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Kinematics of the SN Refsdal host revealed by MUSE: a regularly rotating spiral galaxy at z similar or equal to 1.5

Di Teodoro, Enrico Maria; Grillo, C; Fraternali, F; Gobat, R; Karman, W; Mercurio, A; Rosati, P; Balestra, I; Caminha, G.B.; Caputi, K.I.; Lombardi, M; Suyu, S.H.; Treu, Tommaso; Vanzella, E

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We use Multi Unit Spectroscopic Explorer (MUSE) observations of the galaxy cluster MACS J1149.5+2223 to explore the kinematics of the grand-design spiral galaxy (Sp1149) hosting the supernova ‘Refsdal’. Sp1149 lies at z ≃ 1.49, has a stellar mass M* ≃ 5 × 109 M⊙, has a star formation rate (SFR)≃1--6M⊙yr−1⁠, and represents a likely progenitor of a Milky Way-like galaxy. All the four multiple images of Sp1149 in our data show strong [OII]-line emissions pointing to a clear rotation pattern. We...[Show more]

dc.contributor.authorDi Teodoro, Enrico Maria
dc.contributor.authorGrillo, C
dc.contributor.authorFraternali, F
dc.contributor.authorGobat, R
dc.contributor.authorKarman, W
dc.contributor.authorMercurio, A
dc.contributor.authorRosati, P
dc.contributor.authorBalestra, I
dc.contributor.authorCaminha, G.B.
dc.contributor.authorCaputi, K.I.
dc.contributor.authorLombardi, M
dc.contributor.authorSuyu, S.H.
dc.contributor.authorTreu, Tommaso
dc.contributor.authorVanzella, E
dc.date.accessioned2019-12-20T00:40:44Z
dc.date.available2019-12-20T00:40:44Z
dc.identifier.issn0035-8711
dc.identifier.urihttp://hdl.handle.net/1885/196417
dc.description.abstractWe use Multi Unit Spectroscopic Explorer (MUSE) observations of the galaxy cluster MACS J1149.5+2223 to explore the kinematics of the grand-design spiral galaxy (Sp1149) hosting the supernova ‘Refsdal’. Sp1149 lies at z ≃ 1.49, has a stellar mass M* ≃ 5 × 109 M⊙, has a star formation rate (SFR)≃1--6M⊙yr−1⁠, and represents a likely progenitor of a Milky Way-like galaxy. All the four multiple images of Sp1149 in our data show strong [OII]-line emissions pointing to a clear rotation pattern. We take advantage of the gravitational lensing magnification effect (≃4×) on the [OII] emission of the least distorted image to fit three-dimensional kinematic models to the MUSE data cube and derive the rotation curve and the velocity dispersion profile of Sp1149. We find that the rotation curve steeply rises, peaks at R ≃ 1 kpc, and then (initially) declines and flattens to an average Vflat=128+29−19 km s−1. The shape of the rotation curve is well determined, but the actual value of Vflat is quite uncertain because of the nearly face-on configuration of the galaxy. The intrinsic velocity dispersion due to gas turbulence is almost constant across the entire disc with an average of 27 ± 5 km s−1. This value is consistent with z = 0 measurements in the ionized gas component and a factor of 2–4 lower than other estimates in different galaxies at similar redshifts. The average stellar-to-total mass fraction is of the order of one-fifth. Our kinematic analysis returns the picture of a regular star-forming, mildly turbulent, rotation-dominated (V/σ ≃ 5) spiral galaxy in a 4-Gyr-old Universe.
dc.format.mimetypeapplication/pdf
dc.language.isoen_AU
dc.publisherOxford University Press
dc.rights© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society
dc.sourceMonthly Notices of the Royal Astronomical Society
dc.titleKinematics of the SN Refsdal host revealed by MUSE: a regularly rotating spiral galaxy at z similar or equal to 1.5
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume476
dc.date.issued2018
local.identifier.absfor020103 - Cosmology and Extragalactic Astronomy
local.identifier.absfor020106 - High Energy Astrophysics; Cosmic Rays
local.identifier.ariespublicationu4485658xPUB2065
local.publisher.urlhttp://www.oxfordjournals.org/
local.type.statusPublished Version
local.contributor.affiliationDi Teodoro, Enrico, College of Science, ANU
local.contributor.affiliationGrillo, C, University of Copenhagen
local.contributor.affiliationFraternali, F, University of Bologna
local.contributor.affiliationGobat, R, Korea Institute for Advanced Stud
local.contributor.affiliationKarman, W, University of Groningen
local.contributor.affiliationMercurio, A, INAF – Osservatorio Astronomico di Capodimonte
local.contributor.affiliationRosati, P, Università degli Studi di Ferrara
local.contributor.affiliationBalestra, I, University Observatory Munich
local.contributor.affiliationCaminha, G.B. , Universita degli Studi di ` Ferrara
local.contributor.affiliationCaputi, K.I., University of Groningen
local.contributor.affiliationLombardi, M, Universita degli Studi di Milano
local.contributor.affiliationSuyu, S.H. , Academia Sinica
local.contributor.affiliationTreu, Tommaso, University of California
local.contributor.affiliationVanzella, E, INAF – Osservatorio Astronomico di Bologna
dc.relationhttp://purl.org/au-research/grants/arc/DP160100723
local.bibliographicCitation.issue1
local.bibliographicCitation.startpage804
local.bibliographicCitation.lastpage813
local.identifier.doi10.1093/mnras/sty175
local.identifier.absseo970102 - Expanding Knowledge in the Physical Sciences
dc.date.updated2019-08-04T08:20:11Z
local.identifier.scopusID2-s2.0-85043507532
local.identifier.thomsonID000429276700064
dcterms.accessRightsOpen Access
dc.provenancehttp://sherpa.ac.uk/romeo/issn/0035-8711/..."author can archive publisher's version/PDF" from SHERPA/RoMEO site (as at 20/12/19). This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
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