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Table 2:

Parameters from the literature.

Cluster 		Metallicity Error Age (Gyr) Error Method   Reference
HW 1 -0.7 -- 4-6 -- RP Dias et al., in prep.
K3, L8, ESO28SC19 -1.5, -0.6, -1.41 -- 3 -- RS, RP Gascoigne (1980)
  -1.01 -- 4 -- RP Gascoigne et al. (1981)
  $\sim$-1.22 -- 5-8 -- RP Rich et al. (1984)
  -1.52 $\pm$0.2 $\geq$10 -- IP #1986A
  -1.261 $\pm$0.10 8-10 -- RP Alcaino et al. (1996)
  -1.121, -0.981 $\pm$0.12, $\pm$0.12  -- -- RS Da Costa & Hatzidimitriou (1998)
  -1.001 $\pm$0.28 3.5 $\pm$1.5 IS de Freitas Pacheco et al. (1998)
  -1.161 $\pm$0.09 4.7, 6.0 $\pm$0.6, $\pm$1.3 RP Mighell et al. (1998)
  -1.201 $\pm$0.2 7.0 $\pm$1 IS Piatti et al. (2005a)
  -- -- 6.5 $\pm$0.5 RP Glatt et al. (2008b)
L3, ESO28SC13 -- -- 1-5 -- RP Kontizas (1980)
  -- -- 0.4 $\pm$0.1 RP Hodge (1983)
  -0.7 -- 1-2 -- RP Dias et al., in prep.
L11, K7, ESO28SC22 -- -- 1-5 -- RP Kontizas (1980)
  -- -- 0.3 $\pm$0.1 RP Hodge (1983)
  -0.932 -- 3.5 1.0 RP Mould et al. (1992)
  -0.801, -0.811 $\pm$0.14, $\pm$0.13 -- -- RS Da Costa & Hatzidimitriou (1998)
  -- -- 3.5 $\pm$0.5 IS Piatti et al. (2005a)
  -0.62, -0.32 -- 5.9, 4.0 $ \rm ^{+1.4}_{-0.8}$, $\rm ^{+0.9}_{-0.6}$ IP Rafelski & Zaritsky (2005)

