Mancini, L.L.ManciniSouthworth, J.J.SouthworthNaponiello, L.L.NaponielloBaştürk, Ö.Ö.BaştürkBarbato, D.D.BarbatoBiagiotti, F.F.BiagiottiBRUNI, IVANIVANBRUNICabona, L.L.CabonaD'Ago, G.G.D'AgoDamasso, MarioMarioDamassoErdem, A.A.ErdemEvans, D.D.EvansHenning, ThThHenningÖztürk, O.O.ÖztürkRICCI, DAVIDEDAVIDERICCISOZZETTI, AlessandroAlessandroSOZZETTITregloan-Reed, J.J.Tregloan-ReedYalçınkaya, S.S.Yalçınkaya2022-06-152022-06-1520220035-8711http://hdl.handle.net/20.500.12386/32320We 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.STAMPAenArticle10.1093/mnras/stab26912-s2.0-85121219557https://academic.oup.com/mnras/article/509/1/1447/6373473?login=truehttp://arxiv.org/abs/2105.00889v32022MNRAS.509.1447MFIS/05 - ASTRONOMIA E ASTROFISICA