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dc.rights.license© ESO 2021-
dc.contributor.authorCastro, N.-
dc.contributor.authorCrowther, P. A.-
dc.contributor.authorEvans, C. J.-
dc.contributor.authorVink, J. S.-
dc.contributor.authorPuls, J.-
dc.contributor.authorHerrero, A.-
dc.contributor.authorGarcía, M.-
dc.contributor.authorSelman, F. J.-
dc.contributor.authorRoth, M. M.-
dc.contributor.authorSimón Díaz, S.-
dc.identifier.citationAstronomy and Astrophysics 648: A65(2021)es
dc.descriptionTable 2 is only available at the CDS via anonymous ftp to ( or via Based on observations made with ESO telescopes at the Paranal observatory under programme ID 60.A-9351(A).es
dc.description.abstractWe present the spectroscopic analysis of 333 OB-type stars extracted from VLT-MUSE observations of the central 30 × 30 pc of NGC 2070 in the Tarantula Nebula on the Large Magellanic Cloud, the majority of which are analysed for the first time. The distribution of stars in the spectroscopic Hertzsprung-Russell diagram (sHRD) shows 281 stars in the main sequence. We find two groups in the main sequence, with estimated ages of 2.1 ± 0.8 and 6.2 ± 2 Myr. A subgroup of 52 stars is apparently beyond the main sequence phase, which we consider to be due to emission-type objects and/or significant nebular contamination affecting the analysis. As in previous studies, stellar masses derived from the sHRD are systematically larger than those obtained from the conventional HRD, with the differences being largest for the most massive stars. Additionally, we do not find any trend between the estimated projected rotational velocity and evolution in the sHRD. The projected rotational velocity distribution presents a tail of fast rotators that resembles findings in the wider population of 30 Doradus. We use published spectral types to calibrate the He Iλ4921/He IIλ5411 equivalent-width ratio as a classification diagnostic for early-type main sequence stars when the classical blue-visible region is not observed. Our model-atmosphere analyses demonstrate that the resulting calibration is well correlated with effective
dc.description.sponsorshipThe authors thank the referee for useful comments and helpful suggestions that improved this manuscript. NC gratefully acknowledges funding from the Deutsche Forschungsgemeinschaft (DFG) -CA 2551/1-1. SS-D and AHD acknowledge support from the Spanish Government Ministerio de Ciencia e Innovacion through grants PGC-2018-091 3741-B-C22 and CEX2019-000920-S, and from the Canarian Agency for Research, Innovation and Information Society (ACIISI), of the Canary Islands Government, and the European Regional Development Fund (ERDF), under grant with reference ProID2020010016. Our research used Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration 2013), and APLpy, an open-source plotting package for Python (Robitaille & Bressert 2012).es
dc.publisherEDP Scienceses
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PGC2018-0913741-B-C22-
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internationales
dc.subjectStars: early typees
dc.subjectStars: fundamental parameterses
dc.subjectGalaxies: star clusters: individual: NGC 2070es
dc.subjectMagellanic Cloudses
dc.titleMapping the core of the Tarantula Nebula with VLT-MUSE II. The spectroscopic Hertzsprung-Russell diagram of OB stars in NGC 2070es
dc.contributor.orcidCastro, N. [0000-0003-0521-473X]-
dc.contributor.orcidVink, J. S. [0000-0002-8445-4397]-
dc.contributor.funderDeutsche Forschungsgemeinschaft (DFG)-
dc.contributor.funderAgencia Canaria de Investigación, Innovación y Sociedad de la Información (ACIISI)-
dc.contributor.funderAgencia Estatal de Investigación (AEI)-
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