J/ApJ/896/18 VLA imaging of obscured WISE+NVSS QSOs (Patil+, 2020)
High-resolution VLA imaging of obscured quasars: young radio jets caught in a
dense ISM.
Patil P., Nyland K., Whittle M., Lonsdale C., Lacy M., Lonsdale C.,
Mukherjee D., Trapp A.C., Kimball A.E., Lanz L., Wilkes B.J., Blain A.,
Harwood J.J., Efstathiou A., Vlahakis C.
<Astrophys. J., 896, 18 (2020)>
=2020ApJ...896...18P 2020ApJ...896...18P
ADC_Keywords: QSOs; Radio sources; Infrared sources
Keywords: Active galaxies; Quasars; Supermassive black holes;
Radio loud quasars; Radio jets; Radio telescopes; Galaxy evolution
Abstract:
We present new subarcsecond-resolution Karl G. Jansky Very Large Array
(VLA) imaging at 10GHz of 155 ultraluminous
(Lbol∼1011.7-1014.2L☉) and heavily obscured quasars with
redshifts z∼0.4-3. The sample was selected to have extremely red
mid-infrared-optical color ratios based on data from the Wide-Field
Infrared Survey Explorer (WISE) along with a detection of bright,
unresolved radio emission from the NRAO VLA Sky Survey (NVSS) or Faint
Images of the Radio Sky at Twenty cm Survey. Our high-resolution VLA
observations have revealed that the majority of the sources in our
sample (93 out of 155) are compact on angular scales <0.2 (≤1.7kpc at
z∼2). The radio luminosities, linear extents, and lobe pressures of
our sources are similar to young radio active galactic nuclei (e.g.,
gigahertz-peaked spectrum [GPS] and compact steep-spectrum [CSS]
sources), but their space density is considerably lower. Application
of a simple adiabatic lobe expansion model suggests relatively young
dynamical ages (∼104-7yr), relatively high ambient ISM densities
(∼1-104cm-3), and modest lobe expansion speeds (∼30-10000km/s).
Thus, we find our sources to be consistent with a population of newly
triggered, young jets caught in a unique evolutionary stage in which
they still reside within the dense gas reservoirs of their hosts.
Based on their radio luminosity function and dynamical ages, we
estimate that only ∼20% of classical large-scale FR I/II radio
galaxies could have evolved directly from these objects. We speculate
that the WISE-NVSS sources might first become GPS or CSS sources, of
which some might ultimately evolve into larger radio galaxies.
Description:
A detailed description of our sample selection is given in
Lonsdale+ (2015, J/ApJ/813/45). We obtained spectroscopic redshifts
for 71 out of 80 attempted sources using several telescopes.
We observed 167 sources from Lonsdale+ (2015, J/ApJ/813/45) at X band
(8-12GHz) with the VLA in the A- and B-arrays through projects 12B-127
and 12A-064, respectively.
The A-array observations were divided into 13 separate scheduling
blocks (SBs), and a total of 129 sources were observed between 2012
October and December. The B-array observations were divided into seven
different SBs, and 149 sources were observed from 2012 June to August.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tableb1.dat 75 155 Observational details of our sample
tablec1.dat 82 155 Beam sizes and source measurements
tablec2.dat 235 207 Source spatial measurements for the VLA A- and
B-array observations: results from JMFIT
tablec3.dat 59 91 Physical properties for our sample sources
with redshift available
tablee1.dat 43 25 List of extended sources
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See also:
VIII/65 : 1.4GHz NRAO VLA Sky Survey (NVSS) (Condon+ 1998)
II/311 : WISE All-Sky Data Release (Cutri+ 2012)
VIII/92 : The FIRST Survey Catalog, Version 2014Dec17 (Helfand+ 2015)
V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015)
J/MNRAS/204/151 : Bright radio sources at 178 MHz (3CRR) (Laing+ 1983)
J/A+A/363/887 : High frequency peakers. I. (Dallacasa+, 2000)
J/A+A/369/380 : CSS/GPS radio sources VLA observations (Fanti+, 2001)
J/MNRAS/346/627 : CENSORS (Combined EIS-NVSS Survey) catalog (Best+, 2003)
J/AJ/129/1198 : SDSS quasars in SWIRE ELAIS N1 field (Hatziminaoglou+, 2005)
J/AJ/133/186 : Opt. spectroscopy of 77 luminous AGNs and QSOs (Lacy+, 2007)
