Studying X-ray instruments with galaxy clusters | Astronomy & Astrophysics (A&A)

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Table A.1

Parameters describing the correlations.

	a0		a1		a2		a3		a4
	A	B±σ_B	A	B±σ_B	A	B±σ_B	A	B±σ_B	A	B±σ_B
						MOS1/pn
a0	–	–	−1.40	1.53±0.04	0.65	−0.74±0.04	−0.12	0.141 ±0.011	0.0077	−0.0089±0.0010
a1	−0.68	1.09±0.03	–	–	−0.48	−0.016±0.020	0.094	0.0056±0.0080	−0.0061	−0.00032±0.00081
a2	1.31	1.09±0.05	−1.98	−0.021 ±0.041	–	–	−0.20	0.0012±0.0041	0.014	0.000036±0.000565
a3	−5.85	1.08±0.08	9.13	−0.010±0.079	−4.78	−0.0001 ±0.0199	–	–	−0.070	0.00020±0.00029
a4	71.9	1.04±0.10	−115.9	0.046±0.112	63.1	−0.024±0.039	−13.7	0.0040±0.0041	–	–
						MOS2/pn
a0	–	–	−1.17	1.31 ±0.14	0.60	−0.72±0.04	−0.11	0.14±0.01	0.0066	−0.0086±0.0011
a1	−0.68	1.11±0.04	–	–	−0.48	−0.03±0.02	0.09	0.011 ±0.009	−0.0060	−0.00082±0.00087
a2	1.25	1.12±0.06	−1.94	−0.044±0.046	–	–	−0.21	0.0016±0.0043	0.01	−0.000086±0.000584
a3	−5.1	1.09±0.09	8.4	−0.018±0.083	−4.6	−0.0025±0.0202	–	–	−0.071	0.00017±0.00030
a4	57.4	1.04±0.10	−101.1	0.050±0.113	58.7	−0.030±0.038	−13.4	0.0042±0.0041	–	–

Notes. The parameters of the best-fit linear models a_j- = A × a_i + Β to the coefficient pairs. σ_B is evaluated as a standard deviation of the difference between the Y-axis data and the corresponding model prediction.

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