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Kinematic alignment of non-interacting CALIFA galaxies Quantifying the impact of bars on stellar and ionised gas velocity field orientations



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Marino, Raffaella Anna and otros, ... (2014) Kinematic alignment of non-interacting CALIFA galaxies Quantifying the impact of bars on stellar and ionised gas velocity field orientations. Astronomy & Astrophysics, 568 . ISSN 0004-6361


Official URL: http://dx.doi.org/10.1051/0004-6361/201423488



We present 80 stellar and ionised gas velocity maps from the Calar Alto Legacy Integral Field Area (CALIFA) survey in order to characterise the kinematic orientation of non interacting galaxies. The study of galaxies in isolation is a key step towards understanding how fast external processes, such as major mergers. affect kinematic properties in galaxies. We derived the global and individual (projected approaching and receding sides) kinematic position angles (PAs) for both the stellar and ionised gas line-of-sight velocity distributions. When compared to the photometric PA, we find that morpho-kinematic differences are smaller than 22 degrees in 90% of the sample for both stellar and nebular components and that internal kinematic misalignments are generally smaller than 16 degrees. We find a tight relation between the global stellar and ionised gas kinematic PA consistent with circular-flow pattern motions in both components (~90% of the sample has differences smaller than 16 degrees). This relation also holds, generally in barred galaxies across the bar and galaxy disc scales. Our findings suggest that even in the presence of strong bars, both the stellar and the gaseous components tend to follow the gravitational potential of the disc. As a result, kinematic orientation can be used to assess the degree of external distortions in interacting galaxies.

Item Type:Article
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© ESO, 2014. Artículo firmado por 23 autores. We thank the referee for a thorough reading of this work and for the comments and suggestions. We also thank Lindsay Holmes for allowing us to use her DiskFit kinematic modelling for comparison with our results. This study makes use of the data provided by the Calar Alto Legacy FieldArea (CALIFA) survey (http://www.califa.caha.es). and is based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calor Alto, operated jointly by the Max-Planck-Institut fur Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). CALIFA is the first legacy survey performed at Calar Alto. The CALIFA collaboration would like to thanks the IAA-CSIC and MPIA-MPG as major partners of the observatory, and CAHA itself for the unique access to telescope time and for support in manpower and infrastructures. The CALIFA collaboration also thanks the CAHA staff for their dedication to this project. J.B.-B. and B.G.-L. acknowledge the support from the Plan Nacional de I+D+i (PNAYA) funding programme (AYA2012-39408-C02-02) of the Spanish Ministry of Economy and Competitiveness (MINECO). J.F.-B. acknowledges support from the Ramón y Cajal Program, grants AYA2010-21322-C03-02 from MINECO. We also acknowledge support from the FP7 Marie Curie Actions of the European Commission, via the Initial Training Network DAGAL under REA grant agreement number 289313. R.A.M is funded by the Spanish programme of International Campus of Excellence Moncloa (CEI). L.V.M. acknowledges support from the grant AYA2011-30491-C02-01 co-financed by MICINN and FEDER funds and the Junta de Andalucía (Spain) grants P08-FQM-4205 and TIC-114. J.I.P. acknowledges financial support from the Spanish MINECO under grant AYA2010-21887-C04-01 and from Junta de Andalucía Excellence Project PEX2011-FQM7058. J.M.A. acknowledges support from the European Research Council Starting Grant (SEDmorphi P.I. V. Wild).

Uncontrolled Keywords:Star-forming galaxies; Digital sky survey; Potsdam multiaperture spectrophotometer; Mass-metallicity relation; Emission-line spectra; Spiral galaxies; Luminosity function; High-redshift; HII-regions; Chemical-composition
Subjects:Sciences > Physics > Astrophysics
Sciences > Physics > Astronomy
ID Code:37526
Deposited On:05 May 2016 13:20
Last Modified:10 Dec 2018 15:05

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