0 Assigned ID: 6396 ----- Attempting Submission 1 (Thu Apr 10 08:56:29 GMT 2025) ----- HST Phase I Proposal 6396 successfully submitted. Receipt: # 6396-1 ----- Attempting Submission 2 (Thu Apr 10 11:45:55 GMT 2025) ----- HST Phase I Proposal 6396 successfully submitted. Receipt: # 6396-2 ----- Attempting Submission 3 (Thu Apr 10 14:36:14 GMT 2025) ----- Following very helpful conversations with my CS (Chris Clark) I have designed this phase 2. I have three targets, each of which will be centered in the UVIS1 chip. There are 11 orbits per target, and the first orbit for each has an orient constraint, with each subsequent orbit requiring an orient constraint between +/-10 degree of that first expsoure. These constraints imply good scheduability during Jun/Jul/Aug of 2026. If there are any issues, please let me know. 945952265 ----- Attempting Submission 1 (Fri Aug 08 10:28:00 GMT 2025) ----- The Extended Clusters of Andromeda - dwarf galaxies or globular clusters? New survey data continues to blur the boundary between Globular Clusters (GCs), thought to be single stellar populations devoid of dark matter, and dwarf galaxies. The extended clusters (ECs) of Andromeda were first discovered in 2005 and sit right in the gap between these two populations. Given their sizes (half light radii of ~30pc) and brightnesses (Mv ~ -6), it was unclear whether these were puffed up globular star clusters, or faint dwarf galaxies. In the nearly two decades since, we are still unsure of their nature. Spectroscopic data have shown they could be either dark matter dominated or dark matter free, while shallow HST imaging to their horizontal branches have shown them to have stellar populations consistent with either population. One clear method to break this frustrating degeneracy is to measure their star formation histories. GCs form their stars essentially in a single burst, while even the faintest dSphs have star formation that extends over a Gyr or more. By measuring their star formation histories we can determine which class ECs belong to for the first time, offering a unique opportunity to refine our definition of GCs and dwarfs, test GC formation models and refine using galaxy counts of the faintest dwarfs as a cosmological probe. To achieve our goals, we request 33 orbits of WFC3 observations to image three bright ECs down to their oldest main sequence turn-offs. We propose one field of WFC3 imaging for three ECs in M31. We have selected three bright ECs in Andromeda with reliable existing shallow HST data. Our strategy follows previous campaigns that measure SFHs from the oldest MSTO of faint objects in the Local Group. These include the ISLAndS (Skillman et al. 2017) and M31 dSph multi-cycle treasury programs (Savino et al. 2025). We select the F606W-F814W filter combination, and aim to reach a S/N = 10 at the oldest MSTO (MI = +3.0 for ages of 12.5 Gyr or F814W~27.4 for all our objects.). This is the benchmark required for high fidelity recovery of the SFH at ancient ages (e.g. Savino et al 2023, 2025). As we use the same filter set as for all other M31 dwarf galaxies, we can compare directly with the CMDs and SFHs for the full M31 satellite population (Skillman et al 2017; Savino et al. 2022, 2023). The ECs are compact (~30"), fitting easily within the field-of-view of WFC3. This leaves a significant area around the EC in the WFC3 field, allowing us to well-sample the foreground population and clean our observations of contaminants. Our proposed depth means we reliably distinguish between stellar and galaxy sources even at the oldest MSTO (Radburn-Smith 2011) as the photometric uncertainties do not dominate the observations. Ground based telescopes cannot reach the oldest MSTO stars in the M31 ECs. HST is therefore essential in unlocking the nature of Extended Clusters. While JWST would allow a determination of the SFHs, HST allows us to compare directly with the previous EC observations, and the full M31 satellite system. To reach our precision of S/N = 10 at the MSTO, we require exposure times of 9,051 sec in F606W and 19,640-sec in F814W for each EC. Including standard overheads, this results in 11 orbits per EC, giving a total request of 33 orbits. We will use 4-point dither patterns to achieve 0.5 pixel sampling. The data will be reduced and analyzed with standard well-tested methods. The DOLPHOT stellar photometry package will measure the point spread function photometry (e.g. Dolphin et al. 2000; Monelli et al. 2010) using a similar setup to the Panchromatic Hubble Andromeda Treasury survey (PHAT, Williams et al. 2014). We will perform artificial star tests on our final images to accurately determine photometric errors and incompleteness in each band. We exploit the excellent S/N at the oldest MSTO to compute detailed SFHs and measure the duration of star formation with a