Mostrar el registro sencillo del ítem

dc.contributor.authorMüller, Allan Schnorrpt_BR
dc.contributor.authorTrevisan, Marinapt_BR
dc.contributor.authorRiffel, Rogériopt_BR
dc.contributor.authorChies-Santos, Ana Leonorpt_BR
dc.contributor.authorFurlanetto, Cristinapt_BR
dc.contributor.authorRicci, Tiago Vecchipt_BR
dc.contributor.authorLohmann, Felipe Schmidtpt_BR
dc.contributor.authorFreitas, Rodrigo Flores dept_BR
dc.contributor.authorMallmann, Nícolas Dulliuspt_BR
dc.contributor.authorAlamo-Martínez, Karla A.pt_BR
dc.date.accessioned2022-02-12T04:52:14Zpt_BR
dc.date.issued2021pt_BR
dc.identifier.issn0035-8711pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/235089pt_BR
dc.description.abstractWe characterized the kinematics, morphology, and stellar population (SP) properties of a sample of massive compact quiescent galaxies (MCGs, 10 log M /M 11 and re ∼ 1–3 kpc) in the MaNGA Survey, with the goal of constraining their formation, assembly history, and assessing their relation with non-compact quiescent galaxies. We compared their properties with those of a control sample of median-sized quiescent galaxies (re ∼ 4–8 kpc) with similar effective velocity dispersions. MCGs have elevated rotational support, as evidenced by a strong anticorrelation between the Gauss–Hermite moment h3 and V/σ. In contrast, 30 per cent of control sample galaxies (CSGs) are slow rotators, and fast-rotating CSGs generally show a weak h3–V/σ anticorrelation. MCGs and CSGs have similar ages, but MCGs are more metal-rich and α-enhanced. Both MCGs and CSGs have shallow negative metallicity gradients and flat [α/Fe] gradients. On average, MCGs and CSGs have flat age gradients, but CSGs have a significantly larger dispersion of gradient values. The kinematics and SP properties of MCGs suggest that they experienced highly dissipative gas-rich events, such as mergers, followed by an intense, short, and centrally concentrated burst of star formation, between 4 and 10 Gyr ago (z ∼ 0.4–2), and had a quiet accretion history since then. This sequence of events might be analogous to, although less extreme than, the compaction events that formed compact quiescent galaxies at z ∼ 2. The small sizes of MCGs, and the high efficiency and short duration of their last star formation episode suggest that they are descendants of compact post-starburst galaxies.en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofMonthly notices of the royal astronomical society. Oxford. Vol. 507, no. 1 (Oct. 2021), p. 300-317pt_BR
dc.rightsOpen Accessen
dc.subjectEvolucao galaticapt_BR
dc.subjectGalaxies : Elliptical and lenticular, cDen
dc.subjectGalaxias elipticaspt_BR
dc.subjectGalaxies : Evolutionen
dc.subjectGalaxias lenticularespt_BR
dc.subjectGalaxies : Kinematics and dynamicsen
dc.subjectGalaxies : Statisticsen
dc.subjectCinemáticapt_BR
dc.subjectGalaxies : Stellar contenten
dc.titleThe puzzling origin of massive compact galaxies in MaNGApt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb001132724pt_BR
dc.type.originEstrangeiropt_BR


Ficheros en el ítem

Thumbnail
   

Este ítem está licenciado en la Creative Commons License

Mostrar el registro sencillo del ítem