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dc.contributor.authorStraatman, CMS
dc.contributor.authorVan Der Wel, A
dc.contributor.authorVan Houdt, J
dc.contributor.authorBezanson, R
dc.contributor.authorBell, EF
dc.contributor.authorVan Dokkum, P
dc.contributor.authorD'Eugenio, F
dc.contributor.authorFranx, M
dc.contributor.authorGallazzi, A
dc.contributor.authorDe Graaff, A
dc.contributor.authorMaseda, M
dc.contributor.authorMeidt, SE
dc.contributor.authorMuzzin, A
dc.contributor.authorSobral, D
dc.contributor.authorWu, PF
dc.date.accessioned2022-03-31T10:00:13Z
dc.date.available2022-03-31T10:00:13Z
dc.date.issued2022
dc.date.submitted2021-10-16
dc.identifier.issn0004-637X
dc.identifier.otherapjac4e18
dc.identifier.otherac4e18
dc.identifier.otheraas35447
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/335544
dc.description.abstractWe compare dynamical mass estimates based on spatially extended stellar and ionized gas kinematics ($\mathrm{M_{dyn,*}}$ and $\mathrm{M_{dyn,eml}}$, respectively) of 157 star forming galaxies at $0.6\leq z<1$. Compared to $z\sim0$, 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 dataset providing sufficiently deep measurements of a $K_s-$band limited sample. For $\mathrm{M_{dyn,*}}$ we use Jeans Anisotropic Multi-Gaussian Expansion models. For $\mathrm{M_{dyn,eml}}$ 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, $\mathrm{M_{dyn,eml}}$ is on average lower than $\mathrm{M_{dyn,*}}$, with a mean offset of $-0.15\pm0.016$ 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 to observations lacking the $S/N$ required for spatially extended dynamics.
dc.languageen
dc.publisherAmerican Astronomical Society
dc.subject310
dc.subjectGalaxies and Cosmology
dc.titleLEGA-C: Analysis of Dynamical Masses from Ionized Gas and Stellar Kinematics at z ∼0.8
dc.typeArticle
dc.date.updated2022-03-31T10:00:13Z
prism.issueIdentifier2
prism.publicationNameAstrophysical Journal
prism.volume928
dc.identifier.doi10.17863/CAM.82977
dcterms.dateAccepted2022-01-07
rioxxterms.versionofrecord10.3847/1538-4357/ac4e18
rioxxterms.versionVoR
rioxxterms.licenseref.urihttp://creativecommons.org/licenses/by/4.0/
dc.contributor.orcidStraatman, CMS [0000-0001-5937-4590]
dc.contributor.orcidVan Der Wel, A [0000-0002-5027-0135]
dc.contributor.orcidBezanson, R [0000-0001-5063-8254]
dc.contributor.orcidBell, EF [0000-0002-5564-9873]
dc.contributor.orcidVan Dokkum, P [0000-0002-8282-9888]
dc.contributor.orcidD'Eugenio, F [0000-0003-2388-8172]
dc.contributor.orcidFranx, M [0000-0002-8871-3026]
dc.contributor.orcidGallazzi, A [0000-0002-9656-1800]
dc.contributor.orcidDe Graaff, A [0000-0002-2380-9801]
dc.contributor.orcidMaseda, M [0000-0003-0695-4414]
dc.contributor.orcidMeidt, SE [0000-0002-6118-4048]
dc.contributor.orcidMuzzin, A [0000-0002-9330-9108]
dc.contributor.orcidSobral, D [0000-0001-8823-4845]
dc.contributor.orcidWu, PF [0000-0002-9665-0440]
dc.identifier.eissn1538-4357
pubs.funder-project-idEuropean Research Council (695671)
cam.issuedOnline2022-03-31


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