TY - JOUR
T1 - The GAPS programme at TNG
T2 - XL. A puffy and warm Neptune-sized planet and an outer Neptune-mass candidate orbiting the solar-Type star TOI-1422
AU - Naponiello, L.
AU - Mancini, L.
AU - Damasso, M.
AU - Bonomo, A. S.
AU - Sozzetti, A.
AU - Nardiello, D.
AU - Biazzo, K.
AU - Stognone, R. G.
AU - Lillo-Box, J.
AU - Lanza, A. F.
AU - Poretti, E.
AU - Lissauer, J. J.
AU - Zeng, L.
AU - Bieryla, A.
AU - Hebrard, G.
AU - Basilicata, M.
AU - Benatti, S.
AU - Bignamini, A.
AU - Borsa, F.
AU - Claudi, R.
AU - Cosentino, R.
AU - Covino, E.
AU - De Gurtubai, A.
AU - Delfosse, X.
AU - Desidera, S.
AU - Dragomir, D.
AU - Eastman, J. D.
AU - Essack, Z.
AU - Fiorenzano, A. F.M.
AU - Giacobbe, P.
AU - Harutyunyan, A.
AU - Heidari, N.
AU - Hellier, C.
AU - Jenkins, J. M.
AU - Knapic, C.
AU - Konig, P. C.
AU - Latham, D. W.
AU - Magazzu, A.
AU - Maggio, A.
AU - Maldonado, J.
AU - Micela, G.
AU - Molinari, E.
AU - Molinaro, M.
AU - Morgan, E. H.
AU - Moutou, C.
AU - Nascimbeni, V.
AU - Pace, E.
AU - Pagano, I.
AU - Pedani, M.
AU - Piotto, G.
AU - Pinamonti, M.
AU - Quintana, E. V.
AU - Rainer, M.
AU - Ricker, G. R.
AU - Seager, S.
AU - Twicken, J. D.
AU - Vanderspek, R.
AU - Winn, J. N.
N1 - Funding Information:
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 HighEnd Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. The research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, NASA’s Astrophysics Data System and 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 was also partly supported by the Department of Energy under awards DE-NA0003904 and DE-FOA0002633 (to S.B.J., principal investigator, and collaborator Li Zeng) with Harvard University and by the Sandia Z Fundamental Science Program. This research represents the authors’ views and not those of the Department of Energy. The work is based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundacion Galileo Galilei of the INAF (Istituto Nazionale di Astrofísica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. This work has also 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. L.M. acknowledges support from the “Fondi di Ricerca Scientifica d’Ateneo 2021” of the University of Rome “Tor Vergata”. J.L-B. acknowledges financial support received from “la Caixa” Foundation (ID 100010434) and from the European Union’s Horizon 2020 research and innovation programme under the Marie Slodowska-Curie grant agreement No 847648, with fellowship code LCF/BQ/PI20/11760023. This research has also been partly funded by the Spanish State Research Agency (AEI) Projects No. PID2019-107061GB-C61 and No. MDM-2017-0737 Unidad de Excelencia “Maria de Maeztu”- Centro de Astrobiologia (INTA-CSIC). We acknowledge financial contribution from the agreement ASI-INAF no. 2018-16-HH.0. D.D. acknowledges support from the TESS Guest Investigator Program grants 80NSSC21K0108 and 80NSSC22K0185. L.N. acknowledges the support of the ARIEL ASI-INAF agreement 2021-5-HH.0.
