Determination of the cosmic far-infrared background level with the ISOPHOT instrument

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Table 2:

The estimated zodiacal light emission.
Field	$T_{\rm ZL}$	I(25)	I(90)	I(150)	I(180)	rms
	(K)	(MJy/sr)				error
EBL22	280	40.51	7.69	3.03	2.19	13%
EBL26_ZL1	270	106.05	21.03	8.34	6.02	21%
EBL26_ZL2	270	100.50	19.84	7.87	5.68	7%
EBL26 (aver.)	270	100.98	19.94	7.91	5.71	14%
NGP_ZL1	260	28.65	5.95	2.38	1.72	5%
NGP_ZL2	260	29.15	6.06	2.42	1.75	18%
NGP (aver.)	260	28.69	5.96	2.38	1.72	12%

The columns are: (1) name of the EBL field (see Appendix, Table B.2); (2) temperature of the zodiacal light spectrum (Leinert et al. 2002); (3)-(6) estimated intensity of the zodiacal light at 25 $\mu$ m, 90 $\mu$ m, 150 $\mu$ m, and 180 $\mu$ m; and (7) relative uncertainty of the ZL value calculated on the basis of the difference of the fitted ZL model and the observations in the range 7.3-90 $\mu$ m. The zodiacal light estimates are given at the nominal wavelengths assuming a spectrum $\nu I_{\nu}$ = const. For EBL26 and NGP, two separate positions were observed (see Fig. B.1 and Table B.2).

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