0Assigned ID: 1298
----- Attempting Submission 1 (Mon Nov 07 17:31:56 GMT 2016) -----
HST Phase I Proposal 1298 (caustic_second.apt) successfully submitted.
Receipt: # 1298-1
----- Attempting Submission 2 (Mon Nov 07 17:33:06 GMT 2016) -----Unschedulable Visit
Unschedulable Visit
Unschedulable VisitAt Dr. Momcheva's suggestion, we have replaced the SPARS50 sampling with SPARS25 sampling to
increase the total number of samples during the WFC3 IR integrations, and optimize
the observation's S/N.500593385----- Attempting Submission 1 (Tue Nov 15 00:55:32 GMT 2016) -----
----- Attempting Submission 2 (Tue Dec 13 23:29:47 GMT 2016) -----
----- Attempting Submission 3 (Fri Dec 16 21:12:46 GMT 2016) -----
----- Attempting Submission 4 (Mon Jan 09 21:06:44 GMT 2017) -----
----- Attempting Submission 5 (Wed Jan 11 17:30:33 GMT 2017) -----I am not sure how to fix these errors, since they were found for already executed visits 1--3.A Hidden Potential Counterimage of a Highly Magnified Star at Redshift z=1.49An individual, highly magnified star close to a cluster caustic should provide a unique new window on the composition of dark matter. In late April 2016, we detected a brightening source (named "Icarus") near (<0.1 arcsec) the critical curve of the MACS J1149 galaxy cluster (z=0.54). Its unchanging spectral energy distribution (SED) matches that of a mid-to-late B-type star at the lensed background galaxy's redshift of z=1.49. Near peak brightness in May 2016, the individual star was likely magnified by the cluster by a factor of at least ~2000.
WFC3 imaging taken October 30 2016 after the field re-emerged from behind the sun has revealed an entirely unanticipated new source approximately 0.26 arcsec from Icarus. Its F125W-F160W color is consistent with that of Icarus. If a counterimage, it could potentially have been "hidden" due to temporary demagnification by a massive object (>20 solar masses) in the intracluster medium. However, this possibility only has a reasonable probability if massive black holes account for at least a modest fraction of dark matter, as has been hypothesized to explain the LIGO detection of merging 30 solar-mass black holes in September, 2015.
An alternate explanation is that the new image is of a different star with similar color undergoing an extreme microlensing event. If dark matter is an ultra-light scalar field, which would be granular (Hui et al. 2016), instead of a smoothly distributed WIMP, then the probability of a second event at the large offset from Icarus may be significantly larger. A measurement of the SED of the new source will determine if it can be the counterimage of Icarus, or if it is instead a different star.In April 2016, WFC3-IR imaging of the MACS J1149 galaxy-cluster field showed that a source near the cluster
s critical curve had brightened significantly. This source's characteristics are best explained by a highly magnified, individual star at the redshift z=1.49 of the lensed background galaxy. In new WFC3-IR imaging acquired on September 30, 2016, a new source appeared ~0.26" away from the magnified star. To determine if the new source is a counterimage of the highly magnified star identified in April 2016, a first part of the program will acquire three consecutive orbits consisting of ACS F606W + F814W, WFC3 F125W, and ACS F814W + F606W imaging respectively as soon as they may be scheduled.
The program's most important scientific goal is to measure the object's broadband spectral energy distribution to compare it with that of the potential counterimage. Since the source may vary in flux on short time scales, we would like the first three visits to occur ideally one after the other. We have also chosen the order of integrations in different filters to be able to remove any variation in flux that is first-order in time, assuming that visits are scheduling sequentially.
In a second part of the program, three separate visits will be used to construct the source's light curve. Each of these will be split between WFC3-IR F125W and WFC3-IR F160W integrations, and the visits should follow each other by approximately one week. The first of these visits should be scheduled approximately one week after the initial ACS F606W, ACS F814W, and WFC3 F125W visit.Intergalactic Medium and Cosmology0SUPPORTEDEXT-STARB6-B9.5 III-IJ2000J2000ACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/IRImagingNoNoF125WWFC3/IRImagingNoNoF125WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF125WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF125WWFC3/IRImagingNoNoF160WPOS-TARGDITHER0.135LINEfalsefalse346.84WFC3-UVIS-DITHER-LINE-3PT1falseTiming link suitability includes constraints ([02 After 01 by 0.1 to 0.1 days])The scheduling data was generated by CASM 24.2.CASM was run in Phase II mode.Visits 1, 2, and 3 should be scheduled immediately one after the other if possible. We are trying to avoid the possibility that the source could vary between these visits, since our principal science goal is to measure the object's broadband spectral energy distribution.
An observation scheduled as early as possible would be best.1480353925000303.0(Tic-Visit
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