precision of < 500 Myr. The difference in the stellar populations at the MSTO will clearly be seen in our data, as shown in Fig. 2 where we show model CMDs for a GC and dSph with the brightness of our targets, as well as the difference between them in the Hess diagram. The SFHs will be derived using CMD fitting software MATCH, which has been previously used to obtain SFHs from comparably deep HST imaging for M31 dwarf galaxies (e.g. Savino et al. 2025). As stellar evolution models are the key systematic uncertainty in CMD modeling, we plan to run SFHs using at least two different stellar evolution models (PARSEC, Bressan et al. 2012 and BASTI, Pietrinferni et al. 2004, Hidalgo et al. 2018) and to obtain mock stellar models that include systematic shifts in the stellar evolutionary tracks, luminosities and temperatures. We will position our ECs in the center of one of the two WFC3 chips. Once the first observations begin, we require the same orient to be used throughout so that we can sample the faint background and foreground contaminating populations well, without the need for parallel observations. All of our objects have been observed with HST ACS/WFC before as part of program 10394. However, these shallow observations (2 orbits) only reach the RGB and HB, features common to both old clusters and dwarf galaxies, and thus insufficient for SFH analysis Astha is a PhD student working on the mass-metallicity relation of dwarf galaxies and has experience of working with imaging data. Dr Collins has extensive experience working with resolved stellar populations of Local Group dwarf galaxies, both from photometry and spectroscopy. She was the PI for a successful cycle 25 program to obtain deep HST imaging for Andromeda XIX, a dwarf galaxy of M31. She led the paper from this work (Collins et a. 2020), where the photometry has been used to measure a detailed star formation history for the galaxy. She was also co-I on successful HST Treasury Survey of the M31 Satellite System program (GO-15902) to obtain deep imaging for the satellites of Andromeda. This has led to three papers so far presenting the RR-Lyrae distances to all the galaxies and deep star formation histories for all of the faintest dwarfs (Savino et al. 2022, 2023, 2025). These programs all use the methods proposed for the analysis of these HST data. Dr Doliva-Dolinsky has extensive experience in studying dwarf galaxies around Andromeda and further afield. She is experienced with photometry and deriving survey completeness limits. Ms. Gray is an expert in the EDGE simulations, with a focus on the formation of nuclear and globular clusters. Dr Hutton is an expert in resolved stellar populations and comparisons between observations and simulated data for Local Group objects. Mrs Navabi is an expert in photometric data reduction of both ground and space based data. She is also experienced in measuring structural properties of Local Group dwarf galaxies. Dr Noel has extensive experience in deriving SFH from deep data, particularly for LG galaxies. She is an expert in resolved stellar populations as a tool to understand galaxy evolution. Mr. Pickett has experience in measuring the properties and detailed mass profiles of Andromeda satellite galaxies. Prof. Read is a leading expert in simulating dwarf galaxies and globular clusters, and is the PI of the EDGE simulations, which this program will use to interpret our measured SFHs and chemistries. Dr Rich is a leading expert in studying the resolved stellar populations of GCs, dSphs and the Milky Way bulge. He has led and contributed to many HST proposals over the years, including the Treasury Survey of M31 satellite systems. Dr Sakowska is an expert in the derivation of SFHs for nearby galaxies, in particular the Small Magellanic Cloud. She is also involved in large surveys such as DELVE to find and study Local Group dwarf galaxies. Dr Taylor is leading the analysis of GCs and dSphs in the EDGE simulations. Stellar Populations and the Interstellar Medium 6 false false false false false false SUPPORTED EXT-CLUSTER GLOBULAR CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 EXT-CLUSTER GLOBULAR CLUSTER NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 EXT-CLUSTER GLOBULAR CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 The scheduling data was generated by CASM 33.0. CASM was run in Phase I mode. 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CASM was run in Phase II mode. (Tic-Visit :proposal-id 18020 :visit-id "11" :proposal-version -1 :trans-version "20250624" :date "08-Aug-2025 11:13:43.