J/MNRAS/516/372 Radio galaxies and clusters from 150GHz TGSS (Bhukta+, 2022)
Tailed radio galaxies from the TIFR GMRT sky survey.
Bhukta N., Mondal S.K., Pal S.
<Mon. Not. R. Astron. Soc. 516, 372-390 (2022)>
=2022MNRAS.516..372B 2022MNRAS.516..372B (SIMBAD/NED BibCode)
ADC_Keywords: Radio sources ; Galaxies, radio ; Clusters, galaxy ; Photometry ;
Positional data ; Spectroscopy ; Redshifts ; References ;
Optical
Keywords: galaxies: active - galaxies: formation - galaxies: jets -
galaxies: kinematics and dynamics - radio continuum: galaxies
Abstract:
We present a list of tailed radio galaxies using the Tata Institute of
Fundamental Research (TIFR) Giant Metrewave Radio Telescope (GMRT) Sky
Survey Alternative Data Release 1 (TGSS ADR1) at 150 MHz. We visually
examined 5336 image fields and found 264 tailed radio galaxies. Tailed
radio galaxies are classified as wide-angle tailed (WAT) galaxies or
narrow-angle tailed (NAT) galaxies, based on the angle between the two
jets of the galaxy. Our sample of tailed radio galaxies included
203 WAT- and 61 NAT-type sources. These newly identified tailed
sources are significant additions to the list of known tailed radio
galaxies. The source morphology and luminosity features of the various
galaxies and their optical identifications are presented. Other radio
properties and general features of the sources are also discussed.
Description:
In study, we present classified WAT and NAT galaxy radio sources from
a visual inspection of the 150-MHz TGSS survey consisting of images of
a total of 5536 fields (see details examination procedures in section
2, section 4.3 Bending angle for object classification and TGSS images
server: http://tgssadr.strw.leidenuniv.nl/doku.php). Also we proceeded
to optical and IR counterparts identifications from WISE-Pan-STARRS
combined catalogue (see section 3) as well as radio counterparts
identifications with others previous studies as NVSS at 1.4GHz. For
WAT and NAT candidates, we provided table1.dat and table2.dat which
give positionnal, photometric and spectroscopic results from the two
previous sections.
As explained in section 4.4 Cluster association, we associated our
tailed radio galaxy sample with cluster catalogues from the literature
that cover the TGSS field. We performed a three-dimensional
cross-match with the known clusters across the field using a search
radius of 2 Mpc and assumed that galaxies and clusters are associated
if Δz = |z-zcluster| ≤ 0.005. These clusters have been
detected using various methods, including optical, IR, X-ray, and
Sunyaev-Zel'dovich (SZ) observations. Clusters physical properties and
parameters are listed in the table3.dat and table4.dat for WAT and NAT
galaxy radio sources respectively. Finally, we listed in table5.dat
the 22 known cluster catalogues used for our purpose.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 86 203 *Sample of our candidate wide-angle tail (WAT)
radio sources
table2.dat 83 61 *Sample of our candidate narrow-angle tail (NAT)
radio sources
table3.dat 98 89 Cluster parameters for our candidate wide-angle
tail (WAT) radio sources
table4.dat 98 29 Cluster parameters for our candidate
narrow-angle tail (NAT) radio sources
table5.dat 149 22 Details of various cluster surveys
--------------------------------------------------------------------------------
Note on table1.dat and table2.dat: Because optical/IR counterparts are more
compact than the corresponding radio galaxies, we used the positions of
optical/IR counterparts as the positions of these sources. For the remaining
four (1 per cent of the total detected sources) tailed radio sources, where
optical or IR counterparts are not available, a radio-morphology-based position
was used.
