This is a mid-cycle proposal. We are submitting it before 30 Sept. 2017, as we need the observations requested here to be carried out in the Oct. 1, 2017 - March 31, 2018 period.-1686218968Assigned ID: 1522
----- Attempting Submission 1 (Thu Sep 28 22:12:22 GMT 2017) -----Following discussion with SC, visit 02 now uses only the original target (SN2015F) with a nested dither pattern.
The subpattern parameters have been fixed to reflect UVIS values. Subpattern is now WFC3-UVIS-DITHER-LINE-3PT.271637906----- Attempting Submission 1 (Fri Nov 17 21:19:33 GMT 2017) -----
----- Attempting Submission 2 (Mon Nov 20 23:12:03 GMT 2017) -----
----- Attempting Submission 3 (Wed Dec 06 16:29:03 GMT 2017) -----
HST Phase II Proposal 15415 (GO15415_midcycle_phaseII_new.apt) successfully submitted.
Receipt: # 15415-3
----- Attempting Submission 4 (Wed Dec 06 20:15:51 GMT 2017) -----
HST Phase II Proposal 15415 (GO15415_midcycle_phaseII_pattern.apt) successfully submitted.
Receipt: # 15415-4
----- Attempting Submission 5 (Wed Dec 06 20:57:58 GMT 2017) -----
HST Phase II Proposal 15415 (GO15415_midcycle_phaseII_pattern.apt) successfully submitted.
Receipt: # 15415-5
----- Attempting Submission 6 (Wed Dec 06 21:00:12 GMT 2017) -----One last peek at SN 2015FAs part of GO-14611, we have been observing the fading light curve of the Type Ia supernova (SN Ia) SN 2015F out to 920 days past maximum light. Following similar late-time observations of other SNe Ia, we expected the light curve of this SN to begin to decline at a slower rate as light from the long-lived 57Co decay chain begins to add a measurable boost to the light from the radioactive decay of 56Co. We have one last visit to this SN, on 29 Sep. 2017, but the data have already been surprising. The observations so far are still consistent with both scenarios: 56Co decay alone, as well as a combination of 56Co and 57Co decays. Either the light curve is still solely dominated by 56Co decay or the mass ratio of the two isotopes is much smaller than in other SNe Ia that have been followed out to similar late times. We ask for two more visits in with WFC3 in F555W (four orbits total) to follow the SN out to 1020 days past maximum light and conclusively discriminate between these two scenarios.We will schedule two visits to SN 2015F. In each visit, we will observe the SN in F555W using a 3-point line dither pattern in each orbit. The scheduling of the visits is important. We ask that the first visit be scheduled as early as possible (optimally before 5 December 2017), and that the second visit be scheduled between 22-28 January 2018. To make scheduing easier, we have allocated 1 orbit to the first visit, and 3 orbits to the second one. Please let us know if the first visit cannot be scheduled as early as desired, and we will change our phase II accordingly.Stellar Physics6falsefalsefalsefalsefalsefalseSUPPORTEDEXT-STARSUPERNOVA TYPE IAJ2000J2000WFC3/UVISImagingNoNoF555WPOS-TARGDITHER0.135LINEfalsefalse346.84WFC3-UVIS-DITHER-LINE-3PT1falsePOS-TARGDITHERDITHER31WFC3-UVIS-DITHER-LINE-3PTfalsefalse0.1353135POS-TARGLINE46.842true/home/orgraur/projects/late-time/2015F/midcycle/OP-cache/GO15415_midcycle_phaseII_pattern-v01.xmlThe scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.1512357746000319.9309263865041(Tic-Visit
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)true10/tmp/OPVisit8214084568187800206.xmlThe scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.This visit consists of three orbits, set up in a LINE dither pattern that uses the UVIS-DITHER-LINE-3PT as a subpattern. That way, each orbit is slightly shifted relative to the first orbit, and within each orbit the exposures are dithered along the 3PT pattern.(Tic-Visit
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