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Lucky spectroscopy, an equivalent technique to lucky imaging. II. Spatially resolved intermediate-resolution blue-violet spectroscopy of 19 close massive binaries using the William Herschel Telescope

2021; EDP Sciences; Volume: 646; Linguagem: Inglês

1432-0746

J. Maíz Apellániz, R. H. Barbá, C. Fariña, A. Sota, M. Pantaleoni González, G. Holgado, I. Negueruela, S. Simón‐Díaz,

Astronomy and Astrophysical Research

J.M.A., C.F., A.S., M.P.G., and G.H. acknowledge support from the Spanish Government Ministerio de Ciencia through grant PGC2018-095049-B-C22. R.H.B. acknowledges support from the ESAC Faculty Visitor Program. I.N. and S.S.-D. acknowledge support from the Spanish Government Ministerio de Ciencia through grant PGC2018-093741-B-C21/22 (MICIU/AEI/FEDER, UE). S.S.-D. also acknowledges funding from the Spanish Government Ministerio de Ciencia through grants SEV 2015-0548 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 ProID2017010115. This paper is based on (a) lucky (and regular longslit) spectroscopy obtained with the 4.2m William Herschel Telescope (WHT) at the Observatorio del Roque de los Muchachos (ORM) on the island of La Palma, Spain; (b) lucky imaging obtained with the 2.2m Telescope at the Centro Astronomico Hispano en Andalucia (CAHA) in Almeria, Spain; (c) IFU spectroscopy obtained with the 2 m Liverpool Telescope (LT) at the Observatorio del Roque de los Muchachos (ORM) on the island of La Palma, Spain as part of GOSSS; (d) long-slit spectroscopy obtained with the 2.5 duPont Telescope at the Observatorio de Las Campanas (LCO) in Chile; and (e) high-resolution echelle spectroscopy from the LiLiMaRlin project obtained with a variety of spectrographs: HERMES at the 1.2 m Mercator Telescope (MT) at the Observatorio del Roque de los Muchachos (ORM) on the island of La Palma, Spain; ELODIE at the 1.93 m Observatoire de Haute-Provence (OHP) Telescope, France; FEROS at the 2.2 m Telescope of the Observatorio de La Silla in Chile; CAFE at the 2.2 m Centro Astronomico Hispano en Andalucia (CAHA) Telescope, Almeria, Spain; FIES at the 2.5 Nordic Optical Telescope (NOT) at the Observatorio del Roque de los Muchachos (ORM) on the island of La Palma, Spain; and UVES at the 8.2 m Kueyen Telescope at the Observatorio Paranal in Chile. Some of the MT and NOT data were obtained from the IACOB spectroscopic database (Simon-Diaz et al. 2011b,a, 2015b). This paper has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This paper has also made use of the Washington Double Star (WDS) catalog (Mason et al. 2001) and the Ski ff (2014) catalog of spectral classifications. The authors would like to thank the personnel of the WHT, CAHA, LT, LCO, MT, La Silla, and NOT observatories for their support and hospitality throughout the years. We dedicate this paper to our deceased colleagues, Virpi S. Niemela and Nolan R. Walborn, who they surely would have enjoyed having access to data like the ones presented here.