J/A+A/648/A102 FR-type radio sources at 3GHz VLA-COSMOS (Vardoulaki+, 2021)
FR-type radio sources at 3 GHz VLA-COSMOS:
Relation to physical properties and large-scale environment.
Vardoulaki E., Jimenez Andrade E.F., Delvecchio I., Smolcic V.,
Schinnerer E., Sargent M.T., Gozaliasl G., Finoguenov A., Bondi M.,
Zamorani G., Badescu T., Leslie S.K., Ceraj L., Tisanic K., Karim A.,
Magnelli B., Bertoldi F., Romano-Diaz E., Harrington K.
<Astron. Astrophys. 648, A102 (2021)>
=2021A&A...648A.102V 2021A&A...648A.102V (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, radio ; Active gal. nuclei ; Morphology
Keywords: galaxies: active - galaxies: jets - galaxies: groups: general -
galaxies: star formation - radio continuum: galaxies -
intergalactic medium
Abstract:
Radio active galactic nuclei (AGN) are traditionally separated into
two Fanaro-Riley (FR) type classes, edge-brightened FRII sources or
edge-darkened FRI sources. With the discovery of a plethora of radio
AGN of different radio shapes, this dichotomy is becoming too
simplistic in linking the radio structure to the physical properties
of radio AGN, their hosts, and their environment.
We probe the physical properties and large-scale environment of radio
AGN in the faintest FR population to date, and link them to their
radio structure. We use the VLA-COSMOS Large Project at 3GHz (3GHz
VLA-COSMOS), with a resolution and sensitivity of 0.75" and 2.3Jy/beam
to explore the FR dichotomy down to Jy levels.
We classified objects as FRIs, FRIIs, or hybrid FRI/FRII based on the
surface-brightness distribution along their radio structure. Our
control sample was the jet-less/compact radio AGN objects (COM AGN),
which show excess radio emission at 3GHz VLA-COSMOS exceeding what is
coming from star-formation alone; this sample excludes FRs. The
largest angular projected sizes of FR objects were measured by a
machine-learning algorithm and also by hand, following a parametric
approach to the FR classification. Eddington ratios were calculated
using scaling relations from the X-rays, and we included the jet power
by using radio luminosity as a probe. Furthermore, we investigated
their host properties (star-formation ratio, stellar mass,
morphology), and we explore their incidence within X-ray galaxy groups
in COSMOS, and in the density fields and cosmic-web probes in COSMOS.
Our sample is composed of 59 FRIIs, 32 FRI/FRIIs, 39 FRIs, and 1818
COM AGN at 0.03≤z≤6. On average, FR objects have similar radio
luminosities (L3GHz∼1023W/Hz/sr), spanning a range of
1021-26W/Hz/sr, and they lie at a median redshift of z∼1. The
median linear projected size of FRIIs is 106.6238.236.9kpc,
larger than that of FRI/FRIIs and FRIs by a factor of 2-3. The COM AGN
have sizes smaller than 30kpc, with a median value of
1.74.71.5kpc. The median Eddington ratio of FRIIs is
0.0060.0070.005, a factor of 2.5 less than in FRIs and a factor of
2 higher than in FRI/FRII. When the jet power is included, the median
Eddington ratios of FRII and FRI/FRII increase by a factor of 12 and
15, respectively. FRs reside in their majority in massive quenched
hosts (M*>1010.5M☉), with older episodes of star-formation
linked to lower X-ray galaxy group temperatures, suggesting radio-mode
AGN quenching. Regardless of their radio structure, FRs and COM AGN
are found in all types and density environments (group or cluster,
filaments, field).
By relating the radio structure to radio luminosity, size, Eddington
ratio, and large-scale environment, we find a broad distribution and
overlap of FR and COM AGN populations. We discuss the need for a
different classification scheme, that expands the classic FR
classification by taking into consideration the physical properties of
the objects rather than their projected radio structure which is
frequency-, sensitivity- and resolution-dependent. This point is
crucial in the advent of current and future all-sky radio surveys.
