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Published byReginald Morris Modified over 9 years ago
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High luminosity from the galactic central region L bol ~ 10 44-46 erg/s High X-ray luminosity Supermassive black hole at the center of the galaxy M BH =10 6-10 M mass accretion
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Star burst (M82) AGN-dominant (NGC 1068) (U)LIRG (Arp220) Milky Way AGN-dominant AGN Star-formation
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Star burst (M82) AGN-dominant (NGC 1068) (U)LIRG (Arp220) Milky Way (Ultra-) Luminous Infrared Galaxies ((U)LIRG) dense gas high infrared luminosity L IR >10 11 L sun (AGN) Star-formation
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Star burst (M82) AGN-dominant (NGC 1068) (U)LIRG (Arp220) Milky Way Starburst Star-formation
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Star burst (M82) AGN-dominant (NGC 1068) (U)LIRG (Arp220) Milky Way Star-formation
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AGNs › High CN, HCN abundances in central region of the galaxy (X CN ≡[CN]/[H tot ]~10 -7 ) (U)LIRGs › High HCN, HC 3 N, C 2 H 2 abundances › (X HCN ~10 -7 -10 -6, › X C2H2 >10 -7 ) Starburst › Higher HCO + /HCN ratio than AGNs
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AGNs › High CN, HCN abundances in central region of the galaxy › (X CN ≡[CN]/[H tot ]~10 -7 ) (U)LIRGs › High HCN, HC 3 N, C 2 H 2 abundances › (X HCN ~10 -7 -10 -6, › X C2H2 >10 -7 ) Starburst › Higher HCO + /HCN ratio than AGNs What causes the differences between these galaxies? Can molecules tell us about the X-ray activity in the galaxy with AGN? Can molecules tell us about the star formation rate? What causes the differences between these galaxies? Can molecules tell us about the X-ray activity in the galaxy with AGN? Can molecules tell us about the star formation rate?
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Molecular abundance modeling of a molecular accretion disk of an AGN- dominant galaxy to 100 pc 1+1-dimensional model of a cylindrically symmetric disk Chemical network: High-temperature OSU network (Harada et al. ApJ submitted) Molecular abundance modeling of a molecular accretion disk of an AGN- dominant galaxy to 100 pc 1+1-dimensional model of a cylindrically symmetric disk Chemical network: High-temperature OSU network (Harada et al. ApJ submitted) Top View Side View
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Blackbody Temperature T ~750 K(L/2x10 45 erg/s) 1/4 (r/pc) -1/2 Density NGC 1068 L bol =2x10 45 erg/s M BH =1x10 7 M L X ~10 42 erg/s (obs) NGC 1068 L bol =2x10 45 erg/s M BH =1x10 7 M L X ~10 42 erg/s (obs) Total hydrogen density (cm -3 ) r(pc) z(pc) Inner region Outer region h/r=0.1
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Ionization rate › X-rays › UV-photons › Cosmic-rays Star formation Supernovae E~10 51 erg OB stars L OB ~10 4 L sun Cosmic-rays UV-photons AGN core X-rays Cosmic-rays?
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Ionization rate › X-rays › UV-photons › Cosmic-rays Star formation Supernovae E~10 51 erg OB stars L OB ~10 4 L sun Cosmic-rays UV-photons AGN core X-rays Cosmic-rays?
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Cosmic-rays Star formation rate per volume ν=star formation efficiency (10 -5 – 10 -2 ) Assume some fraction of energy from supernovae or OB stars go to ionization. X-rays Maloney et al (1996)
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CN Observed abundances (source size ~70pc, inclination 40º) X CN =(0.2-1)x10 -7 More abundant at the outer radius Star formation efficiency = 10 -5 Star formation efficiency = 10 -2 X-ray + low SF X-ray + high SF r(pc)
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HCN Star formation efficiency = 10 -5 Observed abundances X HCN =(0.8-1)x10 -7 More abundant at the inner disk Star formation efficiency = 10 -2 X-ray + low SF X-ray + high SF r(pc)
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HCO+ Star formation efficiency = 10 -5 Observed abundances X HCO+ =(0.6-2)x10 -7 Star formation efficiency = 10 -2 X-ray + low SF X-ray + high SF r(pc)
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Cosmic-ray penetration › The ionization rate may not be uniform Disk structure › h/r may be r-dependent UV-photons Radiative transfer Clumpiness Metalicity Shock waves › How much does it dissociate? › Effect of sputtering?
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X-rays alone can produce close to the lower limit of the observed abundances of CN, HCN although some star formation can help produce more. We predict that the chemistry will be different in the inner core - less CN and more HCN. Higher-resolution observation of ALMA can reveal gas properties in AGN disks in greater detail through molecular observations. As a future work, comparison with other types of galaxies will be interesting.
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Yuri Aikawa, Hideko Nomura George Hassel, Paul Rimmer, and Yezhe Pei
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