--------------------------------------------------------------------------------
See also:
J/MNRAS/406/2578 : Galaxies near S1189 (Mao+, 2010)
J/MNRAS/463/2997 : Lockman Hole low-frequency radio sources (Mahony+, 2016)
J/ApJS/194/31 : Morphology for groups in the FIRST database (Proctor, 2011)
J/ApJS/199/34 : Clusters of galaxies in SDSS-III (Wen+, 2012)
J/ApJS/259/31 : Head-tail radio galaxies from the VLA FIRST survey
(Sasmal+, 2022)
J/ApJS/167/1 : Galaxy groups and clusters from SDSS (Berlind+, 2006)
J/ApJ/807/178 : Newly rich galaxy clusters identified in SDSS-DR12
(Wen+, 2015)
J/ApJS/224/18 : Identify giant radio sources from the NVSS (Proctor, 2016)
J/AJ/148/75 : Bent-tailed radio galaxies Chandra Deep Field South
(Dehghan+, 2014)
J/AJ/154/169 : GMRT observations of head-tail radio galaxies
(Sebastian+, 2017)
J/AJ/141/88 : Galaxy cluster environments of radio sources (Wing+, 2011)
J/A+A/626/A8 : WATCAT. Wide-angle tailed radio galaxies (Missaglia+, 2019)
J/A+A/622/A1 : LOFAR Two-metre Sky Survey DR1 source catalog
(Shimwell+, 2019)
J/A+A/598/A78 : The GMRT 150MHz all-sky radio survey (Intema+, 2017)
VII/233 : 2MASS All-Sky Extended Source Catalog (XSC)
(IPAC-UMass, 2003-2006)
V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015)
II/349 : The Pan-STARRS release 1 (PS1) Survey - DR1 (Chambers+,2016)
II/311 : WISE All-Sky Data Release (Cutri+ 2012)
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
II/281 : 2MASS 6X Point Source Working Database / Catalog
(Cutri+ 2006)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- ID Identifier raw number (CatNo)
5- 14 A10 --- Name Name of the radio source as JHHMM±DDMM
(Name)
16- 17 I2 h RAh Right Ascension of the galaxy core (J2000)
(RAcore)
19- 20 I2 min RAm Right Ascension of the galaxy core (J2000)
(RAcore)
22- 26 F5.2 s RAs Right Ascension of the galaxy core (J2000)
(RAcore)
28 A1 --- DE- Declination sign (J2000)
29- 30 I2 deg DEd Declination of the galaxy core (J2000)
(DECcore)
32- 33 I2 arcmin DEm Declination of the galaxy core (J2000)
(DECcore)
35- 36 I2 arcsec DEs Declination of the galaxy core (J2000)
(DECcore)
38- 42 F5.2 arcsec Sep ? The separation angle between the radio and
optical position (Separation)
44- 47 F4.2 --- Rel ? The reliability of the counterpart as
described in section 3 (ρ)
49- 53 F5.2 Jy F150 The total flux density at 150 MHz from TGSS
ADR 1 survey (F150)
55- 58 F4.2 Jy F1400 ? The total flux density at 1400 MHz from
NVSS surveys (F1400)
60- 63 F4.2 --- alpha ? Spectral index between 150 MHz and
1400 MHz fluxes as defined by equation 1
of the section 4.1 (alpha1.40.15) (1)
65- 68 F4.2 --- z ? Redshift obtained by photometry or
spectroscopy (z)
70 A1 --- r_z Litterature reference of z (2)
72- 77 F6.2 10+25W/Hz L150 ? Radio luminosity of the galaxy computed
with redshift of optical counterpart and/or
of the galaxy cluster as described by the
equation 3 of the section 4.2 (L150)
79- 86 A8 --- Ref Reference surveys in which the source is
presented without identification as tailed
radio galaxy (OtherCatalogue) (3)
--------------------------------------------------------------------------------
Note (1): The uncertainty of spectral index measurements arising from flux
density uncertainty (Mahony et al. 2016MNRAS.463.2997M 2016MNRAS.463.2997M,
Cat. J/MNRAS/463/2997) as written in equation 2 of the section 4.1.
Then using this relation, the spectral index uncertainty is
Δα = 0.05.
