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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
1D Kinematics from stars and ionized gas at $z\sim0.8$ from the LEGA-C spectroscopic survey of massive galaxies. / Bezanson, Rachel; Wel, Arjen van der; Straatman, Caroline; Pacifici, Camilla; Wu, Po-Feng; Barišić, Ivana; Bell, Eric F.; Conroy, Charlie; D'Eugenio, Francesco; Franx, Marijn; Gallazzi, Anna; Houdt, Josha van; Maseda, Michael V.; Muzzin, Adam; Sande, Jesse van de; Sobral, David; Spilker, Justin.
In: Astrophysical Journal Letters, Vol. 868, No. 2, L36, 01.12.2018.
Bezanson, R, Wel, AVD, Straatman, C, Pacifici, C, Wu, P-F, Barišić, I, Bell, EF, Conroy, C, D'Eugenio, F, Franx, M, Gallazzi, A, Houdt, JV, Maseda, MV, Muzzin, A, Sande, JVD, Sobral, D & Spilker, J 2018, '1D Kinematics from stars and ionized gas at $z\sim0.8$ from the LEGA-C spectroscopic survey of massive galaxies', Astrophysical Journal Letters, vol. 868, no. 2, L36. https://doi.org/10.3847/2041-8213/aaf16b
Bezanson, R., Wel, A. V. D., Straatman, C., Pacifici, C., Wu, P-F., Barišić, I., ... Spilker, J. (2018). 1D Kinematics from stars and ionized gas at $z\sim0.8$ from the LEGA-C spectroscopic survey of massive galaxies. Astrophysical Journal Letters, 868(2), [L36]. https://doi.org/10.3847/2041-8213/aaf16b
Bezanson R, Wel AVD, Straatman C, Pacifici C, Wu P-F, Barišić I et al. 1D Kinematics from stars and ionized gas at $z\sim0.8$ from the LEGA-C spectroscopic survey of massive galaxies. Astrophysical Journal Letters. 2018 Dec 1;868(2). L36. https://doi.org/10.3847/2041-8213/aaf16b
Bezanson, Rachel ; Wel, Arjen van der ; Straatman, Caroline ; Pacifici, Camilla ; Wu, Po-Feng ; Barišić, Ivana ; Bell, Eric F. ; Conroy, Charlie ; D'Eugenio, Francesco ; Franx, Marijn ; Gallazzi, Anna ; Houdt, Josha van ; Maseda, Michael V. ; Muzzin, Adam ; Sande, Jesse van de ; Sobral, David ; Spilker, Justin. / 1D Kinematics from stars and ionized gas at $z\sim0.8$ from the LEGA-C spectroscopic survey of massive galaxies. In: Astrophysical Journal Letters. 2018 ; Vol. 868, No. 2.
@article{890e779b86c2487a854521f29fd74d78,
title = "1D Kinematics from stars and ionized gas at $z\sim0.8$ from the LEGA-C spectroscopic survey of massive galaxies",
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 {\AA}−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.",
keywords = "astro-ph.GA",
author = "Rachel Bezanson and Wel, {Arjen van der} and Caroline Straatman and Camilla Pacifici and Po-Feng Wu and Ivana Barišić and Bell, {Eric F.} and Charlie Conroy and Francesco D'Eugenio and Marijn Franx and Anna Gallazzi and Houdt, {Josha van} and Maseda, {Michael V.} and Adam Muzzin and Sande, {Jesse van de} and David Sobral and Justin Spilker",
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",
doi = "10.3847/2041-8213/aaf16b",
journal = "Astrophysical Journal Letters",
publisher = "IOP Publishing Ltd",
T1 - 1D Kinematics from stars and ionized gas at $z\sim0.8$ from the LEGA-C spectroscopic survey of massive galaxies
AU - Bezanson, Rachel
AU - Wel, Arjen van der
AU - Straatman, Caroline
AU - Pacifici, Camilla
AU - Wu, Po-Feng
AU - Barišić, Ivana
AU - Bell, Eric F.
AU - Conroy, Charlie
AU - D'Eugenio, Francesco
AU - Franx, Marijn
AU - Gallazzi, Anna
AU - Houdt, Josha van
AU - Maseda, Michael V.
AU - Muzzin, Adam
AU - Sande, Jesse van de
AU - Sobral, David
AU - Spilker, Justin
N1 - 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
N2 - 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.
AB - 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.
KW - astro-ph.GA
U2 - 10.3847/2041-8213/aaf16b
DO - 10.3847/2041-8213/aaf16b
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
M1 - L36