Radial velocity confirmation of a hot super-Neptune discovered by TESS with a warm Saturn–mass companion

Creators: Knudstrup, E.; Gandolfi, D.; Nowak, G.; Persson, C. M.; Furlan, E.; Livingston, J.; Matthews, E.; Lundkvist, M. S.; Winther, M. L.; Rørsted, J. L.; Albrecht, S. H.; Goffo, E.; Carleo, I.; Deeg, H. J.; Collins, K. A.; Narita, N.; Isaacson, H.; Redfield, S.; Dai, F.; Hirano, T.; Akana Murphy, J. M.; Beard, C.; Buchhave, L. A.; Cary, S.; Chontos, A.; Crossfield, I.; Cochran, W. D.; Conti, D.; Dalba, P. A.; Esposito, M.; Fajardo-Acosta, S.; Giacalone, S.; Grunblatt, S. K.; Guerra, P.; Hatzes, A. P.; Holcomb, R.; Horta, F. G.; Howard, A. W.; Huber, D.; Jenkins, J. M.; Kabáth, P.; Kane, S.; Korth, J.; Lam, K. W. F.; Lester, K. V.; Matson, R.; McLeod, K. K.; Orell-Miquel, J.; Murgas, F.; Pallé, E.; Polanski, A. S.; Ricker, G.; Robertson, P.; Rubenzahl, R. A.; Schlieder, J. E.; Seager, S.; Smith, A. M. S.; Tenenbaum, P.; Turtelboom, E.; Vanderspek, R.; Weiss, L.; Winn, J.

Abstract

We report the discovery and confirmation of the planetary system TOI-1288. This late G dwarf harbours two planets: TOI-1288 b and TOI-1288 c. We combine TESS space-borne and ground-based transit photometry with HARPS-N and HIRES high-precision Doppler measurements, which we use to constrain the masses of both planets in the system and the radius of planet b. TOI-1288 b has a period of 2.699835^(+0.000004)_(-0.000003) d, a radius of 5.24 ± 0.09 R_⊕, and a mass of 42 ± 3 M_⊕, making this planet a hot transiting super-Neptune situated right in the Neptunian desert. This desert refers to a paucity of Neptune-sized planets on short period orbits. Our 2.4-yr-long Doppler monitoring of TOI-1288 revealed the presence of a Saturn–mass planet on a moderately eccentric orbit (0.13^(+0.07)_(-0.09)) with a minimum mass of 84 ± 7 M_⊕ and a period of 443⁺¹¹₋₁₃ d. The five sectors worth of TESS data do not cover our expected mid-transit time for TOI-1288 c, and we do not detect a transit for this planet in these sectors.

Additional Information

© 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). We thank the anonymous referee for a timely review. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and the TESS Science Operations Center. Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation (Grant agreement no.: DNRF106). Based on observations (programme IDs: A40TAC_22, A41TAC_19, A41TAC_49, A43TAC_11, CAT19A_162, CAT22A_111, and ITP19_1) made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland, and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. We are extremely grateful to the NOT and TNG staff members for their unique and superb support during the observations. 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. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. 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. We are most fortunate to have the opportunity to conduct observations from this mountain. 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. This research has made use of the Exoplanet Follow-up Observation Program (ExoFOP; DOI: 10.26134/ExoFOP5) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. The 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. The authors are honoured to be permitted to conduct observations on Iolkam Du'ag (Kitt Peak), a mountain within the Tohono O'odham Nation with particular significance to the Tohono O'odham people. This work presents results from the European Space Agency (ESA) space mission Gaia. Gaia data are being processed by the GaiaData Processing and Analysis Consortium (DPAC). Funding for the DPAC is provided by national institutions, in particular, the institutions participating in the GaiaMultiLateral Agreement (MLA). The Gaia mission website is https://www.cosmos.esa.int/gaia. The Gaia archive website is https://archives.esac.esa.int/gaia. Some of the observations in the paper made use of the High-Resolution Imaging instrument 'Alopeke. 'Alopeke 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. Data were reduced using a software pipeline originally written by Elliott Horch and Mark Everett. 'Alopeke was mounted on the Gemini North telescope of the international Gemini Observatory, a program of NSF's OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini 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). E.K. and S.A. acknowledge the support from the Danish Council for Independent Research through a grant no. 2032-00230B. CMP and JK gratefully acknowledge the support of the Swedish National Space Agency (SNSA; DNR 2020-00104). MSL would like to acknowledge the support from VILLUM FONDEN (research grant 42101) and The Independent Research Fund Denmark's Inge Lehmann program (grant agreement no.: 1131-00014B). This work is partly supported by JSPS KAKENHI grant numbers JP17H04574, JP18H05439, JP20K14521, JP19K14783, and JP21H00035, JST CREST grant number JPMJCR1761, the Astrobiology Center of National Institutes of Natural Sciences (NINS) (grant number AB031010). DH acknowledges support from the Alfred P. Sloan Foundation and the National Aeronautics and Space Administration (80NSSC21K0652). KWFL was supported by Deutsche Forschungsgemeinschaft grants RA714/14-1 within the DFG Schwerpunkt SPP 1992, Exploring the Diversity of Extrasolar Planets. KKM acknowledges support from the New York Community Trust Fund for Astrophysical Research. Parts of the numerical results presented in this work were obtained at the Centre for Scientific Computing, Aarhus https://phys.au.dk/forskning/faciliteter/cscaa/. This research made use of Astropy,7 a community-developed core PYTHON package for Astronomy (Astropy Collaboration et al. 2013, 2018, 2022). This research made use of Astroquery (Ginsburg et al. 2019). This research made use of TESS cut (Brasseur et al. 2019). This research has made use of 'Aladin sky atlas' developed at CDS, Strasbourg Observatory, France (Bonnarel et al. 2000; Boch & Fernique 2014). DATA AVAILABILITY. The radial velocities underlying this article are available in its online supplementary material.

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