We present far-infrared images of the Galactic oxygen-rich supernova remnant ( SNR ) G292.0+1.8 , acquired with the PACS and SPIRE instruments of the Herschel Space Observatory .
We find that the SNR shell is detected in the PACS blue ( 100 \micron ) band , but not in the red ( 160 \micron ) band , broadly consistent with results from AKARI observations .
There is no discernible emission from G292.0+1.8 in SPIRE imagery at 250 , 350 and 500 \micron .
Comparing the 100 \micron emission to that observed with Spitzer at 24 and 70 \micron , we find a very similar appearance for G292.0+1.8 at all three wavelengths .
The IR emission is dominated by dust from non-radiative circumstellar shocks .
In addition , the radiatively shocked O-rich clump known as the ’ Spur ’ on the eastern side of G292.0+1.8 is clearly detected in the PACS blue images , with marginal detection in the red .
Fitting the existing 14-40 \micron IRS spectra of the Spur together with photometric measurements from 70 \micron MIPS and 100 \micron PACS photometry , we place an upper limit of \lesssim 0.04 M _ { \odot } of ejecta dust mass in the Spur , under the most conservative assumption that the ejecta dust has a temperature of 15 K. Modeling the dust continuum in the IRS spectra at four positions around the rim , we estimate postshock densities ranging from n _ { p } = 3.5 cm ^ { -3 } to 11 cm ^ { -3 } .
The integrated spectrum of the entire SNR , dominated by swept up circumstellar dust , can be fit with a two-component dust model with a silicate component at 62 K and graphite component at 40 K for a total dust mass of 0.023 M _ { \odot } .