0 Assigned ID: 486 ----- Attempting Submission 1 (Fri Apr 07 11:47:48 GMT 2017) ----- HST Phase I Proposal 486 (HIP116_HST_25.apt) successfully submitted. Receipt: # 486-1 ----- Attempting Submission 2 (Fri Apr 07 11:49:10 GMT 2017) ----- HST Phase I Proposal 486 (HIP116_HST_25.apt) successfully submitted. Receipt: # 486-2 ----- Attempting Submission 3 (Fri Apr 07 13:13:38 GMT 2017) ----- The slit was uncorrectly set to 52x0.1 instead of 52x0.1D1 in Visit 2 / exposure 9. -33101066 ----- Attempting Submission 1 (Fri Jul 07 13:58:38 GMT 2017) ----- ----- Attempting Submission 2 (Tue Aug 01 19:25:49 GMT 2017) ----- The super-Earth HIP116454b was the first exoplanet detected by the K2 mission, in transit across a bright and nearby K1 dwarf (V=10.2, d=55 pc). The low density of the planet suggests it must have at least 30% water or a 0.5% H-He envelope. Given the strong XUV irradiation from the young (2 Gyr) host star, this H-He envelope should have been lost through evaporation in a few hundred millions year, suggesting that HIP 116454b likely contains a large mass fraction of water. The shallow transit depth makes difficult the search for water vapor in the lower atmosphere with HST/WFC3. The moderate orbital distance of this warm (~700 K) planet favors the formation of a super-critical steam envelope, which should be promptly dissociated at high altitude by the XUV irradiation and become observable as hydrogen flowing within and beyond the Roche lobe. The host star is similar to HD 189733, host to an evaporating hot Jupiter, and numerical simulations of HIP116454b show that the hydrogen exosphere resulting from the dissociation of water is observable with HST/STIS at Ly-alpha. The detection of this exosphere would be the first signature of an evolved evaporating ocean on an extrasolar planet, as well as the first validation of internal structure models of exoplanets in this mass regime. It would also determine how to best search for water in the lower atmosphere of HIP116454b with the JWST. A non-detection of escaping hydrogen, as with 55 Cnc e and HD 97658b, would bring useful constraints on the nature of the planetary atmosphere, the evolutionary path of close-in super-Earths, and the progenitors of the rocky evaporation remnants detected by Kepler. This program consists in 3 visits of 5 HST orbits each. In each visit, we will observe the transit of an exoplanet (HIP116454b) in front of its host star. Transits occur every 9.12 days (the orbital period of the planet) and last for 2.25 hours. The goal is to search for a hydrogen exosphere surrounding the planet and occulting the star at Lyman-alpha. The timing requirements are set as phase constraints on the first ACQ exposure of the first orbit in a visit, with allowed start phase range between 19-26 min depending on the visit. We schedule the three visits so that there are always two HST orbits falling within the planet transit. Phase constraints are shifted from visit #1 to #3 so that visit #1 also covers the phase range before the transit, visit #2 before and after the transit, and visit #3 after the transit. This is because the transit of the putative exosphere can begin earlier, and end later, than the planet transit. We set a BETWEEN constraint for all visits between April, 1st 2018 and October, 1st 2018 to optimize airglow contamination in intensity and radial velocity. It would be best for our science goals if the three visits could be scheduled as close as possible to the end of this window. We moved the AUTO-WAVECAL to GO-WAVECAL done during Earth occultation. Planets and Planet Formation 6 false false true false false false false SUPPORTED STAR EXTRA-SOLAR PLANET K III-I NO All target properties come from the SIMBAD database. The star has Hipparcos astrometric coordinates (HIP 116454). We used the confirmation charts to check that the coordinates and proper motion were correct. J2000 J2000 B 11.08; R 9.71; I 9.25; J 8.604 ; H 8.140 ; K 8.029 STIS/FUV-MAMA Spectroscopic No No G140M 1222 1501615359299 The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. We set a BETWEEN constraint to optimize airglow contamination in intensity and radial velocity (Tic-Visit :proposal-id 15127 :visit-id "01" :proposal-version -1 :trans-version "20170613" :date "01-Aug-2017 21:22:38.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1062048 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15127 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15127 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2645 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15127 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2756 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15127 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2756 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15127 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2756 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15127 :visit-id "01" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2756 :al-overhead-at-end 0 :internal-dur-at-end 622 