0 Assigned ID: 1038 ----- Attempting Submission 1 (Fri Apr 07 22:48:43 GMT 2017) ----- HST Phase I Proposal 1038 (HD80606b_-_UVIS_WFC3_Eclipe_and_Partial_Phase_Curve v2.apt) successfully submitted. Receipt: # 1038-1 ----- Attempting Submission 2 (Fri Apr 07 22:50:20 GMT 2017) ----- HST Phase I Proposal 1038 (HD80606b_-_UVIS_WFC3_Eclipe_and_Partial_Phase_Curve v2.apt) successfully submitted. Receipt: # 1038-2 ----- Attempting Submission 3 (Fri Apr 07 22:51:04 GMT 2017) ----- HST Phase I Proposal 1038 (HD80606b_-_UVIS_WFC3_Eclipe_and_Partial_Phase_Curve v2.apt) successfully submitted. Receipt: # 1038-3 ----- Attempting Submission 4 (Fri Apr 07 23:38:17 GMT 2017) ----- HST Phase I Proposal 1038 (HD80606b_-_UVIS_WFC3_Eclipe_and_Partial_Phase_Curve v2.apt) successfully submitted. Receipt: # 1038-4 ----- Attempting Submission 5 (Fri Apr 07 23:45:27 GMT 2017) ----- HST Phase I Proposal 1038 (HD80606b_-_UVIS_WFC3_Eclipe_and_Partial_Phase_Curve v2.apt) successfully submitted. Receipt: # 1038-5 ----- Attempting Submission 6 (Fri Apr 07 23:55:13 GMT 2017) ----- HST Phase I Proposal 1038 (HD80606b_-_UVIS_WFC3_Eclipe_and_Partial_Phase_Curve v2.apt) successfully submitted. Receipt: # 1038-6 ----- Attempting Submission 7 (Fri Apr 07 23:56:45 GMT 2017) ----- HST Phase I Proposal 1038 (HD80606b_-_UVIS_WFC3_Eclipe_and_Partial_Phase_Curve v2.apt) successfully submitted. Receipt: # 1038-7 ----- Attempting Submission 8 (Sat Apr 08 00:00:13 GMT 2017) ----- HST Phase I Proposal 1038 (HD80606b_-_UVIS_WFC3_Eclipe_and_Partial_Phase_Curve v2.apt) successfully submitted. Receipt: # 1038-8 ----- Attempting Submission 9 (Sat Apr 08 00:01:04 GMT 2017) ----- HST Phase I Proposal 1038 (HD80606b_-_UVIS_WFC3_Eclipe_and_Partial_Phase_Curve v2.apt) successfully submitted. Receipt: # 1038-9 ----- Attempting Submission 10 (Sat Apr 08 00:11:47 GMT 2017) ----- HST Phase I Proposal 1038 (HD80606b_-_UVIS_WFC3_Eclipe_and_Partial_Phase_Curve v2.apt) successfully submitted. Receipt: # 1038-10 ----- Attempting Submission 11 (Sat Apr 08 00:14:14 GMT 2017) ----- HST Phase I Proposal 1038 (HD80606b_-_UVIS_WFC3_Eclipe_and_Partial_Phase_Curve v2.apt) successfully submitted. Receipt: # 1038-11 ----- Attempting Submission 12 (Sat Apr 08 00:20:28 GMT 2017) ----- HST Phase I Proposal 1038 (HD80606b_-_UVIS_WFC3_Eclipe_and_Partial_Phase_Curve v2.apt) successfully submitted. Receipt: # 1038-12 ----- Attempting Submission 13 (Sat Apr 08 00:24:29 GMT 2017) ----- 0 Two decades after the discovery of 51 Peg b, the formation processes of short-period gas giants remain poorly understood. Hot Jupiters are predicted to have migrated inwards by means of several possible mechanisms, including the tidal dissipation of their orbital energy. The study of highly eccentric planets allows the quantification of the tidal dissipation efficiency of hot Jupiters, shedding light into the relevant timescales to understand the formation of close-in planets. The atmospheres of hot Jupiters also keep a part of mystery. Clouds seem ubiquitous, challenging our ability to retrieve molecular abundances from the observations. Phase curve observations allow us to map the cloud distribution on a planet, decipher their chemical composition and inform us about the conditions in the deep, usually unobservable layers of the planet. HD80606b is a hot Jupiter in a remarkable orbit. With an eccentricity of more than 0.9, it's atmosphere heats up by a thousand degrees in a few days during periastron passage. The planet is an extremely useful laboratory to understand both tidal dissipation and the response of the atmosphere to a time-dependent forcing. From current thermal phase curve observations we think that the planet