High redshift galaxies in the ALHAMBRA survey I. Selection method and number counts based on redshift PDFs

被引：10

作者：

Viironen, K. ^{[1
]}

Marin-Franch, A. ^{[1
]}

Lopez-Sanjuan, C. ^{[1
]}

Varela, J. ^{[1
]}

Chaves-Montero, J. ^{[1
]}

Cristobal-Hornillos, D. ^{[1
]}

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

Fernandez-Soto, A. ^{[4
,5
]}

Vilella-Rojo, G. ^{[1
]}

Ascaso, B. ^{[3
,6
]}

Cenarro, A. J. ^{[1
]}

Cervino, M. ^{[3
,7
,8
]}

Cepa, J. ^{[7
,8
]}

Ederoclite, A. ^{[1
]}

Marquez, I. ^{[3
]}

Masegosa, J. ^{[3
]}

Moles, M. ^{[1
,3
]}

Oteo, I. ^{[9
,10
]}

Povic, M. ^{[3
]}

Aguerri, J. A. L. ^{[7
,8
]}

Alfaro, E. ^{[3
]}

Aparicio-Villegas, T. ^{[3
,11
]}

Benitez, N. ^{[3
]}

Broadhurst, T. ^{[12
]}

Cabrera-Cano, J. ^{[13
]}

Castander, J. F. ^{[14
]}

Del Olmo, A. ^{[3
]}

Gonzalez Delgado, R. M. ^{[3
]}

Husillos, C. ^{[3
]}

Infante, L. ^{[15
]}

Martinez, V. J. ^{[5
,16
]}

Perea, J. ^{[3
]}

Prada, F. ^{[3
]}

Quintana, J. M. ^{[3
]}

机构：

[1] Ctr Estudios Fis Cosmos Aragon, Teruel 44001, Spain

[2] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508090 Sao Paulo, Brazil

[3] CSIC, IAA, E-18008 Granada, Spain

[4] Inst Fis Cantabria, Santander 39005, Spain

[5] Unidad Asociada Observatori Astron IFCA UV, Paterna 46980, Spain

[6] Observ Paris, GEPI, F-75014 Paris, France

[7] Inst Astrofis Canarias, Tenerife 38200, Spain

[8] Univ La Laguna, Fac Fis, Dept Astrophys, San Cristobal la Laguna 38200, Spain

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

[10] European So Observ, D-85748 Garching, Germany

[11] COAA, Observatorio Nacl, BR-20921400 Rio De Janeiro, Brazil

[12] Univ Basque Country UPV EHU, Dept Theoret Phys, Bilbao, Spain

[13] Univ Seville, Fac Fis, Dept Fis Atom Mol & Nucl, E-41012 Seville, Spain

[14] CSIC, ICE, Fac Ciencies, Bellaterra 08193, Spain

[15] Ponticia Univ Catolica, Dept Astron, Santiago, Chile

[16] Univ Valencia, Dept Astron & Astrofis, E-46100 Burjassot, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2015年 / 576卷

基金：

欧洲研究理事会; 西班牙国家研究理事会;

关键词：

galaxies: evolution; galaxies: distances and redshifts; galaxies: high-redshift; galaxies: statistics; LYMAN-BREAK GALAXIES; STAR-FORMING GALAXIES; REST-FRAME ULTRAVIOLET; SUBARU DEEP FIELDS; PHOTOMETRIC REDSHIFT; SPECTROSCOPIC SURVEY; DATA RELEASE; LUMINOSITY FUNCTIONS; FORMATION RATES; STELLAR MASSES;

D O I：

10.1051/0004-6361/201425382

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Most observational results on the high redshift restframe UV-bright galaxies are based on samples pinpointed using the so-called dropout technique or Ly-alpha selection. However, the availability of multifilter data now allows the dropout selections to be replaced by direct methods based on photometric redshifts. In this paper we present the methodology to select and study the population of high redshift galaxies in the ALHAMBRA survey data. Aims. Our aim is to develop a less biased methodology than the traditional dropout technique to study the high redshift galaxies in ALHAMBRA and other multifilter data. Thanks to the wide area ALHAMBRA covers, we especially aim at contributing to the study of the brightest, least frequent, high redshift galaxies. Methods. The methodology is based on redshift probability distribution functions (zPDFs). It is shown how a clean galaxy sample can be obtained by selecting the galaxies with high integrated probability of being within a given redshift interval. However, reaching both a complete and clean sample with this method is challenging. Hence, a method to derive statistical properties by summing the zPDFs of all the galaxies in the redshift bin of interest is introduced. Results. Using this methodology we derive the galaxy rest frame UV number counts in five redshift bins centred at z = 2.5, 3.0, 3.5, 4.0, and 4.5, being complete up to the limiting magnitude at mUV(AB) = 24, where mUV refers to the first ALHAMBRA filter redwards of the Ly-alpha line. With the wide field ALHAMBRA data we especially contribute to the study of the brightest ends of these counts, accurately sampling the surface densities down to mUV(AB) = 21-22. Conclusions. We show that using the zPDFs it is easy to select a very clean sample of high redshift galaxies. We also show that it is better to do statistical analysis of the properties of galaxies using a probabilistic approach, which takes into account both the incompleteness and contamination issues in a natural way.

引用

页数：15

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