Table 1:

SPIRE observations of the Polaris flare.

	Pixel size	FWHM	G	S0	Noise		P0
(m)	(arcsec)	(arcsec)		(MJy sr-1)	(MJy sr-1)		(Jy2 sr-1)
250	6	18.1	(0.01)	(0.1)	1.26
350	10	25.2	(0.008)	(0.05)	0.55		4
500	14	36.9	(0.003)	(0.02)	0.34

Notes. Columns 4 and 5: gain and offset coefficients of the SPIRE-IRIS 100 m correlations. The uncertainty on G represents the rms of the ratio once the offset S₀ is removed from the SPIRE data. Similarly the uncertainty on S₀ is the rms of . These two uncertainties are correlated, but they give more realistic estimates compared to the statistical ones obtained with the linear regression fit (given in brackets). Column 6: noise level estimated directly on the power spectrum for (3.75<k<5 arcmin^-1 at 250 m). Column 7: power spectrum exponent of the interstellar component. Column 8: level of the Poissonian component associated with point sources and the CIB fluctuations. The fit of the power spectrum ( and P₀) was done between k = 0.025 arcmin^-1 and about twice the FWHM (2.0, 1.2 and 0.86 arcmin^-1 at 250, 350 and 500 m respectively).