J/AcA/70/181 Search for Planets in Hot Jupiter Systems (Maciejewski+, 2020)
Search for Planets in Hot Jupiter Systems with Multi-Sector TESS Photometry.
I. No Companions in Planetary Systems KELT-18, KELT-23, KELT-24, Qatar-8,
WASP-62, WASP-100, WASP-119, and WASP-126.
Maciejewski G.
<Acta Astron. 70, 181-202 (2020)>
=2020AcA....70..181M 2020AcA....70..181M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Photometry
Keywords: stars: individual: KELT-18, KELT-23, KELT-24, Qatar-8, WASP-62,
WASP-100, WASP-119, WASP-126 -
planets and satellites: individual: KELT-18 b, KELT-23 b, KELT-24 b,
Qatar-8 b, WASP-62 b, WASP-100 b, WASP-119 b, WASP-126 b
Abstract:
Origins of giant planets on tight orbits, so called hot Jupiters, are
a long-lasting question in the planetary formation and evolution
theory. The answer seems to be hidden in architectures of those
systems that remain only partially understood. Using multi-sector
time-series photometry from the Transiting Exoplanet Survey Satellite,
we searched for additional planets in the KELT-18, KELT-23, KELT-24,
Qatar-8, WASP-62, WASP-100, WASP-119, and WASP-126 planetary systems
using both the transit technique and transit timing method. Our
homogeneous analysis has eliminated the presence of transiting
companions down to the terrestrial-size regime in the KELT-23 and
WASP-62 systems, and down to mini-Neptunes or Neptunes in the
remaining ones.
Transit timing analysis has revealed no sign of either long-term
trends or periodic perturbations for all the studied hot Jupiters,
including the WASP-126 b for which deviations from a Keplerian model
were claimed in the literature. The loneliness of the planets of the
sample speaks in favor of the high-eccentricity migration mechanism
that probably brought them to their tight orbits observed nowadays. As
a by-product of our study, the transit light curve parameters were
redetermined with a substantial improvement of the precision for six
systems. For KELT-24 b, a joint analysis allowed us to place a tighter
constraint on its orbital eccentricity.
Description:
This is machine-readable Table 3 of the source paper, providing
homogeneously determined transit mid-points for the examined planets:
KELT-18 b, KELT-23 b, KELT-24 b, Qatar-8 b, WASP-62b , WASP-100 b,
WASP-119 b, and WASP-126 b.
Objects:
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RA (2000) DE Designation(s)
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14 26 05.76 +59 26 39.3 KELT-18 = BD+60 1538
15 28 35.19 +66 21 31.5 KELT-23 = BD+66 911
10 47 38.35 +71 39 21.2 KELT-24 = HD 93148
10 29 39.11 +70 31 37.6 Qatar-8 = TYC 4387-1050-1
05 48 33.59 -63 59 18.4 WASP-62 = CPD-64 484
04 35 50.33 -64 01 37.3 WASP-100 = CPD-64 356
03 43 44.02 -65 11 37.9 WASP-119 = 2MASS 03434402-6511378
04 13 29.75 -69 13 36.6 WASP-126 = TYC 9153-833-1
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tt.dat 69 480 Transit mid-points
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See also:
J/AJ/153/263 : Transiting planetary system KELT-18 (McLeod+, 2017)
J/AJ/158/78 : Transiting planetary system KELT-23 (Johns+, 2019)
J/AJ/158/197 : Transiting planetary system KELT-24 (Rodriguez+, 2019)
J/AJ/157/224 : Transiting planetary system Qatar-8 (Alsubai+, 2019)
J/MNRAS/426/739 : Transiting planetary system WASP-62 (Hellier+, 2012)
J/MNRAS/440/1982 : Transiting planetary system WASP-100 (Hellier+, 2014)
J/A+A/591/55 : Planetary systems WASP-119 and WASP-126 (Maxted+, 2016)
J/A+A/631/A76 : MASCARA-3b radial and light curves (Hjorth+, 2019)
Byte-by-byte Description of file: tt.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Planet Planet name
13- 15 I3 --- Ep Epoch
17- 27 F11.6 d BJD Mid-transit time (1)
29- 36 F8.6 d e_BJD Positive error for BJD
38- 45 F8.6 d E_BJD Negative error for BJD
47- 69 A23 --- Datasrc Data source (2)
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Note (1): Barycentric Julian date in Barycentric Dynamical Time (BJD_TDB)
Note (2): Data source as follows:
Alsubai et al. (2019) = Alsubai et al., 2019, Cat. J/AJ/157/224
Hellier et al. (2012) = Hellier et al., 2012, Cat. J/MNRAS/426/739
Hellier et al. (2014) = Hellier et al., 2014, Cat. J/MNRAS/440/1982
Hjorth et al. (2019) = Hjorth et al., 2019, Cat. J/A+A/631/A76
Johns et al. (2019) = Johns et al., 2019, Cat. J/AJ/158/78
Maxted et al. (2016) = Maxted et al., 2016, Cat. J/A+A/591/55
McLeod et al. (2017) = McLeod et al., 2017, Cat. J/AJ/153/263
Rodriguez et al. (2019) = Rodriguez et al., 2019, J/AJ/158/197
This paper = This paper
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Acknowledgements:
Gracjan Maciejewski, gmac(at)umk.pl
Institute of Astronomy, Nicolaus Copernicus University, Poland
(End) Gracjan Maciejewski [Copernicus Univ.], Patricia Vannier [CDS] 25-Mar-2021