0 Assigned ID: 3558 ----- Attempting Submission 1 (Fri Mar 25 21:08:37 GMT 2022) ----- HST Phase I Proposal 3558 successfully submitted. Receipt: # 3558-1 ----- Attempting Submission 2 (Fri Mar 25 21:15:28 GMT 2022) ----- HST Phase I Proposal 3558 successfully submitted. Receipt: # 3558-2 ----- Attempting Submission 3 (Fri Mar 25 23:39:26 GMT 2022) ----- HST Phase I Proposal 3558 successfully submitted. Receipt: # 3558-3 ----- Attempting Submission 4 (Fri Mar 25 23:51:38 GMT 2022) ----- HST Phase I Proposal 3558 successfully submitted. Receipt: # 3558-4 ----- Attempting Submission 5 (Fri Mar 25 23:55:23 GMT 2022) ----- HST Phase I Proposal 3558 successfully submitted. Receipt: # 3558-5 ----- Attempting Submission 6 (Fri Mar 25 23:58:15 GMT 2022) ----- ----- Attempting Submission 7 (Mon Mar 28 12:30:11 GMT 2022) ----- This target is not used in this proposal. This target is not used in this proposal. Phase II Submission 2 Updated the aperture selection for BCG-NORTH target and target location given updated orient range. Followed suggestion to remove non-ideal orients 80-89 as schedulability is not impacted. 1137948222 ----- Attempting Submission 1 (Thu Jul 21 14:36:50 GMT 2022) ----- ----- Attempting Submission 2 (Wed Jul 27 16:55:38 GMT 2022) ----- ----- Attempting Submission 3 (Tue Jan 10 18:29:50 GMT 2023) ----- HST Phase II Proposal 17101 successfully submitted. Receipt: # 17101-3 ----- Attempting Submission 4 (Fri Jan 13 18:14:05 GMT 2023) ----- HST Phase II Proposal 17101 successfully submitted. Receipt: # 17101-4 ----- Attempting Submission 5 (Fri Jan 13 18:19:22 GMT 2023) ----- The unused targets are meant to ensure orient ranges cover the 3 primary target locations. Clash of Titans: Characterizing SPT-CLJ0307-6225, a major merger in the plane of the sky Mergers of galaxy clusters are natural dark matter (DM) colliders. If DM particles self interact, signatures of the interaction can be found in merging clusters as an spatial offset among the collisionless cluster galaxies, the intracluster gas, and the cluster potential, dominated by the DM. Typically, to place constraints on the value of the DM particle self-interacting cross section, ensembles ($\sim 40$) of merging clusters are used. Nevertheless, most of the constraining power comes from a special type of mergers: oriented in the plane of the sky, with (relatively) similar cluster masses, and showing a large displacement between the collisional and the collisionless components. Finding those special mergers would significantly improve the current constraints on the DM particle self-interacting cross section. SPT-CLJ0307-6225 is a merging cluster in the plane of the sky, with {\it Chandra} X--ray showing a comet like gas distribution, Gemini/GMOS and VLT/MUSE spectroscopy that confirms a plane-of-the-sky orientation of the merger, and ground based imaging confirming both, a large gas galaxy offsets ($\sim 790$ and $\sim 360$ kpc) and the need for space base observations, for a robust weak lensing analysis. The superb imaging of HST will allow us to map the dark matter mass density distribution of SPT-CLJ0307-6225, and to use it to place constraints on the self-interacting DM cross section. Our observing plan covers the primary cluster mass with two pointings of ACS (WFC), with 3 orbits covering the most concentrated southern region and 2 orbits in the north. Both pointings use a 4-step dither patter for optimal PSF sampling, with an additional F606W exposure and dither over the chip gap in the southern pointing. The restricted orient rages are intended to align the mosaic with the cluster mass distribution. NOTE that for scheduling purposes, we have included orient ranges that are 180 degrees rotated as it keeps the same coverage of the field. However, if the orient falls in the 280-300deg range then the tiles need to be swapped, ensuring that the pointing with 3 orbits covers the BCG-SOUTH targets regardless of orientation. Overall coverage of the BCG targets 2-4 is critical, so in the scheduling process once the final orientation is set we would like to review the final detector placement to ensure it gives optimal coverage. Dr. Rogerio Monteiro de Oliveira is a postdoc at the University of Taiwan. He is an expert in weak lensing. His research is focused in the study of merging galaxy clusters with WL tools. Dr. Alfredo Zenteno is scientist at CTIO, NOIRLab Chile. He is an expert in galaxy evolution in clusters. He has been working selecting massive merging galaxy clusters from the South Pole Telescope sample and obtaining spectroscopy for them. Dr. Rodrigo Carrasto is an astronomer at Gemini, NOIRLab, Chile. He is an expert in spectroscopy. He has been working with Alfredo Zenteno reducing Gemini/GMOSspectroscopic data of merging clusters. Dr. Ang Liu is an expert in the analysis of X-ray data of galaxy clusters and the study of merging clusters. Dr Mahler is an expert in strong lensing with ample