Parametric strong lensing model of the galaxy cluster Abell 2390 from Euclid and MUSE observations

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Volume 704 (December 2025)

A&A, 704 (2025) A338

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Table 2.

Input and optimized parameter values of the reference lens model (M9) for the galaxy cluster A2390.

Mass component	Free parameter	Prior	Posterior
Cluster halo	x_DM [arcsec]	0 ± 100	2.76 ± 0.08
	y_DM [arcsec]	0 ± 100	$1 . 20_{- 0.05}^{+ 0.06}$ $1.20^{+0.06}_{-0.05}$
	q_DM	0.25 ÷ 1.0	0.73 ± 0.01
	θ_DM [rad]	0 ÷ π	1.1 ± 0.1
	σ_DM [km s⁻¹]	500 ÷ 1500	1195 ± 12
	r_core,DM [arcsec]	0.01 ÷ 30.0	16.7 ± 0.4

G29	σ_G29 [km s⁻¹]	50 ÷ 500	$233_{- 3}^{+ 5}$ $233^{+5}_{-3}$
	r_cut, G29 [arcsec]	0.05 ÷ 25.0	$18 . 2_{- 4.1}^{+ 4.3}$ $18.2^{+4.3}_{-4.1}$

External shear	\|γ\|	0.0 ÷ 0.3	0.17 ± 0.01
	θ_γ [rad]	0 ÷ π	2.22 ± 0.01

Scaling relations	σ_ref [km s⁻¹]	285 ± 41	288 ± 5
	r_cut,ref [arcsec]	0.05 ÷ 30.0	$16 . 1_{- 0.9}^{+ 1.3}$ $16.1^{+1.3}_{-0.9}$

Notes. The first column reports the mass component. The second column contains the parameters of the density profile used to describe the corresponding mass component. The third column shows the prior distributions adopted. When a flat prior on a free parameter value is considered, the boundaries of the prior separated by the ÷ symbol are reported. In case of a Gaussian prior, the notation a ± b is adopted, with a as the mean and b as the standard deviation of the distribution, respectively. The x and y coordinates are measured with respect to the position of the BCG (RA = 328. ° 403 408, Dec = 17. ° 695 475). In the last column, we quote the median value and the 16th and 84th percentiles of the marginalised posterior distribution.

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