Description:
We have investigated the connection of the radio structure in
radio-selected AGN from the 3GHz VLA-COSMOS survey (Smolcic et
al., 2017A&A...602A...2S 2017A&A...602A...2S, Cat. J/A+A/602/A2) to their physical
properties (radio power, size, and accretion rate) and large-scale
environment (hosts, galaxy groups, and density fields). The purpose of
this study was to address the complexity of connecting the radio
structure to physical properties and to determine what drives the
FR-type radio structure. We adopted a parametric classification and
classified our sample into FRIIs, FRIs and FRI/FRIIs. We also included
the jet-less COM AGN in our analysis.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 41 130 Results from by-hand measurements of jet/lobe
sizes to classify objects based on the FR
classification scheme
tablec1.dat 111 130 Basic radio properties and radio classification
for the FR objects in our sample
tablec2.dat 37 130 Host properties of FR objects
tablec3.dat 41 323 Eddington ratios for FRs and COM AGN
tablec4.dat 10 1734 Intrinsic radio sizes of COM AGN
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See also:
J/ApJ/742/125 : Galaxies in X-ray groups I. COSMOS memberships (George+, 2011)
J/ApJS/224/24 : The COSMOS2015 catalog (Laigle+, 2016)
J/A+A/602/A2 : VLA-COSMOS 3 GHz Large Project. II. (Smolcic+, 2017)
J/ApJS/188/384 : The VLA-COSMOS survey. IV. (Schinnerer+, 2010)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- ID 3GHz VLA-COSMOS identification number
7- 10 F4.1 arcsec DL Length of the larger side from the core to the
3σ contour, or the maximum length of
the jet/lobe
12- 15 F4.1 arcsec DS ?=- Length of the shorter side from the core to
the 3σ contour, or the minimum length
of the jet/lobe
17- 20 F4.1 arcsec DLhs ?=- Length of the larger side from the core to
the brightest hot-spot of the jet/lobe
22- 25 F4.1 arcsec DShs ?=- Length of the shorter side from the core to
the brightest hot-spot of the jet/lobe
27- 29 I3 deg BA ?=- Bent angle which is the angle the jets/lobes
form in respect to each other
(180° for symmetrical objects)
31- 38 A8 --- FR Class based on the previous measurements (1)
39 A1 --- u_FR [?] Uncertainty in the visual inspection for FR
40- 41 A2 --- n_FR [OS ] OS for one-sided object
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Note (1): : Class as follows:
FRI = if DLhs<0.5xDL and DShs<0.5xDS (edge-darkened)
FRII = if DLhs>0.5xDL and DShs>0.5xDS (edge-brightened)
FRI/FRII = if one side is FRI-type and the other FRII-type
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Byte-by-byte Description of file: tablec1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- ID 3GHz VLA-COSMOS identification number
7- 25 A19 --- COSMOSVLA3 COSMOSVLA3 designation (JHHMMSS.ss+DDMMSS.s)
27- 35 F9.5 deg RAdeg Radio right ascension (J2000)
37- 42 F6.4 deg DEdeg Radio declination (J2000)
44- 49 F6.3 mJy S3GHz Integrated flux density at 3GHz
51- 55 F5.3 mJy e_S3GHz rms uncertainty on S3GHz (1)
57- 61 F5.3 --- z ?=- Redshift
62 A1 --- n_z [sp] Spectroscopic (s) or photometric (p)
redshift from Laigle et al.
