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Arp102B: An ADAF and a Torus ?

Arp102B: An ADAF and a Torus ?. Ranga-Ram Chary Spitzer Science Center, Caltech. Introduction & Observations. Arp102B at a distance of 105 Mpc, E0, double peaked H α , radio-loud. SMBH~10 8 M  . N H ~3E21 cm -2 , =1.6, no Fe K α (Eracleous et al.)

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Arp102B: An ADAF and a Torus ?

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  1. Arp102B: An ADAF and a Torus ? Ranga-Ram Chary Spitzer Science Center, Caltech R. Chary, Arp102B, Xi’an Oct ‘06

  2. Introduction & Observations • Arp102B at a distance of 105 Mpc, E0, double peaked Hα, radio-loud. SMBH~108 M. NH~3E21 cm-2, =1.6, no Fe Kα (Eracleous et al.) • Keck imaging at 12 and 18 microns (Ho, Scoville, Becklin). Seen as a single unresolved source at 12 microns, size<0.6”. • Spitzer IRS spectroscopy with SL (R~100), SH, LH (R~600) between 5-37 microns (part of Spitzer Teacher’s Education Program) • Spitzer IRS Peak-up on target providing coarse photometric calibration with 5% accuracy R. Chary, Arp102B, Xi’an Oct ‘06

  3. [NeII] 12.81 H2 9.66 H2 17.03 [NeIII] 15.56 SL and SH spectra of Arp 102B R. Chary, Arp102B, Xi’an Oct ‘06

  4. The Broadband SED: Weak variability evidence Keck data 2000 Fνν-1.2 R. Chary, Arp102B, Xi’an Oct ‘06

  5. 3cm 300μm 3μm 300Å 4 keV 400 keV A Comparison with NGC4258x3 Infrared luminosity is about the same as X-ray luminosity but x10 higher than UV Fnunu-1.2 vs Fnu nu-1.4 for NGC4258 L/LEdd~2-6E-3 vs L/Ledd for 1E-4 for NGC4258 Radio spectral index consistent with alpha<-0.25 (thermal is alpha~-0.4) Thermal electron distribution NGC4258 x30 Non-thermal electron distribution ? R. Chary, Arp102B, Xi’an Oct ‘06

  6. H2 lines detected but offset R. Chary, Arp102B, Xi’an Oct ‘06

  7. What is powering the emission ? • [OIV]/[NeII]~0.2 and [FeII]/[OIV]~0.86 indicate a starburst • But no PAH present and no silicate….. • [NeII]/[SiIII]~2.3 and [NeIII]/[ArII]>3.1 which is out of the starburst regime. • Implies mostly photoionization but 20-30% from slow shocks • Broadband SED consistent with self-Comptonized synchrotron emission around a geometrically thick accretion flow. R. Chary, Arp102B, Xi’an Oct ‘06

  8. And the H2 emission ? • Offset from systemic velocity by 500-1000 km/s • Not due to wavelength calibration which is O(100) km/s but don’t have other lines in order to check. • 107 M of molecular gas in a ring at 1 pc radius at a T~450K ? Or is it just redshifted emission like the He I at 1.083 microns ? R. Chary, Arp102B, Xi’an Oct ‘06

  9. 2-3 pc Geometrically thick ADAF ? 100 Million M Black hole Molecular H2 torus Hot Little star-formation Little dust 107 M Double peaked Halpha from the outer disk R. Chary, Arp102B, Xi’an Oct ‘06

  10. NIR Spectroscopy: Rodriguez-Ardila et al. 2006 [FeII] H2 [FeII] R. Chary, Arp102B, Xi’an Oct ‘06

  11. Rodriguez-Ardila et al. 2006 Strong HeI, [SIII], [FeII], [SII], H2 R. Chary, Arp102B, Xi’an Oct ‘06

  12. X-ray spectral analysis: Eracleous et al. 2003 R. Chary, Arp102B, Xi’an Oct ‘06

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