Building the cosmic infrared background brick by brick with Herschel/PEP

被引：142

作者：

Berta, S. ^{[1
]}

Magnelli, B. ^{[1
]}

Nordon, R. ^{[1
]}

Lutz, D. ^{[1
]}

Wuyts, S. ^{[1
]}

Altieri, B. ^{[2
]}

Andreani, P. ^{[3
,4
]}

Aussel, H. ^{[5
]}

Castaneda, H. ^{[6
]}

Cepa, J. ^{[6
,7
]}

Cimatti, A. ^{[8
]}

Daddi, E. ^{[5
]}

Elbaz, D. ^{[5
]}

Schreiber, N. M. Foerster ^{[1
]}

Genzel, R. ^{[1
]}

Le Floc'h, E. ^{[5
]}

Maiolino, R. ^{[9
]}

Perez-Fournon, I. ^{[6
]}

Poglitsch, A. ^{[1
]}

Popesso, P. ^{[1
]}

Pozzi, F. ^{[8
]}

Riguccini, L. ^{[5
]}

Rodighiero, G. ^{[10
]}

Sanchez-Portal, M. ^{[2
]}

Sturm, E. ^{[1
]}

Tacconi, L. J. ^{[1
]}

Valtchanov, I. ^{[2
]}

机构：

[1] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany

[2] ESAC, Herschel Sci Ctr, Madrid 28691, Spain

[3] ESO, D-85748 Garching, Germany

[4] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy

[5] Univ Paris Diderot, Lab AIM, CEA, DSM,CNRS,IRFU,Serv Astrophys, F-91191 Gif Sur Yvette, France

[6] Inst Astrofis Canarias, San Cristobal la Laguna 38205, Spain

[7] Univ La Laguna, Dept Astrofis, E-38207 San Cristobal la Laguna, Spain

[8] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy

[9] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy

[10] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2011年 / 532卷

关键词：

infrared: diffuse background; infrared: galaxies; cosmic background radiation; galaxies: statistics; galaxies: evolution; DEEP FIELD-SOUTH; STAR-FORMATION HISTORY; AREA ISO SURVEY; MULTIBAND IMAGING PHOTOMETER; SUBMILLIMETER NUMBER COUNTS; ACTIVE GALACTIC NUCLEI; MICRON SOURCE COUNTS; MU-M OBSERVATIONS; GALAXY EVOLUTION; VLT/FORS2; SPECTROSCOPY;

D O I：

10.1051/0004-6361/201116844

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The cosmic infrared background (CIB) includes roughly half of the energy radiated by all galaxies at all wavelengths across cosmic time, as observed at the present epoch. The PACS Evolutionary Probe (PEP) survey is exploited here to study the CIB and its redshift differential, at 70, 100 and 160 mu m, where the background peaks. Combining PACS observations of the GOODS-S, GOODS-N, Lockman Hole and COSMOS areas, we define number counts spanning over more than two orders of magnitude in flux: from similar to 1 mJy to few hundreds mJy. Stacking of 24 mu m sources and P(D) statistics extend the analysis down to similar to 0.2 mJy. Taking advantage of the wealth of ancillary data in PEP fields, differential number counts d(2)N/dS/dz and CIB are studied up to z = 5. Based on these counts, we discuss the effects of confusion on PACS blank field observations and provide confusion limits for the three bands considered. While most of the available backward evolution models predict the total PACS number counts with reasonable success, the consistency to redshift distributions and CIB derivatives can still be significantly improved. The new high-quality PEP data highlight the need to include redshift-dependent constraints in future modeling. The total CIB surface brightness emitted above PEP 3 sigma flux limits is vI(v) = 4.52 +/- 1.18, 8.35 +/- 0.95 and 9.49 +/- 0.59 [nW m-(2) sr(-1)] at 70, 100, and 160 mu m, respectively. These values correspond to 58 +/- 7% and 74 +/- 5% of the COBE/DIRBE CIB direct measurements at 100 and 160 mu m. Employing the P(D) analysis, these fractions increase to similar to 65% and similar to 89%. More than half of the resolved CIB was emitted at redshift z <= 1. The 50%-light redshifts lie at z = 0.58, 0.67 and 0.73 at the three PACS wavelengths. The distribution moves towards earlier epochs at longer wavelengths: while the 70 mu m CIB is mainly produced by z <= 1.0 objects, the contribution of z > 1.0 sources reaches 50% at 160 mu m. Most of the CIB resolved in the three PACS bands was emitted by galaxies with infrared luminosities in the range 10(11)-10(12) L-circle dot.

引用

页数：25

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