**Table 2:** The grid of Z01 evolutionary sequences. All sequences assume $Z_{{\rm gas}}=Z_{{\rm stars}}$ , a gas covering factor of 1.0, a hydrogen number density of 100 cm^-3 and 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. In addition to these, 108 sequences with $M_{{\rm up}}=40~M_\odot$ were generated for test purposes with variations in IMF slope, metallicity, star formation history and redshift, but with fixed $M_{{\rm tot}}=10^9~M_\odot$ and filling factor 0.01.
$M_{\rm tot}$ ( $M_\odot$ )	10⁹, 10¹⁰
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
Filling factor	0.01, 0.1
Redshift, z	0.00, 0.01

IMF: ${\rm d}N/{\rm d}m \propto m^{-\alpha}$ .
SFH = Star formation history.
c = Constant star formation rate during the subsequent number of years.
e = Exponentially declining/increasing star formation rate with $\tau$ equal
to the subsequent number of years.

Source LaTeX | All tables | In the text

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