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  • 1811.07900v1

    Rights statement: This is an author-created, un-copyedited version of an article accepted for publication/published in The Astrophysical Journal Letters. 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: 10.3847/2041-8213/aaf16b

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1D Kinematics from stars and ionized gas at $z\sim0.8$ from the LEGA-C spectroscopic survey of massive galaxies

Research output: Contribution to journalJournal article

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  • Rachel Bezanson
  • Arjen van der Wel
  • Caroline Straatman
  • Camilla Pacifici
  • Po-Feng Wu
  • Ivana Barišić
  • Eric F. Bell
  • Charlie Conroy
  • Francesco D'Eugenio
  • Marijn Franx
  • Anna Gallazzi
  • Josha van Houdt
  • Michael V. Maseda
  • Adam Muzzin
  • Jesse van de Sande
  • David Sobral
  • Justin Spilker
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Article numberL36
<mark>Journal publication date</mark>1/12/2018
<mark>Journal</mark>Astrophysical Journal Letters
Issue number2
Volume868
Number of pages7
Publication statusPublished
Early online date29/11/18
Original languageEnglish

Abstract

We present a comparison of the observed, spatially integrated stellar and ionized gas velocity dispersions of ~1000 massive ($\mathrm{log}\,{M}_{\star }/{M}_{\odot }\gtrsim 10.3$) galaxies in the Large Early Galaxy Astrophysics Census survey at 0.6 lesssim z lesssim 1.0. The high S/N ~ 20 Å−1 afforded by 20 hr Very Large Telescope/Visible Multi-Object Spectrograph spectra allows for joint modeling of the stellar continuum and emission lines in all galaxies, spanning the full range of galaxy colors and morphologies. These observed integrated velocity dispersions (denoted as ${\sigma }_{g,\mathrm{int}}^{{\prime} }$ and ${\sigma }_{\star ,\mathrm{int}}^{{\prime} }$) are related to the intrinsic velocity dispersions of ionized gas or stars, but also include rotational motions through beam smearing and spectral extraction. We find good average agreement between observed velocity dispersions, with $\langle \mathrm{log}({\sigma }_{g,\mathrm{int}}^{{\prime} }/{\sigma }_{\star ,\mathrm{int}}^{{\prime} })\rangle =-0.003$. This result does not depend strongly on stellar population, structural properties, or alignment with respect to the slit. However, in all regimes we find significant scatter between ${\sigma }_{g,\mathrm{int}}^{{\prime} }$ and ${\sigma }_{\star ,\mathrm{int}}^{{\prime} }$, with an overall scatter of 0.13 dex of which 0.05 dex is due to observational uncertainties. For an individual galaxy, the scatter between ${\sigma }_{g,\mathrm{int}}^{{\prime} }$ and ${\sigma }_{\star ,\mathrm{int}}^{{\prime} }$ translates to an additional uncertainty of ~0.24 dex on dynamical mass derived from ${\sigma }_{g,\mathrm{int}}^{{\prime} }$, on top of measurement errors and uncertainties from Virial constant or size estimates. We measure the z ~ 0.8 stellar mass Faber–Jackson relation and demonstrate that emission line widths can be used to measure scaling relations. However, these relations will exhibit increased scatter and slopes that are artificially steepened by selecting on subsets of galaxies with progressively brighter emission lines.

Bibliographic note

This is an author-created, un-copyedited version of an article accepted for publication/published in The Astrophysical Journal Letters. 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: 10.3847/2041-8213/aaf16b