Mancini, L, Southworth, J ORCID: https://orcid.org/0000-0002-3807-3198, Naponiello, L, Baştürk, Ö, Barbato, D, Biagiotti, F, Bruni, I, Cabona, L, D’Ago, G, Damasso, M, Erdem, A, Evans, D, Henning, T, Öztürk, O, Ricci, D, Sozzetti, A, Tregloan-Reed, J and Yalçınkaya, S (2021) The ultra-hot-Jupiter KELT-16 b: Dynamical Evolution and Atmospheric Properties. Monthly Notices of the Royal Astronomical Society.

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Abstract

<jats:title>Abstract</jats:title> <jats:p>We present broad-band photometry of 30 planetary transits of the ultra-hot Jupiter KELT-16 b, using five medium-class telescopes. The transits were monitored through standard B, V, R, I filters and four were simultaneously observed from different places, for a total of 36 new light curves. We used these new photometric data and those from the TESS space telescope to review the main physical properties of the KELT-16 planetary system. Our results agree with previous measurements but are more precise. We estimated the mid-transit times for each of these transits and combined them with others from the literature to obtain 69 epochs, with a time baseline extending over more than four years, and searched for transit time variations. We found no evidence for a period change, suggesting a lower limit for orbital decay at 8 Myr, with a lower limit on the reduced tidal quality factor of $Q^{\prime }_{\star }&amp;gt;(1.9 \pm 0.8) \times 10^5$ with $95\%$ confidence. We built up an observational, low-resolution transmission spectrum of the planet, finding evidence of the presence of optical absorbers, although with a low significance. Using TESS data, we reconstructed the phase curve finding that KELT-16 b has a phase offset of 25.25 ± 14.03 ○E, a day- and night-side brightness temperature of 3190 ± 61 K and 2668 ± 56 K, respectively. Finally, we compared the flux ratio of the planet over its star at the TESS and Spitzer wavelengths with theoretical emission spectra, finding evidence of a temperature inversion in the planet’s atmosphere, the chemical composition of which is preferably oxygen-rich rather than carbon-rich.</jats:p>

Item Type: Article
Additional Information: The final version of this manuscript and all relevant information, including copyrights, related to it can be found online at; https://academic.oup.com/mnras/advance-article-abstract/doi/10.1093/mnras/stab2691/6373473?redirectedFrom=fulltext © 2021 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model)
Subjects: Q Science > QB Astronomy
Q Science > QB Astronomy > QB460 Astrophysics
Q Science > QC Physics
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Depositing User: Symplectic
Date Deposited: 05 Oct 2021 08:13
Last Modified: 05 Oct 2021 08:13
URI: https://eprints.keele.ac.uk/id/eprint/10092

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