The sHRD of OB stars in NGC 2070 : J/A+A/648/A65

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Authors : Castro N. orcid , Crowther P.A., Evans C.J. (hide) , Crowther P.A., Evans C.J. et..al

VizieR DOI : 10.26093/cds/vizier.36480065
Bibcode : 2021A&A...648A..65C (ADS) (Simbad) (Objects)
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CDS Keywords : Magellanic Clouds; Clusters, open; Stars, early-type; Stars, OB; Stars, masses; Effective temperatures
UAT : Magellanic Clouds, Open star clusters, Early-type stars, OB stars, Stellar masses, Effective temperature

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Inserted into VizieR : 13-Apr-2021
Last modification : 29-Nov-2022

Mapping the core of the Tarantula Nebula with VLT-MUSE. II. The spectroscopic Hertzsprung-Russell diagram of OB stars in NGC 2070. (2021)

Keywords : stars early-types - stars: fundamental parameters - galaxies: star clusters: individual: NGC 2070 - Magellanic Clouds

Abstract:We present the spectroscopic analysis of 333 OB-type stars extracted from VLT-MUSE observations of the central 30x30pc 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+/-2Myr. 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 ...(more)
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Astronomy and Astrophysics policies
Estimated physical parameters of the 281 early-type stars with logTeff[K]>4.3 in NGC 2070 from the MUSE observations sorted by effective temperature. See section 3 in the publication for a description of the analysis and limitations in the listed parameters.
NC gratefully acknowledge 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. From Norberto Castro Rodriguez, ncastro(at)aip.de, [Leibniz-Institut fuer Astrophysik Potsdam (AIP)

                


                

                    

                


                

                    

                


                

                    
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