Modelling the photometric and morphological evolution of disc galaxies in the cluster environment

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Table B.1.

Model parameters using the MS of Speagle et al. (2014).

Param.	Ref.	Prior	Fiducial	Best-fit
(1)	(2)	(3)	(4)	(5)
Cluster-driven quenching (RPS)

${log}_{10} (τ_{s} / Gyr)$ $Mathematical equation: $ \log_{10}(\tau_{\mathrm{s}}/\rm Gyr) $$	Eq. (3)	[-1.3,1.3]	$- 0 . 33_{- 0.26}^{+ 0.18}$ $Mathematical equation: $ -0.33^{+0.18}_{-0.26} $$	−0.24
α_s	Eq. (3)	[-2.0,2.0]	$- 0 . 95_{- 0.61}^{+ 0.45}$ $Mathematical equation: $ -0.95^{+0.45}_{-0.61} $$	−0.83

Cluster-driven morphological evolution

${log}_{10} (τ_{m} / Gyr)$ $Mathematical equation: $ \log_{10}(\tau_{\mathrm{m}}/\rm Gyr) $$	Eq. (5)	[-1.3,1.3]	$0 . 47_{- 0.33}^{+ 0.21}$ $Mathematical equation: $ 0.47^{+0.21}_{-0.33} $$	0.66
α_m	Eq. (5)	[-2.0,2.0]	$- 0 . 23_{- 0.47}^{+ 0.37}$ $Mathematical equation: $ -0.23^{+0.37}_{-0.47} $$	−0.20
p_max	Eq. (4)	[0.0,1.0]	$0 . 79_{- 0.11}^{+ 0.13}$ $Mathematical equation: $ 0.79^{+0.13}_{-0.11} $$	0.93

Notes. (1)–parameter, (2)–reference Equation in the text, (3)–prior range, assuming uniform distributions, (4)–fiducial values from the 16th, 50th, and 84th percentiles of the marginalised posterior distribution, (5)–values that maximise the likelihood.

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