removed all on holds----- Attempting Submission 2 (Mon Aug 09 18:22:53 GMT 2010) -----
----- Attempting Submission 3 (Fri Aug 20 00:02:55 GMT 2010) -----
HST Phase II Proposal 12330 (12330_submission2_19aug2010.apt) successfully submitted.
----- Attempting Submission 4 (Fri Aug 20 20:39:28 GMT 2010) -----
----- Attempting Submission 5 (Sat Jan 01 02:30:22 GMT 2011) -----
----- Attempting Submission 6 (Wed Jan 19 19:07:03 GMT 2011) -----Spitzer Verification of the Coldest WISE−selected Brown DwarfsWe will use data from WISE to search for brown dwarfs colder than those currently
known. The discovery and subsequent study of low−temperature brown dwarfs will
expand our knowledge of the low−mass end of the "stellar" mass function and of the
physics of low−Teff, high−pressure atmospheres, the latter of which is important in
characterizing exoplanets. Spitzer is an important component in the WISE discovery
process because it is the only observatory capable of providing deeper imaging in
the same wavelength range used by WISE to select candidates (3−5 um). Our WISE
selection process uses the W1 (3.4 um) and W2 (4.6 um) color to identify brown dwarf
candidates; the resulting, red W1−W2 colors are indicative of deep methane absorption
at 3.3 um. For our coldest sources, which are the most important for deciphering the
low−mass cutoff of star formation, these will be color limits because the candidate is
undetected in W1. Spitzer can easily provide much deeper imaging and measure robust
ch1−ch2 colors, which are complementary to W1−W2. The reddest of these sources
will also be the faintest since they are expected to be the coldest ones in the list. For
these, near−infrared spectroscopy will be impossible from the ground, so we also ask
for HST time with WFC3 to obtain low−resolution grism spectra over the 1.1−1.7 um
range to confirm these as brown dwarfs.The G141 grism will be used to obtain R~300 spectra from 1.075-1.700 μm, covering the critical
J- and H-band portions of the spectrum containing telltale temperature-dependent bands of CH4,
H2O, and NH3. Of critical importance to both the confirmation of the low temperature of these
objects as well as the establishment of a Y dwarf class is the NH3 feature expected near 1.565 μm
(Delorme et al. 2008). Direct images taken with the F140W filter to accurately identify
spectroscopic sources and to calibrate the wavelength scale will also provide highly accurate
astrometry at a third epoch, the others being the two Spitzer epochs as the WISE positions will be
poorly constrained due to the faintness of the sources. As a bonus, these direct HST images will
also provide information on binarity of the sample, enabling us to establish a more accurate
absolute magnitude vs. temperature scale for these coldest objects.
Using the HST Exposure Time Calculator for the IR channel of WFC3, we used observed spectra
of two T dwarfs (the T8 2MASS 0415-0935 and the T9 ULAS 1335+1130) to approximate the
SEDs of our typical sources. For a typical J~20.0 mag source, we require a direct, F140W image
to establish the wavelength calibration for the grism image, to provide valuable astrometric
information on our target, and to search for signs of binarity. SNR values of 200, adequate for
excellent astrometry and for searching for companions down to J~24.5 mag (the SNR=5 level),
are possible in only 6m of total exposure time (spread over a four-point dither). For
spectroscopy, we use the G141 grism that covers the 1.075-1.700 μm range. A spectrum having
an SNR=5 at 1.65 μm, which will enable us to determine the strength of the H-band CH4
absorption, will also provide SNR=3 at 1.15 μm, where we can measure the depth of the
combination CH4+H2O band at J; the required integration time for this is 29m (again spread over
a four-point dither). These direct images and their corresponding slitless grism images are paired
in the dither sequence. Assuming overheads of six minutes for target acquisition and one minute
each for the direct image and grism setups, the full dither pattern can be obtained in 50m of
spacecraft time. A sample size of a dozen objects will provide the beginning of a statistical
sample with which we can look for trends of J-H and ch1-ch2 colors with resulting spectral type.COOL STARS12false0.00.0falsefalsefalsefalseSUPPORTEDSTARBROWN DWARFJ200000 00 0.0000+00 00 0.00J2000STARBROWN DWARFJ200000 00 0.0000+00 00 0.00J2000STARBROWN DWARFJ200000 00 0.0000+00 00 0.00J2000STARBROWN DWARFJ200000 00 0.0000+00 00 0.00J2000STARBROWN DWARFJ200000 00 0.0000+00 00 0.00J2000STARBROWN DWARFJ200000 00 0.0000+00 00 0.00J2000STARBROWN DWARFJ200000 00 0.0000+00 00 0.00J2000STARBROWN DWARFJ200000 00 0.0000+00 00 0.00J2000STARBROWN DWARFJ200000 00 0.0000+00 00 0.00J2000STARBROWN DWARFJ200000 00 0.0000+00 00 0.00J2000STARBROWN DWARFJ200000 00 0.0000+00 00 0.00J2000STARBROWN DWARFJ200000 00 0.0000+00 00 0.00J2000WFC3/IRImagingNoNoF140WWFC3/IRImagingNoNoF127MPOS-TARGDITHER5.725LINE3.655falsefalse74.653418.528WFC3-IR-DITHER-BOX-MIN1falseThe scheduling data was generated by CASM 18.3.1.CASM was run in Phase II mode.WISE1405+55(Tic-Visit
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