0 Assigned ID: 1855 ----- Attempting Submission 1 (Fri Mar 01 22:17:24 GMT 2013) ----- re-submission with TOO trigger activation, target new SN in Mrk 1309 adjusted STIS acquistion exposure time to 15 seconds 99680339 ----- Attempting Submission 1 (Mon Jun 24 21:48:52 GMT 2013) ----- ----- Attempting Submission 2 (Sun Mar 16 06:43:05 GMT 2014) ----- HST Phase II Proposal 13351 (mrk1309-trigger-13351.apt) successfully submitted. ----- Attempting Submission 3 (Sun Mar 16 22:17:54 GMT 2014) ----- UV Spectroscopy of a Peculiar White Dwarf Supernova While type Ia supernovae (SNe Ia) have been extremely useful for studying the cosmic expansion history, their explosion mechanism and progenitor system remain unsolved problems. Moreover, as large samples of SNe are observed, the diversity among these explosions has grown: not all exploding white dwarfs look like normal SNe Ia. Understanding why these "peculiar" objects are different from the normal ones can help explain the standard SN Ia scenario, as well as give us a better understanding of the many endpoints of stellar evolution. Connecting observations to physical models has been difficult for both normal and peculiar white dwarf supernovae. The ultraviolet is a largely unexplored wavelength region for peculiar SNe Ia; the high opacity in the UV from typical thermonuclear burning products means that the UV flux in white dwarf supernovae is very sensitive to the outermost layers of ejecta. This material is the least processed, and is thus an ideal place to look for clues to progenitors and explosion mechanisms. Here we propose to take advantage of the Cycle 21 UV Initiative to obtain target-of-opportunity STIS UV spectroscopy of a peculiar white dwarf supernova to add a unique piece of the puzzle connecting peculiar SNe Ia and their progenitors. Our goal is to observe a single peculiar white-dwarf supernova using the STIS CCD for optical spectra and the STIS NUV_MAMA instrument for the near-UV. Many peculiar SNe Ia are faint, so we will restrict ourselves to low redshift events (z < 0.03). Peculiar SNe Ia evolve differently in the UV than their normal counterparts; we will therefore have two visits on our object. The first will be 2 of our 6 allotted orbits, with approximately half of an orbit being used for the optical spectrum using the STIS CCD, and the other 1.5 orbits being used for the STIS NUV-MAMA spectrum. This visit should cover the SN at maximum or prefereably a few days before maximum. By the time of the second visit, the SN will have faded considerably. The second visit will consist of 4 orbits: 0.5 orbits for the STIS CCD optical spectrum and 3.5 orbits with the NUV-MAMA instrument. We request that the second visit be scheduled approximately 1 week after the initial visit. HOT STARS Default false true false false false SUPPORTED STAR SUPERNOVA SUPERNOVA TYPE IA SN-J1144 J2000 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 /private/var/folders/jz/0x6fxq6j4sb70m3vjknhgw2h0000gn/T/OPVisit3800890347552712196.xml Timing link suitability includes constraints ([02 After 01 by 4.0 to 9.0 days]) The scheduling data was generated by CASM 22.0. CASM was run in Phase II mode. 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