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dc.contributor.authorEspinosa-Ponce, C.es_ES
dc.contributor.authorSánchez, S. F.es_ES
dc.contributor.authorMorisset, C.es_ES
dc.contributor.authorBarrera-Ballesteros, J. K.es_ES
dc.contributor.authorGalbany, L.es_ES
dc.contributor.authorGarcía-Benito, Rubénes_ES
dc.contributor.authorLacerda, E. A. D.es_ES
dc.contributor.authorMast, D.es_ES
dc.date.accessioned2020-06-03T06:54:03Z-
dc.date.available2020-06-03T06:54:03Z-
dc.date.issued2020-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society 494(2): 1622-1646 (2020)es_ES
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/10261/213082-
dc.description.abstractWe present a new catalogue of H ii regions based on the integral field spectroscopy (IFS) data of the extended CALIFA and PISCO samples. The selection of H ii regions was based on two assumptions: a clumpy structure with high contrast of H α emission and an underlying stellar population comprising young stars. The catalogue provides the spectroscopic information of 26 408 individual regions corresponding to 924 galaxies, including the flux intensities and equivalent widths of 51 emission lines covering the wavelength range between 3745 and 7200 Å. To our knowledge, this is the largest catalogue of spectroscopic properties of H ii regions. We explore a new approach to decontaminate the emission lines from diffuse ionized gas contribution. This diffuse gas correction was estimated to correct every emission line within the considered spectral range. With the catalogue of H ii regions corrected, new demarcation lines are proposed for the classical diagnostic diagrams. Finally, we study the properties of the underlying stellar populations of the H ii regions. It was found that there is a direct relationship between the ionization conditions on the nebulae and the properties of stellar populations besides the physicals condition on the ionized regions.© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Societyes_ES
dc.description.sponsorshipWe thank the referee for the helpful comments that have improved the quality of this article. We are grateful for the support of CONACYT grants CB-285080, FC-2016-01-1916, and CB2015-254132, and funding from the DGAPA/PAPIIT-IA101217, DGAPA/PAPIITIN100519, and DGAPA/PAPIIT-107215 (UNAM) projects. This study uses data provided by the CALIFA survey (http://ca lifa.caha.es/); it is based on observations collected at the Centro Astronomico Hispano Alem ´ an (CAHA) at Calar Alto, operated ´ jointly by the Max-Planck-Institut fur Astronomie and the Instituto ¨ de Astrof´ısica de Andaluc´ıa (CSIC). LG was funded by the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement no. 839090. This research makes use of python (http://www.python.org), of Matplotlib (a framework to the creation of scientific plots for Python; Hunter 2007), Astropy (a Python package for astronomy; Astropy Collaboration 2013; Price-Whelan et al. 2018), and SciPy (a Python-based ecosystem of open-source software for mathematics, science, and engineering; Jones et al. 2001).es_ES
dc.language.isoenges_ES
dc.publisherOxford University Presses_ES
dc.relationinfo:eu-repo/grantAgreement/EC/H2020/839090es_ES
dc.relation.isversionofPublisher's versiones_ES
dc.rightsopenAccesses_ES
dc.subjectTechniques: spectroscopices_ES
dc.subjectISM: generales_ES
dc.subjectHII regionses_ES
dc.subjectGalaxies: ISMes_ES
dc.subjectGalaxies: star formationes_ES
dc.titleH II regions in the CALIFA survey: I. catalogue presentationes_ES
dc.typeartículoes_ES
dc.identifier.doihttp://dx.doi.org/10.1093/mnras/staa782-
dc.description.peerreviewedPeer reviewedes_ES
dc.relation.publisherversionhttp://dx.doi.org/ 10.1093/mnras/staa782es_ES
dc.contributor.funderConsejo Nacional de Ciencia y Tecnología (México)es_ES
dc.contributor.funderUniversidad Nacional Autónoma de Méxicoes_ES
dc.contributor.funderEuropean Commissiones_ES
dc.relation.csices_ES
oprm.item.hasRevisionno ko 0 false*
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003141es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100005739es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000780es_ES
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