Assigned ID: 1003 ----- Attempting Submission 1 (Sat Feb 25 00:33:41 GMT 2012) ----- HST Phase I Proposal 1003 (PTF11kly_HST_PROPOSAL.pdf.apt) successfully submitted. ----- Attempting Submission 2 (Sat Feb 25 00:51:56 GMT 2012) ----- HST Phase I Proposal 1003 (PTF11kly_HST_PROPOSAL.pdf.apt) successfully submitted. ----- Attempting Submission 3 (Sat Feb 25 00:57:31 GMT 2012) ----- HST Phase I Proposal 1003 (PTF11kly_HST_PROPOSAL.pdf.apt) successfully submitted. ----- Attempting Submission 4 (Sat Feb 25 00:58:55 GMT 2012) ----- ----- Attempting Submission 1 (Mon Jun 25 16:39:57 GMT 2012) ----- Late Time STIS Spectroscopy of the Extremely Nearby Type Ia SN 2011fe In the first 2-3 months after the explosion of a Type Ia supernova, the innermost layers of the ejecta are concealed from view by a brilliant pseudo-photosphere. Observations obtained many months later, when the ejecta become nebular, enable us to peer deep into these layers and probe different explosion physics than is possible earlier on --- but at a cost. By this point, the supernova has faded dramatically, so only the closest events may be observed. SN 2011fe is the nearest Type Ia supernova discovered in a quarter century. We propose to obtain STIS spectroscopy of this remarkable supernova, a year after explosion, and combine these space-based observations with ground-based optical and near-infrared spectroscopy for analysis. Using the focusing lens of radiative transfer simulations, we will constrain the amount of radioactive nickel produced in the explosion, explore the extent of large-scale hydrodynamical mixing, and reconstruct the abundance stratification of the innermost ejecta. SN 2011fe represents a unprecedented opportunity to study how Type Ia supernovae explode, and is likely to remain so for decades to come. Our goal is to obtain ultraviolet spectroscopy of the extremely nearby Type Ia supernova 2011fe in M101 using STIS, 13 months after it reached peak luminosity. We hope our observations can be carried out at the very start of Cycle 20, since the supernova will only continue to fade. We will combine these observations with complementary, time-coordinated ground-based optical and near-infrared observations, and analyze them together using comprehensive radiative transfer simulations. Comparing synthetic spectra to late-time observations will allow us to explore the extent of large-scale hydrodynamic mixing during the explosion, constrain the amount of radioactive nickel produced, and reconstruct the multi-dimensional distribution of the innermost ejecta. Careful examination of nebular phase lines will provide constraints on large-scale explosion asymmetry. We plan a total of 10 orbits split into 3 visits. Our strategy is to maximize S/N we can get in the NUV, but also obtain some optical spectroscopy that can retire risk associated with constraints on ground-based visibility of the target in late September. The first 2 visits are in the STIS/NUV-MAMA configuration. The first visit uses 5 orbits, the second uses 4. We dither along the slit at the end of every few orbits by 11 pixels to reduce the impact of hot pixels. The third and final visit uses the STIS/CCD G430L and G750L configurations in sequence in a single orbit. Exposure time and S/N are estimated by rescaling fluxes estimated from an HST spectrum of SN1992A obtained 291 days past peak and using the appropriate online STIS ETC's. We account for the fact that SN2011fe was over 10 times brighter than SN1992A at peak since it was much closer, and we also account for an additional ~100 days of decline in flux since our observations are later on the light curve of SN2011fe than those of SN1992A. Our observations need to come as close to the beginning of Cycle 20 as possible. If the observations can be scheduled in September, this is not a problem for us at all. All 3 visits need to be scheduled as close together in time as is feasible. We understand the MAMA observing constraints prevent those visits from taking place in the same day. HOT STARS 12 false 0.0 0.0 false false false false SUPPORTED EXT-STAR SUPERNOVA TYPE IA PTF11KLY J2000 J2000 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 POS-TARG DITHER 0.275 LINE false false 2 90.0 STIS-ALONG-SLIT 1 false Timing link suitability includes constraints ([Sequence (01 02 03) within 3.0 days]) The scheduling data was generated by CASM 20.2. 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