Journal article
The loudest stellar heartbeat: Characterizing the most extreme amplitude heartbeat star system
T Jayasinghe, CS Kochanek, J Strader, KZ Stanek, PJ Vallely, TA Thompson, JT Hinkle, BJ Shappee, AK Dupree, K Auchettl, L Chomiuk, E Aydi, K Dage, A Hughes, L Shishkovsky, KV Sokolovsky, S Swihart, KT Voggel, IB Thompson
Monthly Notices of the Royal Astronomical Society | OXFORD UNIV PRESS | Published : 2021
Abstract
We characterize the extreme heartbeat star system MACHO 80.7443.1718 in the Large Magellanic Cloud using Transiting Exoplanet Survey Satellite (TESS) photometry and spectroscopic observations from the Magellan Inamori Kyocera Echelle (MIKE) and SOAR Goodman spectographs. MACHO 80.7443.1718 was first identified as a heartbeat star system in the All-Sky Automated Survey for SuperNovae (ASAS-SN) with Porb =32.83 ± 0.008 d. MACHO 80.7443.1718 is a young (∼6 Myr), massive binary, composed of a B0 Iae supergiant with M1 ≈ 35, M⊙ and an O9.5V secondary with M2≈ 16, M⊙ on an eccentric (e = 0.51 ± 0.03) orbit. In addition to having the largest variability amplitude amongst all known heartbeats stars,..
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Grants
Awarded by Center for African Studies
Funding Acknowledgements
We thank Dr. Jim Fuller for useful discussions on this system and for comments on the manuscript. ASAS-SN is supported by the Gordon and Betty Moore Foundation through grant GBMF5490 to the Ohio State University, and NSF grants AST-1515927, AST1814440, and AST-1908570. Development of ASAS-SN has been supported by NSF grant AST-0908816, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics at the Ohio State University, the Chinese Academy of Sciences South America Center for Astronomy (CAS-SACA), the Villum Foundation, and George Skestos. TJ acknowledges support from the Ohio State Presidential Fellowship. KZS and CSK are supported by NSF grants AST-1515927, AST-1814440, and AST-1908570. JS acknowledges support from the Packard Foundation. JTH was supported by NASA award 80NSSC21K0136. BJS is supported by NSF grants AST-1908952, AST-1920392, and AST-1911074. Support for JLP is provided in part by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium InstituAstrophysics, MAS. EA acknowledges NSF award AST1751874, NASA awards 11-Fermi 80NSSC18K1746, 13-Fermi 80NSSC20K1535, and 16-Swift 80NSSC21K0173, and a Cottrell fellowship of the Research Corporation. KCD acknowledges funding from the McGill Space Institute, the Natural Sciences and Engineering Research Council of Canada (NSERC), and the McGill Bob Wares Science Innovation Prospectors Fund. Parts of this research were supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. Based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Minist erio da Ciencia, Tecnologia e Inovacoes (MCTI/LNA) do Brasil, the US National Science Foundation's NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. This research also made use of ASTROPY, a communitydeveloped core PYTHON package for Astronomy (Astropy Collaboration 2018).te of