CONSTRAINTS ON PHOTOIONIZATION FEEDBACK FROM NUMBER COUNTS OF ULTRA-FAINT HIGH-REDSHIFT GALAXIES IN THE FRONTIER FIELDS

被引：27

作者：

Castellano, M. ^{[1
]}

Yue, B. ^{[2
]}

Ferrara, A. ^{[2
,3
]}

Merlin, E. ^{[1
]}

Fontana, A. ^{[1
]}

Amorin, R. ^{[1
]}

Grazian, A. ^{[1
]}

Marmol-Queralto, E. ^{[4
]}

Michalowski, M. J. ^{[4
]}

Mortlock, A. ^{[4
]}

Paris, D. ^{[1
]}

Parsa, S. ^{[4
]}

Pilo, S. ^{[1
]}

Santini, P. ^{[1
]}

机构：

[1] INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, RM, Italy

[2] Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy

[3] Univ Tokyo, Todai Inst Adv Study, Kavli IPMU WPI, Tokyo, Japan

[4] Univ Edinburgh, Royal Observ, Inst Astron, SUPA,Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2016年 / 823卷 / 02期

基金：

欧洲研究理事会;

关键词：

dark ages; reionization; first stars; galaxies: high-redshift; UV LUMINOSITY FUNCTIONS; WARM DARK-MATTER; RADIATIVE FEEDBACK; REIONIZATION; DENSITY; PHOTOMETRY; EVOLUTION; IMPACT; EPOCH; A2744;

D O I：

10.3847/2041-8205/823/2/L40

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We exploit a sample of ultra-faint high-redshift galaxies (demagnified Hubble Space Telescope, HST, H160 magnitude > 30) in the Frontier Fields clusters A2744 and M0416 to constrain a theoretical model for the UV luminosity function in the presence of photoionization feedback. The objects have been selected on the basis of accurate photometric redshifts computed from multi-band photometry including seven HST bands and deep K-s and IRAC observations. Magnification is computed on an object-by-object basis from all available lensing models of the two clusters. We take into account source detection completeness as a function of luminosity and size, magnification effects, and systematics in the lens modeling of the clusters under investigation. We find that our sample of high-z galaxies constrain the cutoff halo circular velocity below which star formation is suppressed by photoionization feedback to v(c)(cut) < 50 km s(-1). This circular velocity corresponds to a halo mass of approximate to 5.6 x 10(9) M-circle dot and approximate to 2.3 x 10(9) M-circle dot at z = 5 and 10, respectively: higher-mass halos can thus sustain continuous star formation activity without being quenched by external ionizing flux. More stringent constraints are prevented by the uncertainty in the modeling of the cluster lens, as embodied by systematic differences among the lens models available.

引用

页数：6

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