Young galaxy candidates in the Hubble Frontier Fields. III. MACS J0717.5+3745
- Instituto de Astrofísica and Centro de Astroingeniería, Facultad de Física, Pontificia Universidad Católica de Chile, Vicuña Mackenna 4860, 7820436 Macul, Santiago (Chile)
- Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 (United States)
- Instituto de Astronomía, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Cidade Universitária, 05508-090, São Paulo (Brazil)
- IRAP, CNRS—14 Avenue Edouard Belin—F-31400 Toulouse (France)
- Department of Theoretical Physics, University of Basque Country UPV/EHU, Bilbao (Spain)
- Smithsonian Astrophysical Observatory, 60 Garden St. MS09, Cambridge MA 02138 (United States)
- Department of Astronomy, University of Science and Technology of China, Hefei, Anhui 230026 (China)
- Instituto de Astrofísica de Canarias (IAC), E-38200 La Laguna, Tenerife (Spain)
- Department of Physics and Astronomy, Siena College, Loudonville, NY 12211 (United States)
- CAS Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China, Hefei, Anhui 230026 (China)
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, MC 249-17, Pasadena, CA 91125 (United States)
In this paper we present the results of our search for and study of z≳6 galaxy candidates behind the third Frontier Fields (FFs) cluster, MACS J0717.5+3745, and its parallel field, combining data from Hubble and Spitzer. We select 39 candidates using the Lyman break technique, for which the clear non-detection in optical make the extreme mid-z interlopers hypothesis unlikely. We also take benefit from z≳6 samples selected using the previous FF data sets of Abell 2744 and MACS 0416 to improve the constraints on the properties of very high redshift objects. We compute the redshift and the physical properties such emission lines properties, star formation rate, reddening, and stellar mass for all FF objects from their spectral energy distribution using templates including nebular emission lines. We study the relationship between several physical properties and confirm the trend already observed in previous surveys for evolution of star formation rate with galaxy mass and between the size and the UV luminosity of our candidates. The analysis of the evolution of the UV luminosity function with redshift seems more compatible with an evolution of density. Moreover, no robust z⩾8.5 object is selected behind the cluster field and few z∼9 candidates have been selected in the two previous data sets from this legacy survey, suggesting a strong evolution in the number density of galaxies between z∼8 and 9. Thanks to the use of the lensing cluster, we study the evolution of the star formation rate density produced by galaxies with L > 0.03 L{sup ⋆}, and confirm the strong decrease observed between z∼8 and 9.
- OSTI ID:
- 22890065
- Journal Information:
- Astrophysical Journal, Vol. 820, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Since 2009, the country of publication for this journal is the UK.; ISSN 0004-637X
- Country of Publication:
- United Kingdom
- Language:
- English
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