Ionized gas kinematics of galaxies in the CALIFA survey: I. Velocity fields, kinematic parameters of the dominant component, and presence of kinematically distinct gaseous systems

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Show simple item record García-Lorenzo, B. Márquez, I. Barrera-Ballesteros, J. K. Masegosa, J. Husemann, B. Falcón-Barroso, J. Lyubenova, M. Sánchez, S. F. Walcher, J. Mast, D. García-Benito, R. Méndez-Abreu, Jairo Van De Ven, Glenn Spekkens, K. Holmes, L. Monreal-Ibero, Ana Del Olmo, A. Ziegler, B. Bland-Hawthorn, J. Sánchez-Blázquez, Patricia Iglesias-Páramo, J. Aguerri, J. A L Papaderos, P. Gomes, J. M. Marino, R. A. González Delgado, R. M. Cortijo-Ferrero, C. López-Sánchez, A. R. Bekeraite, S. Wisotzki, L. Bomans, D. CALIFA team
dc.contributor.other UAM. Departamento de Física Teórica es_ES 2016-05-31T12:12:47Z 2016-05-31T12:12:47Z 2015-01-01
dc.identifier.citation Astronomy and Astrophysics 573 (2015): A59 en_US
dc.identifier.issn 0004-6361 (print) es_ES
dc.identifier.issn 1432-0746 (online) es_ES
dc.description Astronomy and Astrophysics 573 (2015): A59 reproduced with permission from Astronomy & Astrophysics, © ESO en_US
dc.description.abstract Context. Ionized gas kinematics provide important clues to the dynamical structure of galaxies and hold constraints to the processes driving their evolution. Aims. The motivation of this work is to provide an overall characterization of the kinematic behavior of the ionized gas of the galaxies included in the Calar Alto Legacy Integral field Area (CALIFA), offering kinematic clues to potential users of the CALIFA survey for including kinematical criteria in their selection of targets for specific studies. From the first 200 galaxies observed by CALIFA survey in its two configurations, we present the two-dimensional kinematic view of the 177 galaxies satisfaying a gas content/detection threshold. Methods. After removing the stellar contribution, we used the cross-correlation technique to obtain the radial velocity of the dominant gaseous component for each spectrum in the CALIFA data cubes for different emission lines (namely, [O II] λλ3726,3729, [O III] λλ4959,5007, Hα+[N II] λλ6548,6584, and [SII] λλ6716,6730). The main kinematic parameters measured on the plane of the sky were directly derived from the radial velocities with no assumptions on the internal prevailing motions. Evidence of the presence of several gaseous components with different kinematics were detected by using [O III] λλ4959,5007 emission line profiles. Results. At the velocity resolution of CALIFA, most objects in the sample show regular velocity fields, although the ionized-gas kinematics are rarely consistent with simple coplanar circular motions. Thirty-five percent of the objects present evidence of a displacement between the photometric and kinematic centers larger than the original spaxel radii. Only 17% of the objects in the sample exhibit kinematic lopsidedness when comparing receding and approaching sides of the velocity fields, but most of them are interacting galaxies exhibiting nuclear activity (AGN or LINER). Early-type (E+S0) galaxies in the sample present clear photometric-kinematic misaligments. There is evidence of asymmetries in the emission line profiles in 117 out of the 177 analyzed galaxies, suggesting the presence of kinematically distinct gaseous components located at different distances from the optical nucleus. The kinematic decoupling between the dominant and secondary component/s suggested by the observed asymmetries in the profiles can be characterized by a limited set of parameters. Conclusions. This work constitutes the first determination of the ionized gas kinematics of the galaxies observed in the CALIFA survey. The derived velocity fields, the reported kinematic distortions/peculiarities and the identification of the presence of several gaseous components in different regions of the objects might be used as additional criteria for selecting galaxies for specific studies en_US
