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Register a new userTOI-1431b/MASCARA-5b: A Highly Irradiated Ultra-Hot Jupiter Orbiting One of the Hottest & Brightest Known Exoplanet Host Stars
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We present the discovery of a highly irradiated and moderately inflated ultra-hot Jupiter, TOI-1431b/MASCARA-5b (HD 201033b), first detected by NASAs Transiting Exoplanet Survey Satellite mission (TESS) and the Multi-site All-Sky CAmeRA (MASCARA). The signal was established to be of planetary origin through radial velocity measurements obtained using SONG, SOPHIE, FIES, NRES, and EXPRES, which show a reflex motion of $K=294.1pm1.1$ m s$^{-1}$. A joint analysis of TESS, MuSCAT2, and LCOGT photometry, radial velocity measurements, and the spectral energy distribution of the host star reveals that TOI-1431b has a mass of $M_{p}=3.14_{-0.18}^{+0.19}$ $rm{M_J}$ ($1000pm60$ M$_{oplus}$), an inflated radius of $R_{p}=1.51pm0.06$ $rm{R_J}$ ($16.9_{-0.6}^{+0.7}$ R$_{oplus}$), and an orbital period of $P=2.65022pm0.00001$ d. The planet orbits a bright ($mathrm{V}=8.049$ mag) and young ($0.29^{+0.32}_{-0.19}$ Gyr) Am type star with $T_{rm eff}=7690^{+400}_{-250}$ $rm{K}$, resulting in a highly irradiated planet with an incident flux of $langle F rangle=7.24^{+0.68}_{-0.64}times$10$^9$ erg s$^{-1}$ cm$^{-2}$ ($5300^{+500}_{-470}mathrm{S_{oplus}}$) and an equilibrium temperature of $T_{eq}=2370pm100$ K. TESS photometry also reveals a secondary eclipse with a depth of $124pm5$ppm as well as the full phase curve of the planets thermal emission in the red-optical. This has allowed us to measure the dayside and nightside temperature of its atmosphere as $T_mathrm{day}=2983^{+63}_{-68}$ K and $T_mathrm{night}=2556^{+62}_{-65}$ K, the second hottest measured nightside temperature. The planets low day/night temperature contrast ($sim$400 K) suggests very efficient heat transport between the dayside and nightside hemispheres.
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Ultra-hot Jupiters are defined as giant planets with equilibrium temperatures larger than 2000 K. Most of them are found orbiting bright A-F type stars, making them extremely suitable objects to study their atmospheres using high-resolution spectroscopy. Recent studies show a variety of atoms and molecules detected in the atmospheres of this type of planets. Here we present our analysis of the newly discovered ultra-hot Jupiter TOI-1431b/MASCARA-5b, using two transit observations with the HARPS-N spectrograph and one transit observation with the EXPRES spectrograph. Analysis of the Rossiter-McLaughlin effect shows that the planet is in a polar orbit, with a projected obliquity $ lambda = -155^{+20}_{-10}$ degrees. Combining the nights and applying both cross-correlation methods and transmission spectroscopy, we find no evidences of CaI, FeI, FeII, MgI, NaI, VI, TiO, VO or H$alpha$ in the atmosphere of the planet. Our most likely explanation for the lack of atmospheric features is the large surface gravity of the planet.
We report the discovery of a new transiting planet from the WASP survey. WASP-135b is a hot Jupiter with a radius of 1.30 pm 0.09 Rjup, a mass of 1.90 pm 0.08 Mjup and an orbital period of 1.401 days. Its host is a Sun-like star, with a G5 spectral type and a mass and radius of 0.98 pm 0.06 Msun and 0.96 pm 0.05 Rsun respectively. The proximity of the planet to its host means that WASP-135b receives high levels of insolation, which may be the cause of its inflated radius. Additionally, we find weak evidence of a transfer of angular momentum from the planet to its star.
