Table 3: The grid of PÉGASE.2 evolutionary sequences. All sequences assume the IMF slope, $\alpha$ , to be valid throughout the stellar mass range 0.08-120 $M_\odot$ . The grid consists of all possible combinations of the parameter values listed below. The abbreviations used are described in Table 2.
IMF, $\alpha$ 1.85, 2.35, 2.85

SFH c10⁸, e $5\times10^8$ , e $1\times10^9$ , e $3\times10^9$ , e $6\times10^9$

e $15\times10^9$ , c $15\times10^9$ , e $-15\times10^9$ , e $-2\times10^9$

Metallicity, Z 0.001, 0.004

**Table 3:** The grid of PÉGASE.2 evolutionary sequences. All sequences assume the IMF slope, $\alpha$ , to be valid throughout the stellar mass range 0.08-120 $M_\odot$ . The grid consists of all possible combinations of the parameter values listed below. The abbreviations used are described in Table 2.
IMF, $\alpha$	1.85, 2.35, 2.85
SFH	c10⁸, e $5\times10^8$ , e $1\times10^9$ , e $3\times10^9$ , e $6\times10^9$
	e $15\times10^9$ , c $15\times10^9$ , e $-15\times10^9$ , e $-2\times10^9$
Metallicity, Z	0.001, 0.004

Source LaTeX | All tables | In the text

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