TOI 560: Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS, and HIRES RVs

Creators: El Mufti, Mohammed; Plavchan, Peter P.; Isaacson, Howard; Cale, Bryson L.; Feliz, Dax L.; Reefe, Michael A.; Hellier, Coel; Stassun, Keivan; Eastman, Jason; Polanski, Alex; Crossfield, Ian J. M.; Gaidos, Eric; Kostov, Veselin; Wittrock, Justin M.; Villaseñor, Joel; Schlieder, Joshua E.; Bouma, Luke G.; Collins, Kevin I.; Zohrabi, Farzaneh; Lee, Rena A.; Sohani, Ahmad; Berberian, John; Vermilion, David; Newman, Patrick; Geneser, Claire; Tanner, Angelle; Batalha, Natalie M.; Dressing, Courtney; Fulton, Benjamin; Howard, Andrew W.; Huber, Daniel; Kane, Stephen R.; Petigura, Erik A.; Robertson, Paul; Roy, Arpita; Weiss, Lauren M.; Behmard, Aida; Beard, Corey; Chontos, Ashley; Dai, Fei; Dalba, Paul A.; Fetherolf, Tara; Giacalone, Steven; Hill, Michelle L.; Hirsch, Lea A.; Holcomb, Rae; Lubin, Jack; Mayo, Andrew; Močnik, Teo; Akana Murphy, Joseph M.; Rosenthal, Lee J.; Rubenzahl, Ryan A.; Scarsdale, Nicholas; Stockdale, Christopher; Collins, Karen; Cloutier, Ryan; Relles, Howard; Tan, Thiam-Guan; Scott, Nicholas J.; Hartman, Zach; Matthews, Elisabeth; Ciardi, David R.; Gonzales, Erica; Matson, Rachel A.; Beichman, Charles; Bieryla, Allyson; Furlan, E.; Gnilka, Crystal L.; Howell, Steve B.; Ziegler, Carl; Briceño, César; Law, Nicholas; Mann, Andrew W.; Rabus, Markus; Johnson, Marshall C.; Christiansen, Jessie; Kreidberg, Laura; Berardo, David Anthony; Deming, Drake; Gorjian, Varoujan; Morales, Farisa Y.; Benneke, Björn; Dragomir, Diana; Wittenmyer, Robert A.; Ballard, Sarah; Bowler, Brendan P.; Horner, Jonathan; Kielkopf, John; Liu, Huigen; Shporer, Avi; Tinney, C. G.; Zhang, Hui; Wright, Duncan J.; Addison, Brett C.; Mengel, Matthew W.; Okumura, Jack

Abstract

We validate the presence of a two-planet system orbiting the 0.15–1.4 Gyr K4 dwarf TOI 560 (HD 73583). The system consists of an inner moderately eccentric transiting mini-Neptune (TOI 560 b, P = 6.3980661_(−0.0000097)^(+0.0000095) days, e = 0.294_(−0.062)^(+0.13), M = 0.94_(-0.23)^(+0.31)M_(Nep) initially discovered in the Sector 8 Transiting Exoplanet Survey Satellite (TESS) mission observations, and a transiting mini-Neptune (TOI 560 c, P = 18.8805_(−0.0011)^(+0.0024) days, M = 1.32_(−0.32)^(+0.29)M_(Nep) discovered in the Sector 34 observations, in a rare near-1:3 orbital resonance. We utilize photometric data from TESS Spitzer, and ground-based follow-up observations to confirm the ephemerides and period of the transiting planets, vet false-positive scenarios, and detect the photoeccentric effect for TOI 560 b. We obtain follow-up spectroscopy and corresponding precise radial velocities (RVs) with the iSHELL spectrograph at the NASA Infrared Telescope Facility and the HIRES Spectrograph at Keck Observatory to validate the planetary nature of these signals, which we combine with published Planet Finder Spectrograph RVs from the Magellan Observatory. We detect the masses of both planets at >3σ significance. We apply a Gaussian process (GP) model to the TESS light curves to place priors on a chromatic RV GP model to constrain the stellar activity of the TOI 560 host star, and confirm a strong wavelength dependence for the stellar activity demonstrating the ability of near-IR RVs to mitigate stellar activity for young K dwarfs. TOI 560 is a nearby moderately young multiplanet system with two planets suitable for atmospheric characterization with the James Webb Space Telescope and other upcoming missions. In particular, it will undergo six transit pairs separated by <6 hr before 2027 June.

