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

Seager, Sara and Knapp, Mary and Demory, Brice-Olivier and Krishnamurthy, Akshata and Huang, Chelsea X. and Agusti, Mariona Badenas and Shporer, Avi and Weisserman, Drew and Becker, Juliette and Vanderburg, Andrew and Smith, Matthew and Pong, Christopher M. and Bailey, Vanessa P. and Donner, Amanda and Di Pasquale, Peter and Campuzano, Brian and Smith, Colin and Luu, Jason and Babuscia, Alessandra and Bocchino, Robert L., Jr. and Loveland, Jessica and Colley, Cody and Gedenk, Tobias and Kulkarni, Tejas and Hughes, Kyle and White, Mary and Krajewski, Joel and Fesq, Lorraine and Ricker, George and Vanderspek, Roland and Latham, David W. and Jenkins, Jon M. and Winn, Joshua N. and Caldwell, Douglas A. and Collins, Karen A. and Dragomir, Diana and Fausnaugh, Michael and Glidden, Ana and Schlieder, Joshua E. and Twicken, Joseph D. and Wohler, Bill (2021) HD 219134 Revisited: Planet d Transit Upper Limit and Planet f Transit Nondetection with ASTERIA and TESS. Astronomical Journal, 161 (3). Art. No. 117. ISSN 1538-3881. https://resolver.caltech.edu/CaltechAUTHORS:20210312-081600982

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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.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-3881/abcd3dDOIArticle
ORCID:
AuthorORCID
Seager, Sara0000-0002-6892-6948
Knapp, Mary0000-0002-5318-7660
Demory, Brice-Olivier0000-0002-9355-5165
Krishnamurthy, Akshata0000-0002-8781-2743
Huang, Chelsea X.0000-0003-0918-7484
Agusti, Mariona Badenas0000-0003-4903-567X
Shporer, Avi0000-0002-1836-3120
Weisserman, Drew0000-0002-7992-469X
Becker, Juliette0000-0002-7733-4522
Vanderburg, Andrew0000-0001-7246-5438
Smith, Matthew0000-0003-0103-8820
Bailey, Vanessa P.0000-0002-5407-2806
Campuzano, Brian0000-0002-4761-1875
Babuscia, Alessandra0000-0002-8132-3201
Gedenk, Tobias0000-0002-2705-3394
Ricker, George0000-0003-2058-6662
Vanderspek, Roland0000-0001-6763-6562
Latham, David W.0000-0001-9911-7388
Jenkins, Jon M.0000-0002-4715-9460
Winn, Joshua N.0000-0002-4265-047X
Caldwell, Douglas A.0000-0003-1963-9616
Collins, Karen A.0000-0001-6588-9574
Dragomir, Diana0000-0003-2313-467X
Fausnaugh, Michael0000-0002-9113-7162
Glidden, Ana0000-0002-5322-2315
Schlieder, Joshua E.0000-0001-5347-7062
Twicken, Joseph D.0000-0002-6778-7552
Wohler, Bill0000-0002-5402-9613
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).
Funders:
Funding AgencyGrant Number
NASA/JPL/CaltechUNSPECIFIED
Heising-Simons Foundation51 Pegasi b Fellowship
Juan Carlos Torres FellowshipUNSPECIFIED
NASA Sagan FellowshipUNSPECIFIED
Subject Keywords:Exoplanet astronomy; Broad band photometry
Issue or Number:3
Classification Code:Unified Astronomy Thesaurus concepts: Exoplanet astronomy (486); Broad band photometry (184)
Record Number:CaltechAUTHORS:20210312-081600982
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20210312-081600982
Official Citation:Sara Seager et al 2021 AJ 161 117
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:108411
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:12 Mar 2021 17:44
Last Modified:12 Mar 2021 17:44

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