TOI-1518b: A Misaligned Ultra-hot Jupiter with Iron in Its Atmosphere

Bello-Arufe, Aaron; Mendonça, João M.; Tronsgaard, R.; Wong, Ian; Zhou, George; Buchhave, Lars A.; Fischer, Debra A.; Stassun, Keivan G.; Antoci, V.; Baker, David; Belinski, A. A.; Benneke, Björn; Bouma, Luke G.; Christiansen, Jessie L.; Collins, Karen A.; Goliguzova, Maria V.; Hagey, Simone R.; Jenkins, Jon M.; Jensen, Eric L. N.; Kidwell, Richard C.; Laloum, Didier; Massey, Bob; McLeod, Kim K.; Latham, David W.; Morgan, E.; Ricker, G.; Safonov, Boris; Schlieder, Joshua E.; Seager, Sara; Shporer, Avi; Smith, Jeffrey C.; Srdoč, Gregor; Strakhov, Ivan A.; Torres, Guillermo; Twicken, Joseph D.; Vanderspek, R.; Vezie, Michael; Winn, Joshua N.

doi:10.3847/1538-3881/ac1ba3

Cited by 22 publications

(9 citation statements)

References 142 publications

(162 reference statements)

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“…In order to detect the minute planetary signal, it is necessary to correct for systematic sources of error, most notably the presence of telluric absorption lines in the spectra, but also systematics due to detector imperfections, etc. Most recent studies of exoplanetary atmospheres at high resolution use one of two methods to correct systematics: SYSREM (e.g., Nugroho et al 2020;Merritt et al 2021;Cont et al 2021a) or molecfit (e.g., Stangret et al 2021;Cabot et al 2021;Kesseli et al 2022). The SYSREM algorithm (Tamuz et al 2005) is a PCA-based algorithm to remove common linear or timevarying systematics.…”

Section: Comparison Of Telluric and Systematics Correction Methodsmentioning

confidence: 99%

“…Although molecfit was designed to work on data from ESO facilities, it has also been used for data from other spectrographs (e.g., Cabot et al 2021). We only 2 https://github.com/stephtdouglas/PySysRem used molecfit to correct the PEPSI red arm data, as there are no significant telluric lines in the blue arm.…”

Section: Comparison Of Telluric and Systematics Correction Methodsmentioning

confidence: 99%

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The PEPSI-LBT Exoplanet Transit Survey (PETS). II. A Deep Search for Thermal Inversion Agents in KELT-20 b/MASCARA-2 b with Emission and Transmission Spectroscopy

Johnson¹,

Wang²,

Asnodkar³

et al. 2022

Preprint

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Recent observations have shown that the atmospheres of ultra hot Jupiters (UHJs) commonly possess temperature inversions, where the temperature increases with increasing altitude. Nonetheless, which opacity sources are responsible for the presence of these inversions remains largely observationally unconstrained. We used LBT/PEPSI to observe the atmosphere of the UHJ KELT-20 b in both transmission and emission in order to search for molecular agents which could be responsible for the temperature inversion. We validate our methodology by confirming a previous detection of Fe i in emission at 15.1σ; however, we are unable to reproduce published detections of Fe ii, Cr i, or Si i. We attribute the non-detection of Si i to the lack of lines in our bandpass, but the non-detections of Fe ii and Cr i are puzzling due to our much higher signal-to-noise ratio than previous works. Our search for the inversion agents TiO, VO, FeH, and CaH results in non-detections. Using injection-recovery testing we set 4σ upper limits upon the volume mixing ratios for these constituents as low as ∼ 1 × 10 −10 for TiO. For TiO, VO, and CaH, our limits are much lower than expectations from an equilibrium chemical model, while FeH is lower than the expectations only from a super-Solar metallicity model. We thus rule out TiO, VO, and CaH as the source of the temperature inversion in KELT-20 b, while FeH is disfavored only if KELT-20 b possesses a high-metallicity atmosphere.

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Section: Comparison Of Telluric and Systematics Correction Methodsmentioning

confidence: 99%

Section: Comparison Of Telluric and Systematics Correction Methodsmentioning

confidence: 99%

The PEPSI-LBT Exoplanet Transit Survey (PETS). II. A Deep Search for Thermal Inversion Agents in KELT-20 b/MASCARA-2 b with Emission and Transmission Spectroscopy

Johnson¹,

Wang²,

Asnodkar³

et al. 2022

Preprint

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“…To narrow the list to only well-characterized planets, we excluded objects with relative radius and mass uncertainties larger than 10% and 50%, respectively. We also included two recently discovered ultrahot Jupiters from TESS: TOI-1431b (Addison et al 2021) and TOI-1518b (Cabot et al 2021).…”

Section: Discussionmentioning

confidence: 99%

“…The black points are derived from the comprehensive analysis of Spitzer 4.5 μm phase curves byBell et al (2021). In addition to TOI-2109b, we have included the values for two recently published ultrahot Jupiters from TESS: TOI-1431b(Addison et al 2021) and TOI-1518b(Cabot et al 2021). The horizontal lines denote two fiducial scenarios: the maximum theoretical dayside temperature (no heat recirculation, A B = 0) and the dayside-redistribution equilibrium temperature (uniform dayside temperature, with A B = 0 and T = 0 K on the nightside).…”

