J/A+A/636/A98 WASP-18A, WASP-19, WASP-77A photometry (Cortes-Zuleta+, 2020)
TraMoS V. Updated ephemeris and multi-epoch monitoring of the hot Jupiters
WASP-18Ab, WASP-19b, and WASP-77Ab .
Cortes-Zuleta P., Rojo P., Wang S., Hinse T.C., Hoyer S., Sanhueza B.,
Correa-Amaro P., Albornoz J.
<Astron. Astrophys. 636, A98 (2020)>
=2020A&A...636A..98C 2020A&A...636A..98C (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Photometry
Keywords: 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
Abstract:
We present 22 new transit observations of the exoplanets WASP-18Ab,
WASP-19b, and WASP-77Ab, from the Transit Monitoring in the South
(TraMoS) 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 seconds 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 4M⊕ 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 2.8M⊕, 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
1.5-9M⊕ 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 350M⊕ in 17:5 resonance for WASP-18Ab,
95M⊕ in 4:1 resonance for WASP-19b, and 105M⊕ 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.
Description:
This file contains the full information from Table 2 of the article.
It includes all the photometry of WASP-18A, WASP-19, and WASP-77A from
the TraMoS project considered in the article. The technical details of
these observations are listed in Table 1 of the article.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 38 3 List of studied stars
table2.dat 39 8075 Photometry light curves from the TraMoS project
of WASP-18A, WASP-19, and WASP-77A
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See also:
J/ApJ/707/167 : Transiting planetary system WASP-18 (Southworth+, 2009)
J/MNRAS/436/2 : Transits of WASP-19b (Mancini+, 2013)
J/MNRAS/428/3671 : Transiting planet WASP-19b (Tregloan-Reed+, 2013)
Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Target Name of the star
11- 12 I2 h RAh Simbad right ascension (J2000)
14- 15 I2 min RAm Simbad right ascension (J2000)
17- 21 F5.2 s RAs Simbad right ascension (J2000)
23 A1 --- DE- Simbad declination sign (J2000)
24- 25 I2 deg DEd Simbad declination (J2000)
27- 28 I2 arcmin DEm Simbad declination (J2000)
30- 33 F4.1 arcsec DEs Simbad declination (J2000)
35- 38 I4 --- Nobs Number of observations in table2.dat
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Target Name of the star
10- 23 F14.6 d BJD Barycentric Julian date in the TDB standard
25- 31 F7.5 --- Flux Relative flux
33- 39 F7.5 --- e_Flux Error of the relative flux
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Acknowledgements:
Pia Cortes-Zuleta, pia.cortes(at)lam.fr
References:
Hoyer et al., Paper I 2012ApJ...748...22H 2012ApJ...748...22H
Hoyer et al., Paper III 2013MNRAS.434...46H 2013MNRAS.434...46H
Hoyer et al., Paper IV 2016MNRAS.455.1334H 2016MNRAS.455.1334H
(End) Pia Cortes-Zuleta [LAM, France], Patricia Vannier [CDS] 16-Apr-2020