0 Assigned ID: 1319 ----- Attempting Submission 1 (Thu Jan 26 08:06:13 GMT 2017) ----- Following approval by the STScI, we removed the AUTO-WAVECAL exposures and replaced them by GO-WAVECAL exposures at the end of the science exposures. 1337530795 ----- Attempting Submission 1 (Wed Mar 15 10:33:36 GMT 2017) ----- What is the origin of the UV-absorbing cloud orbiting the iconic star 55 Cnc ? The super-Earth 55 Cnc e transits an extremely bright star (V=6) at a very short separation (P=18 hours). Optical and infrared observations suggest it could be surrounded by a heavyweight atmosphere. Heated to more than 2000 K, the planet surface could indeed be covered by magma oceans that would outgas large amounts of dust and metals, prone to escape. Our recent observations of the transit with HST/STIS at near-UV wavelengths revealed a deep absorption, repeatable over two visits, that could be produced by an extended cloud much larger than the planet. Surprisingly, this absorption occurs before the planet transit, raising the question of whether or not it originates from the planet. Earth occultation prevented the HST from observing the full duration of the occultation produced by the putative cloud. With two independent visits of five orbits each, a Mid-Cycle program is the perfect opportunity to assess the repeatability of the occultation and to complete our phase coverage, thus probing the full extension of the cloud. Its signature was not detected at optical/infrared wavelengths, and the unique UV capabilities of HST provide our only option to characterize the mysterious UV-absorbing cloud present in the 55 Cnc system. This program consists in 2 visits of 5 HST orbits each (total 10 HST orbits), dedicated to the observations of a transiting object in the 55 Cnc system. This object has the same orbital period as the super-Earth 55 Cnc e, but transits about 2.5h earlier. The transit of this object was observed in two different epochs in GO program #14094 (visits #1 and #3). Both visits in our current program aim at completing our coverage of the transit event, and will thus use the same settings as in program #14094 but with different phase constraints. Visits are scheduled so that the transit of the object occurs during the third orbit. The timing requirements are set as phase constraints on the first ACQ exposure of the first orbit in a visit. Because we need to observe the transit in the specific phase window that was not covered in previous HST observations, our phase constraints are relatively stringent and the allowed start phase range is ~15 min. Ideally the two visits should be scheduled close from one another, to observe the transiting object in similar conditions. However we would also like to request, if possible, that the interval between the two visits is long enough that we can can change the scheduling of the second visit based on the results of the first visit, if necessary. Extrasolar Planets and Planet Formation 3 false true false false false false AVAILABLE STAR EXTRA-SOLAR PLANETARY SYSTEM G V-IV NO This star is in a double system (common proper motions) with 55 Cancri B (GJ 324B), a much fainter (V=13) M4 dwarf that is 1.4-arcmin away. It also 4.6-arcmin away from the similarly bright (V=6.3) star 53 Cancri (BO Cancri). HR3522 GJ324A J2000 J2000 U=7.45, B=6.82, R=5.4, I=5.0, J=4.59, H=4.14, K=4.015 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 2707 /private/var/folders/33/rs56p2wx5q174bfyvvm_nq1m0000gn/T/OPVisit536778781690557542.xml Phase windows are not calculated when the gap between schedulable intervals is less than 1 days, assuming no scheduling restrictions for constraint Phase 0.630/0.645. The scheduling data was generated by CASM 25.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 14917 :visit-id "01" :proposal-version -1 :trans-version "20170109" :date "15-Mar-2017 10:31:58.0" :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 2804048 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14917 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14917 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2657 :al-overhead-at-end 81 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14917 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2766 :al-overhead-at-end 81 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14917 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2766 :al-overhead-at-end 81 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14917 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2766 :al-overhead-at-end 81 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14917 :visit-id "01" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2766 :al-overhead-at-end 81 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) true 5 0 For the ACQ and ACQ/PEAK exposures, we selected the same settings as in Program #14094 which consisted of STIS observations of the same star with the same settings (Visits #1 and #3). The count-rate estimated in time-tag mode results in too many buffer dumps. As an alternative for our scientific purpose, we use instead a series of ACCUM mode exposures with the optimal combination between time resolution, SNR, and buffer dumps. This the same strategy that was used in program #14094 (visits #1 and #3) /private/var/folders/33/rs56p2wx5q174bfyvvm_nq1m0000gn/T/OPVisit1923191477227964418.xml Phase windows are not calculated when the gap between schedulable intervals is less than 1 days, assuming no scheduling restrictions for constraint Phase 0.650/0.665. The scheduling data was generated by CASM 25.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 14917 :visit-id "02" :proposal-version -1 :trans-version "20170109" :date "15-Mar-2017 11:33:03.0" :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 2804048 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14917 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14917 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2657 :al-overhead-at-end 81 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14917 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2766 :al-overhead-at-end 81 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14917 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2766 :al-overhead-at-end 81 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14917 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2766 :al-overhead-at-end 81 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14917 :visit-id "02" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2766 :al-overhead-at-end 81 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) true 5 0 For the ACQ and ACQ/PEAK exposures, we selected the same settings as in Program #14094 which consisted of STIS observations of the same star with the same settings (Visits #1 and #3). The count-rate estimated in time-tag mode results in too many buffer dumps. As an alternative for our scientific purpose, we use instead a series of ACCUM mode exposures with the optimal combination between time resolution, SNR, and buffer dumps. This the same strategy that was used in program #14094 (visits #1 and #3) The count-rate estimated in time-tag mode results in too many buffer dumps. As an alternative for our scientific purpose, we use instead a series of ACCUM mode exposures with the same time resolution as the one we usually use our time-tag data. The count-rate estimated in time-tag mode results in too many buffer dumps. As an alternative for our scientific purpose, we use instead a series of ACCUM mode exposures with the same time resolution as the one we usually use our time-tag data. The count-rate estimated in time-tag mode results in too many buffer dumps. As an alternative for our scientific purpose, we use instead a series of ACCUM mode exposures with the same time resolution as the one we usually use our time-tag data.