The Secondary Component of the Extremely Low Mass Ratio Massive Binary HD 165246 Revealed by GHOST
In the pursuit of understanding the multiplicity of massive stars, the OWN Survey has undertaken spectroscopic monitoring of hundreds of targets over the past 20 yr. This effort has led to the discovery of new single-lined spectroscopic binaries. Characterizing the unseen companions of these systems...
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| author | C. N. Rodriguez T. Ansin G. A. Ferrero O. G. Benvenuto R. Gamen N. I. Morrell J. I. Arias R. E. Higa C. Putkuri C. Johnston K. Chiboucas E. Deibert C. R. Hayes J.-E. Heo M. Jeong V. Kalari E. Martioli V. M. Placco K. A. Venn S. Xu R. Diaz M. Gomez-Jimenez R. Ruiz-Carmona C. Simpson A. W. McConnachie J. Pazder G. Burley T. A. M. Berg J. G. Robertson K. Labrie J. Thomas-Osip |
| author_facet | C. N. Rodriguez T. Ansin G. A. Ferrero O. G. Benvenuto R. Gamen N. I. Morrell J. I. Arias R. E. Higa C. Putkuri C. Johnston K. Chiboucas E. Deibert C. R. Hayes J.-E. Heo M. Jeong V. Kalari E. Martioli V. M. Placco K. A. Venn S. Xu R. Diaz M. Gomez-Jimenez R. Ruiz-Carmona C. Simpson A. W. McConnachie J. Pazder G. Burley T. A. M. Berg J. G. Robertson K. Labrie J. Thomas-Osip |
| author_sort | C. N. Rodriguez |
| collection | DOAJ |
| description | In the pursuit of understanding the multiplicity of massive stars, the OWN Survey has undertaken spectroscopic monitoring of hundreds of targets over the past 20 yr. This effort has led to the discovery of new single-lined spectroscopic binaries. Characterizing the unseen companions of these systems is crucial to deriving precise stellar parameters, including the mass of each component, and constraining formation models for massive binary systems. In this paper, we aim to physically and evolutionarily characterize the stellar components of the massive binary HD 165246. We analyzed spectra obtained by the OWN Survey and used Kepler's second mission (K2) photometry, from which we determined the physical parameters of the system. Thanks to the high-resolution capabilities of the new echelle spectrograph Gemini/GHOST, we could directly detect spectral features of the secondary component for the first time. A very low mass ratio for the system is confirmed ( q ~ 0.16), making this binary one of the few extremely low mass ratio systems known. The primary star has a mass of M _a = 22 ± 1 M _⊙ and a radius of R _a = 7.0 ± 0.1 R _⊙ , while the secondary star has a mass of M _b = 3.4 ± 0.1 M _⊙ and a radius of R _b = 2.22 ± 0.02 R _⊙ . Stellar evolution models indicate that the system has undergone approximately two million years of evolution since its formation. Moreover, the secondary star is identified as a pre-main-sequence object, progressing toward the zero-age main sequence. This paper illustrates the power of high-resolution spectrographs such as GHOST in finding much lower mass, previously unseen stellar components of binary star systems. |
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| institution | Kabale University |
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| spelling | doaj-art-ef88f306695d4298a0bb25b6632a17c92025-02-12T07:38:15ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01980216910.3847/1538-4357/ada892The Secondary Component of the Extremely Low Mass Ratio Massive Binary HD 165246 Revealed by GHOSTC. N. Rodriguez0https://orcid.org/0000-0002-8744-803XT. Ansin1https://orcid.org/0009-0004-3544-1751G. A. Ferrero2https://orcid.org/0000-0001-9623-6218O. G. Benvenuto3https://orcid.org/0009-0005-0973-470XR. Gamen4https://orcid.org/0000-0002-5227-9627N. I. Morrell5https://orcid.org/0000-0003-2535-3091J. I. Arias6https://orcid.org/0000-0001-7500-7352R. E. Higa7C. Putkuri8C. Johnston9https://orcid.org/0000-0002-3054-4135K. Chiboucas10https://orcid.org/0000-0002-9020-5004E. Deibert11https://orcid.org/0000-0001-9796-2158C. R. Hayes12J.