Assigned ID: 908 ----- Attempting Submission 1 (Fri Feb 24 23:26:17 GMT 2012) ----- HST Phase I Proposal 908 (V445_20.apt) successfully submitted. ----- Attempting Submission 2 (Fri Feb 24 23:55:17 GMT 2012) ----- post-FLASH currently enabled, would appreciate feedback if the assessment of using this in light of CTE has changed ----- Attempting Submission 1 (Mon Jul 09 15:52:25 GMT 2012) ----- Use of quad filter is acknowledged, a centered 3pt pattern is used with the appropriate aperture. If a special pattern is preferred, we would welcome feedback. Explosive detonations on the surfaces of accreting white dwarfs play a key role in establishing viable progenitor pathways towards Type Ia supernova explosions. If the white dwarf is accreting hydrogen deficient material, helium shell-flash driven eruptions can occur on its surface. Thus far only one such helium nova event has been observed in Nova Puppis 2000 = V445 Pup. We have discovered an expanding bipolar shell involving fast moving ejecta of He-rich material surrounding this binary. This used state of art ground-based AO imaging and IFU spectroscopy. However, we have now reached the limit of what can be done from the ground and therefore request high spatial resolution HST imaging of the ejecta in V445 Pup. We request 2 orbits in Cycle 20 split between three narrow band filters, followed by a repeat epoch two observing cycles later. These narrow band images will allow us to map the expanding ejecta in the [OII], [OIII] and HeI lines, to be directly compared with kinematical measurements based on the same lines. This will allow us to determine a robust distance using the expansion parallax method and study the ionisation structure of the shells and knots we have seen in our broadband AO images. Splitting the observations over two cycles is necessary in order to provide sufficient baseline to accurately measure the on-sky expansion which is estimated to proceed at an angular speed of 0.3"/year. Our imaging targets an extended source resolving the ejecta of a nova eruption in 2000 using WPFC3/UVIS. The filters are chosen to target previously detected emission lines covering [OIII] with F502N, [OII] with FQ727N and HeI with F680N. We have supporting ground-based data that map the kinematics of these lines using IFU spectroscopy while the target position is accurately known from recent ground-based imaging. All our exposures use the same 3-point dither pattern to improve sampling and permit cosmic ray rejection. Exposure times are scaled to reflect the observed relative line strengths while at the same time pack the 2-orbit long visit efficiently. Thus F680N receives the longests exposure time and takes up the whole of orbit 1, followed by F502N and some short FQ727N exposures in orbit 2. We have chosen the optimal UVIS aperture for our F502N and F680N exposures, while the FQ727N exposures will use the quadrant D sub-array only in sync with the filter and to save some overheads. We have decided to enable the post-FLASH as an extra option, since we believe our relatively short exposure times with narrow-band filters will benefit from this procedure. We verified background levels using the ETC and request a post-flash level of 15e for the F502N and FQ727 exposures as these have the lowest background per exposure (<5e), while 10e is sufficient for the F680N exposure (with ~5e). N/A N/A This set of images will be repeated in Cycle 22 HOT STARS 12 false 0.0 0.0 false false false false SUPPORTED STAR CLASSICAL NOVA EMISSION LINE NEBULA Position determined from recent good seeing CCD imaging at the Magellan telescope with a WCS referenced to ICRS. Note that target is currently significantly fainter than on DSS plates as the nova eruption casued extensive local extinction. J2000 J2000 J=17.36 +/- 0.07 The scheduling data was generated by CASM 20.0. CASM was run in Phase I mode. WFC3/UVIS Imaging No No F502N WFC3/UVIS Imaging No No F680N WFC3/UVIS Imaging No No FQ727N The scheduling data was generated by CASM 20.0. CASM was run in Phase I mode. WFC3/UVIS Imaging No No F502N WFC3/UVIS Imaging No No F680N WFC3/UVIS Imaging No No FQ727N POS-TARG DITHER 0.135 Standard 3-pt line dither with centering enabled LINE false true 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 2 false 1341846551382 /tmp/OPVisit3979155009538411065.xml The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. Cycle 20 epoch (Tic-Visit :proposal-id 12899 :visit-id "01" :proposal-version -1 :trans-version "20120604" :date "09-Jul-2012 16:09:11.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1943648 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12899 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12899 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2919 :al-overhead-at-end 122 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3253 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12899 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3029 :al-overhead-at-end 170 :internal-dur-at-end 583 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3253 :pcs-gap 0 ) true 2 0 F680N over 3pt dither post-FLASH of 10e to reflect low expected background F502N over 3pt dither post-FLASH of 15e to reflect low expected background FW727 over 3pt dither, quadrant D sub-array post-FLASH of 15e to reflect low expected background