Single-Stellar Population models SEDs
We have released the SSP model spectra based on the updated stellar populations synthesis code described Vazdekis et al. (2003, 2010, 2015, 2016). Model predictions at moderately high resolution are provided for the following spectral ranges:
|
Models |
Wavelength range | Instrumental Resolution (FWHM) |
Instrumental Resolution (σ) |
Dispersion (Å/px) |
|---|---|---|---|---|
| V99 Blue/Red | 3855-4476 Å, 4795-5465 Å | 1.8Å | 55.0, 44.7 km/s | 0.62 |
| CaT | 8349-8952 Å | 1.5Å | 22.1 km/s | 0.85 |
| MILES | 3540-7410 Å | 2.51Å | 58.4 km/s | 0.90 |
| E-MILES | 0.168-5.0 µm | 2.51 - 23.57Å | 36 - 228 km/s | 0.90 |
We provide the user for appropriate tools to facilitate the retrieval, handling and transformation of the SSP spectra here
Tarfiles with complete model predictions, at their nominal resolution, are available at the individual webpages of the models
These SEDs can be used to analyze galaxy spectra in a very easy and flexible way, allowing us to adapt these models to the characteristics of the data instead of proceeding in the opposite direction as, for example, we must do when working on the Lick/IDS instrumental dependent system. The SSP spectra, with flux-calibrated response, can be smoothed to match the resolution of the data and galaxy internal velocity dispersion, allowing us to analyze the observed spectrum in its own system. Therefore the entire observational spectrum can be compared at one time, or the analysis can be done by means of a particular set of features, which should be measured on both, the galaxy spectrum and the SSP SEDs.