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dc.contributor.authorMartinsson, T.~P.~K.
dc.contributor.authorSarzi, M.
dc.contributor.authorKnapen, J.~H.
dc.contributor.authorCoccato, L.
dc.contributor.authorFalcón-Barroso, J.
dc.contributor.authorElmegreen, B.~G.
dc.contributor.authorde Zeeuw, T.
dc.date.accessioned2018-07-03T16:23:18Z
dc.date.available2018-07-03T16:23:18Z
dc.date.issued2018-04-01
dc.identifier.citationMartinsson , T P K , Sarzi , M , Knapen , J H , Coccato , L , Falcón-Barroso , J , Elmegreen , B G & de Zeeuw , T 2018 , ' MUSE observations of the counter-rotating nuclear ring in NGC 7742 ' , Astronomy & Astrophysics , vol. 612 , A66 . https://doi.org/10.1051/0004-6361/201730955
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 13356828
dc.identifier.otherPURE UUID: 65a15c51-0549-445b-a883-f6dcc5640401
dc.identifier.otherBibtex: urn:9db0aa700b270ebbd2abe74556bdc872
dc.identifier.otherScopus: 85046695974
dc.identifier.urihttp://hdl.handle.net/2299/20242
dc.description© 2018 ESO. Reproduced with permission from Astronomy & Astrophysics. Content in the UH Research Archive is made available for personal research, educational, and non-commercial purposes only. Unless otherwise stated, all content is protected by copyright, and in the absence of an open license, permissions for further re-use should be sought from the publisher, the author, or other copyright holder.
dc.description.abstractAims. We present results from MUSE observations of the nearly face-on disk galaxy NGC 7742. This galaxy hosts a spectacular nuclear ring of enhanced star formation, which is unusual in that it is hosted by a non-barred galaxy, and because this star formation is most likely fuelled by externally accreted gas that counter-rotates with respect to its main stellar body. Methods. We used the MUSE data to derive the star-formation history (SFH) and accurately measure the stellar and ionized-gas kinematics of NGC 7742 in its nuclear, bulge, ring, and disk regions. Results. We have mapped the previously known gas counter-rotation well outside the ring region and deduce the presence of a slightly warped inner disk, which is inclined at approximately 6° compared to the outer disk. The gas-disk inclination is well constrained from the kinematics; the derived inclination 13.7° ± 0.4° agrees well with that derived from photometry and from what one expects using the inverse Tully-Fisher relation. We find a prolonged SFH in the ring with stellar populations as old as 2–3 Gyr and an indication that the star formation triggered by the minor merger event was delayed in the disk compared to the ring. There are two separate stellar components: an old population that counter-rotates with the gas, and a young one, concentrated to the ring, that co-rotates with the gas. We recover the kinematics of the old stars from a two-component fit, and show that combining the old and young stellar populations results in the erroneous average velocity of nearly zero found from a one-component fit. Conclusions. The spatial resolution and field of view of MUSE allow us to establish the kinematics and SFH of the nuclear ring in NGC 7742. We show further evidence that this ring has its origin in a minor merger event, possibly 2–3 Gyr ago.en
dc.format.extent9
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysics
dc.subjectGalaxies: individual: NGC 7742
dc.subjectGalaxies: kinematics and dynamics
dc.subjectGalaxies: structure
dc.subjectTechniques: imaging spectroscopy
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleMUSE observations of the counter-rotating nuclear ring in NGC 7742en
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85046695974&partnerID=8YFLogxK
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361/201730955
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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