-E. Heo13https://orcid.org/0000-0003-2530-3000M. Jeong14https://orcid.org/0009-0009-7838-7771V. Kalari15https://orcid.org/0000-0002-4641-2532E. Martioli16https://orcid.org/0000-0002-5084-168XV. M. Placco17https://orcid.org/0000-0003-4479-1265K. A. Venn18https://orcid.org/0000-0003-4134-2042S. Xu19https://orcid.org/0000-0002-8808-4282R. Diaz20https://orcid.org/0000-0001-9716-5335M. Gomez-Jimenez21R. Ruiz-Carmona22https://orcid.org/0000-0001-7518-1393C. Simpson23https://orcid.org/0000-0001-8589-4055A. W. McConnachie24https://orcid.org/0000-0003-4666-6564J. Pazder25G. Burley26https://orcid.org/0000-0001-7548-5354T. A. M. Berg27https://orcid.org/0000-0002-2606-5078J. G. Robertson28https://orcid.org/0000-0001-5528-7801K. Labrie29https://orcid.org/0000-0002-6633-7891J. Thomas-Osip30https://orcid.org/0000-0003-1033-4402International Gemini Observatory/NSF NOIRLab , Casilla 603, La Serena, Chile ; cinthya.rodriguez@noirlab.eduInstituto de Astrofísica de La Plata , CONICET–UNLP, Paseo del Bosque S/N, B1900FWA La Plata, Argentina; Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata , Paseo del Bosque S/N, B1900FWA La Plata, ArgentinaInstituto de Astrofísica de La Plata , CONICET–UNLP, Paseo del Bosque S/N, B1900FWA La Plata, Argentina; Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata , Paseo del Bosque S/N, B1900FWA La Plata, ArgentinaInstituto de Astrofísica de La Plata , CONICET–UNLP, Paseo del Bosque S/N, B1900FWA La Plata, Argentina; Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata , Paseo del Bosque S/N, B1900FWA La Plata, ArgentinaInstituto de Astrofísica de La Plata , CONICET–UNLP, Paseo del Bosque S/N, B1900FWA La Plata, Argentina; Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata , Paseo del Bosque S/N, B1900FWA La Plata, ArgentinaLas Campanas Observatory, Carnegie Observatories , Casilla 601, La Serena, ChileDepartamento de Astronomía, Universidad de La Serena , Cisternas 1200 Norte, La Serena, ChileInstituto de Astrofísica de La Plata , CONICET–UNLP, Paseo del Bosque S/N, B1900FWA La Plata, Argentina; Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata , Paseo del Bosque S/N, B1900FWA La Plata, ArgentinaInstituto de Astrofísica de La Plata , CONICET–UNLP, Paseo del Bosque S/N, B1900FWA La Plata, Argentina; Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata , Paseo del Bosque S/N, B1900FWA La Plata, ArgentinaDepartment of Astrophysics, IMAPP, Radboud University Nijmegen , PO Box 9010, 6500 GL Nijmegen, The Netherlands; Institute of Astronomy, KU Leuven , Celestijnenlaan 200D, 3001 Leuven, Belgium; Max-Planck-Institut für Astrophysik , Karl-Schwarzschild-Straße 1, 85741 Garching bei München, GermanyInternational Gemini Observatory/NSF NOIRLab , 670 N. A’ohoku Place, Hilo, HI 96720, USAInternational Gemini Observatory/NSF NOIRLab , Casilla 603, La Serena, Chile ; cinthya.rodriguez@noirlab.eduNRC Herzberg Astronomy and Astrophysics Research Centre , 5071 West Saanich Road, Victoria, BC V9E 2E7, CanadaInternational Gemini Observatory/NSF NOIRLab , Casilla 603, La Serena, Chile ; cinthya.rodriguez@noirlab.eduDepartment of Astronomy, Space Science, and Geology, Chungnam National University , Daejeon 34134, Republic of KoreaInternational Gemini Observatory/NSF NOIRLab , Casilla 603, La Serena, Chile ; cinthya.rodriguez@noirlab.eduLaboratório Nacional de Astrofísica , Rua Estados Unidos 154, 37504-364 Itajubá, MG, Brazil; Institut d’Astrophysique de Paris, CNRS, UMR 7095, Sorbonne Université , 98 bis bd Arago, 75014 Paris, FranceNSF NOIRLab , 950 N. Cherry Ave., Tucson, AZ 85719, USADepartment of Physics and Astronomy, University of Victoria , PO Box 3055, STN CSC, Victoria, BC V8W 3P6, CanadaInternational Gemini Observatory/NSF NOIRLab , 670 N. A’ohoku Place, Hilo, HI 96720, USAInternational Gemini Observatory/NSF NOIRLab , Casilla 603, La Serena, Chile ; cinthya.rodriguez@noirlab.eduInternational Gemini Observatory/NSF NOIRLab , Casilla 603, La Serena, Chile ; cinthya.rodriguez@noirlab.eduInternational Gemini Observatory/NSF NOIRLab , Casilla 603, La Serena, Chile ; cinthya.rodriguez@noirlab.eduInternational Gemini Observatory/NSF NOIRLab , 670 N. A’ohoku Place, Hilo, HI 96720, USANRC Herzberg Astronomy and Astrophysics Research Centre , 5071 West Saanich Road, Victoria, BC V9E 2E7, CanadaNRC Herzberg Astronomy and Astrophysics Research Centre , 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada; Department