0Assigned ID: 1980
----- Attempting Submission 1 (Sat Mar 02 00:03:16 GMT 2013) -----Please note that Visit 6 can only be scheduled on 1 day. We realize the orientation
requirements place stringent schedule constraints on the planning of this observation but
they are necessary to make the most efficient use of HST time and target each subcluster in
parallel. Any orientations outside this range will cause a significant portion of the northern
subcluster to fall outside the WFC3 field-of-view.
Note (8/22/2013): Following review of this target by STScI it was recommended that we move the
pointing away from the bright star. We have implemented a move of ~20" from the original
pointing which should enable us to reduce the effects of the bright star while maintaining our
primary science. Additionally it was suggeted that we either shorten each orbit by a minute or
increase the roll constraint from 235 to 257 degrees. We have chosen to shorten the orbit
exposure time so that we can maintain a nice mosaic of the northeast and southwest subclusters.
Note (8/01/2014): We made the following changes:
— Change the ACS/WFC spectral element of Visit 08 from F435W to F816W. It has become
apparent that the current F814W exposure of the southwest subcluster is only 0.5 orbits deep.
It is more important that we have deep F814W coverage for lensing than the extra color band.
— Change the pointing of Visit 05 slightly. We performed our weak lensing analysis of the
existing HST observation focused on the southern subcluster of this merger (from Visit 06)
and found that the weak lensing peak was offset from the well defined galaxy peak much
more than expected. So much so that the weak lensing peak is near the edge of the detector
on the existing image and may actually be just off it. Since this offset is exactly the
measurement we want to accurately make to constrain the dark matter cross-section we have
decided that it is more important to measure exactly where the southern weak lensing peak is
rather than observe the northern subcluster, as previously planned. We wish to mosaic the
Visit 05 ACS observations with the existing Visit 06 ACS observations.-915700333----- Attempting Submission 1 (Wed Jun 26 21:22:24 GMT 2013) -----
----- Attempting Submission 2 (Thu Aug 22 23:05:52 GMT 2013) -----
----- Attempting Submission 3 (Sat Aug 02 00:14:03 GMT 2014) -----The Orbit Planner and Visit planner were run for the two visits that we changed (05 and 08) and
no errors were noted. I didn't run it for the other visits since they have already been observed or are
currently scheduled (visit 03).Probing Dark Matter with a New Class of Merging ClustersWe will obtain multiband imaging in support of a weak lensing analysis of a new radio-selected sample of merging galaxy clusters. After first pericenter passage, merging clusters exhibit a dissociation between gas (which remains in the center of the system due to its collisional nature) and galaxies and dark matter (which are collisionless or nearly so, and continue outbound). Self-interaction of dark matter (DM) will cause the DM to lag the galaxies slightly. Weak lensing analyses with the proposed imaging (using multiband photometry to exclude foreground and cluster member galaxies) will yield measurements of the DM-galaxy offset accurate to ~5", sufficient to test current suggestions that the self-interaction cross section of dark matter may be in the range 0.1-0.5 cm2/gm. Only HST can provide this level of weak lensing precision.
Other merging systems are being studied with similar goals in mind, but this sample is unique in being radio-selected. The "radio relics" represent shocks which are vital in constraining the dynamics of the systems; only a few other mergers have clear evidence of shocks. A further key strength of this proposal is the ensemble approach: each system's unique set of dynamical properties (merger velocity, time since pericenter, etc) provides a unique test of the self-interacting DM (SIDM) hypothesis, so the constraints from the ensemble are powerful. We will derive constraints from the ensemble of these three clusters plus the Musket Ball Cluster (observed by us in a previous cycle), which shows a DM-galaxy offset at a level detectable only by HST.The goal is to determine the weak lensing centroid of each subcluster as accurately as possible. For this goal, the most efficient strategy is to focus the observations on the area nearest the presumed centroid, ie, near the galaxy centroid. Going deep in this area is essential, but covering a wider area is not. We also require multiband photometry to adequately exclude cluster members and foreground sources.
Required filters: F814W is the best filter for deep weak-lensing observations, and this is our primary filter. We need at least one other filter to exclude cluster members and foreground sources from the weak-lensing analysis. The F390W (or F435W) and F606W filters straddle the 4000A break at the relevant redshifts (0.10,0.19, 0.23, 0.366), and so are obvious candidates. This makes for three filters total, and in our experience that provides far superior source selection compared to two filters. Furthermore, because of the geometry our systems (explained below), in a majority (3/4) of the systems we can use source-selection filters in parallel with the lensing filter, so the use of two source-selection filters comes at very little cost.
