0 Assigned ID: 146 ----- Attempting Submission 1 (Wed Apr 06 17:53:03 GMT 2016) ----- FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Resubmitting with the STIS/CCD and STIS/MAMA exposures separated into two different visits, as requested by Molly Peeples 912920543 ----- Attempting Submission 1 (Mon Jul 11 20:47:27 GMT 2016) ----- ----- Attempting Submission 2 (Thu Dec 01 23:23:47 GMT 2016) ----- There are warnings about (1) no ETC run for the MAMA spectra, and (2) whether the amounts of flash for the WFC3 images are enough. 1. We did not run ETC for the MAMA spectra since it was not easily possible to input a poorly known planetary-nebula spectrum into the ETC. We did run simulations separately from the ETC, with the result that we are nowhere near saturation for the MAMA observations. The PN is expected to have a very faint spectrum in the NUV & FUV. 2. There will be considerable background from M31 in the WFC3 images, so we are using only small amounts of flash in F502N and F555W, and based on archival images of the field in F814W, no flash is needed there. Planetary Nebulae in the Open Clusters of M31 Most planetary nebulae (PNe) are field objects. Precious little is known about their progenitor stars' properties and how they relate to those of the PN. The lone exceptions are the very rare cases where a PN is a member of an open star cluster. Then one can determine the ages, masses, and compositions of the progenitors, providing direct tests of stellar-evolution theory. We have recently discovered three PNe belonging to open clusters in M31, the Andromeda Galaxy. Here we propose a set of HST follow-up investigations. For the PN in the M31 cluster B477-D075, we know its precise location, and there are excellent photometric data (from the M31 PHAT project) that establish the host cluster's age (350 Myr) and the mass of the PN progenitor star (3.35 Msun). We will use STIS spectroscopy in the UV and optical to measure He, CNO, and alpha-process abundances in the nebula, based on emission-line fluxes and a photoionization code. Our primary aim is to compare the measured abundances with predictions of post-AGB evolution theory. In particular, "hot-bottom burning" is expected to produce enhanced He/H and N/O abundances when the progenitor star is sufficiently massive, but it is uncertain whether this occurs at masses as low as ~3 Msun, or requires masses of at least ~5 Msun. Thus our observations will provide key new constraints on AGB evolution of intermediate-mass stars. For two other M31 clusters, B458-D049 and SK044A, whose integrated-light spectra show that a PN is present, we will use WFC3 with an [O III] filter to verify the presence of the PNe, and determine their precise astrometric locations. We will then follow up with STIS spectroscopy in a future HST Cycle. This program has 3 targets. For one of the targets we will obtain long-slit spectra with STIS. For the other two, we will obtain direct images with WFC3. 1. STIS: The target is a planetary nebula in the M31 open cluster B477-D075. Since the PN itself is very faint, we do an acquisition on a nearby, brighter star. We have measured the offset from this star to the PN using narrow-band ACS images that show both the star and the PN. Following the acquisition and offset maneuver, we use 4 HST orbits to obtain STIS spectra with the low-resolution gratings. We dither along the slit for these observations. 2. WFC3: For the open clusters B458-D049 and SK044A, each of which is known from ground-based integrated spectra to contain a PN, we will obtain direct images in order to precisely locate the PN (for follow-up STIS spectroscopy in a future cycle). We will obtain a narrow-band F502N image ([O III]), along with a broad-band V (F555W) image. Image subtraction will clearly identify the PN. We will also obtain images in I (F814W) in order to obtain an improved color-magnitude diagram for each cluster. 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