Refined Properties of the HD 130322 Planetary System
Abstract
Exoplanetary systems closest to the Sun, with the brightest host stars, provide the most favorable opportunities for characterization studies of the host star and their planet(s). The Transit Ephemeris Refinement and Monitoring Survey uses both new radial velocity (RV) measurements and photometry in order to greatly improve planetary orbit uncertainties and the fundamental properties of the star, in this case HD 130322. The only companion, HD 130322b, orbits in a relatively circular orbit, e = 0.029 every ~10.7 days. We have compiled RV measurements from multiple sources, including 12 unpublished from the Keck I telescope, over the course of ~14 yr and have reduced the uncertainty in the transit midpoint to ~2 hr. The transit probability for the b-companion is 4.7%, where M_p sin i = 1.15 M_J and a = 0.0925 AU. In this paper, we compile photometric data from the T11 0.8 m Automated Photoelectric Telescope at Fairborn Observatory taken over ~14 yr, including the constrained transit window, which results in a dispositive null result for both full transit exclusion of HD 130322b to a depth of 0.017 mag and grazing transit exclusion to a depth of ~0.001 mag. Our analysis of the starspot activity via the photometric data reveals a highly accurate stellar rotation period: 26.53 ± 0.70 days. In addition, the brightness of the host with respect to the comparison stars is anti-correlated with the Ca ii H and K indices, typical for a young solar-type star.
Additional Information
© 2015 American Astronomical Society. Received 2014 November 21. Accepted 2015 February 7. Published 2015 April 6. The authors would like to thank Howard Isaacson and Geoff Marcy in recognition of their time spent observing the S-indices. N.R.H. would like to acknowledge financial support from the National Science Foundation through grant AST-1109662. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. G.W.H. acknowledges long-term support from NASA, NSF, Tennessee State University, and the State of Tennessee through its Centers of Excellence program. T.S.B. acknowledges support provided through NASA grant ADAP12-0172. J.T.W. and Y.K.F. acknowledge support from the National Science Foundation through grant AST-1211441. A.W.H would like thank the many observers who contributed to the measurements reported here and gratefully acknowledge the efforts and dedication of the Keck Observatory staff. Finally, we extend special thanks to those of Hawai'ian ancestry on whose sacred mountain of Maunakea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible.Attached Files
Published - Hinkel_2015_ApJ_803_8.pdf
Submitted - 1502.03441.pdf
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Additional details
- Eprint ID
- 78382
- Resolver ID
- CaltechAUTHORS:20170620-131913480
- AST-1109662
- NSF
- Pennsylvania State University
- Eberly College of Science
- Pennsylvania Space Grant Consortium
- Tennessee State University
- State of Tennessee Centers of Excellence program
- ADAP12-0172
- NASA
- AST-1211441
- NSF
- Created
-
2017-06-21Created from EPrint's datestamp field
- Updated
-
2021-11-15Created from EPrint's last_modified field
- Caltech groups
- Infrared Processing and Analysis Center (IPAC)