J/MNRAS/512/86 ISM study with nearby AGNs and galaxies (Bernhard+, 2022)
Quantifying the cool ISM in radio AGNs Evidence for late-time retriggering
by galaxy mergers and interactions.
Bernhard E., Tadhunter C.N., Pierce J.C.S., Dicken D., Mullaney J.R.,
Morganti R., Ramos Almeida C., Daddi E.
<Mon. Not. R. Astron. Soc. 512, 86-103 (2022)>
=2022MNRAS.512...86B 2022MNRAS.512...86B (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Combined data ; Infrared ; Optical ;
Photometry ; Interstellar medium ; QSOs ; Positional data ;
Redshifts ; Star Forming Region ; Stars, masses ; Radio sources ;
Spectroscopy ; Active gal. nuclei
Keywords: galaxies: active - galaxies: interactions - galaxies: ISM -
galaxies: starburst - quasars: general
Abstract:
We use deep Herschel observations of the complete 2Jy sample of
powerful radio active galactic nuclei (AGNs) in the local Universe
(0.05 < z < 0.7) to probe their cool interstellar medium (ISM)
contents and star-forming properties, comparing them against other
samples of nearby luminous AGNs and quiescent galaxies. This allows us
to investigate triggering and feedback mechanisms. We find that the
dust masses of the strong-line radio galaxies (SLRGs) in our sample
are similar to those of radio-quiet quasars, and that their median
dust mass (Mdust = 2 * 107 M☉) is enhanced by a factor of ∼200
compared to that of non-AGN ellipticals, but lower by a factor of ∼16
relative to that of local ultraluminous infrared galaxies (ULIRGs).
Along with compelling evidence for merger signatures in optical
images, the SLRGs in our sample also show relatively high star
formation efficiencies, despite the fact that many of them fall below
the main sequence for star-forming galaxies. Together, these results
suggest that most of our SLRGs have been retriggered by late-time
mergers that are relatively minor in terms of their gas contents. In
comparison with the SLRGs, the radio AGNs with weak optical emission
lines (weak-line radio galaxies - WLRGs) and edge-darkened radio jets
(Fanaroff-Riley Class I radio sources - FRIs) have both lower cool ISM
masses and star formation rates (by a factor of >30), consistent with
being fuelled by a different mechanism (e.g. the direct accretion of
hot gas).
Description:
With the advancement of mid-to-far-infrared astronomy via
observatories, it is now possible to trace the dust content of
galaxies, a proxy for the overall cool ISM contents.
In this paper, we use RL AGNs, RQ AGNs, ULIRGs and elliptical galaxies
Herschel(PACS)/WISE/Spitzer MIR/FIR spectral and photometric data
samples (i.e see section 2) to compute dust masses (i.e see section 3)
from SEDs fit and flux ratios methods. Next, we measure SFRs and
stellar masses from (M/L) ratios and IRAGNSEP algorithm methods (i.e
see sections 4 and 5). Results are presented in three parts, firstly 7
tables *tab1.dat for dust masses derived with 100/160 microns flux
ratios method, secondly, 7 tables *tab2.dat dust masses derived with
IR SED fits method and thirdly, 7 tables *tab3.dat the K-band stellar
masses and SFRs.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
2jytab1.dat 183 46 *Properties and dust masses derived with 100/160
microns flux ratios method of the 2Jy sample
3crtab1.dat 183 45 *Properties and dust masses derived with 100/160
microns flux ratios method of the 3CR sample
atlatab1.dat 183 6 *Properties and dust masses derived with 100/160
microns flux ratios method of the Atlas3D sample
hrstab1.dat 183 8 *Properties and dust masses derived with 100/160
microns flux ratios method of the HRS sample
pgqtab1.dat 183 70 *Properties and dust masses derived with 100/160
microns flux ratios method of the PG QSO sample
t2qstab1.dat 183 86 *Properties and dust masses derived with 100/160
