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- Characterisation of YSOs (continuation of 2004 Galactic Demo)
- summary of what the science problem is and likely outcome
The use of VO tools for characterisation of YSOs by age and mass. Multi-wavelength images and spectra (and even variability information) are needed in order to improve the completeness of classification of objects in different star-forming regions. This will help constrain the effects of metallicity, the effects of different triggers etc. on the stellar IMF, conditions for planet formation etc. in our Galaxy and beyond.
- rough outline of the workflow steps involved in addresssing the case
- indication of key data resources required
Optical/IR photometric surveys (2MASS etc.) for 'visible' YSO colours
Halpha and radio 6cm for HII regions
Radio spectral index (e.g. Bernd Vollmer's work)
X-ray photometry
Molecular lines (at least catalogues)
- indication of key algorithms required
Issues (to be sorted out into workflow etc. above):
Accuracy of association for low-res data (e.g. IRAS, even ISO and most
spectra) and extended objects (UCHII, jets). For molecular line-line
assoc, can use velocity too. But still binarity/multiplicity problem.
Bulk processing of spectra? Have all suitable ISO spectra already been
analysed so just get from tables?
Reliability of existing classifications
Should the scoring system be a decision tree or a linear score?
(e.g. age 0 1 2 3 mass in Msun ... take average from different
diagnostics - but how to weight it? How to indicate ranges?)
Suggested starting point:
Take some surveys classifying YSO (15 in Vizier class, but you usually
have to look in papers to find classification criteria)
Choose some regions (Cha 1, NGC1333 etc) and find other data to go
with the classified sources and add to criteria.
In general the presesnt classifications which are applied
systematically for large(ish) Nos sources are optical/IR so these will
dominate the 'training' sets and radio/(sub)mm and X-ray will dominate
the added criteria.
The Spitzer archive is supposed to be available from May 2004.
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