This pattern is not used in this proposal.
This pattern is not used in this proposal.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
Final epoch on GRB 160625B. This will allow us to do the final subtraction. The source will be available until November 25, 2017 at the
required orientation, and we would therefore like to do the observation in the next several weeks.
1844661635
----- Attempting Submission 1 (Thu Dec 10 21:16:38 GMT 2015) -----
----- Attempting Submission 2 (Fri May 27 20:34:24 GMT 2016) -----
HST Phase II Proposal 14353 (GRB_160509a_first_visit.apt) successfully submitted.
Receipt: # 14353-2
----- Attempting Submission 3 (Fri May 27 22:35:50 GMT 2016) -----
HST Phase II Proposal 14353 (GRB_160509a_first_visit.apt) successfully submitted.
Receipt: # 14353-3
----- Attempting Submission 4 (Tue May 31 03:50:53 GMT 2016) -----
----- Attempting Submission 5 (Wed Jun 01 17:22:18 GMT 2016) -----
HST Phase II Proposal 14353 (14345_GRB_160509a_E1.apt) successfully submitted.
Receipt: # 14353-5
----- Attempting Submission 6 (Wed Jun 01 22:09:38 GMT 2016) -----
----- Attempting Submission 7 (Mon Aug 22 04:55:53 GMT 2016) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 8 (Mon Oct 17 22:03:12 GMT 2016) -----
----- Attempting Submission 9 (Thu May 25 22:22:08 GMT 2017) -----
----- Attempting Submission 10 (Mon Oct 23 17:44:24 GMT 2017) -----
There are visibility overrun warnings that will make looked at when the ToO gets activated.
The Astrophysics of the Most Energetic Gamma-Ray Bursts
The Large Area Telescope (LAT) of Fermi has found a sample of highly relativistic gamma-ray bursts (GRBs), which may be among the most energetic bursts ever discovered. Here we propose to use Chandra and HST to follow the late time X-ray and optical light curves of a LAT detected burst that also has excellent early multiwavelength coverage. Our observations, in conjunction with the Fermi data, will allow us to measure the energy and the bulk Lorentz factor of the explosion. Recent work on some of the most powerful GRBs begins to substantially constrain physical models of the progenitors. The energetics of the highly relativistic LAT bursts may greatly strengthen these constraints and provide new insight into the currently unknown mechanism that determines the energy of a GRB.
We plan five visits with HST: the first an orbit long, the second and third each two orbits long, with the fourth and fith three orbits long. The first visit will occur about around twenty days after outburst. The second will be around forty days after outburst. The third 80 days and the fourth 160. The exact times will be scaled according to the decay seen from the ground. The fith visit will be taken at least nine months after the burst to allow an accurate host subtraction. We will use the UVIS camera on WFC3 because WFC3 easily has as good sensitivity on point sources as ACS with smaller detector-induced noise sources (CTE, bias-striping, etc). We will choose the filter at the time of the ToO to match the best observed band from the ground (most likely a red band) and to avoid a SN contribution if possible.
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