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1154976 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18020 :visit-id "11" :obset-id "11" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18020 :visit-id "11" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2620 :al-overhead-at-end 116 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18020 :visit-id "11" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2620 :al-overhead-at-end 116 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) true 2 0 /private/var/folders/zj/ctdhn9fj24d8lbxm3dtrwysm0000gq/T/OPVisit5832502962882259860.xml The scheduling data was generated by CASM 33.1. CASM was run in Phase II mode. (Tic-Visit :proposal-id 18020 :visit-id "12" :proposal-version -1 :trans-version "20250624" :date "08-Aug-2025 11:13:44.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 577488 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18020 :visit-id "12" :obset-id "12" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18020 :visit-id "12" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2620 :al-overhead-at-end 116 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) true 1 0 /private/var/folders/zj/ctdhn9fj24d8lbxm3dtrwysm0000gq/T/OPVisit3693274054001720703.xml The scheduling data was generated by CASM 33.1. CASM was run in Phase II mode. (Tic-Visit :proposal-id 18020 :visit-id "15" :proposal-version -1 :trans-version "20250624" :date "08-Aug-2025 11:17:12.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1154976 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18020 :visit-id "15" :obset-id "15" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18020 :visit-id "15" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2612 :al-overhead-at-end 116 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2992 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18020 :visit-id "15" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2612 :al-overhead-at-end 116 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2992 :pcs-gap 0 ) true 2 0 /private/var/folders/zj/ctdhn9fj24d8lbxm3dtrwysm0000gq/T/OPVisit15417643839730079956.xml The scheduling data was generated by CASM 33.1. CASM was run in Phase II mode. (Tic-Visit :proposal-id 18020 :visit-id "16" :proposal-version -1 :trans-version "20250624" :date "08-Aug-2025 11:17:12.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1154976 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18020 :visit-id "16" :obset-id "16" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18020 :visit-id "16" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2612 :al-overhead-at-end 116 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2992 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18020 :visit-id "16" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2612 :al-overhead-at-end 116 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2992 :pcs-gap 0 ) true 2 0 /private/var/folders/zj/ctdhn9fj24d8lbxm3dtrwysm0000gq/T/OPVisit9279568362215863007.xml The scheduling data was generated by CASM 33.1. CASM was run in Phase II mode. (Tic-Visit :proposal-id 18020 :visit-id "17" :proposal-version -1 :trans-version "20250624" :date "08-Aug-2025 11:17:13.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1154976 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18020 :visit-id "17" :obset-id "17" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18020 :visit-id "17" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2612 :al-overhead-at-end 116 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2992 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18020 :visit-id "17" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2612 :al-overhead-at-end 116 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2992 :pcs-gap 0 ) true 2 0 /private/var/folders/zj/ctdhn9fj24d8lbxm3dtrwysm0000gq/T/OPVisit11403321592186067319.xml The scheduling data was generated by CASM 33.1. CASM was run in Phase II mode. (Tic-Visit :proposal-id 18020 :visit-id "18" :proposal-version -1 :trans-version "20250624" :date "08-Aug-2025 11:17:13.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 577488 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18020 :visit-id "18" :obset-id "18" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18020 :visit-id "18" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2612 :al-overhead-at-end 116 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2992 :pcs-gap 0 ) true 1 0 /private/var/folders/zj/ctdhn9fj24d8lbxm3dtrwysm0000gq/T/OPVisit17895601187017577858.xml The scheduling data was generated by CASM 33.1. CASM was run in Phase II mode. (Tic-Visit :proposal-id 18020 :visit-id "06" :proposal-version -1 :trans-version "20250624" :date "08-Aug-2025 11:10:14.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 577488 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18020 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18020 :visit-id "06" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2620 :al-overhead-at-end 116 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) true 1 0