Cannot find file /Users/kmcquinn/Dropbox/research_2022/proposals/hst/mid_cycle29/hammertime/McQ_HST29_hammer_v3.pdfWe were notified that the previous proposal submission did not have the 'mid-cycle' box checked.
We have updated our installed APT version and have now selected that option.
Thanks! Kristen McQuinn-1996299387Assigned ID: 2676
----- Attempting Submission 1 (Mon Jan 31 15:54:48 GMT 2022) -----
HST Phase I Proposal 2676 successfully submitted.
Receipt: # 2676-1
----- Attempting Submission 2 (Mon Jan 31 19:40:10 GMT 2022) -----0----- Attempting Submission 1 (Mon Mar 28 13:02:37 GMT 2022) -----
HST Phase II Proposal 16916 successfully submitted.
Receipt: # 16916-1
----- Attempting Submission 2 (Mon Mar 28 13:16:02 GMT 2022) -----
HST Phase II Proposal 16916 successfully submitted.
Receipt: # 16916-2
----- Attempting Submission 3 (Wed Apr 06 13:17:07 GMT 2022) -----
----- Attempting Submission 4 (Tue Mar 14 21:06:21 GMT 2023) -----This Phase II resubmission is to re-observe 1 target (LeoK) whose original observations were
unusable due to a guide star acquisition failure. The visit planner has been re-run for the new data,
but not for the already successfully completed visits in this program.Discovery of 3 Ultra-Faint Dwarf Candidates Outside the MW HaloThe lowest mass galaxies known to date - aptly named 'ultra-faint dwarf galaxies' - orbit the Milky Way (MW) as satellites. Follow-up study of these objects have revealed systems that are the oldest, most metal-poor, and most dark matter-dominated galaxies known. They hold the potential for constraining dark matter on small scales, placing limits on the mass threshold for successful galaxy formation, and defining the impact reionization has on small galaxy halos. Such galaxies are predicted to be present in large numbers in the Local Group (and throughout the universe), yet they have belied detection due the challenges in finding instrinsically small and faint systems in a very big sky.
We have discovered three ultra-faint dwarf galaxy candidates in the Dark Energy Spectrscopic Instrument (DESI) Legacy imaging data located outside the halo of the MW at distances estimated to be between 0.4-0.7 Mpc. In contrast to the population of ultra-faint dwarfs discovered as satellites of the MW, these galaxy candidates appear to be outside the halo of the MW system, providing a unique opportunity to test galaxy formation theories without the competing effects of a halo environment. We request 1 orbit of HST per target to confirm their detection, measure secure distances, and determine their structural properties. Their properties will be compared with those of ultra-faint dwarf satellites of MW and M31, as well as isolated very low-mass galaxies. We will determine their star formation histories from their resolved stellar populations to test whether they are quenched, have extended (or delayed) star formation over cosmic times, or distinct characteristics.The observations included ACS/WFC and WFC3/UVIS imaging in the F606W and F814W filters. The data will be used to confirm that the targets are galaxies, measure the distances to the systems from resolved stars (TRGB and/or Horizontal Branch methods), characterize the stellar properites (star formation histories and metallicities), and measure the structural parameters of the galaxies. The parallel pointings will allow us to observe a field region next to our targets. We will thus be able to estimate more precisely the number of background/foreground contaminants present in our ACS fields.
Each of the 3 targets will be observed for 1 orbit. We use a 5x5 pixel dither implemented using pos-targ (equivalent to the ACS WFC DITHER LINE pattern #14) to reject cosmic rays and handle hot pixels. The first pointing is executed with both filters in ACS and with both filters in WFC3 parallel fields. After the dither, the observations are then repeated. The exposure time per orbit is split roughly equally between the F606W and F814W filters.
In order to obtain 4 exposures in both ACS and WFC3 in one orbit and accomodate buffer dumps during exposures, we have added a special requirement to the visibility interval (following the counsel of the STScI help desk). This did not impact schedulablity appreciably.
Each visit is 1-orbit. We have place ORIENT constraints to ensure we maximum coverage of the stellar disk and prevent the galaxy centers from falling in the ACS chip gap, while avoiding nearby bright stars.PI McQuinn is an expert on resolved stellar populations, mesauring distances to galaxies, and recosntructing star formation histories. She has deep expertise with HST images and will be primarily responsible for the data handling. Dr. Mao brings expertise in the formation of low-mass galaxies in the context of CDM and hierarchical structure formation and has experience studying low-mass satellites around Milky Way analog galaxies in the SAGA survey. Drs. Shih and Buckley are both experts on dark matter and built the basis of the search algorithm used to find the galaxy candidate. Dr. Dolphin, author of the photometry software DOLPHOT and the CMD-fitting code MATCH that we will use on the data, brings significant technical expertise and deep knowledge of stellar populations.Stellar Populations and the Interstellar Medium3falsefalsefalsefalsefalsetruefalsefalseSUPPORTEDGALAXYDWARF SPHEROIDALJ2000J2000GALAXYDWARF SPHEROIDALJ2000J2000GALAXYDWARF SPHEROIDALJ2000J2000ACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WThe scheduling data was generated by CASM 30.1.CASM was run in Phase II mode.32851673387326000278.04132032163125(Tic-Visit
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