Characterizing the Molecular Interstellar Medium in ... - Caltech

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ladder FTS Ground JCMT Z−spec 10 12 14 –47– I (K km s −1 ) 10 5 10 4 10 3 10 2 Non-LTE Radiative Transfer Modeling Arp this work ground−based T = 1350 K, V = 350 km s −1 T = 50 K, V = 500 km s −1 0 5 10 15 J upper cted luminosity distribution of the CO ladder from J = 1-0 of J = 10-9 line, which is blended withawaterline. The urements and the blue triangles are average line fluxes from lso shown for comparison are new measurements by Z-spec del fit to the observed CO line temperatures. There are two m component (dotted line) traced by the mid-J to high-J hed line) traced by the low-J lines. %$ # • • • % # 10.0 Mid- to high-J CO are tracing warm 1.0 %# deling of CO: Likelihood distributions for gas kinetic temand pressure. The blue line represents the cold component g low-J transitions and the red line represents the warm from modeling the mid-J to high-J transitions. • • gas low-J CO are tracing cold molecular gas. ARP220 − CO ladder 0 2 4 6 8 10 12 14 J upper T kin(warm CO) = T kin(warm H 2) M gas(warm) ~ 10% M gas(cold) L CO (cold) ~ 8% Total L CO ! $ L [x 10 6 L Sun] 0.1 FTS Ground JCMT Z−spec –47– 220 L [x 10 6 L Sun] 10.0 1.0 0.1 ARP220 − CO ladder FTS Ground JCMT Z−spec 0 2 4 6 8 10 12 14 J upper –47– I (K km s −1 ) 10 5 10 4 10 3 10 2 this work ground−based T = 1350 K, V = 350 km s −1 T = 50 K, V = 500 km s −1 0 5 10 15 J upper Fig. 5.— Left: Extinction corrected luminosity distribution of the CO ladder from J = 1-0 to J = 13-12 with the exception of J = 10-9 line, which is blended withawaterline. The black solid circles are FTS measurements and the blue triangles are average line fluxes from ground-based measurements. Also shown for comparison are new measurements by Z-spec and JCMT. Right: Non-LTE model fit to the observed CO line temperatures. There are two temperature components: a warm component (dotted line) traced by the mid-J to high-J lines and a cold component (dashed line) traced by the low-J lines. %&#" ' !" %% ! $ %$# %# %# Fig. 6.— Radiative transfer modeling of CO: Likelihood distributions for gas kinetic temperature, density, column density and pressure. The blue line represents the cold component at 50 K obtained from modeling low-J transitions and the red line represents the warm component at 1350 K obtained from modeling the mid-J to high-J transitions. I (K km s −1 ) 10 5 10 4 10 3 10 2 this work ground−based T = 1350 K, V = 350 km s −1 T = 50 K, V = 500 km s −1 0 5 10 15 J upper Fig. 5.— Left: Extinction corrected luminosity distribution of the CO ladder from J = 1-0 to J = 13-12 with the exception of J = 10-9 line, which is blended withawaterline. The black solid circles are FTS measurements and the blue triangles are average line fluxes from ground-based measurements. Also shown for comparison are new measurements by Z-spec and JCMT. Right: Non-LTE model fit to the observed CO line temperatures. There are two temperature components: a warm component (dotted line) traced by the mid-J to high-J lines and a cold component (dashed line) traced by the low-J lines. %&#" ' !" %% %$# •Radiative(Transfer(code(maintained(by!Phil!Maloney cooling rate = 22 L /M %# %# Fig. 6.— Radiative transfer modeling of CO: Likelihood distributions for gas kinetic temperature, density, column density and pressure. The blue line represents the cold component at 50 K obtained from modeling low-J transitions and the red line represents the warm component at 1350 K obtained from modeling the mid-J to high-J transitions. Rangwala et al. (2011)
Arp 220: Excitation source of warm molecular gas • • • • Observed ratio: Total L CO/L FIR ~ 10 -4 [T, n(H 2)] cold = [50 K, 1000 cm -3 ] and [T, n(H 2)] warm = [1350 K, 1000 cm -3 ] This ratio along with tight constraints on T kin and n(H 2) rules out PDRs, XDRs and Cosmic ray models Require a non-ionizing source of energy: A small fraction of mechanical energy from supernovae and stellar winds can satisfy a cooling rate = 22 L /M Similar method has been successfully applied in cases NGC 1068 (Spinoglio et al. 2012; Hailey-Dunsheath et al. 2012), M82 (Kamenetzky et al. 2012), NGC 4038/39 (Schirm et al. in prep.) and Cloverleaf (Bradford et al. 2009)
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 and 8: • • • • Description of our
Page 9 and 10: Normalized Luminosity 10 7 10 6 CO
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: Modeling and Preliminary Results
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

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