Publisher Copyright:
©
PY - 2022/11/1
Y1 - 2022/11/1
N2 - Context. Neptunes represent one of the main types of exoplanets and have chemical-physical characteristics halfway between rocky and gas giant planets. Therefore, their characterization is important for understanding and constraining both the formation mechanisms and the evolution patterns of planets. Aims. We investigate the exoplanet candidate TOI-1422 b, which was discovered by the TESS space telescope around the high proper-motion G2 V star TOI-1422 (V = 10.6 mag), 155 pc away, with the primary goal of confirming its planetary nature and characterising its properties. Methods. We monitored TOI-1422 with the HARPS-N spectrograph for 1.5 yr to precisely quantify its radial velocity (RV) variation. We analyse these RV measurements jointly with TESS photometry and check for blended companions through high-spatial resolution images using the AstraLux instrument. Results. We estimate that the parent star has a radius of R = 1.0190.013+0.014 Ra, and a mass of M = 1.0190.013+0.014 Ma. Our analysis confirms the planetary nature of TOI-1422 b and also suggests the presence of a Neptune-mass planet on a more distant orbit, the candidate TOI-1422 c, which is not detected in TESS light curves. The inner planet, TOI-1422 b, orbits on a period of Pb = 12.9972 ± 0.0006 days and has an equilibrium temperature of Teq,b = 867 ± 17 K. With a radius of Rb = 3.960.11+0.13 R, a mass of Mb = 9.02.0+2.3 M and, consequently, a density of ρb = 0.7950.235+0.290g cm3, it can be considered a warm Neptune-sized planet. Compared to other exoplanets of a similar mass range, TOI-1422 b is among the most inflated, and we expect this planet to have an extensive gaseous envelope that surrounds a core with a mass fraction around 10% 25% of the total mass of the planet. The outer non-Transiting planet candidate, TOI-1422 c, has an orbital period of Pc = 29.290.20+0.21 days, a minimum mass, Mcsin i, of 11.12.3+2.6 M, an equilibrium temperature of Teq,c = 661 ± 13 K and, therefore, if confirmed, could be considered as another warm Neptune.
AB - Context. Neptunes represent one of the main types of exoplanets and have chemical-physical characteristics halfway between rocky and gas giant planets. Therefore, their characterization is important for understanding and constraining both the formation mechanisms and the evolution patterns of planets. Aims. We investigate the exoplanet candidate TOI-1422 b, which was discovered by the TESS space telescope around the high proper-motion G2 V star TOI-1422 (V = 10.6 mag), 155 pc away, with the primary goal of confirming its planetary nature and characterising its properties. Methods. We monitored TOI-1422 with the HARPS-N spectrograph for 1.5 yr to precisely quantify its radial velocity (RV) variation. We analyse these RV measurements jointly with TESS photometry and check for blended companions through high-spatial resolution images using the AstraLux instrument. Results. We estimate that the parent star has a radius of R = 1.0190.013+0.014 Ra, and a mass of M = 1.0190.013+0.014 Ma. Our analysis confirms the planetary nature of TOI-1422 b and also suggests the presence of a Neptune-mass planet on a more distant orbit, the candidate TOI-1422 c, which is not detected in TESS light curves. The inner planet, TOI-1422 b, orbits on a period of Pb = 12.9972 ± 0.0006 days and has an equilibrium temperature of Teq,b = 867 ± 17 K. With a radius of Rb = 3.960.11+0.13 R, a mass of Mb = 9.02.0+2.3 M and, consequently, a density of ρb = 0.7950.235+0.290g cm3, it can be considered a warm Neptune-sized planet. Compared to other exoplanets of a similar mass range, TOI-1422 b is among the most inflated, and we expect this planet to have an extensive gaseous envelope that surrounds a core with a mass fraction around 10% 25% of the total mass of the planet. The outer non-Transiting planet candidate, TOI-1422 c, has an orbital period of Pc = 29.290.20+0.21 days, a minimum mass, Mcsin i, of 11.12.3+2.6 M, an equilibrium temperature of Teq,c = 661 ± 13 K and, therefore, if confirmed, could be considered as another warm Neptune.
KW - Methods: data analysis
KW - Planetary systems
KW - Stars: individual: TOI-1422
KW - Techniques: photometric
KW - Techniques: radial velocities
KW - Techniques: spectroscopic
UR - http://www.scopus.com/inward/record.url?scp=85145187556&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85145187556&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202244079
DO - 10.1051/0004-6361/202244079
M3 - Article
AN - SCOPUS:85145187556
SN - 0004-6361
VL - 667
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A8
ER -