Mancini, LLManciniSouthworth, JJSouthworthNaponiello, LLNaponielloBaştürk, ÖÖBaştürkBarbato, DDBarbatoBiagiotti, FFBiagiottiBruni, IIBruniCabona, LLCabonaD’Ago, GGD’AgoDamasso, MMDamassoErdem, AAErdemEvans, DDEvansHenning, ThThHenningÖztürk, OOÖztürkRicci, DDRicciSozzetti, AASozzettiTregloan-Reed, JJTregloan-ReedYalçınkaya, SSYalçınkaya2026-10-092026-10-092021-11-16Mancini, L; Southworth, J; Naponiello, L; Baştürk, Ö; Barbato, D; Biagiotti, F; Bruni, I; Cabona, L; D’Ago, G; Damasso, M; Erdem, A; Evans, D; Henning, Th; Öztürk, O; Ricci, D; Sozzetti, A; Tregloan-Reed, J; Yalçınkaya, S (2021-11-16). The ultra-hot-Jupiter KELT-16 b: dynamical evolution and atmospheric properties. Monthly Notices of the Royal Astronomical Society, 509(1), 1447-1464. https://doi.org/10.1093/mnras/stab26910035-87111365-2966https://hdl.handle.net/20.500.12740/25090ABSTRACT 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 4 yr, 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 $Q^{\prime }_{\star }\gt (1.9 \pm 0.8) \times 10^5$ with $95{{\rm {per\ cent}}}$ 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.http://purl.org/coar/access_right/c_abf2Stellar, planetary, and galactic studiesAstronomy and Astrophysical ResearchAstro and Planetary ScienceArticulohttps://doi.org/10.1093/mnras/stab2691