Required area and pointings: We only need one ACS pointing per subcluster because we know the location of the mass centroid to within a fraction of an ACS field. In three of our four targets the subcluster separations are roughly the same as the ACS-WFC3 offset, so we can very efficiently image one subcluster with ACS+F814W while we image the other with WFC3 and the source-selection filters. Because two orbits with ACS+F814W are ideal for lensing, this nicely provides one orbit with WFC3+F390W and one orbit with WFC3+F606W. The slightly smaller WFC3/UVIS field means that the intersection of the lensing and source selection data covers only a WFC3 field, but this is still easily large enough for our purposes. Of course, we will dither to fill in gaps so that the final field size will be slightly larger than stated here.
In the fourth target (MACS J1752.0+4440), the angular separation of the subclusters is smaller than the ACS/WFC3 separation, so we cannot parallelize the observations to simultaniously observe the second subcluster. Thus we have adopted a more traditional two-pointing ACS mosic (one pointing per subcluster). The parallel WCF3 observations will target the periphery of the cluster merger and be used to study galaxies ejected during the merger as well as improve the weak lensing signal through additional source galaxies. Because the southwest subcluster of MACS J1752.0+4440 was perviously observed with 1 orbit ACS/WFC+F606W (Cycle 18 SNAP-12166) and 1 orbit ACS/WFC+F814W (Cycle 20 SNAP-12884) we only need to observe the southwest subcluster with one ACS/WFC+F435W orbit to provide the necessary color information to perform the weak lensing dependent science.
Required depth: Our experience with the Musket Ball and other clusters is that two orbits with ACS+F814W is sufficient to obtain a weak-lensing centroid accuracy of 7-9 arcsec. These clusters are at lower redshift than the previously observed clusters, thus potentially providing more background sources per square arcmin, but this potential advantage is largely canceled out by the greater Galactic extinction in the directions of these radio-selected systems. Therefore for most systems we will use two orbits with ACS+F814W. In the case of MACS J1752+4440, it was added to the sample list after we found that we could save 4 orbits on the original CIZA J2242 plan. With only 4 orbits we found it better to obtain 3 band photometry and only 1 orbit of F814W rather than 2 band photometry and 2 orbits of F814W. As stated above, the source-selection filters need not be as deep as the lensing filter, which works well with the parallel scheme outlined above.
-------- Realtime Justification --------
N/A
------ Calibration Justification -------
N/ACOSMOLOGYDefaultfalsefalsefalsefalsefalseSUPPORTEDCLUSTER OF GALAXIESGRAVITATIONAL LENSThis pointing is centered on the northern subcluster of 1RXS J0603.3+4214.
Note that there is a bright star (BD+42 1474; V=8.6 magnitude) between the ACS and WFC3 fields-of-view. Approximately 80 arcsec outside the edge of the ACS field-of-view, and approximately 80 arcsec outside the edge of the WFC3 field-of-view.J2000J2000CLUSTER OF GALAXIESGRAVITATIONAL LENSThis pointing is centered on the southern subcluster of 1RXS J0603.3+4214.
Note that there is a bright star (BD+42 1474; V=8.6 magnitude) between the ACS and WFC3 fields-of-view. Approximately 40 arcsec outside the edge of the ACS field-of-view, and approximately 100 arcsec outside the edge of the WFC3 field-of-view.J2000J2000CLUSTER OF GALAXIESGRAVITATIONAL LENSThis pointing is centered on the eastern subcluster of ZwCL J0008.8+5212.J2000J2000CLUSTER OF GALAXIESGRAVITATIONAL LENSThis pointing is centered on the western subcluster of ZwCL J0008.8+5212.J2000J2000CLUSTER OF GALAXIESGRAVITATIONAL LENSJ2000J2000CLUSTER OF GALAXIESGRAVITATIONAL LENSJ2000J2000CLUSTER OF GALAXIESGRAVITATIONAL LENSRICH CLUSTER1RXS-J175201.5+444046J2000CLUSTER OF GALAXIESGRAVITATIONAL LENSRICH CLUSTERThe southwest subcluster of MACS J1752.0+4440 was perviously observed with 1 orbit ACS/WFC+F606W (Cycle 18 SNAP-12166) and 1 orbit ACS/WFC+F814W (Cycle 20 SNAP-12884), however we need to observe the southwest subcluster with one additional ACS/WFC+F435W orbit to provide the necessary color information to perform the weak lensing dependent science.1RXS-J175201.5+444046J2000ACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF606WACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WPOS-TARGDITHER3.393This is the first part of the two part dither pattern LIne-Line. It is an ACS/WFC line dither pattern that performs a (0,0), (1/4,1/4), (1/2,1/2) ACS/WFC subpixel sampling, covers the chip gaps of ACS/WFC and WFC3/UVIS, and it performs a near (0,0), (1/3,1/3), (2/3,2/3) line subpixel sampling of WFC3/UVIS.
