$\mu$m). The observing mode (FIS01), the scan speed (8$''$ s$^{-1}$), and the reset interval (2 s) are the same as those adopted for the sample in H08. The method of data reduction and analysis is the same as that in H08, and the measured fluxes are listed in Table \[tab:flux\]. Below we briefly review the data reduction and analysis (see H08 for details).

The raw data were reduced by using the FIS Slow Scan Tool (version 20070914).[^3] Because the detector response is largely affected by a hit of high energy ionizing particle, we used the local flat; that is, we corrected the detector sensitivities by assuming uniformity of the sky brightness [@verdugo07].[^4] The errors caused by the smoothing procedures are well within 10% for *N60* ($65~\mu$m) and *WIDE-S* ($90~\mu$m), 20% for *WIDE-L* ($140~\mu$m), and 25% for *N160* ($160~\mu$m). These error levels are consistent to or somewhat larger than the background fluctuation mainly caused by a hit of high energy ionizing particle, which implies that the background fluctuation is a major component in the errors. The above values are adopted for the errors, but we adopt larger errors for some galaxies which have larger background noises. At *N160* (160 $\mu$m), some 