J/ApJ/854/158 z<0.5 PG quasars IR energy distributions (Shangguan+, 2018)
On the gas content and efficiency of AGN feedback in low-redshift quasars.
Shangguan J., Ho L.C., Xie Y.
<Astrophys. J., 854, 158 (2018)>
=2018ApJ...854..158S 2018ApJ...854..158S
ADC_Keywords: QSOs; Photometry, infrared; Interstellar medium; Redshifts;
Radio sources; Millimetric/submm sources
Keywords: galaxies: active; galaxies: ISM; galaxies: nuclei; galaxies: Seyfert;
infrared: ISM; quasars: general
Abstract:
The interstellar medium is crucial to understanding the physics of
active galaxies and the coevolution between supermassive black holes
and their host galaxies. However, direct gas measurements are limited
by sensitivity and other uncertainties. Dust provides an efficient
indirect probe of the total gas. We apply this technique to a large
sample of quasars, whose total gas content would be prohibitively
expensive to measure. We present a comprehensive study of the full
(1 to 500µm) infrared spectral energy distributions of 87 redshift
<0.5 quasars selected from the Palomar-Green sample, using photometric
measurements from 2MASS, WISE, and Herschel, combined with Spitzer
mid-infrared (5-40µm) spectra. With a newly developed Bayesian
Markov Chain Monte Carlo fitting method, we decompose various
overlapping contributions to the integrated spectral energy
distribution, including starlight, warm dust from the torus, and
cooler dust on galaxy scales. This procedure yields a robust dust
mass, which we use to infer the gas mass, using a gas-to-dust ratio
constrained by the host galaxy stellar mass. Most (90%) quasar hosts
have gas fractions similar to those of massive, star-forming galaxies,
although a minority (10%) seem genuinely gas-deficient, resembling
present-day massive early-type galaxies. This result indicates that
"quasar mode" feedback does not occur or is ineffective in the host
galaxies of low-redshift quasars. We also find that quasars can boost
the interstellar radiation field and heat dust on galactic scales.
This cautions against the common practice of using the far-infrared
luminosity to estimate the host galaxy star formation rate.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 134 87 Physical properties of Palomar-Green (PG) quasars
table2.dat 96 87 2MASS and WISE NIR and MIR photometry
table3.dat 101 87 Herschel PACS and SPIRE photometry
table4.dat 59 74 Archival FIR and radio data
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See also:
B/hst : HST Archived Exposures Catalog (STScI, 2007)
VIII/2 : Molonglo Reference Catalog of Radio Sources (Large+ 1981)
VIII/14 : 87GB Catalog of radio sources (Gregory et al., 1991)
VIII/42 : Texas Survey of radio sources at 365MHz (Douglas+ 1996)
VIII/65 : 1.4GHz NRAO VLA Sky Survey (NVSS) (Condon+ 1998)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
VIII/79 : The VLA Low-frequency Sky Survey at 74MHz (Cohen+ 2007)
II/328 : AllWISE Data Release (Cutri+ 2013)
J/AJ/108/1163 : Radio structure of Quasars (Kellermann+ 1994)
J/ApJS/166/470 : SDSS-Spitzer type I QSOs IR photometry (Richards+, 2006)
J/ApJ/656/770 : Mid-IR spectrum of star-forming galaxies (Smith+, 2007)
J/ApJS/177/103 : HI survey of AGNs (Ho+, 2008)
J/A+A/495/421 : AGN in XMM-Newton archive (CAIXA) (Bianchi+, 2009)
J/ApJ/701/1965 : Radial dust data of SINGS galaxies (Munoz-Mateos+, 2009)
J/PASP/122/261 : Herschel Reference Survey Sample (Boselli+, 2010)
J/ApJ/723/895 : IR luminosities and aromatic features of 5MUSES (Wu+, 2010)
J/MNRAS/415/32 : COLD GASS survey (Saintonge+, 2011)
J/PASP/124/140 : UBVRI Hp BT and VT photonic responses (Bessell+, 2012)
