J/A+A/647/A180 hot massive Jupiter NGTS-13b photometry (Grieves+, 2021)
NGTS-13b: A hot 4.8 Jupiter-mass planet transiting a subgiant star.
Grieves N., Nielsen L.D., Vines J.I., Bryant E.M., Gill S., Bouchy F.,
Lendl M., Bayliss D., Eigmueller P., Segransan D., Acton J.S.,
Anderson D.R., Burleigh M.R., Casewell S.L., Chaushev A., Cooke B.F.,
Gillen E., Goad M.R., Guenther M.N., Henderson B.A., Hogan A., Jenkins J.S.,
Alves D.R., Jordan A., McCormac J., Moyano M., Queloz D., Raynard L.,
Seidel J.V., Smith A.M.S., Tilbrook R.H., Udry S., West R.G., Wheatley P.J.
<Astron. Astrophys. 647, A180 (2021)>
=2021A&A...647A.180G 2021A&A...647A.180G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Photometry ; Optical
Keywords: planets and satellites: detection -
planets and satellites: individual: NGTS-13b -
techniques: photometric - techniques: radial velocities
Abstract:
We report the discovery of the massive hot Jupiter NGTS-13b by the
Next Generation Transit Survey (NGTS). The V=12.7 host star is likely
in the subgiant evolutionary phase with logg*=4.04±0.05,
Teff=5819±73K, M*=1.30+0.11-0.18M☉, and
R*=1.79±0.06R☉. NGTS detected a transiting planet with a
period of P=4.12 days around the star, which was later validated with
the Transiting Exoplanet Survey Satellite (TESS; TIC 454069765). We
confirm the planet using radial velocities from the CORALIE
spectrograph. Using NGTS and TESS full-frame image photometry combined
with CORALIE radial velocities we determine NGTS-13b to have a radius
of RP=1.142±0.046RJup, mass of MP=4.84±0.44MJup and
eccentricity e=0.086±0.034. Some previous studies suggest that
∼4MJup may be a border between two separate formation scenarios
(e.g., core accretion and disk instability) and that massive giant
planets share similar formation mechanisms as lower-mass brown dwarfs.
NGTS-13b is just above 4MJup making it an important addition to the
statistical sample needed to understand the differences between
various classes of substellar companions. The high metallicity,
[Fe/H]=0.25±0.17, of NGTS-13 does not support previous suggestions
that massive giants are found preferentially around lower metallicity
host stars, but NGTS-13b does support findings that more massive and
evolved hosts may have a higher occurrence of close-in massive planets
than lower-mass unevolved stars.
Description:
We tabulate the TESS and NGTS photometry of NGTS-13 (2MASS
J11445767-38082292). The photometry is in relative flux and reduced as
in the paper.
Objects:
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RA (2000) DE Designation(s)
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11 44 57.66 -38 08 22.98 NGTS-13 = 2MASS J11445767-3808229 = TIC 454069765
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
ngts.dat 38 6030 Reduced NGTS photometry of NGTS-13
tess.dat 38 1080 Reduced TESS photometry of NGTS-13
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Byte-by-byte Description of file: ngts.dat tess.dat
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Bytes Format Units Label Explanations
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1- 16 F16.8 d BJD Barycentric Julian Date (BJD) in the
Barycentric Dynamical Time (TDB) standard
18- 27 F10.8 --- Flux Relative flux
29- 38 F10.8 --- e_Flux Relative flux error
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Acknowledgements:
We thank the Swiss National Science Foundation (SNSF) and the Geneva
University for their continuous support to our planet search programs.
This work was carried out in the frame of the National Centre for
Competence in Research $PlanetS$ supported by the Swiss National
Science Foundation (SNSF). This work uses data collected under the
NGTS project at the ESO La Silla Paranal Observatory. The NGTS
facility is operated by the consortium institutes with support from
the UK Science and Technology Facilities Council (STFC) under projects
ST/M001962/1 and ST/S002642/1. This work includes data collected by
the TESS mission. Funding for the TESS mission is provided by the NASA
Explorer Program.
From Noaln Grieves, nolan.grieves(at)unige.ch
(End) Patricia Vannier [CDS] 25-Jan-2021