Hi Tony, Here are new phase II for visits 20-25 and 1-6 We removed the Occulation blocking mask. We also have positioned 87A to new location so that we can get both the zero order and 2nd & 3rd orders of the GRISM. we also included a HRC acqusition to make sure HST is pointing with the needed arcsecond or so. We would like to keep the Sept-Oct 2005 time slot if possible. If you need to remove the orientation from visits 20-25 or 1-5 please let me know. ----- Submission 1 (Fri May 13 19:14:49 GMT 2005) ----- ----- Submission 2 (Tue Sep 06 16:37:40 GMT 2005) ----- Assigned ID: 222 ----- Submission 1 (Fri Jan 21 16:24:20 GMT 2005) ----- Phase I Proposal 222 (saints_cyc14) successfully submitted. SAINTS - Supernova 1987A INTensive Survey SAINTS is a program to observe SN 1987A, the brightest supernova in 384 years, as it morphs into the youngest supernova remnant at age 18. HST is the unique and perfect tool for spatially-resolved observations of the many physical components of SN 1987A. A violent encounter is underway between the fastest-moving debris and the circumstellar ring, exciting hotspots seen with HST that are suddenly lighting up. The optical and X-ray flux from the ring are both rising rapidly: HST and Chandra observations taken together are needed to understand the physics of these shocked regions. In Cycle14, the hotspots may fuse as the shock fully enters the ring. Photons from these shocks may excite previously hidden gas outside the ring, revealing the true extent of the mass loss that preceded the explosion. The inner debris of the explosion itself, still excited by radioactive isotopes produced in the explosion, is now well resolved by ACS and seen to be aspherical, providing direct clues to the mechanism of the explosion. Our search for a compact remnant is beginning to eliminate some theoretical possibilities and we have the opportunity in Cycle 14 to place much more stringent limits with NICMOS. Many questions about SN 1987A remain unanswered. How did the enigmatic three rings form in the late stages of Sanduleak -69 202? Precisely what took place in the center during the core collapse and bounce? Is a black hole or a neutron star left behind in the debris? SAINTS has been a continuous program since HST was launched-- we propose to extend this rich and deep data set for present use and future reference to answer these central questions in the science of supernovae.
Our ACS/HRC imaging program provides continuing information on the debris luminosity and expansion, eruption of new hotspots, and recombination of the rings at the highest spatial resolution. Observations in a basic set of filters (F330W, F435W, F555W, F625W, F814W, F658N, F606N and F502N) will connect with our earlier observations at similar signal-to-noise ratio (S/N). With 8 orbits we obtain S/N ratios of 5-20 in the debris and 5-100 in the hotspots. In previous cycles, we were able to take advantage of the CVZ and fewer orbits to obtain the observations. In Cycle 14, with the potential of being in the 2 gyro mode and shorter orbits, we are requesting an allocation to match the data from previous cycles. Since the ACS/HRC G800L grism spectra described below will pose some complications in extracting the emission-line strengths of some lines, we would like to use narrow-band images through both F658N and F660N to help extract the strengths of H{$\alpha$ } and [N II]. The reconnaissance for eruption of new hotspots should be done again late in Cycle 14, which takes 2 additional orbits. NICMOS observations were last carried out in 1997 and 1998. Observations done in Cycle 14 would include F110W, F160W, F205W, F108N, F164N, F187N, and F212N and require 5 orbits. Observations in these filters were carried out in Cycles 7 and 8. Those observations will be used as templates to measure changes from 7 years ago. They will also provide the best limits on emission from a compact remnant in the debris. Cycle 14 spectra will be carried out with the ACS/HRC grism (G800L) using the coronographic mask (CORON-3.0) to cut down on the overlapping emission from the circumstellar ring. By using the coronographic mask, and positioning SN1978A carefully behind the mask, we will take grism observations of one half of the ring, then moving slightly to obtain the spectra of other half of the ring as illustrated in Figure 6 and 7. We are proving this technique in Cycle 13, and should soon know how well it works in May 2005. We expect this will be effective in determining the spectra of individual hotspots. Some problems with blending can be resolved with the second order images. We are fortunate in the placement of CORON-3.0 in the focal plane relative to the G800L dispersion so that the entire 1st and 2nd order land on the HRC detector over the useful sensitivity range 5500-11000A. We are planning for 3 orbits of each per side of the ring. Each orbit will be series of drizzled exposures and have a different orientation to help remove the complex background. We expect that this combination of observations can provide data sets that are comparable in wavelength coverage, superior in spatial resolution, and adequate in resolution to provide a direct comparison with our earlier series of STIS spectra. We request to make this observation twice in cycle 14, 6 months or 180 degrees apart to deal with confusion from the stellar background. 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If this is not possible, any oreint between 250-300 is okay. 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