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dc.contributor.authorHasheminia, M
dc.contributor.authorMosleh, M
dc.contributor.authorTacchella, S
dc.contributor.authorHosseini-Shahisavandi, SZ
dc.contributor.authorPark, M
dc.contributor.authorNaidu, RP
dc.date.accessioned2022-06-17T13:00:11Z
dc.date.available2022-06-17T13:00:11Z
dc.date.issued2022
dc.date.submitted2022-04-13
dc.identifier.issn2041-8205
dc.identifier.otherapjlac76c8
dc.identifier.otherac76c8
dc.identifier.otheraas38832
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/338201
dc.description.abstract<jats:title>Abstract</jats:title> <jats:p>The Milky Way (MW) galaxy is in focus, thanks to new observational data. Here we shed new light on the MW’s past by studying the structural evolution of MW progenitors, which we identify from extragalactic surveys. Specifically, we constrain the stellar-mass growth history (SMGH) of the MW with two methods: (i) direct measurement of the MW’s star formation history, and (ii) assuming the MW is a typical star-forming galaxy that remains on the star-forming main sequence. We select MW progenitors based on these two SMGHs at <jats:italic>z</jats:italic> = 0.2–2.0 from the CANDELS/3D-HST data. We estimate the structural parameters (including half-mass radius <jats:italic>r</jats:italic> <jats:sub>50</jats:sub> and Sérsic index) from the stellar-mass profiles. Our key finding is that the progenitors of the MW galaxy grow self-similarly on spatially resolved scales with roughly a constant half-mass radius (∼2–3 kpc) over the past 10 Gyr, while their stellar masses increase by about 1 dex, implying little-to-no inside-out growth. We discover that the radius containing 20% of the stellar mass (<jats:italic>r</jats:italic> <jats:sub>20</jats:sub>) decreases by 60% between redshifts of <jats:italic>z</jats:italic> = 2.0 and <jats:italic>z</jats:italic> = 0.7, while the central stellar-mass density (Σ<jats:sub>1</jats:sub>) increases by a factor of 1.3 dex over the same time and the Sérsic index changes as <jats:inline-formula> <jats:tex-math> <?CDATA $n\propto {\left(1+z\right)}^{-1.41\pm 0.19}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>n</mml:mi> <mml:mo>∝</mml:mo> <mml:msup> <mml:mrow> <mml:mfenced close=")" open="("> <mml:mrow> <mml:mn>1</mml:mn> <mml:mo>+</mml:mo> <mml:mi>z</mml:mi> </mml:mrow> </mml:mfenced> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1.41</mml:mn> <mml:mo>±</mml:mo> <mml:mn>0.19</mml:mn> </mml:mrow> </mml:msup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlac76c8ieqn1.gif" xlink:type="simple" /> </jats:inline-formula>. This is consistent with an early (<jats:italic>z</jats:italic> &gt; 1) formation of a thick disk, followed by the formation of a bar that led to an increase in the mass in the core. The formation and evolution of the thin disk had only little impact on the overall half-mass size. We also show that the constant-size evolution of the MW progenitors challenges semiempirical approaches and numerical simulations.</jats:p>
dc.languageen
dc.publisherAmerican Astronomical Society
dc.subject310
dc.subjectGalaxies and Cosmology
dc.titleNo Evolution in the Half-mass Radius of Milky Way-type Galaxies over the Last 10 Gyr
dc.typeArticle
dc.date.updated2022-06-17T13:00:11Z
prism.issueIdentifier2
prism.publicationNameAstrophysical Journal Letters
prism.volume932
dc.identifier.doi10.17863/CAM.85613
dcterms.dateAccepted2022-06-03
rioxxterms.versionofrecord10.3847/2041-8213/ac76c8
rioxxterms.versionVoR
rioxxterms.licenseref.urihttp://creativecommons.org/licenses/by/4.0/
dc.contributor.orcidHasheminia, M [0000-0003-3428-6441]
dc.contributor.orcidMosleh, M [0000-0002-4111-2266]
dc.contributor.orcidTacchella, S [0000-0002-8224-4505]
dc.contributor.orcidHosseini-Shahisavandi, SZ [0000-0003-3449-2288]
dc.contributor.orcidPark, M [0000-0002-8435-9402]
dc.contributor.orcidNaidu, RP [0000-0003-3997-5705]
dc.identifier.eissn2041-8213
cam.issuedOnline2022-06-17


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