2.  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

3. Star burst (M82) AGN-dominant (NGC 1068) (U)LIRG (Arp220) Milky Way AGN-dominant AGN Star-formation

4. 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

5. Star burst (M82) AGN-dominant (NGC 1068) (U)LIRG (Arp220) Milky Way Starburst Star-formation

6. Star burst (M82) AGN-dominant (NGC 1068) (U)LIRG (Arp220) Milky Way Star-formation

7. 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

8. 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?

9.  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

10.  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

11.  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?

12.  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?

13. 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)

14. 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)

15. 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)

16. 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)

17.  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?

18.  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.

19.  Yuri Aikawa, Hideko Nomura  George Hassel, Paul Rimmer, and Yezhe Pei