VOSA. Help and Documentation

Version 7.5, July 2022

1. Introduction
2. Input files
2.1. Upload files
2.2. VOSA file format
2.3. Single object
2.4. Manage files
2.5. Archiving
2.6. Filters
3. Objects
3.1. Coordinates
3.2. Distances
3.3. Extinction
4. Build SEDs
4.1. VO photometry
4.2. SED
4.3. Excess
5. Analysis
5.1. Model Fit
5.2. Bayes analysis
5.3. Template Fit
5.4. Templates Bayes
5.5. Binary Fit
5.6. HR diagram
5.7. Upper Limits
5.8. Statistics
6. Save results
6.1. Download
6.2. SAMP
6.3. References
6.4. Log file
6.5. Plots
7. VOSA Architecture
8. Phys. Constants
9. FAQ
10. Use Case
11. Quality
11.1. Stellar libraries
11.2. VO photometry
11.3. Binary Fit Quality
12. Credits
12.1. VOSA
12.2. Th. Spectra
12.3. Templates
12.4. Isochrones
12.5. VO Photometry
12.6. Coordinates
12.7. Distances
12.8. Dereddening
12.9. Extinction
13. Helpdesk
14. About
. Excess calculation
. Total flux calculation
. VOphot quality info

Template Bayesian analysis

We can also make the bayes analysis using templates to get an estimation of the probability for each spectral type.

Take into account that, as it happened in the Template fit, the AV extinction parameter is NOT considered a fit parameter.

For more details about the Bayesian approach, please read the section about Bayes analysis.


We enter the "Template Bayes Analysis" tab and we see a form with the available template collections, so that we can choose what ones we want to use for the analysis. In this case we decide to try all of them and click in the "Make the fit" button.

The fit and analysis process is performed asynchronously so that you don't need to stay in front of the computer waiting for the search results. You can close your browser and come back later. If the process is not finished, VOSA will give you some estimation of the status of the operation and the remaining time.

When the process finishes we can see the list of objects and the spectral type with the biggest probability for those collection where there were enough points to make the analysis.

Remember that Av is not considered a fit parameter for the analysis, so its value is fixed and its probability is always 100%.

If we click in one object name, for instance, LOri001, we can see the probability of all the spectral types for each collection.