(skipped
… This figure is the same as that of Paper I(Kawara et al. 1998))Fig. 1. (top) C_90(95 micron) maps of 44'x44' field LHEX at RA(J2000)=10h52m, DEC(J2000)=57deg(left), and LHNW at RA(J2000)=10h34m, DEC(J2000)=58deg(right). These are made up of four 22'x22' sub-fields rebinned into a scale of 4.6"/pixel using bi-linear interpolation. (bottom) C_160(175 micron) maps, processed in the same manner as above.
Fig. 2. The cumulative number counts down to 150mJy: 1.1x105 sources sr-1 at 95 micron and 1.3x105 sources sr-1 at 175 micron are indicated by filled, red circles. The 1 sigma error bars are simply the Poisson statistical ones. The thick solid, and dashed lines "Maximal", and "Minimal" models by Guiderdoni et al.(1997, 1998).
Fig. 3a. The angular power spectrum of the 95 micron sky brightness fluctuation, which is an average of a few power spectra obtained for the 22'x22' sub-fields(red circles). The high-frequency part(>1 arcmin-1) is the structure within the ISOPHOT aperture, and hence does not show the true spatial fluctuation. If the fluctuation at the highest frequency is simply due to the instrumental noise, it should be subtracted from the power spectra, and thus giving the spectrum shown by green circles. The contribution from the infrared cirrus is estimated from Bcirrus(95 micron) = 0.41MJy sr-1 using the model by Gautier et al.(1992) with alpha= -2.9 for the index of power spectrum of the infrared cirrus.
Fig. 3b. The angular power spectrum of the 175 micron sky brightness fluctuation. Symbols are the same as those in Fig. 3a. The contribution from the infrared cirrus is estimated from Bcirrus(175 micron) = 0.81MJy sr-1 using the model by Gautier et al.(1992).
The figure below ( Flux comparison of the point sources) is not for presentation in the poster, but is for the internal use only
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