0 Assigned ID: 1203 ----- Attempting Submission 1 (Thu Feb 28 08:56:05 GMT 2013) ----- 0 ----- Attempting Submission 1 (Wed Jun 19 08:26:39 GMT 2013) ----- Science goals require FP-POS=ALL separately during *each* of the 4 orbits to allow investigation of time variable behavior in spectrum obtained during each orbit. APT flags this configuration as "inefficient" (compared to "normal" strategy of applying FP-POS to the entire, multi-orbit observation). However, I have discussed this configuration with my Contact Scientist (Cristina Oliveira <oliveira@stsci.edu>), who has OK'ed it. We propose to use 4 HST orbits to obtain time-resolved far-UV (FUV) spectra with COS of the rapidly spinning, metal-polluted white dwarf KIC 9535405, in order to explore the distribution of accreted metals over the white dwarf's surface (including the possibility that confinement by the white dwarf's magnetic field is preventing the rapid gravitational settling of heavy elements). This will enable us to explore details of the largely unknown process through which matter transitions from circumstellar space onto the WD itself. We will also obtain the chemical composition of the parent body of the accreted matter, thereby adding to the limited pool of information on direct measurements of the composition and structure of extrasolar planetary (terrestrial) bodies. The proposed HST observations will be complemented by existing, ongoing, and planned ground- and space-based (Kepler, Spitzer) observations obtained by us. The basic observing strategy for this program is relatively straightforward: 1 visit to 1 target lasting 4 orbits. A single COS/FUV configuration (G160M, center at 1309 A, TIME-TAG mode) is used for the entire duration of the visit. Each orbit is configured as a single exposure on the target with the maximum possible total integration time (target visibility minus overheads). Because we want to compare the spectra obtained during each orbit for time variable behavior of the target (not just examine a single spectrum obtained during the entire 4-orbit program), while also ensuring the best possible spectral extraction, we have used FS-POS=ALL for the science exposure in each orbit, to ensure the best results on an orbit-by-orbit basis. Thus, each orbit contains a single science exposure split into 4 sub-exposures. Orbit 1 starts with GS acquisition, followed by target acquisition (COS/FUV ACQ PEAKXD, then COS/FUV ACQ PEAKD). After accounting for the FP-POS overheads, the total remaining science time in Orbit 1 is 2222 s. The S/N achieved in the combined spectrum from Orbit 1 will be approx. 21 (using the online ETC, with the target represented by a 34,000 K blackbody normalized to V=17.15 mag). Orbits 2, 3, and 4 are identical to each other. Like Orbit 1, they start with guide star (re)acquisition, but do not require target (re)acqusition - hence, slightly more time is available for the science exposures. After acounting for FS-POS overheads, a total of 2649 s is available for science exposure in each orbit. Expected S/N for the total combined spectrum in each of Orbits 2, 3, and 4 is approx. 23. HOT STARS Default false true false false false SUPPORTED STAR DA Target coordinates from Spitzer IRAC ch1 pbcd mosaic obtained in Jan 2013. J2000 J2000 UVW2 (Swift UVOT) = 1.60(3) mJy COS/FUV Spectroscopic No No G130M 1309 1371500637591 /Users/hoard/Research/proposals/Hubble/2013-cycle21/1203-KeplerWD/phase2/OP-cache/hoard_13322_phase2-v01.xml The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 13322 :visit-id "01" :proposal-version -1 :trans-version "20130502" :date "17-Jun-2013 22:23:57.0" :trans-errors '(:WARNINGS 3 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 722192 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13322 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13322 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3044 :al-overhead-at-end 0 :internal-dur-at-end 76 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3377 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13322 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3152 :al-overhead-at-end 0 :internal-dur-at-end 76 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3377 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13322 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3152 :al-overhead-at-end 0 :internal-dur-at-end 76 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3377 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13322 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3152 :al-overhead-at-end 0 :internal-dur-at-end 404 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3377 :pcs-gap 0 ) true 4 0 ETC calculation uses 34000 K BB model normalized to V=17.15, gives ACQ exp time = 1.7849 sec. Double-check: the Swift measurement of the target at 0.2 microns (1.6 mJy) corresponds to 3e-14 erg/s/cm^2/A at 0.13 microns, assuming 34000 K BB spectrum. Figure 8.4 in COS IHB gives ACQ exp time of ~1.5 sec. optional parameters are recommended values from COS IHB, Sec 8.6. S/N = 10.4 per resolution element in each FP-POS split spectrum S/N = 11.3 per resolution element in each FP-POS split spectrum S/N = 11.3 per resolution element in each FP-POS split spectrum S/N = 11.3 per resolution element in each FP-POS split spectrum