Observing the Beta Pic Hill sphere transit in the far-UV

0 Assigned ID: 1285 ----- Attempting Submission 1 (Fri Sep 30 23:11:15 GMT 2016) ----- ----- Attempting Submission 2 (Mon Nov 21 14:52:44 GMT 2016) ----- INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS In orbit 2 of visit 1 we perform an offset of -1.25 arcseconds compared to the standard -1.1 arcseconds. This is to test the effectiveness of the newly developed AVM technique (Wilson et al. 2016). This offset will allow us to better understand the AVM technique's abilibity to separate the stellar Ly-alpha signal away from contaminating airglow. ===== We previously stated we wished to observe with a -2.0 arcsecond offeset for Visit 1, Orbit 2. After careful consideration, we realise this will not help our observations due to the diameter of the COS aperture being 2.5 arcsec. We have thus changed the shift back to -1.1 which was the original plan and which was stated in the original proposal. ===== We changed the central wavelength position from 1291 AA to 1327 AA as this increases the number of absorption lines towards longer wavelengths including the valuable CO lines. Previous observations through program 14089 showed that the flux towards shorter wavelengths (using a central wavelength position of 1291 AA) is of very little use to due the low flux. Please can you confirm the timing is correct: What we want is the following visit windows. Visit 1: 21. April - 8. May Visit 2: 9. Juni - 2. July Visit 3: 3. Aug - 15. Aug 62276401 ----- Attempting Submission 1 (Thu Dec 15 15:31:00 GMT 2016) ----- HST Phase II Proposal 14894 (hill_sphere_phase2.apt) successfully submitted. Receipt: # 14894-1 ----- Attempting Submission 2 (Thu Dec 15 15:41:49 GMT 2016) ----- HST Phase II Proposal 14894 (hill_sphere_phase2.apt) successfully submitted. Receipt: # 14894-2 ----- Attempting Submission 3 (Sun Dec 18 09:42:45 GMT 2016) ----- HST Phase II Proposal 14894 (hill_sphere_phase2_2.apt) successfully submitted. Receipt: # 14894-3 ----- Attempting Submission 4 (Mon Dec 19 14:58:54 GMT 2016) ----- The APT warning is raised because we are doing FP=1, 2, 3, 4 several times with no cenwave change in between (just a POS-TARG). The issue was raised and a reply from Julia Duval informs us that this is not something which will cause any problems. We had no BPT problems last time we conducted very similar observations with program 14089. Is the BOT warnings a real problem? Observing the Beta Pic Hill sphere transit in the far-UV Starting in April 2017, the Hill sphere of the directly-imaged planet Beta Pic b will start to transit 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. Photometric data from 1981, during a previous event, shows a potential transit signature. Using an accurate transit ephemeris that was just recently calculated, we can predict the exact dates of the upcoming passage. We propose to monitor this transit event using HST and the COS instrument over three visits. This is a very unique opportunity to monitor the transit of the environment of a ~20 million years old young planet that has been imaged in front of a 4th magnitude star; the next such transit will not happen again for another 20 years. The aims for this proposal are to 1) directly detect the composition of the gas in the Hill Sphere of a young planet 2) track the compositional variations as a function of the Hill Sphere radius 3) monitor temporal variations in the circumstellar dust and gas disk before and during the transit, and 4) determine the composition of exocomets present in the Beta Pic system which is independent of the transit of the Hill sphere. We have a total of three visits scheduled. Each visit consists of three orbits. Each visit has an identical observing strategies. 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. Extrasolar Planets and Planet Formation Extrasolar Planets and Planet Formation 6 false true false false false false AVAILABLE STAR A4-A9 V-IV CIRCUMSTELLAR MATTER DISK 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 1482159318520 Timing link suitability includes constraints ([02 After 01]) The scheduling data was generated by CASM 24.2. 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 -1.25 arcseconds in the dispersion direction Orbit 3: The target (Beta Pictoris) is to be offset +1.1 arcseconds in the dispersion direction In orbit 2 we perform an offset of -1.25 arcseconds compared to the standard -1.1 arcseconds. This is to test the effectiveness of the newly developed AVM technique (Wilson et al. 2016). This offset will allow us to better understand the AVM technique's abilibity to separate the stellar Ly-alpha signal away from contaminating airglow. 1492903198000 128.9724014677111 (Tic-Visit :proposal-id 14894 :visit-id "01" :proposal-version -1 :trans-version "20160601" :date "19-Dec-2016 15:55:17.0" :trans-errors '(:WARNINGS 10 :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 2330944 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14894 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14894 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3068 :al-overhead-at-end 0 :internal-dur-at-end 124 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3403 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14894 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3179 :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 3403 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14894 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3179 :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 3403 :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). 1481816476147 Timing link suitability includes constraints ([02 After 01] [03 After 02]) The scheduling data was generated by CASM 24.2. 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 1497124117000 172.53029429837238 (Tic-Visit :proposal-id 14894 :visit-id "02" :proposal-version -1 :trans-version "20160601" :date "15-Dec-2016 16:41:15.0" :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 2330944 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14894 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14894 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3068 :al-overhead-at-end 0 :internal-dur-at-end 124 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3403 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14894 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3179 :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 3403 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14894 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3179 :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 3403 :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). 1481816478761 Timing link suitability includes constraints ([03 After 02]) The scheduling data was generated by CASM 24.2. 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 14894 :visit-id "03" :proposal-version -1 :trans-version "20160601" :date "15-Dec-2016 16:41:18.0" :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 2330944 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14894 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14894 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3068 :al-overhead-at-end 0 :internal-dur-at-end 124 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3403 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14894 :visit-id "03" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3179 :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 3403 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14894 :visit-id "03" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3179 :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 3403 :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).