J/A+A/543/A161 : Submm obs. of 323 HRS nearby galaxies (Ciesla+, 2012)
J/ApJ/745/95 : KINGFISH sample Herschel FIR & submm photom. (Dale+, 2012)
J/A+A/544/A101 : GALEX obs. of Herschel Reference Survey (Cortese+, 2012)
J/A+A/551/A100 : Panchromatic SED of Herschel sources (Berta+, 2013)
J/A+A/564/A65 : Cold gas data of Herschel Reference Survey (Boselli+, 2014)
J/A+A/562/A21 : AGN feedback from CO observations (Cicone+, 2014)
J/A+A/565/A128 : Dust SED in HRS nearby galaxies (Ciesla+, 2014)
J/ApJ/783/84 : ALMA obs. in 107 galaxies at z=0.2-2.5 (Scoville+, 2014)
J/ApJS/214/23 : IR spectra and photometry of z<0.5 quasars (Shi+, 2014)
J/ApJ/804/34 : Luminous AGNs and early-type SDSS galaxies (Hong+, 2015)
J/A+A/575/A80 : FIR photometry of 3CR galaxies (Podigachoski+, 2015)
J/A+A/583/A120 : AGN torus models. SED library (Siebenmorgen+, 2015)
J/A+A/591/A28 : 2 QSOs SINFONI K-band datacubes (Carniani+, 2016)
J/ApJ/820/83 : ALMA galaxy data in COSMOS survey (Scoville+, 2016)
J/MNRAS/460/2143 : HI size-mass relation of galaxies (Wang+, 2016)
J/AJ/151/120 : z<1 3CR radio gal. and QSOs star formation (Westhues+, 2016)
J/ApJ/819/L27 : Stellar masses of optical & IR QSO hosts (Zhang+, 2016)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Source name
13- 17 F5.3 --- z [0.02/0.5] Spectroscopic redshift
19- 22 I4 Mpc DL [113/2723] Distance (1)
24- 28 F5.2 [Msun] logM* [10.2/11.6]? log host galaxy stellar mass (2)
30- 34 F5.2 [10-7W] logL5100 [43.6/46.2] log monochromatic luminosity
at 5100Å; erg/s
36- 39 I4 km/s FWHMHb [721/9405] Full-Width at Half-Maximum of
broad Hβ emission line
41- 44 F4.2 [Msun] logMBH [6.6/10] log blackhole mass
46- 50 F5.2 [Msun] logMblg [9.2/12.1] log stellar bulge mass estimated
from logMBH
52- 56 F5.2 [-] logUmin [-1/1.4]? log best-fit minimum intensity (3)
58- 61 F4.2 [-] e_logUmin [0/0.4]? Lower uncertainty in logUmin (5)
63- 66 F4.2 [-] E_logUmin [0/0.5]? Upper uncertainty in logUmin (5)
68- 71 F4.2 % qPAH [0.4/4.6]? Best-fit mass fraction of dust
as PAH molecules
73- 76 F4.2 % e_qPAH [0/0.8]? Lower uncertainty in qPAH (5)
78- 81 F4.2 % E_qPAH [0/0.8]? Upper uncertainty in qPAH (5)
83- 87 F5.2 [-] loggam [-4.8/0]? log best-fit mass fraction (4)
89- 92 F4.2 [-] e_loggam [0.03/1.1]? Lower uncertainty in qPAH
94- 97 F4.2 [-] E_loggam [0.03/1.3]? Upper uncertainty in qPAH
99- 99 A1 --- l_logMd Limit flag on logMd
101-104 F4.2 [Msun] logMd [6.2/9] log best-fit total dust mass
106-109 F4.2 [Msun] e_logMd [0.01/0.5]? Lower uncertainty in logMd
111-114 F4.2 [Msun] E_logMd [0.01/0.6]? Upper uncertainty in logMd
116-119 F4.2 [-] logdGDR [2/2.2] log gas-to-dust ratio of galaxy (6)
121-121 A1 --- l_logMg Limit flag on logMg
123-127 F5.2 [Msun] logMg [8.3/11] log total gas mass (7)
129-132 F4.2 [Msun] e_logMg [0.2/0.6]? Uncertainty in logMg
134-134 A1 --- Type Radio type (8)
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Note (1): Calculated with Ωm=0.308, ΩΛ=0.692,
and H0=67.8km/s/Mpc (Planck Collaboration+ 2016A&A...594A..13P 2016A&A...594A..13P).
Note (2): From Zhang+ (2016, J/ApJ/819/L27). In order to convert
from Salpeter (1955ApJ...121..161S 1955ApJ...121..161S) IMF to Kroupa-like IMF,
we divide the stellar mass by 1.5, following
Zhang+ (2016, J/ApJ/819/L27).
Note (3): Relative to that measured in the solar neighborhood.
Note (4): Of the dust associated with the power-law part of the interstellar
radiation field.
Note (5): The quoted uncertainties of the Draine & Li (2007ApJ...657..810D 2007ApJ...657..810D)
model represent the 68 percent confidence interval determined from
the 16th and 84th percentile of the marginalized posterior PDF.
