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,

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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 destructive or promotive role in sustaining in the molecular cloud?

Method 2MASS color-color criteria CTTSs & HAeBe (Not WTTSs)  IR excesses Empirical, but confirmed by spectraspectra Effective, select a plenty of candidates Upto ~1pc CO map Molecular clouds Hα map Ionization fronts (Orion-Eridanus Superbubble)

Orion-Monoceros Complex N E 450 pc deg 12 CO, 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 line

2MASS Color-Color Criteria

Orion A

Orion B

Mon R2

NGC 2194, vdB64 & Crossbones

The Whole Picture of Star Formation in 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 1d Spatial 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 CTTSsHAeBe