This dither pattern will serve the first 3/6 ACS/WFC+F814W exposures, and all 3/3 of the WFC3/UVIS+F606W exposures.LINEfalsefalse3298.006ACS-WFC-DITHER-LINE3falsePOS-TARGDITHER4.226This is the first part of the two part dither pattern LIne-Line. It is an ACS/WFC line dither pattern that performs a (3/4,1/4), (1/2,1/2), (1/4,3/4) ACS/WFC subpixel sampling, covers the chip gaps of ACS/WFC and WFC3/UVIS, and it performs a near (0,0), (1/3,1/3), (2/3,2/3) line subpixel sampling of WFC3/UVIS.
This dither pattern will serve the last 3/6 ACS/WFC+F814W exposures, and all 3/3 of the WFC3/UVIS+F390W exposures.LINEfalsefalse3250.364ACS-WFC-DITHER-LINE4falsePOS-TARGDITHER3.406It is an ACS/WFC line dither pattern that performs a (0,0), (1/3,1/3), (2/3,2/3) ACS/WFC subpixel sampling, covers the chip gaps of ACS/WFC and WFC3/UVIS, and it performs a near (0,0), (1/3,1/3), (2/3,2/3) line subpixel sampling of WFC3/UVIS.LINEfalsefalse3255.440LINE5falseThe scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.Parrallel observations of the dissociative galaxy cluster merger 1RXSJ0603.3+4214 with ACS/WFC and WFC3/UVIS. ACS is centered on the northern subcluster while WCF3 is centered on the southern subcluster. There will be 6 exposures with ACS/WFC+F814W, 3 exposures with WFC3/UVIS+F606W, and 3 exposures with WFC3/UVIS+F390W.
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Revision 2014-08-01:
Change the pointing of Visit 05 slightly. We performed our weak lensing analysis of the existing HST observation focused on the southern subcluster of this merger (from Visit 06) and found that the weak lensing peak was offset from the well defined galaxy peak much more than expected. So much so that the weak lensing peak is near the edge of the detector on the existing image and may actually be just off it. Since this offset is exactly the measurement we want to accurately make to constrain the dark matter cross-section we have decided that it is more important to measure exactly where the southern weak lensing peak is rather than observe the northern subcluster, as previously planned. The plan now is to mosaic the Visit 05 ACS observations with the existing Visit 06 ACS observations. We believe that impact due the loss of color informaiton can be mitigated by using our multi-band Subaru SuprimeCam observations to exclude cluster members for the lensing analysis.(Tic-Visit
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Note (8/22/2013): Following review of this target by STScI it was recommended that we move the pointing away from the bright star. We have implemented a move of ~20" from the original pointing which should enable us to reduce the effects of the bright star while maintaining our primary science. Additionally it was suggeted that we either shorten each orbit by a minute or increase the roll constraint from 235 to 257 degrees. We have chosen to shorten the orbit exposure time so that we can maintain a nice mosaic of the northeast and southwest subclusters.138257887500055.0(Tic-Visit
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:proposal-id 13343
:visit-id "07"
:orbit-number 3
:pcs-time 222
:si-vis-utilization 3051
:al-overhead-at-end 11
:internal-dur-at-end 1015
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3333
:pcs-gap 0
)false30The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode./Users/dawson/OneDrive/Proposals/HST/cycle21/OP-cache/radioprop-v08.xmlBecause the southwest subcluster of MACS J1752.0+4440 was perviously observed with 1 orbit ACS/WFC+F606W (Cycle 18 SNAP-12166) and 1 orbit ACS/WFC+F814W (Cycle 20 SNAP-12884) we only need to observe the southwest subcluster with one orbit of ACS/WFC+F435W to provide the necessary color information to perform the weak lensing dependent science.
Parrallel observations of the dissociative galaxy cluster merger MACS J1752.0+4440 with ACS/WFC and WFC3/UVIS. ACS is centered on the southwestern subcluster while WCF3 will observe the periphery of the cluster merger and be used to study galaxies ejected during the merger as well as improve the weak lensing signal through additional source galaxies. There will be 3 exposures with ACS/WFC+F435W of the southwest subcluster. The peripheral field will be observed with 3 exposures of WFC3/UVIS+F814W.
The orientation requirements are necessary to provide a contiguous mosaic of the cluster merger with two ACS pointings.
Revision 2014-08-01: We were notified by Harald Ebeling that the existing ACS F814W observations of the southwest subcluster are actually only ~0.5 orbits deep rather than the origianly believed 1 orbit deep. Since F814W is our lensing band and this is the most important aspect for our science, we have decide to use this orbit to observe the southwest with F814W rather than F435W. We considered the possability of switching between the F435W and F814W filters half-way through the orbit but found that the overhead losses comprimised the F814 depth and number of exposures to an unacceptable degree.(Tic-Visit
:proposal-id 13343
:visit-id "08"
:proposal-version -1
:trans-version "20140605"
:date "01-Aug-2014 17:05:19.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 1718912
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 13343
:visit-id "08"
:obset-id "08"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 13343
:visit-id "08"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2983
:al-overhead-at-end 5
:internal-dur-at-end 1015
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3316
:pcs-gap 0
)true10