Follow-up observations to the SST discovery of dust emission from SN 2002hh in NGC 6946

Details Follow-up observations to the SST discovery of dust emission from SN 2002hh in NGC 6946 Follow-up observations to the SST discovery of dust emission from SN 2002hh in NGC 6946

Oct 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sptz.prop..230b&link_type=abstract

Spitzer Proposal ID #230

Computer Science

Scientific paper

On September 6th we reported (Barlow et al.; IAUC 8400) the 3.6--8.0-um detection of the Type~II supernova SN 2002hh (located in the face-on spiral galaxy NGC 6946 at a distance of 6~Mpc), in archival Spitzer Space Telescope (SST) SINGS Legacy IRAC images taken on June 10.76 2004, when the 8.0-um flux of the supernova was 20.0 mJy. Since then we have also measured its flux in a SINGS Legacy MIPS 24-um image, taken one month after the IRAC data, which became available this week. SN 2002hh's IRAC+MIPS energy distribution can be fit by a 300K blackbody. Its equivalent blackbody emission radius of 1x10^17 cm is too large for the emitting dust to have been freshly condensed in the supernova (SN) ejecta, so it appears that the dust may have been formed and ejected in an earlier stage of evolution of the massive progenitor star and flash heated by the SN event. Gemini-N Director's Discretionary Time has been awarded to us this week for high angular resolution 3-20-um observations of SN 2002hh, to be be carried out in the next few weeks. We have also submitted a request for HST DD Time, with the aim of obtaining high angular resolution observations of SN 2002hh and its surrounds at optical and near-IR wavelengths, using the ACS and NICMOS (PI: B. Sugerman). Here we request SST Director's Discretionary Time for follow-up IR observations of the likely transient dust emission from this object. We request that IRS spectroscopy, together with IRAC+MIPS photometry, be obtained as early as possible (the supernova could fade to a level several times weaker than on June 10th 2004 and still produce good signal-to-noise ratios throughout most of the IRS spectral domain). As well as allowing the object's overall energy distribution to be constrained, the spectra will enable any dust emission or absorption features to be identified (an Av of 5.0 local to the SN has been deduced), together with any ionic emission lines. Accompanying short-duration IRAC 4-band and MIPS 24-um imaging will provide higher angular resolution than the IRS

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