A Comprehensive Study of Dust Formation in Type II Supernovae with HST, Spitzer and Gemini
The recent discovery of three extremely bright Type II SNe, (2007it, 2007oc, 2007od) gives us a unique opportunity to combine observations with HST, Spitzer and Gemini to study the little understood dust formation process in Type II SNe. Priority 1 Spitzer Cycle 5 and band 1 Gemini 2008A time has already been approved for this project. Since late-time Type II SNe are faint and tend to be in crowded fields, we need the high sensitivity and high spatial resolution of ACS/HRC and NICMOS/NIC2 for these observations. This project is motivated by the recent detection of large amounts of dust in high redshift galaxies. The dust in these high-z galaxies must come from young, massive stars so Type II SNe could be potential sources. The mechanism and the efficiency of dust condensation in Type II SN ejecta are not well understood, largely due to the lack of observational data. We plan to produce a unique dataset, combining spectroscopy and imaging in the visible, near- and mid-IR covering the key phase, 400-700 days after maximum when dust is known to form in the SN ejecta. Therefore, we are proposing for coordinated HST/NOAO observations (HST ACS/HRC, NICMOS/NIC2 & Gemini/GMOS and TReCS) which will be combined with our Spitzer Cycle 5 data to study these new bright SNe. The results of this program will place strong constraints on the formation of dust seen in young high redshift (z>5) galaxies.
We will use SNe 1987A and 2003gd as templates to guide the observing strategy because 2003gd had a detected light
echo and both had a measurable change in flux over a 6 month timescale in both the visible and mid-infrared. See Figure 3.
We propose to use the ACS/HRC in three broad-band filters (F435W, F606W, F814W) and the
NICMOS/NIC2 in three broad-band filters (F110W, F160W, F205W), thereby providing the necessary
flux and colors to constrain the dust properties as well as its 3-D positions should a light
echo be detected. PSF-matched difference imaging, which can provide up to a tenfold increase
in sensitivity over direct photometry, will be used to detect faint signals since multiple epochs will
be available. Since we require (1) accurate photometry of the SNe, (2) images free from cosmic
rays and warm pixels, and (3) the highest resolution possible, we will use a 4-step dither on all
observations, which is optimal at rejecting bad pixels while minimizing overhead. These data will
be resampled using multidrizzle to further increase the resolution when searching for faint
echo signal close to the PSF of the SN.
Our choices of filters, visits, and exposure times have been made to use the smallest number
of orbits while maximizing the scientific content of our data. The three SNe have between 54 and 57 minutes of visibility per orbit minus the telescope acquisition (6 minutes) and the instrument acquisition (2.5 minutes). Since our first goal is to monitor
the light curves of each target, we will observe each SN three
times during Cycle 17, at the beginning middle and end of the cycle, with each visit separated by about 5 months as allowed by scheduling
constraints. This is adequate to measure a change in flux and a movement of a
light echo which, at the distances of our targets, travel across the sky as slowly as 0."1 arcsecs/year.
Based on our previous observations of SN 2003gd we find that the flux in a SN may drop by
a factor of 10 or 2.5 magnitudes over a 6 month period of time but a light echo around SN 2003gd developed which was
brighter, 21st magnitude per sq. arcsecond. Using the ACS/HRC ETC, we estimate
total exposure times of ~160 sec in each of F435W (B), F606W (V ) and F814W
(I) in order to obtain a S/N of at least 5 with B=V=I=26 mag, respectively for
a total of 480 sec. Using the model SED for SN 2003gd, we estimate time for two flux values,
2 muJy and 40 muJy at 1.0 micron and assume a blackbody shape with a temperature of 3000 K to
approximate the flux in all three NICMOS/NIC2 bands. These integration times provide a S/N of 2 per pixel for a light echo of 24 mag. per sq. arcsecond surface brightness. Using the
NICMOS ETC for the NIC2 camera, a S/N 5 is obtained for SN magnitudes of 26
with exposure times of 200 sec in each of F110W, F160W, and F205W, for a total
exposure time of 600 seconds for NICMOS. Assuming a 4 point dither pattern, filter changes and
guide star acquisition overheads, we estimate that we can just fit these observations into two orbits.
Thus, we estimate two orbits per epoch measurement of each SN, or 6 orbits total per SN. Therefore, we propose for 18 orbits for the observations of the three SNe.
If ACS/HRC is not available, this program could also be done with WFC3 with slightly less spatial resolution. There would be some differences in exposure times and overheads but the program could also be done with WFC3. The F438W, F606W and F814W filters on WFC3 could be used to replace the similar ACS/HRC filters.
We would also like to get the first observations of the SNe as early as we can. For that reason we have scheduled the first obvervations of 2007oc and 2007od for before Dec. 23, 2008 and Feb. 05, 2009, respectively, which are the ends of their first visibility of the cycle. If by chance the cycle does not start until after these periods we would like to get them as soon as their visibility allows. We will also most probably like to reschedule the other two observations of each of the SNe so that we get evenly spaced intervals between observations over the cycle.
ISM IN EXTERNAL GALAXIES
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false
1
0
Timing link suitability includes constraints ([Sequence (04 15) within 5.0 days])
The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
SN 2007oc ACS
(Tic-Visit
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false
1
0
The scheduling data was generated by CASM 17.2.
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SN 2007oc WFC3
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:low-sky "N"
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false
1
0
Timing link suitability includes constraints ([Sequence (12 17) within 5.0 days])
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false
1
0
The scheduling data was generated by CASM 17.2.
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false
1
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This is a repeat of visit 01.
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false
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This is a repeat of visit 03.
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false
1
0
The scheduling data was generated by CASM 17.2.
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This is a repeat of visit 51.
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