The Kormendy relation of galaxies in the Frontier Fields clusters: Abell S1063 and MACS J1149.5+2223
Abstract
We analyse the Kormendy relations (KRs) of the two Frontier Fields clusters, Abell S1063, at z = 0.348, and MACS J1149.5+2223, at z = 0.542, exploiting very deep Hubble Space Telescope photometry and Very Large Telescope (VLT)/Multi Unit Spectroscopic Explorer (MUSE) integral field spectroscopy. With this novel data set, we are able to investigate how the KR parameters depend on the cluster galaxy sample selection and how this affects studies of galaxy evolution based on the KR. We define and compare four different galaxy samples according to (a) Sérsic indices: early-type ('ETG'), (b) visual inspection: 'ellipticals', (c) colours: 'red', (d) spectral properties: 'passive'. The classification is performed for a complete sample of galaxies with m_(F814W) ≤ 22.5 ABmag (M* ≳ 10^(10.0) M⊙). To derive robust galaxy structural parameters, we use two methods: (1) an iterative estimate of structural parameters using images of increasing size, in order to deal with closely separated galaxies and (2) different background estimations, to deal with the intracluster light contamination. The comparison between the KRs obtained from the different samples suggests that the sample selection could affect the estimate of the best-fitting KR parameters. The KR built with ETGs is fully consistent with the one obtained for ellipticals and passive. On the other hand, the KR slope built on the red sample is only marginally consistent with those obtained with the other samples. We also release the photometric catalogue with structural parameters for the galaxies included in the present analysis.
Additional Information
© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2018 March 5. Received 2018 February 19; in original form 2017 November 7. Published: 08 March 2018. The authors thank the anonymous referee for its useful and constructive comments that helped to improve the quality of this paper. We also thank Dr. Peng and Dr. Cappellari for their precious advices on how to properly manage GALFIT and PPXF, respectively, and Elisabete da Cunha for providing us with a non-public library of models for the MAGPHYS SED-fitting procedure. We acknowledge financial support from the Progetti di ricerca INAF di rilevante interesse nazionelé (PRIN-INAF) 2014 1.05.01.94.02 (PI: M. Nonino). A.M. acknowledges funding from the INAF PRIN-SKA 2017 programme 1.05.01.88.04. M.P. acknowledges support from the PRIN-INAF 2014 'Fornax Cluster Imaging and Spectroscopic Deep Survey'. The CLASH Multi-Cycle Treasury Programme is based on observations made with the National Aeronautics and Space Administration (NASA)/European Space Agency (ESA) HST. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). The Space Telescope Science Institute (STScI) is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Based on observations made with the ESO/VLT at Cerro Paranal under programme IDs 60.A-9345(A), 095.A-0653(A), 294.A-5032(A), and 186.A-0798(A).Attached Files
Published - sty617.pdf
Accepted Version - 1803.02375.pdf
Supplemental Material - sty617_supp.zip
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Additional details
- Eprint ID
- 86839
- Resolver ID
- CaltechAUTHORS:20180606-111123696
- 1.05.01.94.02
- Istituto Nazionale di Astrofisica (INAF)
- 1.05.01.88.04
- Istituto Nazionale di Astrofisica (INAF)
- NAS 5-26555
- NASA
- Created
-
2018-06-06Created from EPrint's datestamp field
- Updated
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2021-11-15Created from EPrint's last_modified field
- Caltech groups
- Infrared Processing and Analysis Center (IPAC)