0 Assigned ID: 513 ----- Attempting Submission 1 (Fri Apr 11 15:01:44 GMT 2014) ----- Hi Tony, Our first epoch of observations has taught us that our target's photometry is now dominated by the noise from the galaxy background. It makes more sense, then, to split our remaining two orbits into two separate epochs, as we won't gain in S/N by observing for more than one orbit at a time. Cheers, Or 1509702827 ----- Attempting Submission 1 (Thu Jul 24 19:17:46 GMT 2014) ----- ----- Attempting Submission 2 (Fri Sep 26 14:43:18 GMT 2014) ----- ----- Attempting Submission 3 (Mon Oct 20 15:59:58 GMT 2014) ----- ----- Attempting Submission 4 (Mon Dec 29 15:57:44 GMT 2014) ----- We propose to use WFC3 photometry from the near UV to the near IR to sample the bolometric light curve of the nearby Type Ia supernova (SN Ia) SN2012cg at late times (>900 days after maximum light). This light curve will allow us to conduct a fundamental test of the theoretically predicted behavior of SN Ia light curves at late times. We will observationally determine, for the first time, whether the nuclear physics of SN Ia ejecta is solely determined by the radioactive decay of 56Co to 56Fe, or whether (and by how much) other nuclear heating mechanisms (such as the leptonic decays of 57Co and 55Fe) become discernible, as predicted. Due to the high background of the galaxy at the location of the supernova, we will split our orbits between two epochs, the first when the supernova is ~925 days after maximum light, during December 13-19 2014, and the second when it is ~975 days after maximum light, during February 4-7 2015. In each epoch, both orbits will use the WFC3/UVIS F350LP filter, which covers the main UV-optical range of 300-1000 nm in which SNe Ia are usually observed. In each orbit, we will perform three exposures using the default WFC3-UVIS-LINE-3PT dither. To maximize the UVIS orbits, we will use the 1024x1024 UVIS subarray, centered on the location of the supernova. Based on similar images of the supernova in F350LP taken by GO-12880 (PI: A. Riess) and extrapolating the decaying light curve of the supernova out to our epochs, we expect the supernova to be at least as bright as 26-26.5 mag in F350LP. Furthermore, we have determined that two orbits per visit in F350LP are sufficient to obtain a signal-to-noise ratio ~20 in this filter, at our chosen epochs, which is high enough to distinguish between the various predictions tested here. UPDATE: Following our first epoch of observations, we have determined that our images are limited by the noise from the galaxy background. Thus, we cannot improve the signal-to-noise ratio of our target by observing it for more than one orbit. It is better, then, to split our remaining two orbits into two separate epochs. HOT STARS Default false false false false false SUPPORTED EXT-STAR SUPERNOVA TYPE IA J2000 J2000 WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F606W WFC3/UVIS Imaging No No F814W WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F606W WFC3/UVIS Imaging No No F814W WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 2 false 1413820321583 The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. 1418728793000 295.3888074468759 (Tic-Visit :proposal-id 13799 :visit-id "01" :proposal-version -1 :trans-version "20140605" :date "20-Oct-2014 11:52:01.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 104464 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13799 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13799 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2888 :al-overhead-at-end 84 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3222 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13799 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2999 :al-overhead-at-end 84 :internal-dur-at-end 151 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3222 :pcs-gap 0 ) true 2 0 1419372917846 The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. /home/orgraur/projects/sn2012cg/phaseII/OP-cache/phase2_draft7_1214-v02.xml (Tic-Visit :proposal-id 13799 :visit-id "02" :proposal-version -1 :trans-version "20140605" :date "23-Dec-2014 17:15:17.0" :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 52240 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13799 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13799 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2888 :al-overhead-at-end 84 :internal-dur-at-end 94 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3222 :pcs-gap 0 ) true 1 0 1419372918675 The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. /home/orgraur/projects/sn2012cg/phaseII/OP-cache/phase2_draft7_1214-v03.xml (Tic-Visit :proposal-id 13799 :visit-id "03" :proposal-version -1 :trans-version "20140605" :date "23-Dec-2014 17:15:18.0" :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 52240 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13799 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13799 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2888 :al-overhead-at-end 84 :internal-dur-at-end 94 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3222 :pcs-gap 0 ) true 1 0