0 Assigned ID: 114 ----- Attempting Submission 1 (Wed Apr 09 19:02:03 GMT 2014) ----- HST Phase I Proposal 114 (LMCglobs_APT.apt) successfully submitted. ----- Attempting Submission 2 (Thu Apr 10 20:32:28 GMT 2014) ----- HST Phase I Proposal 114 (LMCglobs_APT.apt) successfully submitted. ----- Attempting Submission 3 (Fri Apr 11 23:15:37 GMT 2014) ----- HST Phase I Proposal 114 (LMCglobs_APT.apt) successfully submitted. 0 ----- Attempting Submission 1 (Tue Jul 15 14:13:13 GMT 2014) ----- HST Phase II Proposal 13727 (GO-13727phaseII.apt) successfully submitted. ----- Attempting Submission 2 (Tue Jul 15 14:49:32 GMT 2014) ----- Which Stars Go BOOM? Intermediate mass stars with M = 6 to 10 Msun will end their lives by either losing mass quiescently and forming massive white dwarfs or by exploding as core collapse type II supernovae. The critical mass separating these two stellar evolution channels is not only a fundamental threshold of stellar astrophysics, but is a crucial ingredient to generate reliable galaxy evolution simulations. Given the steepness of the stellar IMF, small changes in the critical mass directly affects chemical evolution scenarios, energetics, and feedback relations. Although most astronomers reference the critical mass at M = 8 Msun, there is a lack of robust theoretical or observational confirmation of this number. We propose to measure the critical mass directly by verifying the end products of stellar evolution in four rich, young, co-eval stellar populations. With ages of 25 to 60 Myr and total stellar masses >10,000 Msun, the Magellanic Cloud globular clusters NGC 1818, NGC 330, NGC 1805, and NGC 2164 have present-day main-sequence turnoff masses of M = 6.2, 7.2, 8.5, and 9.8 Msun, respectively. Existing photometry verifies that each cluster has a rich upper main sequence of massive stars, and therefore would have formed dozen(s) of stars above the present day turnoff. If those stars did not explode as core collapse supernovae, they will populate a clear blue white dwarf cooling sequence. Our experiment uses the full power, wavelength coverage, and resolution of HST/WFC3 to detect these cooling sequences in high-precision, UV-sensitive color-magnitude diagrams. Targeting 3 globular clusters in the LMC and 1 in the SMC in WFC3/UV filters to get deep UV CMDs and find their cooling white dwarfs. Each cluster is contained in one visit with 3 orbits, with a series of F225W and F336W observations. Short exposures are added at the start and end of different orbits to mitigate saturation of bright sources. All exposures (except for shorts) are dithered and offset from the center to avoid the chip gap and to put the bulk of the cluster population on UVIS2 (cleaner flat field pattern). Post flash has been added to ensure 10-12 e- in each exposure to mitigate CTE. RESOLVED STELLAR POPULATIONS Default false true 0.0 0.0 false false false SUPPORTED STELLAR CLUSTER GLOBULAR CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STELLAR CLUSTER GLOBULAR CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STELLAR CLUSTER GLOBULAR CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STELLAR CLUSTER GLOBULAR CLUSTER This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F336W /Users/jkalirai/data/Proposals/HST/Cycle22/JasonUpperMassLimitLMC/PhaseII/OP-cache/GO-13727phaseII-v01.xml The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. (Tic-Visit :proposal-id 13727 :visit-id "02" :proposal-version -1 :trans-version "20140605" :date "15-Jul-2014 09:52:36.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 3753680 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13727 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13727 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3237 :al-overhead-at-end 122 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3572 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13727 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3349 :al-overhead-at-end 124 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3572 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13727 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3349 :al-overhead-at-end 120 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3572 :pcs-gap 0 ) true 3 0 /Users/jkalirai/data/Proposals/HST/Cycle22/JasonUpperMassLimitLMC/PhaseII/OP-cache/GO-13727phaseII-v03.xml The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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