However, for Umin or qPAH, if fewer than 16% of the sampled values
at the discrete grids lie below (above) the best-fit value, the lower
(upper) uncertainty of the parameter is not resolved, and it is
reported as "0.00" in the table.
Note (6): Estimated from the host galaxy stellar mass. For objects without
stellar mass measured, the median value of the sample is adopted,
124±6. The value of δGDR has been corrected using
Equation (17), so that the total gas mass can be compared to the
directly measured gas mass in an unbiased manner.
Note (7): Combining the uncertainties of the dust mass and
the δGDR (0.2 dex).
Note (8): Radio type as follows:
Q = radio-quiet source;
S = steep-spectrum source;
F = flat-spectrum source.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Source name
13- 15 A3 --- f_Name Flag(s) on Name (9)
17- 21 F5.2 mJy FJ [0.6/35] J band (1.235 um) flux from 2MASS
23- 26 F4.2 mJy e_FJ [0.1/1.5] Uncertainty in FJ
28- 32 F5.2 mJy FH [0.6/43] H band (1.662 um) flux from 2MASS
34- 37 F4.2 mJy e_FH [0.1/2] Uncertainty in FH
39- 43 F5.2 mJy FKs [1.4/74] Ks band (2.159 um) flux from 2MASS
45- 48 F4.2 mJy e_FKs [0.1/1.7] Uncertainty in FKs
50- 55 F6.2 mJy FW1 [3.6/137.7] W1 band (3.353 um) flux from WISE
57- 60 F4.2 mJy e_FW1 [0.01/0.2] Uncertainty in FW1
62- 67 F6.2 mJy FW2 [5.4/189.2] W2 band (4.603 um) flux from WISE
69- 72 F4.2 mJy e_FW2 [0.02/0.2] Uncertainty in FW2
74- 79 F6.2 mJy FW3 [10.7/429] W3 band (11.561 um) flux from WISE (10)
81- 84 F4.2 mJy e_FW3 [0.1/1] Uncertainty in FW3
86- 91 F6.2 mJy FW4 [14/864.1] W4 band (22.088 um) flux from WISE (10)
93- 96 F4.2 mJy e_FW4 [0.5/2.5] Uncertainty in FW4
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Note (9): Flag as follows:
a = an extended source measured with 20-arcsec-radius aperture
on 2MASS images.
b = there are projected companions found in the 2MASS images.
c = there are projected companions found in WISE images.
Note (10): The WISE W3 and W4 bands are corrected for a calibration
discrepancy described in the text.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Source name
13 A1 --- n_Name Flag on Name (11)
15- 21 F7.2 mJy F70 [6/2373]? Herschel/PACS flux density at 70um
23- 26 F4.2 mJy e_F70 [1.6/8]? Uncertainty in F70
28- 34 F7.2 mJy F100 [7/2385]? Herschel/PACS flux density at 100um
36- 40 F5.2 mJy e_F100 [1.9/13.2]? Uncertainty in F100
42- 48 F7.2 mJy F160 [18/1905]? Herschel/PACS flux density at 160um
50 A1 --- f_F160 [c] Flag on F160 (11)
52- 56 F5.2 mJy e_F160 [4/38]? Uncertainty in F160
58- 63 F6.2 mJy F250 [20/756]? Herschel/SPIRE flux density at 250um
65- 69 F5.2 mJy e_F250 [6/14.1]? Uncertainty in F250
71- 76 F6.2 mJy F350 [14/706]? Herschel/SPIRE flux density at 350um
78 A1 --- f_F350 [d] Flag on F350 (11)
80- 84 F5.2 mJy e_F350 [7/11]? Uncertainty in F350
86- 92 F7.2 mJy F500 [19/1035]? Herschel/SPIRE flux density at 500um
94 A1 --- f_F500 [d] Flag on F500 (11)
96-101 F6.3 mJy e_F500 [8.5/15]? Uncertainty in F500
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Note (11): Flag as follows:
a = a bright companion is found and removed in the PACS images.
b = a faint companion is found but not removed in the PACS images.
c = the target is heavily blended with the companion in this PACS band.
d = the flux is likely dominated by the companion in this SPIRE band.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Source name
13- 16 I4 um lambda [70/1300]? Wavelength
18- 23 I6 MHz Freq [74/250000]? Frequency
25- 31 F7.1 mJy Fnu [7.6/20820] Flux density for Freq or lambda
33- 39 F7.2 mJy e_Fnu [0.9/2100] Uncertainty in Fnu
41- 59 A19 --- BibCode Reference
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 13-Nov-2018