Observing Star-FormationFrom the Interstellar Mediumto Star-Forming CoresOn-Line Version, 1999

Observing Star Formation From the ISM to Star-Forming Cores

History: Theory and Optical Observations

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Important Distinction to Keep in Mind

Spectral-Line Mapping Adds Velocity Dimension

Orion:13CO ChannelMaps

Molecular Outflows

Jeans Mass, Virial Mass, and Filling Factors in the ISM

What do we need to explain?

Self-similar Structure on Scales from 100 pc to 0.1 pc...in Orion

ìClumpî Mass Distribution

ìLarsonís Lawî Scaling Relations (1981)

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Rough Virial Equilibrium in Star-forming regions

Density-Velocity-Magnetic Field Structure

Velocity Structure

Velocity Coherent Cores*Where does the self-similarity end?

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Similar ìTransitionî Found in Spatial Distribution of Stars

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Magnetic Field Structure

Using Polarizationto Map Magnetic Fields

Using Polarimetry to Map Field Structure

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Magnetic Field Structure: Emission Polarimetry

Cloud Lifetimes

The Effects of a Previous Generation of Stars

Density-Velocity-Magnetic Field Structure

Initial Conditions for Star-Formation(Version 99)

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Thanks to:

What now?

The Pleiades

Bright Nebula: Orion

Dark Nebula: The Horsehead

The Electromagnetic Spectrum

A Dense Core: L1489

A Dark Cloud: IC 5146