**Table 4:** The physical ingredients adopted in the models plotted in Fig. 6.
Authors	Evolutionary tracks^a		Stellar spectral library		IMF
Kurth et al. (1999)	Padua Lib. 1994 +		Lejeune et al. (1998,1997)		Salpeter (1955)
	Chabrier & Baraffe (1997)
Brocato et al. (2000)	Frascati Lib. 1991-2000		Castelli et al. (1997)		Scalo (1986)
Girardi et al. (2000)	Padua Lib. 1994-2000		Kurucz (1992)		Salpeter (1955)
Zhang et al. (2002)	Pols et al. (1998)		Lejeune et al. (1998,1997)		Kroupa et al. (1993)
Anders & Fritze-v. Alvensleben (2003)	Padua Lib. 1994-2000 +		Lejeune et al. (1998,1997)		Salpeter (1955)
	Chabrier & Baraffe (1997)
Bruzual & Charlot (2003)	Padua Lib. 1994 +		Westera et al. (2002)		Chabrier (2003)
	Baraffe et al. (1998)
Maraston (2005)	Cassisi et al. (2000)		Lejeune et al. (1998)^b		Kroupa (2001)^c
Present work	Pisa Lib. 2004 +		Castelli (1999)		Kroupa (2002)
	Baraffe et al. (1997)
Authors	Normalization	Thermal Pulses	OS^d	$M_{\rm up}$	WD^e	${\cal M}/L$ ^f
Kurth et al. (1999)	-^g	No	$\approx$ 0.2	5	No	No
Brocato et al. (2000)	Number of stars &	Groenewegen &	No	5	Yes	No
	$M_V^{\rm tot}$	de Jong (1993)
Girardi et al. (2000)	$1~M_{\odot}$	Groenewegen &	$\approx$ 0.25	5	Yes	No
		de Jong (1993)
		+ Marigo (1998)
Zhang et al. (2002)	$1~M_{\odot}$	Vassiliadis &	$0.22\div0.4$	5	Yes	No
		Wood (1993)
Anders & Fritze-v. Alvensleben (2003)	Initial cluster mass^h	Groenewegen &	$\approx$ 0.25	-^h	Yes	Yes
		de Jong (1993)
Bruzual & Charlot (2003)	$1~M_{\odot}$	Vassiliadis &	$\approx$ 0.2	5	Yes	Yes
		Wood (1993)ⁱ
Maraston (2005)	$1~M_{\odot}$	Renzini (1992)^i,j	No	8.5	Yes	Yes
Present work	$M_V^{\rm tot}$	Wagenhuber &	No	6.5	Yes	Yes
		Groenewegen (1998)

^a Detailed information on the adopted evolutionary tracks can be found in the paper quoted in Col. 1.
^b The latest version available on the web, see Maraston (2005).
^c Synthetic models are also calculated for the IMF of Salpeter (1955).
^d The quoted values for the overshooting (OS) efficiency, expressed in units of pressure-scale-height above the Schwarzschild convective border, are only indicative because different sets of evolutionary tracks adopt different prescriptions for the overshooting mechanisms and for the minimum mass at which the overshooting is fully efficient (see the related papers for more details);
^e This column indicates if WDs are included in the calculations.
^f This column indicates if mass-to-light ratio values are available.
^g In the paper by Kurth et al. (1999) the normalization procedure is not described.
^h In the paper by Anders & Fritze-v. Alvensleben (2003) the SSPs have been evolved to the selected ages starting with an initial stellar mass of $10^6~M_{\odot}$ ; the adopted value for $M_{\rm up}$ is not specified.
ⁱ Carbon stars are included.
^j See discussion in Maraston (2005).

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