0Assigned ID: 6137
----- Attempting Submission 1 (Mon Apr 07 17:51:39 GMT 2025) -----
HST Phase I Proposal 6137 successfully submitted.
Receipt: # 6137-1
----- Attempting Submission 2 (Tue Apr 08 20:34:43 GMT 2025) -----
HST Phase I Proposal 6137 successfully submitted.
Receipt: # 6137-2
----- Attempting Submission 3 (Tue Apr 08 20:43:27 GMT 2025) -----
HST Phase I Proposal 6137 successfully submitted.
Receipt: # 6137-3
----- Attempting Submission 4 (Wed Apr 09 16:32:40 GMT 2025) -----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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
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
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browserWe have changed pointings slightly in the Phase II from those in the Phase I. These modifications were made,
taking into account the range of roll angles from the visit planner, in order to 1. ensure better overlap with
archival broadband F606W and F814W ACS imaging, and 2. to capture as much of the total stellar light of
the individual galaxies as possible. As the range of possible roll angles was generally still somewhat large,
it was difficult in some cases to find optimal pointings to ensure maximum overlap across all possible orientations
(i.e., in some cases, corners of the simulated WFC3 pointing fell outside of the ACS footprint). It would be great
to keep in touch as scheduling finalizes to see if further minor adjustments can be made to some of the pointings,
especially after there is more certainty on the expected orientation.1222308233----- Attempting Submission 1 (Tue Aug 12 20:56:50 GMT 2025) -----The remaining warnings prior to submission are a
result of the APT identifying the FLASH level as too high.
During the Phase II process, we consulted with the
Contact Scientist about the logic behind this warning.
We were told that while the APT is programmed to aim for
a background level of 20e, it is actually more ideal to aim
for a background level in a range between 20-35e,
and that a FLASH=20 given our exposure durations in F395N
would be able to ensure this. Following consultation with the
Contact Scientist, and given that FLASH=20 has also
been used in past successful HST F395N programs, we maintain
this setting for our F395N exposures against the APT warnings.The Metallicity Distribution Functions of M31 Ultra-Faint Dwarf GalaxiesWe propose to measure the first well-populated stellar metallicity distributions (MDFs) in ultra-faint dwarf galaxies (UFDs) that orbit M31. We will use UVIS F395N (Ca H&K) and F475W imaging to measure precise metallicities (0.1-0.2 dex) of ~400 stars in 7 M31 UFDs, all of which show diverse and extended star formation that is not clearly compatible with quenching due to reionization, at odds with MW UFDs and expectations from cosmological simulations of galaxy formation. These extended SFHs leave unique imprints on each galaxy's MDF, which encode the signature of baryonic processes that shaped their evolution (e.g., inflows, outflows, stripping, SNe enrichment). From our MDFs we will: (i) measure the strength of feedback-induced outflows, via the mass-loading factor. We will compare them to predictions from cosmological simulations, which underestimate the strength and variation in outflows at low-redshifts and are unconstrained over the mass and age range of our sample; (ii) constrain the physical processes (e.g., stripping, gas depletion) that result in these galaxies quenching at intermediate cosmic epochs (z~2-5); (iii) search for metallicity gradients that have been discovered in some MW UFDs, but whose origins are unclear; (iv) catalog extremely metal-poor star ([Fe/H] < -3.5) candidates that will make for efficient community follow-up in the ELT era.
This program will increase the number of stellar metalliticies in these galaxies by a factor of ~20. Measuring high-fidelity MDFs is only possible due to the excellent blue-sensitivity and angular resolution of HST -- no other ground- or space-based facility can acquire these data.We will obtain F395N imaging of 7 M31 ultra-faint dwarf galaxies using UVIS and new F475W imaging to obtain a sufficient color (temperature) baseline for stellar metallicity measurements. Combined with archival F814W imaging from the HST treasury program GO-15902, we will measure the metallicity distribution functions of each galaxy using well-established photometric metallicity techniques. All visits are 1-2 orbits in duration. In F395N, we obtain orbit-long integrations to aid with alignment to archival data. In consultation with STScI and following past successful HST CaHK programs, we set FLASH=20. In F475W, we integrate two exposures per orbit for four exposures total in order to sample more dither patterns. We match all of our dither patterns to those used by GO-15902. We do not use CR-SPLIT. We do not place constraints on overall orientation, but require that all orbits for each galaxy have the same orientation.Dr. Sal Wanying Fu (program PI) has led multiple studies on HST CaHK narrowband metallicities and abundances in resolved dwarf galaxies. Dr. Daniel Weisz (co-PI) is an expert on resolved stellar populations with HST, the Local Group, color-magnitude diagrams, star formation histories, and the formation and evolution of dwarf galaxies. Fu and Weisz will oversee the execution of this program. Dr. Else Starkenburg is a co-PI of the PRISTINE CaHK survey of the MW and an expert in both theory and observations of metal-poor stars, the Galactic halo, and dwarf galaxies. Dr. Nicolas Martin is a co-PI of the PRISTINE CaHK survey of the MW and is an expert in observations of metal-poor stars and satellite galaxies around the MW and M31, particularly with SDSS, Pan-STARRS, and Keck/DEIMOS. Dr. Patrick Cote is an expert on ground-based observations of nearby galaxies and galaxy groups, particularly with the CFHT. Dr. Andrew Dolphin is an expert on resolved stellar populations, is the author of DOLPHOT, the most widely used PSF photometry reduction routine for HST, and is also author of MATCH, the CMD fitting package that we will use to measure SFHs in this program. Prof. Michael Boylan-Kolchin and Dr. Jenna Samuel are theorists with particular expertise in dwarf galaxies and dark matter, and are members of the FIRE collaboration. They will help facilitate theoretical interpretation of our findings. Dr. Evan Skillman is an expert on dwarf galaxies. Dr. Alessandro Savino is a an expert on resolved stellar populations in nearby galaxies and in CMD analysis and resolved stellar populations. Dr. Nathan Sandford is an expert on stellar stellar spectroscopy and chemical evolution modeling. Dr. Meredith Durbin is an expert on resolved stellar populations in nearby galaxies and performing resolved star photometry on HST images of nearby galaxies. Katie Sharpe is a graduate student working with co-PI Weisz on Local Group stellar spectroscopy.GalaxiesStellar Populations and the Interstellar Medium0falsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF SPHEROIDALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYDWARF SPHEROIDALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYDWARF SPHEROIDALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYDWARF SPHEROIDALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYDWARF SPHEROIDALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYDWARF SPHEROIDALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYDWARF SPHEROIDALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoF395NWFC3/UVISImagingNoNoF395NWFC3/UVISImagingNoNoF395NWFC3/UVISImagingNoNoF395NWFC3/UVISImagingNoNoF395NWFC3/UVISImagingNoNoF395NWFC3/UVISImagingNoNoF395NWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF475WHst Same orient constraint links visits (01 02 03 04 05 06)The scheduling data was generated by CASM 33.1.CASM was run in Phase II mode.1782251189000260.6(Tic-Visit
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