Table 5: Estimated uncertainties of the different instrumental artifacts present in band 3 for the 10 AOT 01 speed 4 spectra of our sample of standard stars.
Uncertainty source 3A 3C 3D

bad detector data points, scan jumps & glitches $\sim$ 2% $\sim$ 2.5% $\sim$ 4%

fringe residuals

$\ \ \ \$ before correction with resp_inter & fringes $\sim$ 8% $\sim$ 4% $\sim$ 3%

$\ \ \ \$ after correction with resp_inter & fringes $\sim$ 2% $\sim$ 2% $\sim$ 2%

baseline ripples $\sim$ 2% $\sim$ 2% $\sim$ 1%

leakage at 27.5 $\mu$ m ^a $\sim$ 30%

RSRF artifact at 12.3 $\mu$ m $\sim$ 4%

Photometric calibration (scaling factors) ^b $\sim$ 6.5% ( $\sim$ 9.5%) $\sim$ 5.5% ( $\sim$ 9.5%) $\sim$ 9% ( $\sim$ 12%)

Notes:
^a Calculated as $F_{27.5~\mu\mbox{\scriptsize m}}/$ $G_{27.5~\mu\mbox{\scriptsize m}}$ with F the flux of the SWS spectrum, G the flux of the synthetic spectrum.
^b The estimated errors originate from our scaling factors. Between brackets: the mean of the scaling factors,
with inclusion of higher scanner speed observations of the sample of standard stars.

**Table 5:** Estimated uncertainties of the different instrumental artifacts present in band 3 for the 10 AOT 01 speed 4 spectra of our sample of standard stars.
Uncertainty source	3A	3C	3D
bad detector data points, scan jumps & glitches	$\sim$ 2%	$\sim$ 2.5%	$\sim$ 4%
fringe residuals
$\ \ \ \$ before correction with `resp_inter` & `fringes`	$\sim$ 8%	$\sim$ 4%	$\sim$ 3%
$\ \ \ \$ after correction with `resp_inter` & `fringes`	$\sim$ 2%	$\sim$ 2%	$\sim$ 2%
baseline ripples	$\sim$ 2%	$\sim$ 2%	$\sim$ 1%
leakage at 27.5 $\mu$ m ^a			$\sim$ 30%
RSRF artifact at 12.3 $\mu$ m	$\sim$ 4%
Photometric calibration (scaling factors) ^b	$\sim$ 6.5% ( $\sim$ 9.5%)	$\sim$ 5.5% ( $\sim$ 9.5%)	$\sim$ 9% ( $\sim$ 12%)

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