of Physics and Astronomy, University of Victoria , PO Box 3055, STN CSC, Victoria, BC V8W 3P6, CanadaNRC Herzberg Astronomy and Astrophysics Research Centre , 5071 West Saanich Road, Victoria, BC V9E 2E7, CanadaNRC Herzberg Astronomy and Astrophysics Research Centre , 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada; European Southern Observatory , Alonso de Cordova, 3107, Casilla, 19001 Santiago, ChileAustralian Astronomical Optics, Macquarie University , 105 Delhi Rd, North Ryde, NSW 2113, Australia; Sydney Institute for Astronomy, School of Physics, The University of Sydney , NSW 2006, AustraliaInternational Gemini Observatory/NSF NOIRLab , 670 N. A’ohoku Place, Hilo, HI 96720, USAInternational Gemini Observatory/NSF NOIRLab , Casilla 603, La Serena, Chile ; cinthya.rodriguez@noirlab.eduIn the pursuit of understanding the multiplicity of massive stars, the OWN Survey has undertaken spectroscopic monitoring of hundreds of targets over the past 20 yr. This effort has led to the discovery of new single-lined spectroscopic binaries. Characterizing the unseen companions of these systems is crucial to deriving precise stellar parameters, including the mass of each component, and constraining formation models for massive binary systems. In this paper, we aim to physically and evolutionarily characterize the stellar components of the massive binary HD 165246. We analyzed spectra obtained by the OWN Survey and used Kepler's second mission (K2) photometry, from which we determined the physical parameters of the system. Thanks to the high-resolution capabilities of the new echelle spectrograph Gemini/GHOST, we could directly detect spectral features of the secondary component for the first time. A very low mass ratio for the system is confirmed ( q ~ 0.16), making this binary one of the few extremely low mass ratio systems known. The primary star has a mass of M _a = 22 ± 1 M _⊙ and a radius of R _a = 7.0 ± 0.1 R _⊙ , while the secondary star has a mass of M _b = 3.4 ± 0.1 M _⊙ and a radius of R _b = 2.22 ± 0.02 R _⊙ . Stellar evolution models indicate that the system has undergone approximately two million years of evolution since its formation. Moreover, the secondary star is identified as a pre-main-sequence object, progressing toward the zero-age main sequence. This paper illustrates the power of high-resolution spectrographs such as GHOST in finding much lower mass, previously unseen stellar components of binary star systems.https://doi.org/10.3847/1538-4357/ada892Massive starsEarly-type starsFundamental parameters of starsClose binary starsEclipsing binary stars |
| spellingShingle | C. N. Rodriguez T. Ansin G. A. Ferrero O. G. Benvenuto R. Gamen N. I. Morrell J. I. Arias R. E. Higa C. Putkuri C. Johnston K. Chiboucas E. Deibert C. R. Hayes J.-E. Heo M. Jeong V. Kalari E. Martioli V. M. Placco K. A. Venn S. Xu R. Diaz M. Gomez-Jimenez R. Ruiz-Carmona C. Simpson A. W. McConnachie J. Pazder G. Burley T. A. M. Berg J. G. Robertson K. Labrie J. Thomas-Osip The Secondary Component of the Extremely Low Mass Ratio Massive Binary HD 165246 Revealed by GHOST The Astrophysical Journal Massive stars Early-type stars Fundamental parameters of stars Close binary stars Eclipsing binary stars |
| title | The Secondary Component of the Extremely Low Mass Ratio Massive Binary HD 165246 Revealed by GHOST |
| title_full | The Secondary Component of the Extremely Low Mass Ratio Massive Binary HD 165246 Revealed by GHOST |
| title_fullStr | The Secondary Component of the Extremely Low Mass Ratio Massive Binary HD 165246 Revealed by GHOST |
| title_full_unstemmed | The Secondary Component of the Extremely Low Mass Ratio Massive Binary HD 165246 Revealed by GHOST |
| title_short | The Secondary Component of the Extremely Low Mass Ratio Massive Binary HD 165246 Revealed by GHOST |
| title_sort | secondary component of the extremely low mass ratio massive binary hd 165246 revealed by ghost |
| topic | Massive stars Early-type stars Fundamental parameters of stars Close binary stars Eclipsing binary stars |
| url | https://doi.org/10.3847/1538-4357/ada892 |
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