**Table 2:** Photometric systems for which our new isochrones are made available (updated to November 2007).
Photometric system	Filter names	Central	Kind of	References	Additional information
		wavelength range	zero-points	for filters
Johnson	UBV	3642-5502 Å	Vega^a	Maíz-Apellániz (2006)	supersedes Girardi et al. (2002)
Bessell & Brett	$U_{\rm X}B_{\rm X}BV(RI)_{\rm C}$	3627 Å-4.72 $\mu$ m	Vega	Bessell (1990)
	JHKLL'M			Bessell & Brett (1988)
UBVRIJHK^b	$UBV(RI)_{\rm C}JHK$	3642 Å-2.15 $\mu$ m	Vega	Maíz-Apellániz (2006)	^a
				Bessell & Brett (1988), Bessell (1990)
Strömgren-Crawford	uvby	3474-5479 Å	Vega^a	Maíz-Apellániz (2006)
	H $\beta_{\rm w}$ H $\beta_{\rm n}$			Moro & Munari (2000)	^f
Tycho	$V_{\rm T}B_{\rm T}$	4250-5303 Å	Vega^a	Maíz-Apellániz (2006)
SDSS	ugriz	3587-8934 Å	AB^c	Fukugita et al. (1996)	details in Girardi et al. (2004)
OGLE-II	UBVI	3695-8321 Å	Vega	OGLE website	details in Vanhollebeke et al. (2007)
ESO/WFI	wide filters	3469-8590 Å	Vega	ESO/WFI website	supersedes Girardi et al. (2002)
Washington	CMT₁T₂	3982-8078 Å	Vega	Geisler (1996)	details in Girardi et al. (2002)
DENIS	$IJK_{\rm s}$	7927 Å-2.15 $\mu$ m	Vega	Fouqué et al. (2000)	details in Cioni et al. (2006)
2MASS	$JHK_{\rm s}$	1.23-2.16 $\mu$ m	Vega^e	Cohen et al. (2003)	supersedes Bonatto et al. (2004)
UKIDSS	$ZYJHK_{\rm s}$	8823 Å-2.20 $\mu$ m	Vega	Hewett et al. (2006)	supersedes files distributed since 2006
BATC	all 15 filters	3383-9722 Å	AB	Yan et al. (2000)	supersedes files distributed since 2006
HST/WFPC2	all wide filters	1700-9092 Å	Vega+ST+AB	Holtzman et al. (1995)	details in Girardi et al. (2007)
HST/ACS	all WFC+HRC	2645-9130 Å	Vega	Sirianni et al. (2005)	details in Girardi et al. (2007)
HST/NICMOS	JHK-equivalent	1.11-2.04 $\mu$ m	Vega+ST+AB	D. Figer, priv. comm.	details in Girardi et al. (2002)
Spitzer	all MIPS+IRAC	3.52-154 $\mu$ m	Vega,AB^d	Spitzer website	details in Groenewegen (2006)
AKARI	all filters	2.32-160 $\mu$ m	Vega,AB^d	AKARI website	details in Groenewegen (2006)

^a Zero-points are also taken from Maíz-Apellániz (2006).
^b Combines UBV from Maíz-Apellániz (2006) with $(RI)_{\rm C}JHK$ from Bessell & Brett (1988) and Bessell (1990). This combination is provided as being the most useful for the analysis of ground-based data. Supersedes Girardi et al. (2002).
^c We adopt the traditional definition of magnitudes, using Pogson's rather than Lupton et al.'s (1999) formula; see Girardi et al. (2004) for the motivations of this choice.
^d A Vegamag zero-point reproduces the photometry quite accurately for most IR systems (see Reach et al. 2005). AB magnitudes, however, may be convenient because then the magnitudes can be easily converted to the flux in milli-Jansky by means of a single formula, i.e. $f_\nu~{\rm (mJy)} = -0.4~m_{\rm AB}~{\rm (mag)} - 6.56$ .
^e We use zero-points determined by Maíz Apellániz (2007) using Bohlin's (2007) Vega spectrum. As a consequence, the 2MASS zero-point offsets measured by Cohen et al. (2003) do not apply.
^f For the H $\beta$ filters, we simply assume $\beta={\rm H}\beta_{\rm wide}-{\rm H}\beta_{\rm narrow}=2.873$ for Vega (cf. Hauck & Mermilliod 1998). The zero-point is arbitrarily set as ${\rm H}\beta_{\rm wide}{\rm (Vega)}=0$ .

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