microns flux ratios method of Type-II QSO sample
ulirtab1.dat 183 41 *Properties and dust masses derived with 100/160
microns flux ratios method of the ULIRG sample
2jytab2.dat 146 8 *Properties and dust masses derived with IR SED
fits method of the 2Jy sample
3crtab2.dat 146 4 *Properties and dust masses derived with IR SED
fits method of the 3CR sample
atlatab2.dat 146 3 *Properties and dust masses derived with IR SED
fits method of the Atlas3D sample
pgqtab2.dat 146 9 *Properties and dust masses derived with IR SED
fits method of the PG QSO sample
t2qstab2.dat 146 12 *Properties and dust masses derived with IR SED
fits method of the Type-II QSO sample
ulirtab2.dat 146 14 *Properties and dust masses derived with IR SED
fits method of the ULIRG sample
2jytab3.dat 56 46 *K-band stellar mass and SFRs for the 2Jy sample
3crtab3.dat 56 45 *K-band stellar mass and SFRs for the 3CR sample
atlatab3.dat 56 6 *K-band stellar mass and SFRs for Atlas3D sample
hrstab3.dat 56 8 *K-band stellar mass and SFRs for the HRS sample
pgqtab3.dat 56 70 *K-band stellar mass and SFRs for PG QSO sample
t2qstab3.dat 56 86 *K-band stellar mass and SFRs for Type-II QSO
sample
ulirtab3.dat 56 41 *K-band stellar mass and SFRs for ULIRG sample
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Note on *tab1.dat: Informations on samples in the section 2. Repetitive
temperatures correspond to those sources where we could not calculate the
100/160 microns flux ratios corresponding to the average of the sample for
which we could calculate T. More, the negative LOIII and dust mass values
correspond to upper limits. The dust masses are only calculated for the TC and
the TCBF models as we discarded the one component model.
Note on *tab2.dat: We only present the best fitting parameters for the colder
dust components and not the warmer contributions. This is because the warmer
dust contributions have been modelled with a modified black body curve which
does not represent the true IR emission of AGNs. The dust masses are only
calculated for the TC and the TCBF models as we discarded the OC model. The
uncertainties are the uncertainties on the median parameters measured from the
posterior distributions.
Note on *tab3.dat: Negative values are upper limits. For Mstar, these correspond
to those sources with potential significant AGN contamination in the K-band.
For SFR, these are those without enough IR photometry to calculate SFRs, or
those that are potentially contaminated by non-thermal emission. The default
value is -99.
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See also:
J/ApJ/854/158 : z<0.5 PG quasars IR energy distributions (Shangguan+, 2018)
J/PASP/97/932 : 3CR Source Identifications (Spinrad+, 1985)
J/AJ/151/120 : z<1 3CR radio galaxies and quasars star formation
(Westhues+, 2016)
J/ApJ/854/158 : z<0.5 PG quasars IR energy distributions (Shangguan+, 2018)
J/A+A/565/A128 : Dust SED in HRS nearby galaxies (Ciesla+, 2014)
J/A+A/605/A74 : AKARI fluxes of ATLAS3D early-type galaxies (Kokusho+, 2017)
II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986)
VII/221 : PSCz catalog (Saunders+, 2000)
VIII/1 : The 3C and 3CR Catalogues (Edge+ 1959-1962)
Byte-by-byte Description of file: *tab1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Name Name identification of the source (ID)
17- 27 F11.7 deg RAdeg Right Ascension (J2000) (RA_deg)
29- 39 F11.7 deg DEdeg Declination (J2000) (DEC_deg)
41- 47 F7.5 --- z Redshift (z)
49- 54 A6 --- Classrad Radio classification only for the 91
radio AGN objects (rad_class) (1)
56- 59 A4 --- Classopt Optical classification only for 91
radio AGN objects (opt_class) (2)
61- 83 E23.17 [W] L[OIII] ? The [OIII] 5007 Å luminosity only
for AGN objects (LOIII_W)
