HD 219134 Revisited: Planet d Transit Upper Limit and Planet f Transit Nondetection with ASTERIA and TESS

Creators: Seager, Sara; Knapp, Mary; Demory, Brice-Olivier; Krishnamurthy, Akshata; Huang, Chelsea X.; Agusti, Mariona Badenas; Shporer, Avi; Weisserman, Drew; Becker, Juliette; Vanderburg, Andrew; Smith, Matthew; Pong, Christopher M.; Bailey, Vanessa P.; Donner, Amanda; Di Pasquale, Peter; Campuzano, Brian; Smith, Colin; Luu, Jason; Babuscia, Alessandra; Bocchino, Robert L., Jr.; Loveland, Jessica; Colley, Cody; Gedenk, Tobias; Kulkarni, Tejas; Hughes, Kyle; White, Mary; Krajewski, Joel; Fesq, Lorraine; Ricker, George; Vanderspek, Roland; Latham, David W.; Jenkins, Jon M.; Winn, Joshua N.; Caldwell, Douglas A.; Collins, Karen A.; Dragomir, Diana; Fausnaugh, Michael; Glidden, Ana; Schlieder, Joshua E.; Twicken, Joseph D.; Wohler, Bill

Abstract

HD 219134 is a K3V dwarf star with six reported radial-velocity discovered planets. The two innermost planets b and c show transits, raising the possibility of this system to be the nearest (6.53 pc), brightest (V = 5.57) example of a star with a compact multiple transiting planet system. Ground-based searches for transits of planets beyond b and c are not feasible because of the infrequent transits, long transit duration (~5 hr), shallow transit depths (<1%), and large transit time uncertainty (~half a day). We use the space-based telescopes the Arcsecond Space Telescope Enabling Research in Astrophysics (ASTERIA) and the Transiting Exoplanet Survey Satellite (TESS) to search for transits of planets f (P = 22.717 days and M sin i = 7.3 ± 0.04M_⊕) and d (P = 46.859 days and M sin i = 16.7 ± 0.64M_⊕). ASTERIA was a technology demonstration CubeSat with an opportunity for science in an extended program. ASTERIA observations of HD 219134 were designed to cover the 3σ transit windows for planets f and d via repeated visits over many months. While TESS has much higher sensitivity and more continuous time coverage than ASTERIA, only the HD 219134 f transit window fell within the TESS survey's observations. Our TESS photometric results definitively rule out planetary transits for HD 219134 f. We do not detect the Neptune-mass HD 219134 d transits and our ASTERIA data are sensitive to planets as small as 3.6 R_⊕. We provide TESS updated transit times and periods for HD 219134 b and c, which are designated TOI 1469.01 and 1469.02 respectively.

Additional Information

© 2021. The American Astronomical Society. Received 2020 May 17; revised 2020 November 14; accepted 2020 November 22; published 2021 February 12. We acknowledge contributions from the extended team that supported ASTERIA development, integration and test, and operations, including Len Day, Maria de Soria Santacruz-Pich, Carl Felten, Janan Ferdosi, Kristine Fong, Harrison Herzog, Jim Hofman, David Kessler, Roger Klemm, Jules Lee, Jason Munger, Lori Moore, Esha Murty, Chris Shelton, David Sternberg, Rob Sweet, Kerry Wahl, Jacqueline Weiler, Thomas Werne, Shannon Zareh, and Ansel Rothstein-Dowden. We also recognize the JPL line organization and technical mentors for the expertise they provided throughout the project. We thank the JPL program management, especially Sarah Gavit and Pat Beauchamp, who oversaw ASTERIA within the Engineering and Science Directorate at JPL. We also thank Daniel Coulter and Leslie Livesay for their support. The research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Government sponsorship acknowledged. We would also like to thank the DSS-17 ground station team at Morehead State University (MSU) in Kentucky. We acknowledge the outstanding efforts of the student operators, technical staff, and program management at Morehead State University, including Chloe Hart, Sarah Wilczewski, Alex Roberts, Maria Lemaster, Lacy Wallace, Rebecca Mikula, Bob Kroll, Michael Combs, and Benjamin Malphrus. Funding for the TESS mission is provided by NASA's Science Mission directorate. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). 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. J.C.B. has been supported by the Heising-Simons 51 Pegasi b postdoctoral fellowship. We acknowledge the Massachusett Tribe, the tribe of indigenous peoples from whom the Colony, Province, and Commonwealth of Massachusetts have taken their name. We would like to pay our respects to the ancestral bloodline of the Massachusett tribe and their descendants who still inhabit historical Massachusett tribe territories to this day. Facilities: TESS - , ASTERIA - , MAST. - Software: SPOC R4.0, QLP, Numpy (van der Walt et al. 2011), Scipy (Virtanen et al. 2020), Astropy (Astropy Collaboration et al. 2013, 2018), allesfitter (Günther & Daylan 2020), photutils (Bradley et al. 2019).

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