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

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Table E.1:

Comparison of existing CIRB estimates in the FIR range. The error estimates quoted by the authors are shown in parenthesis. In our case, we include only the statistical uncertainty.
$\lambda$	$I_{\nu}$	Reference	Instrument
( $\mu$ m)	(MJy sr^-1)
90	<2.3	this paper	ISO/ISOPHOT
150/180	1.08 (0.32)²	this paper	ISO/ISOPHOT
100	<1.1¹	Hauser et al. 1998	COBE/DIRBE
	0.73 (0.20)¹
100	0.37 (0.10)	Dwek et al. 1998	COBE/DIRBE
100	0.78 (0.20)	Lagache et al. 2000	COBE/DIRBE
100	0.83 (0.27)	Finkbeiner et al. 2000	COBE/DIRBE
140	1.49 (0.33)	Schlegel et al. 1998	COBE/DIRBE
140	1.17 (0.33)	Hauser et al. 1998	COBE/DIRBE
140	0.70 (0.28)	Hauser et al. 1998	COBE/FIRAS
140	0.70 (0.28)	Lagache et al. 1999	COBE/DIRBE
140	1.12 (0.56)	Lagache et al. 2000	COBE/DIRBE
140	1.17 (0.37)	Odegard et al. 2007	COBE/DIRBE
240	1.36 (0.16)	Schlegel et al. 1998	COBE/DIRBE
240	1.12 (0.24)	Hauser et al. 1998	COBE/DIRBE
240	1.04 (0.16)	Hauser et al. 1998	COBE/FIRAS
240	0.88 (0.16)	Lagache et al. 1999	COBE/DIRBE
240	0.88 (0.56)	Lagache et al. 2000	COBE/DIRBE
240	1.04 (0.24)	Odegard et al. 2007	COBE/DIRBE

¹ Hauser et al. did not claim detection at 100 $\mu$ m, because the CIRB signal failed
test for isotropy; ² only the statistical error is quoted.

Source LaTeX | All tables | In the text

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