0
Assigned ID: 994
----- Attempting Submission 1 (Fri Apr 11 22:54:48 GMT 2014) -----
HST Phase I Proposal 994 (smc_cycle22.apt) successfully submitted.
----- Attempting Submission 2 (Fri Apr 11 23:25:53 GMT 2014) -----
HST Phase I Proposal 994 (smc_cycle22.apt) successfully submitted.
----- Attempting Submission 3 (Fri Apr 11 23:33:06 GMT 2014) -----
Changes for Visits 4 & 5 orient 191.5 192.7. Shifted positions of relevant fields.
-1401508171
----- Attempting Submission 4 (Wed Nov 19 00:54:56 GMT 2014) -----
----- Attempting Submission 5 (Wed Apr 22 19:04:18 GMT 2015) -----
These have been run before.
A New View of Dust at Low Metallicity: The First Maps of SMC Extinction Curves
In order to constrain basic dust physics and anchor the interpretation of both UV/optical extinction and IR emission at low and high redshifts, we propose seven-filter photometry of a key region in the Small Magellanic Cloud (SMC). Via a cutting-edge technique demonstrated to work in M31 we will use these data to construct the first ever maps of the extinction curve shape (Rv), 2175 Angstrom bump strength, and dust column (Av) across a low metallicity environment. These maps will allow us to (1) measure the true distribution of extinction curves in the SMC, which is frequently used as a template for low metallicity extinction; (2) rigorously test whether PAHs are the carriers of the 2175 Angstrom extinction feature; and (3) place the estimation of dust masses from IR emission in low metallicity systems on a firm empirical and observational footing. Dust regulates the structure and evolution of interstellar medium (ISM) and shapes the optical and ultraviolet emission of galaxies. Its emission at infrared and mm wavelengths represents a powerful tool to probe the ISM out to the highest redshifts. Understanding the physics and interpretation of dust absorption and emission as a function of metallicity is critical to a vast range of science and mapping key dust properties is a new application, uniquely possible with UV through NIR imaging from HST. As such, we expect this program to have wide ranging scientific impact.
Our observations cover a 12 arcmin by 6.5 arcmin region with 9 HST broadband filters, with WFC3 and ACS operated in parallel in each orbit. The observing design is based on the strategy from the Pan-chromatic Hubble Andromeda Treasury. The filters we employ are the following: with WFC3/UVIS - F225W, F275W, F336W; with ACS/WFC F475W, F814W, F550M, F658N; with WFC3/IR F110W, F160W.
We adopt the PHAT tiling/exposure strategy for this project, which represents the most efficient way to map a several arcmin region in multiple WFC3 and ACS bands. This consists of 1 orbit in WFC3/IR and 2 in WFC3/UVIS at each pointing with parallel ACS exposures.There are 18 fields tiled in a 6 by 3 arrangement that cover the full area we will map. Each field requires 3 orbits worth of observations for observations in all 9 filters. We have defined one visit for each field, with 3 orbits in the visit.
The field we target is chosen to cover the same region we have mapped using the IRS instrument on Spitzer, which provides a fully sampled mid-IR spectral map. To match this region, we require half of the orbits to be at an orientation of 357 degrees and the other half to be 180 degrees rotated, at 177 degrees. This rotation allows us to map one half of the brick in parallel. The FOV of WFC3/IR is the smallest of the cameras, so tiling the region with WFC3/IR pointings results in an overlapping grid in ACS which is oriented at 45 degrees with double coverage at all points. The 180 degree flip in the middle ensures that the three primary fields from the first half overlap the parallel fields from the second half.
The first two orbits of each visit have the identical filters as PHAT - 6 bands covering the near-UV to near-IR. In the 3rd orbit, we employ the WFC3/UVIS F225W filter to cover the 2200 Angstrom bump. In parallel we use the ACS/WFC F658N and F550M filters to map Halpha and nearby continuum (to remove from Halpha). F658N covers the Halpha line at the velocity of M31. We chose F550M for continuum removal since it is covers a region of the stellar continuum free from any other strong emission lines.
The exposure times for the first two orbits per visit are very similar to what was done by PHAT, although we have rearranged some of the exposure time to make use of a small increase in the orbit duration in the SMC compared to M31. In addition, to recover some information about the brightest stars in the region, we also employ short "guard" exposures in F475W.
