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dc.contributor.authorTokuoka, T
dc.contributor.authorInoue, AK
dc.contributor.authorHashimoto, T
dc.contributor.authorEllis, RS
dc.contributor.authorLaporte, N
dc.contributor.authorSugahara, Y
dc.contributor.authorMatsuo, H
dc.contributor.authorTamura, Y
dc.contributor.authorFudamoto, Y
dc.contributor.authorMoriwaki, K
dc.contributor.authorRoberts-Borsani, G
dc.contributor.authorShimizu, I
dc.contributor.authorYamanaka, S
dc.contributor.authorYoshida, N
dc.contributor.authorZackrisson, E
dc.contributor.authorZheng, W
dc.date.accessioned2022-07-01T09:00:09Z
dc.date.available2022-07-01T09:00:09Z
dc.date.issued2022
dc.date.submitted2022-02-22
dc.identifier.citationThe Astrophysical Journal Letters, volume 933, issue 1, article-number L19
dc.identifier.issn2041-8205
dc.identifier.otherapjlac7447
dc.identifier.otherac7447
dc.identifier.otheraas37867
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/338651
dc.description.abstract<jats:title>Abstract</jats:title> <jats:p>We present new observations with the Atacama Large Millimeter/submillimeter Array for a gravitationally lensed galaxy at <jats:italic>z</jats:italic> = 9.1, MACS1149-JD1. [O <jats:sc>iii</jats:sc>] 88 <jats:italic>μ</jats:italic>m emission is detected at 10<jats:italic>σ</jats:italic> with a spatial resolution of ∼0.3 kpc in the source plane, enabling the most distant morphokinematic study of a galaxy. The [O <jats:sc>iii</jats:sc>] emission is distributed smoothly without any resolved clumps and shows a clear velocity gradient with Δ<jats:italic>V</jats:italic> <jats:sub>obs</jats:sub>/2<jats:italic>σ</jats:italic> <jats:sub>tot</jats:sub> = 0.84 ± 0.23, where Δ<jats:italic>V</jats:italic> <jats:sub>obs</jats:sub> is the observed maximum velocity difference and <jats:italic>σ</jats:italic> <jats:sub>tot</jats:sub> is the velocity dispersion measured in the spatially integrated line profile, suggesting a rotating system. Assuming a geometrically thin self-gravitating rotation disk model, we obtain <jats:inline-formula> <jats:tex-math> <?CDATA ${V}_{\mathrm{rot}}/{\sigma }_{V}={0.67}_{-0.26}^{+0.73}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>V</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>rot</mml:mi> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:msub> <mml:mrow> <mml:mi>σ</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>V</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>0.67</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.26</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.73</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlac7447ieqn1.gif" xlink:type="simple" /> </jats:inline-formula>, where <jats:italic>V</jats:italic> <jats:sub>rot</jats:sub> and <jats:italic>σ</jats:italic> <jats:sub> <jats:italic>V</jats:italic> </jats:sub> are the rotation velocity and velocity dispersion, respectively, still consistent with rotation. The resulting disk mass of <jats:inline-formula> <jats:tex-math> <?CDATA ${0.65}_{-0.40}^{+1.37}\times {10}^{9}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>0.65</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.40</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>1.37</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo>×</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>9</mml:mn> </mml:mrow> </mml:msup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlac7447ieqn2.gif" xlink:type="simple" /> </jats:inline-formula> <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub> is consistent with being associated with the stellar mass identified with a 300 Myr old stellar population independently indicated by a Balmer break in the spectral energy distribution. We conclude that the most of the dynamical mass is associated with the previously identified mature stellar population that formed at <jats:italic>z</jats:italic> ∼ 15.</jats:p>
dc.languageen
dc.publisherAmerican Astronomical Society
dc.subject310
dc.subjectGalaxies and Cosmology
dc.titlePossible Systematic Rotation in the Mature Stellar Population of a z = 9.1 Galaxy
dc.typeArticle
dc.date.updated2022-07-01T09:00:09Z
prism.publicationNameAstrophysical Journal Letters
dc.identifier.doi10.17863/CAM.86062
dcterms.dateAccepted2022-05-27
rioxxterms.versionofrecord10.3847/2041-8213/ac7447
rioxxterms.versionVoR
rioxxterms.licenseref.urihttp://creativecommons.org/licenses/by/4.0/
dc.contributor.orcidInoue, AK [0000-0002-7779-8677]
dc.contributor.orcidHashimoto, T [0000-0002-0898-4038]
dc.contributor.orcidEllis, RS [0000-0001-7782-7071]
dc.contributor.orcidLaporte, N [0000-0001-7459-6335]
dc.contributor.orcidSugahara, Y [0000-0001-6958-7856]
dc.contributor.orcidMatsuo, H [0000-0003-3278-2484]
dc.contributor.orcidTamura, Y [0000-0003-4807-8117]
dc.contributor.orcidFudamoto, Y [0000-0001-7440-8832]
dc.contributor.orcidMoriwaki, K [0000-0003-3349-4070]
dc.contributor.orcidRoberts-Borsani, G [0000-0002-4140-1367]
dc.contributor.orcidYamanaka, S [0000-0002-7738-5290]
dc.contributor.orcidYoshida, N [0000-0001-7925-238X]
dc.contributor.orcidZackrisson, E [0000-0003-1096-2636]
dc.contributor.orcidZheng, W [0000-0002-0205-5174]
dc.identifier.eissn2041-8213
pubs.funder-project-idNational Astronomical Observatory of Japan (NAOJ) (2020-16B)
pubs.funder-project-idMinistry of Education, Culture, Sports, Science and Technology (MEXT) (HJH02007)
pubs.funder-project-idMEXT ∣ Japan Society for the Promotion of Science (JSPS) (20K22358)
pubs.funder-project-idEC ∣ European Research Council (ERC) (669253)
pubs.funder-project-idMEXT ∣ Japan Society for the Promotion of Science (JSPS) (22H01258)
cam.issuedOnline2022-07-01


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