X-Shooting ULLYSES: Massive stars at low metallicity. II. DR1: Advanced optical data products for the Magellanic Clouds

Sana, H. et al. Full list of authors: Sana, H.; Tramper, F.; Abdul-Masih, M.; Blomme, R.; Dsilva, K.; Maravelias, G.; Martins, L.; Mehner, A.; Wofford, A.; Banyard, G.; Barbosa, C. L.; Bestenlehner, J.; Hawcroft, C.; John Hillier, D.; Todt, H.; Larkin, C. J. K.; Mahy, L.; Najarro, F.; Ramachandran,...

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Detalles Bibliográficos
Autores: Sana, H., Najarro, Francisco, Kehrig, C.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2024
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/387873
Acceso en línea:http://hdl.handle.net/10261/387873
Access Level:acceso abierto
Palabra clave:Techniques: spectroscopic
Atlases
Stars: early-type
Stars: massive
Magellanic Clouds
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dc.title.none.fl_str_mv X-Shooting ULLYSES: Massive stars at low metallicity. II. DR1: Advanced optical data products for the Magellanic Clouds
title X-Shooting ULLYSES: Massive stars at low metallicity. II. DR1: Advanced optical data products for the Magellanic Clouds
spellingShingle X-Shooting ULLYSES: Massive stars at low metallicity. II. DR1: Advanced optical data products for the Magellanic Clouds
Sana, H.
Techniques: spectroscopic
Atlases
Stars: early-type
Stars: massive
Magellanic Clouds
title_short X-Shooting ULLYSES: Massive stars at low metallicity. II. DR1: Advanced optical data products for the Magellanic Clouds
title_full X-Shooting ULLYSES: Massive stars at low metallicity. II. DR1: Advanced optical data products for the Magellanic Clouds
title_fullStr X-Shooting ULLYSES: Massive stars at low metallicity. II. DR1: Advanced optical data products for the Magellanic Clouds
title_full_unstemmed X-Shooting ULLYSES: Massive stars at low metallicity. II. DR1: Advanced optical data products for the Magellanic Clouds
title_sort X-Shooting ULLYSES: Massive stars at low metallicity. II. DR1: Advanced optical data products for the Magellanic Clouds
dc.creator.none.fl_str_mv Sana, H.
Najarro, Francisco
Kehrig, C.
author Sana, H.
author_facet Sana, H.
Najarro, Francisco
Kehrig, C.
author_role author
author2 Najarro, Francisco
Kehrig, C.
author2_role author
author
dc.contributor.none.fl_str_mv Fundación la Caixa
Fundação de Amparo à Pesquisa do Estado de São Paulo
Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil)
German Research Foundation
Federal Ministry of Education and Research (Germany)
Science and Technology Facilities Council (UK)
European Research Council
Ministerio de Economía y Competitividad (España)
Junta de Andalucía
Agencia Estatal de Investigación (España)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Techniques: spectroscopic
Atlases
Stars: early-type
Stars: massive
Magellanic Clouds
topic Techniques: spectroscopic
Atlases
Stars: early-type
Stars: massive
Magellanic Clouds
description Sana, H. et al. Full list of authors: Sana, H.; Tramper, F.; Abdul-Masih, M.; Blomme, R.; Dsilva, K.; Maravelias, G.; Martins, L.; Mehner, A.; Wofford, A.; Banyard, G.; Barbosa, C. L.; Bestenlehner, J.; Hawcroft, C.; John Hillier, D.; Todt, H.; Larkin, C. J. K.; Mahy, L.; Najarro, F.; Ramachandran, V.; Ramírez-Tannus, M. C.; Rubio-Díez, M. M.; Sander, A. A. C.; Shenar, T.; Vink, J. S.; Backs, F.; Brands, S. A.; Crowther, P.; Decin, L.; de Koter, A.; Hamann, W. -R.; Kehrig, C.; Kuiper, R.; Oskinova, L.; Pauli, D.; Sundqvist, J.; Verhamme, O.; Xshoot-U Collaboration
publishDate 2024
dc.date.none.fl_str_mv 2024
2025
2025
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status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/387873
url http://hdl.handle.net/10261/387873
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dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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spelling X-Shooting ULLYSES: Massive stars at low metallicity. II. DR1: Advanced optical data products for the Magellanic CloudsSana, H.Najarro, FranciscoKehrig, C.Techniques: spectroscopicAtlasesStars: early-typeStars: massiveMagellanic CloudsSana, H. et al. Full list of authors: Sana, H.; Tramper, F.; Abdul-Masih, M.; Blomme, R.; Dsilva, K.; Maravelias, G.; Martins, L.; Mehner, A.; Wofford, A.; Banyard, G.; Barbosa, C. L.; Bestenlehner, J.; Hawcroft, C.; John Hillier, D.; Todt, H.; Larkin, C. J. K.; Mahy, L.; Najarro, F.; Ramachandran, V.; Ramírez-Tannus, M. C.; Rubio-Díez, M. M.; Sander, A. A. C.; Shenar, T.; Vink, J. S.; Backs, F.; Brands, S. A.; Crowther, P.; Decin, L.; de Koter, A.; Hamann, W. -R.; Kehrig, C.; Kuiper, R.; Oskinova, L.; Pauli, D.; Sundqvist, J.; Verhamme, O.; Xshoot-U CollaborationContext. The XShootU project aims to obtain ground-based optical to near-infrared spectroscopy of all targets observed by the Hubble Space Telescope (HST) under the Director’s Discretionary program ULLYSES. Using the medium-resolution spectrograph X-shooter, spectra of 235 OB and Wolf-Rayet (WR) stars in subsolar metallicity environments have been secured. The bulk of the targets belong to the Large and Small Magellanic Clouds, with the exception of three stars in NGC 3109 and Sextans A.Aims. This second paper in the series focuses on the optical observations of Magellanic Clouds targets. It describes the uniform reduction of the UVB (300–560 nm) and VIS (550–1020 nm) XShootU data as well as the