Additional Information

© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. M.M. and P.P.P. acknowledge support from NASA (Exoplanet Research Program award No. 80NSSC20K0251, TESS Cycle 3 Guest Investigator Program award No. 80NSSC21K0349, JPL Research and Technology Development, and Keck Observatory Data Analysis) and the NSF (Astronomy and Astrophysics grants No. 1716202 and 2006517), and the Mt Cuba Astronomical Foundation. This paper includes data collected by the NASA TESS mission that are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA's Science Mission Directorate. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community, where the iSHELL and HIRES observations were recorded. We are most fortunate to have the opportunity to conduct observations from this mountain. The authors also wish to thank the California Planet Search (CPS) collaboration for carrying out the HIRES observations recorded in 2020 presented in this work. This work includes observations obtained at the international Gemini Observatory, a program of NSF's NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. Some of the observations in the paper made use of the High-Resolution Imaging instrument Zorro obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. Zorro was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. On behalf of the Gemini Observatory partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). Data were collected as part of program GN-2019A-LP-101. Based on data collected under the NGTS project at the ESO La Silla Paranal Observatory. The NGTS facility is operated by the consortium institutes with support from the UK Science and Technology Facilities Council (STFC) projects ST/M001962/1 and ST/S002642/1. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This paper is based on observations obtained from the Las Campanas Remote Observatory that is a partnership between Carnegie Observatories, The Astro-Physics Corporation, Howard Hedlund, Michael Long, Dave Jurasevich, and SSC Observatories. MINERVA-Australis is supported by Australian Research Council LIEF grant LE160100001, Discovery grant DP180100972, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. We respectfully acknowledge the traditional custodians of all lands throughout Australia, and recognize their continued cultural and spiritual connection to the land, waterways, cosmos, and community. We pay our deepest respects to all Elders, ancestors and descendants of the Giabal, Jarowair, and Kambuwal nations, upon whose lands the Minerva-Australis facility at Mt Kent is situated. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. E.A.P. acknowledges the support of the Alfred P. Sloan Foundation. L.M.W. is supported by the Beatrice Watson Parrent Fellowship and NASA ADAP grant 80NSSC19K0597. A.C. is supported by the NSF Graduate Research Fellowship, grant No. DGE 1842402. D.H. acknowledges support from the Alfred P. Sloan Foundation, the National Aeronautics and Space Administration (80NSSC19K0379), and the National Science Foundation (AST-1717000). I.J.M.C. acknowledges support from the NSF through grant AST-1824644. P.D. acknowledges support from a National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1903811. A.B. is supported by the NSF Graduate Research Fellowship, grant No. DGE 1745301. R.A.R. is supported by the NSF Graduate Research Fellowship, grant No. DGE 1745301. C.D.D. acknowledges the support of the Hellman Family Faculty Fund, the Alfred P. Sloan Foundation, the David & Lucile Packard Foundation, and the National Aeronautics and Space Administration via the TESS Guest Investigator Program (80NSSC18K1583). J.M.A.M. is supported by the NSF Graduate Research Fellowship, grant No. DGE-1842400. J.M.A.M. also acknowledges the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining grant No. 1829740, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. T.F. acknowledges support from the University of California President's Postdoctoral Fellowship Program. C.A.B notes that some of the research described in this publication was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Facilities: NASA IRTF - , Keck Observatory - , Magellan Telescope - , Gemini North - , Gemini South - , Fred L. Whipple Observatory - , TESS - , ESO La Silla Paranal Observatory - , Las Cumbres Observatory - , SOAR telescope. - Software: Python: pychell (Cale et al. 2019), AstroImageJ (Collins et al. 2017), EDI-Vetter Unplugged (Zink et al. 2020),DAVE (Kostov et al. 2019), tpfplotter (Aller et al. 2020), REBOUND (Rein & Liu 2012; Rein & Spiegel 2015), NumPy (Harris et al. 2020), SciPy (Virtanen et al. 2020), Matplotlib (Hunter 2007), AstroPy (Astropy Collaboration et al. 2013), Numba (Finkel et al. 2015), EXOFASTv2 (Eastman et al. 2013).

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