(2016ApJS..224...24L 2016ApJS..224...24L, Cat. J/ApJS/224/24)
64- 71 A8 --- Class3GHz Radio classification performed by visual
inspection of the VLA-COSMOS at 3GHz,
as described in Sec. A
72 A1 --- u_Class3GHz [?] Uncertainty flag on Class3GHz
74- 77 A4 --- Class1.4GHz VLA radio classification at 1.4GHz given by
Schinnerer et al. (2010ApJS..188..384S 2010ApJS..188..384S,
Cat. J/ApJS/188/384)
79 A1 --- radioexcess [FT] Radio excess as in
Delvecchio et al. (2017A&A...602A...3D 2017A&A...602A...3D) (2)
81- 83 I3 --- XrayGroup ?=- X-ray group ID (groups from
George et al., 2011ApJ...742..125G 2011ApJ...742..125G,
Cat. J/ApJ/742/125)
85- 89 F5.2 arcsec LAS Largest angular size, projected, measured
by a semi-automatic technique and verified
by eye (see Sec. C)
91- 95 F5.1 kpc D ?=- Linear projected size, calculated
using z and LAS
97-110 A14 --- COSMOSVLADP VLA 1.4 GHz ID from Schinnerer et al.
(2010ApJS..188..384S 2010ApJS..188..384S, Cat. J/ApJS/188/384)
111 A1 --- n_COSMOSVLADP [T]
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Note (1): for the multi-component sources the error corresponds to the 5% of the
calibration error, while for the rest is the error given by blobcat.
Note (2): Radio excess as in Delvecchio et al. (2017A&A...602A...3D 2017A&A...602A...3D) as follows:
T = radio excess object, i.e. radio AGN
F = non-radio excess
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Byte-by-byte Description of file: tablec2.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- ID 3GHz VLA-COSMOS identification number
7- 13 F7.2 Msun/yr SFR(IR+UV) ?=-Star formation rate (1)
15- 19 F5.2 [Msun] logM* ?=- Stellar mass (1)
21 A1 -- SEDAGN [T/F] AGN (T) based on the SED fit as in
Delvecchio et al. (2017A&A...602A...3D 2017A&A...602A...3D)
23- 29 I7 --- CtpID ?=- Counterpart ID from Smolcic et al.
(2017A&A...602A...2S 2017A&A...602A...2S, Cat. J/A+A/602/A2)
31- 33 A3 --- n_CtpID Note on CtpID (2)
35- 37 A3 --- OClass Optical morphology from Schinnerer et al.
((2010ApJS..188..384S 2010ApJS..188..384S,
Cat. J/ApJS/188/384)) (3)
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Note (1): from the fit to the IR+UV SED Delvecchio et al. (2017A&A...602A...3D 2017A&A...602A...3D).
Note (2): Note as follows:
C15 = COSMOS2015
IR = IRAC ID
I = i-band ID
Note (3): Optical morphology as follows:
E = early-type elliptical
D = disk galaxy
IRR = irregular/peculiar galaxy
DB = disk galaxy with bulge dominated disk
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Byte-by-byte Description of file: tablec3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- ID 3GHz VLA-COSMOS identification number
7- 14 A8 --- RadioClass Radio class
16- 20 F5.2 --- lambdar Radiative luminosity over the Eddington
luminosity (Lrad/LEdd)
22- 25 F4.1 --- lambdark Radiative luminosity over the Eddington
luminosity with the addition of the jet
kinetic energy to the numerator
((Lrad+Qjet)//LEdd_)
27- 31 F5.2 [10-7W] logLjet Jet luminosity
33- 36 F4.2 --- LX/Lradio X-ray to radio luminosity ratio
38- 41 F4.2 [Msun] logMBH Black hole mass
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Byte-by-byte Description of file: tablec4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- ID 3GHz VLA-COSMOS identification number
7- 10 F4.1 kpc D Intrinsic radio size (1)
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Note (1): Intrinsic sizes are estimated after using pyBDSF
(Mohan & Rafferty, 2015, ASCL, 1502.007) on the 3GHz mosaic
(Jimenez-Andrade et al., 2019A&A...625A.114J 2019A&A...625A.114J, Cat. J/A+A/625/A114).
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Acknowledgements:
Eleni Vardoulaki, elenivard(at)gmail.com
(End) Patricia Vannier [CDS] 15-Apr-2021