TY - JOUR
T1 - Spitzer Secondary Eclipses of WASP-18b
AU - Sarah, Nymeyer
AU - Joseph, Harrington
AU - Hardy Ryan, A.
AU - Stevenson Kevin, B.
AU - Campo Christopher, J.
AU - Nikku, Madhusudhan
AU - Andrew, Collier-Cameron
AU - Loredo Thomas, J.
AU - Jasmina, Blecic
AU - Jasmina, Blecic
AU - Britt Christopher, B.T.
AU - Patricio, Cubillos
AU - Michael, Gillon
AU - Maxted Pierre, F.L.
AU - Leslie, Hebb
AU - Wheatley Peter, J.
AU - Pollacco, Don
AU - Anderson David, R.
PY - 2011/11/20
Y1 - 2011/11/20
N2 - The transiting exoplanet WASP-18b was discovered in 2008 by the Wide Angle Search for Planets project. The Spitzer Exoplanet Target of Opportunity Program observed secondary eclipses of WASP-18b using Spitzer's Infrared Array Camera in the 3.6 µm and 5.8 µm bands on 2008 December 20, and in the 4.5 µm and 8.0 µm bands on 2008 December 24. We report eclipse depths of 0.30% ± 0.02%, 0.39% ± 0.02%, 0.37% ± 0.03%, 0.41% ± 0.02%, and brightness temperatures of 3100 ± 90, 3310 ± 130, 3080 ± 140, and 3120 ± 110 K in order of increasing wavelength. WASP-18b is one of the hottest planets yet discovered—as hot as an M-class star. The planet's pressure-temperature profile most likely features a thermal inversion. The observations also require WASP-18b to have near-zero albedo and almost no redistribution of energy from the day side to the night side of the planet.
AB - The transiting exoplanet WASP-18b was discovered in 2008 by the Wide Angle Search for Planets project. The Spitzer Exoplanet Target of Opportunity Program observed secondary eclipses of WASP-18b using Spitzer's Infrared Array Camera in the 3.6 µm and 5.8 µm bands on 2008 December 20, and in the 4.5 µm and 8.0 µm bands on 2008 December 24. We report eclipse depths of 0.30% ± 0.02%, 0.39% ± 0.02%, 0.37% ± 0.03%, 0.41% ± 0.02%, and brightness temperatures of 3100 ± 90, 3310 ± 130, 3080 ± 140, and 3120 ± 110 K in order of increasing wavelength. WASP-18b is one of the hottest planets yet discovered—as hot as an M-class star. The planet's pressure-temperature profile most likely features a thermal inversion. The observations also require WASP-18b to have near-zero albedo and almost no redistribution of energy from the day side to the night side of the planet.
U2 - 10.1088/0004-637X/742/1/35
DO - 10.1088/0004-637X/742/1/35
M3 - Article
VL - 742
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 35
ER -