Photometric Predictions
Here we provide links to different photometric predictions generated by the Vazdekis et al. (2010) code based on both photometric stellar libraries and SEDs. The following predictions are provided for SSPs covering a large range of ages, metallicities and IMF types and slopes:
- Colours
- Magnitudes
- Mass-to-light ratios
- Masses
- Surface Brightness Fluctuations (SBFs) and their corresponding colour fluctuations
The following filter systems are used for the photometric predictions described above:
- U,B,V,J,H,K (Johnson)
- R,I (Cousin)
- F439W,F555W,F675W,F814W (WFPC2-HST)
The appropriate references for these predictions are Vazdekis et al. 1996 and Blakeslee, Vazdekis & Ajhar (2001) (for the SBF and WFPC2 HST filter system predictions). We have adopted the Vega system for the Johnson-Cousins filters, assuming Vega magnitudes: U=V=B=R=0.03 mag; I=0.07 mag.
Magnitudes, colours and mass-to-light ratios
Magnitudes, colours and mass-to-light ratios are provided for the SSPs specified in the table below. For computing the mass-to-light ratios we take into account the remnants and the mass loss during the latest phases of the stellar evolution. It is also important to note that the adopted lower and upper mass cutoffs for all the IMFs are 0.1 and 100 Mo respectively (see Notes), and the faintest star is 0.1 Mo. These model predictions can be obtained from the following files:
Isochrone |
[α/Fe] |
Unimodal |
Bimodal |
Kroupa Universal |
Kroupa Revised |
Chabrier |
Padova+00 |
baseFe |
|||||
BaSTI |
baseFe |
Each file contain the following columns: (1)IMF type, (2)IMF slope, (3)[M/H], (4)Age, (5)U, (6)B, (7)V, (8)R, (9)I, (10)J, (11)H, (12)K, (13)U-V, (14)B-V, (15)V-R, (16)V-I, (17)V-J, (18)V-H, (19)V-K, (20)(M/L)U, (21)M/L)B, (22)(M/L)V, (23)(M/L)R, (24)(M/L)I, (25)(M/L)J, (26)(M/L)H, (27)(M/L)K, (28)F439W, (29)F555W, (30)F675W, (31)F814W, (32)F439W-F555W, (33)F555W-F675W, (34)F555W-F814W.
HEADER_ssp_phot includes the appropriate header for these files.
Surface brightness fluctuations
Surface brightness fluctuations model predictions for ages larger than 4 Gyr (for younger ages the predictions are uncertain due to the large contribution of the AGB evolutionary phase) can be obtained from the following files:
Isochrone |
[α/Fe] |
Unimodal |
Bimodal |
Kroupa Universal |
Kroupa Revised |
Chabrier |
Padova+00 |
baseFe |
|||||
BaSTI |
baseFe |
Each file contains the following columns: (1)IMF type, (2)IMF slope, (3)[M/H], (4)Age, (5)Ubar, (6)Bbar, (7)Vbar, (8)Rbar, (9)Ibar, (10)Jbar, (11)Hbar, (12)Kbar, (13)U-Vbar, (14)B-Vbar, (15)V-Rbar, (16)V-Ibar, (17)V-Jbar, (18)V-Hbar, (19)V-Kbar, (20)F439Wbar, (21)F555Wbar, (22)F675Wbar, (23)F814Wbar, (24)F439W-F555Wbar, (25)F555W-F675Wbar, (26)F555W-F814Wbar
HEADER_ssp_sbf includes the appropriate header for these files.
Please note that predictions for Ages below 4 Gyr are rather uncertain
Masses
Masses relative to models of different stellar population parameters are provided in the table below. Note that the normalization is set to 1 Msun. These model predictions can be obtained from the following files:
Isochrone |
[α/Fe] |
Unimodal |
Bimodal |
Kroupa Universal |
Kroupa Revised |
Chabrier |
Padova+00 |
baseFe |
|||||
BaSTI |
baseFe |
|||||
BaSTI |
+0.00 |
|||||
BaSTI |
+0.40 |
Each file contain the following columns: (1)IMF type, (2)IMF slope, (3)[M/H], (4)Age, (5)Mtotal, (6)M(*+remn), (7)M*, (8)Mremn, (9)Mgas, (10)M(*+remn)/Lv, (11)M*/Lv, (12) Mv.
HEADER_ssp_mass includes the appropriate header for these files.