We propose to use the NICMOS camera to search for transit NIR signatures of atmospheric water in HD189733b. While water absorption bands exist in the optical and IR, space-based NIR signatures are uniquely positioned to offer the best chance at detection. Using narrow band photometric filters, we will be able to detect absorption signatures while the planet is in primary transit. A positive detection would be the first proof of water on an extrasolar planet. Furthermore, it would provide invaluable planetary information, constraining the entire chemistry. As a byproduct of the high SNR required for our primary science goal, we will be able to improve on the value of the planetary radius, a result independent of our primary science objective. The accurate radius estimate, together with planet structure models, will allow constraining the planet interior and its relationship with formation models and stellar metallicity.

Visits: 4 consisting of 4 HST orbits each. Two visits will be observed primary with the F187N filter while the other two will be done primary in the F166N filter. A set of observations at the begining of the 1st orbit, the middle of the 3rd orbit, and the end of the 4rth orbit, are to be done in the opposing filter. The exposure times for the two filters are 4 seconds with each orbit consisiting of repeated exposures. No dithering is to be done and a small amount of defocusing is to applied for each visit. Each exposure for all visits should be as close to identical as possible. STAR FORMATION 12 false 0.0 0 false false false false false AVAILABLE STAR K III-I J2000 20 00 43.7133 +22 42 39.07 J2000 NIC1 Imaging No No F166N NIC1 Imaging No No F187N Phase windows are not calculated when the period is less than 7.0 days. Assuming no scheduling restrictions for Phase 0.925/0.940. The scheduling data was generated by CASM 17.0. 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The third orbit should contain the central transit depth, with the constraints set to begin or end the third orbit science observations at that point. Phase windows are not calculated when the period is less than 7.0 days. Assuming no scheduling restrictions for Phase 0.925/0.940. The scheduling data was generated by CASM 17.0. CASM was run in Phase II mode. 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The third orbit should contain the central transit depth, with the constraints set to begin or end the third orbit science observations at that point. Phase windows are not calculated when the period is less than 7.0 days. Assuming no scheduling restrictions for Phase 0.925/0.940. The scheduling data was generated by CASM 17.0. 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The third orbit should contain the central transit depth, with the constraints set to begin or end the third orbit science observations at that point. Phase windows are not calculated when the period is less than 7.0 days. Assuming no scheduling restrictions for Phase 0.943/0.953. The scheduling data was generated by CASM 17.0. 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HOPR repeat of visit 3. 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Phase windows are not calculated when the period is less than 7.0 days. Assuming no scheduling restrictions for Phase 0.943/0.953. The scheduling data was generated by CASM 17.0. CASM was run in Phase II mode. 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Phase windows are not calculated when the period is less than 7.0 days. Assuming no scheduling restrictions for Phase 0.943/0.953. The scheduling data was generated by CASM 17.0. 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