1 / 12

Nuclear starbursts in the dusty tori of Seyfert 1s and 2s

Nuclear starbursts in the dusty tori of Seyfert 1s and 2s. Masa Imanishi (NAO Japan). Sy1. Sy2. Nuclear starbursts (SB) may occur. Outer part of the torus. Gravitationally unstable (smaller Q-value) if Sigma(gas) = r^(> -1.5). Nuclear starbursts in the AGN torus.

yvette-fitzpatrick
Download Presentation

Nuclear starbursts in the dusty tori of Seyfert 1s and 2s

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Nuclear starbursts in the dusty tori of Seyfert 1s and 2s Masa Imanishi (NAO Japan)

  2. Sy1 Sy2 Nuclear starbursts (SB) may occur Outer part of the torus Gravitationally unstable (smaller Q-value) if Sigma(gas) = r^(> -1.5) Nuclear starbursts in the AGN torus Dusty AGN torus is molecular gas rich

  3. NGC1068 Nuclear SB in the torus kpc-scale ring-shaped circum-nuclear SB (Le Floch et al. 2001) Nuclear SB : <a few 100 pc (< 1” at z > 0.01) Slit spectroscopy

  4. 3-4 um spectroscopy 1: 3.3um PAH (SB ○, AGN×) Excellent probe for a SB PAH PAH PAH 2: PAH is intrinsically strong (EW~0.1um) Weak SB detectable

  5. 3-4 um spectroscopy 3: Lower dust extinction L(SB) from OBSERVED PAH || L(SB) from Av-corrected UV For 3 Sy2s (Imanishi 2002 ApJ 569 44) Starbust luminosity is quantifiable

  6. Data Infrared 3-4um (L-band) slit spectroscopy of 32 Sy2s and 23 Sy1s z = 0.008-0.035 CfA, 12 micron samples IRTF 3m SpeX Subaru 8.2m IRCS

  7. Sy2 EW~0.01um EW~0.1um PAH detected (11/32) PAH non-detected (21/32) Imanishi 2003 ApJ 599 918

  8. Sy1 EW~0.01um EW~0.01um PAH detected (10/23) PAH non-detected (13/23) Imanishi & Wada 2004 2004 ApJ 617 214

  9. Surface brightness: PAH > 20*10^39 [ergs / s / kpc^2] IR > 20*10^42 SB Origin of nuclear PAH emission excluded • Circumnuclear (kpc) SB • AGN / Old bulge stars (central regions) • Disk stars / Nuclear SB in the torus no PAH PAH emission is of nuclear SB origin

  10. L(3.3 PAH) = nuclear SB IRAS 12um, 25um = AGN power Nuclear SB luminosity Sy2 = Sy1 or Sy2 > Sy1 (?) SB inflate torus Sy2 (Wada et al. 2002, Levenson et al. 2002)

  11. L(3.3 PAH) = nuclear SB Nuclear N-band, radio core = AGN power

  12. L(nuclear SB) and L(AGN) : correlated Mass accretion enhanced (Wada et al. 2002) Summary L(nuclear SB) : Sy1 = Sy2 Imanishi 2003 ApJ 599 918 Imanishi and Wada 2004 ApJ 617 214

More Related