Characterizing the Molecular Interstellar Medium in ... - Caltech

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• • • • • • Goals of the Program Determine the molecular gas (and dust) properties as a function of L FIR and galaxy type (starburst, AGN, disks and ellipticals) Address the origin of the excitation of warm molecular gas of varying L FIR: Star-Formation vs AGN? Compare the gas excitation and dust properties of the local IR luminous galaxies to high-z submm galaxies. Explore *Total* L CO - L FIR Relation Direct measurement of [CO/H 2] abundance for warm molecular gas. Substantial public database of legacy value for nearby galaxies
Normalized Luminosity 10 7 10 6 CO SLED: diagnostic for Star Formation Vs AGN? 0 1 2 3 4 5 6 7 8 9 10 11 12 13 14 J upper Mrk 231 (AGN) Arp 220 (Starburst) M82 (Starburst) Mid- to High-J CO traces warm gas and dominates the CO luminosity and cooling
Page 1 and 2: Characterizing the Molecular Inters
Page 3 and 4: • Description of our Archival Pro
Page 5 and 6: • • Description of our Archival
Page 7: • • • • Description of our
Page 11 and 12: Herschel! Archive! Literature! data
Page 13 and 14: Flux (Jy) 600 400 200 0 CO (43) CI
Page 15 and 16: Flux (Jy) 10 8 6 4 2 0 CO (43) CI (
Page 17 and 18: Modeling and Preliminary Results
Page 19 and 20: Arp 220: Excitation source of warm
Page 21 and 22: 3 4 5 6 Log 10 n(H 2) (cm 3 ) 4 5 6
Page 23 and 24: Dust Modeling Arp220 NGC 6240 S( )=
Page 25 and 26: Extra Slides
Page 27 and 28: UGC 05101 (LIRG/AGN) Flux [Jy] 3456
Page 29 and 30: L CO (65) (L sun) 10 10 10 9 10 8 1
Page 31 and 32: 3060 M. S. Bothwell et al. 4.3 The

Characterizing the Molecular Interstellar Medium in ... - Caltech

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