Testing the models of X-ray driven photoevaporation with accreting stars in the Orion Nebula Cluster

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Volume 648 (April 2021)

A&A, 648 (2021) A121

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Table 2

Summary of the correlation analysis results.

Parameters	N⁽¹⁾	a⁽²⁾	b⁽²⁾	ρ ⁽³⁾	p ⁽⁴⁾	r ⁽⁵⁾	\⁽⁶⁾
L_X vs. M	332	30.58 ± 0.07	2.08 ± 0.16	0.62	<0.001	0.62 ± 0.04	0.58
L_{X, soft} vs. M	332	30.39 ± 0.07	2.00 ± 0.16	0.60	<0.001	0.62 ± 0.04	0.58
L_{X, char} vs. M	332	30.45 ± 0.07	2.12 ± 0.15	0.64	<0.001	0.65 ± 0.04	0.55
Ṁ_acc vs. M	332	− 8.11 ± 0.10	1.07 ± 0.22	0.32	<0.001	0.32 ± 0.06	0.80

Ṁ_acc∕Ṁ_acc(M) vs. L_X∕L_X(M)	332	0.00 ± 0.04	− 0.27 ± 0.10	− 0.12	0.031	−0.21 ± 0.07	0.79
Ṁ_acc∕Ṁ_acc(M) vs. L_{X, soft}∕L_{X, soft}(M)	332	0.00 ± 0.04	−0.32 ± 0.10	−0.14	0.008	−0.25 ± 0.07	0.79
Ṁ_acc∕Ṁ_acc(M) vs. L_{X, char}∕L_{X, char}(M)	332	0.00 ± 0.04	−0.37 ± 0.11	−0.16	0.004	− 0.26 ± 0.07	0.79
Ṁ_acc∕Ṁ_acc(M, τ) vs. L_X∕L_X(M, τ)	332	0.00 ± 0.04	−0.27 ± 0.07	−0.19	<0.001	−0.20 ± 0.05	0.74
L_acc∕L_acc(M, τ) vs. L_X∕L_X(M, τ)	332	0.00 ± 0.04	−0.26 ± 0.07	−0.18	<0.001	−0.20 ± 0.05	0.73

L_X∕L_X(M) vs. T₂	229	−6.26 ± 2.27	0.86 ± 0.30	0.20	0.003	0.27 ± 0.10	0.48
Ṁ_acc∕Ṁ_acc(M) vs. T₂	229	− 13.68 ± 3.51	1.81 ± 0.47	0.30	<0.001	0.36 ± 0.09	0.74

Notes. The relations correspond to the logarithmic equation of the parameters and have the form log y = a + b × logx. The parameters were determined with the LINMIX_ERR method. ⁽¹⁾Sample size. ⁽²⁾ a is the intercept and b the slope of the linear regression line. Errors for the least squares analysis are the standard deviations. ⁽³⁾ Spearman’s ρ rank correlation coefficient. ⁽⁴⁾ p-value: two-sided significance of ρ’s deviation from zero. ⁽⁵⁾Linear correlation coefficient determined with LINMIX_ERR. ⁽⁶⁾Standard deviation of the residuum (scatter).

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