0
Assigned ID: 3101
----- Attempting Submission 1 (Fri Mar 25 01:47:41 GMT 2022) -----
HST Phase I Proposal 3101 successfully submitted.
Receipt: # 3101-1
----- Attempting Submission 2 (Fri Mar 25 18:52:45 GMT 2022) -----
HST Phase I Proposal 3101 successfully submitted.
Receipt: # 3101-2
----- Attempting Submission 3 (Fri Mar 25 20:27:42 GMT 2022) -----
HST Phase I Proposal 3101 successfully submitted.
Receipt: # 3101-3
The list of Investigators does not match the STScI records for this program.
I have added Ben Williams and Wendy Freedman as CoIs following approval by Claus Leitherer on July 11 (for budgetary reasons). Please advise if I should adjust anything in this Phase II.
1100594430
----- Attempting Submission 1 (Wed Jul 13 18:58:34 GMT 2022) -----
I have added Ben Williams and Wendy Freedman as CoIs following approval by Claus Leitherer on July 11 (for budgetary reasons). Please advise if I should adjust anything in this Phase II.
The lowest luminosity galaxy candidates ever discovered outside of the Milky Way
Faint dwarf galaxies are the observational bedrock of small-scale cosmology and galaxy formation. The faintest of these, the ultra-faint satellites of the Milky Way, are particularly informative: as they have formed so few stars, they are very sensitive to the details of dark matter properties, feedback and reionization. While many models have been tuned to reproduce the Milky Way's satellite population well, large variations between the luminosity functions of bright dwarfs in nearby groups coupled with theoretical expectations for variations in ultra-faint populations motivate searches for ultra-faint dwarfs in other groups.
Recent advances in wide-field deep multi-band imaging, star-galaxy separation and dwarf candidate search techniques place us in a position to explore this issue on a statistical footing. Sufficient data exists in five nearby galaxy groups: M31, M81, M64, M83 and M94. We have identified 55 faint and ultra-faint satellite candidates using criteria designed to be as selective and restrictive as possible, while recovering artificial galaxies 3-10x deeper than current limits in these groups. We request 55 SNAPs with ACS and WFC3 in parallel (for local 'background' estimation and legacy stellar halo science) to confirm a subset of this statistical sample. This program will confirm the faintest ever galaxy found outside the Milky Way, will allow measurement of their luminosities and sizes, will provide deep enough color-magnitude diagrams to constrain distance, metallicity and young stellar populations, and will propel robust Local Volume ultra-faint galaxy searches on an industrial scale with next-generation facilities like the Vera Rubin Observatory.
The main observational goal of this program is the confirmation of faint and ultra-faint dwarf galaxy candidates in the M31, M81, M64, M83 and M94 groups through HST ACS imaging, complemented when possible by coordinated parallel WFC3, for background measurement and stellar halo legacy science. These candidates were discovered in the best publicly available ground-based imaging data of nearby galaxy groups. The observations need to:
i) Confirm (or possibly refute) that the clumps of compact objects are indeed stars,
ii) Increase by factors of >4 the number of detected stars, dramatically increasing the significance of the detection, and providing accurate measures of dwarf luminosity,
position, and size.
iii) Provide deeper and more accurate CMDs.
For the latter point, a few particular CMD features are important for our scientific goals.
a) For systems at the distance of M31, a horizontal branch or red clump will be easily visible and provide a distance estimate.
b) For luminous systems M_V<~-7.5, the RGB will be populated enough to provide a TRGB distance estimate sufficient to place it within 0.5 Mpc of the group distance.
c) For ultra-faint systems with poorly populated RGBs, constraints on distance still exist. If the system was substantially closer than the target galaxy group, a horizontal branch/red clump would be seen. If the system is substantially farther away, in order to have the observed apparent magnitude, its absolute magnitude will be bright enough to expect a well-populated TRGB that would yield a background distance measurement.
d) The color of the RGB stars will allow us to obtain metallicity measurements of the UFDs. If young and intermediate-aged stars exist, they may be prominent enough to show up on the high-mass main sequence or as helium burning stars (bluer than the RGB).
There are three different distance ranges for the candidates: M31 distance (~780kpc), M81 distance (~3.5Mpc) and M64 distance (~4.5Mpc). This gives 3 different relevant magnitude limits. In all cases, the dither between CR splits is carried out using a POS TARG instead of a pattern, to allow better packing of prime and parallel exposures.
