0Assigned ID: 310
----- Attempting Submission 1 (Fri Apr 05 01:05:24 GMT 2019) -----
HST Phase I Proposal 310 (FRBs.apt) successfully submitted.
Receipt: # 310-1
----- Attempting Submission 2 (Fri Apr 05 02:29:37 GMT 2019) -----
HST Phase I Proposal 310 (FRBs.apt) successfully submitted.
Receipt: # 310-2
----- Attempting Submission 3 (Fri Apr 05 12:29:23 GMT 2019) -----
HST Phase I Proposal 310 (FRBs.apt) successfully submitted.
Receipt: # 310-3
----- Attempting Submission 4 (Fri Apr 05 18:29:51 GMT 2019) -----
HST Phase I Proposal 310 (FRBs.apt) successfully submitted.
Receipt: # 310-4
----- Attempting Submission 5 (Fri Apr 05 18:32:24 GMT 2019) -----Increased IR dither pattern size to better deal with self persistence and IR blobs.-168202096----- Attempting Submission 1 (Tue Jul 09 16:40:57 GMT 2019) -----
----- Attempting Submission 2 (Thu Aug 22 12:36:31 GMT 2019) -----Uncovering the birthplace of FRBsFast Radio Bursts (FRBs) are an enigmatic class of extragalactic object, whose study so far has been almost exclusively the domain of radio telescopes due to the inability to localize them to better than a few arcminutes. We propose to use HST to spatially resolve the morphology and distribution of star formation and stellar mass for the host galaxies of the first three non-repeating FRBs ever localized to <1" accuracy by the Australian SKA Pathfinder telescope. Analogous to previous advances with gamma-ray bursts, supernovae, and gravitational-wave counterparts, we will explore the origin of these FRBs through detailed examination of their host galaxies. By contrast with the dwarf galaxy host of the unusual repeating FRB 121102, our complementary ground-based observations have shown these non-repeating FRBs to lie in the outskirts of early-type galaxies having low star formation rates. However only HST offers the spatial resolution necessary to match the precision of the radio localizations in the ultraviolet through near-infrared that is required to properly characterize their environment, and thereby shed light on the nature of their progenitor objects.This program images three newly discovered FRB host galaxies to measure the distributions of the star formation and mass using WFC3 UVIS and IR. The sources are all moderately luminous galaxies at redshifts <0.5, enabling the observations in a single orbit per filter. The FUV and NUV will be sampled by the WFC3/UVIS F300X filter. This filter is the broadest FUV/NUV filter available on HST enabling us to trace recent star formation via young stars. This cleanly samples the rest-frame FUV and NUV continuum of our galaxies and provides the highest throughput possible for morphological measurements. The NIR will be sampled by the WFC3/IR F160W filter. This is the reddest wide filter available on HST to measure the distribution of the stellar mass as traced by the old stellar populations.
In order to obtain images clean of cosmic rays and image artifacts and sampling the PSF phase, we use a minimum of four dither positions. For the UV measurements we will obtain four exposures, which also ensures no saturation for our bright targets. Given the short exposure times in F300X, this requires us to utilize 8-9e- post-flash to reach 12e- per pixel. To maximize UV throughput and minimize our pixel-based CTE correction, we place the target on chip 2 close to the readout. For the NIR observations, we wish to stay in the linear regime and minimize persistence with our bright targets, and therefore will use SPAR25 with NSAMP of 15 or 14. Since this sets the exposure time per dither position, we end up with 7 dither positions per orbit.
For the WFC3/UVIS exposures we use a dither pattern that is 5 times the standard box pattern to remove residual background patterns and enable sky darks. For the WFC3/IR exposures we use the 7-point wide dither pattern from WFC3 ISR 2016-14 (pg 17) to get a good dither for the pixel phase and artificat mitigation. We multiply those values by 3 to better deal with IR blobs, and self persistence.
We do not place any orient constraints on the program, which makes this easy to schedule. We therefore do not forsee any issues if we have to go to 1 gyro mode. We note that this means that the UV and IR overlap in our area of interest, but depending on the orient they will not overlap significantly in other areas.Professor Xavier Prochaska (UCSC) is an expert in cosmic baryons and experienced with measuring properties of galaxies hosting transient events (e.g. GRBs). Dr Marc Rafelski (STSCI) is an expert at planning for, reducing, and analyzing WFC3 data. He also has experience in measuring photometry and morphology of galaxies. Dr Stuart Ryder (Macquarie University) is an experienced user of 8 metre-class optical and infrared telescopes including Gemini, Keck, and the VLT for imaging, spectroscopy, and adaptive optics. Associate Professor Adam Deller (Swinburne University) is an expert in radio astrometry and has delivered accurate FRB positions based on radio data. Cherie Day is a graduate student working with Associate Professor Deller. Professor Jean-Pierre Macquart is an expert in theoretical analysis of fast radio bursts and will interpret the HST measurements in the context of burst progenitor models. Professor Elaine Sadler (CSIRO and University of Sydney) is an expert in observational extragalactic astronomy and will use the HST measurements to classify the burst host galaxies. Dr Ryan Shannon (Swinburne) and Keith Bannister (CSIRO) are experts in observation of fast radio bursts and burst emission properties in the context of progenitor models. Prof. Nicolas Tejos (PUCV) is an expert in studies of the intergalactic medium and large-scale structure connection using HST UV spectroscopy and ground-based optical follow-up observations. As Chilean researcher, he has direct access to state-of-the-art ground based optical facilities located in Chile, providing further support to the follow-up campaigns of these Southern FRBs.Galaxies and the IGM6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000GALAXYHIGH REDSHIFT GALAXYJ2000J2000WFC3/UVISImagingNoNoF300XWFC3/IRImagingNoNoF160WWFC3/UVISImagingNoNoF300XWFC3/IRImagingNoNoF160WWFC3/UVISImagingNoNoF300XWFC3/IRImagingNoNoF160WPOS-TARGDITHER0.865LINE0.56falsefalse81.785423.884WFC3-UVIS-DITHER-BOX1false/private/var/folders/t2/c39hm9n15t3bbrhwh0w6hy6h0001t3/T/OPVisit4745592550925863807.xmlThe scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.(Tic-Visit
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