Note (2): Litterature reference of the redshift z as follows:
a = Represents photometric redshift, 5 sources in our sample
b = Represents spectroscopic redshift, 34 sources in our sample
Note (3): List of reference surveys as follows:
1 = NVSS, Condon et al. 1998AJ....115.1693C 1998AJ....115.1693C, Cat. VIII/65
2 = VLSS, Cohen et al. 2007AJ....134.1245C 2007AJ....134.1245C, Cat. VIII/97A
and Lane et al. 2014MNRAS.440..327L 2014MNRAS.440..327L, Cat. VIII/97
3 = 4C, Pilkington & Scott 1965MmRAS..69..183P 1965MmRAS..69..183P, Cat. VIII/4,
Gower et al. 1967MmRAS..71...49G 1967MmRAS..71...49G, Cat. VIII/4 and
Caswell & Crowther 1969MNRAS.145..181C 1969MNRAS.145..181C
4 = 6C, Baan & McKee 1985A&A...143..136B 1985A&A...143..136B,
Hales et al. 1988MNRAS.234..919H 1988MNRAS.234..919H, Cat. VIII/21,
Hales et al. 1990MNRAS.246..256H 1990MNRAS.246..256H, Cat. VIII/22,
Hales et al. 1991MNRAS.251...46H 1991MNRAS.251...46H, Cat. VIII/23,
Hales et al. 1993MNRAS.263...25H 1993MNRAS.263...25H, Cat. VIII/25,
Hales et al. 1993MNRAS.262.1057H 1993MNRAS.262.1057H, Cat. VIII/24
5 = 7C, McGilchrist et al. 1990MNRAS.246..110M 1990MNRAS.246..110M, Cat. J/MNRAS/246/110
Kollgaard et al. 1994ApJS...93..145K 1994ApJS...93..145K, Cat. J/ApJS/93/145
Waldram et al. 1996MNRAS.282..779W 1996MNRAS.282..779W, Cat. J/MNRAS/282/779
Vessey & Green 1998MNRAS.294..607V 1998MNRAS.294..607V, Cat. J/MNRAS/294/607
6 = PMN, Griffith et al. 1994ApJS...90..179G 1994ApJS...90..179G, Cat. VIII/38
7 = PKS, Bolton et al. 1964AuJPh..17..340B 1964AuJPh..17..340B
8 = 87GB, Gregory & Condon 1991ApJS...75.1011G 1991ApJS...75.1011G, Cat. VIII/14
9 = B2, Colla et al. 1970A&AS....1..281C 1970A&AS....1..281C, Cat. VIII/36,
Colla et al. 1972A&AS....7....1C 1972A&AS....7....1C, Cat. VIII/36,
Colla et al. 1973A&AS...11..291C 1973A&AS...11..291C, Cat. VIII/36,
Fanaroff & Riley 1974MNRAS.167P..31F 1974MNRAS.167P..31F
10 = B3, Ficarra et al. 1985A&AS...59..255F 1985A&AS...59..255F, Cat. VIII/37
11 = VFK, Van Velzen et al. 2015MNRAS.446.2985V 2015MNRAS.446.2985V,
Cat. J/MNRAS/446/2985
12 = CRATES, Healey et al. 2007ApJS..171...61H 2007ApJS..171...61H, Cat. J/ApJS/171/61
13 = FIRST, Becker et al. 1995ApJ...450..559B 1995ApJ...450..559B
14 = SUMSS, Mauch et al. 2003MNRAS.342.1117M 2003MNRAS.342.1117M, Cat. VIII/78,
Cat. VIII/81, Cat. VIII/70
15 = 2MASS, Skrutskie et al. 2006AJ....131.1163S 2006AJ....131.1163S, Cat. VII/233
16 = MG2, Bennett et al. 1986ApJS...61....1B 1986ApJS...61....1B, Cat. VIII/52
17 = MRC, Large et al. 1981MNRAS.194..693L 1981MNRAS.194..693L, Cat. VIII/2
18 = SSTSL, Randall et al. 2012MNRAS.421.1644R 2012MNRAS.421.1644R, Cat. J/MNRAS/421/1644
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- ID Identifier raw number (CatNo)
4- 13 A10 --- Name Name of the radio source as JHHMM±DDMM
(Name)
15- 16 I2 h RAh Right Ascension of the galaxy core (J2000)
(RAcore)
18- 19 I2 min RAm Right Ascension of the galaxy core (J2000)
(RAcore)
21- 25 F5.2 s RAs Right Ascension of the galaxy core (J2000)
(RAcore)
27 A1 --- DE- Declination sign (J2000)
28- 29 I2 deg DEd Declination of the galaxy core (J2000)
(DECcore)
31- 32 I2 arcmin DEm Declination of the galaxy core (J2000)