M31 : In order to reach below the Horizontal Branch, one wants to reach F814W ~ 25.6 and F606W ~ 26.2. Buffer constraints are the driving constraint for such short SNAPs. We are designing the SNAP to be as short as possible given our scientific needs. Our observing plan has either WFC3 as prime (no parallel) for candidates enclosed entirely by the WFC3 field (visits named M31-OBJXXXX), giving a 23 minute long SNAP, or ACS as prime (WFC3 parallel F814W only) for larger candidates (visits named M31A-OBJXXXX), giving a 30 minute long SNAP. For both cameras, the prime fields have 3 frames (2 in F606W, one in F814W), with a cosmic ray split in F606W for a robust stellar catalog and a single F814W frame for color information for the majority of the stars without cosmic ray contamination. Cosmic ray contaminated stars will be excessively red; very red stars (metallicity or dust) are not expected in UFDs, whereas blue stars could be expected (if a satellite has some ongoing star formation, or if it has a blue horizontal branch, for example).
M81 : Our dwarf recovery simulations demonstrate that we must reach S/N of 5 or greater at m_F814W ~ 26.3 and m_F606W ~ 27.3. Our SNAP design has ACS as primary (to enclose the largest possible field for a background value) with 800 and 690s in F606W and F814W respectively; our parallel is somewhat uneven owing to buffer constraints (1175s CR split in F606W, and single 685s exposure in F814W, again optimized for CR split in F606W so as to recover stars bluer than the RGB with confidence). The SNAPs are 44 minutes long.
M64,M83,M94 - Our dwarf recovery simulations demonstrate that we must reach S/N of 5 or greater at m_F814W ~ 26.7 and m_F606W ~ 27.7. To reach these limits, we need longer SNAPs. With buffer constraints in mind, we reach ~1020 and 820s in F606W and F814W with ACS as primary (to enclose the largest possible field for a background value), and ~880 and ~1160s in F606W and F814W with WFC3 in parallel (each with 2 images allowing CR rejection). These SNAPs are longer, nearly 50 minutes long. Our exploration of SNAP completion rates in previous cycles suggests that such long SNAPs are executed comparably often to rather shorter SNAPs); at any rate such exposure times are driven by the science requirements.
Most targets are so diffuse that the positioning of the chip gap isn't critical. Some targets are so compact as to prefer a pointing that is 7-20" from the location using a POS TARG, so as to not land the candidate on the chip gap.
Prof. Eric Bell has expertise in the analysis of resolved star datasets with HST, particularly for the satellite systems and stellar halos of nearby massive galaxies, interpreting these datasets in the light of simulations of galaxy formation and evolution, and analyzing galaxy structural and star formation history properties in the light of galaxy evolution models to constrain the physical processes and ingredients affecting galaxies. Dr. Adam Smercina is a postdoctoral scholar, with experience in resolved stellar populations from ground and space, with particular experience in HST resolved star photometry, SFH fitting with MATCH, dwarf satellite discovery, completeness and characterization. Dr. In-Sung Jang, Dr. Roelof de Jong, Prof. Antonela Monachesi and Prof. Jeremy Bailin have rich and deep experience in data reduction, HST resolved star photometry, artificial star tests, star formation history fitting with IAC-POP, TRGB distance estimation, and measuring the structures of galaxies as a function of stellar population age. Dr. Richard D'Souza, Prof. Oleg Gnedin, Prof. Jeremy Bailin, and Prof. Antonela Monachesi are experts in the creation and use of powerful hydrodynamical simulations of galaxy and dwarf satellite formation in a cosmological context - these simulations will be invaluable in interpreting what we learn about ultra-faint satellites in the Local Volume in a cosmologically-motivated and theoretically-grounded context. Dr. Paul Price, Dr. Colin Slater and Dr. David Nidever are experts in the reduction, analysis and optimization of extremely deep ground-based multi-band survey datasets for resolved star science, and play an important role in reducing and understanding the completeness/contamination of the datasets used to discover these candidates.
