I have modified the dither spacing to 1.022 arcseconds. I have changed the NICMOS exposure sequence to SPARSE16. Both at the reccomendation of support scientist de Jong. These slight modifications have been done on the approve phase II of this program. Used center pattern on all three patterns. ----- Attempting Submission 2 (Wed Jun 06 02:45:43 GMT 2007) ----- ----- Attempting Submission 3 (Wed Jun 06 20:26:18 GMT 2007) ----- none SEEDS: The Search for Evolution of Emission from Dust in Supernovae with HST and Spitzer The role that massive stars play in the dust content of the Universe is extremely uncertain. It has long been hypothesized that dust can condense within the ejecta of supernovae (SNe), however there is a frustrating discrepancy between the amounts of dust found in the early Universe, or predicted by nucleation theory, and inferred from SN observations. Our SEEDS collaboration has been carefully revisiting the observational case for dust formation by core-collapse SNe, in order to quantify their role as dust contributors in the early Universe. As dust condenses in expanding SN ejecta, it will increase in optical depth, producing three simultaneously observable phenomena: (1) increasing optical extinction; (2) infrared (IR) excesses; and (3) asymmetric blue-shifted emission lines. Our SEEDS collaboration recently reported all three phenomena occuring in SN2003gd, demonstrating the success of our observing strategy, and permitting us to derive a dust mass of up to 0.02 solar masses created in the SN. To advance our understanding of the origin and evolution of the interstellar dust in galaxies, we propose to use HST's WFPC2 and NICMOS instruments plus Spitzer's photometric instruments to monitor ten recent core-collapse SNe for dust formation and, as a bonus, detect light echoes that can affect the dust mass estimates. These space-borne observations will be supplemented by ground-based spectroscopic monitoring of their optical emission line profiles. These observations would continue our 2-year HST and Spitzer monitoring of this phenomena in order to address two key questions: Do all SNe produce dust? and How much dust do they produce? As all the SN are witin 15 Mpc, each SN stands an excellent chance of detection with HST and Spitzer and of resolving potential light echoes.
The combined use ofWFPC2 and NICMOS on HST and IRAC, IRS PUI 16-?m and MIPS 24-?m on Spitzer will allow us to derive a single SED extending from the optical to mid-infrared for each target at each epoch. Contemporaneous optical and infra-red photometry will make it possible to distinguish between dust condensing in the supernova ejecta and emission from previously existing dust, and it is therefore crucial that the data be temporally homogeneous. As a bonus, we will be able to resolve SNe light echoes that can affect the dust mass estimates because photometry of an unresolved light echo will cause the optical photometry in a SNe light curve to appear brighter than expected. We propose to observe each target two times in HST Cycle 16/SST Cycle 4, as accommodated by their visibility windows and as can be coordinated between the telescopes, except for our three oldest targets which, as their fluxes are not expected to change substantially over the course of a year at this late stage in their evolution, we will observe only once. Each Spitzer/Hubble set of observations of a given object will need to be carried out within 30 days of each other. Where two sets of observations are to be carried out, these will need to be separated by approximately six months. The HST strategy is described below and the Spitzer observations are described in the coordinated observations section of this proposal. HST Observing Strategy We use SN 2003gd as a template to guide the observing strategy because it had a detected light echo and a measurable drop in flux over a 6 month timescale in both the visible and mid-infrared. We propose to use the WFPC2/PC in three broad-band filters (F450W, 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 two 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. Since our first goal is to monitor the light curves of each object (with the exception of the three older supernovae), we will observe each SN two times during Cycle 16, with each visit separated by at least 6 months as allowed by scheduling constraints. A six month time scale 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 slow as 0.001 yr?1. 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 the light echo develops which is brighter, 21 magnitue per sq. arcsecond for SN 2003gd. Using theWFPC2/PC ETC, we estimate total exposure times of 2500 sec in F450W(B), 1000 sec in F606W(V ) and 2000 sec in F814W(I) in order to obtain a SNR of 7 for for SNe with B=27, V =27.0, and I=26.0, respectively for a total of 5500 sec. These integration times provide a SN ratio of 2 per pixel for a light echo of 24 mag. per sq. arcsecond surface brightness. Using the model SED for SN 2003gd, we estimate time for two flux values, 2 ?Jy and 40 ?Jy 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. Using the NICMOS ETC for the NIC2 camera, a SNR of 20 for the fainter flux value of 2 ?Jy is obtained with exposure times of 200 sec in F110W, 200 sec in F160W, and 500 sec in F205W, for a total exposure time of 900 seconds for NICMOS. Assuming a 4 point dither pattern, filter changes and guide star acquisition overheads, we estimate that we can just fit these WFPC2 and NICMOS observations into two orbits. Thus, we estimate two orbits per epoch measurement of the SN, or 4 orbits total per SN. Special Requirements The HST and Spitzer observations should be scheduled within one month of each other and it does not matter which comes first. Coordinated Observations: We will primarily use 8?m IRAC, 16?m IRS blue PUI and 24?m MIPS photometry, in conjunction with HST optical and near-infrared photometry, to characterise the SEDs. ISM AND CIRCUMSTELLAR MATTER 12 false 16.1 false false false false false false SUPPORTED EXT-STAR CIRCUMSTELLAR MATTER SUPERNOVA TYPE II This object was generated by the targetselector and retrieved from the NED database. J2000 10 19 46.8000 +45 31 35.00 J2000 EXT-STAR CIRCUMSTELLAR MATTER SUPERNOVA TYPE II This object was generated by the targetselector and retrieved from the NED database. J2000 20 34 44.3000 +60 07 19.00 J2000 EXT-STAR CIRCUMSTELLAR MATTER SUPERNOVA TYPE II This object was generated by the targetselector and retrieved from the NED database. J2000 01 36 42.6000 +15 44 20.00 J2000 EXT-STAR CIRCUMSTELLAR MATTER SUPERNOVA TYPE II This object was generated by the targetselector and retrieved from the NED database. J2000 07 37 17.0000 +65 35 58.00 J2000 EXT-STAR CIRCUMSTELLAR MATTER SUPERNOVA TYPE II This object was generated by the targetselector and retrieved from the NED database. J2000 20 35 25.3000 +60 07 18.00 J2000 EXT-STAR CIRCUMSTELLAR MATTER SUPERNOVA TYPE II This object was generated by the targetselector and retrieved from the NED database. J2000 13 29 53.4000 +47 10 28.00 J2000 EXT-STAR CIRCUMSTELLAR MATTER SUPERNOVA TYPE II This object was generated by the targetselector and retrieved from the NED database. 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