TY - JOUR
T1 - A hot sub-Neptune in the desert and a temperate super-Earth around faint M dwarfs
T2 - Color validation of TOI-4479b and TOI-2081b
AU - Esparza-Borges, E.
AU - Parviainen, H.
AU - Murgas, F.
AU - Pallé, E.
AU - Maas, A.
AU - Morello, G.
AU - Zapatero-Osorio, M. R.
AU - Barkaoui, K.
AU - Narita, N.
AU - Fukui, A.
AU - Casasayas-Barris, N.
AU - Oshagh, M.
AU - Crouzet, N.
AU - Galán, D.
AU - Fernández, G. E.
AU - Kagetani, T.
AU - Kawauchi, K.
AU - Kodama, T.
AU - Korth, J.
AU - Kusakabe, N.
AU - Laza-Ramos, A.
AU - Luque, R.
AU - Livingston, J.
AU - Madrigal-Aguado, A.
AU - Mori, M.
AU - Orell-Miquel, J.
AU - Puig-Subirà, M.
AU - Stangret, M.
AU - Terada, Y.
AU - Watanabe, N.
AU - Zou, Y.
AU - Baliga Savel, A.
AU - Belinski, A. A.
AU - Collins, K.
AU - Dressing, C. D.
AU - Giacalone, S.
AU - Gill, H.
AU - Goliguzova, M. V.
AU - Ikoma, M.
AU - Jenkins, J. M.
AU - Tamura, M.
AU - Twicken, J. D.
AU - Ricker, G. R.
AU - Schwarz, R. P.
AU - Seager, S.
AU - Shporer, A.
AU - Vanderspek, R.
AU - Winn, J.
N1 - Funding Information:
We thank the anonymous referee for insightful suggestions, which added the clarity of this paper. 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. 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. We acknowledge the use of public TESS 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. This paper includes data collected by the TESS mission that are publicly available from the Mikulski Archive for Space Telescopes (MAST). This paper is based on observations made with the MuS-CAT2 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 based on observations made with the MuSCAT3 instrument, developed by the Astrobiology Center and under financial supports by JSPS KAKENHI (JP18H05439) and JST PRESTO (JPMJPR1775), at Faulkes Telescope North on Maui, HI, operated by the Las Cumbres Observatory. 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. 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 Astrofísica de Canarias. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofísica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOT. This work made use of tpfplotter by J. Lillo-Box (publicly available in www.github.com/jlillo/tpfplotter ), which also made use of the python packages astropy, lightkurve, matplotlib and numpy. E.E.-B. acknowledges financial support from the European Union and the State Agency of Investigation of the Spanish Ministry of Science and Innovation (MICINN) under the grant PRE2020-093107 of the Pre-Doc Program for the Training of Doctors (FPI-SO) through FSE funds. G.M. has received funding from the European Union s Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No. 895525. C.D.D. acknowledges support provided by the NASA Exoplanets Research Program (XRP) via grant 80NSSC20K0250. J.K. gratefully acknowledge the support of the Swedish National Space Agency (SNSA; DNR 2020-00104). R.L. acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación, through project PID2019-109522GB-C52, and the Centre of Excellence “Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). A.A.B. and M.V.G. acknowledge the support of Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780(N13.1902.21.0039). M.T. is supported by JSPS KAK-ENHI grant Nos.18H05442, 15H02063, and 22000005. M.R.Z.O. acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación through project PID2019-109522GB-C51. This work is partly supported by JSPS KAK-ENHI Grant Numbers 22000005, JP15H02063, JP17H04574, JP18H05439, P18H05442, JP20K14518, JP20K14521, JP21K13975, JP21K20376, Grant-in-Aid for JSPS Fellows Grant Number JP20J21872, JST CREST Grant Number JPMJCR1761, and the Astrobiology Center of National Institutes of Natural Sciences (NINS) (Grant Numbers AB022006, AB031010, AB031014).
Publisher Copyright:
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PY - 2022/10/1
Y1 - 2022/10/1
N2 - Aims. We report the discovery and validation of two TESS exoplanets orbiting faint M dwarfs: TOI-4479b and TOI-2081b. Methods. We jointly analyzed space (TESS mission) and ground-based (MuSCAT2, MuSCAT3 and SINISTRO instruments) light curves using our multicolor photometry transit analysis pipeline. This allowed us to compute contamination limits for both candidates and validate them as planet-sized companions. Results. We found TOI-4479b to be a sub-Neptune-sized planet (Rp = 2.82-0.63+0.65 R⊕) and TOI-2081b to be a super-Earth-sized planet (Rp = 2.04-0.54+0.50 R⊕). Furthermore, we obtained that TOI-4479b, with a short orbital period of 1.15890-0.00001+0.00002 days, lies within the Neptune desert and is in fact the largest nearly ultra-short period planet around an M dwarf known to date. Conclusions. These results make TOI-4479b rare among the currently known exoplanet population of M dwarf stars and an especially interesting target for spectroscopic follow-up and future studies of planet formation and evolution.
AB - Aims. We report the discovery and validation of two TESS exoplanets orbiting faint M dwarfs: TOI-4479b and TOI-2081b. Methods. We jointly analyzed space (TESS mission) and ground-based (MuSCAT2, MuSCAT3 and SINISTRO instruments) light curves using our multicolor photometry transit analysis pipeline. This allowed us to compute contamination limits for both candidates and validate them as planet-sized companions. Results. We found TOI-4479b to be a sub-Neptune-sized planet (Rp = 2.82-0.63+0.65 R⊕) and TOI-2081b to be a super-Earth-sized planet (Rp = 2.04-0.54+0.50 R⊕). Furthermore, we obtained that TOI-4479b, with a short orbital period of 1.15890-0.00001+0.00002 days, lies within the Neptune desert and is in fact the largest nearly ultra-short period planet around an M dwarf known to date. Conclusions. These results make TOI-4479b rare among the currently known exoplanet population of M dwarf stars and an especially interesting target for spectroscopic follow-up and future studies of planet formation and evolution.
KW - Methods: observational
KW - Planets and satellites: detection
KW - Planets and satellites: general
KW - Planets and satellites: individual: TOI-2081b
KW - Planets and satellites: individual: TOI-4479b
KW - Techniques: photometric
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U2 - 10.1051/0004-6361/202243731
DO - 10.1051/0004-6361/202243731
M3 - Article
AN - SCOPUS:85141010423
VL - 666
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
M1 - A10
ER -