J/A+A/654/A117 The nature of hyper luminous infrared galaxies (Gao+, 2021)
The nature of hyper luminous infrared galaxies.
Gao F., Wang L., Efstathiou E., Malek K., Best P.N., Bonato M., Farrah D.,
Kondapally R., McCheyne I., Rottgering H.J.A.
<Astron. Astrophys. 654, A117 (2021)>
=2021A&A...654A.117G 2021A&A...654A.117G (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Galaxies, IR ; Active gal. nuclei ;
Infrared sources
Keywords: galaxies: active - galaxies: star formation - galaxies: evolution
Abstract:
Hyperluminous infrared galaxies (HLIRGs) are shown to have been more
abundant in early epochs. The small samples used in earlier studies
are not sufficient to draw robust statistical conclusions regarding
the physical properties and the power sources of these extreme
infrared (IR) bright galaxies.
We make use of multi-wavelength data of a large hyper luminous galaxy
sample to derive the main physical properties, such as stellar mass,
star formation rate (SFR), volume density, and the contribution to the
cosmic stellar mass density and the cosmic SFR density. We also study
the black hole (BH) growth rate and its relationship with the SFR of
the host galaxy.
We selected 526 HLIRGs in three deep fields (Bootes, Lockman-Hole,
and ELAIS-N1) and adopted two spectral energy distribution (SED)
fitting codes: CIGALE, which assumes energy balance, and CYGNUS, which
is based on radiative transfer models and does not adopt an energy
balance principle. We used two different active galactic nucleus (AGN)
models in CIGALE and three AGN models in CYGNUS to compare results
that were estimated using different SED fitting codes and a range of
AGN models.
The stellar mass, total IR luminosity, and AGN luminosity agree well
among different models, with a typical median offset of 0.1dex. The
SFR estimates show the largest dispersions (up to 0.5dex). This
dispersion has an impact on the subsequent analysis, which may suggest
that the previous contradictory results could partly have been due to
the different choices in methods. HLIRGs are ultra-massive galaxies,
with 99% of them having stellar masses larger than 1011M☉. Our
results reveal a higher space density of ultra-massive galaxies than
what was found by previous surveys or predicted via simulations. We
find that HLIRGs contribute more to the cosmic SFR density as redshift
increases. In terms of BH growth, the two SED fitting methods provide
different results. We can see a clear trend in whereby SFR decreases
as AGN luminosity increases when using CYGNUS estimates. This may
possibly imply quenching by AGN in this case, whereas this trend is
much weaker when using CIGALE estimates. This difference is also
influenced by the dispersion between SFR estimates obtained by the two
codes.
Description:
Source id, positions, redshift and SED fitting results using different
codes and AGN Models for 526 hyperluminous infrared galaxies selected
in Bootes, Lockman-Hole and ELAIS-N1 fields are presented.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
catalog.dat 1164 526 Catalog
--------------------------------------------------------------------------------
Byte-by-byte Description of file: catalog.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- ID Source id
7- 13 A7 --- Field Field name (Bootes, EN1 or Lockman)
15- 32 F18.14 deg RAdeg Right Ascension (J2000)
34- 51 F18.15 deg DEdeg Declination (J2000)
53- 70 F18.16 --- z Redshift
72 I1 --- r_z [0/1]?=- Source of redshift (1)
74- 91 F18.15 [Msun] logMassCiF06 Stellar mass from CIGALE Fritz model
93- 112 F20.18 [Msun] e_logMassCiF06 Uncertainty of stellarMass
