Cannot find file /Users/kmcquinn/astro/proposals/hst/cycle31/ufds_candidates/McQ_HST31_ufd_candidates_v1.pdf0Assigned ID: 4166
----- Attempting Submission 1 (Tue May 23 20:04:14 GMT 2023) -----
HST Phase I Proposal 4166 successfully submitted.
Receipt: # 4166-1
----- Attempting Submission 2 (Wed May 24 13:16:45 GMT 2023) -----The number of orbits used exceeds the number allocated
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 browserLeo B: 6/21/24
NEW orbit
Reduced total orbit time to 3128 to allow schedulablity in RGM
Reduced integration times in the first prime and parallel exposures to reflect new total orbit time.
Added flash=6 to the first wfc3 f606w exposure
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previous changes:
have added flash=6 to the first wfc3 f606w exposure for cetus-k-1469576778----- Attempting Submission 1 (Wed Sep 13 13:42:10 GMT 2023) -----
----- Attempting Submission 2 (Fri Sep 15 16:08:41 GMT 2023) -----
----- Attempting Submission 3 (Mon Sep 25 17:01:24 GMT 2023) -----
----- Attempting Submission 4 (Tue Oct 03 12:13:33 GMT 2023) -----
----- Attempting Submission 5 (Wed Jan 24 19:07:56 GMT 2024) -----
HST Phase II Proposal 17481 successfully submitted.
Receipt: # 17481-5
----- Attempting Submission 6 (Wed Jan 24 22:59:37 GMT 2024) -----
HST Phase II Proposal 17481 successfully submitted.
Receipt: # 17481-6
----- Attempting Submission 7 (Mon Jan 29 14:35:01 GMT 2024) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 8 (Mon Jan 29 17:27:33 GMT 2024) -----working with Carol to iterate on phase ii.Discovery of Six Isolated Ultra-Faint Dwarf Galaxy Candidates in the Local GroupUltra-faint dwarf galaxies are the least luminous, most dark matter dominated, and least chemically evolved galaxies known. Detailed studies have shown that their star formation quenched at early times, which is generally thought to be caused by reionization and stellar feedback. Intriguingly, the recently discovered, relatively isolated ultra-faint dwarf, Pegasus W, has had an extended star formation history, suggesting it was not quenched by reionization and contradicting the generally accepted framework that reionization ubiquitously quenches ultra-faint dwarfs. This suggests that, in addition to reionization, environment may play a role in quenching ultra-faint dwarfs.
Pegasus W is thought to be the tip-of-the-iceberg of a population of low mass halos in the Local Group at farther distances that have yet to be detected. Indeed, we have found six ultra-faint dwarf galaxy candidates that appear to be in the Local Group, but, similar to Pegasus W, outside the halos of the MW, M31, and the LMC. Here, we propose 1-orbit of HST imaging per target to confirm these systems are bona fide ultra-faint dwarf galaxies and characterize their properties. The data will be of sufficient depth to (i) robustly measure their distances via horizontal branch stars, (ii) determine the systems' structural parameters and total luminosities, and (iii) derive the star formation histories, placing constraints on the quenching timescales. We will explore the role of enviroment in determining their properties via comparison with Pegasus W as well as ultra-faint dwarf galaxies that are satellite galaxies, all as a fuction of distance to a massive host.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 6 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 intervals, which has been approved via PCR 92614.
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.Our team is comprised of scientists responsible for the discovery and characterization of the ultra-faint dwarf galaxy Pegasus W. PI McQuinn and Co-I Cohen are experts on resolved stellar populations, mesauring distances to galaxies, and recosntructing star formation histories, and measuring the structural parameters to galaxies. They both have significant 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. Mao, Shih, and Buckley are all experts on dark matter and built the basis of the search algorithm used to find the galaxy candidates. 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 knowledge of stellar populations.Stellar Populations and the Interstellar Medium6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF SPHEROIDALJ2000J2000GALAXYDWARF SPHEROIDALJ2000J2000GALAXYDWARF SPHEROIDALJ2000J2000GALAXYDWARF SPHEROIDALJ2000J2000GALAXYDWARF SPHEROIDALJ2000J2000GALAXYDWARF SPHEROIDALJ2000J2000GALAXYDWARF SPHEROIDALJ2000J2000ACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814W3267The scheduling data was generated by CASM 31.1.CASM was run in Phase II mode.170462730200084.0(Tic-Visit
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