(DECcore)
34- 35 I2 arcsec DEs Declination of the galaxy core (J2000)
(DECcore)
37- 41 F5.2 arcsec Sep The separation angle between the radio and
optical position (Separation)
43- 46 F4.2 --- Rel The reliability of the counterpart as
described in section 3 (ρ)
48- 52 F5.2 Jy F150 The total flux density at 150 MHz from TGSS
ADR 1 survey (F150)
54- 57 F4.2 Jy F1400 ? The total flux density at 1400 MHz from
NVSS surveys (F1400)
59- 62 F4.2 --- alpha ? Spectral index between 150 MHz and
1400 MHz fluxes as defined by equation 1
of the section 4.1 (alpha1.40.15) (1)
64- 67 F4.2 --- z ? Redshift obtained by photometry or
spectroscopy (z)
69 A1 --- r_z Litterature reference of z (2)
71- 75 F5.2 10+25W/Hz L150 ? Radio luminosity of the galaxy computed
with redshift of optical counterpart and/or
of the galaxy cluster as described by the
equation 3 of the section 4.2 (L150)
77- 83 A7 --- Ref Reference surveys in which the source is
presented without identification as tailed
radio galaxy (OtherCatalogue) (3)
--------------------------------------------------------------------------------
Note (1): The uncertainty of spectral index measurements arising from flux
density uncertainty (Mahony et al. 2016MNRAS.463.2997M 2016MNRAS.463.2997M,
Cat. J/MNRAS/463/2997) as written in equation 2 of the section 4.1.
Then using this relation, the spectral index uncertainty is
Δα = 0.05.
Note (2): Litterature reference of the redshift z as follows:
a = Represents photometric redshift, 5 sources in our sample
b = Represents spectroscopic redshift, 34 sources in our sample
Note (3): List of reference surveys as follows:
1 = NVSS, Condon et al. 1998AJ....115.1693C 1998AJ....115.1693C, Cat. VIII/65
2 = VLSS, Cohen et al. 2007AJ....134.1245C 2007AJ....134.1245C, Cat. VIII/97
and Lane et al. 2014MNRAS.440..327L 2014MNRAS.440..327L, Cat. VIII/97
3 = 4C, Pilkington & Scott 1965MmRAS..69..183P 1965MmRAS..69..183P, Cat. VIII/4,
Gower et al. 1967MmRAS..71...49G 1967MmRAS..71...49G, Cat. VIII/4 and
Caswell & Crowther 1969MNRAS.145..181C 1969MNRAS.145..181C
4 = 6C, Baan & McKee 1985A&A...143..136B 1985A&A...143..136B,
Hales et al. 1988MNRAS.234..919H 1988MNRAS.234..919H, Cat. VIII/21,
Hales et al. 1990MNRAS.246..256H 1990MNRAS.246..256H, Cat. VIII/22,
Hales et al. 1991MNRAS.251...46H 1991MNRAS.251...46H, Cat. VIII/23,
Hales et al. 1993MNRAS.263...25H 1993MNRAS.263...25H, Cat. VIII/25,
Hales et al. 1993MNRAS.262.1057H 1993MNRAS.262.1057H, Cat. VIII/24
5 = 7C, McGilchrist et al. 1990MNRAS.246..110M 1990MNRAS.246..110M, Cat. J/MNRAS/246/110
Kollgaard et al. 1994ApJS...93..145K 1994ApJS...93..145K, Cat. J/ApJS/93/145
Waldram et al. 1996MNRAS.282..779W 1996MNRAS.282..779W, Cat. J/MNRAS/282/779
Vessey & Green 1998MNRAS.294..607V 1998MNRAS.294..607V, Cat. J/MNRAS/294/607
6 = PMN, Griffith et al. 1994ApJS...90..179G 1994ApJS...90..179G, Cat. VIII/38
7 = PKS, Bolton et al. 1964AuJPh..17..340B 1964AuJPh..17..340B
8 = 87GB, Gregory & Condon 1991ApJS...75.1011G 1991ApJS...75.1011G, Cat. VIII/14
9 = B2, Colla et al. 1970A&AS....1..281C 1970A&AS....1..281C, Cat. VIII/36,
Colla et al. 1972A&AS....7....1C 1972A&AS....7....1C, Cat. VIII/36,
