J/A+A/671/A34 The WISSH quasars project. XI. (Saccheo+, 2023)
The WISSH quasars project. XI. The mean spectral energy distribution and
bolometric corrections of the most luminous quasars.
Saccheo I., Bongiorno A., Piconcelli E., Testa V., Bischetti M., Bisogni S.,
Bruni G., Cresci G., Feruglio C., Fiore F., Grazian A., Luminari A.,
Lusso E., Mainieri V., Maiolino R., Marconi A., Ricci F., Tombesi F.,
Travascio A., Vietri G., Vignali C., Zappacosta L., La Franca F.
<Astron. Astrophys. 671, A34 (2023)>
=2023A&A...671A..34S 2023A&A...671A..34S (SIMBAD/NED BibCode)
ADC_Keywords: QSOs ; Photometry, SDSS ; Photometry, infrared ; Radio sources ;
X-ray sources
Keywords: galaxies: active - quasars: general
Abstract:
Hyper-luminous Quasi-Stellar Objects (QSOs) represent the ideal
laboratory to investigate Active Galactic Nuclei (AGN) feedback
mechanism since their formidable energy release causes powerful winds
at all scales and thus the maximum feedback is expected.
We aim at deriving the mean Spectral Energy Distribution (SED) of a
sample of 85 WISE-SDSS Selected Hyper-luminous (WISSH) quasars. Since
the SED provides a direct way to investigate the AGN structure, our
goal is to understand if quasars at the bright end of the luminosity
function have peculiar properties compared to the bulk of the
population. We built a mean intrinsic SED after correcting for the
dust extinction, absorption and emission lines and intergalactic
medium absorption. We also derived bolometric, IR band and
monochromatic luminosities together with bolometric corrections at
lambda=5100Å and 3 micron. We define a new relation for the
3 micron bolometric correction. We find that the mean SED of
hyper-luminous WISSH QSOs is different from that of less luminous
sources, i.e. a relatively lower X-ray emission and a near and mid IR
excess which can be explained assuming a larger dust contribution.
WISSH QSOs have stronger emission from both warm and very hot dust,
the latter being responsible for shifting the typical dip of the AGN
SED from 1.3 to 1.1 micron. We also derived the mean SEDs of two
sub-samples created according to the presence of Broad Absorption
Lines and equivalent width of CIV line. We confirm that BALs are X-ray
weak and that they have a reddened UV-optical continuum. We also find
that BALs tend to have stronger emission from the hot dust component.
This analysis suggests that hyper-luminous QSOs have a peculiar SED
compared to less luminous objects. It is therefore critical to use SED
templates constructed exclusively from very bright quasars samples
when dealing with particularly luminous sources.
Description:
The WISSH sample (Bischetti et al., 2017A&A...598A.122B 2017A&A...598A.122B) is composed
of 85 type 1 radio-quiet hyperluminous quasars with
log(Lbol/[erg/s])≥47.0 (Duras et al., 2017A&A...604A..67D 2017A&A...604A..67D). The
sample was assembled cross-correlating the SDSS (Shen et al.,
2011ApJS..194...45S 2011ApJS..194...45S, Cat. J/ApJS/194/45) and the WISE (Wright et al.,
2010AJ....140.1868W 2010AJ....140.1868W) catalogs and selecting, among the sources with a
flux density Sv,22um>3mJy, the 100 most luminous QSOs at
λ=7.8um (Weedman et al., 2012ApJ...761..184W 2012ApJ...761..184W, Cat.
J/ApJ/761/184).
Entire photometry of the WISSH sample is reported in table 2.
Bolometric and monochromatic luminosities for WISSH QSOs are reported
in table3, and derived mean SEDs of WISSH QSOs in table4.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 396 85 Photometric data of the WISSH sample
table3.dat 61 85 Bolometric and monochromatic luminosities for
WISSH QSOs
table4.dat 71 346 Derived mean SEDs of WISSH QSOs
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See also:
J/A+A/635/A157 : QSO J1538+0855 MUSE datacube (Travascio+, 2020)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- ID ID of each target
9- 24 F16.13 mag umag SDSS u-band magnitude
26- 30 F5.3 mag e_umag rms uncertainty on u-band magnitude
32- 47 F16.13 mag gmag SDSS g-band magnitude
49- 53 F5.3 mag e_gmag rms uncertainty on g-band magnitude
55- 70 F16.13 mag rmag SDSS r-band magnitude
72- 76 F5.3 mag e_rmag rms uncertainty on r-band magnitude
78- 93 F16.13 mag imag SDSS i-band magnitude
95- 99 F5.3 mag e_imag rms uncertainty on i-band magnitude
101-106 F6.3 mag zmag SDSS z-band magnitude
108-112 F5.3 mag e_zmag rms uncertainty on z-band magnitude
