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LEGA-C: Analysis of Dynamical Masses from Ionized Gas and Stellar Kinematics at z ∼ 0.8

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LEGA-C: Analysis of Dynamical Masses from Ionized Gas and Stellar Kinematics at z ∼ 0.8. / Straatman, Caroline M. S.; van der Wel, Arjen; van Houdt, Josha et al.

In: The Astrophysical Journal, Vol. 928, No. 2, 126, 01.04.2022.

Research output: Contribution to Journal/MagazineJournal articlepeer-review

Harvard

Straatman, CMS, van der Wel, A, van Houdt, J, Bezanson, R, Bell, EF, van Dokkum, P, D’Eugenio, F, Franx, M, Gallazzi, A, de Graaff, A, Maseda, M, Meidt, SE, Muzzin, A, Sobral, D & Wu, P-F 2022, 'LEGA-C: Analysis of Dynamical Masses from Ionized Gas and Stellar Kinematics at z ∼ 0.8', The Astrophysical Journal, vol. 928, no. 2, 126. https://doi.org/10.3847/1538-4357/ac4e18

APA

Straatman, C. M. S., van der Wel, A., van Houdt, J., Bezanson, R., Bell, E. F., van Dokkum, P., D’Eugenio, F., Franx, M., Gallazzi, A., de Graaff, A., Maseda, M., Meidt, S. E., Muzzin, A., Sobral, D., & Wu, P-F. (2022). LEGA-C: Analysis of Dynamical Masses from Ionized Gas and Stellar Kinematics at z ∼ 0.8. The Astrophysical Journal, 928(2), [126]. https://doi.org/10.3847/1538-4357/ac4e18

Vancouver

Straatman CMS, van der Wel A, van Houdt J, Bezanson R, Bell EF, van Dokkum P et al. LEGA-C: Analysis of Dynamical Masses from Ionized Gas and Stellar Kinematics at z ∼ 0.8. The Astrophysical Journal. 2022 Apr 1;928(2):126. Epub 2022 Mar 31. doi: 10.3847/1538-4357/ac4e18

Author

Straatman, Caroline M. S. ; van der Wel, Arjen ; van Houdt, Josha et al. / LEGA-C: Analysis of Dynamical Masses from Ionized Gas and Stellar Kinematics at z ∼ 0.8. In: The Astrophysical Journal. 2022 ; Vol. 928, No. 2.

Bibtex

@article{32ed75af305545d287c8e4def6b0c010,
title = "LEGA-C: Analysis of Dynamical Masses from Ionized Gas and Stellar Kinematics at z ∼ 0.8",
abstract = "We compare dynamical mass estimates based on spatially extended stellar and ionized gas kinematics (M dyn,* and M dyn,eml, respectively) of 157 star-forming galaxies at 0.6 ≤ z <1. Compared with z ∼ 0, these galaxies have enhanced star formation rates, with stellar feedback likely affecting the dynamics of the gas. We use LEGA-C DR3, the highest-redshift data set that provides sufficiently deep measurements of a K s -band limited sample. For M dyn,*, we use Jeans anisotropic multi-Gaussian expansion models. For M dyn,eml, we first fit a custom model of a rotating exponential disk with uniform dispersion, whose light is projected through a slit and corrected for beam smearing. We then apply an asymmetric drift correction based on assumptions common in the literature to the fitted kinematic components to obtain the circular velocity, assuming hydrostatic equilibrium. Within the half-light radius, M dyn,eml is on average lower than M dyn,*, with a mean offset of –0.15 ± 0.016 dex and galaxy-to-galaxy scatter of 0.19 dex, reflecting the combined random uncertainty. While data of higher spatial resolution are needed to understand this small offset, it supports the assumption that the galaxy-wide ionized gas kinematics do not predominantly originate from disruptive events such as star formation–driven outflows. However, a similar agreement can be obtained without modeling from the integrated emission line dispersions for axis ratios q <0.8. This suggests that our current understanding of gas kinematics is not sufficient to efficiently apply asymmetric drift corrections to improve dynamical mass estimates compared with observations lacking the signal-to-noise ratio required for spatially extended dynamics.",
keywords = "310, Galaxies and Cosmology",
author = "Straatman, {Caroline M. S.} and {van der Wel}, Arjen and {van Houdt}, Josha and Rachel Bezanson and Bell, {Eric F.} and {van Dokkum}, Pieter and Francesco D{\textquoteright}Eugenio and Marijn Franx and Anna Gallazzi and {de Graaff}, Anna and Michael Maseda and Meidt, {Sharon E.} and Adam Muzzin and David Sobral and Po-Feng Wu",
year = "2022",
month = apr,
day = "1",
doi = "10.3847/1538-4357/ac4e18",
language = "English",
volume = "928",
journal = "The Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing",
number = "2",

}

RIS

TY - JOUR

T1 - LEGA-C: Analysis of Dynamical Masses from Ionized Gas and Stellar Kinematics at z ∼ 0.8

AU - Straatman, Caroline M. S.

