SSPs:
line-strengths, magnitudes, colours,
mass-to-light ratios, SBFs
Absorption
line-strengths computed on the basis of empirical fitting functions:
Line-strengths are computed
for all the SSPs described in this Table. However the age ranges (in Gyr) where these
predictions are safe (since do not require many extrapolations of the empirical
fitting functions employed by the models) are listed below:
|
|
[M/H] = -2.32 | [M/H] = -1.71 |
[M/H]
= -1.31 |
[M/H]
= -0.71 |
[M/H]
= -0.40 |
[M/H]
= 0.0 |
[M/H]
= +0.22 |
|
SAFE Lick/IDS line-strength predictions |
[0.7-18] |
[0.2-18] |
[0.1-18] |
[0.1-18] |
[0.1-18] |
The full set of predictions
for each IMF type can be obtained from the following files:
|
|
IMF
slope |
Unimodal |
Bimodal |
Kroupa
Universal |
Kroupa
Revised |
|
SAFE |
1.3 |
||||
|
ALL |
|
The first column of these
files contain two letters identifying the IMF type: UN (unimodal), BI
(bimodal), KU (Kroupa Universal) and KB (Kroupa Revised). The
second column indicates the IMF slope (does not apply for the models calculated
with Kroupa IMFs). The third column indicates the age (in Gyr). The information
per column is the following: (1)IMF type, (2)IMF slope, (3)[M/H], (4)Age,
(5)CN1, (6)CN2, (7)Ca4227, (8)G-band, (9)Fe4383, (10)Ca4455, (11)Fe4531,
(12)Fe4668, (13)Hβ, (14)Fe5015, (15)Mg1, (16)Mg2, (17)Mgb, (18)Fe5270,
(19)Fe5335, (20)Fe5406, (21)Fe5709, (22)Fe5782, (23)NaD, (24)TiO1,
(25)TiO2, (26)HδA, (27)HγA, (28)HδF, (29)HγF, (30)D4000,
(31)CaT*, (32)PaT,(33)CaT
HEADER_ssp_li includes the appropriate header for
these files.
Magnitudes, colours and
mass-to-light ratios:
Magnitudes, colours and
mass-to-light ratios are provided for the SSPs specified in this Table. 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:
|
Age
range |
IMF
slope |
Unimodal |
Bimodal |
Kroupa
Universal |
Kroupa
Revised |
|
[0.063,17.8] |
1.3 |
||||
|
[0.063,17.8] |
[0.3-3.3] |
|
|
Each file contain the
following columns: (1)IMF type, (2)IMF slope,
(3)[Fe/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:
|
Age
range |
IMF
slope |
Unimodal |
Bimodal |
Kroupa
Universal |
Kroupa
Revised |
|
[4.0,17.8] |
1.3 |
||||
|
[4.0,17.8] |
[0.3,3.3] |
|
|
Each file contains the following columns: (1)IMF type, (2)IMF slope, (3)[Fe/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.
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