Cannot find file /Users/dmales/Downloads/HST_221009A___DDT.pdf Please find attached our request for HST non-disruptive ToO imaging of the recent "once-in-a-lifetime" GRB 221009A. 37818959 Assigned ID: 3814 ----- Attempting Submission 1 (Fri Oct 14 14:06:02 GMT 2022) ----- Apologies for the delay to this. Attached is a version where I have removed all timing constraints from visit 08. It is a late time visit for host subtraction, and so can be scheduled whenever it is suitable. 307489086 ----- Attempting Submission 1 (Tue Oct 25 19:18:50 GMT 2022) ----- HST Phase II Proposal 17264 successfully submitted. Receipt: # 17264-1 ----- Attempting Submission 2 (Tue Oct 25 20:49:58 GMT 2022) ----- HST Phase II Proposal 17264 successfully submitted. Receipt: # 17264-2 ----- Attempting Submission 3 (Tue Oct 25 21:08:13 GMT 2022) ----- ----- Attempting Submission 4 (Wed Oct 26 08:12:02 GMT 2022) ----- ----- Attempting Submission 5 (Mon Feb 06 17:54:55 GMT 2023) ----- ----- Attempting Submission 6 (Wed Aug 23 12:58:46 GMT 2023) ----- Unique opportunities from the brightest gamma-ray burst of all time The exceptional gamma-ray burst GRB 221009A is the brightest GRB ever observed by almost two orders of magnitude, and rate estimates suggest it is a once per millenium event. It is now the subject of an intensive series of multi-wavelength observations with detections of individual photons with tens to hundreds of TeV to low frequency radio, including approved NIR spectroscopy from JWST. Remarkably, it is also a relatively nearby event with a redshift of only z=0.15. The worldwide follow-up is building what will become a legacy data set for the field. The collapsars accompanying such lumonous bursts have been proposed as a source of r-process heavy elements, and this case offers the best opportunity for the foreseeable future to test this hypothesis. We propose here non-disruptive HST ToO imaging observations at mid- to late-times post burst, sampling the spectral energy distribution evolution, in order to characterise the accompanying SN, compare its properties to those of more ordinary GRBs, and crucially to seek the signature of r-process nucleosynthesis, expected to produce NIR excess starting after the SN peak, that is 3-6 weeks after the GRB. These data will also pinpoint the burst position on its host, allowing future studies of the GRB progenitor environment. HST data are essential because of the target faintness and crucially because it will not be observable from ground (nor JWST) on the critical epochs requested here. We propose to obtain three epochs of observation of GRB 221009A. At each epoch we will obtain observations in 5 filters to be sensitive to evolving supernova + afterglow light (F625W/F775W/F098M/F125W/F160W). For the first two epochs we will obtain observations with UVIS in a single orbit using a 3-point dither in each optical filter. To ensure that we avoid buffer dump issues we will use the sub-array, and will flash the chip to bring the background to 20 electrons. We also ask for orients between 45-65 degrees to minimize the risk of diffraction spikes from nearby bright stars overlapping our target (we do not ask for a fixed orient because there is no one orient that is available at all epochs). For the final epoch we will obtain 1 orbit each in the optical filters with a standard 4-point box dither pattern. In the IR we will obtain F098M/F125W/F160W in a single orbit. The final orbit is slightly shorter than the others to aid schedulability. This proposal represents a co-ordinated effort from many of the key groups involved in the study of GRB 221009A and its afterglow. This includes the Fermi and Swift teams who first discovered the burst and the Stargate collaboration which measured the redshift. Our team also includes groups who have been heavily involved in studies of kilonovae and their implications for the r-process. This ensures that we have the necessary scientifc expertise to interpret the data, combine it with other observations and maximise the scientific return from observations of this exceptional burst. We also have significant techncial expertise (the PI of this proposal is the PI of >40 other HST proposals, and between the CoIs we have experience within a further 100+ HST proposals). We have the necessary resources to rapidly reduce and analyse the requested HST observations. 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