期刊
ASTROPHYSICAL JOURNAL
卷 757, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/757/2/133
关键词
binaries: eclipsing; methods: data analysis; planets and satellites: detection; stars: low-mass; techniques: photometric; white dwarfs
资金
- W. M. Keck Foundation
- California Institute of Technology
- Inter-University Centre for Astronomy and Astrophysics
- National Science Foundation [AST-0906060, AST-0960343, AST-0908886]
- University of Toronto
- NASA through STScI [51257.01]
- ANSA [NAS 5-26555]
- Hubble Fellowship
- Carnegie-Princeton Fellowship
- Richard & Rhoda Goldman Fund
- TABASGO Foundation
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0908886] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0906060, 1009991, 1009987] Funding Source: National Science Foundation
- Office Of The Director
- Office of Integrative Activities [0941742] Funding Source: National Science Foundation
We present three new eclipsing white-dwarf/M-dwarf binary systems discovered during a search for transiting planets around M-dwarfs. Unlike most known eclipsing systems of this type, the optical and infrared emission is dominated by the M-dwarf components, and the systems have optical colors and discovery light curves consistent with being Jupiter-radius transiting planets around early M-dwarfs. We detail the PTF/M-dwarf transiting planet survey, part of the Palomar Transient Factory (PTF). We present a graphics processing unit (GPU)-based box-least-squares search for transits that runs approximately 8 x faster than similar algorithms implemented on general purpose systems. For the discovered systems, we decompose low-resolution spectra of the systems into white-dwarf and M-dwarf components, and use radial velocity measurements and cooling models to estimate masses and radii for the white dwarfs. The systems are compact, with periods between 0.35 and 0.45 days and semimajor axes of approximately 2R(circle dot) (0.01 AU). The M-dwarfs have masses of approximately 0.35M(circle dot), and the white dwarfs have hydrogen-rich atmospheres with temperatures of around 8000 K and have masses of approximately 0.5M(circle dot). We use the Robo-AO laser guide star adaptive optics system to tentatively identify one of the objects as a triple system. We also use high-cadence photometry to put an upper limit on the white-dwarf radius of 0.025R(circle dot) (95% confidence) in one of the systems. Accounting for our detection efficiency and geometric factors, we estimate that 0.08%(+0.10%)(-0.05%) (90% confidence) of M-dwarfs are in these short-period, post-common-envelope white-dwarf/M-dwarf binaries where the optical light is dominated by the M-dwarf. The lack of detections at shorter periods, despite near-100% detection efficiency for such systems, suggests that binaries including these relatively low-temperature white dwarfs are preferentially found at relatively large orbital radii. Similar eclipsing binary systems can have arbitrarily small eclipse depths in red bands and generate plausible small-planet-transit light curves. As such, these systems are a source of false positives for M-dwarf transiting planet searches. We present several ways to rapidly distinguish these binaries from transiting planet systems.
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