@article{
 title = {The gas/dust ratio in spiral galaxies},
 type = {article},
 year = {1990},
 identifiers = {[object Object]},
 pages = {42-56},
 volume = {359},
 websites = {http://adsabs.harvard.edu/doi/10.1086/169031,http://adsabs.harvard.edu/abs/1990ApJ...359...42D},
 month = {8},
 id = {a01b2891-67e3-39fd-8acf-f8d74c2e66f3},
 created = {2017-03-14T02:43:47.000Z},
 accessed = {2017-01-30},
 file_attached = {true},
 profile_id = {d9ca9665-cda3-3617-b3e8-ecfc7a8d9739},
 group_id = {5a95a0b6-1946-397c-b16a-114c6fdf3127},
 last_modified = {2017-03-21T14:34:41.516Z},
 read = {false},
 starred = {false},
 authored = {false},
 confirmed = {true},
 hidden = {false},
 citation_key = {Devereux1990},
 notes = {NULL},
 private_publication = {false},
 abstract = {IRAS data are used here to calculate warm dust masses, which are then \ncompared with the molecular and atomic gas masses for 58 spiral galaxies \nin order to constrain the fraction and the phase of the interstellar \nmedium in spiral galaxies that contributes to the emission measured by \nIRAS. The dispersion in the ratio of dust mass to total gas mass is \nlarger than expected on the basis of measurement errors. The dispersion \nin the ratio of dust mass to inner disk gas mass is less than the \ndispersion in the ratio of IR to radio emission. The inner gas to warm \ndust mass ratio for spiral galaxies is 1080 + or - 70, indicating that \n80-90 percent of the dust mass in spiral galaxies is radiating at over \n100 microns and has a temperature less than about 30 K. However, the \nbulk of the dust in spiral galaxies is less than about 15 K regardless \nof the phase of the ISM. Both H I and H2-associated dust contributes to \nthe warm 30 K emission.},
 bibtype = {article},
 author = {Devereux, Nicholas A. and Young, Judith S.},
 journal = {The Astrophysical Journal}
}

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