Bibcode
Ciceri, S.; Mancini, L.; Southworth, J.; Lendl, M.; Tregloan-Reed, J.; Brahm, R.; Chen, G.; D'Ago, G.; Dominik, M.; Figuera Jaimes, R.; Galianni, P.; Harpsøe, K.; Hinse, T. C.; Jørgensen, U. G.; Juncher, D.; Korhonen, H.; Liebig, C.; Rabus, M.; Bonomo, A. S.; Bott, K.; Henning, Th.; Jordán, A.; Sozzetti, A.; Alsubai, K. A.; Andersen, J. M.; Bajek, D.; Bozza, V.; Bramich, D. M.; Browne, P.; Calchi Novati, S.; Damerdji, Y.; Diehl, C.; Elyiv, A.; Giannini, E.; Gu, S.-H.; Hundertmark, M.; Kains, N.; Penny, M.; Popovas, A.; Rahvar, S.; Scarpetta, G.; Schmidt, R. W.; Skottfelt, J.; Snodgrass, C.; Surdej, J.; Vilela, C.; Wang, X.-B.; Wertz, O.
Bibliographical reference
Monthly Notices of the Royal Astronomical Society, Volume 456, Issue 1, p.990-1002
Advertised on:
2
2016
Citations
20
Refereed citations
17
Description
Accurate measurements of the physical characteristics of a large number
of exoplanets are useful to strongly constrain theoretical models of
planet formation and evolution, which lead to the large variety of
exoplanets and planetary-system configurations that have been observed.
We present a study of the planetary systems WASP-45 and WASP-46, both
composed of a main-sequence star and a close-in hot Jupiter, based on 29
new high-quality light curves of transits events. In particular, one
transit of WASP-45 b and four of WASP-46 b were simultaneously observed
in four optical filters, while one transit of WASP-46 b was observed
with the NTT obtaining a precision of 0.30 mmag with a cadence of
roughly 3 min. We also obtained five new spectra of WASP-45 with the
FEROS spectrograph. We improved by a factor of 4 the measurement of the
radius of the planet WASP-45 b, and found that WASP-46 b is slightly
less massive and smaller than previously reported. Both planets now have
a more accurate measurement of the density (0.959 ± 0.077
ρJup instead of 0.64 ± 0.30 ρJup
for WASP-45 b, and 1.103 ± 0.052 ρJup instead of
0.94 ± 0.11 ρJup for WASP-46 b). We tentatively
detected radius variations with wavelength for both planets, in
particular in the case of WASP-45 b we found a slightly larger
absorption in the redder bands than in the bluer ones. No hints for the
presence of an additional planetary companion in the two systems were
found either from the photometric or radial velocity measurements.