dc.description.sponsorship We thank the Viabilidad, Diseño, Acceso y Mejora funding program (ICTS-2009-10) for supporting the initial developement of this project. B.G.-L. and J.B.-B. thank the support from the Plan Nacional de I+D+i (PNAYA) funding programs (AYA2012- 39408-C02-02) of the Spanish Ministerio de Economía y Competitividad (MINECO). I.M., J.M. and A.d.O. acknowledge financial support from the Spanish grant AYA2010-15169 and Junta de Andalucia TIC114 and Excellence Project P08-TIC-03531. S.F.S. and D.M. also thank the support given to this project from the PNAYA of the MINECO under grant AYA2012-31935. S.F.S. thanks the Ramón y Cajal project (RyC-2011-07590) of the Spanish MINECO, for the support giving to this project. J.M.A. acknowledges support from the European Research Council Starting Grant (SEDmorph; P.I. V. Wild). We acknowledge financial support for the ESTALLIDOS collaboration by the Spanish MINECO under grant AYA2010- 21887-C04-03. J.F.-B. acknowledges financial support from the Ramón y Cajal Program and grant AYA2010-21322-C03-02 from the MINECO, as well as to the DAGAL network from the People Programme (Marie Curie Actions) of the European Unions Seventh Framework Programme FP7/2007-2013/ under REA grant agreement number PITN-GA-2011-289313. K.S. acknowledges support from the National Sciences and Engineering Research Council of Canada. A.M.-I. acknowledges support from Agence Nationale de la Recherche through the STILISM project (ANR-12-BS05-0016-02) and from BMBF through the Erasmus-F project (grant number 05 A12BA1). P.P. is supported by Ciencia 2008 Contract, funded by FCT/MCTES (Portugal) and POPH/FSE (EC), and J.M.G. by a Post-Doctoral grant, funded by FCT/MCTES (Portugal) and POPH/FSE (EC). P.P., and J.M.G. acknowledge support by the Fundação para a Ciência e a Tecnologia (FCT) under project FCOMP-01-0124-FEDER-029170 (Reference FCT PTDC/FIS-AST/3214/2012), funded by FCTMEC (PIDDAC) and FEDER (COMPETE) en_US
dc.format.extent 43 pag. es_ES
dc.format.mimetype application/pdf en
dc.language.iso eng en
dc.publisher EDP Sciences en_US
dc.relation.ispartof Astronomy and Astrophysics en_US
dc.rights © 2014 ESO en_US
dc.subject.other cD en_US
dc.subject.other Galaxies: elliptical and lenticular en_US
dc.subject.other Galaxies: evolution en_US
dc.subject.other Galaxies: kinematics and dynamics en_US
dc.subject.other Galaxies: spiral en_US
dc.subject.other Galaxies: star formation en_US
dc.subject.other Techniques: spectroscopic en_US
dc.title Ionized gas kinematics of galaxies in the CALIFA survey: I. Velocity fields, kinematic parameters of the dominant component, and presence of kinematically distinct gaseous systems en_US
dc.type article en
dc.subject.eciencia Física es_ES
dc.relation.publisherversion es_ES
dc.identifier.doi 10.1051/0004-6361/201423485 es_ES
dc.identifier.publicationfirstpage A59 es_ES
dc.identifier.publicationlastpage A59 es_ES
dc.identifier.publicationvolume 573 es_ES
dc.relation.projectID info:eu-repo/grantAgreement/EC/FP7/289313 es_ES
dc.relation.projectID Gobierno de España. AYA2010-15169 es_ES
dc.relation.projectID Gobierno de España. AYA2012-31935 es_ES
dc.relation.projectID Gobierno de España. AYA2010- 21887-C04-03 es_ES
dc.relation.projectID Gobierno de España. AYA2012- 39408- C02-02 es_ES
dc.relation.projectID Gobierno de España. RyC-2011-07590 es_ES
dc.relation.projectID Gobierno de España. AYA2010-21322-C03-02 es_ES
dc.type.version info:eu-repo/semantics/publishedVersion en
dc.rights.accessRights openAccess en
dc.authorUAM Sánchez Blázquez, Patricia (264444)

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