. This study is the largest
WALLABY sub-sample to date and also allows us to further validate the
performance of ASKAP and the data reduction pipeline ASKAPSOFT.
Extended HI emission is seen in six galaxies indicating interaction
within the group, although no HI debris is found. We also detect HI in
a known ultra-faint dwarf galaxy (dw 1328-29), which demonstrates that
it is not a satellite of the M 83 group as previously thought. In
conjunction with multiwavelength data, we find that our galaxies
follow the atomic gas fraction and baryonic Tully-Fisher scaling
relations derived from the GALEX Arecibo SDSS Survey. In addition,
majority of our galaxies fall within the star formation main sequence
indicating inefficiency of gas removal processes in this loose galaxy
group.
Description:
ASKAP is a radio interferometer (700-1800MHz) that consists of 36
antennas and has a bandwidth of ∼300MHz. Each antenna is 12m in
diameter and is equipped with a state-of-the-art MK II phased array
feed (PAF). ASKAP is designed to provide high angular and spectral
resolution as well as an instantaneous large field of view
(5.5°x5.5°) with 36 beams for achieving a fast survey speed
(Johnston et al. 2007PASA...24..174J 2007PASA...24..174J; Hotan et al.
2014PASA...31...41H 2014PASA...31...41H; McConnell et al. 2016PASA...33...42M 2016PASA...33...42M). An early
science program with 12 and, later, 16 MK II PAF-equipped antennas
(hereafter ASKAP-12) was conducted during 2016 October to 2018
January. The observations allow us to test the automated data
processing software, ASKAPSOFT, assess the data quality, and optimize
our data analysis and imaging techniques.
The M 83 field is one of four selected WALLABY early science phase 1
fields, with the majority of the observations taken using 12 antennas.
We perform source finding using SOFIA (Serra et al.
2015MNRAS.448.1922S 2015MNRAS.448.1922S) and obtain a catalogue of 40 HI sources. Among
these sources, two are new HI galaxies that do not have optical
identifications and one is a tidally interacting pair.
We adopt the 2MASS Ks-band to stellar mass relation to derive
stellar masses. We also calculate HI masses, HI deficiency parameters,
and rotational velocities. We derive the total SFRs of 34 galaxies
using NUV and MIR calibration, using archival GALEX data (Martin et
al. 2005ApJ...619L...1M 2005ApJ...619L...1M, Morrissey et al. 2007ApJS..173..682M 2007ApJS..173..682M) in the
Kepler field and WISE band-4 data (Wright et al. 2010AJ....140.1868W 2010AJ....140.1868W).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 130 40 Source catalogue and derived parameters
table5.dat 93 40 Photometry of sources and relevant derived
parameters
table6.dat 69 34 NUV and MIR photometries of sources and
associated star formation rate
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See also:
II/311 : WISE All-Sky Data Release (Cutri+ 2012)
II/312 : GALEX-DR5 (GR5) sources from AIS and MIS (Bianchi+ 2011)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- ID [1/40] Internal object identifier
4- 25 A22 --- Name Galaxy name (WALLABY JHHMMSS+DDMMSS)
27- 51 A25 --- OName Alternative galaxy name
53- 61 F9.5 deg RAdeg Right ascension (J2000) (1)
63- 71 F9.5 deg DEdeg Declination (J2000) (1)
73- 81 F9.4 MHz nuobs Detected central frequency of the source
83- 88 F6.4 --- z Redshift (2)
90- 93 I4 km/s Vopt Velocity in the optical frame (Vopt=cz)
95- 98 I4 km/s VCMB Recession velocity
100-103 F4.1 Mpc DH Hubble distance
105-108 F4.1 Mpc DL Luminosity distance
110-113 F4.1 10+19cm-2 NH 1σ HI column density sensitivity
115 A1 --- l_Sint Limit flag on Sint
117-123 F7.1 Jy.Hz Sint Integrated flux
125 A1 --- l_logMHI Limit flag on logMHI
127-130 F4.2 [Msun] logMHI Logarithm of the observed HI mass
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Note (1): The coordinates are based on the HI detection
Note (2): Redshift defined as z=(νrest-νobs)/νobs, where
νrest is HI rest frequency at 1420.405751MHz and νobs is
the observed frequency
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- ID [1/40] Internal object identifier
4- 25 A22 --- Name Galaxy name (WALLABY JHHMMSS+DDMMSS)
27- 32 F6.4 mag E(B-V) Galactic dust extinction
34- 39 F6.3 mag Ksmag ? 2MASS Ks-band magnitude
41- 45 F5.3 mag e_Ksmag ? Error on Ksmag
47- 51 F5.3 Jy FKs ? Intrinsic flux density in 2MASS Ks-band
53- 57 F5.2 10+9Lsun nuLnu ? Luminosity in 2MASS Ks-band
59- 62 F4.1 [Msun] logM* ? Logarithm of stellar mass
64- 69 A6 --- Morph Morphology retrieved from NED or SIMBAD
71- 74 F4.1 kpc d25 ? B-band optical isophotal diameter
measured at 25mag.arcsec-2 (1)
76- 80 F5.2 --- DEFHI ? HI deficiency (2)
82- 83 I2 deg i ? Inclination as given by minor/major
axial ratio to 3σ in 2MASS Ks-band
85- 89 F5.1 km/s w20c Corrected w20 linewidth provided by SoFiA
91- 93 I3 km/s Vrot ? Calculated rotational velocity from the
HI linewidth
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Note (1): d25=DLtan(B25,maj), where B25,maj is the homogenized major axis
from NED
Note (2): DEFHI is defined as the logarithmic difference between the expected
and observed HI masses of a galaxy,
DEFHI=log(MHI,exp/M☉)-log(MHI,obs/M☉)
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 22 A22 --- Name Galaxy name (WALLABY JHHMMSS+DDMMSS)
24- 28 F5.2 mag NUVmismag ? GALEX NUV AB magnitude obtained from the
Medium Imaging Survey (1)
30- 34 F5.2 mag NUVaismag ? GALEX NUV AB magnitude obtained from the
All-sky Imaging Survey (1)
36- 40 F5.2 mag W4mag ? WISE W4 (22um) band magnitude (1)
42- 45 F4.2 mag e_W4mag ? Error on W4mag
47- 50 F4.2 Msun/yr SFRNUV ? Calculated star formation rates based on
the NUV flux
52- 56 F5.2 Msun/yr SFRW4 ? Calculated star formation rates based on
the W4 flux
58 A1 --- l_SFR Limit flag on SFR
60- 64 F5.2 Msun/yr SFR Total star formation rate (SFR=SFRNUV+SFRW4)
66- 69 F4.2 Msun/yr e_SFR ? Error on SFR
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Note (1): Magnitudes have been corrected for the Galactic dust extinction
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 19-Jan-2023