0 Assigned ID: 757 ----- Attempting Submission 1 (Fri Apr 10 20:13:41 GMT 2015) ----- HST Phase I Proposal 757 (HST23_supers_submission.pdf.apt) successfully submitted. Receipt: # 757-1 ----- Attempting Submission 2 (Fri Apr 10 20:49:52 GMT 2015) ----- HST Phase I Proposal 757 (HST23_supers_submission.pdf.apt) successfully submitted. Receipt: # 757-2 ----- Attempting Submission 3 (Fri Apr 10 21:00:07 GMT 2015) ----- HST Phase I Proposal 757 (HST23_supers_submission.pdf.apt) successfully submitted. Receipt: # 757-3 ----- Attempting Submission 4 (Fri Apr 10 22:57:46 GMT 2015) ----- Phase II updated with target coordinates for SN2016cjj and scheduling information Aquisition exposures increased to 3 s. Time between STIS and MAMA in Visit 2, Orbit 1 were modified (200 sec shifted from STIS to MAMA) -1374284699 ----- Attempting Submission 1 (Tue Jul 21 19:31:08 GMT 2015) ----- ----- Attempting Submission 2 (Fri May 06 19:05:39 GMT 2016) ----- HST Phase II Proposal 14144 (SN2016ccj_apt2.apt) successfully submitted. Receipt: # 14144-2 ----- Attempting Submission 3 (Sat May 07 00:06:17 GMT 2016) ----- An Ultraviolet View of Overluminous Type Ia Supernonovae Type Ia supernova (SNe) are important cosmological tools because of their standardizable luminosities in the optical and near-infrared. Ultraviolet (UV) wavelengths, however, show a great diversity even in normal objects. Though all SNe Ia are UV-faint, a small and heterogeneous group of SNe have UV luminosities ten times larger than the brightest "normal" SNe Ia. We refer to these as UV-bright, even though the spectral energy distribution still peaks in the optical. The origin of this UV flux is uncertain but could result from hotter explosions (with reduced line opacities) or interaction with a companion star or the circumstellar medium. While evidence of such would be important for understanding these standard candles, these scenarios cannot be distinguished by UV photometry alone. We propose to follow up a UV-bright SN Ia (to be identified by Swift/UVOT observations) with HST/STIS to obtain high quality UV spectra near peak brightness. We will use the HST spectra to search for a hot thermal component arising from ejecta-companion or ejecta-CSM interaction. If the UV excess is not caused by a thermal component, the HST spectra can be used to model the elements responsible for the excess UV emission (or lack of absorption). The origin of the UV flux is key to understanding the progenitor star, companion, local environment, or the explosion. The time to understand the physics behind the UV luminosity is now with Swift/UVOT and HST. We will observe for three epochs/visits separated by about 5 days, with 2,2, and 3 orbits. Each epoch includes 1000 sec in STIS/CCD 52x0.2E1 and the rest in STIS/NUV-MAMA G230L 52x0.2. The target will likely have an optical magnitude V ~16. For the case where the SN is especially nearby and bright, we would like to shorten the observation times in the other epochs and add an observation in the G140L filter to extend the observation to even shorter wavelengths as was done for SN~2011fe. 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