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Published May 2014 | Submitted + Published
Journal Article Open

Intracluster light properties in the CLASH-VLT cluster MACS J1206.2-0847

Abstract

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 R_(500). 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.

Additional Information

© 2014 ESO. Article published by EDP Sciences. Received 13 December 2013; Accepted 11 March 2014; Published online 26 May 2014. Based on data collected at the NASJ Subaru telescope, at the ESO VLT (prog.ID 186.A-0798), and the NASA HST. We thank the anonymous referee for constructive comments that helped us to improve the manuscript. V.P. is grateful to Monaco, P., Murante, G., and De Grandi, S. for useful discussion and comments. V.P. acknowledges the grant "Cofinanziamento di Ateneo 2010" and financial support from PRIN-INAF2010 and MIUR PRIN2010-2011 (J91J12000450001). W.C. acknowledges a fellowship from the European Commission's Framework Programme 7, through the Marie Curie Initial Training Network CosmoComp (PITN-GA-2009-238356), supports from ARC DP130100117 and from the Survey Simulation Pipeline (SSimPL; http://ssimpl-universe.tk/). A.F. acknowledges the support by INAF through VIPERS grants PRIN 2008 and PRIN 2010. The work of LAM was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for A.Z. is provided by NASA through Hubble Fellowship grant #HST-HF- 51334.01-A awarded by STScI.

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Submitted - 1403.4979v1.pdf

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Created:
August 22, 2023
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October 26, 2023