0 Assigned ID: 435 ----- Attempting Submission 1 (Fri Apr 07 08:13:13 GMT 2017) ----- HST Phase I Proposal 435 (87a_2017_phase1.apt) successfully submitted. Receipt: # 435-1 ----- Attempting Submission 2 (Fri Apr 07 14:16:28 GMT 2017) ----- Hi, This proposal is for cycles 26 sn1987A 15503 -1626161634 ----- Attempting Submission 1 (Wed Jul 12 18:00:11 GMT 2017) ----- HST Phase II Proposal 15256 (15256.apt) successfully submitted. Receipt: # 15256-1 ----- Attempting Submission 2 (Tue Jul 18 16:34:37 GMT 2017) ----- ----- Attempting Submission 3 (Tue Sep 19 20:33:08 GMT 2017) ----- ----- Attempting Submission 4 (Wed Aug 08 22:05:08 GMT 2018) ----- SN 1987A is the great supernova (SN) of the HST era. An unbroken string of observations is the essential tool for detecting change and establishing a uniform legacy archive. Previous imaging has shown that the SN ejecta has changed from being powered by radioactive 44Ti up to day 5000, to being powered by the X-rays from the ring collision. This is seen both in the light curve and the rapidly changing morphology of the ejecta. As the X-rays penetrate further in we expect the metal rich core to also become illuminated. As the ejecta expand the dust in the center may become transparent and our limits on a compact object will become stronger, or yield a detection. Also the circumstellar ring surrounding the SN is undergoing a dramatic change. After a rapid increase, the flux reached a maximum around day 8000 and is now decaying rapidly. This marks the final destruction of the ring and we estimate that by 2025 it will be dissolved. At the same time, diffuse emission and new hot spots outside the inner ring are becoming visible, providing a tool to study the unknown circumstellar environment outside the ring. Imaging in both narrow and broad bands allow us to follow these developments. The HST observations have a unique blend of photometric fidelity and angular resolution that makes them the indispensable partner to ongoing ground-based, X-ray and sub-mm ALMA observations, providing the morphology of both the inner metal rich core and the H-rich envelope. They will also be a necessary complement to our approved STIS and COS observations and by 2019 also of the JWST GTO observations. This is a long term study: given the rapid change we see, sampling every year is necessary. The WFC3/UVIS observations using filters F438W, F625W, F502N and F657N connect with our earlier observations at similar, or better S/N ratio through drizzled observations. As described above, these new images will allow us to follow the light curve, the morphology of the ejecta, the ring emission as well as new spots and diffuse gas outside the ring. Broad band images: We request imaging with F438W and F625W in all three years. To obtain a similar quality as our previous observations we need half an orbit per filter. This is our request for F438W all three years and for F625W in year one and year three. In year two, we request a significantly deeper observation of 1.5 orbits for F625W. This observation will allow us to probe the faintest structures in the ejecta, ring and reverse shock. Such a deep observation also offers the possibility of detecting previously unseen emission components. The total request for the broad filters is thus 1+2+1=4 orbits. Narrow band images: We request imaging in F502N and F657N in year one and year three only. To obtain similar quality as our previous observations we need two orbits for F502N and one orbit for F657N. Stellar Physics 6 false false false false false false false SUPPORTED EXT-STAR SUPERNOVA SUPERNOVA TYPE II This object was generated by the targetselector and retrieved from the SIMBAD database. frpk our astrometric STIS image 5:35:28.107 -69:16:11.050 fk5 514 503 142.747 J2000 J2000 WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F438W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F438W WFC3/UVIS Imaging No No F502N WFC3/UVIS Imaging No No F657N POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 1 false 1533749544628 /private/var/folders/t2/3zsjbp3d7mb77q2fgk641_n40000gn/T/OPVisit1457963559815580609.xml Timing link suitability includes constraints ([Sequence (10 11) within 14.0 days]) The scheduling data was generated by CASM 26.0. CASM was run in Phase II mode. 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