We present 3.6 - 160 \mu m infrared images of Kepler ’ s supernova remnant ( SN1604 ) obtained with the IRAC and MIPS instruments on the Spitzer Space Telescope .
We also present MIPS SED low resolution spectra in the 55 - 95 \mu m region .
The observed emission in the MIPS 24 \mu m band shows the entire shell .
Emission in the MIPS 70 \mu m and IRAC 8 \mu m bands is seen only from the brightest regions of 24 \mu m emission , which also correspond to the regions seen in optical H \alpha images .
Shorter wavelength IRAC images are increasingly dominated by stars , although faint filaments are discernible .
The SED spectrum of shows a faint continuum dropping off to longer wavelengths and confirms that strong line emission does not dominate the mid-IR spectral region .
The emission we see is due primarily to warm dust emission from dust heated by the primary blast wave ; no excess infrared emission is observed in regions where supernova ejecta are seen in X-rays .
We use models of the dust to interpret the observed 70/24 \mu m ratio and constrain the allowed range of temperatures and densities .
We estimate the current mass of dust in the warm dust component to be 5.4 \times 10 ^ { -4 } M _ { \odot } , and infer an original mass of about 3 ~ { } \times~ { } 10 ^ { -3 } M _ { \odot } before grain sputtering .
The MIPS 160 \mu m band shows no emission belonging to the remnant .
We place a conservative but temperature dependent upper limit on any cold dust component roughly a factor of 10 below the cold dust mass inferred from SCUBA observations .
Finally , we comment on issues relevant to the possible precursor star and the supernova type .