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confidence: 99%

TOI-2109: An Ultrahot Gas Giant on a 16 hr Orbit

Wong

Shporer

Zhou

et al. 2021

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We report the discovery of an ultrahot Jupiter with an extremely short orbital period of 0.67247414 ± 0.00000028 days (∼16 hr). The 1.347 ± 0.047 R Jup planet, initially identified by the Transiting Exoplanet Survey Satellite (TESS) mission, orbits TOI-2109 (TIC 392476080)—a T eff ∼ 6500 K F-type star with a mass of 1.447 ± 0.077 M ☉, a radius of 1.698 ± 0.060 R ☉, and a rotational velocity of v sin i * = 81.9 ± 1.7 km s−1. The planetary nature of TOI-2109b was confirmed through radial-velocity measurements, which yielded a planet mass of 5.02 ± 0.75 M Jup. Analysis of the Doppler shadow in spectroscopic transit observations indicates a well-aligned system, with a sky-projected obliquity of λ = 1.°7 ± 1.°7. From the TESS full-orbit light curve, we measured a secondary eclipse depth of 731 ± 46 ppm, as well as phase-curve variations from the planet’s longitudinal brightness modulation and ellipsoidal distortion of the host star. Combining the TESS-band occultation measurement with a K s -band secondary eclipse depth (2012 ± 80 ppm) derived from ground-based observations, we find that the dayside emission of TOI-2109b is consistent with a brightness temperature of 3631 ± 69 K, making it the second hottest exoplanet hitherto discovered. By virtue of its extreme irradiation and strong planet–star gravitational interaction, TOI-2109b is an exceptionally promising target for intensive follow-up studies using current and near-future telescope facilities to probe for orbital decay, detect tidally driven atmospheric escape, and assess the impacts of H2 dissociation and recombination on the global heat transport.

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“…Their close-in orbits, large radii, and large-scale heights make UHJs especially suitable for atmospheric studies. Recently, a large diversity of neutral and ionized atomic metals have been found in UHJs using high-resolution transmission spectroscopy in the optical and near-infrared (e.g., Casasayas-Barris et al 2018Hoeijmakers et al 2019;Nugroho et al 2020aNugroho et al , 2020bBen-Yami et al 2020;Cabot et al 2020;Hoeijmakers et al 2020;Stangret et al 2020;Yan et al 2020;Cabot et al 2021;Cont et al 2021;Deibert et al 2021;Kesseli et al 2022;Merritt et al 2021;Prinoth et al 2022). On the other hand, the inventory of molecular species in UHJs is lacking.…”

Section: Introductionmentioning

confidence: 99%

A First Look at CRIRES+: Performance Assessment and Exoplanet Spectroscopy

Holmberg¹,

Madhusudhan²

2022

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High-resolution spectroscopy has proven to be a powerful avenue for atmospheric remote sensing of exoplanets. Recently, ESO commissioned the CRIRES+ high-resolution infrared spectrograph at the Very Large Telescope. CRIRES+ is a cross-dispersed spectrograph with high throughput and wide wavelength coverage across the near-infrared (0.95–5.3 μm), designed to be particularly suited for atmospheric characterization of exoplanets. In this work, we report early insights into the performance of CRIRES+ for exoplanet spectroscopy and conduct a detailed assessment of the data reduction procedure. Because of the novelty of the instrument, we perform two independent data reduction strategies using the official CR2RES pipeline and our new custom-built ExoRES pipeline. Using science verification observations we find that the spectral resolving power of CRIRES+ can reach R ≳ 100,000 for optimal observing conditions. Similarly, we find the signal-to-noise ratio (S/N) to be consistent with expected and empirical estimates for the observations considered. As a case study, we perform the first application of CRIRES+ to the atmospheric characterization of an exoplanet—the ultrahot Jupiter MASCARA-1 b. We detect CO and H2O in the atmosphere of MASCARA-1 b at a S/N of 12.9 and 5.3, respectively, and a temperature inversion revealed through the CO and H2O emission lines, the first for an exoplanet. We find a combined S/N of 13.8 for CO and H2O together, with a preference for lower H2O abundance compared to CO. Our findings demonstrate the scientific potential of CRIRES+ and highlight the excellent opportunity for high-resolution atmospheric spectroscopy of diverse exoplanets.

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TOI-1518b: A Misaligned Ultra-hot Jupiter with Iron in Its Atmosphere

Cited by 22 publications

References 142 publications

The PEPSI-LBT Exoplanet Transit Survey (PETS). II. A Deep Search for Thermal Inversion Agents in KELT-20 b/MASCARA-2 b with Emission and Transmission Spectroscopy

The PEPSI-LBT Exoplanet Transit Survey (PETS). II. A Deep Search for Thermal Inversion Agents in KELT-20 b/MASCARA-2 b with Emission and Transmission Spectroscopy

TOI-2109: An Ultrahot Gas Giant on a 16 hr Orbit

A First Look at CRIRES+: Performance Assessment and Exoplanet Spectroscopy

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