The PEPSI exoplanet transit survey (PETS) I: investigating the presence of a silicate atmosphere on the super-earth 55 Cnc e

Keles, Engin; Mallonn, M.; Kitzmann, Daniel; Poppenhaeger, Katja; Hoeijmakers, H. J.; Ilyin, I.; Alexoudi, X.; Carroll, T. A.; Alvarado‐Gómez, Julián D.; Ketzer, Laura; Bonomo, A. S.; Borsa, F.; Gaudi, Scott; Henning, Thomas; Malavolta, L.; Molaverdikhani, Karan; Nascimbeni, V.; Patience, Jennifer; Pino, L.; Scandariato, G.; Schlawin, Everett; Shkolnik, Evgenya L.; Sicilia, D.; Sozzetti, A.; Foster, Mary G.; Veillet, Christian; Wang, Ji; Yan, F.; Strassmeier, K. G.

doi:10.1093/mnras/stac810

Cited by 26 publications

(13 citation statements)

References 58 publications

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“…Unlike D16b, our excellent transit depth agreement with Morris et al (2021) and Meier Valdés et al (2022) tentatively excludes a cloud-free hydrogen-dominated atmosphere (see details in Appendix D). This is consistent with unsuccessful searches for atoms and molecules in transit (Ehrenreich et al 2012;Ridden-Harper et al 2016;Esteves et al 2017;Tabernero et al 2020;Zhang et al 2021b;Keles et al 2022). While Tsiaras et al (2016) reported a hint of HCN based on Hubble observations, no molecules-including HCN-were detected in ground-based high-dispersion spectroscopy (Deibert et al 2021).…”

Section: Interpretation Of Resultssupporting

confidence: 63%

Revisiting the Iconic Spitzer Phase Curve of 55 Cancri e: Hotter Dayside, Cooler Nightside, and Smaller Phase Offset

Mercier

Dang

Cowan

et al. 2022

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Thermal phase curves of short-period exoplanets provide the best constraints on the atmospheric dynamics and heat transport in their atmospheres. The published Spitzer Space Telescope phase curve of 55 Cancri e, an ultra-short-period super-Earth, exhibits a large phase offset suggesting significant eastward heat recirculation, unexpected on such a hot planet. We present our rereduction and analysis of these iconic observations using the open source and modular Spitzer Phase Curve Analysis pipeline. In particular, we attempt to reproduce the published analysis using the same instrument detrending scheme as the original authors. We retrieve the dayside temperature ( T day = 3771 − 520 + 669 K), nightside temperature ( T night < 1649 K at 2σ), and longitudinal offset of the planet's hot spot, and quantify how they depend on the reduction and detrending. Our reanalysis suggests that 55 Cancri e has a negligible hot spot offset of − 12 − 18 + 21 degrees east. The small phase offset and cool nightside are consistent with the poor heat transport expected on ultra-short-period planets. The high dayside 4.5 μm brightness temperature is qualitatively consistent with SiO emission from an inverted rock vapor atmosphere.

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Section: Interpretation Of Resultssupporting

confidence: 63%

Revisiting the Iconic Spitzer Phase Curve of 55 Cancri e: Hotter Dayside, Cooler Nightside, and Smaller Phase Offset

Mercier

Dang

Cowan

et al. 2022

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“…The raw and detrended photometric time-series data are available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/ cgi-bin/qcat?J/A+A/ Winn et al 2011;Demory et al 2011;Bourrier et al 2018), and an orbital period of only 17.7 hr, 55 Cnc e is larger than most USP planets. 55 Cnc e's bulk density favours the presence of an atmosphere (Dorn et al 2017;Crida et al 2018;Bourrier et al 2018), possibly SiO- (Schaefer & Fegley 2009) or N-dominated (Miguel 2019), but so far no observations have provided definitive evidence for such an atmosphere (Ehrenreich et al 2012;Ridden-Harper et al 2016;Tsiaras et al 2016;Esteves et al 2017;Jindal et al 2020;Tabernero et al 2020;Deibert et al 2021;Zhang et al 2021;Keles et al 2022).…”

Section: Introductionmentioning

confidence: 99%

55 Cancri e’s occultation captured with CHEOPS

Demory¹,

Sulis²,

Valdes³

et al. 2023

A&A

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Past occultation and phase-curve observations of the ultra-short period super-Earth 55 Cnc e obtained at visible and infrared wavelengths have been challenging to reconcile with a planetary reflection and emission model. In this study, we analyse a set of 41 occultations obtained over a two-year timespan with the CHEOPS satellite. We report the detection of 55 Cnc e's occultation with an average depth of 12 ± 3 ppm. We derive a corresponding 2-σ upper limit on the geometric albedo of A g < 0.55 once decontaminated from the thermal emission measured by Spitzer at 4.5µm. CHEOPS's photometric performance enables, for the first time, the detection of individual occultations of this super-Earth in the visible and identifies short-timescale photometric corrugations likely induced by stellar granulation. We also find a clear 47.3-day sinusoidal pattern in the time-dependent occultation depths that we are unable to relate to stellar noise, nor instrumental systematics, but whose planetary origin could be tested with upcoming JWST occultation observations of this iconic super-Earth.

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“…The PEPSI-LBT Exoplanet Transit Survey (PETS) is a large (∼400 hour) survey of transiting exoplanets using the PEPSI high-resolution spectrograph on the Large Binocular Telescope (LBT). The first paper resulting from the survey set limits on the atmospheric presence of atomic species that could be vaporized from the crust of the super-Earth 55 Cnc e (Keles et al 2022). In this second paper in the series, we analyze our emission and transmission spectra of KELT-20 b.…”

Section: Introductionmentioning

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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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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The PEPSI exoplanet transit survey (PETS) I: investigating the presence of a silicate atmosphere on the super-earth 55 Cnc e

Cited by 26 publications

References 58 publications

Revisiting the Iconic Spitzer Phase Curve of 55 Cancri e: Hotter Dayside, Cooler Nightside, and Smaller Phase Offset

Revisiting the Iconic Spitzer Phase Curve of 55 Cancri e: Hotter Dayside, Cooler Nightside, and Smaller Phase Offset

55 Cancri e’s occultation captured with CHEOPS

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

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