Many of the investigators have collaborated previously on the GHOSTS survey, and the team has developed a robust pipeline for the analysis of pipeline-reduced ACS and WFC3 data, including PSF estimation, source detection, photometry, star-galaxy separation, and artificial star tests. The collaboration has developed tools and methods to construct mock satellites and star catalogs from simulation datasets. The collaboration releases the reduced data and pipeline photometry products (including artificial star tests) through MAST (https://archive.stsci.edu/prepds/ghosts/) and a (currently under construction during an upgrade) GHOSTS team page (http://vo.aip.de/ghosts/survey.html), and makes the rest of its results and inferences public in the data tables of publications. The team has published 15 refereed papers using previous HST data.
Galaxies
Stellar Populations and the Interstellar Medium
6
false
SUPPORTED
GALAXY
DWARF SPHEROIDAL
M31 candidate; priority
C02393+2935
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate; Compact
C00667+4010
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate
C01628+4183
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate
C01075+4392
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate; stream-like? ; must be ACS!
C01331+4402
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate; priority
C00851+4685
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate; compact.
C01917+4765
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate.
C02019+2959
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate.
C02432+3090
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate
C02524+3233
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate
C00799+3388
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate
C01317+3520
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate; compact
C01162+4511
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate; very diffuse.
C01713+4570
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate
C01832+3466
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate; priortity.
C01790+4207
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate; diffuse.
C00174+4261
J2000
GALAXY
DWARF SPHEROIDAL
M31 candidate; diffuse.
C02281+3825
J2000
GALAXY
DWARF SPHEROIDAL
M81 candidate; priority
J2000
J2000
GALAXY
DWARF SPHEROIDAL
Smercina17 resolved star discovery
J2000
GALAXY
DWARF SPHEROIDAL
Okamoto19 discovery; resolved stars.
J2000
GALAXY
DWARF SPHEROIDAL
Okamoto19 discovery; resolved stars.
J2000
GALAXY
DWARF SPHEROIDAL
Diffuse light clearly visible
J2000
GALAXY
DWARF SPHEROIDAL
priority
J2000
GALAXY
DWARF SPHEROIDAL
priority
J2000
GALAXY
DWARF SPHEROIDAL
priority
J2000
GALAXY
DWARF SPHEROIDAL
priority
J2000
GALAXY
DWARF SPHEROIDAL
Lower confidence
J2000
GALAXY
DWARF SPHEROIDAL
Lower confidence
J2000
GALAXY
DWARF SPHEROIDAL
M81 candidate; Poss bck GC
C14889+7018
J2000
GALAXY
DWARF SPHEROIDAL
M94 candidate
J2000
GALAXY
DWARF SPHEROIDAL
M94 candidate; priority
C19304+4089
J2000
GALAXY
DWARF SPHEROIDAL
M94 candidate; priority
C19300+4101
J2000
GALAXY
DWARF SPHEROIDAL
M94 candidate
C19336+4085
J2000
GALAXY
DWARF SPHEROIDAL
M94 candidate
C19329+4200
J2000
GALAXY
DWARF SPHEROIDAL
M83 candidate; priority
C20371-3005
J2000
GALAXY
DWARF SPHEROIDAL
M83 candidate; priority
C20309-2926
J2000
GALAXY
DWARF SPHEROIDAL
M83 candidate
C20438-2940
J2000
GALAXY
DWARF SPHEROIDAL
M83 candidate; priority
C20389-2974
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate; priority
C19293+2182
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate; priority
C19561+2198
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate
C19375+2093
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate
C19351+2086
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate
C19427+2372
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate, diffuse light; also dw1258+2329; priority
C19471+2349
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate; diffuse light; priority
ASC19562+2082
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate; diffuse light; priority
ASC19509+2106
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate; diffuse light; priority
ASC19519+2132
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate; diffuse light; priority
ASC19366+2229
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate; diffuse light; SDSS J125259.08+222455.9
ASC19325+2241
SDSSJ125259.08+222455.9
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate; priority
ASC19302+2227
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate; from deep coverage; UCD?; priority
DC19506+2121
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate; from deep coverage; priority
DC19475+2134
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate; from deep coverage; close to M64; priority
DC19433+2154
J2000
GALAXY
DWARF SPHEROIDAL
M64 candidate; from deep coverage
DC19390+2111
J2000
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
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