Universidad Complutense de Madrid
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Stellar kinematics and structural properties of virgo cluster dwarf early-type galaxies from the smakced project. III. Angular momentum and constraints on formation scenarios

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Toloba, E. y Guhathakurta, P. y Boselli, A. y Peletier, R. F. y Emsellem, E. y Lisker, T. y van de Ven, G. y Simon, J. D. y Falcón Barroso, J. y Adams, J. J. y Benson, A. J. y Boissier, S. y den Brok, M. y Gorgas García, Francisco Javier y Hensler, G. y Janz, J. y Laurikainen, E. y Paudel, S. y Rys, A. y Salo, H. (2015) Stellar kinematics and structural properties of virgo cluster dwarf early-type galaxies from the smakced project. III. Angular momentum and constraints on formation scenarios. Astrophysical journal, 799 (2). ISSN 0004-637X

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URL Oficial: http://dx.doi.org/10.1088/0004-637X/799/2/172


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http://iopscience.iop.org/Editorial


Resumen

We analyze the stellar kinematics of 39 dwarf early-type galaxies (dEs) in the Virgo Cluster. Based on the specific stellar angular momentum lambda(Re) and the ellipticity, we find 11 slow rotators and 28 fast rotators. The fast rotators in the outer parts of the Virgo Cluster rotate significantly faster than fast rotators in the inner parts of the cluster. Moreover, 10 out of the 11 slow rotators are located in the inner 3 degrees (D < 1 Mpc) of the cluster. The fast rotators contain subtle disk-like structures that are visible in high-pass filtered optical images, while the slow rotators do not exhibit these structures. In addition, two of the dEs have kinematically decoupled cores and four more have emission partially filling in the Balmer absorption lines. These properties suggest that Virgo Cluster dEs may have originated from late-type star-forming galaxies that were transformed by the environment after their infall into the cluster. The correlation between lambda(Re) and the clustercentric distance can be explained by a scenario where low luminosity star-forming galaxies fall into the cluster, their gas is rapidly removed by ram-pressure stripping, although some of it can be retained in their core, their star formation is quenched but their stellar kinematics are preserved. After a long time in the cluster and several passes through its center, the galaxies are heated up and transformed into slow rotating dEs.


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© 2015. The American Astronomical Society. All rights reserved. The authors thank the referee for useful suggestions that improved this manuscript. E.T. acknowledges the financial support of the Fulbright Program jointly with the Spanish Ministry of Education. P.G. acknowledges the NSF grant AST-1010039. T.L. was supported within the framework of the Excellence Initiative by the German Research Foundation (DFG) through the Heidelberg Graduate School of Fundamental Physics (grant Number GSC 129/1). R.F.P., G.vdV., J.F.B., E.L., and H.S. acknowledge the DAGAL network from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme FP7/2007-2013/under REA grant agreement Number PITN-GA-2011-289313. G.H. acknowledges support by the FWF project P21097-N16. J.J. thanks the ARC for financial support (DP130100388). This work has made use of the GOLDMine database (Gavazzi et al. 2003) and the NASA/IPAC Extragalactic Database (NED).

Palabras clave:Newton-telescope library; Initial mass function; Digital sky survey; Elliptic galaxies; Spheroidal galaxies; Atlas(3D) project; Internal dynamics; Sauron project; Slow rotators; Densest environments
Materias:Ciencias > Física > Astrofísica
Ciencias > Física > Astronomía
Ciencias > Física > Física atmosférica
Código ID:29197
Depositado:13 Mar 2015 08:18
Última Modificación:23 Mar 2015 09:46

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