The Interstellar Medium Interstellar Medium

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• Stellar absorptionlines are still presentand can be used todetermine spectraltype of star.• If the spectral typeof a star is known,its luminosity,temperature and truespectral shape areknown.• Comparing the true stellar spectrum to the observedspectrum tells us how much dust the light has traveled thru.
Dust Temperatures: <strong>The</strong>rmal (Blackbody) Emission.Horsehead Nebula (Orion) visible lightIn visible light the dust causes obscuration (dark clouds)In visible light, the dust causes obscuration (dark clouds).But in the far infrared…….Warm dust grainsemit likeblackbodies, withspectra peaking inthe infrared.<strong>The</strong> peak wavelengthreveals thetemperature (Wien’sLaw).
Page 1 and 2: The Interstellar MediumGas and Dust
Page 3 and 4: Emission Nebula - glowing gas
Page 5 and 6: The Milky Way: View towards the Gal
Page 7 and 8: Dust absorbs/scatters blue light mo
Page 9 and 10: The Milky Way: View towards the Gal
Page 11: How do we learnabout DUST in theISM
Page 15 and 16: How do we learn about GAS in the IS
Page 17 and 18: How do we learn about gas in the IS
Page 19 and 20: Average ISM Characteristics:(mostly
Page 21 and 22: Measuring cool gas: 21-cm Radiation
Page 23 and 24: Measuring cool gas: Interstellar Mo
Page 25 and 26: This formaldehyde “map” shows w
Page 27 and 28: Eagle Nebula (M16, in Orion)d k l d
Page 29 and 30: The gravitational force of a few at
Page 31 and 32: Stage 2: Continuing Collapse of eac
Page 33 and 34: Stage 3: Fragmentation Ceases, a Pr
Page 35 and 36: Stage 5: Protostar II (10 million y
Page 37 and 38: Stage 7: The Main Sequence (10 bill
Page 39 and 40: Star Clusters - the result of fragm

The Interstellar Medium Interstellar Medium

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