Measurements of Transit Timing Variations for WASP-5b

Fukui, A.; Narita, Norio; Tristram, P. J.; Sumi, T.; Abe, F.; Itow, Y.; Sullivan, D. J.; Bond, I. A.; Hirano, Teruyuki; Tamura, Motohide; Bennett, D. P.; Furusawa, K.; Hayashi, F.; Hearnshaw, John; Hosaka, S.; Kamiya, K.; Kobara, S.; Korpela, A.; Kilmartin, P. M.; Lin, Wei; Ling, C. H.; Makita, S.; Masuda, K.; Matsubara, Y.; Miyake, N.; Muraki, Y.; Nagaya, M.; Nishimoto, K.; Ohnishi, Kouhei; Omori, K.; Perrott, Y. C.; Rattenbury, N. J.; Saito, Toshiharu; Skuljan, L.; Suzuki, D.; Sweatman, W. L.; Wada, K.

doi:10.1093/pasj/63.1.287

Cited by 87 publications

(61 citation statements)

References 59 publications

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“…The images were reduced by the BANZAI pipeline (McCully et al 2018), and aperture photometry was performed with a custom code (Fukui et al 2011). Photometry was also performed on five nearby and isolated stars, to allow for correction of the effects due to differential extinction by the Earth's atmosphere.…”

Section: Simultaneous Photometrymentioning

confidence: 99%

Evidence for Spin–Orbit Alignment in the TRAPPIST-1 System

Hirano

Gaidos

Winn

et al. 2020

ApJL

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In an effort to measure the Rossiter-McLaughlin effect for the TRAPPIST-1 system, we performed high-resolution spectroscopy during transits of planets e, f, and b. The spectra were obtained with the InfraRed Doppler spectrograph on the Subaru 8.2-m telescope, and were supplemented with simultaneous photometry obtained with a 1-m telescope of the Las Cumbres Observatory Global Telescope. By analyzing the anomalous radial velocities, we found the projected stellar obliquity to be λ = 1 ± 28 degrees under the assumption that the three planets have coplanar orbits, although we caution that the radial-velocity data show correlated noise of unknown origin. We also sought evidence for the expected deformations of the stellar absorption lines, and thereby detected the "Doppler shadow" of planet b with a false alarm probability of 1.7 %. The joint analysis of the observed residual cross-correlation map including the three transits gave λ = 19 +13 −15 degrees. These results indicate that the the TRAPPIST-1 star is not strongly misaligned with the common orbital plane of the planets, although further observations are encouraged to verify this conclusion.

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Section: Simultaneous Photometrymentioning

confidence: 99%

Evidence for Spin–Orbit Alignment in the TRAPPIST-1 System

Hirano

Gaidos

Winn

et al. 2020

ApJL

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“…This implies that Ω2 = 0 • and ω2 = 0 • for the circular case of the perturbing planet. This setting provides a most conservative estimate of the upper mass limit of a possible perturber (Bean 2009;Fukui et al 2011;Hoyer et al 2011Hoyer et al , 2012. We refer the interested reader to Wang et al (2018a) where the authors have studied the effect on upper mass limit for various initial orbital parameters.…”

Section: Constraints On the Mass Of A Possible Perturbermentioning

confidence: 99%

Discarding orbital decay in WASP-19b after one decade of transit observations★†

Petrucci

Jofré

Chew

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a empirical study of orbital decay for the exoplanet WASP-19b, based on mid-time measurements of 74 complete transits (12 newly obtained by our team and 62 from the literature), covering a 10-year baseline. A linear ephemeris best represents the mid-transit times as a function of epoch. Thus, we detect no evidence of the shortening of WASP-19b's orbital period and establish an upper limit of its steady changing rate,Ṗ = −2.294 ms yr −1 , and a lower limit for the modified tidal quality factor Q = (1.23 ± 0.231) × 10 6 . Both are in agreement with previous works. This is the first estimation of Q directly derived from the mid-times of WASP-19b obtained through homogeneously analyzed transit measurements. Additionally, we do not detect periodic variations in the transit timings within the measured uncertainties in the midtimes of transit. We are therefore able to discard the existence of planetary companions in the system down to a few M ⊕ in the first order mean-motion resonances 1:2 and 2:1 with WASP-19b, in the most conservative case of circular orbits. Finally, we measure the empirical Q values of 15 exoplanet host stars which suggest that stars with T eff 5600K dissipate tidal energy more efficiently than hotter stars. This tentative trend needs to be confirmed with a larger sample of empirically measured Q .

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“…15 The exposure times were 60 s, 30 s, and 60 s for g , 2 ¢ r , 2 ¢ and z s,2 bands, respectively. Bias subtraction, flat-fielding, and aperture photometry are performed by a customized pipeline (Fukui et al 2011). Aperture radii are selected as 17, 18, and 19 pixels for g , 2 ¢ r , 2 ¢ and z s,2 bands, respectively.…”

Section: Oao 188 M Telescope/muscatmentioning

confidence: 99%

Characterization of the K2-19 Multiple-Transiting Planetary System via High-Dispersion Spectroscopy, Ao Imaging, and Transit Timing Variations

Narita

Hirano

Fukui

et al. 2015

ApJ

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K2-19 (EPIC201505350) is an interesting planetary system in which two transiting planets with radii ∼7 R ⊕ (inner planet b) and ∼4 R ⊕ (outer planet c) have orbits that are nearly in a 3:2 mean-motion resonance. Here, we present results of ground-based follow-up observations for the K2-19 planetary system. We have performed highdispersion spectroscopy and high-contrast adaptive-optics imaging of the host star with the HDS and HiCIAO on the Subaru 8.2 m telescope. We find that the host star is a relatively old (8 Gyr) late G-type star (T eff ∼5350 K, M s ∼0.9 M e , and R s ∼0.9 R e ). We do not find any contaminating faint objects near the host star that could be responsible for (or dilute) the transit signals. We have also conducted transit follow-up photometry for the inner planet with KeplerCam on the FLWO 1.2 m telescope, TRAPPISTCAM on the TRAPPIST 0.6 m telescope, and MuSCAT on the OAO 1.88 m telescope. We confirm the presence of transit timing variations (TTVs), as previously reported by Armstrong and coworkers. We model the observed TTVs of the inner planet using the synodic chopping formulae given by Deck & Agol. We find two statistically indistinguishable solutions for which the period ratios (P c /P b ) are located slightly above and below the exact 3:2 commensurability. Despite the degeneracy, we derive the orbital period of the inner planet P b ∼7.921 days and the mass of the outer planet M c ∼20 M ⊕ . Additional transit photometry (especially for the outer planet) as well as precise radial-velocity measurements would be helpful to break the degeneracy and to determine the mass of the inner planet.

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Measurements of Transit Timing Variations for WASP-5b

Cited by 87 publications

References 59 publications

Evidence for Spin–Orbit Alignment in the TRAPPIST-1 System

Evidence for Spin–Orbit Alignment in the TRAPPIST-1 System

Discarding orbital decay in WASP-19b after one decade of transit observations★†

Characterization of the K2-19 Multiple-Transiting Planetary System via High-Dispersion Spectroscopy, Ao Imaging, and Transit Timing Variations

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