J/AN/330/223 : High frequency peakers: faint sample (Stanghellini+, 2009)
J/MNRAS/408/2261 : Compact steep spectra (Kunert-Bajraszewska+, 2010)
J/MNRAS/421/1569 : Properties of 18286 SDSS radio galaxies (Best+, 2012)
J/AJ/144/49 : Quasars from SDSS-DR7, WISE and UKIDSS surveys (Wu+, 2012)
J/ApJ/772/26 : AGN with WISE. II. The NDWFS Bootes field (Assef+, 2013)
J/ApJS/208/24 : Spitzer MIR AGN survey. I. (Lacy+, 2013)
J/MNRAS/445/955 : Radio-AGN feedback for 0.5<z<1 (Best+, 2014)
J/MNRAS/438/796 : Local radio-galaxy population at 20GHz (Sadler+, 2014)
J/ApJ/804/27 : NIR photometry of hot dust-obscured galaxies (Assef+, 2015)
J/ApJ/813/45 : ALMA observations in z∼0.5-3 quasars (Lonsdale+, 2015)
J/ApJ/805/90 : WISE ELIRGs and comparison with QSOs (Tsai+, 2015)
J/ApJ/818/105 : CNSS pilot survey (Mooley+, 2016)
J/MNRAS/458/2221 : ATLAS3D Project. XXXI (Nyland+, 2016)
J/A+A/598/A78 : The GMRT 150MHz all-sky radio survey (Intema+, 2017)
J/MNRAS/464/3882 : Mergers and galaxy-galaxy interactions (Weston+, 2017)
J/A+A/609/A1 : FR0CAT: FIRST catalog of FR0 radio galaxies (Baldi+, 2018)
J/ApJS/235/34 : Deep JVLA imaging of GOODS-N at 20cm (Owen, 2018)
Byte-by-byte Description of file: tableb1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- AName Abbreviated name used in this work (JHHMM+DD)
10- 27 A18 --- WISE WISE positional identifier
(HHMMSS.ss+DDMMSS.s; J2000)
29- 32 I4 yr ObsA.Y [2012]? Observation Year, A-array
34- 35 I2 "month" ObsA.M ? Observation Month, A-array
37- 38 I2 d ObsA.D ? Observation day in month, A-array
40- 41 I2 uJy/beam RMSA [13/97]? 1σ rms noise level,
A-array continuum image
43- 43 A1 --- l_SNA Limit flag on SN-A
45- 50 F6.1 --- SNA [3.5/2599.0]? Signal-to-noise, A-array
52- 53 A2 --- q_SNA Quality flag, A-array (1)
55- 58 I4 yr ObsB.Y [2012]? Observation Year, B-array
60- 61 I2 "month" ObsB.M [6/8]? Observation Month, B-array
63- 64 I2 d ObsB.D ? Observation day in month, B-array
66- 68 I3 uJy/beam RMSB [12/397]? 1σ rms noise level,
B-array continuum image
70- 73 I4 --- SNB [3/2142]? Signal-to-noise ration, B-array
75- 75 A1 --- q_SNB Quality flag, B-array (1)
--------------------------------------------------------------------------------
Note (1): Quality flags for the final continuum image as follows:
G = an image free of any artifacts or calibration issues;
ND = No detection;
P = Poor quality image due to bad calibration or phase closure errors;
F = Pipeline failed to calibrate uv-data.
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Byte-by-byte Description of file: tablec1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- AName Abbreviated name used in this work
10 A1 --- Array [AB] VLA array of the best continuum image
12- 13 A2 --- Morph Source morphology (2)
15- 17 F3.1 arcsec aA [0.2/1.5]? Major axis, synthesized beam,
A-array
19- 21 F3.1 arcsec bA [0.1/0.5]? Minor axis, synthesized beam,
A-array
23- 25 I3 deg PAA [-81/89]? Position angle, synthesized beam,
A-array, measured anti-clockwise from North
27- 31 F5.2 mJy/beam SpeakA [0.15/44.94]? X band (8-12GHz) peak flux
density of the A-array image
33- 36 F4.2 mJy/beam e_SpeakA [0.01/1.35]? Uncertainty in Speak-A
38- 42 F5.2 mJy StotA [0.18/45.1]? Integrated flux of source
A-array image
44- 47 F4.2 mJy e_StotA [0.02/1.35]? Uncertainty in Stot-A
49- 51 F3.1 arcsec aB [0.6/2.9]? Major axis, synthesized beam,
B-array
53- 55 F3.1 arcsec bB [0.4/0.9]? Minor axis, synthesized beam,
B-array
57- 60 I4 deg PAB [-180/87]? Position angle, synthesized
beam, B-array, measured anti-clockwise from
North
62- 66 F5.2 mJy/beam SpeakB [0.08/60.55]? X band (8-12GHz) peak flux
density of the B-array image
68- 71 F4.2 mJy/beam e_SpeakB [0.01/1.82]? Uncertainty in Speak-B
73- 77 F5.2 mJy StotB [0.16/60.66]? Integrated flux of source
B-array image
79- 82 F4.2 mJy e_StotB [0.04/4.52]? Uncertainty in Stot-B
--------------------------------------------------------------------------------
Note (2): Source morphology based on the criteria defined in Section 4.3.
