Hello Guest, here there is some information about Sed@
Sed@ and the Violent Star Formation (VSF) Legacy Tool:
Sed@ is one of the programs included in the
VSF Legacy Tool. It is written in ANSI C and their objective is to
compute the composed Spectral Energy Distribution of an ensemble of stars; their associated Spectral Energy Dispersion, with their corresponding sampling distributions; and the Luminosity Function and HR diagrams of resolved stellar systems.
Sed@ is included in the VSF Legacy Tool, as well as other synthesis models and additional tools for the study of extragalactic objects and data-mining of astronomical databases. It is only a small piece in the big puzzle that the VSF Legacy Tool is. However, Sed@ developement is closely related to the VSF Legacy Tool, and the current structure of the code can not be understood without the inputs from the VSF Network, specially: Elena Terlevich, Arurelio López, Roberto Terlevich, Miguel Chávez, Emmanuel Bettone, and the Computer Center at the INAOE, and Rosa González Delgado, Enrique Pérez and Valentina Luridiana at the IAA.
How Sed@ works?:
Sed@ is structured in such a way that read any isocrone table and atmosphere model grid from the literature. Currently the code does not compute isochrones; it makes the isochrone-atmosphere model asignation, integrate it with the Initial Mass Function and Star Formation Rate, and computes the spectral energy distributions and their asociated Probability Density Distributions. The code only assume the responsability to make an integration the more correct as possible, and it is responsability of the users to make the more adecuate choice of isochrones and atmosphere libraries for their specific problem. For this reason, the output of Sed@ contains large headers with the relevant information (and the corresponding references) of the used inputs. Also for this reason any publication that make use of this database must contain the references to the input data that is especified in the header results; in the other hand, there is no reference paper for the code (since Sed@ is an evolving code, any paper would become obsolete when the research in synthesis models will improve) and only a footnote to the reference manual should be needed; additionally, we would acknowledge an acknowledge to the VSF Network.
The current isochrones supported includes the ones from
Geneva, Padova, Pisa and Teramo groups. (An exception are the enchanced Mass lost rates isocrones from Geneva group, since, observationally, the
actual mass lost rate is even lower than the one assumed in the standard (non-enchanced) scenary).
The current grids of Low Resolution atmosphere models includes the complete ATLAS9 and its new version, BaSeL2.0 library and the two versions of BaSeL3.1 libaries. Extensions to hot-stars will be performed in the future.
The current grids of High Resolution atmosphere models includes the grid from Martins et al. (2004) and González Delgado et al. (2004). Extensions to others High Resolution libraries will be performed in the future.
What you can found in this server?:
At this moment, the server is under developement and no more information that this page is included (the partial information about the PGos3 system is under developement). In a quite near future, you will found here the Low Resolution and High Resolution results for the models yet includes in in the code. The database results will be updated when improvements will be performed.
It will be also aviable a search engime, and, if it is possible, a form to run directly the code in this server.
Last but not least, here there will be an access for donwload the code and the corresponding information (physical and mathematical asuptions, input and output description and tecnical details at astrophisical, computational and mathematical level).
However, you can directlly acess to the models (High and low resolution for the
different atmosphere models and isochrones described before) at the PGos3 official server at:
Sed@ server will be fully operative at the end of January 2005