85- 90 F6.3 [-] logBnuTCNorm Log-normalisation of the cold
component of the black body curve
obtained with the TC model (logNorm_TC)
(3)
92- 96 F5.3 [-] e_logBnuTCNorm Mean uncertainty of logBnuTCNorm
(elogNorm_TC)
98- 104 F7.4 K TcoldTC Temperature of the cool dust component
obtained with the TC model (T_TC) (3)
106- 112 F7.4 K e_TcoldTC Mean uncertainty of TcoldTC (eT_TC)
114- 118 F5.3 --- BetaTC Beta index of the modified black body
obtained with the TC model (beta_TC)
(3)
120- 124 F5.3 --- e_BetaTC Mean uncertainty of BetaTC (ebeta_TC)
126- 132 F7.3 [-] logBnuTCBFNorm Log-normalisation of the cold
component of the black body curve
obtained with the TCBF model
(logNorm_TCBF) (4)
134- 138 F5.3 [-] e_logBnuTCBFNorm Mean uncertainty of logBnuTCBFNorm
(elogNorm_TCBF)
140- 146 F7.4 K TcoldTCBF Temperature of the cool dust component
obtained with the TCBF model (T_TCBF)
(4)
148- 153 F6.4 K e_TcoldTCBF Mean uncertainty of TcoldTCBF (eT_TCBF)
155- 157 F3.1 --- BetaTCBF Beta index of the modified black body
fixed to 2 with the TCBF model
(beta_TCBF) (4)
159- 162 F4.1 [Msun] logMdustTC The log of the dust mass calculated
using TC model (logMdust_TC) (3)
164- 168 F5.1 [Msun] e_logMdustTC ?=-99 Mean uncertainty of logMdustTC
(elogMdust_TC)
170- 175 F6.3 [Msun] logMdustTCBF The log of the dust mass calculated
using TCBF model (logMdust_TCBF) (4)
177- 183 F7.3 [Msun] e_logMdustTCBF ?=-99 Mean uncertainty of logMdustTCBF
(elogMdust_TCBF)
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Note (1): Radio classifications are as follows:
FRI = Fanaroff-Riley Class I radio sources from Fanaroff & Riley
1974MNRAS.167P..31F 1974MNRAS.167P..31F, 10 objects in our samples
FRII = Fanaroff-Riley Class II radio sources from Fanaroff & Riley
1974MNRAS.167P..31F 1974MNRAS.167P..31F, 74 objects in our samples
CSS = Compact Steep Spectrum sources, 6 objects in our samples
GPS = Gigahertz-Peaked Spectrum sources, 1 object in our samples
Note (2): Optical classification based on the optical spectroscopic data
are as follows:
SLRG = Strong-line radio galaxies sources, 67 objects in our
samples
WLRG = Weak-line radio galaxies sources, 24 objects in our samples
Note (3): To determine specific intensity of a blackbody curve and dust
temperature, we use a two component model with two black body curves
and β index free to vary.
Then to derive dust masses, we use 100/160 microns flux ratio and the
Mdust equation 1 of the section 3 measuring dust masses.
Note (4): To determine specific intensity of a blackbody curve and dust
temperature, we use a two component Beta Fixed model with two black
body curves and β index fixed to 2.
Then to derive dust masses, we 100/160 microns flux ratio and the
Mdust equation 1 of the section 3 measuring dust masses.
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Byte-by-byte Description of file: *tab2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Name Name identification of the source (ID)
17- 23 F7.3 [-] logBnuOCNorm Log-normalisation of the cold
component of the black body curve
obtained with the OC model (logNorm_OC)
(1)
25- 29 F5.3 [-] e_logBnuOCNorm Mean uncertainty of logBnuOCNorm
(elogNorm_OC)
31- 35 F5.2 K TcoldOC Temperature of the cool dust component
obtained with the OC model (T_OC) (1)
37- 40 F4.2 K e_TcoldOC Mean uncertainty of TcoldOC (eT_OC)
42- 46 F5.3 --- BetaOC Beta index of the modified black body
obtained with the OC model (beta_OC)
(1)
48- 52 F5.3 --- e_BetaOC Mean uncertainty of BetaOC (ebeta_OC)
54- 60 F7.3 [-] logBnuTCNorm Log-normalisation of the cold
component of the black body curve
obtained with the TC model (logNorm_TC)
(2)
62- 66 F5.3 [-] e_logBnuTCNorm Mean uncertainty of logBnuTCNorm
(elogNorm_TC)
68- 72 F5.2 K TcoldTC Temperature of the cool dust component
