\begin{table}%t1
\caption{Photometric systems for which our new isochrones are made
available (updated to November 2007).}
\label{tab_photsys}
\small%\centerline
 {
\begin{tabular}{llllll}
\hline \hline
Photometric system & Filter names & Central & Kind of &
References & Additional information \\
 & & wavelength range & zero-points & for filters & \\
\hline
%&&&&& \\[-8pt]
Johnson  & $UBV$ & 3642--5502 \AA  & Vega$^{a}$ & Ma\'{\i}z-Apell\'aniz (\cite{Maza06}) & supersedes Girardi et~al. (\cite{Gira02}) \\
Bessell \& Brett & $U_{\rm X}B_{\rm X}BV(RI)_{\rm C}$ & 3627 \AA--4.72~$\mu$m & Vega & Bessell (\cite{Bess90}) & \\
               & $JHKLL'M$ &                        &  & Bessell \& Brett (\cite{Bess88}) & \\
$UBVRIJHK$$^{b}$ & $UBV(RI)_{\rm C}JHK$ & 3642 \AA--2.15~$\mu$m & Vega & Ma\'{\i}z-Apell\'aniz (\cite{Maza06}) & $^{a}$ \\
           &            &                         &      & Bessell \& Brett (\cite{Bess88}), Bessell (\cite{Bess90}) &  \\
Str\"omgren-Crawford & $uvby$ & 3474--5479 \AA & Vega$^{a}$ & Ma\'{\i}z-Apell\'aniz (\cite{Maza06}) & \\
                     & H$\beta_{\rm w}$H$\beta_{\rm n}$ &                  &      & Moro \& Munari (\cite{Moro00}) & $^{f}$ \\
Tycho & $V_{\rm T}B_{\rm T}$ & 4250--5303 \AA & Vega$^{a}$ & Ma\'{\i}z-Apell\'aniz (\cite{Maza06}) & \\
SDSS & $ugriz$ & 3587--8934 \AA & AB$^{c}$ & Fukugita et~al. (\cite{Fuku96}) & details in Girardi et~al. (\cite{Gira04}) \\
OGLE-II & $UBVI$ & 3695--8321 \AA & Vega & OGLE website & details in Vanhollebeke et~al. (\cite{Vanho07}) \\
ESO/WFI & wide filters & 3469--8590 \AA & Vega & ESO/WFI website & supersedes Girardi et~al. (\cite{Gira02}) \\
Washington & $CMT_1T_2$ & 3982--8078 \AA & Vega & Geisler (\cite{Geis96}) & details in Girardi et~al. (\cite{Gira02}) \\
DENIS & $IJK_{\rm s}$ & 7927 \AA--2.15~$\mu$m & Vega & Fouqu\'e et~al. (\cite{Fouq00}) & details in Cioni et~al. (\cite{Cion06}) \\
2MASS & $JHK_{\rm s}$ & 1.23--2.16~$\mu$m & Vega$^{e}$ & Cohen et~al. (\cite{Cohe03}) & supersedes Bonatto et~al. (\cite{Bona04}) \\
UKIDSS & $ZYJHK_{\rm s}$ & 8823 \AA--2.20~$\mu$m & Vega & Hewett et~al. (\cite{Hewe06}) & supersedes files distributed since 2006 \\
BATC & all 15 filters & 3383--9722 \AA & AB & Yan et~al. (\cite{Yan00}) & supersedes files distributed since 2006 \\
HST/WFPC2 & all wide filters & 1700--9092 \AA & Vega+ST+AB & Holtzman et~al. (\cite{Holtz95}) & details in Girardi et~al. (2007) \\
HST/ACS & all WFC+HRC & 2645--9130 \AA & Vega & Sirianni et~al. (\cite{Siria05}) & 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. (\cite{Gira02}) \\
Spitzer & all MIPS+IRAC & 3.52--154~$\mu$m & Vega,AB$^{d}$ & Spitzer website & details in Groenewegen (\cite{Groene06}) \\
AKARI & all filters &  2.32--160~$\mu$m & Vega,AB$^{d}$ & AKARI website & details in Groenewegen (\cite{Groene06}) \\
\hline
\end{tabular}}
\medskip
$^{a}$ Zero-points are also taken from Ma\'{\i}z-Apell\'aniz (\cite{Maza06}). \\ 
$^{b}$ Combines $UBV$ from Ma\'{\i}z-Apell\'aniz (\cite{Maza06}) with $(RI)_{\rm C}JHK$ from Bessell \& Brett (\cite{Bess88}) and Bessell (\cite{Bess90}). This combination is provided as being the most useful for the analysis of ground-based data.  Supersedes Girardi et~al. (\cite{Gira02}). \\
$^{c}$ We adopt the traditional definition of magnitudes, using Pogson's
rather than Lupton et~al.'s (\cite{Lupt99}) formula; see Girardi et~al. (\cite{Gira04})
for the motivations of this choice. \\ 
$^{d}$ A Vegamag zero-point reproduces the photometry quite accurately for most IR systems (see
Reach et~al. \cite{Reac05}). $AB$ 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 Ma{\'{\i}}z Apell{\'a}niz (2007) using Bohlin's (\cite{Bohl07}) Vega spectrum. As a consequence, the 2MASS zero-point offsets measured
by Cohen et~al. (\cite{Cohe03}) 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 \cite{Hauc98}). The
zero-point is arbitrarily set as ${\rm H}\beta_{\rm wide}{\rm
(Vega)}=0$.
\end{table}