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Subaru and Gemini high-spatial-resolution 20um imaging of nearby LIRGs

Subaru. Subaru and Gemini high-spatial-resolution 20um imaging of nearby LIRGs. （今西　昌俊）. NAOJ (Subaru Telescope). Masa Imanishi. Gemini-S. optical. (U)LIRGs. IR. IR. optical. Luminous energy source is hidden behind dust. Luminous infrared galaxies （ LIRGs ）. ULIRGs:>10 12 Lo.

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Subaru and Gemini high-spatial-resolution 20um imaging of nearby LIRGs

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  1. Subaru Subaru and Gemini high-spatial-resolution 20um imaging of nearby LIRGs （今西　昌俊） NAOJ(Subaru Telescope) Masa Imanishi Gemini-S

  2. optical (U)LIRGs IR IR optical Luminous energy source is hidden behind dust Luminous infrared galaxies（LIRGs） ULIRGs:>1012Lo L(IR) > 1011 Lo (Normal spiral ~ 1010 Lo) M100（Sbc）

  3. > 10kpc Starburst AGN Mass accretion onto supermassive blackholes（>106 Mo） < 1pc (U)LIRGs L(IR) > 1011Lo Luminous energy sources behind dust

  4. LIRG ULIRG LIRG ULIRG 0 1 0 1 2 Le Floc’h et al. 2005 Caputi et al. 2007 (U)LIRGs: important at high-z L(IR) LIRG ULIRG

  5. NLR (U)LIRGs have a large amount of nuclear gas and dust Buried AGNs are elusive >70% (U)LIRGs = non-Sy Veilleux+99 AGNs in (U)LIRGs are buried Sy2 AGNs obscured by torus-shaped dust HII LI Sy2 Detectable via optical spectroscopy Veilleux+99;Yuan+10

  6. ★ SB AGN IR spectroscopy AKARI 2.5-5um PAH Normal SB Buried AGN Extreme SB (?)

  7. Buried AGN E = 6-40% Mc2 >>1013 Lo / kpc2 1011 Lo / kpc2 <1013 Lo / kpc2 Supported by Eddington-limited SB theory M42 M82 Thompson+05 SB HII-region core Emission surface brightness SB ★ SB E = 0.5% Mc2

  8. Why 20um? PAH contamination small Diffraction-limited image achieved Stable PSF If >>1013 Lo / kpc2, then buried AGN Ground-based large 8-10m telescope is better than space satellites (0.7-0.85m)

  9. Subaru COMICS Diffraction-limited images are usually achieved 20um compact extended Standard star 1012 Lo / kpc2 size<0.2” Mitsubishi- pattern >3*1013 Lo / kpc2 Imanishi+11

  10. Gemini-S/T-ReCS Diffraction-limited images are usually achieved 20um extended compact Standard star <1012 Lo / kpc2 size<0.25” Diffraction ring >2*1013 Lo / kpc2 Imanishi+11

  11. Super star cluster NGC 5253 (d=4Mpc) Gemini-S T-ReCS 20um ~1013 Lo / kpc2 Imanishi+11 submitted

  12. IR spectroscopy vs imaging (I) extended SB ~1012 Lo / kpc2 (z=0.016) (z=0.025)

  13. IR spectroscopy vs imaging (II) B-AGN compact >1013 Lo / kpc2 (z=0.055) (z=0.058)

  14. Distant ULIRGs (z>0.1) >0.5*1013Lo/kpc2 Need higher-spatial-resolution of TMT/MICHI

  15. Summary B-AGN and SB are distinguishable, based on 20um emission surface brightness, if z < 0.06 Generally agree with IR spectroscopic energy diagnostic method Imanishi+11 submitted (accepted soon)

  16. End

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