experience in dark matter mass modelling of clusters. He has strong experience in both Hubble imaging and MUSE IFU spectroscopy analysis. Dr. Hector Cuevas is a professor at the University of La Serena. He is an expert in spectroscopy. He has been working with Alfredo Zenteno reducing Gemini/GMOSspectroscopic data of merging clusters. Dr. Matt Bayliss is a professor at the University of Cinncinatti. He is an expert in spectroscopy. He is collaborating with Alfredo Zenteno on reducing Gemini/GMOSspectroscopy of SPT-CLJ2228-5828, a merging cluster for which it was recently granted XMM+HST observations. Dr. Armin Rest is an expert in transient science, in particular SN Ia cosmology, light echoes of historic SN, and exotic transients. His technical expertise lies in data reduction, image analysis, photometry, and their application to wide-field time-domain surveys. Dr. Annalisa Calamida is STScI scientist and the WFC3/HST deputy branch lead. She is an expert in photometric calibration and reduction techniques. She is an expert of stellar populations, stellar evolution and variable stars. Mr. Daniel Hernandez-Lang is a PhD student at LMU Germany focused on the study of the merger event on the galaxy population. Dr. Alexandro Saro is a professor at the University of Trieste. He is an expert working in simulations. Mr. Hugo Prado is a PhD student at the University of La Serena Chile. He will participate in the analysis of the data as part of his thesis. Mr. Simon Veliz is a Master student at the University of La Serena Chile. He will participate in the analysis of the data as part of his thesis. Large Scale Structure of the Universe Galaxies 6 false true false false false false false SUPPORTED CLUSTER OF GALAXIES HIGH REDSHIFT CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 GALAXY GRAVITATIONAL LENS J2000 GALAXY GRAVITATIONAL LENS J2000 GALAXY GRAVITATIONAL LENS J2000 ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F814W POS-TARG DITHER 0.262 LINE 0.192 false false 68.14 4 18.39 ACS-WFC-DITHER-BOX 1 false The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. /private/var/folders/9x/wtzrcm85559bwf_5h58_8ml40002rz/T/OPVisit6507892323430853846.xml Orient ranges are inteded to follow the cluster mass distribution, but this tile MUST comfortably cover target BCG-NORTH. (Tic-Visit :proposal-id 17101 :visit-id "03" :proposal-version -1 :trans-version "20220630" :date "13-Jan-2023 10:18:03.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 2273792 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17101 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17101 :visit-id "03" :orbit-number 1 :pcs-time 383 :si-vis-utilization 3019 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3411 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17101 :visit-id "03" :orbit-number 2 :pcs-time 392 :si-vis-utilization 3016 :al-overhead-at-end 0 :internal-dur-at-end 347 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3411 :pcs-gap 0 ) true 2 0 Part of a ACS WFC Dither Box pattern, which alternates with the F814W filter over the course of 2 orbits. A deeper F606W exposure is preferred for the science case. Part of a ACS WFC Dither Box pattern, which alternates with the F606W filter over the course of 2 orbits. The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. /private/var/folders/9x/wtzrcm85559bwf_5h58_8ml40002rz/T/OPVisit5150078989112004836.xml Orient ranges are inteded to follow the cluster mass distribution, but this tile MUST comfortably cover target BCG-SOUTH-1 and 2. (Tic-Visit :proposal-id 17101 :visit-id "04" :proposal-version -1 :trans-version "20220630" :date "13-Jan-2023 10:12:45.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 2558016 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17101 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17101 :visit-id "04" :orbit-number 1 :pcs-time 383 :si-vis-utilization 3026 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3411 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17101 :visit-id "04" :orbit-number 2 :pcs-time 392 :si-vis-utilization 3017 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3411 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17101 :visit-id "04" :orbit-number 3 :pcs-time 392 :si-vis-utilization 3018 :al-overhead-at-end 0 :internal-dur-at-end 347 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3411 :pcs-gap 0 ) true 3 0 Part of a ACS WFC Dither Box pattern, which alternates with the F814W filter over the course of 2 orbits.This is the deeper of the two pointings, and the extra exposure is in F606W as a deeper F606W exposure is preferred for the science case. Part of a ACS WFC Dither Box pattern, which alternates with the F606W filter over the course of 2 orbits. This is the deeper of the two pointings. The 5th exposure in F606W for this pointing, which brings the total F606W exposure to 3200s. We add a final dither after the box to step over the chip gap.