Observing the beta Pic Hill Sphere Transit in the far-UV

0 Assigned ID: 1515 ----- Attempting Submission 1 (Tue Sep 19 14:28:05 GMT 2017) ----- Please could Dr. Alain Lecavelier des Etangs and Dr. Alfred Vial-Madjar be added as Co-Pi's? I selected this in the phase 1 of the proposal, but now it seems they are only Co-I's and not Co-PI's. Thank you! 1036690106 ----- Attempting Submission 1 (Wed Sep 27 08:14:37 GMT 2017) ----- Your proposal could not be saved. Submission aborted. ----- Attempting Submission 2 (Wed Sep 27 16:57:36 GMT 2017) ----- These exact phase 2 instructions have been safely executed before in program #14894. I chose to turn on proper motion in BOT to resolve the conflict, but it did not work this time either. I hope the PM parameters are now still the same as they were in #14894. Could this be checked? Kind Regards, Dr. Paul A. Wilson (PI) Observing 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 the Cycle 24 HST/COS observations of 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. We propose to monitor the second half of the Hill sphere transit, which will take place in October-November 2017, 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 20 years. The aims for this proposal are to 1) probe the shape and the dynamics of the gas in the Hill sphere 2) continue to probe the composition of the gas in the Hill sphere, and 3) Track the compositional variations as a function of Hill sphere radius. 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 0 AVAILABLE STAR A4-A9 V-IV CIRCUMSTELLAR MATTER DISK EXTRA-SOLAR PLANET NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1291 1506499585744 Timing link suitability includes constraints ([02 After 01 by 30.0 to 80.0 days]) 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 1508517775000 305.5230127269312 (Tic-Visit :proposal-id 15396 :visit-id "01" :proposal-version -1 :trans-version "20170613" :date "27-Sep-2017 10:06:25.0" :trans-errors '(:WARNINGS 16 :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 1948208 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15396 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15396 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2712 :al-overhead-at-end 0 :internal-dur-at-end 95 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3046 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15396 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2816 :al-overhead-at-end 0 :internal-dur-at-end 133 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3046 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15396 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2816 :al-overhead-at-end 0 :internal-dur-at-end 426 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3046 :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). 1506499578170 Timing link suitability includes constraints ([02 After 01 by 30.0 to 80.0 days]) 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 15396 :visit-id "02" :proposal-version -1 :trans-version "20170613" :date "27-Sep-2017 10:06:18.0" :trans-errors '(:WARNINGS 16 :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 1948208 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15396 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15396 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2712 :al-overhead-at-end 0 :internal-dur-at-end 95 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3046 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15396 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2816 :al-overhead-at-end 0 :internal-dur-at-end 133 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3046 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15396 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2816 :al-overhead-at-end 0 :internal-dur-at-end 426 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3046 :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).