CO and H2O in the exoplanetary atmosphere of HD189733b (continued)

Details CO and H2O in the exoplanetary atmosphere of HD189733b (continued) CO and H2O in the exoplanetary atmosphere of HD189733b (continued)

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007sptz.prop40732v&link_type=abstract

Spitzer Proposal ID #40732

Computer Science

Scientific paper

Water and carbon monoxide are predicted to be among the most abundant species in the atmospheres of Hot-Jupiters. Here, we propose to observe the signatures of these two crucial species in the atmosphere of the exoplanet HD189733b, utilizing high signal-to-noise IRAC observations during primary transit of its bright parent star. In Cycle 3, we observed primary transits with IRAC at 3.6 and 5.8 microns, obtaining clear transit detections in the two bands. Analysis of this IRAC data has provided occultation depth measurements with high accuracy. As expected, the occultation depth is found to be larger at 5 microns, which can be attributed to the signature of water band absorption. However, following advice of Spitzer technical staff, in Cycle 3 we did not observe at 4.5 and 8 microns to avoid switching between the two stellar observation modes. Observations of these two additional channels will help confirm our atmospheric water detection and allow us to discriminate between competing absorbers. Additionally, the 3.6 micron observations are close to saturation and require additional observations to ensure non-linearity issues do not compromise our atmospheric detection. We propose new observations of two planetary transits to both confirm the results of Cycle 3 observations and to complement them by the search for CO absorption in the band at 4.5 microns. Because the transit time is short, the present program can be executed in only 9 hours of Spitzer time.

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