preparation of advanced data products that are suitable for homogeneous scientific analyses.Methods. The data reduction of the RAW data is based on the ESO CPL X-shooter pipeline. We paid particular attention to the determination of the response curves. This required equal flat-fielding of the science and flux standard star data and the derivation of improved flux standard models. The pipeline products were then processed with our own set of routines to produce a series of advanced data products. In particular, we implemented slit-loss correction, absolute flux calibration, (semi-)automatic rectification to the continuum, and a correction for telluric lines. The spectra of individual epochs were further corrected for the barycentric motion, re-sampled and co-added, and the spectra from the two arms were merged into a single flux-calibrated spectrum covering the entire optical range with maximum signal-to-noise ratio.Results. We identify and describe an undocumented recurrent ghost visible on the RAW data. We present an improved flat-fielding strategy that limits artifacts when the SCIENCE and FLUX standard stars are observed on different nights. The improved FLUX standard models and the new grid of anchor points limit artifacts of the response curve correction, for example on the shape of the wings of the Balmer lines, from a couple of per cent of the continuum level to less than 0.5%. We confirm the presence of a radial velocity shift of about 3.5 km s−1 between the UVB and the VIS arm of X-shooter and that there are no short term variations impacting the RV measurements. RV precision better than 1 km s-1 can be obtained on sharp telluric lines while RV precision on the order of 2 to 3 km s-1 is obtained on data with the best S/N.Conclusions. For each target observed by XShootU, we provide three types of data products: (i) two-dimensional spectra for each UVB and VIS exposure before and after correction for the instrument response; (ii) one-dimensional UVB and VIS spectra as produced by the X-shooter pipeline before and after response-correction, and applying various processing, including absolute flux calibration, telluric removal, normalization and barycentric correction; and (iii) co-added flux-calibrated and rectified spectra over the full optical range, for which all available XShootU exposures were combined. For the large majority of the targets, the final signal-to-noise ratio per resolution element is above 200 in the UVB and in the VIS co-added spectra. The reduced data and advanced scientific data products are made available to the community. Together with the HST UV ULLYSES data, they should enable various science goals, from detailed stellar atmosphere and stellar wind studies, and empirical libraries for population synthesis, to the study of the local nebular environment and feedback of massive stars in subsolar metallicity environments. © The Authors 2024We thank the referee for their constructive comments. This project has received funding from the KU Leuven Research Council (grant C16/17/007: MAESTRO). M.A. acknowledges support from “la Caixa” Foundation (ID 100010434) under the fellowship code LCF/BQ/PI23/11970035. L.M. thanks FAPESP (grant 2022/03703-1) and CNPQ (grant 307115/2021-6) for partial funding of this research. AACS and VR are supported by the Deutsche Forschungsgemeinschaft (DFG - German Research Foundation) in the form of an Emmy Noether Research Group - Project-ID 445674056 (SA4064/1-1, PI Sander). AACS and VR are further supported by funding from the Federal Ministry of Education and Research (BMBF) and the Baden-Württemberg Ministry of Science as part of the Excellence Strategy of the German Federal and State Governments. JSV gratefully acknowledges support from STFC via grant ST/V000233/1. CJKL gratefully acknowledges support from the International Max Planck Research School for Astronomy and Cosmic Physics at the University of Heidelberg in the form of an IMPRS PhD fellowship. GM acknowledges funding support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 772086). F.N. acknowledges funding by grants PID2019-105552RB-C41 and MDM- 2017-0737-19-3 Unidad de Excelencia “María de Maeztu”. C.K. acknowledges financial support from the Spanish Ministerio de Economía y Competitividad under grants AYA2016-79724-C4-4-P and PID2019-107408GB-C44, from Junta de Andalucía Excellence Project P18-FR-2664, and from the grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033. PAC and JB are supported by the Science and Technology Facilities Council research grant ST/V000853/1 (PI. V. Dhillon). R.K. acknowledges financial support via the Heisenberg Research Grant funded by the German Research Foundation (DFG) under grant no. KU 2849/9.With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).Peer reviewedEDP SciencesFundación la CaixaFundação de Amparo à Pesquisa do Estado de São PauloConselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil)German Research FoundationFederal Ministry of Education and Research (Germany)Science and Technology Facilities Council (UK)European Research CouncilMinisterio de Economía y Competitividad (España)Junta de AndalucíaAgencia Estatal de Investigación (España)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202520252024info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/387873reponame:DIGITAL.CSIC. 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