Second Cycle 28 submission
979433984
Assigned ID: 191
----- Attempting Submission 1 (Wed Mar 04 22:42:07 GMT 2020) -----
HST Phase I Proposal 191 successfully submitted.
Receipt: # 191-1
----- Attempting Submission 2 (Thu Mar 05 21:00:26 GMT 2020) -----
6/30/2020 First submission. Note that I have dropped one orbit (F110W/F160W) from target UGC 8091 following the duplication report from the TTRB.
6/30/2020 Second submission: changed aperture to IR-UVIS-FIX from IR-FIX to enable greater overlap between the UVIS observations and the IR observations. The UVIS observations use the UVIS-IR-FIX aperture.
9/17/2020: Revision: this version switches the order of F110W/F160W in visits 21, 25, 28, 31, & 34 to mitigate issues with He I airglow
10/20/2020: Revision: constraining the orient in visits 25 and 31 & combining the two WLM-POS2-IR visits into a single visit (new visit 35) --> these changes ensure the same parallel field is observed for both F606W and F814W.
256279275
----- Attempting Submission 1 (Tue Jun 30 15:39:34 GMT 2020) -----
HST Phase II Proposal 16162 successfully submitted.
Receipt: # 16162-1
----- Attempting Submission 2 (Wed Jul 01 00:26:14 GMT 2020) -----
HST Phase II Proposal 16162 successfully submitted.
Receipt: # 16162-2
----- Attempting Submission 3 (Thu Sep 17 17:24:00 GMT 2020) -----
----- Attempting Submission 4 (Tue Oct 20 16:56:46 GMT 2020) -----
Solving the metallicity dependence of evolved star evolution and completing HST's near-IR legacy in the Local Volume
Thermally-pulsing (TP-)AGB stars and red helium-burning (RHeB) stars dominate the near-infrared (NIR) flux in star-forming galaxies (up to 70%) and thus have a strong impact on the appearance of galaxies. These stars are notoriously difficult to model, and the only empirical constraints on their evolution come from the Magellanic Clouds, at just 20% and 50% solar metallicity. Lower metallicity models are entirely uncalibrated and these uncertainties propagate to stellar population synthesis, leading to (sometimes wildly) inaccurate derived galaxy properties such as the star-formation rate and stellar mass. The HST is capable of rectifying this. By adding NIR and some additional optical imaging to existing optical and UV imaging of an optimally selected sample of nearby (< 3.1 Mpc) metal-poor dwarf galaxies, we can produce observables (luminosity functions, stellar counts, CMD morphology, stellar SEDs) that stringently constrain the metallicity dependencies on the processes that drive model uncertainties, including mass loss, dredge up, convective overshoot, and rotation. Understanding the metallicity dependence of these parameters is invaluable to interpreting observations of metal-poor galaxies, which dominate the number density of galaxies in the Universe. Given the prior HST investment of observations in these galaxies, this relatively modest amount of observing time promises to revolutionize the field and leave a lasting HST legacy in the Local Volume.
All targets overlap UV coverage from program 15275 (PI Gilbert).
Orbits split into multiple visits per target.
We do not anticipate that reduced gyro mode would negatively affect these observations. We have no orientation restrictions.
Orbits designed following Table 1 in the approved proposal, which outlines which targets are being observed in which filters and at what depth.
========================
IR Medium-band observations (19 orbits)
3 Filters: F127M, F139M, F153M
Total depth for each filter is ~800-900s
Dithers added manually in [x/y]postargs to minimize unused orbit, following the WFC3-IR-DITHER-LINE-3PT pattern.
Nyquist sampling will be obtained by bootstrapping to wide IR data obtained here or from other programs that have 4 dither positions.
========================
IR Wide-band observations (20 orbits)
2 Filters: F110W, F160W
Total depth for each filter is ~1100-1300s
4-point dithers employed, sometimes entered manually, following WFC3-IR-DITHER-BOX-MIN.
***Cutting the wide-band IR orbit for target UGC 8091, as directed by the TTRB, because it duplicates observations in program 16292 (PI Choi).
========================
UVIS F475W observations (11 orbits)
1 Filter: F475W
Total depth is 1 orbit, individual images have depth of approx. 830s.
3-point dither: WFC3-UVIS-LINE-3PT
Lowest expected background on other observations of F475W is 21.2 e/pix. with a 830s exposure.
========================
ACS parallels (13 orbits)
Parallels in F606W and F814W attached to IR wide and/or IR medium orbits for 7 targets. Available depth split approximately evenly between both filters.
========================
resubmission revision: switched the order of F110W/F160W in visits 21, 25, 28, 31, & 34 to mitigate issues with He I airglow
resubmission 10/20/20: combined the WLM-POS2 IR orbits into a single visit (visit 35) so that the parallels fields are the same. TTRB approved additional +/3 degree orient constraints to visits 25 and 31 to make sure the parallel fields are the same as visits 26 and 30, respectively (visits 36 and 30 have already been observed).
Our team includes members of multiple Treasury, large GO, and Archival programs of resolved stellar populations in the Local Group and Volume (e.g., PHAT, ANGST, ANGRRR, ANGST-SNAP, GHOSTS). We have observed, reduced, analyzed, and disseminated >1500 orbits of HST imaging, resulting in publicly released photometry in excess of 100 million stars. All necessary software, analysis, and data dissemination tools are in place and tested, maximizing the efficiency of our scientific program while minimizing the time needed to release high level data products. Our team also includes key members of the Padova modeling group - experts in evolve star evolution.