Code as follows:
UR = Unresolved;
SR = Slightly resolved;
R = Fully resolved;
D = Double;
T = Triple;
M = Multi-component Sources.
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Byte-by-byte Description of file: tablec2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- AName Abbreviated name used in this work
10- 28 A19 --- WISE WISE positional identifier
30- 34 A5 --- Reg Region/Source component (1)
36- 37 I2 h RAh ? Hour of Right Ascension (J2000)
39- 40 I2 min RAm ? Minute of Right Ascension (J2000)
42- 47 F6.3 s RAs ? Second of Right Ascension (J2000)
49- 54 F6.2 arcsec dRA [-17/20]? Separation in arcseconds in RA
from Reg 1 (2)
56 A1 --- DE- Sign of the Declination (J2000)
57- 58 I2 deg DEd ? Degree of Declination (J2000)
60- 61 I2 arcmin DEm ? Arcminute of Declination (J2000)
63- 67 F5.2 arcsec DEs ? Arcsecond of Declination (J2000)
69- 73 F5.2 arcsec dDE [-9.6/8.4]? Separation in arcseconds in DE
from Reg 1 (2)
75 A1 --- l_aA0 Limit flag for aA0 (3)
77- 80 I4 mas aA0 [8/2870]? Deconvolved source size, major
axis (3)
82- 84 I3 mas e_aA0 [1/101]? Uncertainty in aA0 (3)
86 A1 --- l_bA0 Limit flag for bA0 (3)
88- 91 I4 mas bA0 [0/1160]? Deconvolved source size, minor
axis (3)
93- 94 I2 mas e_bA0 [0/91]? Uncertainty in aA0 (3)
96- 98 I3 deg PAA0 [0/180]? Deconvolved source position angle
(4)
100- 101 I2 deg e_PAA0 [0/78]? Uncertainty in PAA0 (4)
103- 107 F5.2 mJy/beam SpeakA [0.13/45]? Peak flux density of the
A-array source
109- 112 F4.2 mJy/beam e_SpeakA [0.01/1.4]? Uncertainty in SpeakA
114- 118 F5.2 mJy StotA [0.16/45.1]? Integrated flux of A-array
source
120- 123 F4.2 mJy e_StotA [0.02/1.4]? Uncertainty in StotA
125- 126 I2 h RABh ? Hour of Right Ascension (J2000)
128- 129 I2 min RABm ? Minute of Right Ascension (J2000)
131- 136 F6.3 s RABs ? Second of Right Ascension (J2000)
138- 143 F6.2 arcsec dRAB [-17/64]? Separation in arcseconds in RA
from Reg 1 (2)
145 A1 --- DEB- Sign of the Declination (J2000)
146- 147 I2 deg DEBd ? Degree of Declination (J2000)
149- 150 I2 arcmin DEBm ? Arcminute of Declination (J2000)
152- 156 F5.2 arcsec DEBs ? Arcsecond of Declination (J2000)
158- 163 F6.2 arcsec dDEB [-41.1/23.2]? Separation in arcseconds in
DE from Reg 1 (2)
165 A1 --- l_aB0 Limit flag for aB0 (3)
167- 171 I5 mas aB0 [0/23490]? Deconvolved source size, major
axis (3)
173- 176 I4 mas e_aB0 [2/1592]? Uncertainty in aB0 (3)
178 A1 --- l_bB0 Limit flag for bB0 (3)
180- 184 I5 mas bB0 [0/11210]? Deconvolved source size, minor
axis (3)
186- 188 I3 mas e_bB0 [2/353]? Uncertainty in bB0 (3)
190- 192 I3 deg PAB0 [0/180]? Deconvolved source position angle
(4)
194- 195 I2 deg e_PAB0 [0/71]? Uncertainty in PAB0 (4)
197- 201 F5.2 mJy/beam SpeakB [0.08/61]? Peak flux density of the
B-array source
203- 206 F4.2 mJy/beam e_SpeakB [0.01/2]? Uncertainty in SpeakB
208- 212 F5.2 mJy StotB [0.16/61]? Integrated flux of B-array
source
214- 217 F4.2 mJy e_StotB [0.03/4.5]? Uncertainty in StotB
219- 223 F5.2 --- alphaIB [-4.7/4.8]? In-band spectral index (5)
225- 228 F4.2 --- e_alphaIB [0/2]? Uncertainty in alphaIB
230- 235 I6 --- SN [3/2183]? Source detection signal-to-noise
ratio (6)
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Note (1): For a single component source, the entire component is named Reg 1.
