Microsimulations

It is not so well defined to what we call "Microsimulations".

In a way, it is was first used as opposed to "cosmological simulations" (macrosimulations). In fact, we tend to use that word to include any theoretical model that is simple enough so that it does not need a complex schema as that of SimDB/SimDAP to be incorporated in the VO framework.

In other words, we want to define a simple protocol so that theoretical models can be included in the VO. Those models that can be implemented with this simple protocol are, in that sense, "microsimulations".

TSAP (SSAP theory use case)

The first attempt (as an ESAVO-SVO collaboration) to define such a protocol was TSAP (Theory Simple Access Protocol), designed to access theoretical spectra. Now TSAP is part of the SSAP protocol as a Use Case.

General information about TSAP

• SSAP protocol
• TSAP: how to use it (SVO web page)
• TSAP interface (an interface to check a TSAP service, check if it works as expected or retrieve data from it)

Model services using TSAP

• Web access to SVO theoretical spectra model services

• • Dalessio disk models
  • Kurucz ODFNEW/NOVER models
  • NextGen models
  • COND00 models
  • DUSTY00 models
  • Coelho models

Applications using TSAP

• VOSpec
  • An ESA-VO tool able to handle Spectra in the VO context as well as providing analysis capabilities and easy integration of spectra coming from different data providers, wavelengths, and different metadata
  • accesses theoretical spectra in the VO allowing to compare them with observed data.
• VOSed
  • An SVO tool that permits to characterize the protoplanetary disks around young stars taking advantage of the already existing VO standards and tools.
  • uses TSAP to access Dalessio models to fit observed data.
• VOSA
  • a web application developed using VO resources to fit observational data with theoretical models to infer physical properties for the observed objects.
  • uses TSAP to access several theoretical spectra collections and synthetic photometry corresponding to those spectra and find the best fit for observed photometry.

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