0 Assigned ID: 7210 ----- Attempting Submission 1 (Wed Apr 15 21:14:31 GMT 2026) ----- The number of orbits used exceeds the number allocated STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS SCIENCE TOO FAR FROM WAVECAL STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS SCIENCE TOO FAR FROM WAVECAL STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS 0 ----- Attempting Submission 1 (Sat Aug 29 01:23:44 GMT 2026) ----- The visit planner would not run on the APT version 2026.3.2 on my mac. I need to add wavecals within a pattern, but get error messges when I try to do that. The failed supernova candidate in the low metallicity galaxy PHL293B: Still there, but what is it? The metal-poor dwarf galaxy PHL293B (23 Mpc) contained a luminous blue variable (LBV) identified by its spectrum. This source had roughly constant luminosity during 2001-2009, and was modeled as a massive LBV similar to Eta Carinae, and notably, similar to the progenitors of SN2009ip and SN2015bh. In more recent data, the source faded beyond ground-based limits, and spectral signatures of the LBV disappeared. PHL293B was proposed as the first viable candidate of a failed SN event from a massive LBV star. Subsequent HST images, however, reveal a lingering blue source at the same position. So what happened? If this was indeed a failed SN, the lingering source could be a host cluster. Or if the sudden fading marks the end of an LBV giant eruption, then characterizing its current faint post-eruption state with spectroscopy is important for two reasons: (1) We know very little about the recovery time and the physical state of massive stars after an eruption, or if they return to their pre-outburst state. (2) This object offers a cautionary tale for other failed SN candidates. Whether a failed SN or not, spectroscopy is essential for assessing the star's post-eruption state, but ground-based data cannot do this because the source is lost in galaxy light. We propose deep STIS spectroscopy to determine once and for all if the LBV disappeared as a failed SN, and 2 orbits of imaging photometry to reproiduce the Cycle 28 imaging and measure its UV/optical SED. The SED is needed to evaluate the LBVs current luminosity, or to estimate the age of the host cluster and thus the approximate initial mass of the LBV) if indeed the LBV has disappeared. This program repeats earlier imaging to obtain a current epoch of photometry in several filters. The STIS observations will obtain a spectrum of the LBV that is resolved from surrounding galaxy light for the first time, both low and medium resolution. PI N. Smith is an expert in studying LBVs and supernovae. Smith has broad experience in observational studies in both spectroscopy and multi-wavelength imaging. CoIs A. Allan and E. Farrell were graduate students working with Prof. Groh (no longer in astronomy) on this topic, and Allan was the first author of our paper on the fading seen in optical data. J. Andrews is an expert on observational studies of supernovae and massive star populations. A. Mehner is an expert on observational studies of LBVs. Stellar Physics and Stellar Types 6 false true false false false false false SUPPORTED EXT-STAR LUMINOUS BLUE VARIABLE J2000 J2000 STIS/CCD Spectroscopic No No G750M 6581 STIS/CCD Spectroscopic No No G430L 4300 WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F606W WFC3/UVIS Imaging No No F438W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F225W POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 1 false POS-TARG DITHER 0.2 LINE false false 2 90.0 STIS-ALONG-SLIT 2 false The scheduling data was generated by CASM 34.2. 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