For multi-component sources, brightest radio emission component is named
Reg 1.
Note (2): In case of sources with more than one component, a source separation
(in arcseconds) from the Reg 1 is provided.
Note (3): Deconvolved source sizes for the A-array data. If source is
resolved only along the major axis, the deconvolved minor axis is
specified as 0. In case of unresolved source, we provide an upper limit
on the major axis. A detailed description is provided in Section 4.2.
For extended sources with non-gaussian like emission, we provide the
size of 3σ contour as the angular size of the respective region.
Note (4): Position angle of the fitted gaussian, measured anti-clockwise
from North.
Note (5): In-band spectral index for the best image available. We used A-array
data when a good quality image is available.
Note (6): Source detection S/N averaged from the 8.6 and 11.4GHz images used
for calculating alphaIB.
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Byte-by-byte Description of file: tablec3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- AName Abbreviated name used in this work
10- 13 F4.2 --- z [0.3/2.85] Quasar redshift
15- 19 A5 --- Reg Region/Source component
21- 21 A1 --- l_amaj Upper limit flag on major axis (1)
23- 27 F5.1 kpc amaj [0.1/147.4] Linear size, major axis
29- 29 A1 --- l_bmin Upper limit flag on minor axis (1)
31- 34 F4.1 kpc bmin [0/70.3]? Linear size, minor axis
36- 40 F5.2 [W/Hz] logL1.4GHz [24.4/27.7]? log of rest-frame 1.4GHz
luminosity (2)
42- 46 F5.2 --- alpha [-2.1/0.5]? Spectral index, NVSS to
10GHz observations (3)
48- 51 F4.2 --- e_alpha [0.02/0.3]? Uncertainty on alpha
53- 53 A1 --- l_logPl Limit flag on logPl
55- 59 F5.2 [0.1Pa] logPl [-9.7/-3.3] log, Equipartition lobe
pressure, dyne/cm2 (Section 5.4)
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Note (1): For an unresolved source, we use an upper limit on the angular major
axis to estimate the limit on the source linear size.
Note (2): We use NVSS flux and the spectral index between NVSS and 10GHz
continuum observations to calculate the luminosity.
Note (3): Fluxes from all of the regions are added up to estimate the spectral
indices.
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Byte-by-byte Description of file: tablee1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- AName Abbreviated name used in this work
10- 11 A2 --- Morph1 Source Morphology, VLA-X (1)
13- 14 A2 --- Morph2 Source Morphology, VLASS (1)
16- 17 A2 --- Morph3 Source Morphology, FIRST (1)
19- 21 A3 --- Morph4 Source Morphology, TGSS (1)
23- 27 F5.2 arcsec Ang1 [0.02/46.1] Angular extent, VLA-X (2)
29- 32 F4.1 arcsec Ang2 [2.4/47] Angular extent, VLASS (2)
34- 37 F4.1 arcsec Ang3 [5.4/47.3]? Angular extent, FIRST (2)
39- 43 F5.1 arcsec Ang4 [12/153.1]? Angular extent, TGSS (2)
--------------------------------------------------------------------------------
Note (1): The morphological classes are as follows:
UR = unresolved;
SR = slightly or marginally resolved;
D = double;
T = triple;
M = multicomponent sources.
The detailed description of morphological classes is given in Section 4.3.
Note (2): Largest angular extent in arcseconds for the radio emission
detected in our 10GHz VLA survey, VLASS (VLA Sky Survey,
Lacy+ 2020PASP..132c5001L 2020PASP..132c5001L), FIRST (VIII/92), and TGSS (the GMRT Sky Survey,
Intema+ 2017A&A...598A..78I 2017A&A...598A..78I), respectively. For sources with a single
component emission, we provide angular size estimates from their
respective source catalogs. For multi-component sources, we provide
largest source separation measured manually using CASA task Viewer.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 29-Sep-2021