Journal
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
Volume 133, Issue 1022, Pages -Publisher
IOP Publishing Ltd
DOI: 10.1088/1538-3873/abeaf7
Keywords
Eclipsing binary stars; Light curves; Radial velocity; Starspots; Spectroscopic binary stars
Categories
Funding
- NSF [AST-1449476]
- National Aeronautics and Space Administration by the Washington NASA Space Grant Consortium
- Chandra X-ray Center [GO9-20006X]
- National Aeronautics Space Administration [NAS8-03060]
- Alfred P. Sloan Foundation
- U.S. Department of Energy Office of Science
- Brazilian Participation Group
- Carnegie Institution for Science
- Carnegie Mellon University
- Center for Astrophysics -Harvard Smithsonian
- Chilean Participation Group
- French Participation Group
- Instituto de Astrofisica de Canarias
- Johns Hopkins University
- Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo
- Korean Participation Group
- Lawrence Berkeley National Laboratory
- Leibniz Institut fur Astrophysik Potsdam (AIP)
- Max-PlanckInstitut fur Astronomie (MPIA Heidelberg)
- Max-Planck-Institut fur Astrophysik (MPA Garching)
- Max-Planck-Institut fur Extraterrestrische Physik (MPE)
- National Astronomical Observatories of China
- New Mexico State University
- New York University
- University of Notre Dame
- Observatario Nacional/MCTI
- Ohio State University
- Pennsylvania State University
- Shanghai Astronomical Observatory
- United Kingdom Participation Group
- Universidad Nacional Autonoma de Mexico
- University of Arizona
- University of Colorado Boulder
- University of Oxford
- University of Portsmouth
- University of Utah
- University of Virginia
- University of Washington
- University of Wisconsin
- Vanderbilt University
- Yale University
- Center for High Performance Computing at the University of Utah
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This study calculated and modeled the physical and orbital properties of 2M06464003+0109157, a double lined spectroscopic binary. The analysis showed components with nearly equal masses and comparable radii, requiring the inclusion of star spots to explain eclipse variations in the light curve. The research highlights the potential for similar analyses using survey data to measure precise properties for eclipsing binaries.
We calculated physical and orbital properties for 2M06464003+0109157, a 1.06 day eclipsing double lined spectroscopic binary. We modeled the system's ASAS-SN and TESS light curves, measuring the system's inclination and radii of each component. Extracting radial velocities for each component from 6 SDSS/APOGEE spectra, we measured the system's mass ratio and performed a full orbital fit. Our analysis indicates that 2M06464003+0109157 has components with nearly equal masses (m(1)/m(2) = 0.99 0.01; M-1,M-2 = 0.57 0.015 M-circle dot) and comparable radii (R-1 = 0.66 0.05 R-circle dot, R-2 = 0.57 0.06 R-circle dot). The solution required two star spots to incorporate the out of eclipse variation that is seen in the light curve. We report our full characterization of this system, and prospects for similar analyses using survey data to measure precise physical and orbital properties for EBs.
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