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

M. Juvela; K. Mattila; D. Lemke; U. Klaas; C. Leinert; Cs. Kiss

doi:10.1051/0004-6361/200811351

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Volume 500 / No 2 (June III 2009)

A&A, 500 2 (2009) 763-768

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Table 1:

Parameters of linear fits of FIR surface brightness versus the HI line area.
Field	$\lambda$	Offset	Slope
	( $\mu$ m)	(MJy sr^-1)	(10^-3 MJy sr^-1 K^-1 km^-1 s)
EBL22	90	5.53 (0.30)	35.15 (4.26)
EBL22	150	3.56 (0.34)	38.91 (4.38)
EBL22	180	3.10 (0.38)	27.95 (5.42)
EBL26¹	90	18.66 (1.22)	17.28 (6.57)
EBL26¹	150	6.38 (1.33)	27.42 (7.36)
EBL26¹	180	6.00 (1.30)	25.76 (7.41)
NGP	90	6.31 (0.17)	24.60 (3.98)
NGP	150	3.53 (0.23)	28.61 (5.58)
NGP	180	3.20 (0.19)	31.91 (4.22)

The 1- $\sigma$ error estimates determined with the bootstrap method are given in parentheses. For NGP, the results correspond to a fit to the combined data of the northern and southern sub-fields (see Appendix B.2).
¹ Fit to data with $W({\rm HI})<$ 200 K km s^-1 only.

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