Journal
ASTRONOMICAL JOURNAL
Volume 162, Issue 5, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/1538-3881/ac1798
Keywords
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Categories
Funding
- NSF [AST-1715662, PHY 14-30152]
- Research Corporation via a Time Domain Astrophysics Scialog award [24217]
- NASA ADAP [80NSSC19K0591]
- NASA [ATP-170070]
- UNAM-DGAPA-PAPIIT [112620]
- CONACYT
- State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU)
- European Regional Development Fund (FEDER) [AYA2017-88254-P]
- Posgrado en Astrofisica graduate program at Instituto de Astronomia, UNAM
- U.S. National Science Foundation
- Alfred P. Sloan Foundation
- U.S. Department of Energy Office of Science
- Center for High-Performance Computing at the University of Utah
- Carnegie Institution for Science
- Chilean Participation Group
- French Participation Group
- Harvard-Smithsonian Center for Astrophysics
- Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo
- Max-PlanckInstitut fur Extraterrestrische Physik (MPE)
- New Mexico State University, New York University, University of Notre Dame, Observatario Nacional/MCTI
- Shanghai Astronomical Observatory, United Kingdom Participation Group
- Yale University
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Researchers use APOGEE spectra to automatically identify multiple systems such as double-lined spectroscopic binaries, finding a 3% SB2 fraction among main-sequence dwarfs with some variation in temperature and metallicity. They also determine that some of these systems are eclipsing binaries through light curve analysis.
APOGEE spectra offer less than or similar to 1 km s(-1) precision in the measurement of stellar radial velocities. This holds even when multiple stars are captured in the same spectrum, as happens most commonly with double-lined spectroscopic binaries (SB2s), although random line-of-sight alignments of unrelated stars can also occur. We develop a code that autonomously identifies SB2s and higher order multiples in the APOGEE spectra, resulting in 7273 candidate SB2s, 813 SB3s, and 19 SB4s. We estimate the mass ratios of binaries, and for a subset of these systems with a sufficient number of measurements we perform a complete orbital fit, confirming that most systems with periods of <10 days have circularized. Overall, we find an SB2 fraction (F (SB2)) similar to 3% among main-sequence dwarfs, and that there is not a significant trend in F (SB2) with temperature of a star. We are also able to recover a higher F (SB2) in sources with lower metallicity, however there are some observational biases. We also examine light curves from TESS to determine which of these spectroscopic binaries are also eclipsing. Such systems, particularly those that are also pre- and post-main sequence, are good candidates for a follow-up analysis to determine their masses and temperatures.
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