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dc.contributor.authorPérez, Isabel
dc.contributor.authorFreeman, K. C.
dc.contributor.authorFux, R.
dc.contributor.authorZurita, A.
dc.date.accessioned2013-10-17T12:26:17Z
dc.date.available2013-10-17T12:26:17Z
dc.date.issued2010
dc.identifier.citationPérez, I.; et al. Deriving the pattern speed using dynamical modelling of gas flows in barred galaxies. Memorie della Società Astronomica Italiana, 18(sup): 47-52 (2011). [http://hdl.handle.net/10481/28441]es_ES
dc.identifier.issn1824-0178
dc.identifier.otherarXiv:1002.1252v1
dc.identifier.urihttp://hdl.handle.net/10481/28441
dc.descriptionE.M. Corsini and V.P. Debattista (eds.), Tumbling, twisting and winding galaxies: pattern speeds along the Hubble sequence. Padova, august 25-28 2008.es_ES
dc.description.abstractIn this paper we analyse the methodology to derive the bar pattern speed from dynamical simulations. The results are robust to the changes in the vertical-scale height and in the mass-to-light (M/L) ratios. There is a small range of parameters for which the kinematics can be fitted. We have also taken into account the use of different type of dynamical modelling and the effect of using 2-D vs 1-D models in deriving the pattern speeds. We conclude that the derivation of the bar streaming motions and strength and position of shocks is not greatly affected by the fluid dynamical model used. We show new results on the derivation of the pattern speed for NGC 1530. The best fit pattern speed is around 10 km/s/kpc, which corresponds to a R_cor/R_bar = 1.4, implying a slower bar than previously derived from more indirect assumptions. With this pattern speed, the global and most local kinematic features are beautifully reproduced. However, the simulations fail to reproduce the velocity gradients close to some bright HII regions in the bar. We have shown from the study of the Halpha equivalent widths that the HII regions that are located further away from the bar dust-lane in its leading side, downstream from the main bar dust-lane, are older than the rest by 1.5-2.5 Myr. In addition, a clear spatial correlation was found between the location of HII regions, dust spurs on the trailing side of the bar dust-lane, and the loci of maximum velocity gradients parallel to the bar major axis.es_ES
dc.language.isoenges_ES
dc.rightsCreative Commons Attribution-NonCommercial-NoDerivs 3.0 Licensees_ES
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/es_ES
dc.subjectGalaxies es_ES
dc.subjectKinematics and dynamicses_ES
dc.subjectSpirales_ES
dc.subjectStructurees_ES
dc.titleDeriving the pattern speed using dynamical modelling of gas flows in barred galaxieses_ES
dc.typeinfo:eu-repo/semantics/preprintes_ES
dc.rights.accessRightsinfo:eu-repo/semantics/openAccesses_ES


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