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. (arXiv:2205.12162v1 [astro-ph.EP])

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. (arXiv:2205.12162v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Johnson_M/0/1/0/all/0/1">Marshall C. Johnson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_J/0/1/0/all/0/1">Ji Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asnodkar_A/0/1/0/all/0/1">Anusha Pai Asnodkar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonomo_A/0/1/0/all/0/1">Aldo S. Bonomo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaudi_B/0/1/0/all/0/1">B. Scott Gaudi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henning_T/0/1/0/all/0/1">Thomas Henning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ilyin_I/0/1/0/all/0/1">Ilya Ilyin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keles_E/0/1/0/all/0/1">Engin Keles</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malavolta_L/0/1/0/all/0/1">Luca Malavolta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mallonn_M/0/1/0/all/0/1">Matthias Mallonn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Molaverdikhani_K/0/1/0/all/0/1">Karan Molaverdikhani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nascimbeni_V/0/1/0/all/0/1">Valerio Nascimbeni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Patience_J/0/1/0/all/0/1">Jennifer Patience</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poppenhaeger_K/0/1/0/all/0/1">Katja Poppenhaeger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scandariato_G/0/1/0/all/0/1">Gaetano Scandariato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schlawin_E/0/1/0/all/0/1">Everett Schlawin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shkolnik_E/0/1/0/all/0/1">Evgenya Shkolnik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sicilia_D/0/1/0/all/0/1">Daniela Sicilia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sozzetti_A/0/1/0/all/0/1">Alessandro Sozzetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Strassmeier_K/0/1/0/all/0/1">Klaus G. Strassmeier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Veillet_C/0/1/0/all/0/1">Christian Veillet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yan_F/0/1/0/all/0/1">Fei Yan</a>

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 $15.1sigma$;
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 $4sigma$ upper limits upon the volume mixing ratios for these
constituents as low as $sim1times10^{-10}$ 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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