0 Assigned ID: 200 ----- Attempting Submission 1 (Thu Apr 07 08:03:33 GMT 2016) ----- HST Phase I Proposal 200 (mergers.apt) successfully submitted. Receipt: # 200-1 ----- Attempting Submission 2 (Thu Apr 07 10:26:20 GMT 2016) ----- HST Phase I Proposal 200 (mergers.apt) successfully submitted. Receipt: # 200-2 FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser 0 ----- Attempting Submission 1 (Tue Jul 05 15:53:26 GMT 2016) ----- I believe a FLASH has been added to the observations in order to get away from the limit. However, if a contact scientist has a suggestion, I would be very happy to hear it (if the flash should be increased or decreased or another strategy followed). Constraining the Origin of Multiple Populations in Globular Clusters Ancient Globular Clusters (GCs), once thought to be the quintessential single stellar population, are now known to host multiple populations, with varying metal (and presumably helium) content between stars. Many scenarios have been put forward to explain the presence of the multiple populations, several of which rely on multiple generations of stars, with the first generation chemically enriching further generations. Testing these scenarios is difficult as nearby young clusters, that can be resolved into their constituent stars, do not show age/abundance spreads. It has been suggested that this is the case because the young clusters are not massive enough (>5*10^5 Msun) to hold onto their stellar ejecta, and hence follow a different evolutionary path than GCs. We propose UV imaging of a sample of massive (>10^6 Msun) young (50-500 Myr) clusters, in order to combine them with our ground based medium resolution high S/N VLT/X-shooter spectroscopy (and existing HST U-band and optical imaging), to confirm or refute age spreads within them. We will be able to place limits of >10-to-1, first-to-second generation mass ratios, which will directly test popular globular cluster formation models. This programme will provide UV imaging in the F275W filter with WFC3 of three ongoing/recent galactic mergers, NGC 34, NGC 4038 (the Antennae), and NGC 7252. It is designed to compliment previous WFC3 and ACS imaging of these galaxies in the optical. Stellar Populations 12 false false false false false false SUPPORTED GALAXY INTERACTING GALAXY STARBURST This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 GALAXY INTERACTING GALAXY STARBURST This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 GALAXY INTERACTING GALAXY STARBURST This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Imaging No No F275W WFC3/UVIS Imaging No No F275W WFC3/UVIS Imaging No No F275W POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 1 false /private/var/folders/pq/mpky14_s2fv3sct19h7w3ftr0000gq/T/OPVisit360517187883045219.xml The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 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