0Assigned ID: 7075
----- Attempting Submission 1 (Tue Apr 14 15:57:24 GMT 2026) -----
HST Phase I Proposal 7075 successfully submitted.
Receipt: # 7075-1
----- Attempting Submission 2 (Wed Apr 15 16:43:00 GMT 2026) -----
HST Phase I Proposal 7075 successfully submitted.
Receipt: # 7075-2
----- Attempting Submission 3 (Thu Apr 16 15:16:23 GMT 2026) -----
HST Phase I Proposal 7075 successfully submitted.
Receipt: # 7075-3
----- Attempting Submission 4 (Thu Apr 16 15:32:06 GMT 2026) -----Could not connect to APT Status Server
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
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
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
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
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
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 browserI believe that this will complete my phase II planning for HST-GO-18406.
There are a small number of changes relative to that which was stated previously:
1) Some of the field centers have been moved, by less than an arcminute, to better overlap with JWST data, which was an aim discussed in the proposal.
2) The 2-field mosaics of each field are now completed by a combination of a small shift in RA/DEC, and an orient angle difference of between 20 and 180 degrees. That is to deal with CTE issues.
3) To mitigate for cosmic rays, individual exposures in F390W have been reduced from 2400 seconds to 2x1100 seconds. That in turn necessitates mitigating for CTE, so I added a flash of 7 electrons to every F390W exposure.-925957931----- Attempting Submission 1 (Wed Aug 12 19:49:52 GMT 2026) -----These are flash -related warnings which I have accounted for.Measuring Andromeda's Alpha-Element Enrichment in 100,000 Red GiantsThe bimodal distribution of stars in the [alpha/Fe] -[Fe/H] plane of the Milky Way is among the most debated signatures in Galactic archaeology, separating an old, alpha-enhanced thick disk from a younger, alpha-poor thin disk. Whether this bimodality is a peculiarity of our Galaxy or a generic feature of large disk galaxies remains unknown. Simulations disagree sharply, and no comparable galaxy has been studied with sufficient sample size and chemical resolution to arbitrate. Andromeda (M31) is the nearest galaxy where this can be resolved observationally.
We propose HST imaging in F390W+F606W toward four fields spanning M31's bulge and disk. These sightlines are selected to overlap archival JWST imaging and spectroscopy, and to trace Andromeda's chemical enrichment with galactocentric radius. The F390W filter, situated where iron-peak line blanketing dramatically suppresses stellar flux relative to alpha-element opacity, provides sensitivity to [Fe/H] independently of bulk metallicity, breaking the degeneracy limiting optical or infrared photometry. Combined with archival JWST/NIRCam and HST photometry, fitting the spectral energy distributions will yield joint [Fe/H] and [alpha/Fe] posteriors for ~100,000 red giants, the largest chemically-resolved stellar sample ever assembled beyond the Milky Way. Spectra from archival JWST/NIRSpec programs provide ~300-star validation samples. As byproducts, the survey yields a precise M31 extinction curve and targeting diagnostics for future campaigns.
This method can be applied to a handful of large, nearby galaxies (e.g. M33, NGC 300), and eventually dozens more with the Habitable Worlds Observatory's ultraviolet capabilities.Four fields of Andromeda's disk are observed in primary + parallel. These fields are called (from outer to inner disk) Nidever's window, Mackereth's window, Sanford's window, and M31-BULGE-PHAT-BRICK-01-EAST. The first three fields are named after the PIs that got JWST-GO programs (2609, 2301, 4735) approved toward these fields, where they obtained both NIRCam and NIRSpec data. The fourth field is named after the PHAT brick (PI: Dalcanton) on which it is located, and will be the subject of coordinated JWST observations approved with this program (JWST-GO-12720).
For each field, the aim is to align the primary WFC3 observations (F390W and F606W) with the JWST data. There are 10 orbits for each field, of which 8 go to F390W observations, and 2 go to F606W observations. These are in turn split into two subsets, totalling 3 visits and 5 orbits total, where the two subsets are offset by a small shift of 30 arcseconds in each of RA and DEC, and an orient angle shift of between 20 and 180 degrees. That offset and orient angle shift is to help account for detector artefacts such as CTE. The overlap of approximately 70% will produce deeper, more precise imaging in F390W.
The parallel observations are taken with ACS. At 10 orbits per field, there are 4 orbits associated with F435W, 4 orbits associated with F625W, and 2 orbits associated with F555W. These were discussed in the proposal as having two uses: legacy value as these are filters that were not imaged with the Panchromatic Hubble Andromeda Treasury, and also to help study the extinction curve in Andromeda.PI David Nataf is an expert on resolved stellar populations and on the study of the interstellar extinction curve.
Michael Rich, Gail Zasowski, Ricardo Schiavon, Danny Horta, David Nidever, and Michael Hayden are experts on Local Group stellar populations in both of the imaging and spectroscopic domains.
Gail Zasowsksi, Rachel Pauline, and David Nidever are experts on the study of interstellar extinction.
Sarah Loebman, Megan Barry, and Rosemary Wyse are experts on the chemodynamics of stellar populations, and theior use as tracers of galaxy evolution.
Christian Johnson, Gagandeep Anand, and Domenico Nardiello are experts on data reduction with space-based imaging.
Santi Cassisi is an expert on stellar evolution models.Stellar Populations and the Interstellar MediumGalaxies6falsefalsefalsefalsefalsefalsefalsetruePRIMARY7trueSUPPORTEDGALAXYDISKJ2000J2000GALAXYDISKJ2000J2000GALAXYDISKJ2000J2000GALAXYDISKJ2000J2000WFC3/UVISImagingNoNoF390WWFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF625WWFC3/UVISImagingNoNoF390WWFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF625WWFC3/UVISImagingNoNoF390WWFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF625WWFC3/UVISImagingNoNoF390WWFC3/UVISImagingNoNoF606WPOS-TARGDITHER0.145LINEfalsefalse346.84WFC3-UVIS-DITHER-LINE3false/private/var/folders/wp/mj71n53j5z10ygyyzht3m9_c0000gn/T/OPVisit16840361970120742856.xmlHst Same orient constraint links visits (01 02 03)The scheduling data was generated by CASM 34.2.CASM was run in Phase II mode.Each prime+parallel group corresponds to a dither point, this is for dither points 1 and 2(Tic-Visit
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