J/A+A/680/A84 TOI-1736 and TOI-2141 SOPHIE observations (Martioli+, 2023)
TOI-1736 and TOI-2141: Two systems including sub-Neptunes around solar analogs
revealed by TESS and SOPHIE.
Martioli E., Hebrard G., de Almeida L., Heidari N., Lorenzo-Oliveira D.,
Kiefer F., Almenara J.M., Bieryla A., Boisse I., Bonfils X., Briceno C.,
Collins K.A., Cortes-Zuleta P., Dalal S., Deleuil M., Delfosse X.,
Demangeon O., Eastman J.D., Forveille T., Furlan E., Howell S.B.,
Hoyer S., Jenkins J.M., Latham D.W., Law N., Mann A.W., Moutou C.,
Santos N.C., Sousa S.G., Stassun K.G., Stockdale C., Torres G.,
Twicken J.D., Winn J.N., Ziegler C.
<Astron. Astrophys. 680, A84 (2023)>
=2023A&A...680A..84M 2023A&A...680A..84M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Stars, G-type ;
Photometry ; Optical ; Radial velocities
Keywords: planetary systems - stars: individual: TOI-1736 -
stars: individual: TOI-2141 - stars: solar-type -
techniques: photometric - techniques: radial velocity
Abstract:
Planetary systems around solar analogs inform us about how planets
form and evolve in solar system-like environments. We report the
detection and characterization of two planetary systems around the
solar analogs TOI-1736 and TOI-2141 using TESS photometry data and
spectroscopic data obtained with the SOPHIE instrument on the 1.93 m
telescope at the Observatoire de Haute-Provence (OHP). We performed a
detailed spectroscopic analysis of these systems to obtain the precise
radial velocities and physical properties of their host stars.
TOI-1736 and TOI-2141 each host a transiting sub-Neptune with radii of
2.44±0.18 and 3.05±0.23R⊕, orbital periods of 7.073088(7)d
and 18.26157(6)d, and masses of 12.8±1.8M⊕ and
24±4M⊕, respectively. TOI-1736 shows long-term radial
velocity variations that are consistent with a two-planet solution
plus a linear trend of -0.177m/s/d. We measured an RV semi-amplitude
of 201.1±0.7m/s for the outer companion, TOI-1736 c, implying a
projected mass of msin(i)=8.09±0.20MJup. From the GAIA DR3
astrometric excess noise, we constrained the mass of TOI-1736 c at
8.7±1.5M{Jup}. This planet is in an orbit of 570.2±0.6d with an
eccentricity of 0.362±0.003 and a semi-major axis of
1.381±0.017au, where it receives a flux of 0.71±0.08 times the
bolometric flux incident on Earth, making it an interesting case of a
supergiant planet that has settled into an eccentric orbit in the
habitable zone of a solar analog. Our analysis of the mass-radius
relation for the transiting sub-Neptunes shows that both TOI-1736 b
and TOI-2141 b likely have an Earth-like dense rocky core and a
water-rich envelope.
Description:
Quantities derived from high-resolution spectroscopic observations of
TOI-1736 and TOI-2141. These observations were conducted using the
SOPHIE instrument at OHP and include measured radial velocities and
activity indexes.
Objects:
-----------------------------------------------------
RA (2000) DE Designation(s)
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02 53 44.40 +69 06 05.0 TOI-1736 = TIC 408618999
20 17 46.69 +77 09 58.2 TOI-2161 = TIC 366563452
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
toi1736.dat 102 152 SOPHIE data for TOI-1736 (table A1)
toi2141.dat 102 90 SOPHIE data for TOI-2141 (table A2)
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Byte-by-byte Description of file: toi1736.dat toi2141.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- ObsID Observation index
5- 17 F13.5 d BJD Barycentric Julian date
19- 26 F8.4 km/s RV Radial velocity
28- 33 F6.4 km/s e_RV 1-sigma uncertainty in the radial velocity
35- 42 F8.4 km/s BERV Barycentric Earth radial velocity
44- 47 I4 s ExpTime Exposure time
49- 51 I3 --- S/N Signal-to-noise ratio measured at 649nm
53- 57 F5.3 km/s FWHM Full width at half maximum of CCF
59- 63 F5.3 km/s e_FWHM 1-sigma uncertainty in the FWHM of CCF
65- 70 F6.3 km/s Bis Bisector span
72- 76 F5.3 km/s e_Bis 1-sigma uncertainty in the bisector span
78- 82 F5.3 --- SMW S-index calibrated to the Mount Wilson
Observatory system
84- 88 F5.3 --- e_SMW 1-sigma uncertainty in the SMW
90- 95 F6.4 --- Halpha H-alpha index
97-102 F6.4 --- e_Halpha 1-sigma uncertainty in the H-alpha index
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History:
From Eder Martioli, martioli(at)iap.fr
Acknowledgements:
E.M. acknowledges funding from the Fundacao de Amparo a Pesquisa do
Estado de Minas Gerais (FAPEMIG) under project number APQ-02493-22 and
a research productivity grant (PQ) number 309829/2022-4 awarded by the
National Council for Scientific and Technological Development (CNPq),
Brazil. We thank the staff at the Observatoire de Haute-Provence
(CNRS) for their support. This work was supported by the Programme
National de Planetologie (PNP) of CNRS/INSU and CNES. This paper
includes data collected with the TESS mission, obtained from the MAST
data archive at the Space Telescope Science Institute (STScI). 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. This publication makes use of
The Data & Analysis Center for Exoplanets (DACE), which is a facility
based at the University of Geneva (CH) dedicated to extrasolar planet
data visualization, exchange, and analysis. DACE is a platform of the
Swiss National Centre of Competence in Research (NCCR) PlanetS,
federating Swiss expertise in Exoplanet research. The DACE platform is
available at https://dace.unige.ch. We acknowledge funding from the
French ANR under contract number ANR18CE310019 (SPlaSH). X.D. and T.F.
acknowledge support from the French National Research Agency within
the framework of the Investissement d'Avenir program
(ANR-15-IDEX-02), through funding for the "Origin of Life" project of
Grenoble-Alpes University. This work was supported by FCT - Fundacao
para a Ciencia e a Tecnologia through national funds and by FEDER
through COMPETE2020 - Programa Operacional Competitividade e
Internacionalizacao, under these grants: UID/FIS/04434/2019,
UIDB/04434/2020, UIDP/04434/2020, PTDC/FIS-AST/32113/2017 &
POCI-01-0145-FEDER- 032113, PTDC/FIS-AST/28953/2017 &
POCI-01-0145-FEDER-028953, PTDC/FIS-AST/28987/2017 &
POCI-01-0145-FEDER-028987. NCS further acknowledges funding from the
European Union (ERC, FIERCE, 101052347). However, the views and
opinions expressed are those of the author(s) only and do not
necessarily reflect those of the European Union or the European
Research Council. Neither the European Union nor the granting
authority can be held responsible for them. This work utilizes
observations from the LCOGT network. A portion of the LCOGT telescope
time was granted by NOIRLab through the Mid-Scale Innovations Program
(MSIP), funded by NSF. KAC acknowledges support from the TESS mission
via subaward s3449 from MIT. S.D. is funded by the UK Science and
Technology Facilities Council (grant number ST/V004735/1). S.G.S
acknowledges support from FCT through the contract
nr.CEECIND/00826/2018 and POPH/FSE (EC).
(End) Patricia Vannier [CDS] 02-Oct-2023