Star Formation in Orion-Monoceros Complex VO Tool Application - online catalog & Aladin
章展誥 (Chang, Chan-Kao),高仲明 (Ko, Chung-Ming)Institute of Astronomy, National Central University, Taiwan
This report is base on the dissertation of 李昫岱
Outline
Motivation Method Orion-Monocerus Complex Conclusion Using VO tools
Motivation
Destructive or Promotive Do massive stars play a decisively destru
ctive or promotive role in sustaining in the molecular cloud?
Method 2MASS color-color criteria
CTTSs & HAeBe (Not WTTSs) IR excesses Empirical, but confirmed by spectra Effective, select a plenty of candidates Upto ~1pc
CO map Molecular clouds
Hα map Ionization fronts (Orion-Eridanus Superbubble)
Orion-Monoceros ComplexN
E450 pc20-30 deg
12CO, Dame et al. 2001
Orion-Eridanus Superbubble
H alpha, Finkbeiner 2003
Orion-Monoceros Complex
2MASS Color-Color Criteria
CTTSs - diamond HAeBe – triangle B[e] – crosses Classical Be – plus Main Seq. – Solid line CTTS locus – dash lin
e
2MASS Color-Color Criteria
Orion A
Orion B
Mon R2
NGC 2194, vdB64 & Crossbones
The Whole Picture of Star Formationin Orion-Monoceros Complex
Conclusion
The SF in Orion-Monoceros complex appears to be dominated by Orion-Eridanus superbubble.
SF start from 1a, 1b, 1c then 1dSpatial distribution (this study)Age distribution (Brown et. al., 1994)
Benefits & Challenges Benefits
Online Catalog & images + Integrated tool Efficient and easy to retrieve data Data visualization is much easier
Challenges Query limitations – not fully meet
requirements Records limitation Query constrain limitation (sky region, condition…
etc) Large memory resource needs Spectra data is unavailable so far Survey image is not complete
Back Up
CTTSs & HAeBe CTTSs
Low-Mass PMS Class II H alpha emission, CaII (H, K line emission) IR excess
HAeBe Intermediate-Mass PMS H alpha emission IR excess Balmer lines absorption
Other Methods Object-prism (Hα emission)
Sensitive to CTTSs, HAeBe, not WTTSc Contaminated by late-type dwarf
X-ray survey (ROAST All Sky Survey) within hundred pcs Contaminated by chromospherically active K & M dwarfs
Proper motion Magnitude limitation (accuracy)
Variability survey Multi-epoch variability survey is time-consuming
Spectra of CTTSs & HAeBe
CTTSs HAeBe