Dreizler, S., Crossfield, M., Kossakowski, D., Plavchan, P., Jeffers, V., Kemmer, J., Luque, R., Espinoza, N., Pallé, E., Stassun, K., Matthews, E., Cale, B., Caballero, A., Schlecker, M., Lillo-Box, J., Zechmeister, M., Lalitha, S., Reiners, A., Soubkiou, A., Bitsch, B., Osorio, R. Zapatero, Chaturvedi, P., Hatzes, P., Ricker, G., Vanderspek, R., Latham, W., Seager, S., Winn, J., Jenkins, J. M., Aceituno, J., Amado, J., Barkaoui, K., Barbieri, M., Batalha, M., Bauer, F., Benneke, B., Benkhaldoun, Z., C, Beichman, Berberian, J., Burt, J., Butler, P., Caldwell, A., Chintada, A., Chontos, A., Christiansen, L., Ciardi, D. R., Cifuentes, C., Collins, A., Collins, I., Combs, D., Cortés-Contreras, M., Crane, D., Daylan, T., Dragomir, D., Esparza-Borges, E., Evans, P., Feng, F., Flowers, E., Fukui, A., Fulton, B., Furlan, E., Gaidos, E., Geneser, C., Giacalone, S., Gillon, M., Gonzales, E., Gorjian, V., Hellier, C., Hidalgo, D., Howard, W., Howell, S., Huber, D., Isaacson, H., Jehin, E., Jensen, N., Kaminski, A., Kane, R., Kawauchi, K., Kielkopf, F., Klahr, H., Kosiarek, R., Kreidberg, L., Kürster, Lafarga, M., Livingston, J., Louie, D., Mann, A., Madrigal-Aguado, A., Matson, A., Mocnik, T., Morales, C., Muirhead, S., Murgas, F., Nandakumar, S., Narita, N., Nowak, G., Oshagh, M., Parviainen, H., Passegger, M., Pollacco, D., Pozuelos, J., Quirrenbach, A., Reefe, M., Ribas, I., Robertson, P., Rodríguez-López, C., Rose, E., Roy, A., Schweitzer, A., Schlieder, J., Shectman, S., Tanner, A., Şenavcı, V., Teske, J., Twicken, D., Villasenor, J., Wang, S. X., Weiss, M., Wittrock, J., Yılmaz, M., Zohrabi, F., German Research Foundation, Max Planck Society, European Commission, Consejo Superior de Investigaciones Científicas (España), Thuringian Ministry of Education, Science and Culture, Klaus Tschira Foundation, Ministerio de Economía y Competitividad (España), Junta de Andalucía, European Research Council, Ministerio de Ciencia, Innovación y Universidades (España), Comisión Nacional de Investigación Científica y Tecnológica (Chile), Science and Technology Facilities Council (UK), Generalitat de Catalunya, Dreizler, Stefan https://orcid.org/0000-0001-6187-5941, Plavchan, Peter https://orcid.org/0000-0002-8864-1667, Kemmer, Jonas https://orcid.org/0000-0003-3929-1442, Pallé, Enric https://orcid.org/0000-0003-0987-1593, Caballero, José https://orcid.org/0000-0002-7349-1387, Lillo Box, Jorge https://orcid.org/0000-0003-3742-1987, Amado, Pedro José https://orcid.org/0000-0002-8388-6040, Cifuentes, C. https://orcid.org/0000-0003-1715-5087, European Union through, FEDER/ERF FICTS-2011-02, Spanish Ministry of Economy, Klaus Tschira Stiftung, state of Baden-Wurttemberg, state of Niedersachsen, Junta de Andalucia, National Aeronautics & Space Administration, NASA, Alfried Krupp von Bohlen und Halbach Foundation, Spanish Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades, European FEDER/ERF funds, Generalitat de Catalunya through CERCA programme, UK Research & Innovation, UKRI, Science & Technology Facilities Council, STFC, Ministry of Education, MEXT Culture, Sports, Science and Technology (Japan), Japan Society for the Promotion of Science Grants-in-Aid for Scientific Research, KAKENHI, MDM-2017-0737, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, National Aeronautics and Space Administration (NASA), European Research Council (ERC), Agencia Estatal de Investigación (AEI), Ministerio de Economía y Competitividad (MINECO), Science and Technology Facilities Council (STFC), Centre National de la Recherche Scientifique (CNRS), and Japan Society for the Promotion of Science (KAKENHI)
We report the discovery of a Neptune-like planet (LP 714-47 b, P = 4.05204 d, mb = 30.8 ± 1.5Mpdbl, Rb = 4.7 ± 0.3 Rpdbl) located in the "hot Neptune desert". Confirmation of the TESS Object of Interest (TOI 442.01) was achieved with radial-velocity follow-up using CARMENES, ESPRESSO, HIRES, iSHELL, and PFS, as well as from photometric data using TESS, Spitzer, and ground-based photometry from MuSCAT2, TRAPPIST-South, MONET-South, the George Mason University telescope, the Las Cumbres Observatory Global Telescope network, the El Sauce telescope, the TÜBITAK National Observatory, the University of Louisville Manner Telescope, and WASP-South. We also present high-spatial resolution adaptive optics imaging with the Gemini Near-Infrared Imager. The low uncertainties in the mass and radius determination place LP 714-47 b among physically well-characterised planets, allowing for a meaningful comparison with planet structure models. The host star LP 714-47 is a slowly rotating early M dwarf (Teff = 3950 ± 51 K) with a mass of 0.59 ± 0.02Mpdbl and a radius of 0.58 ± 0.02Rpdbl. From long-term photometric monitoring and spectroscopic activity indicators, we determine a stellar rotation period of about 33 d. The stellar activity is also manifested as correlated noise in the radial-velocity data. In the power spectrum of the radial-velocity data, we detect a second signal with a period of 16 days in addition to the four-day signal of the planet. This could be shown to be a harmonic of the stellar rotation period or the signal of a second planet. It may be possible to tell the difference once more TESS data and radial-velocity data are obtained. © ESO 2020., CARMENES is an instrument for the Centro Astronomico Hispano-Aleman de Calar Alto (CAHA, Almeria, Spain). CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Institut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia and Centro Astronomico Hispano-Aleman), with additional contributions by the Spanish Ministry of Economy, the German Science Foundation through the Major Research Instrumentation Programme and DFG Research Unit FOR2544 "Blue Planets around Red Stars", the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, and by the Junta de Andalucia. Based on data from the CARMENES data archive at CAB (INTA-CSIC). We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. 