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) false 5 0 The target is too bright for the longpass filter, and the F28X50OII was selected instead. Time to reach signal to noise ratio of 40 is estimated at 1.8s, with time to saturation 187s. We set exposure time to 5s. 10s allows to reach over S/N=70 with STIS/CCD/G430L at 4300 Angstroms, and is well below the time to saturation (200s). The Spectroscopic ETC yields a warning about the issue with charge transfer efficiency for low background, but we are just using the CCD for the target acquisition, after which we switch to the MAMA. We are basically photon-starved and set the exposure time to the maximum possible value. The star is a near twin of HD189733 (see above ETC run) and HD97658, observed with the same settings in previous programs, except that it is farther away and fainter. We thus expect lower count rates, and can define the buffer-time as Texp/2 for the orbits of all visits. 1501615362363 The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. We set a BETWEEN constraint to optimize airglow contamination in intensity and radial velocity 1527482431000 247.56737527237084 (Tic-Visit :proposal-id 15127 :visit-id "02" :proposal-version -1 :trans-version "20170613" :date "01-Aug-2017 21:22:41.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1062048 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15127 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15127 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2645 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15127 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2756 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15127 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2756 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15127 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2756 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15127 :visit-id "02" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2756 :al-overhead-at-end 0 :internal-dur-at-end 622 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) false 5 0 The target is too bright for the longpass filter, and the F28X50OII was selected instead. Time to reach signal to noise ratio of 40 is estimated at 1.8s, with time to saturation 187s. We set exposure time to 5s. 10s allows to reach over S/N=70 with STIS/CCD/G430L at 4300 Angstroms, and is well below the time to saturation (200s). The Spectroscopic ETC yields a warning about the issue with charge transfer efficiency for low background, but we are just using the CCD for the target acquisition, after which we switch to the MAMA. We are basically photon-starved and set the exposure time to the maximum possible value. The star is a near twin of HD189733 (see above ETC run) and HD97658, observed with the same settings in previous programs, except that it is farther away and fainter. We thus expect lower count rates, and can define the buffer-time as Texp/2 for the orbits of all visits. 1501615365472 The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. We set a BETWEEN constraint to optimize airglow contamination in intensity and radial velocity (Tic-Visit :proposal-id 15127 :visit-id "03" :proposal-version -1 :trans-version "20170613" :date "01-Aug-2017 21:22:44.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1062048 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15127 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15127 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2645 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15127 :visit-id "03" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2756 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15127 :visit-id "03" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2756 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15127 :visit-id "03" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2756 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15127 :visit-id "03" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2756 :al-overhead-at-end 0 :internal-dur-at-end 622 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2978 :pcs-gap 0 ) false 5 0 The target is too bright for the longpass filter, and the F28X50OII was selected instead. Time to reach signal to noise ratio of 40 is estimated at 1.8s, with time to saturation 187s. We set exposure time to 5s. 10s allows to reach over S/N=70 with STIS/CCD/G430L at 4300 Angstroms, and is well below the time to saturation (200s). The Spectroscopic ETC yields a warning about the issue with charge transfer efficiency for low background, but we are just using the CCD for the target acquisition, after which we switch to the MAMA. We are basically photon-starved and set the exposure time to the maximum possible value. The star is a near twin of HD189733 (see above ETC run) and HD97658, observed with the same settings in previous programs, except that it is farther away and fainter. We thus expect lower count rates, and can define the buffer-time as Texp/2 for the orbits of all visits.