0 Assigned ID: 1773 ----- Attempting Submission 1 (Fri Apr 09 00:59:45 GMT 2021) ----- HST Phase I Proposal 1773 successfully submitted. Receipt: # 1773-1 ----- Attempting Submission 2 (Fri Apr 09 18:59:40 GMT 2021) ----- HST Phase I Proposal 1773 successfully submitted. Receipt: # 1773-2 ----- Attempting Submission 3 (Fri Apr 09 19:51:33 GMT 2021) ----- FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser 0 ----- Attempting Submission 1 (Thu Jul 29 15:46:54 GMT 2021) ----- ----- Attempting Submission 2 (Wed Oct 06 20:39:18 GMT 2021) ----- HST Phase II Proposal 16649 successfully submitted. Receipt: # 16649-2 ----- Attempting Submission 3 (Wed Oct 06 23:21:28 GMT 2021) ----- Jay told me to increase the FLASH values. The final word on SN 2009ip: is it dead? We propose 10 yr post-explosion UV/optical imaging of the remarkable transient SN 2009ip, in order to determine its ultimate fate. This object was discovered in a non-terminal eruption in 2009, and then appeared to explode in a much more extreme supernova (SN)-like event in 2012. A very massive (80 Msun) quiescent progenitor was identified in an archival HST image, and the star had several luminous blue variable (LBV)-like eruptions before 2012. Many SNe IIn are inferred to have LBV progenitors to make their dense circumstellar material (CSM), but SN2009ip is an extraordinary case where the LBV-like progenitor was detected directly, and where spectra of numerous pre-SN eruptions were obtained. No other SN has this treasure trove of detailed information about the progenitor (not even SN1987A). This was one of the most important transient events of the past decade, because if it was a true core-collapse (CC) SN, then it is the first definitive case of a very massive star above 30 Msun that went SN and didn't collapse to a black hole. However, the interpretation of SN2009ip as a true CCSN is controversial for 2 reasons: (1) its lightcurve could also be explained by shell collisions from non-terminal explosive transients, and (2) the tell-tale signs of nucleosynthetic products, if present, were largely masked by CSM interaction. As with all SN progenitor candidates, proof that the star is dead requires that it disappear in late time data. Five years ago the source was only marginally fainter than the progenitor and apparently still fading. Cycle 29 will be 10 years since explosion. Our proposed observations will determine once and for all if the progenitor is gone. The goal of these observations is to measure the UV/optical/IR spectral energy distrbution (SED) and H-alpha emission line strength of the source at SN 2009ip's position at a time of roughly 10 years after its 2012 explosion. If the source at SN 2009ip's position has faded beyond detectability, these observations will place deep-enough upper limits on a late-time source to confirm that the progenitor star is gone. If a detectable source remains, the observations are designed to be able to distinguish between three competing possibilities: (1) A massive luminous blue variable (LBV) progenitor star that survived, possibly obscured by dust that was ejected in the event or returning to a hot state, (2) A SN explosion where the late-time source is dominated by ongoing late-time circumstellar material (CSM) interaction, or (3) A companion star or star cluster that is coincident with the SN position. Of course, the late time source may be due to a combination of these sources, and the UV/optical/IR SED plus H-alpha emission will be able to distinguish them. It is impossible to rule out or distinguish between these possibilities with only optical/IR continuum filters; both the UV flux and the H-alpha emission are essential as well. Although we have organized the observations into separate visits, they should be executed as close together in time as possible. Whether the lingering source is a SN powered by late-time CSM interaction or a surviving LBV star, it is likely to be variable. LBVs can vary on short (few days) timescales, and late-time CSM interaction luminosity can change quickly if the CSM is clumpy or has shell structure. In order to produce a useful SED to test the various hypotheses, the full continuum broad-band set of filters from UV to IR must be obtained close together in time. Most importantly, the narrow F657N filter (tracing H-alpha emission) should be obtained as close to quasi-simultaneously with the F555W, F606W, and F814W filter images as possible. The F657N filter will be used to measure the equivalent width of H-alpha emission - but to do this, we need to know the off-line optical continuum emission level measured by the F555W, F606W, and F814W filters at the same time. Both the continuum luminosity and H-alpha emission can be variable (and they may be independently variable). It is impossible to complete the science goals of this program without comparably deep optical continuum filters to subtract from the Halpha filter. Also, it will greatly improve the archival value of the images if the F657N and broad continuum filters (at least F555W and F814W) are obtained at nearly the same time, with the SN located at the same position on the detector, and with the same roll angle. This is because well-aligned and simultaneous continuum images are needed to make a continuum-subtracted image of the H-alpha emission. We do not strictly need this spatial alignment to complete the goal of measuring the H-alpha equivalent width from SN 2009ip (we could do this even if the target were at a slightly different position on the detector, as long as the observations were close in time). However this alignment is needed in order to make a continuum-subtracted H-alpha emission map of the surrounding environment in the host galaxy in order to study star forming HII regions or search for emission line stars, for example. It would significantly decrease the archival value if the F657N and broad-band filters were not obtained with the same target positon on the detector and a very close roll angle. This is because the differences in distortion correction and pixel resampling are minimized or eliminated when the roll angle and field of view aer the same, and obviously, the overlapping area on the sky in the F657N and continuum filters is optimum if they are spatially aligned. If it turns out that there is a source remaining at SN2009ip's position and that source is consistent with a star cluster contributing to the observed light, the UV/optical/IR SED will be used to contrain the age of that cluster with comparison to population synthesis models. If the remaining light is a combination of a star cluster (presumabl not variable) and late-time CSM interaction (variable) then the SED would be corrupted if images in different filters are obtained at significantly different times. Nathan Smith is an expert in the properties and evolution of massive stars (especially LBVs), winds from massive stars, and their environments, as well as an expert in observational studies of supernovae that interact with circumstellar material (Type IIn and Ibn supernovae). He wrote the first paper on SN 2009ip before it became a supernova, which presented the discovery of its progenitor in archival HST data. Jon Mauerhan is an expert in Wolf-Rayet stars and other massive stars, supernovae interacting with circumstellar material, and supernova spectropolarimetry. He wrote the first paper analyzing the 2012 explosion of SN 2009ip and proposed that it was a true SN event. J. Andrews is an expert on observational studies of core-collapse supernovae, dust formation in SNe, and observations of extragalactic massive star populations. Alex Filippenko led the highly successful Lick Observatory Supernova Search for more than 2 decades, has been studying images and spectra of supernovae (SNe) for more than 3 decades, and has led numerous HST studies of nearby SNe. Schuyler Van Dyk is an expert in HST photometry of SNe, in the identification of SN progenitors and determination of their masses, and in the study of stellar populations around SNe. Ori Fox is an expert in SN late-time shock interaction; he also studies dust, its formation in SN ejecta, and how it affects SN photometry, spectra, and interpretations. The above investigators have fruitfully worked together in the past and have many joint HST papers. Every member of the team has previously worked with planning HST imaging observations and analyzing HST data. 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