Transiting Exoplanet Monitoring Project (TEMP). II. Refined System Parameters and Transit Timing Analysis of HAT-P-33b
- Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 (China)
- Department of Astronomy, Yale University, New Haven, CT 06511 (United States)
- School of Astronomy and Space Science and Key Laboratory of Modern Astronomy and Astrophysics in Ministry of Education, Nanjing University, Nanjing 210093 (China)
- Korea Astronomy and Space Science Institute, Daejeon 305-348 (Korea, Republic of)
- Computational Engineering and Science Research Centre, University of Southern Queensland, Toowoomba, Queensland 4350 (Australia)
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States)
- Astrobiology Center, NINS, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan)
- Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008 (China)
We present 10 R-band photometric observations of eight different transits of the hot Jupiter HAT-P-33b, which has been targeted by our Transiting Exoplanet Monitoring Project. The data were obtained by two telescopes at the Xinglong Station of National Astronomical Observatories of China (NAOC) from 2013 December through 2016 January, and exhibit photometric scatter of 1.6--3.0 mmag. After jointly analyzing the previously published photometric data, radial-velocity (RV) measurements, and our new light curves, we revisit the system parameters and orbital ephemeris for the HAT-P-33b system. Our results are consistent with the published values except for the planet to star radius ratio (R{sub P}/R{sub ∗}), the ingress/egress duration (τ) and the total duration (T {sub 14}), which together indicate a slightly shallower and shorter transit shape. Our results are based on more complete light curves, whereas the previously published work had only one complete transit light curve. No significant anomalies in Transit Timing Variations (TTVs) are found, and we place upper mass limits on potential perturbers, largely supplanting the loose constraints provided by the extant RV data. The TTV limits are stronger near mean-motion resonances, especially for the low-order commensurabilities. We can exclude the existence of a perturber with mass larger than 0.6, 0.3, 0.5, 0.5, and 0.3 M{sub ⊕} near the 1:3, 1:2, 2:3, 3:2, and 2:1 resonances, respectively.
- OSTI ID:
- 22863057
- Journal Information:
- The Astronomical Journal (Online), Vol. 154, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 1538-3881
- Country of Publication:
- United States
- Language:
- English
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