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Improved strong lensing modelling of galaxy clusters using the Fundamental Plane: Detailed mapping of the baryonic and dark matter mass distribution of Abell S1063

Granata, G. and Mercurio, A. and Grillo, C. and Tortorelli, L. and Bergamini, P. and Meneghetti, M. and Rosati, P. and Caminha, G. B. and Nonino, M. (2022) Improved strong lensing modelling of galaxy clusters using the Fundamental Plane: Detailed mapping of the baryonic and dark matter mass distribution of Abell S1063. Astronomy and Astrophysics, 659 . Art. No. A24. ISSN 0004-6361. doi:10.1051/0004-6361/202141817. https://resolver.caltech.edu/CaltechAUTHORS:20220301-900063000

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Abstract

Aims. From accurate photometric and spectroscopic information, we build the Fundamental Plane (FP) relation for the early-type galaxies of the cluster Abell S1063. We use this relation to develop an improved strong lensing model of the cluster, and we decompose the cluster’s cumulative projected total mass profile into its stellar, hot gas, and dark matter mass components. We compare our results with the predictions of cosmological simulations. Methods. We calibrate the FP using Hubble Frontier Fields photometry and data from the Multi Unit Spectroscopic Explorer on the Very Large Telescope. The FP allows us to determine the velocity dispersions of all 222 cluster members included in the model from their measured structural parameters. As for their truncation radii, we test a proportionality relation with the observed half-light radii. Fixing the mass contribution of the hot gas component from X-ray data, the mass density distributions of the diffuse dark matter haloes are optimised by comparing the observed and model-predicted positions of 55 multiple images of 20 background sources distributed over the redshift range 0.73 − 6.11. We determine the uncertainties on the model parameters with Monte Carlo Markov chains. Results. We find that the most accurate predictions of the positions of the multiple images are obtained when the truncation radii of the member galaxies are approximately 2.3 times their effective radii. Compared to earlier work on the same cluster, our model allows for the inclusion of some scatter on the relation between the total mass and the velocity dispersion of the cluster members. We notice a lower statistical uncertainty on the value of some model parameters. For instance, the main dark matter halo of the cluster has a core radius of 86 ± 2 kpc: the uncertainty on this value decreases by more than 30% with respect to previous work. Taking advantage of a new estimate of the stellar mass of all cluster members from the HST multi-band data, we measure the cumulative two-dimensional mass profiles out to a radius of 350 kpc for all baryonic and dark matter components of the cluster. At the outermost radius of 350 kpc, we obtain a baryon fraction of 0.147 ± 0.002. We study the stellar-to-total mass fraction of the high-mass cluster members in our model, finding good agreement with the observations of wide galaxy surveys and some disagreement with the predictions of halo occupation distribution studies based on N-body simulations. Finally, we compare the features of the sub-haloes as described by our model with those predicted by high-resolution hydrodynamical simulations. We obtain compatible results in terms of the stellar over total mass fraction. On the other hand, we report some discrepancies both in terms of the maximum circular velocity, which is an indication of the halo compactness, and the sub-halo total mass function in the central cluster regions.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1051/0004-6361/202141817DOIArticle
https://arxiv.org/abs/2107.09079arXivDiscussion Paper
ORCID:
AuthorORCID
Granata, G.0000-0002-9512-3788
Mercurio, A.0000-0001-9261-7849
Grillo, C.0000-0002-5926-7143
Tortorelli, L.0000-0002-8012-7495
Bergamini, P.0000-0003-1383-9414
Meneghetti, M.0000-0003-1225-7084
Rosati, P.0000-0002-6813-0632
Caminha, G. B.0000-0001-6052-3274
Nonino, M.0000-0001-6342-9662
Alternate Title:Improved strong lensing modelling of galaxy clusters using the Fundamental Plane: the case of Abell S1063
Additional Information:© ESO 2022. Received: 16 July 2021. Accepted: 3 January 2022. We thank the anonymous referee for some useful suggestions that helped to improve the paper. We acknowledge financial support by PRIN-MIUR 2017WSCC32 “Zooming into dark matter and proto-galaxies with massive lens-ing clusters” (P.I.: P. Rosati), INAF “main-stream” 1.05.01.86.20 (P.I.: M. Nonino) and INAF 1.05.01.86.31 (P.I.: E. Vanzella). G.G. thanks Ana Acebron Muñoz and Andrea Bolamperti for their help and suggestions. P.B. acknowledges financial support from ASI through the agreement ASI-INAF n. 2018-29-HH.0. M.M. acknowledges support from ASI through the grants ASI-INAF n. 2018-23-HH.0 and ASI-INAF n. 2017-14-H.0. G.B.C. acknowledges the Max Planck Society for financial support through the Max Planck Research Group for S.H. Suyu and the academic support from the German Centre for Cosmological Lensing.
Funders:
Funding AgencyGrant Number
Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR)2017WSCC32
Istituto Nazionale di Astrofisica (INAF)1.05.01.86.20
Istituto Nazionale di Astrofisica (INAF)1.05.01.86.31
Agenzia Spaziale Italiana (ASI)2018-29-HH.0
Agenzia Spaziale Italiana (ASI)2018-23-HH.0
Agenzia Spaziale Italiana (ASI)2017-14-H.0
Max Planck SocietyUNSPECIFIED
Subject Keywords:gravitational lensing: strong / galaxies: clusters: general / galaxies: clusters: individual: Abell S1063 / galaxies: kinematics and dynamics / dark matter / cosmology: observations
DOI:10.1051/0004-6361/202141817
Record Number:CaltechAUTHORS:20220301-900063000
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20220301-900063000
Official Citation:Improved strong lensing modelling of galaxy clusters using the Fundamental Plane: Detailed mapping of the baryonic and dark matter mass distribution of Abell S1063 G. Granata, A. Mercurio, C. Grillo, L. Tortorelli, P. Bergamini, M. Meneghetti, P. Rosati, G. B. Caminha and M. Nonino A&A, 659 (2022) A24 DOI: https://doi.org/10.1051/0004-6361/202141817
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:113671
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:02 Mar 2022 00:08
Last Modified:02 Mar 2022 00:08

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