Census of H II regions in NGC 6754 derived with MUSE: Constraints on the metal mixing scale
Entity
UAM. Departamento de Física TeóricaPublisher
EDP SciencesDate
2015-01-01Citation
10.1051/0004-6361/201424950
Astronomy and Astrophysics 573 (2015): A105
ISSN
0004-6361 (print); 1432-0746 (online)DOI
10.1051/0004-6361/201424950Funded by
Support for L.G. and H.K. is provided by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC12009, awarded to The Millennium Institute of Astrophysics, MAS. L.G. and H.K. acknowledge support by CONICYT through FONDECYT grants 3140566 and 3140563, respectively. S.F.S. acknowledges the Mexican National Council for Science and Technology (CONACYT) for financial support under the program Proyectos de Ciencia Basica. E.P. acknowledges funding from the Spanish MINECO grant AYA2010-15081Project
Gobierno de España. AYA2010-15081Editor's Version
http://dx.doi.org/10.1051/0004-6361/201424950Subjects
Galaxies: abundances; Galaxies: individual: NGC 6754; Galaxies: ISM; Galaxies: star formation; FísicaNote
Astronomy and Astrophysics 573 (2015): A105 reproduced with permission from Astronomy & AstrophysicsRights
© ESO, 2015Abstract
We present a study of the H II regions in the galaxy NGC 6754 from a two pointing mosaic comprising 197 637 individual spectra, using integral field spectroscopy recently acquired with the MUSE instrument during its Science Verification program. The data cover the entire galaxy out to ∼2 effective radii (re), sampling its morphological structures with unprecedented spatial resolution for a wide-field Integral Field Unit. A complete census of the H II regions limited by the atmospheric seeing conditions was derived, comprising 396 individual ionized sources. This is one of the largest and most complete catalogues of H II regions with spectroscopic information in a single galaxy. We use this catalogue to derive the radial abundance gradient in this SBb galaxy, finding a negative gradient with a slope consistent with the characteristic value for disk galaxies recently reported. The large number of H II regions allows us to estimate the typical mixing scale length (rmix ∼ 0. 4 re), which sets strong constraints on the proposed mechanisms for metal mixing in disk galaxies, like radial movements associated with bars and spiral arms. We found evidence of an azimuthal variation in the oxygen abundance that may be connected with the radial migration. These results illustrate the unique capabilities of MUSE for the study of the enrichment mechanisms in Local Universe galaxies
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Google Scholar:Sánchez, S. F.
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Galbany, L.
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Pérez, E.
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Sánchez-Blázquez, Patricia
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Falcón-Barroso, J.
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Rosales Ortega, F. Fabián
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Sánchez-Menguiano, L.
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Marino, R. A.
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Kuncarayakti, H.
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Anderson, J. P.
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Kruehler, T.
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Cano-Díaz, M.
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Barrera-Ballesteros, J. K.
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González-González, J. J.
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