TY - JOUR
T1 - H-band thermal emission from the 19-h period planet WASP-19b
AU - Anderson, D.~R.
AU - Gillon, M.
AU - Maxted, P.~F.~L.
AU - Barman, T.~S.
AU - Collier Cameron, A.
AU - Hellier, C.
AU - Queloz, D.
AU - Smalley, B.
AU - Triaud, A.~H.~M.~J.
PY - 2010/4/1
Y1 - 2010/4/1
N2 - We present the first ground-based detection of thermal emission from an exoplanet in the H-band. Using HAWK-I on the VLT, we observed an occultation of WASP-19b by its G8V-type host star. WASP-19b is a Jupiter-mass planet with an orbital period of only 19 h, and thus, being highly irradiated, is expected to be hot. We measure an H-band occultation depth of 0.259$^+0.046$$_-0.044$ which corresponds to an H-band brightness temperature of T$_H$ = 2580 plusmn 125 K. A cloud-free model of the planet's atmosphere, with no redistribution of energy from day-side to night-side, under predicts the planet/star flux density ratio by a factor of two. As the stellar parameters, and thus the level of planetary irradiation, are well-constrained by measurement, it is likely that our model of the planet's atmosphere is too simple. Based on data collected with the VLT/HAWKI instrument at ESO Paranal Observatory, Chile (programs 083.C-0377(A)).The photometric time-series used in this work are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/513/L3
AB - We present the first ground-based detection of thermal emission from an exoplanet in the H-band. Using HAWK-I on the VLT, we observed an occultation of WASP-19b by its G8V-type host star. WASP-19b is a Jupiter-mass planet with an orbital period of only 19 h, and thus, being highly irradiated, is expected to be hot. We measure an H-band occultation depth of 0.259$^+0.046$$_-0.044$ which corresponds to an H-band brightness temperature of T$_H$ = 2580 plusmn 125 K. A cloud-free model of the planet's atmosphere, with no redistribution of energy from day-side to night-side, under predicts the planet/star flux density ratio by a factor of two. As the stellar parameters, and thus the level of planetary irradiation, are well-constrained by measurement, it is likely that our model of the planet's atmosphere is too simple. Based on data collected with the VLT/HAWKI instrument at ESO Paranal Observatory, Chile (programs 083.C-0377(A)).The photometric time-series used in this work are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/513/L3
KW - planets and satellites: atmospheres, planetary systems, stars: individual: WASP-19b, techniques: photometric
U2 - 10.1051/0004-6361/201014226
DO - 10.1051/0004-6361/201014226
M3 - Article
SN - 0004-6361
VL - 513
SP - L3
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
ER -