SED@ History

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SED@
Evolutionary Synthesis Models

History

The origins: Form UV to Radio

These models where performed originally by José Miguel Mas-Hesse and Phillipe Arnault under supervision of Daniel Kunth in their respective Ph.D. in 1991 (defended in Madrid and Paris).
- The first version of the code computed the continua and related parameters from UV to radio ranges for two different metallicities (Maeder and Meynet 1987, 1989). This work is the basis of the posterior versions (updates and some extensions). The description of the models and some of the results can be found in:
- A second version (unpublished) was performed by Miguel Cerviño (under the supervision of J.M. Mas-Hesse). It included four sets of metallicities (Maeder 1990) with a synthetic stellar track of the star with the lower WR mas limit (following the evolution from the stellar wind mass lost channel) and another one with a lower mass (M(WR lim) - 0.1 Mo) for each metallicity. This method overrides spurious effects at the end of WR phases.
  We updated this version with five set of metallicity tracks (Schaller et al. 1992 and posterior grids). The results was showed in:
  - Cerviño & Mas-Hesse 1994, A&A, 284, 749
Extensions: High energy and new inputs
- The third version of the code, we included binary evolution and the X-ray emission from star forming regions. This work was part of the Ph.D. project of M.Cerviño supervised by J.M. Mas-Hesse. The code has been presented in:
  - Cerviño, Mas-Hesse and Kunth, 2002, A&A, 392, 19 Showing only the X-ray emission without binaries but including dispersion, see below
  and applied to a set of star forming galaxies and circumnuclear regions in AGNs in:
  - Mas-Hesse and Kunth, 1999, A&A, 349, 765
  - Jiménez-Bailón et al. 2003, ApJ (accepted astro-ph/0304465)
- The fourth version of the code includes several changes:
  - atmosphere models of different metallicities, WR atmosphere models and CoStar models (thanks to Daniel Schaerer and David Valls-Gabaud ;).
  - complete set of Geneva tracks
  - chemical yields (including radioactive isotopes like ²⁶Al, ⁶⁰Fe which are gamma ray emitters).
  This version was performed during a Post-doc of Miguel Cervño in the Toulose. The results from ²⁶Al and ⁶⁰Fe gamma-ray lines for solar metallicity are accessible here and presented in Cerviño et al. 2000 A&A 363, 970
Confidence levels

We had updated (again) the code to include an estimation of the dispersion and confidence levels of the different observables. That are the results you can find here. The theory and background has been establish in the following series of papers. But we want to stress that more revisions to synthesis models must be done. See On some Uncertainties in Evolutionary Synthesis Models, Cerviño & Valls-Gabaud ASP Conference Proceedings, Vol. 274, 560 (ps.gz file, 58Kb) for an overview

More info in:
1. Confidence levels of evolutionary synthesis models: Qualitative analysis of the dispersion of Synthesis models due to IMF fluctuations.
  Full paper
  Reference: Cerviño, M., Luridiana, V. & Castander, F.J., 2000, A&Aletters, 360, L5
2. Confidence levels of evolutionary synthesis models II. On sampling and Poissonian fluctuations: Quantitative analysis and complete theoretical background valid to any synthesis model (output results here :)
  Full paper
  Reference: Cerviño, M., Valls-Gabaud, D., Luridiana, V. & Mas-Hesse, J.M., 2002, A&A 381, 51
3. Confidence levels of evolutionary synthesis models III. On time-integrated quantities: Study of the problems related with the time-step and time interpolation in isochrones. Click here to access to the output tables and parabolic subroutine.
  Full paper
  Reference: Cerviño, M., Gómez-Flechoso, M.A., Castander, F.J., Schaerer, D., Mollá, M., Knödlseder, J. & Luridiana, V. 2001, A&A 376, 422.
4. On the effect of discrete numbers of stars in chemical evolution models: Effects of the IMF sampling in chemical Evolution models
  Full paper
  Reference: Cerviño, M. & Mollá, M. 2002, A&A 394, 525.
5. On biases in the predictions of stellar population synthesis models: When the results of synthesis models are biased and not longer apply.
  Full paper
  Reference: Cerviño, M. & Valls-Gabaud, D. 2003, M.N.R.A.S. 338, 481.
6. On the limits of synthesis models to obtain the properties of stellar clusters: The Lowest Luminosity Limit: Absolute limits for the use of synthesis models in the standard way.
  Full paper
  Reference: Cerviño, M. & Luridiana, V. (submitted to A&A; astro-ph/0304061; see also astro-ph/0302577
7. On emission-line spectra obtained from evolutionary synthesis models I. Dispersion in the ionizing flux and Lowest Luminosity Limits: First step for the study of the sampling problem to the emission-line diagnostic diagrams. Go to Database to access to the output tables.
  Full paper
  Reference: Cerviño, M., Luridiana, V., Pérez, E., Vílchez, J.M. & Valls-Gabaud, D. (accepted in A&A; astro-ph/0304062)
Public Release:

Currently, we are working on an update of the code, that will we written in ANSI-C and will be available to the community (together with complete manuals) during 2003 (tentative date).

Finally, We want thanks to Jesús Maíz-Apellaníz their continuously helps to improve this models.

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Justicia, no venganza

Justice, not revenge
We thanks to the LAEFF for the space for host this server

Miguel Cerviño 2003