AU - van der Wel, Arjen

AU - van Houdt, Josha

AU - Bezanson, Rachel

AU - Bell, Eric F.

AU - van Dokkum, Pieter

AU - D’Eugenio, Francesco

AU - Franx, Marijn

AU - Gallazzi, Anna

AU - de Graaff, Anna

AU - Maseda, Michael

AU - Meidt, Sharon E.

AU - Muzzin, Adam

AU - Sobral, David

AU - Wu, Po-Feng

PY - 2022/4/1

Y1 - 2022/4/1

N2 - We compare dynamical mass estimates based on spatially extended stellar and ionized gas kinematics (M dyn,* and M dyn,eml, respectively) of 157 star-forming galaxies at 0.6 ≤ z <1. Compared with z ∼ 0, these galaxies have enhanced star formation rates, with stellar feedback likely affecting the dynamics of the gas. We use LEGA-C DR3, the highest-redshift data set that provides sufficiently deep measurements of a K s -band limited sample. For M dyn,*, we use Jeans anisotropic multi-Gaussian expansion models. For M dyn,eml, we first fit a custom model of a rotating exponential disk with uniform dispersion, whose light is projected through a slit and corrected for beam smearing. We then apply an asymmetric drift correction based on assumptions common in the literature to the fitted kinematic components to obtain the circular velocity, assuming hydrostatic equilibrium. Within the half-light radius, M dyn,eml is on average lower than M dyn,*, with a mean offset of –0.15 ± 0.016 dex and galaxy-to-galaxy scatter of 0.19 dex, reflecting the combined random uncertainty. While data of higher spatial resolution are needed to understand this small offset, it supports the assumption that the galaxy-wide ionized gas kinematics do not predominantly originate from disruptive events such as star formation–driven outflows. However, a similar agreement can be obtained without modeling from the integrated emission line dispersions for axis ratios q <0.8. This suggests that our current understanding of gas kinematics is not sufficient to efficiently apply asymmetric drift corrections to improve dynamical mass estimates compared with observations lacking the signal-to-noise ratio required for spatially extended dynamics.

AB - We compare dynamical mass estimates based on spatially extended stellar and ionized gas kinematics (M dyn,* and M dyn,eml, respectively) of 157 star-forming galaxies at 0.6 ≤ z <1. Compared with z ∼ 0, these galaxies have enhanced star formation rates, with stellar feedback likely affecting the dynamics of the gas. We use LEGA-C DR3, the highest-redshift data set that provides sufficiently deep measurements of a K s -band limited sample. For M dyn,*, we use Jeans anisotropic multi-Gaussian expansion models. For M dyn,eml, we first fit a custom model of a rotating exponential disk with uniform dispersion, whose light is projected through a slit and corrected for beam smearing. We then apply an asymmetric drift correction based on assumptions common in the literature to the fitted kinematic components to obtain the circular velocity, assuming hydrostatic equilibrium. Within the half-light radius, M dyn,eml is on average lower than M dyn,*, with a mean offset of –0.15 ± 0.016 dex and galaxy-to-galaxy scatter of 0.19 dex, reflecting the combined random uncertainty. While data of higher spatial resolution are needed to understand this small offset, it supports the assumption that the galaxy-wide ionized gas kinematics do not predominantly originate from disruptive events such as star formation–driven outflows. However, a similar agreement can be obtained without modeling from the integrated emission line dispersions for axis ratios q <0.8. This suggests that our current understanding of gas kinematics is not sufficient to efficiently apply asymmetric drift corrections to improve dynamical mass estimates compared with observations lacking the signal-to-noise ratio required for spatially extended dynamics.

KW - 310

KW - Galaxies and Cosmology

U2 - 10.3847/1538-4357/ac4e18

DO - 10.3847/1538-4357/ac4e18

M3 - Journal article

VL - 928

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 126

ER -