arp102b: an adaf and a torus ?
DESCRIPTION
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.) - PowerPoint PPT PresentationTRANSCRIPT
R. Chary, Arp102B, Xi’an Oct ‘06 1/12
Arp102B: An ADAF and a Torus ?
Ranga-Ram CharySpitzer Science Center, Caltech
R. Chary, Arp102B, Xi’an Oct ‘06 2/12
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 3/12
SL and SH spectra of Arp 102BH
2 9.
66 [NeI
I] 1
2.81
[NeI
II]
15.5
6
H2
17.0
3
R. Chary, Arp102B, Xi’an Oct ‘06 4/12
The Broadband SED: Weak variability evidence
Keck data 2000
Fνν-1.2
R. Chary, Arp102B, Xi’an Oct ‘06 5/12
A Comparison with NGC4258x3
NGC4258 x30Non-thermal electron distribution ?
Infrared luminosity is about the same as X-ray luminositybut x10 higher than UV
Fnunu-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)
3cm 300μm 3μm 300Å 4 keV 400 keV
Thermal electron distribution
R. Chary, Arp102B, Xi’an Oct ‘06 6/12
H2 lines detected but offset
R. Chary, Arp102B, Xi’an Oct ‘06 7/12
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 8/12
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 9/12
2-3 pc
Molecular H2 torusHotLittle star-formationLittle dust107 M
100 Million M
Black hole
Geometrically thickADAF ?
Double peakedHalpha from the outerdisk
R. Chary, Arp102B, Xi’an Oct ‘06 10/12
NIR Spectroscopy: Rodriguez-Ardila et al. 2006
[FeII] [FeII] H2
R. Chary, Arp102B, Xi’an Oct ‘06 11/12
Rodriguez-Ardila et al. 2006 Strong HeI, [SIII], [FeII], [SII], H2
R. Chary, Arp102B, Xi’an Oct ‘06 12/12
X-ray spectral analysis: Eracleous et al. 2003