Browsing by Author "Bruni, I"

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    Full orbital solution for the binary system in the northern Galactic disc microlensing event Gaia16aye
    (2020) Wyrzykowski, L; Mroz, P; Rybicki, KA; Gromadzki, M; Kolaczkowski, Z; Zielinski, M; Zielinski, P; Britavskiy, N; Gomboc, A; Sokolovsky, K; Hodgkin, ST; Abe, L; Aldi, GF; AlMannaei, A; Altavilla, G; Al Qasim, A; Anupama, GC; Awiphan, S; Bachelet, E; Bakis, V; Baker, S; Bartlett, S; Bendjoya, P; Benson, K; Bikmaev, IF; Birenbaum, G; Blagorodnova, N; Blanco-Cuaresma, S; Boeva, S; Bonanos, AZ; Bozza, V; Bramich, DM; Bruni, I; Burenin, RA; Burgaz, U; Butterley, T; Caines, HE; Caton, DB; Novati, SC; Carrasco, JM; Cassan, A; Cepas, V; Cropper, M; Chruslinska, M; Clementini, G; Clerici, A; Conti, D; Conti, M; Cross, S; Cusano, F; Damljanovic, G; Dapergolas, A; D'Ago, G; de Bruijne, JHJ; Dennefeld, M; Dhillon, VS; Dominik, M; Dziedzic, J; Erece, O; Eselevich, MV; Esenoglu, H; Eyer, L; Jaimes, RF; Fossey, SJ; Galeev, AI; Grebenev, SA; Gupta, AC; Gutaev, AG; Hallakoun, N; Hamanowicz, A; Han, C; Handzlik, B; Haislip, JB; Hanlon, L; Hardy, LK; Harrison, DL; van Heerden, HJ; Hoette, VL; Horne, K; Hudec, R; Hundertmark, M; Ihanec, N; Irtuganov, EN; Itoh, R; Iwanek, P; Jovanovic, MD; Janulis, R; Jelinek, M; Jensen, E; Kaczmarek, Z; Katz, D; Khamitov, IM; Kilic, Y; Klencki, J; Kolb, U; Kopacki, G; Kouprianov, VV; Kruszynska, K; Kurowski, S; Latev, G; Lee, CH; Leonini, S; Leto, G; Lewis, F; Li, Z; Liakos, A; Littlefair, SP; Lu, J; Manser, CJ; Mao, S; Maoz, D; Martin-Carrillo, A; Marais, JP; Maskoliunas, M; Maund, JR; Meintjes, PJ; Melnikov, SS; Ment, K; Mikolajczyk, P; Morrell, M; Mowlavi, N; Mozdzierski, D; Murphy, D; Nazarov, S; Netzel, H; Nesci, R; Ngeow, CC; Norton, AJ; Ofek, EO; Pakstiene, E; Palaversa, L; Pandey, A; Paraskeva, E; Pawlak, M; Penny, MT; Penprase, BE; Piascik, A; Prieto, JL; Qvam, JKT; Ranc, C; Rebassa-Mansergas, A; Reichart, DE; Reig, P; Rhodes, L; Rivet, JP; Rixon, G; Roberts, D; Rosi, P; Russell, DM; Sanchez, RZ; Scarpetta, G; Seabroke, G; Shappee, BJ; Schmidt, R; Shvartzvald, Y; Sitek, M; Skowron, J; Sniegowska, M; Snodgrass, C; Soares, PS; van Soelen, B; Spetsieri, ZT; Stankeviciute, A; Steele, IA; Street, RA; Strobl, J; Strubble, E; Szegedi, H; Ramirez, LMT; Tomasella, L; Tsapras, Y; Vernet, D; Villanueva, S; Vince, O; Wambsganss, J; van der Westhuizen, IP; Wiersema, K; Wium, D; Wilson, RW; Yoldas, A; Zhuchkov, RY; Zhukov, DG; Zdanavicius, J; Zola, S; Zubareva, A
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    The ultra-hot-Jupiter KELT-16 b: dynamical evolution and atmospheric properties
    (2022) Mancini, L.; Southworth, J.; Naponiello, L.; Basturk, O.; Barbato, D.; Biagiotti, F.; Bruni, I; Cabona, L.; D'Ago, G.; Damasso, M.; Erdem, A.; Evans, D.; Henning, Th; Ozturk, O.; Ricci, D.; Sozzetti, A.; Tregloan-Reed, J.; Yalcinkaya, S.
    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 ICELT-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(*)' > (1.9 +/- 0.8) x 10(5) with 95 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 degrees 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.