0 Assigned ID: 680 ----- Attempting Submission 1 (Fri Apr 08 18:44:44 GMT 2016) ----- HST Phase I Proposal 680 (ugc.apt) successfully submitted. Receipt: # 680-3 ----- Attempting Submission 4 (Fri Apr 08 21:20:01 GMT 2016) ----- Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. 0 ----- Attempting Submission 1 (Wed Jul 20 21:04:52 GMT 2016) ----- We rna the ETC for Phase I. No bright stars nearby, no danger of saturation. Exposures are similar to our recent sSTIS spectra of SN2005ip (PI=Fox). The optical transient in the dwarf galaxy UGC2773 that was discovered in 2009 (called UGC2773-OT) has proven to be the best known extragalactic analog of the 19th century giant luminous blue variable (LBV) eruption of Eta Carinae. While most non-supernova transients of comparable peak luminosity fade in about 100 days, UGC2773-OT is the only one that has remained in eruption for a decade, like Eta Car. Moreover, spectra of Eta Car's light echoes most closely resemble spectra of UGC2773-OT, and it had a luminous blue progenitor detected by HST. Current debate about Eta Car's eruption centers around it being powered by a super-Eddington wind, or alternatively, an explosion where a shock interacting with dense circumstellar material (CSM) powers the visible display. Interestingly, a recent study of the optical spectra of UGC2773-OT showed evidence of shock emission reminscent of some Type IIn supernovae that are also powered by shock interaction. At visible wavelengths, however, the signatures of a very strong wind can sometimes be similar to those seen in some Type IIn supernovae. Here we propose UV spectroscopy of UGC~2773-OT to either confirm or refute the hypothesis that it has strong shock interaction occuring, by looking for unambiguous UV signatures of shock excitation. While an extremely dense wind with a pseudo photosphere will tend to fall off in flux in the UV due to line blanketing, shock diagnostics like MgII 2800, HeII 1641, and some other lines are expected to be bright in the UV, as they are in Type IIn supernovae. This is a rare opportunity to provide a fairly clean test to discriminate between two quite different models. This program will obtain the NUV and FUV spectrum of the optical transient discovered in the dwarf galaxy UGC2773. Although it was discovered in 2009, the transient had faded very slowly and shows signs of shock interaction in the recent optical spectrum. The purpose of the UV spectra is to determine if the UV sows clear signs of shock excitation or line blanketing from a cool wind. The program will use STIS NUV and FUV MASA detectors with the 230L and 140L elements. Stellar Physics 12 false true false false false false SUPPORTED STAR LUMINOUS BLUE VARIABLE NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 The scheduling data was generated by CASM 24.0. CASM was run in Phase I mode. STIS/NUV-MAMA Spectroscopic No No G230L 2376 The scheduling data was generated by CASM 24.0. CASM was run in Phase I mode. STIS/FUV-MAMA Spectroscopic No No G140L 1425 1469048165473 /private/var/folders/qh/l7959jcd6jjblv_9fwgs0lvw0000gn/T/OPVisit4870658385843852030.xml The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 2 orbits, low resolution spectrum. Long-lived transient, but fading. Need to schedule observations as early as possible. 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