The Herschel* PEP/HerMES luminosity function - I. Probing the evolution of PACS selected Galaxies to z ≃ 4

被引：368

作者：

Gruppioni, C. ^{[1
]}

Pozzi, F. ^{[2
]}

Rodighiero, G. ^{[3
]}

Delvecchio, I. ^{[2
]}

Berta, S. ^{[4
]}

Pozzetti, L. ^{[1
]}

Zamorani, G. ^{[1
]}

Andreani, P. ^{[5
]}

Cimatti, A. ^{[2
]}

Ilbert, O. ^{[6
]}

Le Floc'h, E. ^{[7
]}

Lutz, D. ^{[4
]}

Magnelli, B. ^{[4
]}

Marchetti, L. ^{[3
,8
]}

Monaco, P. ^{[9
]}

Nordon, R. ^{[4
]}

Oliver, S. ^{[10
]}

Popesso, P. ^{[4
]}

Riguccini, L. ^{[7
]}

Roseboom, I. ^{[10
,11
]}

Rosario, D. J. ^{[4
]}

Sargent, M. ^{[7
]}

Vaccari, M. ^{[3
,12
]}

Altieri, B. ^{[13
]}

Aussel, H. ^{[7
]}

Bongiovanni, A. ^{[14
]}

Cepa, J. ^{[14
]}

Daddi, E. ^{[7
]}

Dominguez-Sanchez, H. ^{[1
,14
]}

Elbaz, D. ^{[7
]}

Schreiber, N. Foerster ^{[4
]}

Genzel, R. ^{[4
]}

Iribarrem, A. ^{[5
,15
]}

Magliocchetti, M. ^{[16
]}

Maiolino, R. ^{[17
]}

Poglitsch, A. ^{[4
]}

Perez Garcia, A. ^{[13
]}

Sanchez-Portal, M. ^{[13
]}

Sturm, E. ^{[4
]}

Tacconi, L. ^{[4
]}

Valtchanov, I. ^{[13
]}

Amblard, A. ^{[18
]}

Arumugam, V. ^{[11
]}

Bethermin, M. ^{[7
]}

Bock, J. ^{[19
,20
]}

Boselli, A. ^{[6
]}

Buat, V. ^{[6
]}

Burgarella, D. ^{[6
]}

Castro-Rodriguez, N. ^{[14
,21
]}

Cava, A. ^{[22
]}

机构：

[1] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy

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

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

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

[5] ESO, D-85748 Garching, Germany

[6] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France

[7] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France

[8] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England

[9] Univ Trieste, Dipartimento Fis, Sez Astron, I-34131 Trieste, Italy

[10] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England

[11] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland

[12] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Bellville, South Africa

[13] ESA Herschel Sci Ctr, E-28692 Villafranca, Spain

[14] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Spain

[15] Univ Fed Rio de Janeiro, Observ Valongo, BR-21941 Rio De Janeiro, Brazil

[16] INAF IFSI, I-00133 Rome, Italy

[17] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England

[18] NASA, Ames Res Ctr, Moett Field, CA 94035 USA

[19] CALTECH, Pasadena, CA 91125 USA

[20] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[21] Univ La Laguna ULL, Dept Astrofis, E-38205 San Cristobal la Laguna, Spain

[22] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain

[23] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, 3Astrophys Grp, London SW7 2AZ, England

[24] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA

[25] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA

[26] NASA, Observ Cosmol Lab, Code 665, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[27] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales

[28] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA

[29] UK Astron Technol Ctr, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland

[30] ESTEC SRE SA, ESA Res & Sci Support Dept, NL-2201 AZ Noordwijk, Netherlands

[31] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France

[32] CNRS, UMR 8617, F-91405 Orsay, France

[33] CALTECH, Infrared Proc & Anal Ctr, JPL, Pasadena, CA 91125 USA

[34] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England

[35] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England

[36] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada

[37] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England

[38] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada

[39] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia

[40] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England

[41] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[42] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France

[43] Swiss Fed Inst Technol ETH Honggerberg, Inst Astron, CH-8093 Zurich, Switzerland

[44] Univ Toulouse, CNRS, Inst Rech Astrophys & Plantol, F-31400 Toulouse, France

[45] INAF Osservatorio Astron Padova, I-35122 Padua, Italy

[46] INAF IASF Milano, I-20133 Milan, Italy

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2013年 / 432卷 / 01期

关键词：

galaxies: active; galaxies: evolution; galaxies: luminosity function; mass function; galaxies: starburst; cosmology: observations; infrared: galaxies; STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; SUPERMASSIVE BLACK-HOLES; ORIGINS DEEP SURVEY; GOODS-SOUTH FIELD; REDSHIFT SURVEY; MU-M; PHOTOMETRIC REDSHIFTS; FORMATION HISTORY;

D O I：

10.1093/mnras/stt308

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We exploit the deep and extended far-IR data sets (at 70, 100 and 160 mu m) of the Herschel Guaranteed Time Observation (GTO) PACS Evolutionary Probe (PEP) Survey, in combination with the Herschel Multi-tiered Extragalactic Survey data at 250, 350 and 500 mu m, to derive the evolution of the rest-frame 35-, 60-, 90-and total infrared (IR) luminosity functions (LFs) up to z similar to 4. We detect very strong luminosity evolution for the total IR LF (L-IR alpha (1 + z)(3.55 +/- 0.10) up to z similar to 2, and. (1 + z) 1.62 similar to 0.51 at 2 < z less than or similar to 4) combined with a density evolution ( (1 + z)-0.57 +/- 0.22 up to z similar to 1 and. (1 + z)-3.92 +/- 0.34 at 1 < z less than or similar to 4). In agreement with previous findings, the IR luminosity density (.IR) increases steeply to z similar to 1, then flattens between z similar to 1 and z similar to 3 to decrease at z similar to 3. Galaxies with different spectral energy distributions, masses and specific star formation rates (SFRs) evolve in very different ways and this large and deep statistical sample is the first one allowing us to separately study the different evolutionary behaviours of the individual IR populations contributing to.IR. Galaxies occupying the well-established SFR-stellar mass main sequence (MS) are found to dominate both the total IR LF and.IR at all redshifts, with the contribution from off-MS sources (= 0.6 dex above MS) being nearly constant (similar to 20 per cent of the total IR) and showing no significant signs of increase with increasing z over the whole 0.8 < z < 2.2 range. Sources with mass in the range 10 = log(M/M-circle dot) = 11 are found to dominate the total IR LF, with more massive galaxies prevailing at the bright end of the high-z (greater than or similar to 2) LF. A two-fold evolutionary scheme for IR galaxies is envisaged: on the one hand, a starburst-dominated phase in which the Super Massive Black Holes (SMBH) grows and is obscured by dust (possibly triggered by a major merging event), is followed by an AGN-dominated phase, then evolving towards a local elliptical. On the other hand, moderately star-forming galaxies containing a low-luminosity AGN have various properties suggesting they are good candidates for systems in a transition phase preceding the formation of steady spiral galaxies.

引用

页码：23 / 52

页数：30

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