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  • 2103.12753v1

    Rights statement: This is an author-created, un-copyedited version of an article accepted for publication/published in the Astrophysical journal. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at doi:10.3847/1538-4357/abf1e7

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The Fundamental Plane in the LEGA-C Survey: unraveling the $M/L$ variations of massive star-forming and quiescent galaxies at $z\sim0.8$

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  • Anna de Graaff
  • Rachel Bezanson
  • Marijn Franx
  • Arjen van der Wel
  • Bradford Holden
  • Jesse van de Sande
  • Eric F. Bell
  • Francesco D'Eugenio
  • Michael V. Maseda
  • Adam Muzzin
  • David Sobral
  • Caroline M. S. Straatman
  • Po-Feng Wu
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Article number103
<mark>Journal publication date</mark>1/06/2021
<mark>Journal</mark>The Astrophysical Journal
Issue number2
Volume913
Publication StatusPublished
Early online date28/05/21
<mark>Original language</mark>English

Abstract

We explore the connection between the kinematics, structures and stellar populations of massive galaxies at $0.610.5$) galaxies that span a wide range in morphology, star formation activity and environment, and therefore is representative of the massive galaxy population at $z\sim0.8$. We find that quiescent and star-forming galaxies occupy the parameter space of the $g$-band FP differently and thus have different distributions in the dynamical mass-to-light ratio ($M_{\rm dyn}/L_g$), largely owing to differences in the stellar age and recent star formation history, and, to a lesser extent, the effects of dust attenuation. In contrast, we show that both star-forming and quiescent galaxies lie on the same mass FP at $z\sim 0.8$, with a comparable level of intrinsic scatter about the plane. We examine the variation in $M_{\rm dyn}/M_*$ through the thickness of the mass FP, finding no significant residual correlations with stellar population properties, S\'ersic index, or galaxy overdensity. Our results suggest that, at fixed size and velocity dispersion, the variations in $M_{\rm dyn}/L_g$ of massive galaxies reflect an approximately equal contribution of variations in $M_*/L_g$, and variations in the dark matter fraction or initial mass function.

Bibliographic note

This is an author-created, un-copyedited version of an article accepted for publication/published in the Astrophysical journal. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at doi:10.3847/1538-4357/abf1e7