Boyer and Williams will lead the data processing with input from Dolphin, author of DOLPHOT. Gordon will lead SED analysis with the BEAST tool. The BEAST is publicly available and ready for use - our team continuously improves on its capabilities (Gordon, Hagen, Goldman). Photometry, images, and SED fits will be released via a database interface developed for PHAT. Science will be coordinated through working groups: RHeB/BHeB stars (McQuinn, Rosenfield, Boyer, Girardi, Marigo, Costa, Guhathakurta), TP-AGB stars (Boyer, Girardi, Marigo, Pastorelli, Goldman, Rosenfield), dust (Gordon, Dalcanton); SFHs (Williams, Weisz, Gilbert, McQuinn); SFR indicator calibration (Guhathakurta, Weisz, Williams, Gilbert, Dalcanton, Skillman, Dolphin); stellar halos (Gilbert, Williams, Boyer).
Stellar Populations and the Interstellar Medium
Stellar Physics and Stellar Types
6
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false
false
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SUPPORTED
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WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/IR
Imaging
No
No
F153M
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/IR
Imaging
No
No
F153M
WFC3/UVIS
Imaging
No
No
F475W
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/IR
Imaging
No
No
F153M
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F475W
WFC3/IR
Imaging
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No
F127M
WFC3/IR
Imaging
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No
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WFC3/IR
Imaging
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Imaging
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Imaging
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No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/IR
Imaging
No
No
F153M
WFC3/UVIS
Imaging
No
No
F475W
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
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No
F160W
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/IR
Imaging
No
No
F153M
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
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No
F139M
WFC3/IR
Imaging
No
No
F153M
WFC3/UVIS
Imaging
No
No
F475W
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
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No
F160W
WFC3/IR
Imaging
No
No
F127M
WFC3/IR
Imaging
No
No
F139M
WFC3/IR
Imaging
No
No
F153M
WFC3/UVIS
Imaging
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No
F475W
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No
F127M
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No
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F153M
WFC3/IR
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WFC3/IR
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F160W
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F127M
WFC3/IR
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No
F139M
WFC3/IR
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WFC3/UVIS
Imaging
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F475W
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F127M
WFC3/IR
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F139M
WFC3/IR
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No
F153M
ACS/WFC
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F606W
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No
F814W
WFC3/UVIS
Imaging
No
No
F475W
WFC3/IR
Imaging
No
No
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WFC3/IR
Imaging
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No
F160W
WFC3/IR
Imaging
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No
F127M
WFC3/IR
Imaging
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No
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WFC3/IR
Imaging
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No
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WFC3/IR
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WFC3/IR
Imaging
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WFC3/IR
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WFC3/IR
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WFC3/IR
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ACS/WFC
Imaging
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No
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No
No
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No
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WFC3/IR
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(Tic-Orbit
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true
2
0
The scheduling data was generated by CASM 28.2.
CASM was run in Phase II mode.
1604948661000
278.6839699836695
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(Tic-Orbit
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true
2
0
The scheduling data was generated by CASM 28.2.
CASM was run in Phase II mode.
1604182297000
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(Tic-Visit
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(Tic-Obset
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:low-sky "N"
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)
true
1
0
The scheduling data was generated by CASM 28.2.
CASM was run in Phase II mode.
TTRB approved the addition of an +/- 3 degree orient tie to visit 26 so that the parallel field is the same for both orbits. -- MB 10/20/20
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)
true
1
0
The scheduling data was generated by CASM 28.2.
CASM was run in Phase II mode.
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true
1
0
The scheduling data was generated by CASM 28.2.
CASM was run in Phase II mode.
1603600128000
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(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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)
true
1
0
The scheduling data was generated by CASM 28.2.
CASM was run in Phase II mode.
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(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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:low-sky "N"
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)
true
1
0
The scheduling data was generated by CASM 28.2.
CASM was run in Phase II mode.
1604691574000
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(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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)
true
1
0
The scheduling data was generated by CASM 28.2.
CASM was run in Phase II mode.
1602081079000
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(Tic-Visit
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false
1
0
The scheduling data was generated by CASM 28.2.
CASM was run in Phase II mode.
TTRB approved the addition of an +/- 3 degree orient tie to visit 30 so that the parallel field is the same for both orbits. -- MB 10/20/20
1605924649000
50.91672
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true
1
0
This is a HOPR repeat for failed visit 36
TTRB approved the addition of an +/- 3 degree orient tie to visit 30 so that the parallel field is the same for both orbits. -- MB 10/20/20
1608058238000
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(Tic-Obset
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(Tic-Orbit
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false
1
0
The scheduling data was generated by CASM 28.2.
CASM was run in Phase II mode.
1605799420000
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(Tic-Visit
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(Tic-Obset
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)
true
1
0
The scheduling data was generated by CASM 28.2.
CASM was run in Phase II mode.
This is a new visit that combines the original visists 33 & 34 into a single visit so that the PA is the same for both orbits. -- MB 10/20/20
1609070423000
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(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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true
2
0