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Assigned ID: 113
----- Attempting Submission 1 (Wed Apr 08 14:27:56 GMT 2015) -----
HST Phase I Proposal 113 (prop.apt) successfully submitted.
Receipt: # 113-1
----- Attempting Submission 2 (Wed Apr 08 17:37:24 GMT 2015) -----
Please check the proper motion as well as the units since the entered value exceeds the fastest object in Luyten's Half-Second Catalogue.
ACS apertures changed from WFC1-1K subarry to WFC1-CTE, as discussed with PI.
Total ACS exposure time slightly increased from 14580 to 14634 seconds:
exposures auto-adjusted to completely fill orbits
from 810 seconds each
to 781 (1st orbit each visit) and 845 (2nd orbit each visit) seconds each
627607249
----- Attempting Submission 1 (Tue Jul 07 15:37:25 GMT 2015) -----
----- Attempting Submission 2 (Thu Mar 03 15:04:09 GMT 2016) -----
The proper motion of the target is correct.
Testing Model Atmospheres with the Coldest Known Brown Dwarf
Last year, we discovered a brown dwarf, WISE 0855-0714, that has a distance of 2.3 pc and a temperature of ~250 K, making it the 4th closest neighbor of the Sun and the coldest known brown dwarf. Because of its extreme proximity and temperature, it represents an unparallaled laboratory for studying planet-like atmospheres in an unexplored temperature regime. In Cycle 22, we obtained images of WISE 0855-0714 in the single most sensitive band of WFC3 for brown dwarfs (F110W) to assess the feasibility of spectroscopy and multi-band photometry, and to begin using it to test the colors predicted by model atmospheres. We have detected WISE 0855-0714 in those data, and the resulting photometry indicates that it is too faint for spectroscopy, but that photometry in additional HST bands is feasible. Therefore, we propose to observe WISE 0855-0714 with ACS and WFC3 in three bands that are well-suited for testing and discriminating between competing models of very cold atmospheres.
This program consists of WFC3/IR and ACS/WFC images in F105W, F127M, and F850LP of a single faint point source during 18 orbits (6 orbits per filter). The observations have been designed to maximize the total exposure time, optimize the spatial resolution, and provide sufficient flexibility for scheduling. For each of the three filters, the images will be obtained through three identical two-orbit visits. In each orbit, one exposure (SPARS100, NSAMP=10, 900 sec for WFC3; 810 sec for ACS) will be collected at each position in a three-point dither pattern. In each visit, the dither patterns in the two orbits will be offset from each other by 3.5 pixels along the x-axis of the array. The target will be observed at the IR and WFC1-1K apertures for WFC3 and ACS, respectively.
COOL STARS
12
false
false
false
false
false
false
SUPPORTED
STAR
BROWN DWARF
NO
J2000
J2000
ACS/WFC
Imaging
No
No
F850LP
WFC3/IR
Imaging
No
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F105W
WFC3/IR
Imaging
No
No
F127M
POS-TARG
DITHER
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WFC3-IR-DITHER-LINE-3PT
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POS-TARG
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POS-TARG
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ACS-WFC-DITHER-LINE
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POS-TARG
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