First survey of Wolf-Rayet star populations over the full extension of nearby galaxies observed with CALIFA
Autor corporativo
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CALIFA Collaboration
es_ES
Author
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Miralles Caballero, D.
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Díaz, A.
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López Sánchez, Ángel R.
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Rosales Ortega, F.
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Monreal Ibero, A.
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Pérez Montero, E.
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Kehrig, C.
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García Benito, R.
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Sánchez, S.
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Walcher, C.
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Galbany, Lluis
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Iglesias Páramo, J.
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Vílchez, J.
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González Delgado, R. M.
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van de Ven, G.
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Barrera Ballesteros, J.
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Lyubenova, M.
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Meidt, S.
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Falcon Barroso, J.
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Mast, D.
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Mendoza, M.
Admission date
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2017-10-26T13:38:42Z
Available date
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2017-10-26T13:38:42Z
Publication date
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2016-08
Cita de ítem
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A&A 592, A105 (2016)
es_ES
Identifier
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10.1051/0004-6361/201527179
Identifier
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https://repositorio.uchile.cl/handle/2250/145369
Abstract
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The search of extragalactic regions with conspicuous presence of Wolf-Rayet (WR) stars outside the Local Group is challenging task owing to the difficulty in detecting their faint spectral features. In this exploratory work, we develop a methodology to perform an automated search of WR signatures through a pixel-by-pixel analysis of integral field spectroscopy (IFS) data belonging to the Calar Alto Legacy Integral Field Area survey, CALIFA. This procedure has been applied to a sample of nearby galaxies spanning a wide range of physical, morphological, and environmental properties. This technique allowed us to build the first catalogue of regions rich in WR stars with spatially resolved information, and enabled us to study the properties of these complexes in a two-dimensional (2D) context. The detection technique is based on the identification of the blue WR bump (around He II lambda 4686 angstrom, mainly associated with nitrogen-rich WR stars; WN) and the red WR bump (around C IV lambda 5808 angstrom, mainly associated with carbon-rich WR stars; WC) using a pixel-by-pixel analysis that maximizes the number of independent regions within a given galaxy. We identified 44 WR-rich regions with blue bumps distributed in 25 out of a total of 558 galaxies. The red WR bump was identified only in 5 of those regions. Most of the WR regions are located within one effective radius from the galaxy centre, and around one-third are located within similar to 1 kpc or less from the centre. We found that the majority of the galaxies hosting WR populations in our sample are involved in some kind of interaction process. Half of the host galaxies share some properties with gamma-ray burst (GRB) hosts where WR stars, such as potential candidates to the progenitors of GRBs, are found. We also compared the WR properties derived from the CALIFA data with stellar population synthesis models, and confirm that simple star models are generally not able to reproduce the observations. We conclude that other effects, such as binary star channel (which could extend the WR phase up to 10 Myr), fast rotation, or other physical processes that cause the loss of observed Lyman continuum photons, very likely affect the derived WR properties, and hence should be considered when modelling the evolution of massive stars.
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Patrocinador
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D.M.C., A.I.D., and F.F.R.O. would like to acknowledge financial support provided by the project AYA2010-21887-C04-03 (former Ministerio de Ciencia e Innovacion, Spain) as well as the exchange programme "Study of Emission-Line Galaxies with Integral-Field Spectroscopy" (SELGIFS, FP7-PEOPLE-2013-IRSES-612701), funded by the EU through the IRSES scheme. A.M.I. acknowledges support from Agence Nationale de la Recherche through the STILISM project (ANR-12-BS05-0016-02). R.G.D. acknowledges support through the project AYA2014-57490-P. C.J.W. acknowledges support through the Marie Curie Career Integration Grant 303912. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Support for L.G. is provided by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astro-physics, MAS. L.G. acknowledges support by CONICYT through FONDECYT grant 3140566.