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Colección SciELO Chile

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

Indexado

WoS	WOS:000615917300005
Scopus	SCOPUS_ID:85100304198

DOI

10.1051/0004-6361/202039479

Año

2021

Tipo

artículo de investigación

Citas Totales

Autores Afiliación Chile

Instituciones Chile

% Participación
Internacional

Autores
Afiliación Extranjera

Instituciones
Extranjeras

Abstract

Context. Many massive stars have nearby companions. These hamper a characterization of massive stars through spectroscopy.Aims. We continue to obtain spatially resolved spectroscopy of close massive visual binaries to derive their spectral types.Methods. We used the lucky spectroscopy technique to obtain a large number of short long-slit spectroscopic exposures of 19 close visual binaries under good seeing conditions. We selected those with the best characteristics, extracted the spectra using multiple-profile fitting, and combined the results to derive spatially separated spectra. The results were analyzed in combination with data from lucky imaging, regular intermediate-resolution single-order spectroscopy, and echelle high-resolution spectroscopy.Results. The new application of lucky spectroscopy has allowed us (among other results) to [a] spatially disentangle two O stars (FN CMa B and 6 Cas B) with brighter BA supergiant companions for the first time; [b] determine that two B stars (alpha Sco B and HD 164 492 B) with close and more massive companions are fast rotators (in the second case, solving a case of mistaken identity); [c] extend the technique to cases with extreme magnitude differences (the previous two cases plus CS Cam A,B), shorter separations (HD 193 443 A,B), and fainter primary magnitudes down to B=11 (HD 219 460 A,B); [d] spatially disentangle the spectra of stars with companions as diverse as an A supergiant (6 Cas A), a Wolf-Rayet star (HD 219 460 B = WR 157), and an M supergiant (alpha Sco A); [e] discover the unexpected identity of some targets such as two previously unknown bright O stars (HD 51 756 B and BD +60 544) and a new member of the rare OC category (HD 8768 A); and [f] identify and classify (in some cases for the first time) which of the components of four visual binaries (sigma Ori, HD 219 460, HD 194 649, and HD 191 201) is a double-lined spectroscopic binary. For another seven systems (FN CMa, sigma Sco, HD 51 756, HD 218 195, HD 17 520, HD 24 431, and HD 164 492), we detect signs of spectroscopic binarity using high-spectral-resolution spectroscopy. We also determine the limits of the technique.

Revista

Revista	ISSN
Astronomy & Astrophysics	0004-6361

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Disciplinas de Investigación

WOS
Astronomy & Astrophysics

Scopus
Sin Disciplinas

SciELO
Sin Disciplinas

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Publicaciones WoS (Ediciones: ISSHP, ISTP, AHCI, SSCI, SCI), Scopus, SciELO Chile.

Colaboración Institucional

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Autores - Afiliación

Ord.	Autor	Género	Institución - País
1	Maiz Apellaniz, J.	Hombre	CSIC - España Centro de Astrobiología (CSIC-INTA) - España CSIC-INTA - Centro de Astrobiología (CAB) - España
2	BARBA-SUAREZ, RODOLFO HECTOR	Hombre	Universidad de la Serena - Chile
3	Farina, C.	Mujer	Inst Astrofis Canarias - España Grupo de Telescopios Isaac Newton, España - España Instituto Astrofisico de Canarias - España Isaac Newton Group - España Isaac Newton Grp Telescopes - España
4	Sota, Alfredo	Hombre	CSIC - España Instituto de Astrofísica de Andalucía - CSIC - España CSIC - Instituto de Astrofísica de Andalucía (IAA) - España
5	PANTALEONI-GONZALEZ, MICHELANGELO	Hombre	CSIC - España UNIV COMPLUTENSE MADRID - España Centro de Astrobiología (CSIC-INTA) - España Universidad Complutense de Madrid - España CSIC-INTA - Centro de Astrobiología (CAB) - España
6	Holgado, Gonzalo	Hombre	CSIC - España Centro de Astrobiología (CSIC-INTA) - España CSIC-INTA - Centro de Astrobiología (CAB) - España
7	Negueruela, Ignacio	Hombre	Univ Alicante - España Universitat d'Alacant - España
8	Simon-Diaz, S.	Hombre	Inst Astrofis Canarias - España UNIV LA LAGUNA - España Instituto Astrofisico de Canarias - España Universidad de La Laguna - España

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Financiamiento

Fuente
European Regional Development Fund
Federación Española de Enfermedades Raras
Ministerio de Ciencia, Innovacion y Universidades
European Regional Development Fund (ERDF)
Agencia Estatal de Investigación
ESAC
Canary Islands Government
Agencia Canaria de Investigacion, Innovacion y Sociedad de la Informacion
MICIU/AEI/FEDER
Spanish Government Ministerio de Ciencia
ESAC Faculty Visitor Program
Telescope, France
Canarian Agency for Research, Innovation and Information Society (ACIISI)

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Agradecimientos

Agradecimiento
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.
Acknowledgements. 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 long-slit) spectroscopy obtained with the 4.2 m 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 2.2 m Telescope at the Centro Astronómico Hispano en Andalucía (CAHA) in Almería, 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 échelle spectroscopy from the LiLiMaRlin project obtained with a variety of spectrographs: HERMES at the 1.2 m Mercator Telescope (MT) at the Observa-torio 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; CAFÉ at the 2.2 m Centro Astronómico Hispano en Andalucía (CAHA) Telescope, Almería, 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 Observato-rio Paranal in Chile. Some of the MT and NOT data were obtained from the IACOB spectroscopic database (Simón-Díaz 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 Skiff (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. Niemelä and Nolan R. Walborn, who they surely would have enjoyed having access to data like the ones presented here.

Agradecimiento

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.

Acknowledgements. 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 long-slit) spectroscopy obtained with the 4.2 m 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 2.2 m Telescope at the Centro Astronómico Hispano en Andalucía (CAHA) in Almería, 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 échelle spectroscopy from the LiLiMaRlin project obtained with a variety of spectrographs: HERMES at the 1.2 m Mercator Telescope (MT) at the Observa-torio 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; CAFÉ at the 2.2 m Centro Astronómico Hispano en Andalucía (CAHA) Telescope, Almería, 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 Observato-rio Paranal in Chile. Some of the MT and NOT data were obtained from the IACOB spectroscopic database (Simón-Díaz 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 Skiff (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. Niemelä and Nolan R. Walborn, who they surely would have enjoyed having access to data like the ones presented here.