# Table 4 - Fitting parameters for Galaxy theoretical and empirical AMR.^(a)
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#                                    Yield metallicity
# Source                              zeta  [Fe/H]_10
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This work^(b)                         0.23    +0.17 +/- 0.04
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                                         Models
Source                                zeta  [Fe/H]_10
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Matteucci & Fracois (1989)            0.84    +0.11
Wyse & Silk (1989) (n=1)              0.79    -0.07
Wyse & Silk (1989) (n=2)              0.49    -0.04
Carigi (1994)                         1.14    +0.08
Pardi & Ferrini (1994)                1.04    +0.00
Prantzos & Aubert (1995)              0.76    +0.00
Timmes, Woosley & Weaver (1995)       0.42    +0.02
Giovagnoli & Tosi (1995)              1.06    +0.09
Pilyugin & Edmunds (1996)             0.81    -0.06
Mihara & Takahara (1996)              1.28    -0.00
Chiappini, Matteucci & Gratton (1997) 0.71    -0.00
Portinari, Chiosi & Bressan (1998)    0.73    -0.13
Boissier & Pranztos (1999)            0.82    +0.02
Alibes, Labay & Canal (2001)          0.73    -0.03
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                                          Observations
Milky Way 13 Gyr old
                                      zeta           [Fe/H]_10
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Twarog (1980)                         0.63 +/- 0.04   -0.01 +/- 0.03
Carlberg et al. (1985)                0.56 +/- 0.08   +0.02 +/- 0.07
Meusinger, Stecklum & Reimann (1991)  0.54 +/- 0.06   +0.02 +/- 0.05
Edvardsson et al. (1993)              0.62 +/- 0.12   -0.10 +/- 0.11
Rocha-Pinto et al. (2000)             0.88 +/- 0.04   -0.05 +/- 0.04
Holmberg, Nordstrom & Andersen (2007) 0.30 +/- 0.01   -0.12 +/- 0.01
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Mean of all surveys                   0.59 +/- 0.08   -0.04 +/- 0.03
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^(a) Assuming [Fe/H] = zeta log(t9) + omega, with t9 in Gyr. 
By definition, [Fe/H]_10 = zeta+ omega  is the expected metallicity at t = 10Gyr.
^(b) From eq. (25), for R=3. [Fe/H]_10 range limits from varying galaxy 
birthrate b = 0.5 +/- 0.5.