J/A+A/668/A29 TOI-5542 SAAO and EulerCam photometry (Grieves+, 2022)
An old warm Jupiter orbiting the metal-poor G-dwarf TOI-5542.
Grieves N., Bouchy F., Ulmer-Moll S., Gill S., Anderson D.R., Psaridi A.,
Lendl M., Stassun K.G., Jenkins J.M., Burleigh M.R., Acton J.S., Boyd P.T.,
Casewell S.L., Eigmueller P., Goad M.R., Goeke R.F., Guenther M.N.,
Hawthorn F., Henderson B.A., Henze C.E., Jordan A., Kendall A., Mishra L.,
Moldovan D., Moyano M., Osborn H., Revol A., Sefako R.R., Tilbrook R.H.,
Udry S., Unger N., Vines J.I., West R.G., Worters H.L.
<Astron. Astrophys. 668, A29 (2022)>
=2022A&A...668A..29G 2022A&A...668A..29G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Photometry ; Optical
Keywords: planets and satellites: detection -
dynamical evolution and stability -
planets and satellites: formation -
planets and satellites: fundamental parameters -
planets and satellites: gaseous planets
Abstract:
We report the discovery of a 1.32+0.10-0.10MJup planet orbiting
on a 75.12 day period around the G3V 10.8+2.1-3.6Gyr old star
TOI-5542 (TIC 466206508; TYC 9086-1210-1). The planet was first
detected by the Transiting Exoplanet Survey Satellite (TESS) as a
single transit event in TESS Sector 13. A second transit was observed
376 days later in TESS Sector 27. The planetary nature of the object
has been confirmed by ground-based spectroscopic and radial velocity
observations from the CORALIE and HARPS spectrographs. A third transit
event was detected by the ground-based facilities NGTS, EulerCam, and
SAAO. We find the planet has a radius of 1.009+0.036-0.035RJup
and an insolation of 9.6+0.9-0.8S☉, along with a circular
orbit that most likely formed via disk migration or in situ formation,
rather than high-eccentricity migration mechanisms. Our analysis of
the HARPS spectra yields a host star metallicity of
[Fe/H]=-0.21±0.08, which does not follow the traditional trend of
high host star metallicity for giant planets and does not bolster
studies suggesting a difference among low- and high-mass giant planet
host star metallicities. Additionally, when analyzing a sample of 216
well-characterized giant planets, we find that both high masses
(4MJup<Mp<13MJup) and low masses (0.5MJup<Mp<4MJup), as
well as both both warm (P>10-days) and hot (P<10-days) giant planets
are preferentially located around metal-rich stars (mean [Fe/H]>0.1).
TOI-5542b is one of the oldest known warm Jupiters and it is cool
enough to be unaffected by inflation due to stellar incident flux,
making it a valuable contribution in the context of planetary
composition and formation studies.
Description:
We tabulate the SAAO and EulerCam photometry of TOI-5542. The
photometry is in relative flux and reduced as described in the paper.
Objects:
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RA (2000) DE Designation(s)
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20 11 11.63 -61 08 07.6 TOI-5542 = TIC 466206508
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
saao.dat 85 970 SAAO photometry
ecam.dat 86 77 EulerCam photometry
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Byte-by-byte Description of file: ecam.dat saao.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
40- 45 F6.2 pix xshift Target x position shift
47- 51 F5.2 pix yshift Target y position shift
53- 62 F10.8 --- Airmass Airmass
63- 72 F10.7 arcsec FWHM Target FWHM
74- 79 F6.3 --- Sky Sky background
81- 86 F6.2 s ExpTime Exposure time
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History:
From Nolan Grieves, nolangrieves(at)gmail.com
Acknowledgements:
We thank the Swiss National Science Foundation (SNSF) and the Geneva
University for their
continuous support to our planet low-mass companion search programs.
This work was carried out in the frame of the Swiss National Centre
for Competence in Research (NCCR) PlanetS supported by the Swiss
National Science Foundation (SNSF). 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 NCCR
PlanetS and is avail- able at https://dace.unige.ch. This paper
includes data collected by the TESS mission. Funding for the TESS
mission is provided by the NASA Explorer Program. 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
paper uses observations made at the South African Astronomical
Observatory (SAAO).
The Starlink software (Currie et al., 2014, ASP Conf. Ser., 485, 391)
is currently supported by the East Asian Observatory. MNG acknowledges
support from the European Space Agency (ESA) as an ESA Research
Fellow. AJ acknowledges support from ANID - Millennium Science
Initiative - ICN12_009 and from FONDE-CYT project 1210718. M.L.
acknowledges support of the Swiss National Science Foundation under
grant number PCEFP2_194576.NG thanks Tara Grieves for her support,
passion, and kindness over the years.
(End) Patricia Vannier [CDS] 29-Sep-2022