0 Assigned ID: 777 ----- Attempting Submission 1 (Fri Apr 11 20:37:46 GMT 2014) ----- HST Phase I Proposal 777 (BlazarsCosmicRays_Cycle22.apt) successfully submitted. For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting. Only minor typo changes in second submission. Dr. Roger Blandford is now the Admin PI for this program, not Dr. Greg Madejski. 264425272 ----- Attempting Submission 1 (Fri Jul 18 22:27:56 GMT 2014) ----- HST Phase II Proposal 13651 (BlazarsCosmicRays_Cycle22.apt) successfully submitted. ----- Attempting Submission 2 (Mon Jul 21 17:51:06 GMT 2014) ----- The 15A gap from ~1280 to 1295 angstroms is acceptable. Three of the four FP-POS positions will be sufficient to account for detector imperfections. Blazars have been postulated as possible progenitors of ultra-high-energy cosmic rays (UHECRs; E>1 PeV) for decades. This is particularly compelling in the case of blazars observed as TeV gamma-ray sources, since acceleration of particles to extreme energies must take place there. Unfortunately, convincing evidence supporting this theory has yet to be collected, mainly due to lack of firm measurements of blazar distances. Leveraging a novel technique that we successfully used to robustly pin-down redshifts in four blazars via absorption spectroscopy, we propose HST/COS observations of B2 1215+30, a blazar with the unique potential to address the validity of blazars as acceleration sources of UHECRs. These observations will provide firm limits on the distance to B2 1215+30, which will be used in conjunction with archival observations in the very high energy (VHE; E>100 GeV) band to enable a detailed study of the interaction of UHECRs with the lower-energy extragalactic photon fields along the line of sight between B2 1215+30 and the Earth. The seven orbits granted will comprise of a single visit with initial target acquisition followed by three G130M target exposures (FP_POS positions 1, 2 and 3, respectively) and four G160M target exposures (FP_POS positions 1, 2, 3, 4, respectively). The target acquisition involves a 45 second PEAKXD exposure followed by a series of five 60 second PEAKD exposures with 0.9 arcsecond steps, each onto the G130M grating at 1291 angstroms. The first target exposure will immediately follow the target acquisition and cover the remainder of the first orbit (1940 in FP_POS 1). The fourth through ninth target exposures will use the remaining 6 orbits. --------- Additional Comments ---------- This target is a variable target, found to vary by +/- an optical magnitude in the R-band (http://users.utu.fi/kani/1m/ON_325.html). In order to ensure that our measurement will be successful independent of state, we have calculated the proposed observing plan assuming the target is in the faintest state (FUV ~18.5 magnitude). With the safety of the instrument in mind, a check was made on the proposed target acquisition exposures on the chance that the target will be in the brightest state during observations (FUV~16.5). The exposures requested are found to produce no instrumental risk (see below for ETC run numbers). This visit sequence is requested independent of the source magnitude at time of observation. Exposure Time Calculator run with FUV magnitude of 16.5: Exposure 1 ETC Run #: 620592 Exposure 2 ETC Run #: 620593 Exposure 3 ETC Run #: 620594 Exposure 4 ETC Run #: 620595 Exposure 5 ETC Run #: 620595 Exposure 6 ETC Run #: 620596 Exposure 7 ETC Run #: 620596 Exposure 8 ETC Run #: 620596 Exposure 9 ETC Run #:620596 AGN/QUASARS Default false true false false false SUPPORTED GALAXY BL LAC LYMAN ALPHA CLOUD 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 G160M 1611 1412881705590 /private/var/folders/bl/s7q0tqnn5gbcbyvcfnrhj2rh0004nc/T/OPVisit3726572591082094042.xml The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. This target is a variable target, found to vary by +/- an optical magnitude in the R-band (http://users.utu.fi/kani/1m/ON_325.html). In order to ensure that our measurement will be successful independent of state, we have alculated the proposed observing plan assuming the target is in the faintest state (FUV ~18.5 magnitude). With the safety of the instrument in mind, a check was made on the proposed target acquisition exposures on the chance that the target will be in the brightest state during observations (FUV~16.5). The exposures requested are found to produce no instrumental risk (see below for ETC run numbers). This visit sequence is requested independent of the source magnitude at time of observation. Exposure Time Calculator with FUV magnitude of 16.5: Exposure 1 ETC Run #: 622524 Exposure 2 ETC Run #: 622525 (Tic-Visit :proposal-id 13651 :visit-id "01" :proposal-version -1 :trans-version "20140605" :date "09-Oct-2014 15:08:24.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 7 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 756864 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13651 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13651 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2667 :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 3000 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13651 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2778 :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 3000 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13651 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2778 :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 3000 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13651 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2778 :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 3000 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13651 :visit-id "01" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2778 :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 3000 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13651 :visit-id "01" :orbit-number 6 :pcs-time 222 :si-vis-utilization 2778 :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 3000 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13651 :visit-id "01" :orbit-number 7 :pcs-time 222 :si-vis-utilization 2778 :al-overhead-at-end 0 :internal-dur-at-end 395 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3000 :pcs-gap 0 ) true 7 0 The ~15A gap from ~1280 to 1295 angstroms is acceptable. Three of the four FP-POS positions will be sufficient to account for detector imperfections. The ~15A gap from ~1280 to 1295 angstroms is acceptable. Three of the four FP-POS positions will be sufficient to account for detector imperfections. The ~15A gap from ~1280 to 1295 angstroms is acceptable. Three of the four FP-POS positions will be sufficient to account for detector imperfections.