ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: THE INFRARED EXCESS OF UV-SELECTED z=2-10 GALAXIES AS A FUNCTION OF UV-CONTINUUM SLOPE AND STELLAR MASS

被引：240

作者：

Bouwens, Rychard J. ^{[1
]}

Aravena, Manuel ^{[2
]}

Decarli, Roberto ^{[3
]}

Walter, Fabian ^{[3
,4
,5
]}

Da Cunha, Elisabete ^{[6
,7
]}

Labbe, Ivo ^{[1
]}

Bauer, Franz E. ^{[8
,9
,10
]}

Bertoldi, Frank ^{[11
]}

Carilli, Chris ^{[5
,12
]}

Chapman, Scott ^{[13
]}

Daddi, Emanuele ^{[14
]}

Hodge, Jacqueline ^{[1
]}

Ivison, Rob J. ^{[15
,16
]}

Karim, Alex ^{[11
]}

Le Fevre, Olivier ^{[17
]}

Magnelli, Benjamin ^{[11
]}

Ota, Kazuaki ^{[12
]}

Riechers, Dominik ^{[18
]}

Smail, Ian R. ^{[19
]}

van der Werf, Paul ^{[1
]}

Weiss, Axel ^{[11
]}

Cox, Pierre ^{[20
]}

Elbaz, David ^{[14
]}

Gonzalez-Lopez, Jorge ^{[8
]}

Infante, Leopoldo ^{[8
]}

Oesch, Pascal ^{[21
]}

Wagg, Jeff ^{[22
]}

Wilkins, Steve ^{[23
]}

机构：

[1] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands

[2] Univ Diego Portales, Nucleo Astron, Fac Ingn, Av Ejercito 441, Santiago, Chile

[3] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[4] CALTECH, Dept Astron, MC105-24, Pasadena, CA 91125 USA

[5] NRAO, Pete V Domenici Array Sci Ctr, POB O, Socorro, NM 87801 USA

[6] Swinburne Univ Technol, Ctr Astrophys & Supercomputing, Hawthorn, Vic 3122, Australia

[7] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia

[8] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile

[9] Millennium Inst Astrophys, Nuncio Monsenor Sotero Sanz 100, Santiago, Chile

[10] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA

[11] Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany

[12] Univ Cambridge, Cavendish Lab, 19 JJ Thomson Ave, Cambridge CB3 0HE, England

[13] Dalhousie Univ, Halifax, NS, Canada

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

[15] European Southern Observ, Alonso de Cordova 3107,Casilla 19001, Vitacura Santiago, Chile

[16] Univ Edinburgh, Royal Observ, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland

[17] IRAM, 300 Rue Piscine, F-38406 St Martin Dheres, France

[18] Cornell Univ, 220 Space Sci Bldg, Ithaca, NY 14853 USA

[19] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England

[20] Joint ALMA Observ ESO, Av Alonso de Cordova, Santiago 3104, Chile

[21] Yale Univ, Dept Astron, New Haven, CT 06511 USA

[22] SKA Org, Lower Withington, Cheshire, England

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

来源：

ASTROPHYSICAL JOURNAL | 2016年 / 833卷 / 01期

基金：

美国国家科学基金会;

关键词：

galaxies: evolution; galaxies: ISM; galaxies: star formation; galaxies: statistics; instrumentation: interferometers; submillimeter: galaxies; STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; SIMILAR-TO; 7; SPECTRAL ENERGY-DISTRIBUTIONS; FORMATION RATE DENSITY; ULTRAVIOLET LUMINOSITY DENSITY; HIGH-REDSHIFT GALAXIES; REST-FRAME ULTRAVIOLET; LESS-THAN; C II LINE;

D O I：

10.3847/1538-4357/833/1/72

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We make use of deep 1.2 mm continuum observations (12.7 mu Jy beam(-1) rms) of a 1 arcmin(2) region in the Hubble Ultra Deep Field to probe dust-enshrouded star formation from 330 Lyman-break galaxies spanning the redshift range z = 2-10 (to similar to 2-3 M-circle dot yr(-1) at 1 sigma over the entire range). Given the depth and area of ASPECS, we would expect to tentatively detect 35 galaxies, extrapolating the Meurer z similar to 0 IRX-beta relation to z >= 2 (assuming dust temperature T-d similar to 35 K). However, only six tentative detections are found at z greater than or similar to 2 in ASPECS, with just three at > 3 sigma. Subdividing our z = 2-10 galaxy samples according to stellar mass, UV luminosity, and UV-continuum slope and stacking the results, we find a significant detection only in the most massive (>10(9.75) M-circle dot) subsample, with an infrared excess (IRX = L-IR/L-UV) consistent with previous z similar to 2 results. However, the infrared excess we measure from our large selection of sub-L* (<10(9.75) M-circle dot) galaxies is 0.11(-0.32)(+0.42) +/- 0.34 (bootstrap and formal uncertainties) and 0.14(0.14)(+0.15) +/- 0.18 at z = 2-3 and z = 4-10, respectively, lying below even an IRX-beta relation for the Small Magellanic Cloud (95% confidence). These results demonstrate the relevance of stellar mass for predicting the IR luminosity of z greater than or similar to 2 galaxies. We find that the evolution of the IRX-stellar mass relationship depends on the evolution of the dust temperature. If the dust temperature increases monotonically with redshift (proportional to(1 + z)(0.32)) such that T-d similar to 44-50 K at z >= 4, current results are suggestive of little evolution in this relationship to z similar to 6. We use these results to revisit recent estimates of the z >= 3 star formation rate density.

引用

页数：32

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