0Assigned ID: 160
----- Attempting Submission 1 (Thu Apr 10 05:23:54 GMT 2014) -----
HST Phase I Proposal 160 (z10GrismC22.apt) successfully submitted.
----- Attempting Submission 2 (Fri Apr 11 03:44:49 GMT 2014) -----
HST Phase I Proposal 160 (z10GrismC22.apt) successfully submitted.
----- Attempting Submission 3 (Fri Apr 11 03:47:57 GMT 2014) -----use single guide star152724853----- Attempting Submission 1 (Wed Jul 16 18:45:28 GMT 2014) -----
----- Attempting Submission 2 (Wed Jul 16 19:17:26 GMT 2014) -----
----- Attempting Submission 3 (Thu Jul 17 13:12:40 GMT 2014) -----Following previous grism programs, I use an F140W direct pre-image before (or after) each G141 grism exposure. These exposures should be taken at the same pointing, which is why I used SAME POS AS, and made sure that the aperture definition (for GRISM1024) is the same for the image and the grism. If this flag is not required, I'm happy to remove it.A Spectroscopic Redshift for the Most Luminous Galaxy Candidate at z~10We recently discovered an unexpectedly bright and hence very luminous z~10 galaxy candidate in the GOODS-North field (GN-z10-1; Oesch et al. 2014). This source is the brightest and highest-redshift z>9 candidate in the complete 900-orbit CANDELS dataset. It is also the only z>8 candidate that is robustly detected in both Spitzer 3.6 and 4.5 micron channels, allowing for an unprecedented sampling of the rest-frame UV to optical spectral energy distribution for such an early galaxy. The existence of such a luminous and massive source at z~10, just 500 Myr after the Big Bang, raises significant questions about our understanding of early galaxy formation: it would imply that massive galaxies built up their masses faster than hitherto thought. Our comprehensive photometric tests indicate that this galaxy lies at z>9. However, without a spectroscopic redshift, we can not exclude other possibilities, such as a low redshift galaxy with very unusual continuum and emission line properties. The unusual brightness of this candidate together with the unique continuum sensitivity of the WFC3/IR grism G141 opens up the possibility for spectroscopic confirmation with HST. Because of its high redshift, this source cannot be observed from the ground due to very low atmospheric transparency at the wavelengths of its redshifted Lyman break. Before JWST, HST with the WFC3/IR G141 grism is uniquely capable amongst all existing telescopes of establishing a breakthrough in high-redshift galaxy spectroscopy by enabling a spectroscopic *continuum* detection at z~10.The goal of this program is to obtain a deep WFC3/IR grism spectrum of a bright (H=26 mag) candidate z~10 galaxy in the GOODS-N field (GN-z10-1 at 12:36:25.46,+62:14:31.4; Oesch et al. 2014). We will observe this source for a total of 12 orbits at different orientations, which were selected to minimize contamination of the resulting grism spectrum from neighboring sources.
The absolute best possbile roll angles (ORIENTS=50-53) are unfortunately only schedulable for 1 day in August 2014. We therefore identified a series of other possible angles with acceptably low expected contamination. ORIENTS=(181), (42), (213)
Our observation strategy is to obtain 3 visits of two orbits at two different orientations. Each visit contains four short pre-images of F140W each followed by a long G141 grism exposure. The four sets of exposures are dithered following our successful 4-point dithering strategy used for the 3D-HST survey (e.g., Brammer et al. 2012). I.e. we set POS-TARG: (0,0) (1.355,0.424) (0.881,1.212) (-0.474,0.788).
The structure of each visit is thus four sets of (direct F140W image, G141 grism exposure, dither offset). Due to the possibility of excess Earth-glow by a bright He line at either the beginning or at the end of each orbit, we exchanged the F140W and G141 exposures for the second set of dither offsets within each orbit. This will minimize the impact of background variations on our G141 science exposures.
The aperture is set to GRISM1024, which uses the same reference pixel and definition for both F140W and the G141 grism. In addition to the primary exposures, we also take parallel F435W ACS imaging.
G141 exposures use SPARS100 sampling with NSAMP=14-15, and F140W exposures are taken with SPARS50 with NSAMP=5 and 4 (where NSAMP is optimized to fill the orbits). While NSAMP=4 for the direct images is very low, we only use this setting for the second direct image at the end of each orbit, which is only used to make sure no pointing problems or drifts are present relative to the commanded POS-TARG.
We submit 6 visits of 2 orbit duration. Visits 1-3 have constraints of ORIENT=181. Visits 4-6 have various orient constraints to allow for schedulability ORIENT=(50-53), (42), (213). We request that both sets are taken at the same orient, and we have set the "Same Orient as" special requirement.COSMOLOGY12falsefalse0.00.0falsefalsefalseSUPPORTEDGALAXYHIGH REDSHIFT GALAXYTarget is a J-band dropout, and is not visible in any filter shortward of 1.1um.J2000J2000H=26 mag ABWFC3/IRSpectroscopicNoNoG141WFC3/IRImagingNoNoF140WHst Same orient constraint links visits (01 02 03)The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.(Tic-Visit
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