J/A+A/705/A210 TOI-333b light-curve and radial velocities (Alves+, 2026)
TOI-333b: A Neptune-desert planet around a F7V star.
Alves D., Jenkins J.S., Vines J.I., Moyano M., Anderson D.R., Magliano C.,
Covone G., Covone G., Stassun K.G., Soubkiou A., Gillen E., Battley M.,
Hugues A., Armstrong D.J., Saha S., Hawthorn F., Wheatley P.J.,
Collins K.A., Schwarz R.P., Srdoc G., Apergis I., Zivave T., Lendl M.,
Tofflemire B.M., Doty J.P., Hedges C., Mireles I., Burleigh M.R.,
Kendall A., Harvey G.T., Goad M.R., Casewell S.L., Edkins T.
<Astron. Astrophys. 705, A210 (2026)>
=2026A&A...705A.210A 2026A&A...705A.210A (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Stars, F-type ;
Transient ; Photometry ; Optical ; Spectroscopy ;
Radial velocities
Keywords: techniques: photometric - techniques: radial velocities -
planets and satellites: detection -
planets and satellites: fundamental parameters -
planets and satellites: general - stars: general
Abstract:
Observations have shown that planets similar to Neptune are rarely
found orbiting Sun-like stars with periods up to ∼4 days, defining the
so-called Neptune desert region. Therefore, the detection of each
individual planet in this region holds a high value, providing
detailed insights into how such a population came to form and evolve.
Here we report the detection of TOI-333b, a Neptune desert planet
with a mass, radius, and bulk density of 20.1 ± 2.4 M⊕,
4.26 ± 0.11 R⊕, and 1.42 ± 0.21 g.cm-3, respectively.
The planet orbits a F7V star every 3.78 d, whose mass, radius and
effective temperature are of 1.2 ± 0.1 M☉,
1.10 ± 0.03 R☉, and 6241-62+73K, respectively.
TOI-333b is likely younger than 1 Gyr, which is supported by the
presence of the doublet Li line around 6707.856 Å and its
comparison to Li abundances in open clusters with well constrained
ages. The planet is expected to host only 8.5-8.3+10.9%
gas-to-core mass ratio for a H/He envelope. On the other hand,
irradiated ocean world models predict 20-10+11% H2O mass
fraction with a core fraction of 35-23+20%. Therefore, we expect
that TOI-333b internal composition may be dominated by a pure rocky
composition with almost no H/He envelope, or a rocky world with almost
equal mass fraction of water. Finally, TOI-333b is more massive and
larger than 77% and 82% of its Neptune desert counterparts,
respectively, while its host ranks among the hottest known for Neptune
Desert planets, making this system a unique laboratory to study the
evolution of such planets around hot stars.
Description:
In this study of TOI-333b planet, we provide observational photometric
light curve of TOI-333 for TESS, NGTS and SAAO instruments as presented
in lc.dat and observational spectroscopic of TOI-333 computed radial
velocities from HARPS and FEROS spectrograph as presented in rvs.dat.
Objects:
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RA (2000) DE Designation(s)
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23 33 25.77 -41 10 17.4 TOI-333 = 2MASS J23332579-4110174
23 33 25.77 -41 10 17.4 TOI-333.01 = TOI-333.01
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
lc.dat 49 32807 Observvational photometry light curve of
TOI-333 (table A1)
rvs.dat 60 44 Observational spectroscopic radial velocities
of TOI-333 (table A2)
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See also:
J/A+A/689/A250 : Kepler DR25 cat. transit and detec. prob.
(Castro-Gonzale+, 2024)
J/A+A/615/A90 : Kepler-419 radial velocities (Almenara+, 2018)
J/A+A/615/A76 : Spectroscopic parameters of stars (SPECIES). I.
(Soto+, 2018)
J/A+A/468/1115 : Thorium and argon lines in the visible (Lovis+, 2007)
J/MNRAS/513/2719 : Stellar parameters study with SED fit algo (Vines+, 2022)
J/MNRAS/486/5094 : NGTS-4b A sub-Neptune transiting in the desert
(West+, 2019)
J/MNRAS/421/2342 : 4 Kepler systems transit timing observations
(Steffen+, 2012)
J/ApJ/903/L7 : Planet parameters from IRAC measurements
(Crossfield+, 2020)
J/ApJ/888/L5 : Transits, occultation times and RVs of WASP-12b
(Yee+, 2020)
J/ApJ/784/45 : Kepler's multiple planet candidates. III. (Rowe+, 2014)
J/ApJ/770/69 : Kepler planet candidates radii (Petigura+, 2013)
J/ApJ/695/679 : Stellar rotation in M35 (Meibom+, 2009)
J/ApJ/687/1264 : Age estimation for solar-type dwarfs (Mamajek+, 2008)
J/ApJS/254/39 : Exoplanet candidates from TESS first 2yr obs
(Guerrero+, 2021)
J/AJ/163/175 : WASP-12 individual transit fit with TESS (Wong+, 2022)
J/AJ/161/70 : Radial velocities for WASP-107 with HIRES & CORALIE
(Piaulet+, 2021)
J/AJ/157/124 : DAVE. I. Benchmarking K2 vetting tools (Kostov+, 2019)
J/AJ/156/102 : The TESS Input Catalog and Candidate Target List
(Stassun+, 2018)
J/AJ/153/136 : Planets and their host stars with Gaia parallaxes
(Stassun+, 2017)
J/AJ/152/180 : Bolometric fluxes of eclipsing binaries in Tycho-2
(Stassun+, 2016)
J/other/A+ARV/18.67 : Accurate masses and radii of normal stars (Torres+, 2010)
VII/233 : 2MASS All-Sky Extended Source Catalog (XSC)
(IPAC-UMass, 2003-2006)
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
Byte-by-byte Description of file: lc.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 F18.10 d BJD Barycentric Julian Date at TDB of measurement
(BJDTDB)
20- 31 F12.10 mag LCmag TESS/NGTS/SAAO relative optical magnitude in
respectively 600-1000nm TESS band, Sloan i' SAAO
band and 520-890nm NGTS band ranges
33- 44 F12.10 mag e_LCmag Uncertainty in LCmag
46- 49 A4 --- Inst Instrument of measurement (1)
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Note (1): Observational instrument names are as follows:
TESS = Transiting Exoplanet Survey Satellite, 30934 occurences in
our sample
NGTS = Next Generation Transit Survey, 728 occurences in our sample
SAAO = South Africa Astronomical Observatory near Sutherland, 1145
occurences in our sample
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Byte-by-byte Description of file: rvs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 F17.9 d BJD Barycentric Julian Date at TDB of measurement
(BJDTDB)
19- 36 F18.14 m/s RV HARPS/FEROS modelled radial velocity (RV)
38- 54 F17.14 m/s e_RV Uncertainty of RV
56- 60 A5 --- Inst [HARPS FEROS] Spectroscopic instrument (1)
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Note (1): Spectroscopic instrument names are as follows:
HARPS = HARPS spectrograph, 37 occurences in our sample
FEROS = FEROS spectrograph, 7 occurences in our sample
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Acknowledgements:
Douglas R. Alves, douglasalvesastro12(at)gmail.com
(End) Douglas R. Alves [Univ. de Chile], Luc Trabelsi [CDS] 25-Nov-2025