J/MNRAS/471/59 Intrinsic AGN SEDs in PG quasars (Lani+, 2017)
Intrinsic AGN SED & black hole growth in the Palomar-Green quasars.
Lani C., Netzer H., Lutz D.
<Mon. Not. R. Astron. Soc., 471, 59-79 (2017)>
=2017MNRAS.471...59L 2017MNRAS.471...59L (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; QSOs ; Energy distributions
Keywords: galaxies: active - galaxies: star formation -
quasars: supermassive black holes
Abstract:
We present a new analysis of the Palomar-Green quasar sample based on
Spitzer and Herschel observations. (i) Assuming polycyclic aromatic
hydrocarbon (PAH)-based star formation luminosities (LSF) similar to
Symeonidis et al. (S16, 2016MNRAS.459..257S 2016MNRAS.459..257S), we find mean and median
intrinsic active galactic nucleus (AGN) spectral energy distributions
(SEDs). These, in the far-infrared (FIR), appear hotter and
significantly less luminous than the S16 mean intrinsic AGN SED. The
differences are mostly due to our normalization of the individual SED
that properly accounts for a small number of very FIR-luminous
quasars. Our median, PAH-based SED represents ∼6 per cent increase on
the 1-243µm luminosity of the extended Mor & Netzer (EM12,
2012MNRAS.420..526M 2012MNRAS.420..526M) torus SED, while S16 find a significantly larger
difference. It requires large-scale dust with T∼20-30K, which, if
optically thin and heated by the AGN, would be outside the host
galaxy. (ii) We also explore the black hole and stellar mass growths,
using LSF estimates from fitting Herschel/PACS observations after
subtracting the EM12 torus contribution. We use rough estimates of
stellar mass, based on scaling relations, to divide our sample into
groups: on, below and above the star formation main sequence (SFMS).
Objects on the SFMS show a strong correlation between star formation
luminosity and AGN bolometric luminosity, with a logarithmic slope of
∼0.7. Finally, we derive the relative duty cycles of this and another
sample of very luminous AGN at z=2-3.5. Large differences in this
quantity indicate different evolutionary pathways for these two
populations characterized by significantly different black hole
masses.
Description:
We consider a sample of PG QSOs, which was in turn selected from the
Palomar Bright Quasar Survey Catalogue from Schmidt & Green
(1983ApJ...269..352S 1983ApJ...269..352S, Cat. J/ApJ/269/352).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 93 85 Quantities for our PG QSOs sample
tabled1.dat 63 250 Data for the intrinsic AGN SEDs considered in
our work
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See also:
J/ApJ/269/352 : Quasar evolution (Schmidt+, 1983)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Name
12- 14 A3 --- n_Name Note on Name (1)
16- 27 A12 --- OName Other Name
29- 36 F8.4 deg RAdeg Right ascension (J2000)
38- 45 F8.4 deg DEdeg Declination (J2000)
47- 51 F5.3 --- z Redshift
53- 58 F6.3 [10-7W] logL5100 Uncorrected for host galaxy contamination
which, in our sample, we estimate to be
typically ∼20 per cent
60- 64 F5.3 [Msun] logMBH Black hole mass
66- 72 F7.4 [10-7W] logL5um 5um luminosity
74- 78 F5.3 [10-7W] e_logL5um rms uncertainty on logL5um
80- 85 F6.3 [10-7W] logLSF ? Star formation luminosity
87- 89 F3.1 [10-7W] e_logLSF ? rms uncertainty on logLSF
91 I1 --- Loc [0/2]? Location w.r.t. SFMS (2)
93 I1 --- Temp [1/3]? Choice of EM12 template (3)
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Note (1): Notes as follows:
e = Source missing LL spectral information from Spitzer/IRS.
b = Upper limit in one or two Herschel/PACS bands (70 and 160um;
with 3σ being the requirement for a detection).
g = Upper limit in all three Herschel/PACS bands (with 3σ:
being the requirement for a detection).
a = Bad torus fit.
d = Source with Herschel/PACS 160um observation affected by blending with
a nearby source.
p = Source showing SF activity consistent with zero upon visual inspection;
its logLSF was arbitrarily set to 42.0±0.3.
Note (2): Location w.r.t. SFMS as follows:
0 = refers to sources below the SFMS
1 = refers to sources on the SFMS
2 = refers to potential starbursts.
For a description for how we determined the three groups we refer the
reader to Section 4.5.1.
Note (3): Choice of EM12 (Mor & Netzer, 2012MNRAS.420..526M 2012MNRAS.420..526M) template
as follows:
1 = refers to the 25th percentile of the median EM12 template
2 = refers to the median EM12 template
3 = refers to the 75th of the median EM12 template. These have negative,
flat and positive gradient in the optical-NIR (see grey and black lines
in Fig. 2), and are characteristic by Ltorus/L5um=[4.27, 3.58, 3.18],
respectively.
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Byte-by-byte Description of file: tabled1.dat
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Bytes Format Units Label Explanations
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1- 6 F6.2 um lambda Rest wavelength
8- 13 F6.4 --- lamndaLl1 Extended EM12- median
(λLλ, arbitrary units)
15- 20 F6.4 --- lambdaLl1-25 Extended EM12- 25th percentile
(λLλ, arbitrary units)
22- 27 F6.4 --- lambdaLl1-75 Extended EM12- 75th percentile
(λLλ, arbitrary units)
29- 36 F8.4 --- lambdaLl2 ?=-99 PAH-based median intrinsic AGN SED
for full PG sample
(λLλ, arbitrary units)
38- 45 F8.4 --- lambdaLl2-25 ?=-99 PAH-based 25th percentile
for full PG sample
(λLλ, arbitrary units)
47- 54 F8.4 --- lambdaLl2-75 ?=-99 PAH-based 75th percentile
for full PG sample
(λLλ, arbitrary units)
56- 63 F8.4 --- lambdaLl3 ?=-99 PAH-based median intrinsic AGN SED
for the top 1 sigma sources
(lambdaLλ, arbitrary units)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 13-May-2020