0 Assigned ID: 1536 ----- Attempting Submission 1 (Fri Sep 29 18:03:13 GMT 2017) ----- HST Phase I Proposal 1536 (HillTransit_mid-cycle.apt) successfully submitted. Receipt: # 1536-1 ----- Attempting Submission 2 (Sat Sep 30 18:33:31 GMT 2017) ----- Removed NUM-POS keyword from PEAKXD which allows me to select LP4/1291 without hvaing to enable "Allow restricted" ===== Enabled "Allowed restricted" to be able to select LP4 for PEAKXD observations ===== I have updated the PEAKD observations to be done at LP4/1291. I need to change the PEAKXD to do the same but can't change it away from LP3/1327. Help is needed here. ===== I have requested the old LP3 setting to be used so that the instrument setup remains exactly the same as previous observations such as #14089 and #14894 and #15396. This was requested in the accepted mid-term proposal. 1619300574 ----- Attempting Submission 1 (Tue Dec 12 14:07:20 GMT 2017) ----- HST Phase II Proposal 15412 (HillTransitMidTerm.apt) successfully submitted. Receipt: # 15412-1 ----- Attempting Submission 2 (Sat Dec 30 19:37:24 GMT 2017) ----- ----- Attempting Submission 3 (Wed Jan 03 18:59:26 GMT 2018) ----- ----- Attempting Submission 4 (Thu Jan 04 09:52:05 GMT 2018) ----- These messages were also shown during the last four phase 2 submissions. Please let me know if something needs doing there. Observing the final part of the beta Pic Hill Sphere Transit in the far-UV The Hill sphere of the directly-imaged planet Beta Pic b is currently transiting its host-star, Beta Pic. During this event, material in the Hill sphere (e.g. left-over debris from planet formation, rings, gas torus around satellites, etc.) could transit the star. With Cycle 24 HST/COS observations which probed the first half of the Hill sphere transit from April to August 2017, we detected a significant flux decrease in the blue and red wings of the HI Ly-alpha emission line and the 1334.53 CII absorption line. This is consistent with the first ever detection of an extended envelope of hydrogen and carbon surrounding Beta Pic b. With the upcoming Director's Discretionary Program #15396 we will observe the second half of the Hill sphere transit. We propose to monitor the final part of the Hill sphere transit (the expected trailing Hill sphere gas) and post-transit baseline (for Hill sphere transit verification), using the same instrument setup and observation strategy. As with the previous 2017 observations, we will again use the "Airglow Virtual Motion" technique, which is an extremely powerful technique to observe Lyman-alpha with COS. This is a very unique opportunity to monitor the transit of the environment of a ~20 million years old young planet that has been directly imaged orbiting a 4th magnitude star; the next such transit will not happen again for another 22 years. The aims for this proposal are to 1) obtain a post-transit baseline for transit verification 2) probe the shape and the dynamics of the gas trailing the Hill sphere, and 3) probe the composition of the gas trailing the Hill sphere. We have a total of two visits scheduled. Each visit consists of three orbits. Each visit has an identical observing strategy. For each visit: Orbit 1: Observe target centered in the aperture Orbit 2: The target (Beta Pictoris) is to be offset -1.1 arcseconds in the dispersion direction Orbit 3: The target (Beta Pictoris) is to be offset +1.1 arcseconds in the dispersion direction The 1.1 arcsecond offsets shifts are important for the detection of hydrogen, nitrogen and oxygen which are all affected by airglow contamination. An increase in the off-axis target distance along the dispersion axis effectively shifts the line emission feature in wavelength relative to the airglow emission. Planets and Planet Formation 6 false true false false false false AVAILABLE STAR A4-A9 V-IV CIRCUMSTELLAR MATTER DISK EXTRA-SOLAR PLANET NO J2000 J2000 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1291 The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. Orbit 1: Observe target centered in the aperture Orbit 2: The target (Beta Pictoris) is to be offset -1.1 arcseconds in the dispersion direction Orbit 3: The target (Beta Pictoris) is to be offset +1.1 arcseconds in the dispersion direction (Tic-Visit :proposal-id 15412 :visit-id "01" :proposal-version -1 :trans-version "20171009" :date "03-Jan-2018 19:56:49.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 2296128 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15412 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15412 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3037 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3393 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15412 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3167 :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 3393 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15412 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3167 :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 3393 :pcs-gap 0 ) false 3 0 The strength of the Stellar Lyman-alpha line has been set to an conservative upper limit to calculate the Buffer-time and check the Bright Objects Limit (FWHM=5 Angstrom, Flux=1e-11). The strength of the Stellar Lyman-alpha line has been set to an conservative upper limit to calculate the Buffer-time and check the Bright Objects Limit (FWHM=5 Angstrom, Flux=1e-11). The strength of the Stellar Lyman-alpha line has been set to an conservative upper limit to calculate the Buffer-time and check the Bright Objects Limit (FWHM=5 Angstrom, Flux=1e-11). The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. Orbit 1: Observe target centered in the aperture Orbit 2: The target (Beta Pictoris) is to be offset -1.1 arcseconds in the dispersion direction Orbit 3: The target (Beta Pictoris) is to be offset +1.1 arcseconds in the dispersion direction (Tic-Visit :proposal-id 15412 :visit-id "02" :proposal-version -1 :trans-version "20171009" :date "03-Jan-2018 19:57:04.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 2296128 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15412 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15412 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3037 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3393 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15412 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3167 :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 3393 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15412 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3167 :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 3393 :pcs-gap 0 ) false 3 0 The strength of the Stellar Lyman-alpha line has been set to an conservative upper limit to calculate the Buffer-time and check the Bright Objects Limit (FWHM=5 Angstrom, Flux=1e-11). The strength of the Stellar Lyman-alpha line has been set to an conservative upper limit to calculate the Buffer-time and check the Bright Objects Limit (FWHM=5 Angstrom, Flux=1e-11). The strength of the Stellar Lyman-alpha line has been set to an conservative upper limit to calculate the Buffer-time and check the Bright Objects Limit (FWHM=5 Angstrom, Flux=1e-11).