J/A+A/689/A53 The TROY project III. (Balsalobre-Ruza+, 2024)
The TROY project. III. Exploring co-orbitals around low-mass stars.
Balsalobre-Ruza O., Lillo-Box J., Barrado D., Correia A., Faria J.P.,
Figueira P., Leleu A., Robutel P., Santos N., Herrero-Cisneros E.
<Astron. Astrophys. 689, A53 (2024)>
=2024A&A...689A..53B 2024A&A...689A..53B (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Radial velocities ;
Optical
Keywords: techniques: photometric - techniques: radial velocities -
minor planets, asteroids: general -
planets and satellites: detection - stars: low-mass
Abstract:
Co-orbital objects, also known as trojans, are frequently found in
simulations of planetary system formation. In these configurations, a
planet shares its orbit with other massive bodies. It is still unclear
why there have not been any co-orbitals discovered thus far in
exoplanetary systems (exotrojans) or even pairs of planets found in
such a 1:1 mean motion resonance. Reconciling observations and theory
is an open subject in the field. The main objective of the TROY
project is to conduct an exhaustive search for exotrojans using
diverse observational techniques. In this work, we analyze the radial
velocity time series informed by transits, focusing the search around
low-mass stars. We employed the alpha-test method on confirmed planets
searching for shifts between spectral and photometric mid-transit
times. This technique is sensitive to mass imbalances within the
planetary orbit, allowing us to identify non-negligible co-orbital
masses. Among the 95 transiting planets examined, we find one robust
exotrojan candidate with a significant 3-sigma detection.
Additionally, 25 exoplanets show compatibility with the presence of
exotrojan companions at a 1-sigma level, requiring further
observations to better constrain their presence. For two of those weak
candidates, we find dimmings in their light curves within the
predicted Lagrangian region. We established upper limits on the
co-orbital masses for either the candidates and null detections. Our
analysis reveals that current high-resolution spectrographs
effectively rule out co-orbitals more massive than Saturn around
low-mass stars. This work points out to dozens of targets that have
the potential to better constraint their exotrojan upper mass limit
with dedicated radial velocity observations. We also explored the
potential of observing the secondary eclipses of the confirmed
exoplanets in our sample to enhance the exotrojan search, ultimately
leading to a more accurate estimation of the occurrence rate of
exotrojans.
Description:
Archival radial velocity datasets per system used in the analysis of
the paper.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 45 84 List of studied stars
tableb2.dat 96 5175 Archival radial velocities
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See also:
J/A+A/609/A96 : TROY project. I. (Lillo-Box+, 2018)
Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- System Host star name
19- 20 I2 h RAh Right ascension (J2000)
22- 23 I2 min RAm Right ascension (J2000)
25- 31 F7.4 s RAs Right ascension (J2000)
33 A1 --- DE- Declination sign (J2000)
34- 35 I2 deg DEd Declination (J2000)
37- 38 I2 arcmin DEm Declination (J2000)
40- 45 F6.3 arcsec DEs Declination (J2000)
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Byte-by-byte Description of file: tableb2.dat
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Bytes Format Units Label Explanations
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1- 18 F18.10 d JD Julian date (format as in the original paper)
20- 42 F23.16 m/s RV Radial velocity or relative velocity
44- 63 F20.16 m/s e_RV Uncertainty associated to the radial velocity
65- 82 A18 --- Inst Spectrograph identificator
84- 96 A13 --- System Host star name
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History:
From Olga Balsalobre-Ruza, obalsalobre(at)cab.inta-csic.es
Acknowledgements:
We thank to all the authors who have helped us to access their data or
who have provided relevant information on the targets: J.M. Almenara,
C. Cadieux, D. Dragomir, X. Dumusque, E. Gonzalez-Alvarez, R. Luque,
and M. Mallorquin. This research has made use of 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 Project has been funded
by grant No.PID2019-107061GB-C61 by the Spanish Ministry of Science
and Innovation/State Agency of Research
MCIN/AEI/10.13039/501100011033. O. B.-R. is supported by INTA grant
PRE-MDM-07. J. L.-B. was partly funded by grants LCF/BQ/PI20/11760023
(La Caixa), Ramon y Cajal fellowship with code RYC2021-031640-I, and
CNS2023-144309. P. F. acknowledges the financial support of the SNSF,
the work has been carried out within the framework of the National
Centre of Competence in Research PlanetS supported by the Swiss
National Science Foundation under grant 51NF40_205606. AL acknowledges
support from the Swiss NCCR PlanetS and the Swiss National Science
Foundation. This work has been carried out within the framework of the
NCCR PlanetS supported by the Swiss National Science Foundation under
grants 51NF40_182901 and 51NF40_205606. AL acknowledges support of the
Swiss National Science Foundation under grant number TMSGI2_211697.
Co-funded by the European Union (ERC, FIERCE, 101052347). Views and
opinions expressed are however 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 was supported by
FCT - Fundacao para a Ciencia e a Tecnologia through national funds
and by FEDER through COMPETE2020 - Programa Operacional
Competitividade e Internacionalizacao by these grants:
UIDB/04434/2020; UIDP/04434/2020. E. H.-C. aknowledges support from
grant PRE2020-094770 under project PID2019-109522GB-C51 funded by the
Spanish Ministry of Science and Innovation / State Agency of Research,
MCIN/AEI/10.13039/501100011033, and by 'ERDF, A way of making
Europe'.
References:
Lillo-Box et al., Paper I 2018A&A...609A..96L 2018A&A...609A..96L, Cat. J/A+A/609/A96
Lillo-Box et al., Paper II 2018A&A...618A..42L 2018A&A...618A..42L
(End) Patricia Vannier [CDS] 02-Jul-2024