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 observations in the paper made use of the High-Resolution Imaging instrument Zorro. 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. Zorro was mounted on the Gemini South 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 Investigacion y Desarrollo (Chile), Ministerio de Ciencia, Tecnologia e Innovacion (Argentina), Ministerio da Ciencia, Tecnologia, Inovacoes e Comunicacoes (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This work makes use of observations from the LCOGT network. This article is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sanchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. This paper is also based on observations made in the Observatorios de Canarias del IAC with the Nordic Optical Telescope operated on the island of La Palma by NOTSA in the Observatorio del Roque de los Muchachos. Data were partly obtained with the MONET/South telescope of the MOnitoring NEtwork of Telescopes, funded by the Alfried Krupp von Bohlen und Halbach Foundation, Essen, and operated by the Georg-August-Universitat Gottingen, the McDonald Observatory of the University of Texas at Austin, and the South African Astronomical Observatory. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research made use of Lightkurve, a Python package for Kepler and TESS data analysis (Lightkurve Collaboration 2018). We acknowledge financial support from the Spanish Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades and the European FEDER/ERF funds through projects AYA2015-69350-C3-2-P, PGC2018098153-B-C31/C33, AYA2016-79425-C3-1/2/3-P, AYA2018-84089, BES-2017080769, ESP2016-80435-C2-1/2-R, ESP2017-87676-C5-1/2/5-R, Instituto de Astrofisica de Andalucia (SEV-2017-0709), the Generalitat de Catalunya through CERCA programme, the UK Science and Technology Facilities Council through grant ST/P000592/1, the JSPS KAKENHI through grants 17H04574, JP18H01265, and 18H05439, and the JST PRESTO through grant JPMJPR1775, the "la Caixa" INPhINIT Fellowship Grant LCF/BQ/IN17/11620033 for Doctoral studies at Spanish Research Centres of Excellence, V.M.P. acknowledges support from NASA Grant NNX17AG24G, Support for this work was provided to J.K.T. by NASA through Hubble Fellowship grant HST-HF2-51399.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. The research leading to these results has received funding 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. S.D. acknowledges support from the Deutsche Forschungsgemeinschaft under Research Unit FOR2544 "Blue Planets around Red Stars", project no. RE 281/32-1. M.Z. acknowledges support from the Deutsche Forschungsgemeinschaft under DFG RE 1664/12-1 and Research Unit FOR2544 "Blue Planets around Red Stars", project no. RE 1664/14-1. M.S. was supported by the DFG Research Unit FOR2544 "Blue Planets around Red Stars", project no. RE 2694/4-1. I.J.M.C. and E.M. acknowledge support from the National Science Foundation through grant AST-1824644. B.B. thanks the European Research Council (ERC Starting Grant 757 448-PAMDORA) for their financial support. D.D. acknowledges support from NASA through Caltech/JPL grant RSA-1006130 and through the TESS Guest Investigator Program Grant 80NSSC19K1727. P.P. acknowledges support from NASA (16-APROBES16-0020 and the Exoplanet Exploration Program) and the National Science Foundation (Astronomy and Astrophysics grant 1716202), the Mt Cuba Astronomical Foundation, and George Mason University start-up and instructional equipment funds. The NASA Infrared Telescope Facility is operated by the University of Hawaii under contract NNH14CK55B with the National Aeronautics and Space Administration. M.R.K is supported by the NSF Graduate Research Fellowship, grant No. DGE 1 339 067. M.Y. and H.V.S. thank to TUB.ITAK for a partial support in using T100 telescope with project number 19AT100-1474. J.N.W. thanks the Heising-Simons Foundation for support. D.H. acknowledges support from the Alfred P. Sloan Foundation, the National Aeronautics and Space Administration (80NSSC18K1585, 80NSSC19K0379), and the National Science Foundation (AST-1 717 000). T.D. acknowledges support from MIT's Kavli Institute as a Kavli postdoctoral fellow. This work made use of tpfplotter (developed by J. Lillo-Box, which also made use of the python packages astropy, lightkurve, matplotlib and numpy. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). The authors wish to recognise and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Finally, we thank the referee for detailed and helpful comments.