We would like to make ISO follow-up observations of Kepler, a young
galactic supernova remnant (SNR). Previous ISOCAM observations of this
remnant have been performed with two broad-band filters (LW8 and LW9) and
five CVF positions (9.8, 10.5 11.3, 12, 12.8 microns). The IR emission has
been resolved and intringuing features, such as a "line" at 12 microns near
the center of the remnant, have been revealed (see Figure 1).
In order to better assess the origin of the observed emission, we propose
to perform a full ISOCAM CVF scan of the remnant. We expect to detect
gaseous forbidden lines from Ne, Ar, S, Ni and perhaps Fe. The Ni and Fe
lines are of particular interest, as these elements are typical nuclear
burning products of type I SN, so that information on the nucleosynthesis
can be retreived. We also aim at detecting the circumstellar dust continuum
emission and at caracterising the dust composition (e.g. silicate feature).
The observations of Kepler (possibly a type Ia SN) will complement ISO CVF
scans of two other young galactic SNR's: Cas-A (probably a type Ib SN) and
the Crab nebula (a type II SN).
Given the expected fluxes from Kepler and given the need for
spectro-imaging observations over the whole remnant, the CVF mode of ISOCAM
appears to be the ideal way to conduct the observations.
The total time requested to perform the observations is 1 hour 35 minutes.