114-130 F17.13 mag Jmag 2MASS/TNG J-band magnitude
132-148 F17.15 mag e_Jmag rms uncertainty on J-band magnitude
150-156 F7.3 mag Hmag 2MASS/TNG H-band magnitude
158-175 F18.16 mag e_Hmag rms uncertainty on H-band magnitude
177-193 F17.13 mag Kmag 2MASS/TNG K-band magnitude
195-211 F17.15 mag e_Kmag rms uncertainty on K-band magnitude
213-228 F16.13 mag W1mag WISE W1-band (3.4um) magnitude
230-234 F5.3 mag e_W1mag rms uncertainty on W1-band magnitude
236-241 F6.3 mag W2mag WISE W2-band (4.6um) magnitude
243-247 F5.3 mag e_W2mag rms uncertainty on W2-band magnitude
249-254 F6.3 mag W3mag WISE W3-band (12um) magnitude
256-272 F17.15 mag e_W3mag rms uncertainty on W3-band magnitude
274-279 F6.3 mag W4mag WISE W4-band (22um) magnitude
281-297 F17.15 mag e_W4mag rms uncertainty on W4-band magnitude
299-305 F7.3 mag S250 ? Herschel/SPIRE 250um-band magnitude
307-312 F6.3 mag e_S250 ? rms uncertainty on 250um-band magnitude
314-320 F7.3 mag S350 ? Herschel/SPIRE 350um-band magnitude
322-327 F6.3 mag e_S350 ? rms uncertainty on 350um-band magnitude
329-335 F7.3 mag S500 ? Herschel/SPIRE 500um-band magnitude
337-342 F6.3 mag e_S500 ? rms uncertainty on 500um-band magnitude
344-349 F6.1 GHz Band ? ALMA/NOEMA observed continuum frequency
351-356 F6.3 mJy Flux ? ALMA/NOEMA continuum flux
358-363 F6.3 mJy e_Flux ? rms uncertainty on ALMA/NOEMA measured
flux
365-369 F5.1 GHz BandJVLA ? JVLA observed continuum frequency
371-376 F6.3 mJy FJVLA ? JVLA continuum flux
378-383 F6.3 mJy e_FJVLA ? rms uncertainty on JVLA measured flux
385-390 F6.2 [mW/m2] logL(2-10) ? Chandra/XMM integrated 2-10Kev luminosity
392-396 F5.2 --- Gamma ? X-ray photon index
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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- 7 A7 --- ID ID of each target
9- 13 F5.2 10-7W Lbol Bolometric luminosity
15- 18 F4.2 10-7W e_Lbol Lower uncertainty on Lbol
20- 23 F4.2 10-7W E_Lbol Upper uncertainty on Lbol
25- 29 F5.2 10-7W L2500 2500Å monochromatic luminosity
31- 34 F4.2 10-7W e_L2500 rms uncertainty on 2500Å luminosity
36- 40 F5.2 10-7W L5100 5100Å monochromatic luminosity
42- 45 F4.2 10-7W e_L5100 rms uncertainty on 5100Å luminosity
47- 51 F5.2 10-7W L30000 3um monochromatic luminosity
53- 56 F4.2 10-7W e_L30000 rms uncertainty on 3um luminosity
58- 61 F4.2 mag E(B-V) E(B-V) colour excess
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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- 4 F4.2 0.1nm loglambda Wavelength
6- 10 F5.2 [10-7W] logmean Mean SED (lambdaLlambda) of the
full WISSH sample (in erg/s)
12- 15 F4.2 [10-7W] s_logmean rms uncertainty on the mean SED
(lambdaLlambda) of the full sample
17- 22 F6.2 [10-7W] logBAL ? Mean SED (lambdaLlambda) of the
BAL subsample (in erg/s)
24- 29 F6.2 [10-7W] s_logBAL ? rms uncertainty on the mean SED
(lambdaLlambda) of the BAL subsample
31- 36 F6.2 [10-7W] logNonBAL ? Mean SED (lambdaLlambda) of the
non-BAL subsample (in erg/s)
38- 43 F6.2 [10-7W] s_logNonBAL ? rms uncertainty on the mean SED
(lambdaLlambda) of the non-BAL subsample
45- 50 F6.2 [10-7W] logWeak ? Mean SED (lambdaLlambda) of the
CIV weak subsample (in erg/s)
52- 57 F6.2 [10-7W] s_logWeak ? rms uncertainty on the mean SED
(lambdaLlambda) of the CIV weak
subsample
59- 64 F6.2 [10-7W] logNonWeak ? Mean SED (lambdaLlambda) of the
non-CIV weak subsample (in erg/s)
66- 71 F6.2 [10-7W] s_logNonWeak ? rms uncertainty on the mean SED
(lambdaLlambda) of the non-CIV weak
subsample
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Acknowledgements:
Ivano Saccheo, ivano.saccheo(at)uniroma3.it
References:
Bischetti et al., Paper I 2017A&A...598A.122B 2017A&A...598A.122B
Duras et al., Paper II 2017A&A...604A..67D 2017A&A...604A..67D
Martocchia et al., Paper III 2017A&A...608A..51M 2017A&A...608A..51M
Vietri et al., Paper IV 2018A&A...617A..81V 2018A&A...617A..81V
Bischetti et al., Paper V 2018A&A...617A..82B 2018A&A...617A..82B
Bruni et al., Paper VI 2019A&A...630A.111B 2019A&A...630A.111B
Zappacosta et al., Paper VII 2020A&A...635L...5Z 2020A&A...635L...5Z
Travascio et al., Paper VIII 2020A&A...635A.157T 2020A&A...635A.157T, Cat. J/A+A/635/A157
Bischetti et al., Paper IX 2021A&A...645A..33B 2021A&A...645A..33B
History:
02-Mar-2023: on-line version
11-Apr-2023: units of luminosities in table3 corrected
(End) Patricia Vannier [CDS] 28-Nov-2022