Volume 565, May 2014
|Number of page(s)||17|
|Section||Cosmology (including clusters of galaxies)|
|Published online||26 May 2014|
Intracluster light properties in the CLASH-VLT cluster MACS J1206.2-0847⋆
1 Dipartimento di Fisica, Univ. degli Studi di Trieste, via Tiepolo 11, 34143 Trieste, Italy
2 INAF/Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, 34143 Trieste, Italy
3 INAF/Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy
4 Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark
5 Dipartimento di Fisica e Scienze della Terra, Universita’ di Ferrara, via Saragat, 1, 44122 Ferrara, Italy
6 ICRAR, University of Western Australia, 35 Stirling Highway, Crawley, Western Australia 6009, Australia
7 INFN, Sezione di Trieste, via Valerio 2, 34127 Trieste, Italy
8 Department of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore MD 21218, USA
9 Instituto de Astrofísica de Andalucía (CSIC), C/Camino Bajo de Huétor 24, 18008 Granada, Spain
10 Department of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville NY 12211, USA
11 INAF/IASF-Milano, via Bassini 15, 20133 Milano, Italy
12 University of Vienna, Department of Astrophysics, Türkenschanzstr. 17, 1180 Wien, Austria
13 INAF/Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
14 INFN, Sezione di Bologna ; via Ranzani 1, 40127 Bologna, Italy
15 Dipartimento di Fisica, Universitá degli Studi di Milano, via Celoria 16, 20133 Milan, Italy
16 Department of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore MD 21218, USA
17 CEA Saclay, Orme des Merisiers, 91191 Gif-sur-Yvette, France
18 INAF/Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
19 Institut für Theoretische Astrophysik, Zentrum für Astronomie, Universität Heidelberg, Philosophenweg 12, 69120 Heidelberg, Germany
20 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore MD 21218, USA
21 Department of Theoretical Physics, University of the Basque Country, PO Box 644, 48080 Bilbao, Spain
22 Department of Physics and Astronomy, Michigan State University, East Lansing MI 48824, USA
23 Laboratoire AIM-Paris-Saclay, CEA/DSM-CNRS, Université Paris Diderot, Irfu/Service d’Astrophysique, CEA Saclay, Orme des Merisiers, 91191 Gif-sur-Yvette, France
24 Department of Astronomy, University of California, Berkeley CA, USA
25 Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA
26 Observatories of the Carnegie Institution of Washington, Pasadena, CA 91 101, USA
27 Department of Physics, The Ohio State University, Columbus, OH, USA
28 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr, Pasadena, CA 91109, USA
29 European Laboratory for Particle Physics (CERN), 1211, Geneva 23, Switzerland
30 University Observatory Munich, Scheinerstrasse 1, 81679 München, Germany
31 Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., 85741 Garching, Germany
32 Institute of Astronomy and Astrophysics, Academia Sinica, PO Box 23-141, 10617 Taipei, Taiwan
33 Cahill Center for Astronomy and Astrophysics, California Institute of Technology, MS 249-17, Pasadena CA 91125, USA
Received: 13 December 2013
Accepted: 11 March 2014
Aims. We aim constrain the assembly history of clusters by studying the intracluster light (ICL) properties, estimating its contribution to the fraction of baryons in stars, f∗, and understanding possible systematics or bias using different ICL detection techniques.
Methods. We developed an automated method, GALtoICL, based on the software GALAPAGOS, to obtain a refined version of typical BCG+ICL maps. We applied this method to our test case MACS J1206.2-0847, a massive cluster located at z ~ 0.44, which is part of the CLASH sample. Using deep multiband Subaru images, we extracted the surface brightness (SB) profile of the BCG+ICL and studied the ICL morphology, color, and contribution to f∗ out to R500. We repeated the same analysis using a different definition of the ICL, SBlimit method, i.e., a SB cut-off level, to compare the results.
Results. The most peculiar feature of the ICL in MACS1206 is its asymmetric radial distribution, with an excess in the SE direction and extending toward the second brightest cluster galaxy, which is a post starburst galaxy. This suggests an interaction between the BCG and this galaxy that dates back to τ ≤ 1.5 Gyr. The BCG+ICL stellar content is ~8% of M∗,500, and the (de-) projected baryon fraction in stars is f∗ = 0.0177(0.0116), in excellent agreement with recent results. The SBlimit method provides systematically higher ICL fractions and this effect is stronger at lower SB limits. This is due to the light from the outer envelopes of member galaxies that contaminate the ICL. Though more time consuming, the GALtoICL method provides safer ICL detections that are almost free of this contamination. This is one of the few ICL study at redshift z > 0.3. At completion, the CLASH/VLT program will allow us to extend this analysis to a statistically significant cluster sample spanning a wide redshift range: 0.2 ≲ z ≲ 0.6.
Key words: galaxies: clusters: individual: MACS J1206.2-0847 / cosmology: observations
© ESO, 2014
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