is either poorly efficient at dissipating it's energy, or is covered by a thick cloud layer. Here we propose to break the degeneracies between the two scenarii by detecting the light reflected by the clouds during the periastron passage of the planet with WFC3/UVIS. This small HST program will also provide critical insights into the cloud formation and vertical mixing timescales that will be relevant for the study of hot Jupiters in general. This visit acquires time-series observations of HD 80606 for 15 consecutive orbits. Interruptions for SAA crossing will need to be scheduled at a later date. Each orbit uses WFC3/UVIS in scanning mode to spread the light across the detector. We scan at a rate of 1.412 arcsec/sec in both forward and reverse directions along AXIS1 (~X_POSTARG). The total length of the scan is 1695 pixels. To improve observation efficiency and avoid mid-orbit buffer dumps, we make use of a custom subarray (2500 x 350 pixels) centered at coordinates (1253, 176) relative to the origin, which is located in AMP C's corner (See Figure 6.1 of the WFC3 IHB). This subarray size also contains HD 80606's nearby companion when observing with an orient of 303 degrees (November 2018 visit). We select POSTARG values of (-75.92,-34.96) to start the scan near pixel (150,150), relative to the origin. The scan will end near pixel (1845,150). Because we are using a custom subarray, we must acquire bias frames at the end of the observation. The bias frames have the same dimension as the science frames. Planets and Planet Formation 6 false false false false false false false AVAILABLE STAR EXTRA-SOLAR PLANETARY SYSTEM G V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 K=7.316 WFC3/UVIS Imaging No No F350LP 1541082280545 The scheduling data was generated by CASM 26.0.5. CASM was run in Phase II mode. This visit acquires time-series observations of HD 80606 for 15 consecutive orbits. Interruptions for SAA crossing will need to be scheduled at a later date. Each orbit uses WFC3/UVIS in scanning mode to spread the light across the detector. We scan at a rate of 1.412 arcsec/sec in both forward and reverse directions along AXIS1 (~X_POSTARG). The total length of the scan is 1695 pixels. To improve observation efficiency and avoid mid-orbit buffer dumps, we make use of a custom subarray (2100 x 400 pixels) centered at coordinates (1053, 201) relative to the origin, which is located in AMP C's corner (See Figure 6.1 of the WFC3 IHB). We select POSTARG values of (-73.92,-32.96) to start the scan near pixel (200,200), relative to the origin. The scan will end near pixel (1895,200). Because we are using a custom subarray, we must acquire bias frames at the end of the observation. 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Interruptions for SAA crossing will need to be scheduled at a later date. Each orbit uses WFC3/UVIS in scanning mode to spread the light across the detector. We scan at a rate of 1.412 arcsec/sec in both forward and reverse directions along AXIS1 (~X_POSTARG). The total length of the scan is 1695 pixels. To improve observation efficiency and avoid mid-orbit buffer dumps, we make use of a custom subarray (2100 x 400 pixels) centered at coordinates (1053, 201) relative to the origin, which is located in AMP C's corner (See Figure 6.1 of the WFC3 IHB). We select POSTARG values of (-73.92,-32.96) to start the scan near pixel (200,200), relative to the origin. The scan will end near pixel (1895,200). Because we are using a custom subarray, we must acquire bias frames at the end of the observation. The bias frames have the same dimension as the science frames. 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