Two New HATNet Hot Jupiters around A Stars and the First Glimpse at the Occurrence Rate of Hot Jupiters from TESS

Creators: Zhou, G.; Fulton, B. J.

Abstract

Wide-field surveys for transiting planets are well suited to searching diverse stellar populations, enabling a better understanding of the link between the properties of planets and their parent stars. We report the discovery of HAT-P-69 b (TOI 625.01) and HAT-P-70 b (TOI 624.01), two new hot Jupiters around A stars from the Hungarian-made Automated Telescope Network (HATNet) survey that have also been observed by the Transiting Exoplanet Survey Satellite. HAT-P-69 b has a mass of 3.58^(+0.58)_(-0.58) M_(Jup_ and a radius of 1.676^(+0.051)_(-0.033) R_(Jup) and resides in a prograde 4.79 day orbit. HAT-P-70 b has a radius of 1.87^(+0/15)_(-0.10) R_(Jup) and a mass constraint of <6.78 (3 σ) M_(Jup) and resides in a retrograde 2.74 day orbit. We use the confirmation of these planets around relatively massive stars as an opportunity to explore the occurrence rate of hot Jupiters as a function of stellar mass. We define a sample of 47,126 main-sequence stars brighter than T_(mag) = 10 that yields 31 giant planet candidates, including 18 confirmed planets, 3 candidates, and 10 false positives. We find a net hot Jupiter occurrence rate of 0.41 ± 0.10% within this sample, consistent with the rate measured by Kepler for FGK stars. When divided into stellar mass bins, we find the occurrence rate to be 0.71 ± 0.31% for G stars, 0.43 ± 0.15% for F stars, and 0.26 ± 0.11% for A stars. Thus, at this point, we cannot discern any statistically significant trend in the occurrence of hot Jupiters with stellar mass.

Additional Information

© 2019 The American Astronomical Society. Received 2019 June 2; revised 2019 July 26; accepted 2019 July 28; published 2019 September 11. Based on observations obtained with the Hungarian-made Automated Telescope Network. Based in part on observations obtained with the Tillinghast Reflector 1.5 m telescope and the 1.2 m telescope, both operated by the Smithsonian Astrophysical Observatory at the Fred Lawrence Whipple Observatory in Arizona. This work makes use of the Smithsonian Institution High Performance Cluster (SI/HPC). Based in part on observations made with the Southern African Large Telescope (SALT). We thank the referee for their careful reading of the manuscript; the comments significantly improved the quality of the paper. Work by G.Z. is provided by NASA through Hubble Fellowship grant HST-HF2-51402.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA under contract NAS 5-26555. HATNet operations have been funded by NASA grants NNG04GN74G and NNX13AJ15G. Follow-up of HATNet targets has been partially supported through NSF grant AST-1108686. G.Á.B., Z.C., and K.P. acknowledge partial support from NASA grant NNX09AB29G. J.H. acknowledges support from NASA grant NNX14AE87G. K.P. acknowledges support from NASA grants 80NSSC18K1009 and NNX17AB94G. We acknowledge partial support also from the Kepler Mission under NASA Cooperative Agreement NNX13AB58A (D.W.L., PI). Data presented in this paper are based on observations obtained at the HAT station at the Submillimeter Array of SAO, and the HAT station at the Fred Lawrence Whipple Observatory of SAO. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Observations on the LCO 1 m network were made through NOAO program 2017B-0039, and time on the WIYN 3.5 m was awarded through NOAO programs 2016B-0078 and 2017A-0125. Observations on the SMARTS 1.5 m CHIRON facility were made through the NOAO program 2019A-0004. M.G. and E.J. are FNRS Senior Research Associates. The research leading to these results has received funding from the grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. Funding for the TESS mission is provided by NASA's Science Mission directorate. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). G.K. is grateful for the support from the National Research, Development and Innovation Office (grant K 129249). G.K. is grateful for the support from the National Research, Development and Innovation Office (grant K 129249). The observations by the CHIRON spectrograph have been supported by the grant of the Hungarian Scientific Research Fund (OTKA, K-81373) to G.K. WASP-South is hosted by the South African Astronomical Observatory, and we are grateful for their ongoing support and assistance. Funding for WASP comes from consortium universities and from the UK's Science and Technology Facilities Council. Work by J.N.W. was supported by the Heising-Simons Foundation. This work is partly supported by JSPS KAKENHI grant Nos. JP18H01265 and JP18H05439, and JST PRESTO grant No. JPMJPR1775. Observations in the paper made use of the NN-EXPLORE Exoplanet and Stellar Speckle Imager (NESSI). NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. I.W. is supported by a Heising-Simons 51 Pegasi b postdoctoral fellowship. A. K. acknowledges support from the National Research Foundation (NRF) of South Africa. Some of the observations reported in this paper were obtained with the Southern African Large Telescope (SALT). Facilities: HATNet - , FLWO 1.5 m - , CTIO:1.5m, TESS - , SALT. - Software: lightkurve (Barentsen et al. 2019), emcee (Foreman-Mackey et al. 2013), simultrans (Herman et al. 2018), Astropy (Astropy Collaboration et al. 2013, 2018), fitsh (Pál 2012).

Attached Files

Published - Zhou_2019_AJ_158_141.pdf

Accepted Version - 1906.00462.pdf

Files

1906.00462.pdf

Files (42.3 MB)

Name	Size	Download all
1906.00462.pdf md5:3fd6133e8b695e7a0ce57bdb76ecbd3a	2.1 MB	Preview Download
Zhou_2019_AJ_158_141.pdf md5:36d20edd836f6fea5e8b80babd3ea557	40.2 MB	Preview Download

Additional details

	All versions	This version
Views	0	0
Downloads	0	0
Data volume	0 Bytes	0 Bytes