0 Assigned ID: 1142 ----- Attempting Submission 1 (Wed Feb 27 17:04:50 GMT 2013) ----- HST Phase I Proposal 1142 (BetaPic_COS_Cy21.apt) successfully submitted. ----- Attempting Submission 2 (Thu Feb 28 09:17:27 GMT 2013) ----- HST Phase I Proposal 1142 (BetaPic_COS_Cy21.apt) successfully submitted. ----- Attempting Submission 3 (Thu Feb 28 10:00:43 GMT 2013) ----- HST Phase I Proposal 1142 (BetaPic_COS_Cy21.apt) successfully submitted. ----- Attempting Submission 4 (Fri Mar 01 08:42:09 GMT 2013) ----- New version with the following changes: - ACQ/Search has been removed because the coordinate uncertainty is < 0.4" - Exposure time of acquisitions has been increased from 0.8 to 1.6 second to take care of uncertainties in the flux in the 1300-1430 Ang wavelength range. - The "auto-adjust" has NOT be used to keep the observation for the off-target offset position in orbit #1 as for the on-target in orbit #2 AT THE SAME ORBITAL POSITION, and to keep the total time below 54 minutes per orbit (and to allow a chedule in February 2014). - Phase constraints have been relaxed to allow a schedule in February 2014. 1158092424 ----- Attempting Submission 1 (Thu Jun 20 15:22:10 GMT 2013) ----- ----- Attempting Submission 2 (Tue Jan 14 17:01:07 GMT 2014) ----- The FP-Split order has been selected in order to observe with exactly the same FP-split position on the target during the 1st orbit, as off-the-target during the 2nd orbit at the same HST orbital phase. The Beta Pictoris system is a young planetary system (about 10 million years old), likely at the end of the telluric planets formation phases. It is embedded in a disk which is the prototype of debris disks where both gas and dust are continuously replenished via collision and evaporation of planetesimals and comet-like bodies. Because of its edge-on inclination, the gas component of the disk can be observed in great details through absorption spectroscopy. FUSE far UV observations allowed the discovery that the Beta Pictoris debris disk is extremely carbon rich. This unexpected carbon over-abundance is due to either a peculiar composition of the original protoplanetary system, to radiation forces blowing-out radiation-sensitives species, or to condensation/evaporation processes. Fortunately, hydrogen, deuterium and nitrogen are key volatiles sensitive to the radiation, condensation and evaporation processes. They can serve as diagnostics of the still puzzling gaseous disk history. Using COS far-UV capabilities, we propose to search for those species, which have up to now never been observed in this system. We will measure the HI, DI, and NI column density to trace the gas disk origin and provide constraints on its dynamics. The measurement of N/C ratio will also provide key information for the understanding of the observed carbon excess. These observations will bring new informations on the physical processes taking place in this active system during the last stages of the planet formation. In the first orbit, we will observe using the G130M/1291A setup with the target Beta Pictoris centered in the aperture. The second orbit will be used to obtain a T-Tag image of the Lyman-alpha airglow contamination by observing off-target (1 arcmin), just one orbit after the first orbit. The exposures have been ajusted to obtain the same exposures (same FP-Split positions) for the off-target offset position as for the on-target AT THE SAME ORBITAL POSITION OF THE TELESCOPE to correctly map the airglow contamination. A single on-target (FP-Split position=1) is required at the beginning of orbit #2 : - (1) to obtain the off-target exposures of orbit #2 at the same telescope's orbital position as for the on-target exposures of orbit #1 - (2) obtain additional science exposure on the target Beta Pictoris is at opposition near December 15. The observations should be scheduled close to the opposition in order to reduce the Airglow contamination. In that purpose, we used the time constraints defined by the Period (365.25 days), Zero Phase (2456658.5 = 1 Jan 2014) and Phase Constraints of the 1st exposure (Phase 0.833 = 1 Nov to 0.165 = 28 Feb) for the observations to be scheduled within 2.5 months from opposition. The "auto-adjust" has not be used to keep the observation for the off-target offset position as for the on-target AT THE SAME ORBITAL POSITION, and to keep the total time below 54 minutes per orbit (and to schedulable in February 2014). DEBRIS DISKS 12 false true 0.0 0.0 false false false SUPPORTED CALIBRATION UNDESIGNATED This is a background direction to measure the geocoronal airglow, off the science target. V -magnitude is arbitrarily set to 20 (required for "Bright Object Sensitive Detectors") J2000 ~5e-13 erg /s/cm2/A at 1216A (Earth airglow at Lyman-alpha) STAR A4-A9 V-IV CIRCUMSTELLAR MATTER DISK This object was generated by the targetselector and retrieved from the SIMBAD database. Target Coordinates and proper motion are from Hipparcos, the New Reduction (van Leeuwen, 2007) J2000 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1291 /solaris/user1/aroman/work/OP-cache/13406-v01.xml 1389720296566 The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. 54 (Tic-Visit :proposal-id 13406 :visit-id "01" :proposal-version -1 :trans-version "20131031" :date "14-Jan-2014 12:24:55.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 800208 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13406 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13406 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2895 :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 3240.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13406 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3006 :al-overhead-at-end 0 :internal-dur-at-end 442 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3240.0 :pcs-gap 0 ) false 2 0 In the ETC run, the strength of the Stellar Lyman-alpha line has been set to an extremely conservative upper limit to calculate the Buffer-time and check the Bright Object Limit (FWHM=2 Angstrom., Flux=4e-12).