dc.contributor.author Shetty, Shravan dc.contributor.author Cappellari, Michele dc.contributor.author McDermid, Richard M. dc.contributor.author Krajnovic, Davor dc.contributor.author Zeeuw, P. T. de dc.contributor.author Davies, Roger L. dc.contributor.author Kobayashi, Chiaki dc.date.accessioned 2020-10-09T00:09:25Z dc.date.available 2020-10-09T00:09:25Z dc.date.issued 2020-04-26 dc.identifier.citation Shetty , S , Cappellari , M , McDermid , R M , Krajnovic , D , Zeeuw , P T D , Davies , R L & Kobayashi , C 2020 , ' A Precise Benchmark for Cluster Scaling Relations: Fundamental Plane, Mass Plane and IMF in the Coma Cluster from Dynamical Models ' , Monthly Notices of the Royal Astronomical Society . https://doi.org/10.1093/mnras/staa1043 dc.identifier.issn 0035-8711 dc.identifier.other PURE: 21253709 dc.identifier.other PURE UUID: 874438a3-17e6-4691-bc52-27a8cb7e4025 dc.identifier.other ArXiv: http://arxiv.org/abs/2004.07449v1 dc.identifier.other ORCID: /0000-0002-4343-0487/work/81741562 dc.identifier.uri http://hdl.handle.net/2299/23222 dc.description This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. https://doi.org/10.1093/mnras/staa1043. dc.description.abstract We study a sample of 148 early-type galaxies in the Coma cluster using SDSS photometry and spectra, and calibrate our results using detailed dynamical models for a subset of these galaxies, to create a precise benchmark for dynamical scaling relations in high-density environments. For these galaxies, we successfully measured global galaxy properties, modeled stellar populations, and created dynamical models, and support the results using detailed dynamical models of 16 galaxies, including the two most massive cluster galaxies, using data taken with the SAURON IFU. By design, the study provides minimal scatter in derived scaling relations due to the small uncertainty in the relative distances of galaxies compared to the cluster distance. Our results demonstrate low ($\leq$55% for 90$^{th}$ percentile) dark matter fractions in the inner 1$R_{\rm e}$ ~of galaxies. Owing to the study design, we produce the tightest, to our knowledge, IMF-$\sigma_e$ relation of galaxies, with a slope consistent with that seen in local galaxies. Leveraging our dynamical models, we transform the classical Fundamental Plane of the galaxies to the Mass Plane. We find that the coefficients of the mass plane are close to predictions from the virial theorem, and have significantly lower scatter compared to the Fundamental plane. We show that Coma galaxies occupy similar locations in the (M$_*$ - $R_{\rm e}$) and (M$_*$ - $\sigma_e$) relations as local field galaxies but are older. This, and the fact we find only three slow rotators in the cluster, is consistent with the scenario of hierarchical galaxy formation and expectations of the kinematic morphology-density relation. en dc.language.iso eng dc.relation.ispartof Monthly Notices of the Royal Astronomical Society dc.subject astro-ph.GA dc.title A Precise Benchmark for Cluster Scaling Relations: Fundamental Plane, Mass Plane and IMF in the Coma Cluster from Dynamical Models en dc.contributor.institution Centre for Astrophysics Research dc.contributor.institution School of Physics, Astronomy and Mathematics dc.description.status Peer reviewed rioxxterms.version AM rioxxterms.versionofrecord https://doi.org/10.1093/mnras/staa1043 rioxxterms.type Journal Article/Review herts.preservation.rarelyaccessed true
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