  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 blueimages, 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 <~ 0.04 solar masses, 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 solar masses.