114- 131 F18.16 [Msun/yr] logSFRCiF06 SFR from CIGALE Fritz model
133- 152 F20.18 [Msun/yr] e_logSFRCiF06 Uncertainty of SFR
154- 171 F18.15 [Lsun] logLIRCiF06 Total LIR from CIGALE Fritz model
173- 192 F20.18 [Lsun] e_logLIRCiF06 Uncertainty of Total LIR
194- 214 F21.17 [Lsun] logLAGNCiF06 LAGN from CIGALE Fritz model
216- 236 F21.18 [Lsun] e_logLAGNCiF06 Uncertainty of LAGN
238- 259 E22.17 --- fAGNCiF06 AGN fraction from CIGALE Fritz model
261- 282 E22.17 --- e_fAGNCiF06 Uncertainty of AGN fraction
284- 303 F20.17 --- chi2CiF06 Reduced χ^2
305- 322 F18.15 [Msun] logMassCiS12 Stellar mass from CIGALE SKIRTOR
model
324- 343 F20.18 [Msun] e_logMassCiS12 Uncertainty of stellarMass
345- 362 F18.16 [Msun/yr] logSFRCiS12 SFR from CIGALE SKIRTOR model
364- 383 F20.18 [Msun/yr] e_logSFRCiS12 Uncertainty of SFR
385- 402 F18.15 [Lsun] logLIRCiS12 Total LIR from CIGALE SKIRTOR
model
404- 423 F20.18 [Lsun] e_logLIRCiS12 Uncertainty of Total LIR
425- 443 F19.16 [Lsun] logLAGNCiS12 LAGN from CIGALE SKIRTOR model
445- 464 F20.18 [Lsun] e_logLAGNCiS12 Uncertainty of LAGN
466- 487 E22.17 --- fAGNCiS12 AGN fraction from CIGALE SKIRTOR
model
489- 510 E22.17 --- e_fAGNCiS12 Uncertainty of AGN fraction
512- 531 F20.17 --- chi2CiS12 Reduced χ^2
533- 550 F18.15 [Msun] logMassCyE95 Stellar mass from CYGNUS E95 model
552- 573 E22.17 [Msun] e_logMassCyE95 Uncertainty of stellarMass
575- 592 F18.16 [Msun/yr] logSFRCyE95 SFR from CYGNUS E95 model
594- 614 E21.16 [Msun/yr] e_logSFRCyE95 Uncertainty of SFR
616- 633 F18.15 [Lsun] logLIRCyE95 Total LIR from CYGNUS E95 model
635- 656 E22.17 [Lsun] e_logLIRCyE95 Uncertainty of Total LIR
658- 676 F19.16 [Lsun] logLAGNCyE95 LAGN from CYGNUS E95 model
678- 699 F22.20 [Lsun] e_logLAGNCyE95 Uncertainty of LAGN
701- 710 E10.5 --- fAGNCyE95 AGN fraction from CYGNUS E95 model
712- 721 E10.5 --- e_fAGNCyE95 Uncertainty of AGN fraction
723- 744 F22.19 --- chi2CyE95 Reduced χ^2
746- 763 F18.15 [Msun] logMassCyF06 Stellar mass from CYGNUS Fritz model
765- 785 F21.19 [Msun] e_logMassCyF06 Uncertainty of stellarMass
787- 804 F18.16 [Msun/yr] logSFRCyF06 SFR from CYGNUS Fritz model
806- 827 F22.20 [Msun/yr] e_logSFRCyF06 Uncertainty of SFR
829- 846 F18.15 [Lsun] logLIRCyF06 Total LIR from CYGNUS Fritz model
848- 869 F22.20 [Lsun] e_logLIRCyF06 Uncertainty of Total LIR
871- 888 F18.15 [Lsun] logLAGNCyF06 LAGN from CYGNUS Fritz model
890- 910 F21.19 [Lsun] e_logLAGNCyF06 Uncertainty of LAGN
912- 921 F10.8 --- fAGNCyF06 AGN fraction from CYGNUS Fritz model
923- 932 F10.8 --- e_fAGNCyF06 Uncertainty of AGN fraction
934- 954 F21.18 --- chi2CyF06 Reduced χ^2
956- 973 F18.15 [Msun] logMassCyS12 Stellar mass from CYGNUS SKIRTOR
model
975- 996 F22.20 [Msun] e_logMassCyS12 Uncertainty of stellarMass
998-1015 F18.16 [Msun/yr] logSFRCyS12 SFR from CYGNUS SKIRTOR model
1017-1038 F22.20 [Msun/yr] e_logSFRCyS12 Uncertainty of SFR
1040-1057 F18.15 [Lsun] logLIRCyS12 Total LIR from CYGNUS SKIRTOR
model
1059-1079 F21.19 [Lsun] e_logLIRCyS12 Uncertainty of Total LIR
1081-1098 F18.15 [Lsun] logLAGNCyS12 LAGN from CYGNUS SKIRTOR model
1100-1120 F21.19 [Lsun] e_logLAGNCyS12 Uncertainty of LAGN
1122-1131 F10.8 --- fAGNCyS12 AGN fraction from CYGNUS SKIRTOR
model
1133-1142 F10.8 --- e_fAGNCyS12 Uncertainty of AGN fraction
1144-1164 F21.18 --- chi2CyS12 Reduced χ^2
--------------------------------------------------------------------------------
Note (1): Source of redshift as follows:
0 = photometric
1 = spectroscopic
--------------------------------------------------------------------------------
Acknowledgements:
Fangyou Gao, gfymargaret(at)gmail.com
(End) Patricia Vannier [CDS] 06-Aug-2021