TESS Transit Timing of Hundreds of Hot Jupiters

Abstract

We provide a database of transit times and updated ephemerides for 382 planets based on data from the NASA Transiting Exoplanet Survey Satellite (TESS) and previously reported transit times, which were scraped from the literature in a semiautomated fashion. In total, our database contains 8667 transit-timing measurements for 382 systems. About 240 planets in the catalog are hot Jupiters (i.e., planets with mass >0.3 M Jup and period <10 days) that have been observed by TESS. The new ephemerides are useful for scheduling follow-up observations and searching for long-term period changes. WASP-12 remains the only system for which a period change is securely detected. We remark on other cases of interest, such as a few systems with suggestive (but not yet convincing) evidence for period changes, and the detection of a second transiting planet in the NGTS-11 system. The compilation of light curves, transit times, ephemerides, and timing residuals are made available online, along with the Python code that generated them (visit https://transit-timing.github.io).

Near-infrared and optical emission of WASP-5 b

“…The error on the period was calculated from (σ 2 1 + σ 2 2 ) 1/2 /2444, where σ 1 = 0.00019 d as given in Fukui et al (2011), σ 2 is the epoch error as given in Table 4, and the integer in the denominator is the elapsed epoch number between the two epochs. It is worth noting that the currently published ephemerides by Ivshina & Winn (2022) are in complete agreement with ours. There are 7 ms and 17 s differences between the periods and transit centers, respectively, corresponding an agreement within 1−2σ.…”

Spatially-resolving the terminator: Variation of Fe, temperature and winds in WASP-76 b across planetary limbs and orbital phase

“…The Δ𝑉 sys values are dependent on the orbital period and transit time centre, but by propagating the uncertainties reported in Ehrenreich et al (2020), we find that Δ𝑉 sys changes by at most ∼0.5 km/s. By using other recently published precise orbital values (Kokori et al 2022;Ivshina & Winn 2022), we also find consistent results to within the uncertainties and ∼1 km/s. Therefore, any red-or blue-shift of the spectrum indicates the presence of a wind and cannot be explained by variations in orbital parameters.…”

The Hubble PanCET Program: A Featureless Transmission Spectrum for WASP-29b and Evidence of Enhanced Atmospheric Metallicity on WASP-80b

“…Comparing our best-fit transit shape parameters for WASP-29b with the results from Gibson et al (2013), we find that our values for b and a/R * are consistent with theirs at better than the 1σ level, while having significantly smaller uncertainties. Meanwhile, we obtained an updated orbital period of 3.9227090 +0.0000017 −0.0000018 d, which is roughly 1.5σ shorter than the recently published period measurement in Ivshina & Winn (2022): 3.92271159 ± 0.00000038 d. The Spitzer transits of WASP-29b were previously analyzed by Baxter et al (2021), who obtained 3.6 and 4.5 µm transit depths of 9500 ± 100 and 9300 ± 100 ppm, respectively, which agree with our measurements at better than the 1σ level.…”