| Issue |
A&A
Volume 636, April 2020
|
|
|---|---|---|
| Article Number | A98 | |
| Number of page(s) | 17 | |
| Section | Planets and planetary systems | |
| DOI | https://doi.org/10.1051/0004-6361/201936279 | |
| Published online | 24 April 2020 | |
TraMoS
V. Updated ephemeris and multi-epoch monitoring of the hot Jupiters WASP-18Ab, WASP-19b, and WASP-77Ab★
1
Departamento de Astronomía, Universidad de Chile,
Camino El Observatorio 1515,
Las Condes,
Santiago,
Chile
e-mail: pia.cortes@ug.uchile.cl
2
Department of Astronomy, Yale University,
New Haven,
CT
06511, USA
3
Chungnam National University, Department of Astronomy and Space Science,
34134
Daejeon,
Republic of Korea
4
Aix-Marseille Univ., CNRS, CNES, LAM,
Marseille,
France
Received:
9
July
2019
Accepted:
29
January
2020
We present 22 new transit observations of the exoplanets WASP-18Ab, WASP-19b, and WASP-77Ab, from the Transit Monitoring in the South project. We simultaneously model our newly collected transit light curves with archival photometry and radial velocity data to obtain refined physical and orbital parameters. We include TESS light curves of the three exoplanets to perform an extended analysis of the variations in their transit mid-time (TTV) and to refine their planetary orbital ephemeris. We did not find significant TTVRMS variations larger than 47, 65, and 86 s for WASP-18Ab, WASP-19b, and WASP-77Ab, respectively. Dynamical simulations were carried out to constrain the masses of a possible perturber. The observed mean square (RMS) could be produced by a perturber body with an upper limit mass of 9, 2.5, 11 and 4 M⊕ in 1:2, 1:3, 2:1, and 3:1 resonances in the WASP-18Ab system. In the case of WASP-19b, companions with masses up to 0.26, 0.65, 1, and 2.8 M⊕, in 1:2, 2:1, 3:1, and 5:3 resonances respectively, produce the RMS. For the WASP-77Ab system, this RMS could be produced by a planet with mass in the range of 1.5−9 M⊕ in 1:2, 1:3, 2:1, 2:3, 3:1, 3:5, or 5:3 resonances. Comparing our results with RV variations, we discard massive companions with 350 M⊕ in 17:5 resonance for WASP-18Ab, 95 M⊕ in 4:1 resonance for WASP-19b, and 105 M⊕ in 5:2 resonance for WASP-77Ab. Finally, using a Lomb-Scargle period search we find no evidence of a periodic trend on our TTV data for the three exoplanets.
Key words: planets and satellites: dynamical evolution and stability / planets and satellites: individual: WASP-77Ab / planets and satellites: individual: WASP-18b / planets and satellites: individual: WASP-19b / planets and satellites: general
Photometry tables (full Table 2) are available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/636/A98
© ESO 2020
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