We announce the discovery of KELT-16b, a highly irradiated, ultra-short period hot Jupiter transiting the relatively bright ($V = 11.7$) star TYC 2688-1839-1. A global analysis of the system shows KELT-16 to be an F7V star with $T_textrm{eff} = 6236pm54$ K, $log{g_star} = 4.253_{-0.036}^{+0.031}$, [Fe/H] = -0.002$_{-0.085}^{+0.086}$, $M_star = 1.211_{-0.046}^{+0.043} M_odot$, and $R_star = 1.360_{-0.053}^{+0.064} R_odot$. The planet is a relatively high mass inflated gas giant with $M_textrm{P} = 2.75_{-0.15}^{+0.16} M_textrm{J}$, $R_textrm{P} = 1.415_{-0.067}^{+0.084} R_textrm{J}$, density $rho_textrm{P} = 1.20pm0.18$ g cm$^{-3}$, surface gravity $log{g_textrm{P}} = 3.530_{-0.049}^{+0.042}$, and $T_textrm{eq} = 2453_{-47}^{+55}$ K. The best-fitting linear ephemeris is $T_textrm{C} = 2457247.24791pm0.00019$ BJD$_{tdb}$ and $P = 0.9689951 pm 0.0000024$ d. KELT-16b joins WASP-18b, -19b, -43b, -103b, and HATS-18b as the only giant transiting planets with $P < 1$ day. Its ultra-short period and high irradiation make it a benchmark target for atmospheric studies by HST, Spitzer, and eventually JWST. For example, as a hotter, higher mass analog of WASP-43b, KELT-16b may feature an atmospheric temperature-pressure inversion and day-to-night temperature swing extreme enough for TiO to rain out at the terminator. KELT-16b could also join WASP-43b in extending tests of the observed mass-metallicity relation of the Solar System gas giants to higher masses. KELT-16b currently orbits at a mere $sim$ 1.7 Roche radii from its host star, and could be tidally disrupted in as little as a few $times 10^{5}$ years (for a stellar tidal quality factor of $Q_* = 10^5$). Finally, the likely existence of a widely separated bound stellar companion in the KELT-16 system makes it possible that Kozai-Lidov oscillations played a role in driving KELT-16b inward to its current precarious orbit.
We present the discovery of TOI-1518b -- an ultra-hot Jupiter orbiting a bright star $V = 8.95$. The transiting planet is confirmed using high-resolution optical transmission spectra from EXPRES. It is inflated, with $R_p = 1.875pm0.053,R_{rm J}$, and exhibits several interesting properties, including a misaligned orbit (${240.34^{+0.93}_{-0.98}}$ degrees) and nearly grazing transit ($b =0.9036^{+0.0061}_{-0.0053}$). The planet orbits a fast-rotating F0 host star ($T_{mathrm{eff}} simeq 7300$ K) in 1.9 days and experiences intense irradiation. Notably, the TESS data show a clear secondary eclipse with a depth of $364pm28$ ppm and a significant phase curve signal, from which we obtain a relative day-night planetary flux difference of roughly 320 ppm and a 5.2$sigma$ detection of ellipsoidal distortion on the host star. Prompted by recent detections of atomic and ionized species in ultra-hot Jupiter atmospheres, we conduct an atmospheric cross-correlation analysis. We detect neutral iron (${5.2sigma}$), at $K_p = 157^{+68}_{-44}$ km s$^{-1}$ and $V_{rm sys} = -16^{+2}_{-4}$ km s$^{-1}$, adding another object to the small sample of highly irradiated gas-giant planets with Fe detections in transmission. Detections so far favor particularly inflated gas giants with radii $gtrsim 1.78,R_{rm J}$; although this may be due to observational bias. With an equilibrium temperature of $T_{rm eq}=2492pm38$ K and a measured dayside brightness temperature of $3237pm59$ K (assuming zero geometric albedo), TOI-1518b is a promising candidate for future emission spectroscopy to probe for a thermal inversion.
Ultra-hot Jupiters are the most highly irradiated gas giant planets, with equilibrium temperatures from 2000 to over 4000 K. Ultra-hot Jupiters are amenable to characterization due to their high temperatures, inflated radii, and short periods, but their atmospheres are atypical for planets in that the photosphere possesses large concentrations of atoms and ions relative to molecules. Here we evaluate how the atmospheres of these planets respond to irradiation by stars of different spectral type. We find that ultra-hot Jupiters exhibit temperature
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