Eclipsing Binary Science via the Merging of Transit and Doppler Exoplanet Survey Data—A Case Study with the MARVELS Pilot Project and SuperWASP

August 2011 • 2011AJ....142...50F

Authors • Fleming, Scott W. • Maxted, Pierre F. L. • Hebb, Leslie • Stassun, Keivan G. • Ge, Jian • Cargile, Phillip A. • Ghezzi, Luan • De Lee, Nathan M. • Wisniewski, John • Gary, Bruce • Porto de Mello, G. F. • Ferreira, Leticia • Zhao, Bo • Anderson, David R. • Wan, Xiaoke • Hellier, Coel • Guo, Pengcheng • West, Richard G. • Mahadevan, Suvrath • Pollacco, Don • Lee, Brian • Collier Cameron, Andrew • van Eyken, Julian C. • Skillen, Ian • Crepp, Justin R. • Nguyen, Duy Cuong • Kane, Stephen R. • Paegert, Martin • Nicolaci da Costa, Luiz • Maia, Marcio A. G. • Santiago, Basilio X.

Abstract • Exoplanet transit and Doppler surveys discover many binary stars during their operation that can be used to conduct a variety of ancillary science. Specifically, eclipsing binary stars can be used to study the stellar mass-radius relationship and to test predictions of theoretical stellar evolution models. By cross-referencing 24 binary stars found in the MARVELS Pilot Project with SuperWASP photometry, we find two new eclipsing binaries, TYC 0272-00458-1 and TYC 1422-01328-1, which we use as case studies to develop a general approach to eclipsing binaries in survey data. TYC 0272-00458-1 is a single-lined spectroscopic binary for which we calculate a mass of the secondary and radii for both components using reasonable constraints on the primary mass through several different techniques. For a primary mass of M ₁ = 0.92 ± 0.1 M _sun, we find M ₂ = 0.610 ± 0.036 M _sun, R ₁ = 0.932 ± 0.076 R _sun, and R ₂ = 0.559 ± 0.102 R _sun, and find that both stars have masses and radii consistent with model predictions. TYC 1422-01328-1 is a triple-component system for which we can directly measure the masses and radii of the eclipsing pair. We find that the eclipsing pair consists of an evolved primary star (M ₁ = 1.163 ± 0.034 M _sun, R ₁ = 2.063 ± 0.058 R _sun) and a G-type dwarf secondary (M ₂ = 0.905 ± 0.067 M _sun, R ₂ = 0.887 ± 0.037 R _sun). We provide the framework necessary to apply this analysis to much larger data sets.

Links

• SIMBAD http://simbad.u-strasbg.fr/simbo.pl?bibcode=2011AJ....142...50F
• PDF https://iopscience.iop.org/article/10.1088/0004-6256/142/2/50/pdf
• PDF https://stacks.iop.org/1538-3881/142/50/pdf
• PREPRINT http://arxiv.org/abs/1105.2027
• DATA https://irsa.ipac.caltech.edu/bibdata/2011/F/2011AJ....142...50F.html
• ELECTR https://doi.org/10.1088%2F0004-6256%2F142%2F2%2F50
• SPIRES http://inspirehep.net/search?p=find+eprint+arXiv:1105.2027