Effective area calibration of the reflection grating spectrometers of XMM-Newton - I. X-ray spectroscopy of the Crab nebula

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Volume 497 / No 1 (April I 2009)

A&A, 497 1 (2009) 291-310

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Table 5:

Summary of systematic and statistical uncertainties in the Crab spectrum.
$\lambda$	E	a	b	c	d	e	f	g	h	i	j	k	l	m
Å	keV
5	2.5	0.1	0.008	0.003	0.000	0.000	0.001	0.001	0.003	0.050	0.000	0.30	1.0	0.0031
7	1.8	0.1	0.011	0.005	0.000	0.003	0.002	0.002	0.000	0.010	0.001	0.04	0.022	0.0025
10	1.2	0.1	0.015	0.007	0.001	0.005	0.004	0.002	0.004	0.004	0.002	0.01	0.010	0.0025
15	0.8	0.1	0.019	0.010	0.001	0.000	0.006	0.010	0.008	0.005	0.002	0.00	0.008	0.0026
20	0.6	0.1	0.022	0.011	0.002	0.005	0.007	0.001	0.010	0.015	0.001	0.00	0.008	0.0045
25	0.5	0.1	0.024	0.013	0.002	0.005	0.009	0.003	0.012	0.020	0.001	0.00	0.008	0.0048
30	0.4	0.1	0.026	0.014	0.003	0.002	0.010	0.001	0.014	0.050	0.000	0.00	0.010	0.0090
type		c	c	c	c	u	c	c	c	u	c	u	u	u
$\Delta\alpha$		0.016	0.010	0.006	0.002	0.001	0.005	0.001	0.010	0.010	0.000	0.027	0.006	-
$\Delta A$		0.100	0.019	0.010	0.001	0.001	0.004	0.005	0.004	0.003	0.002	0.005	0.002	-

Main power-law: ^a uncertainty in the K01 continuum model.
Curvature corrections: ^b a 50% change in the lower energy of the 2-8 keV range used for the normalisation of the Chandra data; ^c break size $\Delta\Gamma=0.006$ at low E if a break (at 4 keV) is present in the Kuiper et al. data; ^d 0.5% of the absorption with $N{_{\rm H}}$ higher by 7.5 $\times$ 10²⁴ m^-2; ^e numerical approximation of $f_{\rm c}(E)$ by (3).
Interstellar absorption: ^f systematic uncertainty in the dust model; ^g neglect of hot gas; ^h interstellar carbon abundance.
Instrumental corrections: ⁱ cross-dispersion correction; ^j pile-up correction for 2 CCD mode; adopts 5% uncertainty in a ( $2\sigma$ ); ^k redistribution errors, estimated from difference fit residuals RGS1 and RGS2; ^l errors in the Chebychev polynomials used for the effective area correction; ^m typical combined RGS1/RGS2 statistical uncertainty for a full 1 Å wide bin.

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