TESS Spots a Hot Jupiter with an Inner Transiting Neptune

Creators: Huang, Chelsea X.; Quinn, Samuel N.; Vanderburg, Andrew; Becker, Juliette; Rodriguez, Joseph E.; Pozuelos, Francisco J.; Gandolfi, Davide; Zhou, George; Mann, Andrew W.; Collins, Karen A.; Crossfield, Ian; Barkaoui, Khalid; Collins, Kevin I.; Fridlund, Malcolm; Gillon, Michaël; Gonzales, Erica J.; Günther, Maximilian N.; Henry, Todd J.; Howell, Steve B.; James, Hodari-Sadiki; Jao, Wei-Chun; Jehin, Emmanuël; Jensen, Eric L. N.; Kane, Stephen R.; Lissauer, Jack J.; Matthews, Elisabeth; Matson, Rachel A.; Paredes, Leonardo A.; Schlieder, Joshua E.; Stassun, Keivan G.; Shporer, Avi; Sha, Lizhou; Tan, Thiam-Guan; Georgieva, Iskra; Mathur, Savita; Palle, Enric; Persson, Carina M.; Eylen, Vincent Van; Ricker, George R.; Vanderspek, Roland K.; Latham, David W.; Winn, Joshua N.; Seager, S.; Jenkins, Jon M.; Burke, Christopher J.; Goeke, Robert F.; Rinehart, Stephen; Rose, Mark E.; Ting, Eric B.; Torres, Guillermo; Wong, Ian

Abstract

Hot Jupiters are rarely accompanied by other planets within a factor of a few in orbital distance. Previously, only two such systems have been found. Here, we report the discovery of a third system using data from the Transiting Exoplanet Survey Satellite (TESS). The host star, TOI-1130, is an eleventh magnitude K-dwarf in Gaia G-band. It has two transiting planets: a Neptune-sized planet (3.65 ± 0.10 R⊕) with a 4.1 days period, and a hot Jupiter (1.50^(+0.27)_(-0.22 R_J) with an 8.4 days period. Precise radial-velocity observations show that the mass of the hot Jupiter is 0.974^(+0.043)_(-0.044 M_J. For the inner Neptune, the data provide only an upper limit on the mass of 0.17 M_J (3σ). Nevertheless, we are confident that the inner planet is real, based on follow-up ground-based photometry and adaptive-optics imaging that rule out other plausible sources of the TESS transit signal. The unusual planetary architecture of and the brightness of the host star make TOI-1130 a good test case for planet formation theories, and an attractive target for future spectroscopic observations.

Additional Information

© 2020 The American Astronomical Society. Received 2019 December 8; revised 2020 January 27; accepted 2020 January 31; published 2020 March 19. We thank the TESS Mission team and Follow-up Working Group for the valuable data set. This Letter includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA's Science Mission directorate. C.X.H. and M.N.G. acknowledge support from MIT's Kavli Institute as Torres postdoctoral fellows. A.V.'s work was performed under contract with the California Institute of Technology/Jet Propulsion Laboratory funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. J.J.L.'s work was supported by the TESS GI grant G011108. J.N.W.'s work was partly supported by the Heising-Simons Foundation. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This work is based in part on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO program P103.C-0449. M.F., I.G., and C.M.P. gratefully acknowledge the support of the Swedish National Space Agency (DNR 163/16 and 174/18). The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013) ERC grant Agreement No. 336480, from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant FRFC 2.5.594.09.F, with the participation of the Swiss National Science Foundation (SNF). M.G. and E.J. are FNRS Senior Research Associates. This work makes use of observations from the LCOGT network. Facilities: TESS - , CHIRON - , LCOGT - , PEST - , TRAPPIST-South - , VLT. - Software: We made use of the Python programming language (Rossum 1995) and the open-source Python packages numpy (van der Walt et al. 2011), emcee (Foreman-Mackey et al. 2013), batman (Kreidberg 2015) rebound (Rein & Liu 2012). We also used Mercury (Chambers 1999) and AstroImageJ (Collins et al. 2017).

Attached Files

Published - Huang_2020_ApJL_892_L7.pdf

Files

Huang_2020_ApJL_892_L7.pdf

Files (1.9 MB)

Name	Size	Download all
Huang_2020_ApJL_892_L7.pdf md5:3deeaa891b806f9657446393b10537ce	1.9 MB	Preview Download

Additional details

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