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Why is interesting to investigate The chemical composition of early B MS stars in the Orion star forming region (in a more general context) O’Dell (yesterday): One must understand the best example of a class of objects before generalizing about more distant objects Ori OB1 contains a large number of bright, low vsini, early B-type stars (covering the full range B0-B2) we can test our codes, methods, and atomic data with a set of high quality spectra + identification of problematic/best diagnostic lines + identification of possible biases and systematics a reference for abundance studies of more distant stars (and/or larger vsini) Ideal !! Still good ! More difficult SNR > 150 100 < SNR < 150 km/s SNR < 100 km/s
Why is interesting to investigate The chemical composition of early B MS stars in the Orion star forming region (in a more general context) Put more constraints to the present-day chemical composition* of the solar vicinity, including elements which cannot be easily studied from HII regions (e.g. Si, Mg) * No dust depletion !!
Page 2 and 3: The Orion Nebula (M42) Chemical com
Page 4 and 5: Why is interesting to investigate T
Page 8 and 9: Chemical abundance studies of early
Page 10 and 11: The chemical composition of early-B
Page 14 and 15: How to perform a stellar abundance
Page 16 and 17: How to perform a stellar abundance
Page 18 and 19: What is new/different between CL94
Page 20 and 21: A new analysis of the B-type stars
Page 38 and 39: Conclusions - Recent accurate abund
Page 40 and 41: Orion OB1: B-type stars vs nebular

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