Colla et al. 1973A&AS...11..291C 1973A&AS...11..291C, Cat. VIII/36,
Fanaroff & Riley 1974MNRAS.167P..31F 1974MNRAS.167P..31F
10 = B3, Ficarra et al. 1985A&AS...59..255F 1985A&AS...59..255F, Cat. VIII/37
11 = VFK, Van Velzen et al. 2015MNRAS.446.2985V 2015MNRAS.446.2985V,
Cat. J/MNRAS/446/2985
12 = FIRST, Becker et al. 1995ApJ...450..559B 1995ApJ...450..559B
13 = SUMSS, Mauch et al. 2003MNRAS.342.1117M 2003MNRAS.342.1117M, Cat. VIII/78,
Cat. VIII/81B, Cat. VIII/70
14 = 2MASS, Skrutskie et al. 2006AJ....131.1163S 2006AJ....131.1163S, Cat. VII/233
15 = MG2, Bennett et al. 1986ApJS...61....1B 1986ApJS...61....1B, Cat. VIII/52
16 = MRC, Large et al. 1981MNRAS.194..693L 1981MNRAS.194..693L, Cat. VIII/2
17 = SSTSL, Randall et al. 2012MNRAS.421.1644R 2012MNRAS.421.1644R, Cat. J/MNRAS/421/1644
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- ID Identifier raw number (CatNo)
4- 13 A10 --- Name Name of the radio source as JHHMM±DDMM
(Name)
15- 36 A22 --- Cluster The parent galaxy cluster (Cluster)
38- 43 F6.2 --- zcl ? Redshift of the cluster (zcl)
45- 50 F6.1 Mpc Dc ? Comoving distance of the radio source
(Dc)
52- 56 F5.1 arcsec Theta The angular separation between the center
of the cluster and the radio galaxy source
(θ)
58- 64 F7.2 kpc D ? Linear distance of the radio galaxy
source from the cluster center (D)
66- 70 F5.2 mag rmag ? The r band magnitude of brightest
cluster galaxy member (mr) (1)
72- 75 F4.2 Mpc r500 ? Radius within which the mean density of
the cluster is 500 times that of the
critical density of the Universe called
ρc = 3H2(z)/8πG (r500) (1)
77- 82 F6.2 --- RL ? The cluster richness describing how many
member galaxies or how much mass the
cluster possesses (RL) (1)
84- 85 I2 --- N500 ? Number of member galaxy candidates are
within r500 (N500) (1)
87- 91 F5.2 10+14Msun M500 ? The cluster mass within r500 (M500)
(2)
93- 98 F6.2 1/Mpc3 rho ? Cluster density computed based above
parameters (ρ_co)
--------------------------------------------------------------------------------
Note (1): For the purposes of having a homogeneous study, various parameters
(mr, r200,N500,RL) of cluster were collected from Wen et al.
(2012ApJS..199...34W 2012ApJS..199...34W, Cat. J/ApJS/199/34) and Wen & Han
(2015ApJ...807..178W 2015ApJ...807..178W, Cat. J/ApJ/807/178).
Note (2): We calculated the cluster optical mass M500 from the cluster
richness RL (Wen & Han 2015ApJ...807..178W 2015ApJ...807..178W, Cat. J/ApJ/807/178),
which is strongly correlated as the equation 4 of the section 5.2
shows.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- ID Identifier raw number (SerialNumber)
4- 10 A7 --- CatName Name of the cluster catalogue (CatalogueName)
12- 24 A13 --- Band Observation bands (ObservationBand)
26- 27 I2 --- Nz ? The number of clusters with a redshift (Nz)
29 I1 --- N ? The number of clusters within the TGSS field
without a redshift (N)
31- 32 I2 --- Nt The total number of clusters (Nt)
34- 50 A17 --- Aut Author's names (Author)
52- 70 A19 --- BibCode Paper reference bibcode (BibCode)
72- 149 A78 --- Cat Catalog in Vizier (Catalogue)
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 11-Jul-2025