0Assigned ID: 3889
----- Attempting Submission 1 (Fri Feb 17 16:47:33 GMT 2023) -----
HST Phase I Proposal 3889 successfully submitted.
Receipt: # 3889-1
----- Attempting Submission 2 (Fri Feb 17 19:37:37 GMT 2023) -----
HST Phase I Proposal 3889 successfully submitted.
Receipt: # 3889-2
----- Attempting Submission 3 (Fri Feb 17 21:20:08 GMT 2023) -----
HST Phase I Proposal 3889 successfully submitted.
Receipt: # 3889-3
----- Attempting Submission 4 (Fri Feb 17 22:16:33 GMT 2023) -----
HST Phase I Proposal 3889 successfully submitted.
Receipt: # 3889-4
----- Attempting Submission 5 (Fri Feb 17 22:25:42 GMT 2023) -----This should be fairly straightforward. The main question I have is whether the CTE losses are
sufficiently controlled. I put the object on UVIS2, and the background in each exposure is
~85 electrons. If needed the aperture can be changed so it is even closer to amplifier C, although
that would limit the exposed area around the object of course. We can also reduce the number of
exposures per orbit to 2 (from 3) so the background is even higher. My impression is that we are
already "safe" but please check!1108905297----- Attempting Submission 1 (Thu Apr 13 14:04:00 GMT 2023) -----Ultraviolet imaging of a candidate runaway supermassive black holeA recent study announced the discovery in HST/ACS data of a remarkably thin, 62 kpc long feature associated with a compact galaxy at z=0.964. It was proposed that we are witnessing shocks and star formation in the wake of a runaway supermassive black hole (SMBH). The existing HST data sample the rest-frame near-UV, and show where stars have formed in the feature. A ground-based u band image shows that the rest-frame far-UV emission is qualitatively different from the rest-frame near-UV: the linear feature is longer, extending all the way to the compact galaxy, and there is flux on the other side of the galaxy, opposite the linear feature that is in the ACS data. The rest-frame far-UV emission likely traces shocked gas rather than (only) hot stars, and the u band detection on the other side may be another wake, behind a simultaneously ejected binary SMBH. The interpretation is hampered by the low resolution of the ground-based u band data. Here we propose to obtain high resolution, deep UV imaging of this remarkable system with UVIS. These observations will show whether there is indeed a counter linear feature, whether it is connected to a compact object that would be the location of the binary SMBH, and whether it shows the characteristic fanning out from the tip that is expected for the wake of a SMBH. The data will also map the rest-frame far-UV emission around the tip of the main feature, which could resolve into a spectacular kpc-scale bow shock. The observations will be done in the difference bandpass F200LP - F350LP. As a bonus, the summed image (F200LP + F350LP) will provide a monochromatic image of the entire system that is 30x deeper than the existing ACS data.The observations are split into 6 visits of 2 orbits each.
Within each visit, the first orbit is in F200LP and the second in F350LP. As the science comes from the difference frames F200LP - F350LP, we want to make sure that the F200LP data are taken in the exact same way (with the same ORIENT etc) as the F350LP data. We therefore observe in both filters in each visit.
(Rather than, say, having 6 visits of F200LP observations and 6 visits in F350LP).
The target is placed at the UVIS2 aperture. The UVIS2 chip has a higher QE in the UV than UVIS1, and as the target is small we do not need to place it near the center of the full array. We contemplated placing the target nearer amplifier C to improve CTE, but given the high background in the long pass filters we figured that UVIS2 is going to be OK.
Within each orbit, three exposures are obtained with the WFC3-UVIS-DITHER-LINE-3PT pattern. We are not concerned with dithering over the chip gap, and this pattern improves subpixel sampling. Doing 3 pointings (rather than 2 or a box of 2x2) is a compromise between limiting overheads, having a high enough background to limit CTE losses, and having enough exposures for redundancy and subpixel sampling. In the end we will have 18 exposures in each band and that will certainly be sufficient. The sky background of each exposure is about 85 counts, which is hopefully sufficient.
There are no ORIENT or timing constraints. It is also fine if different visits are taken at different ORIENTs.The team has extensive expertise with all aspects of HST imaging. The PI has used UVIS several times, as well as most other HST instruments. All tools and procedures are in place for immediate analysis of the data when they are taken.
We are the team that discovered the candidate runaway black hole and wrote the paper that this proposal is based on (van Dokkum et al. 2023). That paper was based on our Cycle 29 GO-16912 midcycle program with ACS: the data were obtained in September 2022 and we have already analyzed and published a key result from them. This hopefully demonstrates that we have the required background and expertise, and that we will move rapidly if this proposal is approved!Supermassive Black Holes and Active GalaxiesGalaxies3falsefalsetruefalsefalsetruefalsefalseSUPPORTEDGALAXYHIGH REDSHIFT GALAXYSHOCK FRONTYESJ2000J2000WFC3/UVISImagingNoNoF200LPWFC3/UVISImagingNoNoF350LPPOS-TARGDITHER0.135LINEfalsefalse346.84WFC3-UVIS-DITHER-LINE-3PT1falseThe scheduling data was generated by CASM 31.0.CASM was run in Phase II mode.(Tic-Visit
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