0 Assigned ID: 1247 ----- Attempting Submission 1 (Thu Sep 29 12:10:15 GMT 2016) ----- HST Phase I Proposal 1247 (apt_55Cnc.apt) successfully submitted. Receipt: # 1247-2 ----- Attempting Submission 3 (Thu Sep 29 12:42:27 GMT 2016) ----- INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS Following the suggestions of our contact scientist, we have changed the acquisition settings to one single acquisition per visit. It now uses mirror A instead of mirror B, with an exposure time of 80s. 2010670535 ----- Attempting Submission 1 (Wed Dec 07 12:42:15 GMT 2016) ----- HST Phase II Proposal 14877 (apt_55cnc_FUV_II.apt) successfully submitted. Receipt: # 14877-1 ----- Attempting Submission 2 (Tue Dec 20 00:14:03 GMT 2016) ----- APT mentions an inefficient ordering of the FP-POS positions, although I have not changed their order compared to the previous submission wich did not issue this warning. The super-Earth 55 Cnc e transits an extremely bright star (V=6) at a very short separation (a=0.016 au). Transit spectroscopy of the planet in the ultraviolet detected no significant amounts of hydrogen or water, while optical and infrared observations suggest it could either have no atmosphere, or be surrounded by a heavyweight metal-rich envelope. Located within a carbon-rich system, 55 Cnc e might indeed be a 'Super-Venus' with a carbon-dioxyde atmosphere that could expand under the strong stellar irradiation. Our recent observation of the transit at far UV wavelengths with HST/COS may bring a new and decisive insight in favor of this scenario. Indeed, we detect a significant absorption signature of ionized carbon during and after the optical transit of 55 Cnc e. However, while this could represent the first clear detection of an exosphere around a super Earth, it relies on a single visit and previous experience demonstrates the importance of repeatability. Furthermore, a single visit is not enough to fully interpret the dynamics of the putative carbon exosphere. With two independent visits of five orbits each, a Mid-Cycle program is the perfect opportunity to assess the repeatability of this absorption, and characterize an envelope of carbon around 55 Cnc e. For the foreseeable future, the Hubble Space Telescope provides our only option to observe the transit of this super Earth at UV wavelengths, and indeed represents a unique possibility to characterize the atmosphere of this small planet, its composition, and its evolution. This program consists in 2 visits of 5 HST orbits each (total of 10 HST orbits), dedicated to the observations of the transits of the exoplanet 55 Cancri e in front of their host-star. The aim is to confirm a signature detected in the frame of Visit 2 in GO#14094, and this program will thus use the same instrumental settings. The scheduling will be slightly different however, because this new program has one more orbit per visit, and we need to obtain a good baseline by measuring the stellar flux farther from the planet transit. The transits of the targeted planet 55 Cancri 'e' occur every 17.7 hours and last for about 1.5 hours. The timing requirements for both visits are set as phase constraints on the first ACQ exposure of the first orbit. Extrasolar Planets and Planet Formation 3 false true false false false false SUPPORTED 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 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1291 /private/var/folders/33/rs56p2wx5q174bfyvvm_nq1m0000gn/T/OPVisit9051213657529005893.xml 1482192236610 Phase windows are not calculated when the gap between schedulable intervals is less than 1 days, assuming no scheduling restrictions for constraint Phase 0.737/0.754. The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 14877 :visit-id "01" :proposal-version -1 :trans-version "20160601" :date "20-Dec-2016 01:03:56.0" :trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 991808 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14877 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14877 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2649 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14877 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2771 :al-overhead-at-end 0 :internal-dur-at-end 86 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14877 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2771 :al-overhead-at-end 0 :internal-dur-at-end 86 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14877 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2771 :al-overhead-at-end 0 :internal-dur-at-end 86 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14877 :visit-id "01" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2771 :al-overhead-at-end 0 :internal-dur-at-end 379 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) true 5 0 We compared the counts for the brightest pixel in the acquisition image of GO#14094, and the value predicted for similar settings with the ETC but the GALEX magnitude (12.93 in NUV band). There is a ratio of about 7.5 between the actual count (lower) and the predicted count. Then, we used the ETC with the GALEX magnitude and mirror A to find that an exposure time of 80s is required to obtain a predicted count of 3230 for the brightest pixel, which should correspond to a true count of 430 and a SNR of 55 (assuming the ratio of 7.5 between the predicted and true counts) In the ETC run, the strength of the stellar Lyman-alpha line has been set to an extremely conservative value, and the airglow as set to its higher value, in order to calculate the buffer-time. We use the same settings as in Visit 2 of GO#14094, which was successfully obtained. In the ETC run, the strength of the stellar Lyman-alpha line has been set to an extremely conservative value, and the airglow as set to its higher value, in order to calculate the buffer-time. In the ETC run, the strength of the stellar Lyman-alpha line has been set to an extremely conservative value, and the airglow as set to its higher value, in order to calculate the buffer-time. In the ETC run, the strength of the stellar Lyman-alpha line has been set to an extremely conservative value, and the airglow as set to its higher value, in order to calculate the buffer-time. In the ETC run, the strength of the stellar Lyman-alpha line has been set to an extremely conservative value, and the airglow as set to its higher value, in order to calculate the buffer-time. /private/var/folders/33/rs56p2wx5q174bfyvvm_nq1m0000gn/T/OPVisit929089499149703573.xml 1482192245590 Phase windows are not calculated when the gap between schedulable intervals is less than 1 days, assuming no scheduling restrictions for constraint Phase 0.779/0.815. The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 14877 :visit-id "02" :proposal-version -1 :trans-version "20160601" :date "20-Dec-2016 01:04:05.0" :trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 991808 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14877 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14877 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2649 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14877 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2771 :al-overhead-at-end 0 :internal-dur-at-end 86 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14877 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2771 :al-overhead-at-end 0 :internal-dur-at-end 86 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14877 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2771 :al-overhead-at-end 0 :internal-dur-at-end 86 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14877 :visit-id "02" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2771 :al-overhead-at-end 0 :internal-dur-at-end 379 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2993 :pcs-gap 0 ) true 5 0 See visit #01 In the ETC run, the strength of the stellar Lyman-alpha line has been set to an extremely conservative value, and the airglow as set to its higher value, in order to calculate the buffer-time. We use the same settings as in Visit 2 of GO#14094, which was successfully obtained. In the ETC run, the strength of the stellar Lyman-alpha line has been set to an extremely conservative value, and the airglow as set to its higher value, in order to calculate the buffer-time. In the ETC run, the strength of the stellar Lyman-alpha line has been set to an extremely conservative value, and the airglow as set to its higher value, in order to calculate the buffer-time. In the ETC run, the strength of the stellar Lyman-alpha line has been set to an extremely conservative value, and the airglow as set to its higher value, in order to calculate the buffer-time. In the ETC run, the strength of the stellar Lyman-alpha line has been set to an extremely conservative value, and the airglow as set to its higher value, in order to calculate the buffer-time.