Kinematic alignment of non-interacting CALIFA galaxies Quantifying the impact of bars on stellar and ionised gas velocity field orientations
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...
| Autores: | , |
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| Tipo de recurso: | artículo |
| Fecha de publicación: | 2014 |
| País: | España |
| Institución: | Universidad Complutense de Madrid (UCM) |
| Repositorio: | Docta Complutense |
| Idioma: | inglés |
| OAI Identifier: | oai:docta.ucm.es:20.500.14352/35169 |
| Acceso en línea: | https://hdl.handle.net/20.500.14352/35169 |
| Access Level: | acceso abierto |
| Palabra clave: | 52 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 Astrofísica Astronomía (Física) |
| Sumario: | 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. |
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