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Angular Momentum across the Hubble sequence from the CALIFA survey

Published online by Cambridge University Press:  10 April 2015

Jesús Falcón-Barroso ,
Mariya Lyubenova ,
Glenn van de Ven  and
the CALIFA collaboration
Jesús Falcón-Barroso
Affiliation:
Instituto de Astrofísica de Canarias, Vía Láctea s/n, La Laguna, Tenerife, Spain Departamento de Astrofísica, Univ. de La Laguna, E-38205 La Laguna, Tenerife, Spain. email: [email protected]
Mariya Lyubenova
Affiliation:
Kapteyn Astronomical Institute, University of Groningen Postbus 800, 9700 AV Groningen, The Netherlands. email: [email protected] Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany. email: [email protected]
Glenn van de Ven
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany. email: [email protected]
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Abstract

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We investigate the stellar angular momentum of galaxies across the Hubble sequence from the CALIFA survey. The distribution of CALIFA elliptical and lenticular galaxies in the λRe - εe diagram is consistent with that shown by the Atlas3D survey. Our data, however, show that the location of spiral galaxies in this diagram is significantly different. We have found two families of spiral galaxies with particularly peculiar properties: (a) spiral galaxies with much higher λRe values than any elliptical and lenticular galaxy; (b) low-mass spiral galaxies with observed λRe values much lower than expected for their apparent flattening. We use these two families of objects to argue that (1) fading alone cannot explain the transformation of spiral to lenticular galaxies, and (2) that those low-mass spiral galaxies are in fact dark matter dominated, which explains the unusually low angular momentum.

Keywords

galaxies: elliptical and lenticularcD - galaxies: evolution - galaxies: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S311: Galaxy Masses as Constraints of Formation Models , July 2014 , pp. 78 - 81
Copyright
Copyright © International Astronomical Union 2015 

References

Cappellari, M., et al., 2011, MNRAS, 413, 813CrossRefGoogle Scholar
Cappellari, M., et al., 2012, Nature, 484, 485Google Scholar
Emsellem, E., et al., 2011, MNRAS, 414, 888Google Scholar
Gadotti, D. A., 2009, MNRAS, 393, 1531Google Scholar
González Delgado, R. M., et al., 2014, A&A, 562, A47Google Scholar
La Barbera, F., Ferreras, I., Vazdekis, A., de la Rosa, I. G., de Carvalho, R. R., Trevisan, M., Falcón-Barroso, J., & Ricciardelli, E., 2013, MNRAS, 433, 3017Google Scholar
Marino, R. A., et al., 2013, A&A, 559, A114Google Scholar
Papastergis, E., Cattaneo, A., Huang, S., Giovanelli, R., & Haynes, M. P., 2012, ApJ, 759, 138Google Scholar
Pérez, E., et al., 2013, ApJ, 764, L1CrossRefGoogle Scholar
Sánchez, S. F., et al., 2012, A&A, 538, A8Google Scholar
Walcher, C. J., et al., 2014, A&A, 569, A1Google Scholar