SEDs name convention

SEDs at moderately high spectral resolution are computed for all the SSPs described in this Table. The spectra are named according to the following notation:

Spectral Range

 IMF type IMF slope value [M/H] value
(“p” for “+”, “m” for “-“)		 Age (Gyr)

E [E-MILES, 0.168-5.0 μm]

M [MILES, 3540-7410 Å]

B [V99_Blue, 3855-4476 Å]

R [V99_Red, 4795-5465 Å]

 C [CaT, 8349-8952 Å ]

un
bi
ku
kb

ch

0.3
0.5
0.8
1.3
1.5
1.8
2.0
2.3
2.5
2.8
3.0
3.3
3.5

-2.32 (Padova+00)

-1.71 (Padova+00)
-1.31 (Padova+00)
-0.71 (Padova+00)
-0.40 (Padova+00)
 +0.00 (Padova+00)
 +0.22 (Padova+00)
-2.27 (BaSTI)
-1.79 (BaSTI)
-1.49 (BaSTI)
-1.26 (BaSTI)
-0.96 (BaSTI)
-0.66 (BaSTI)
-0.35 (BaSTI)
-0.25 (BaSTI)
 +0.06 (BaSTI)
 +0.15 (BaSTI)
 +0.26 (BaSTI)
 +0.40 (BaSTI)

[0.0631-17.7828] (Padova+00)
[0.03,14.0] (BaSTI)

where:
Z refers to [M/H], T to age, iP and iT refer to the isochrones Padova+00 or BaSTI respectively. The isochrones can also have +0.00 or +0.40 values depending on the alpha-enhancement of the isochrone used to generate the model. Finally, the alpha-enhancement of the model is in the last part of the name: baseFe (for canonical base models), p0.00, p0.40. The first letter identifies the different set of models (wavelength ranges): B,R,C,M,E refer to the spectral ranges [3855.50-4476.44Å], [4794.95-5465.09Å], [8348.85-8951.50Å], [3540.5-7409.6Å], [1680Å-5.0µm] respectively.

For example, the following file

Mkb1.30Zp0.06T13.0000_iTp0.00_Ep0.00

corresponds to the spectral range [3540.5-7409.6Å] for a SSP computed with Kroupa revised IMF of slope 1.3, +0.06 metallicity, 13.0 Gyr, BaSTI isochrone, and scaled-solar abundance.

Please note that the relation between the total metallicity and iron metallicity is

[Fe/H]=[M/H]-0.75[Mg/Fe]

Thus when selecting a scaled-solar model with total metallicity [M/H] then [Fe/H]=[M/H], whereas for the alpha-enhanced models with the same metallicity [Fe/H]=[M/H]-0.3. Finally for the "base" models it is assumed that [Fe/H]=[M/H], although this is only true at high metallicities. For low metallicities the input stars are alpha-enhanced and therefore when selecting a model with total metallicity [M/H] its [Fe/H] is lower. To summarize the base models follow the abundance pattern of The Galaxy. Note that these models are inconsistent at low metallicities because the adopted isochrones are always scaled-solar.

As an example, if only models with total metallicity [M/H]=+0.06, 10 Gyr and bimodal IMF shape with slope 1.30 are requested , then the following set of models computed with BaSTI isochrones can  be downloaded:

*Mbi1.30Zp0.06T10.0000_iTp0.00_Ep0.00 scaled-solar abundance ratio ([M/H]=[Fe/H]=+0.06)

*Mbi1.30Zp0.06T10.0000_iTp0.40_Ep0.40 alpha-enhanced abundance ratio ([M/H]=+0.06; [Fe/H]=-0.24)

*Mbi1.30Zp0.06T10.0000_iTp0.00_baseFe base models where no consideration about the abundance ratio is being made. The stars feeding the models are picked on the basis of their [Fe/H] metallicity, and therefore these models follow the abundance pattern of The Galaxy.

as well as base models computed with the Padova00 isochrones with nearly similar metallicity:

*Mbi1.30Zp0.00T10.0000_iPp0.00_baseFe