Table 5: The allowed range of stellar M/L ratios among the blue LSBGs in our sample for which the Z01 and PÉGASE.2 models are able to provide adequate fits at levels of $1\sigma$ and $2\sigma$ , respectively. Only the results from model sequences assuming a Salpeter IMF with $M_{\rm up}=120~M_\odot$ have been used. Here, the BVRI filters are in the Cousins system and $\it JHK$ in the Johnson system, while i is in the Thuan-Gunn system. To obtain values of M/L consistent with the IMF of Kroupa (2001), these values should be multiplied by a factor of $\approx$ 0.6, as discussed in Sect. 4.3.
Model Confidence M/L_B M/L_V M/L_R M/L_i M/L_I M/L_J M/L_H M/L_K

Z01 $1\sigma$ 0.6-2.5 0.8-3.1 0.9-2.9 0.9-2.7 0.9-2.9 0.8-2.4 0.7-2.2 0.7-2.0

$2\sigma$ 0.6-3.0 0.8-3.5 0.9-3.3 0.9-3.1 0.9-3.2 0.8-2.6 0.7-2.4 0.7-2.2

PÉGASE.2 $1\sigma$ 0.4-1.7 0.5-2.0 0.6-1.9 0.6-2.0 0.7-2.1 0.5-1.5 0.4-1.4 0.4-1.3

$2\sigma$ 0.4-2.1 0.5-2.4 0.6-2.3 0.6-2.3 0.7-2.4 0.5-1.7 0.4-1.6 0.4-1.4

**Table 5:** The allowed range of stellar M/L ratios among the blue LSBGs in our sample for which the Z01 and PÉGASE.2 models are able to provide adequate fits at levels of $1\sigma$ and $2\sigma$ , respectively. Only the results from model sequences assuming a Salpeter IMF with $M_{\rm up}=120~M_\odot$ have been used. Here, the *BVRI* filters are in the Cousins system and $\it JHK$ in the Johnson system, while i is in the Thuan-Gunn system. To obtain values of M/L consistent with the IMF of Kroupa (2001), these values should be multiplied by a factor of $\approx$ 0.6, as discussed in Sect. 4.3.
Model	Confidence	M/L_B	M/L_V	M/L_R	M/L_i	M/L_I	M/L_J	M/L_H	M/L_K
Z01	$1\sigma$	0.6-2.5	0.8-3.1	0.9-2.9	0.9-2.7	0.9-2.9	0.8-2.4	0.7-2.2	0.7-2.0
	$2\sigma$	0.6-3.0	0.8-3.5	0.9-3.3	0.9-3.1	0.9-3.2	0.8-2.6	0.7-2.4	0.7-2.2
PÉGASE.2	$1\sigma$	0.4-1.7	0.5-2.0	0.6-1.9	0.6-2.0	0.7-2.1	0.5-1.5	0.4-1.4	0.4-1.3
	$2\sigma$	0.4-2.1	0.5-2.4	0.6-2.3	0.6-2.3	0.7-2.4	0.5-1.7	0.4-1.6	0.4-1.4

Source LaTeX | All tables | In the text

	1 Introduction
	2 The data
	3 Spectral evolutionary modelling
	4 Results
	5 Discussion
	6 Summary
	References