obtained with the TC model (T_TC) (2)
74- 77 F4.2 K e_TcoldTC Mean uncertainty of TcoldTC (eT_TC)
79- 83 F5.3 --- BetaTC Beta index of the modified black body
obtained with the TC model (beta_TC)
85- 89 F5.3 --- e_BetaTC Mean uncertainty of BetaTC (ebeta_TC)
91- 98 F8.4 [-] logBnuTCBFNorm Log-normalisation of the cold
component of the black body curve
obtained with the TCBF model
(logNorm_TCBF) (3)
100- 105 F6.4 [-] e_logBnuTCBFNorm Mean uncertainty of logBnuTCBFNorm
(elogNorm_TCBF)
107- 112 F6.3 K TcoldTCBF Temperature of the cool dust component
obtained with the TCBF model (T_TCBF)
(3)
114- 118 F5.3 K e_TcoldTCBF Mean uncertainty of TcoldTCBF (eT_TCBF)
120- 122 F3.1 --- BetaTCBF Beta index of the modified black body
fixed to 2 with the TCBF model
(beta_TCBF) (3)
124- 127 F4.2 [Msun] logMdustTC The log of the dust mass calculated
using TC model (logMdust_TC) (2)
129- 132 F4.2 [Msun] e_logMdustTC Mean uncertainty of logMdustTC
(elogMdust_TC)
134- 139 F6.4 [Msun] logMdustTCBF The log of the dust mass calculated
using TCBF model (logMdust_TCBF) (3)
141- 146 F6.4 [Msun] e_logMdustTCBF Mean uncertainty of logMdustTCBF
(elogMdust_TCBF)
--------------------------------------------------------------------------------
Note (1): To fit our IR SEDs of specific intensity of a blackbody curve, we use
a single modified blackbody curve one component OC, for which T and
β were free to change. Then to derive dust masses, we use the
Mdust equation 1 of the section 3 measuring dust masses.
Note (2): To fit our IR SEDs of specific intensity of a blackbody curve, we use
the two component TC model which is a combination of two modified
blackbody curves, defined with two dust temperatures and beta indices
for the cold and the warm dust, all of these parameters were free to
change.Then to derive dust masses, we use the Mdust equation 1 of
the section 3 measuring dust masses.
Note (3): To fit our IR SEDs of specific intensity of a blackbody curve, we use
the two component beta fixed model TCBF which is consisted of two
modified blackbody curves, with temperatures Tcold and Twarm, but
with βcold = 2 fixed. Then to derive dust masses, we use the
Mdust equation 1 of the section 3 measuring dust masses.
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Byte-by-byte Description of file: *tab3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Name Name identification of the source (ID)
17- 22 F6.2 [Msun] logM* ?=- Stellar mass estimated converting the
K-band luminosities using M/L ratios (logMstar)
24- 29 F6.2 [Msun] e_logM* ?=- Mean uncertainty of logM* (elogMstar)
31- 35 F5.1 --- f_logM* ?=- Flag indicating the method used to
calculate stellar masses (Mstar_flag) (1)
37- 46 F10.5 Msun/yr SFR Star formation rate computed with IRAGNSEP
decomposes IR SEDs into an AGN and a galaxy
contributions (SFR)
48- 56 F9.5 Msun/yr e_SFR ?=-99 Mean uncertainty on SFR (eSFR)
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Note (1): Methods used to calculate stellar masses as follows:
1.0 = Decomposed (i.e. AGN removed) K-band magnitude from
Inskip et al. 2010MNRAS.407.1739I 2010MNRAS.407.1739I
2.0 = K-band magnitude in a 64 kpc aperture from
Inskip et al. 2010MNRAS.407.1739I 2010MNRAS.407.1739I
3.0 = Extended K-band magitude fro 2MASS
4.0 = Point Source Ks-band magnitude from 2MASS corrected for the
missed extended flux
5.0 = VISTA K-band magnitude
6.0 = Redshifted WISE W1 magnitude
The stellar masses for the PG and T2 QSOs are not reported here
since taken from Shangguan et al. 2018ApJ...854..158S 2018ApJ...854..158S,
Cat. J/ApJ/854/158 and Shangguan et al. 2019ApJ...873...90S 2019ApJ...873...90S
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History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 28-Feb-2025