Issue |
A&A
Volume 513, April 2010
|
|
---|---|---|
Article Number | L3 | |
Number of page(s) | 5 | |
Section | Letters | |
DOI | https://doi.org/10.1051/0004-6361/201014226 | |
Published online | 14 April 2010 |
Letter to the Editor
H-band thermal emission from the 19-h period planet WASP-19b *,**
1
Astrophysics Group, Keele University, Staffordshire ST5 5BG, UK e-mail: dra@astro.keele.ac.uk
2
Institut d'Astrophysique et de Géophysique, Université de
Liège, Allée du 6 Août 17, Bat. B5C, 4000 Liège, Belgium
3
Observatoire de Genève, Université de Genève, 51 Chemin des
Maillettes, 1290 Sauverny, Switzerland
4
Lowell Observatory, 1400 West Mars Hill Road, Flagstaff,
AZ 86001, USA
5
School of Physics and Astronomy, University of St. Andrews,
North Haugh, Fife KY16 9SS, UK
Received:
9
February
2010
Accepted:
10
March
2010
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%, which
corresponds to an H-band brightness temperature of TH = 2580 ± 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.
Key words: planets and satellites: atmospheres / planetary systems / stars: individual: WASP-19b / techniques: photometric
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
© ESO, 2010
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