L113, ESO30SC4

 -1.42 $\pm$0.2 4-5 -- RP Mould et al. (1984)
  -1.441, -1.171 $\pm$0.16, $\pm$0.12 -- -- RS Da Costa & Hatzidimitriou (1998)
  -1.241 $\pm$0.11 4.0, 5.3 $\pm$0.7, $\pm$1.3 RP Mighell et al. (1998)
NGC 121, L10, K2, ESO50SC12 -1.5, -1.1, -1.41 -- 12 -- RS, RP Gascoigne (1980)
  -- -- 13 $\pm$5 RP Hodge (1983)
  -- -- 12, 9 $\pm$2, $\pm$2 RP Stryker et al. (1985)
  -1.32 $\pm$0.2 $\geq$10 -- IP #1986A
  -1.461, -1.191 $\pm$0.10, $\pm$0.12 -- -- RS Da Costa & Hatzidimitriou (1998)
  -1.201 $\pm$0.32 12 $\pm$5 IS de Freitas Pacheco et al. (1998)
  -1.711 $\pm$0.10 10.6, 11.9 $\pm$0.7, $\pm$1.3 RP Mighell et al. (1998)
  -1.031 -- 10.6 $\pm$0.5 RP Dolphin et al. (2001)
  -- -- 12 $\pm$1 IS #2002A
  -- -- 11.8, 11.2, $\pm$0.5, $\pm$0.5, RP Glatt et al. (2008a)
  -- -- 10.5, 10.9, $\pm$0.5, $\pm$0.5, RP Glatt et al. (2008a)
  -- -- 11.5, 10.8 $\pm$0.5, $\pm$1.0, RP Glatt et al. (2008a)
NGC 152, L15, K10, ESO28SC24 -- -- 1-5 -- RP Kontizas (1980)
  -- -- 0.61 $\pm$0.09 RP Hodge (1983)
  -1.252 $\pm$0.25 3.2 $\pm$0.3 IP #1986A
NGC 222, L24, K19, ESO29SC4, SMC0009(OGLE) -0.62 -- 0.10 $\pm$0.01 RP Pietrzynski & Udalski (1999)
  -- -- 0.070 $\pm$0.007 RP #2000A
  -0.62, -0.32 -- 0.092, 0.100 $\rm ^{+0.018} _{-0.004}$, $\rm ^{+0.046} _{-0.002}$ IP Rafelski & Zaritsky (2005)
  -0.32 -- 0.10 $\pm<$0.03 RP Chiosi et al. (2006)
NGC 256, L30, K23 ESO29SC11, SMC0032(OGLE) -0.62 -- 0.10 $\pm$0.01 RP Pietrzynski & Udalski (1999)
  -- -- 0.05 $\pm$0.01 IS #2002A
  -0.32 -- 0.10 $\pm$<0.03 RP Chiosi et al. (2006)
NGC 269, L37, K26, ESO29SC16, SMC0046(OGLE) -- -- 0.6 $\pm$0.2 IS Piatti et al. (2005a)
  -0.32 -- 0.3 $\pm$>0.2 RP Chiosi et al. (2006)
NGC 294, L47, ESO29SC22, SMC0090(OGLE) -0.62 -- 0.32 $\pm$0.3 RP Pietrzynski & Udalski (1999)
  -- -- 0.30 $\pm$0.05 RP #2000A
  -- -- 0.3 $\pm$0.1 IS Piatti et al. (2005a)
  -0.62, -0.32 -- 0.42, 0.32 $\rm ^{+0.04} _{-0.08}$, $\rm ^{+0.03} _{-0.11}$ IP Rafelski & Zaritsky (2005)
  -0.32 -- 0.4 $\pm$<0.2 RP Chiosi et al. (2006)
NGC 361, L67, ESO51SC12 -- -- 4 -- RP Hodge (1981)
  -- -- >0.5 -- RP Hodge (1983)
  -1.252 $\pm$0.2 8 $\pm$1.5 IP #1986A
  -1.451 $\pm$0.11 6.8, 8.1 $\pm$0.5, $\pm$1.2 RP Mighell et al. (1998)
NGC 419, L85, K58, ESO29SC33, SMC0159(OGLE)  -- -- 0.67 $\pm$0.05 RP Hodge (1983)
  -1.22 $\pm$1.2 3.5 $\pm$0.3 IP #1986A
  -0.601 $\pm$0.21 1.2 $\pm$0.5 IS de Freitas Pacheco et al. (1998)
  -0.62 -- >1 -- RP Pietrzynski & Udalski (1999)
  -- -- 1.2 $\pm$0.4 IS Piatti et al. (2005a)
  -0.32 -- 0.4 $\pm$>0.2 RP Chiosi et al. (2006)
  -- -- 1.2-1.6 -- RP Glatt et al. (2008b)
NGC 458, L96, K69, ESO51SC26 -- -- 0.05 $\pm$0.01 RP Hodge (1983)
  -0.23 -- 0.13 $\pm$0.06 IS Piatti et al. (2005a)
  -0.62, -0.32 -- 0.100, 0.100 $\rm ^{+0.002} _{-0.028}$, $\rm ^{+0.018} _{-0.002}$  IP Rafelski & Zaritsky (2005)

Notes. Metallicity values refer to 1: [Fe/H], 2: [M/H] = [Z] = [ $Z/Z_{\odot}$], assuming $Z_{\odot}$ = 0.017. The fields with more than one value refer to distinct criteria adopted by the authors. The methods are indicated by ``RP'' or ``IP'' for resolved or integrated photometry, and ``RS'' or ``IS'' for resolved or integrated spectroscopy.


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