HERMES: CURRENT COSMIC INFRARED BACKGROUND ESTIMATES CAN BE EXPLAINED BY KNOWN GALAXIES AND THEIR FAINT COMPANIONS AT z \textless 4
M. P. Viero
,
L. Moncelsi
,
R. F. Quadri
,
M. Bethermin
(1)
,
J. Bock
(2)
,
D. Burgarella
(3)
,
S. C. Chapman
(4)
,
D. L. Clements
(5)
,
A. Conley
(6)
,
L. Conversi
(7)
,
S. Duivenvoorden
,
J. S. Dunlop
,
D. Farrah
(8)
,
A. Franceschini
(9)
,
M. Halpern
(10)
,
R. J. Ivison
(11)
,
Guilaine Lagache
(3)
,
G. Magdis
(1)
,
L. Marchetti
(12)
,
J. Alvarez-Marquez
,
G. Marsden
(10)
,
S. J. Oliver
(13)
,
M. J. Page
(14)
,
I. Pérez-Fournon
(5)
,
B. Schulz
,
Douglas Scott
(15)
,
I. Valtchanov
(16)
,
J. D. Vieira
,
L. Wang
,
J. Wardlow
(17)
,
M. Zemcov
(18)
1
AIM (UMR7158 / UMR_E_9005 / UM_112) -
Astrophysique Interprétation Modélisation
2 ONF - Office national des forêts
3 LAM - Laboratoire d'Astrophysique de Marseille
4 CFSA - Centre for Fusion Space and Astrophysics [Coventry]
5 AUTRES
6 University of Colorado [Boulder]
7 Herschel Science Center [Madrid]
8 Department of Physics [Blacksburg]
9 Dipartimento di Fisica e Astronomia "Galileo Galilei"
10 Department of Physics and Astronomy [Vancouver]
11 ROE - Royal Observatory Edinburgh
12 SECM - Service d'Etudes du Comportement des Matériaux de Conditionnement
13 University of Sussex
14 Department of Chemistry and Biochemistry
15 UBC - University of British Columbia
16 Herschel Science Centre
17 Department of Astronomy
18 CALTECH - California Institute of Technology
2 ONF - Office national des forêts
3 LAM - Laboratoire d'Astrophysique de Marseille
4 CFSA - Centre for Fusion Space and Astrophysics [Coventry]
5 AUTRES
6 University of Colorado [Boulder]
7 Herschel Science Center [Madrid]
8 Department of Physics [Blacksburg]
9 Dipartimento di Fisica e Astronomia "Galileo Galilei"
10 Department of Physics and Astronomy [Vancouver]
11 ROE - Royal Observatory Edinburgh
12 SECM - Service d'Etudes du Comportement des Matériaux de Conditionnement
13 University of Sussex
14 Department of Chemistry and Biochemistry
15 UBC - University of British Columbia
16 Herschel Science Centre
17 Department of Astronomy
18 CALTECH - California Institute of Technology
M. P. Viero
- Fonction : Auteur
L. Moncelsi
- Fonction : Auteur
R. F. Quadri
- Fonction : Auteur
D. Burgarella
- Fonction : Auteur
- PersonId : 755483
- ORCID : 0000-0002-4193-2539
- IdRef : 03334700X
S. C. Chapman
- Fonction : Auteur
- PersonId : 852134
S. Duivenvoorden
- Fonction : Auteur
J. S. Dunlop
- Fonction : Auteur
Guilaine Lagache
- Fonction : Auteur
- PersonId : 21058
- IdHAL : guilaine-lagache
J. Alvarez-Marquez
- Fonction : Auteur
B. Schulz
- Fonction : Auteur
Douglas Scott
- Fonction : Auteur
- PersonId : 755592
- ORCID : 0000-0002-6878-9840
J. D. Vieira
- Fonction : Auteur
L. Wang
- Fonction : Auteur
Résumé
We report contributions to cosmic infrared background (CIB) intensities originating from known galaxies and their faint companions at submillimeter wavelengths. Using the publicly available UltraVISTA catalog and maps at 250, 350, and 500 mu m from the Herschel Multi-tiered Extragalactic Survey, we perform a novel measurement that exploits the fact that uncataloged sources may bias stacked flux densities-particularly if the resolution of the image is poor-and intentionally smooth the images before stacking and summing intensities. By smoothing the maps we are capturing the contribution of faint (undetected in K-S similar to 23.4) sources that are physically associated, or correlated, with the detected sources. We find that the cumulative CIB increases with increased smoothing, reaching 9.82 +/- 0.78, 5.77 +/- 0.43 and 2.32 +/- 0.19 nWm(-2) sr(-1) at 250, 350, and 500 mu m at 300 arcsec FWHM. This corresponds to a fraction of the fiducial CIB of 0.94 +/- 0.23, 1.07 +/- 0.31, and 0.97 +/- 0.26 at 250, 350, and 500 mu m, where the uncertainties are dominated by those of the absolute CIB. We then propose, with a simple model combining parametric descriptions for stacked flux densities and stellar mass functions, that emission from galaxies with log(M/M-circle dot) \textgreater 8.5 can account for most of the measured total intensities and argue against contributions from extended, diffuse emission. Finally, we discuss prospects for future survey instruments to improve the estimates of the absolute CIB levels, and observe any potentially remaining emission at z \textgreater 4.