0 ----- Attempting Submission 1 (Tue Aug 28 18:12:45 GMT 2012) ----- ----- Attempting Submission 2 (Tue Aug 28 19:52:39 GMT 2012) ----- ----- Attempting Submission 3 (Fri Feb 15 23:13:40 GMT 2013) ----- Spectral Time Series of the Cas A Supernova We propose to obtain time-resolved spectroscopy of the outburst of the enigmatic historical supernova Cas A using STIS spectroscopy of light scattered by a narrow filament of interstellar dust. Our group has identified recent, high-surface brightness filaments that are likely to provide high signal-to-noise reproduction of the evolving spectrum of the Cas A outburst using verified, published techniques developed by us. The timescales to see any appreciable evolution in individual astrophysical objects are typically many orders of magnitudes larger than a human life. As a result, astronomers study large numbers of objects at different stages of their evolution to connect how a single object should change with time. Cas A can provide us with the ability, to look back in time to the point of explosion by observing its light echoes -- SN light scattered off of dust in the Milky Way, which causes a time delay in reaching us. In obtaining spectra of light echoes, we have been able to determine the maximum-light characteristics of the SN. Our goal here is to obtain a single STIS spectrum of a bright Cas A LE, which will provide us a time series of spectra and a spatially resolved light curve of the Cas A SN. With these data, we will measure the properties of the cooling envelope after the shock breakout of the SN to estimate the radius of the progenitor star. We will then be able to connect the progenitor star to the explosion to the SN to the SNR. Hi, visit #1 well be expected as a non-distrutive ToO when we discover our Cas A light echo. Cas A is near the CVZ, so we expect the orbits to be longer than indicated here, and we will adjust all the exposure times accordingly. Visit #2,3,4,5 to be scheduled all within 1-2 days, need to be executed about 10-40 days after visit 1. The reason for this is to measure precisely the position and orientation of the STIS slit in visits 3,4,5 ISM AND CIRCUMSTELLAR MATTER 12 false false 0.0 0.0 false false false SUPPORTED ISM SHOCK FRONT SNR This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 ISM SNR J2000 ISM SNR J2000 WFC3/UVIS Imaging No No F606W STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Imaging No No 50CCD WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F606W WFC3/UVIS Imaging No No F814W POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 1 false POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 2 false The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. After we get the data from visit 1, we can provide a proper acqusition star and offset (Or slew) to the light echo. The time between visit 1 and visits 2,3,4,5 is on the order of a couple weeks. angle of 180 is desireable, but +/- 5 degrees is okay 1348736129000 189.99999999999994 (Tic-Visit :proposal-id 12577 :visit-id "01" :proposal-version -1 :trans-version "20120802" :date "29-Aug-2012 04:11:10.0" :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 633488 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12577 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12577 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3130 :al-overhead-at-end 167 :internal-dur-at-end 498 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3511 :pcs-gap 0 ) false 1 0 The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. 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