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dc.contributor.authorCortesi, Ariannapt_BR
dc.contributor.authorChies-Santos, Ana Leonorpt_BR
dc.contributor.authorPota, Vincenzopt_BR
dc.contributor.authorFoster, Carolinept_BR
dc.contributor.authorCoccato, Lodovicopt_BR
dc.contributor.authorOliveira, Claudia Lucia Mendes dept_BR
dc.contributor.authorForbes, Duncan Alanpt_BR
dc.contributor.authorMerrifield, Michaelpt_BR
dc.contributor.authorBamford, Steven Peterpt_BR
dc.contributor.authorRomanowsky, Aaron J.pt_BR
dc.contributor.authorBrodie, Jean P.pt_BR
dc.contributor.authorKartha, Sreeja S.pt_BR
dc.contributor.authorAlabi, Adebusola B.pt_BR
dc.contributor.authorProctor, Robert Neilpt_BR
dc.contributor.authorAlmeida, Andrespt_BR
dc.date.accessioned2016-05-21T02:08:33Zpt_BR
dc.date.issued2016pt_BR
dc.identifier.issn0035-8711pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/141498pt_BR
dc.description.abstractGlobular clusters (GCs) can be considered discrete, long-lived, dynamical tracers that retain crucial information about the assembly history of their parent galaxy. In this paper, we present a new catalogue of GC velocities and colours for the lenticular galaxy NGC 1023, we study their kinematics and spatial distribution, in comparison with the underlying stellar kinematics and surface brightness profile, and we test a new method for studying GC properties. Specifically, we decompose the galaxy light into its spheroid (assumed to represent the bulge+halo components) and disc components and use it to assign to each GC a probability of belonging to one of the two components. Then we model the galaxy kinematics, assuming a disc and spheroidal component, using planetary nebulae and integrated stellar light. We use this kinematic model and the probability previously obtained from the photometry to recalculate for each GC its likelihood of being associated with the disc, the spheroid, or neither. We find that the reddest GCs are likely to be associated with the disc, as found for faint fuzzies in this same galaxy, suggesting that the disc of this S0 galaxy originated at z 2. The majority of blue GCs are found likely to be associated with the spheroidal (hot) component. The method also allows us to identify objects that are unlikely to be in equilibrium with the system. In NGC 1023 some of the rejected GCs form a substructure in phase space that is connected with NGC 1023 companion galaxy.en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofMonthly notices of the Royal Astronomical Society. Oxford. Vol. 456, no. 3 (Mar. 2016), p. 2611-2621pt_BR
dc.rightsOpen Accessen
dc.subjectAglomerados globularespt_BR
dc.subjectGalaxies: elliptical and lenticular, cDen
dc.subjectGalaxias elipticaspt_BR
dc.subjectGalaxies: individual:NGC1023en
dc.subjectCinemáticapt_BR
dc.subjectGalaxies: kinematics and dynamicsen
dc.subjectGaláxia NGC 1023pt_BR
dc.titleThe SLUGGS survey : chromodynamical modelling of the lenticular galaxy NGC 1023pt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000991495pt_BR
dc.type.originEstrangeiropt_BR


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