Table 1: Comparison of the extragalactic and asteroid full fluctuation power levels at some representative wavelengths of infrared and submillimetre space instruments. Asteroid fluctuation power was derived at the specified $\lambda$ - $\lambda _{\odot }$ helioecliptic longitude, and at the ecliptic plane. The columns of the table are: 1) name of the instrument; 2) wavelength; 3) extragalactic background fluctuation power (EGB); 4) asteroid fluctuation power (MBA); 5) solar elongation used in the MBA fluctuation power calibration, in accordance with the visibility constraints of the instrument; 6) Ecliptic latitude range above/below the ecliptic plane, where a specific instrument is considered as "affected'' by asteroid confusion noise. Missing values indicate that the instrument is not affected.
Instrument $\lambda_i$ $\ensuremath{\log_{10}(\delta F_0/{\rm Jy}^2~{\rm sr}^{-1})}$ $\lambda - \lambda_{\odot}$ $\vert{\Delta\beta}\vert$

( $\mu{\rm m}$ ) (EGB) (MBA) (deg) (deg)

Spitzer/IRAC 8 1.49 2.11 120 20

Akari/IRC 9 1.47 1.21 90 13

Akari/IRC 18 1.39 2.23 90 16

Spitzer/MIPS 24 2.04 2.70 120 21

Akari/FIS 65 3.47 1.34 90 -

Spitzer/MIPS & Herschel/PACS 70 3.69 1.62 120 -

Akair/FIS 90 4.06 0.98 90 -

Herschel/PACS 100 4.42 0.95 120 -

Akari/FIS 140 4.42 0.41 90 -

Akari/FIS 160 4.43 0.23 90 -

Spitzer/MIPS & Herschel/PACS 160 4.43 0.36 120 -

Herschel/SPIRE 250 4.29 -0.21 120 -

Herschel/SPIRE 350 3.88 -0.59 120 -

Herschel/SPIRE 500 3.27 -1.64 120 -

**Table 1:** Comparison of the extragalactic and asteroid full fluctuation power levels at some representative wavelengths of infrared and submillimetre space instruments. Asteroid fluctuation power was derived at the specified $\lambda$ - $\lambda _{\odot }$ helioecliptic longitude, and at the ecliptic plane. The columns of the table are: 1) name of the instrument; 2) wavelength; 3) extragalactic background fluctuation power (EGB); 4) asteroid fluctuation power (MBA); 5) solar elongation used in the MBA fluctuation power calibration, in accordance with the visibility constraints of the instrument; 6) Ecliptic latitude range above/below the ecliptic plane, where a specific instrument is considered as "affected'' by asteroid confusion noise. Missing values indicate that the instrument is *not* affected.
Instrument	$\lambda_i$	$\ensuremath{\log_{10}(\delta F_0/{\rm Jy}^2~{\rm sr}^{-1})}$	$\lambda - \lambda_{\odot}$	$\vert{\Delta\beta}\vert$
	( $\mu{\rm m}$ )	(EGB)	(MBA)	(deg)	(deg)
Spitzer/IRAC	8	1.49	2.11	120	20
Akari/IRC	9	1.47	1.21	90	13
Akari/IRC	18	1.39	2.23	90	16
Spitzer/MIPS	24	2.04	2.70	120	21
Akari/FIS	65	3.47	1.34	90	-
Spitzer/MIPS & Herschel/PACS	70	3.69	1.62	120	-
Akair/FIS	90	4.06	0.98	90	-
Herschel/PACS	100	4.42	0.95	120	-
Akari/FIS	140	4.42	0.41	90	-
Akari/FIS	160	4.43	0.23	90	-
Spitzer/MIPS & Herschel/PACS	160	4.43	0.36	120	-
Herschel/SPIRE	250	4.29	-0.21	120	-
Herschel/SPIRE	350	3.88	-0.59	120	-
Herschel/SPIRE	500	3.27	-1.64	120	-

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