The galaxy stellar mass function at 3.5 ≤ z ≤ 7.5 in the CANDELS/UDS, GOODS-South, and HUDF fields

被引：233

作者：

Grazian, A. ^{[1
]}

Fontana, A. ^{[1
]}

Santini, P. ^{[1
]}

Dunlop, J. S. ^{[2
]}

Ferguson, H. C. ^{[3
]}

Castellano, M. ^{[1
]}

Amorin, R. ^{[1
]}

Ashby, M. L. N. ^{[4
]}

Barro, G. ^{[5
]}

Behroozi, P. ^{[3
]}

Boutsia, K. ^{[1
]}

Caputi, K. I. ^{[6
]}

Chary, R. R. ^{[7
]}

Dekel, A. ^{[8
]}

Dickinson, M. E. ^{[9
]}

Faber, S. M. ^{[5
]}

Fazio, G. G. ^{[4
]}

Finkelstein, S. L. ^{[10
]}

Galametz, A. ^{[11
]}

Giallongo, E.

Giavalisco, M. ^{[12
]}

Grogin, N. A. ^{[3
]}

Guo, Y. ^{[5
]}

Kocevski, D. ^{[13
]}

Koekemoer, A. M. ^{[3
]}

Koo, D. C. ^{[5
]}

Lee, K. -S. ^{[14
]}

Lu, Y. ^{[15
,16
]}

Merlin, E. ^{[1
]}

Mobasher, B. ^{[17
]}

Nonino, M. ^{[18
]}

Papovich, C. ^{[19
]}

Paris, D. ^{[1
]}

Pentericci, L. ^{[1
]}

Reddy, N. ^{[17
]}

Renzini, A. ^{[20
]}

Salmon, B. ^{[19
]}

Salvato, M. ^{[11
]}

Sommariva, V. ^{[21
]}

Song, M. ^{[10
]}

Vanzella, E. ^{[22
]}

机构：

[1] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy

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

[3] Space Telescope Sci Inst, Baltimore, MD 21218 USA

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

[5] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA

[6] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands

[7] CALTECH, Pasadena, CA 91125 USA

[8] Hebrew Univ Jerusalem, Racah Inst Phys, Ctr Astrophys & Planetary Sci, IL-91904 Jerusalem, Israel

[9] Natl Opt Astron Observ, Tucson, AZ 85719 USA

[10] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA

[11] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[12] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA

[13] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA

[14] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA

[15] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA

[16] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA

[17] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA

[18] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy

[19] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA

[20] Osserv Astron Padova, INAF, I-35122 Padua, Italy

[21] Univ Bologna, Dept Phys & Astron DIFA, I-40127 Bologna, Italy

[22] Osservatorio Astron Bologna, INAF, Bologna, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2015年 / 575卷

基金：

美国国家科学基金会;

关键词：

galaxies: luminosity function; mass function; galaxies: distances and redshifts; galaxies: evolution; galaxies: high-redshift; STAR-FORMATION RATES; LYMAN BREAK GALAXIES; ORIGINS DEEP SURVEY; HIGH-REDSHIFT GALAXIES; GIANT BRANCH STARS; LUMINOSITY FUNCTION; NEBULAR EMISSION; FORMATION HISTORIES; QUIESCENT GALAXIES; FORMING GALAXIES;

D O I：

10.1051/0004-6361/201424750

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The form and evolution of the galaxy stellar mass function (GSMF) at high redshifts provide crucial information on star formation history and mass assembly in the young Universe, close or even prior to the epoch of reionization. Aims. We used the unique combination of deep optical/near-infrared/mid-infrared imaging provided by HST, Spitzer, and the VLT in the CANDELS-UDS. GOODS-South, and HUDF fields to determine the GSMF over the redshift range 3.5 <= z <= 7.5. Methods. We used the LIST WEC3/IR near-infrared imaging from CANDELS and HUDF09, reaching H similar or equal to 27-28.5 over a total area of 369 arcmin(2), in combination with associated deep usT ACS optical data, deep Spitzer IRAC imaging from the SEDS programme, and deep Y and K-band VI l Hawk-I images from the ElliGS programme, to select a galaxy sample with high-quality photometric redshifts. These have been calibrated with more than 150 spectroscopic redshifts in the range 3.5 <= z <= 7.5, resulting in an overall precision of sigma(z)/(1 + z) similar to 0.037. With this database we have determined the low-mass end of the high-redshift GSMF with unprecedented precision, reaching down to masses as low as M* similar to 10(9) M-circle dot at z = 4 and similar to 6 x 10(9) M-circle dot at z = 7. Results. We find that the GSMF at 3.5 <= z <= 7.5 depends only slightly on the recipes adopted to measure the stellar masses, namely the photometric redshifts, the star formation histories, the nebular contribution, or the presence of AGN in the parent sample. The low-mass end of the GSMF is steeper than has been found at lower redshifts, but appears to be unchanged over the redshift range probed here. Meanwhile the high-mass end of the GSMF appears to evolve primarily in density, although there is also some evidence of evolution in characteristic mass. Our results are very different from previous mass function estimates based on converting UV galaxy luminosity functions into mass functions via tight mass-to-light relations. Integrating our evolving GSMF over mass, we find that the growth of stellar mass density is barely consistent with the time-integral of the star formation rate (lensity over cosmic time at z > 4. Conclusions. These results confirm the unique synergy of the CANDELS+HUDF, and SIDS surveys for the discovery and study of moderate/low-mass galaxies at high iredshifts, and reaffirm the importance of space-based infrared selection for the unbiased measurement of the evolving GSMF in the young Universe.

引用

页数：25

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