I have changed visit 3 to just one orbit, and reallocated that orbit to "visit 24" to observe SN 2002hh. ----- Submission 1 (Wed May 11 21:11:45 GMT 2005) -----
----- Submission 2 (Thu May 25 21:51:51 GMT 2006) -----
Assigned ID: 307
----- Submission 1 (Fri Jan 21 19:22:13 GMT 2005) -----
Probing Circumstellar and Interstellar Dust with Scattered-Light EchoesScattered-light echoes are one of the most powerful and efficient probes of the structure and composition of dust in circumstellar and interstellar (ISM) environments. Observations of light echoes provide exact three-dimensional positions of dust while constraining its density, grain-size and chemical make-up. Furthermore, echoes can be used as distance indicators via polarization measurements.
We propose to take deep, high-resolution ACS/HRC images of five supernovae (SNe). Two of these, SNe 1991T and 1998bu, have known circumstellar echoes that have only recently become fully resolvable with HST, and therefore require new observations. Only four echo-producing SNe are currently known, and in an attempt to increase this sample, we will also observe SNe 1999bw, 2002hh, and 2004dj. All three SNe are strong candidates for producing echoes from circumstellar and ISM dust, but only at angular sizes that HST can resolve. With these observations, we will use light echoes to their full advantage, to study (1) the mass-loss histories of Type II and Ia SN progenitors, (2) the contributions of these SNe and their progenitors to the dust content of their galaxies, (3) the structure of gas and stars in the ISM of external galaxies, and (4) we will independently measure the distance to the host galaxies, including a member of the Virgo cluster, and M96, a Type Ia cosmological distance-scale calibrator.Our primary observational goals are to carefully map the positions, fluxes,
and polarization of light echoes. With these data, we will determine the
distances to the SNe, the morphology of the scattering materials and the
properties of that dust, the mass-loss history of the SN progenitors, the
structure and composition of dust in the host galaxys' ISM, and evaluate
the impact of these results on models for the evolution of dust in these
environments.
Guided by Sugerman (2003) and practical experience with SNe 1987A and
1993J, we can maximize the efficiency of, and information contained
in, each observation by using ACS/HRC in three broad-band filters
(F435W, F606W, F814W), thereby providing the necessary flux and colors
to contrain the dust properties as well as its 3-D positions. When
needed, one emission-line (F658N) image will rule out positional
coincidence of echo-like nebular features. Based on the signal-to-noise
achieved in these previous echo observations, and the echo observability
calculations of Sugerman (2003), total exposure times of at least 1800 sec
in F435W, 1200 sec in F606W and 1500 sec in F814W will be sufficient for our goals.
Since echoes can be faint and/or small features, we must take data so
as to minimize the possible contamination from cosmic rays and warm
pixels. We adopt a 4-step HRC box dither sequence, which is optimal
at rejecting bad pixels while minimizing overhead and allowing a 25%
increase in image resolution.
For SNe 1991T and 1998bu, we already know that echoes are present,
that the field is not confused with nebular emission, and that
polarization data can be taken. We therefore need only observe in
F606W, F814W and the three polarizers with F435W. Using the APT orbit
planner, we find that they can be observed in 5 and 4 orbits, respectively.
The region around SN 1999bw does not appear to be confused with any
nebular emission in the only image present in the HST archive,
thus we will only take deep broad-band exposures (F435W, F606W, F814W)
with the exposure times listed above, which just fit in two orbits.
SN 2002hh is located a few arcsec from a suspected H II region,
and may itself be confused with another H2 region that was not
resolved by Spitzer. We will add narrow H-alpha (F658N) imaging
to the full-complement of broad-band observations (Polarized 435W;
unpolarized 606W and 814W), to rule out nebular contamination/confusion
and also to confirm the identification of the SN. This will require four orbits.
Follow-up imaging will be taken 6 months later in F606W to search for
faint echo structures using PSF-matched difference imaging.
SN 2004dj was observed in Nov 2004 in F330W with ACS/HRC,
revealing little detail about the SN field. However, an
11000 sec F469N WFPC2 image 1arcmin away shows considerable
structure, and since the SN is in a spiral arm, we extrapolate that
nebular structures may be present in our field. We will therefore take
the full series of broad-band and H-alpha images, requiring four orbits.
The SN is fading at a rate of 1 V mag every 3-4 months, and should be at
V=17 when observations can be taken. Broad-band 606W and 814W
observations are taken with short exposure times to avoid saturation.
Due to scheduling constraints, no follow-up observations are possible
in Cycle 14.Observations of SNe 1991T, 1998bu, 1999bw, and 2004hh have no observing constraints. Observations of SN 2002hh must be taken at least 6 months apart, thus we have requested that the first visit occur before the end of observability in 2005 Nov, with the follow-up visit scheduled more than 180-days later.ISM AND CIRCUMSTELLAR MATTER12false0.0falsefalsefalsefalsefalseSUPPORTEDEXT-STARSUPERNOVAThis object was generated by the targetselector and retrieved from the NED database.J200012 34 10.2000+02 39 56.40J2000EXT-STARSUPERNOVAThis object was generated by the targetselector and retrieved from the SIMBAD database.J200010 46 46.0900+11 50 7.00J2000EXT-STARSUPERNOVAThis object was generated by the targetselector and retrieved from the SIMBAD database.J200010 19 46.8100+45 31 35.00J2000EXT-STARSUPERNOVAThis object was generated by the targetselector and retrieved from the SIMBAD database.J200020 34 44.2900+60 07 19.00J2000EXT-STARSUPERNOVAThis object was generated by the targetselector and retrieved from the SIMBAD database.J200007 37 17.0200+65 35 57.80J2000EXT-STARSUPERNOVAThis object was generated by the targetselector and retrieved from the SIMBAD database.J200020 34 44.2900+60 07 19.00J2000ACS/HRCImagingNoYesF435WACS/HRCImagingNoNoF606WACS/HRCImagingNoNoF814WACS/HRCImagingNoYesF435WACS/HRCImagingNoNoF606WACS/HRCImagingNoNoF814WACS/HRCImagingNoNoF435WACS/HRCImagingNoNoF606WACS/HRCImagingNoNoF814WACS/HRCImagingNoNoF435WACS/HRCImagingNoNoF606WACS/HRCImagingNoNoF814WACS/HRCImagingNoNoF658NACS/HRCImagingNoNoF435WACS/HRCImagingNoNoF606WACS/HRCImagingNoNoF814WACS/HRCImagingNoNoF658NACS/HRCImagingNoYesF435WACS/HRCImagingNoNoF435WACS/HRCImagingNoNoF606WACS/HRCImagingNoNoF814WPOS-TARGDITHER0.15LINE0.098falsefalse63.5419.89ACS-HRC-DITHER-BOX1falsePOS-TARGDITHERDITHER40.198ACS-HRC-DITHER-BOXfalse63.5false0.0980.15244.28POS-TARGACS-HRC-DITHER-LINE19.892truePOS-TARGDITHER0.198LINEfalsefalse344.28ACS-HRC-DITHER-LINE3falseSN 1991T
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