Follow-up observations of PTFO 8-8695: a 3 MYR old T Tauri star hosting a Jupiter-mass planetary candidate
Article
Article Title | Follow-up observations of PTFO 8-8695: a 3 MYR old T Tauri star hosting a Jupiter-mass planetary candidate |
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ERA Journal ID | 1057 |
Article Category | Article |
Authors | Ciardi, David R. (Author), van Eyken, Julian C. (Author), Barnes, Jason W. (Author), Beichman, Charles A. (Author), Carey, Sean J. (Author), Crockett, Christopher J. (Author), Eastman, Jason (Author), Johns-Krull, Christopher M. (Author), Howell, Steve B. (Author), Kane, Stephen R. (Author), McLane, Jacob N. (Author), Plavchan, Peter (Author), Prato, L. (Author), Stauffer, John (Author), van Belle, Gerard T. (Author) and von Braun, Kaspar (Author) |
Journal Title | The Astrophysical Journal: an international review of astronomy and astronomical physics |
Journal Citation | 809 (1), pp. 42-52 |
Article Number | 42 |
Number of Pages | 11 |
Year | 2015 |
Publisher | IOP Publishing |
Place of Publication | United States |
ISSN | 0004-637X |
1538-4357 | |
Digital Object Identifier (DOI) | https://doi.org/10.1088/0004-637X/809/1/42 |
Web Address (URL) | http://iopscience.iop.org/article/10.1088/0004-637X/809/1/42 |
Abstract | We present Spitzer 4.5 μm light curve observations, Keck NIRSPEC radial velocity observations, and LCOGT optical light curve observations of PTFO 8-8695, which may host a Jupiter-sized planet in a very short orbital period (0.45 days). Previous work by van Eyken et al. and Barnes et al. predicts that the stellar rotation axis and the planetary orbital plane should precess with a period of 300-600 days. As a consequence, the observed transits should change shape and depth, disappear, and reappear with the precession. Our observations indicate the long-term presence of the transit events ( years), and that the transits indeed do change depth, disappear and reappear. The Spitzer observations and the NIRSPEC radial velocity observations (with contemporaneous LCOGT optical light curve data) are consistent with the predicted transit times and depths for the precession model and demonstrate the disappearance of the transits. An LCOGT optical light curve shows that the transits do reappear approximately 1 year later. The observed transits occur at the times predicted by a straight-forward propagation of the transit ephemeris. The precession model correctly predicts the depth and time of the Spitzer transit and the lack of a transit at the time of the NIRSPEC radial velocity observations. However, the precession model predicts the return of the transits approximately 1 month later than observed by LCOGT. Overall, the data are suggestive that the planetary interpretation of the observed transit events may indeed be correct, but the precession model and data are currently insufficient to confirm firmly the planetary status of PTFO 8-8695b. |
Keywords | planetary systems; stars: individual (PTFO 8-8695, 2MASS J05250755+0134243, CVSO 30); stars: pre-main sequence; |
Contains Sensitive Content | Does not contain sensitive content |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
Public Notes | For access to this article, please click on the URL link provided. |
Institution of Origin | University of Southern Queensland |
Byline Affiliations | National Aeronautics and Space Administration (NASA), United States |
University of Idaho, United States | |
California Institute of Technology (Caltech), United States | |
Science News, United States | |
Center for Astrophysics Harvard and Smithsonian, United States | |
Rice University, United States | |
San Francisco State University, United States | |
Lowell Observatory, United States | |
Missouri State University, United States |
https://research.usq.edu.au/item/q4301/follow-up-observations-of-ptfo-8-8695-a-3-myr-old-t-tauri-star-hosting-a-jupiter-mass-planetary-candidate
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