The WFC3/IR primary orbits use STEP MULTIACCUM sequences (NSAMP=9-10) to produce 4x400s exposures in F160W and 1x700s in F110W. The parallel ACS exposures are 4x454s and 1x5s and 1x700s in F475W. The first primary WFC3/UVIS orbits contain 1x560s and 1x700s in F336W and 2x600 in F275W. For the primary orbits with WFC3/UVIS F225W we do one additional 400s exposure in F275W to aid in cosmic ray removal. The remaining WFC3/UVIS exposures in that orbit are all F225W 1x650, 1x1050, and 1x570. In parallel with the first WFC3/UVIS orbit, the ACS exposure times are 1x600, 1x700 and 1x550 in F814W plus 1x10s to avoid saturation. For the second WFC3/UVIS primary orbit we observe with F550M for 1x350s and 1x400s and F658N for 1x650s and 1x950s. Because of the larger FOV for ACS, the final exposure times are doubled by the tiling required to cover a contiguous region with WFC3/IR and eliminate any issues with ACS chip gaps. Finally, we use a dither pattern that works for both the primary and parallel orbits to produce Nyquist-sampled images in F475W, F814W and F160W, which allows us to perform optimal photometry in crowded fields.
ISM IN EXTERNAL GALAXIES
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WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
No
No
F160W
ACS/WFC
Imaging
No
No
F475W
ACS/WFC
Imaging
No
No
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Imaging
No
No
F275W
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Imaging
No
No
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Imaging
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No
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WFC3/IR
Imaging
No
No
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Imaging
No
No
F160W
ACS/WFC
Imaging
No
No
F475W
ACS/WFC
Imaging
No
No
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WFC3/UVIS
Imaging
No
No
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WFC3/UVIS
Imaging
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No
F336W
ACS/WFC
Imaging
No
No
F814W
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
No
No
F160W
ACS/WFC
Imaging
No
No
F475W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F275W
WFC3/UVIS
Imaging
No
No
F336W
ACS/WFC
Imaging
No
No
F814W
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
No
No
F160W
ACS/WFC
Imaging
No
No
F475W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F275W
WFC3/UVIS
Imaging
No
No
F336W
ACS/WFC
Imaging
No
No
F814W
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
No
No
F160W
ACS/WFC
Imaging
No
No
F475W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F275W
WFC3/UVIS
Imaging
No
No
F336W
ACS/WFC
Imaging
No
No
F814W
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No
No
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WFC3/IR
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No
F160W
ACS/WFC
Imaging
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No
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No
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No
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No
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No
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No
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No
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WFC3/UVIS
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No
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No
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WFC3/IR
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No
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Imaging
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No
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No
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Imaging
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F814W
WFC3/UVIS
Imaging
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No
F275W
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Imaging
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No
F336W
ACS/WFC
Imaging
No
No
F814W
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Imaging
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No
F110W
WFC3/IR
Imaging
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No
F160W
ACS/WFC
Imaging
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No
F475W
ACS/WFC
Imaging
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No
F814W
WFC3/UVIS
Imaging
No
No
F275W
WFC3/UVIS
Imaging
No
No
F336W
ACS/WFC
Imaging
No
No
F814W
WFC3/IR
Imaging
No
No
F110W
WFC3/IR
Imaging
No
No
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Imaging
No
No
F475W
ACS/WFC
Imaging
No
No
F814W
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Imaging
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No
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WFC3/UVIS
Imaging
No
No
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Imaging
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No
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No
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No
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No
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Imaging
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No
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Imaging
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No
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Imaging
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WFC3/UVIS
Imaging
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No
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Imaging
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No
F814W
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
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No
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Imaging
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No
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ACS/WFC
Imaging
No
No
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WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
WFC3/UVIS
Imaging
No
No
F225W
WFC3/UVIS
Imaging
No
No
F275W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F660N
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false
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The scheduling data was generated by CASM 22.2.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 22.2.
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The scheduling data was generated by CASM 22.2.
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The scheduling data was generated by CASM 22.2.
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The scheduling data was generated by CASM 22.2.
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The scheduling data was generated by CASM 22.2.
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false
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0
The scheduling data was generated by CASM 22.2.
CASM was run in Phase II mode.
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false
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The scheduling data was generated by CASM 22.2.
CASM was run in Phase II mode.
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