0 Assigned ID: 382 ----- Attempting Submission 1 (Fri Apr 08 04:30:56 GMT 2016) ----- HST Phase I Proposal 382 (R106.apt) successfully submitted. Receipt: # 382-1 ----- Attempting Submission 2 (Fri Apr 08 08:20:17 GMT 2016) ----- 0 ----- Attempting Submission 1 (Tue Jul 19 20:44:02 GMT 2016) ----- Submission failed due to error communicating with the submission server. Please retry in a few minutes. If this error persists please contact the help desk at help@stsci.edu ----- Attempting Submission 2 (Tue Jul 19 20:44:23 GMT 2016) ----- Ruprecht 106: Too small to succeed? Photometric studies with HST have completely changed our understanding of globular clusters (GCs), to the point where features that were once considered anomalous (light-element abundance variations, multiple populations) are now part of the definition of the term 'globular cluster'. With this proposal, we seek to establish some minimum requirements for the formation of multiple stellar populations in GCs. We will apply the unique UV and blue imaging capabilities of the Wide Field Camera 3 UVIS channel to search for multiple stellar sequences, or lack thereof, in the CMD of the peculiar GC Ruprecht 106. Ruprecht 106 is exceptional among the Galactic GC population in its primordial chemical composition, low mass, and (likely) extra-Galactic origin. The limited abundance information available from spectroscopy indicates a low oxygen abudance (average [O/Fe] ~ 0 at [Fe/H] ~ -1.5) with no significant star-to-star scatter in the light elements. Light element abundance variations are one of the fundamental signatures of multiple stellar populations in GCs; the other is the presence of multiple stellar sequences in the CMD. The first line of inquiry, spectroscopy, suggests Ruprecht 106 may be a true simple stellar population. This proposal addresses the second line of inquiry, the photometric signature, which has never before been attempted. The unrivaled resolution and sensitivity of the Hubble Space Telescope will allow us to discover whether the CMD of Ruprecht 106 reveals multiple and/or broadened stellar sequences and, thus, hosts multiple stellar populations -- or not. The observing program is designed to image Ruprecht 106 in two WFC3/UVIS filters, F336W and F438W. These data will be combined with existing ACS/WFC data in F814W to make the "CUBI" index (F336W-F438W)-(F438W-F814W), which is sensitive to light-element abudance variations. There are 4 1-orbit visits, each separated by approximately 90-degree change in the orientation angle. This allows for maximum sampling of the PSF. Stellar Populations 6 false false false false false false SUPPORTED STELLAR CLUSTER GLOBULAR CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F438W POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 2 false The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 1490793524000 355.29984 (Tic-Visit :proposal-id 14726 :visit-id "01" :proposal-version -1 :trans-version "20160601" :date "19-Jul-2016 14:58:59.0" :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 866240 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14726 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14726 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3070 :al-overhead-at-end 121 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3403 :pcs-gap 0 ) false 1 0 The scheduling data was generated by CASM 24.2. 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