Imaging the Distribution of Iron in a Type Ia Supernova

Dear Alison Vick: I have prepared a Phase II proposal for my GO program 11722 "Imaging the Distribution of Iron in a Type Ia Supernova" I think I've done it all OK. I didn't see this time a box to check off CR-Split so I guess that isn't done by default any longer. The exposures I have enetered have been auto-adjusted and are mostly either 591 sec long or 646 sec long. Please let me know if I have mis-understood something. Otherwise, I think its a fairly simple program. It does have 5 orbits in 1 visit. I hope this can be done. If not, I can revise it to be either 4 + 1 or 3 +2. best regards, -Rob Fesen ----- Attempting Submission 1 (Thu Jun 26 15:04:49 GMT 2008) ----- The only warning in this program is one about not shifting the target around much due to the fact I am using a ramp filter. Please let me know if there is any problem with this proposal. Thank you. -R. Fesen Assigned ID: 682 ----- Attempting Submission 1 (Fri Mar 07 22:46:35 GMT 2008) ----- Imaging the Distribution of Iron in a Type Ia Supernova We know Type Ia supernovae are thermonuclear explosions of CO white dwarfs, but we don't know the specifics of how the nuclear burning proceeds from the core outward to the surface once it starts. Thermonuclear instability in a WD core is thought to start off as a subsonic, turbulent deflagration wave or "burning" wave but then may, at some point, transition into a supernova blast or detonation wave. In such a "delayed detonation" model, differences between normal and subluminous Type Ia SNe reflect differences in the amount of burning that has occurred in the pre-detonation phase. More burning helps to pre-expand the WD before passage of the detontation wave which then lowers the density of the outer layers and, in turn, results in a different element production and internal structure. Directly imaging the 2D chemical distribution of ejecta from a Type Ia SN is actually possible in the case of the subluminous Type Ia SN 1885 which occurred on the near-side of M31's central bulge. The entire 123 year old remnant -- core to outer edge -- is visible via strong near-UV, Ca and Fe line absorptions, and remarkably, is still in near free expansion. This means that elemental stratification seen today is likely to accurately reflect the explosive nucleosynthesis physics. We propose ACS WFC images of SN 1885 to take advantage of this extraordinary situation: Having a young, nearby Type Ia SN remnant visible in silhouette against a galaxy-size light table. The proposed observations will reveal the Fe ejecta distribution, density structure, sphericity, and ionization state as a function of expansion velocity, thereby testing SN Ia explosion models with direct Fe-rich ejecta mapping data.

This project is to image the remnant of SN 1885A in the bulge of M31 using the ramp filter FR388N centered on the remnant at the wavelength of 3710 Angstroms. All five orbits will be used to image the target in this filter. The target (SNR 1885A) is only 0.8 arcsec across (diameter). none. none. ISM IN EXTERNAL GALAXIES 12 false 0.0 0.0 false false false false false SUPPORTED ISM SNR EJECTA J2000 00 42 42.9000 +41 16 5.00 J2000 ACS/WFC RampFilter No No FR388N POS-TARG DITHER DITHER 2 0.149 ACS-WFC-DITHER-LINE false false 0.29 5 34.25 POS-TARG ACS-WFC-DITHER-LINE 47.23 2

true

The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. /private/tmp/OPVisit12890.xml 1214491664944 (Tic-Visit :proposal-id 11722 :visit-id "01" :proposal-version -1 :trans-version "20080515" :date "26-Jun-2008 10:47:44.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 5684480 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11722 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11722 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3018 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3351 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11722 :visit-id "01" :orbit-number 2 :pcs-time 195 :si-vis-utilization 3156 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3351 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11722 :visit-id "01" :orbit-number 3 :pcs-time 195 :si-vis-utilization 3156 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3351 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11722 :visit-id "01" :orbit-number 4 :pcs-time 195 :si-vis-utilization 3156 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3351 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11722 :visit-id "01" :orbit-number 5 :pcs-time 195 :si-vis-utilization 3156 :al-overhead-at-end 0 :internal-dur-at-end 349 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3351 :pcs-gap 0 ) true 5 0