The Origins, Applications and Mysteries of the Fluorescent Iron Line p.1/29
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1 The Origins, Applications and Mysteries of the Fluorescent Iron Line Scott C. Noble November 3, 2004 CTA, Physics Dept., UIUC The Origins, Applications and Mysteries of the Fluorescent Iron Line p.1/29
2 Outline Who? When? How? (history) What? (fluorescence) Where? (origins, disk models) Why? (spacetime/disk probing, reverberation) Wassup? (problems...) Really? (resolutions...) Won t he ever stop talking? (conclusions...) The Origins, Applications and Mysteries of the Fluorescent Iron Line p.2/29
3 First Broad Iron Line Cyg X-1 Obs. by Barr, White, Page (1985) w/ EXOSAT Peak at 6.2keV EW 120keV Variability t orb Interpreted by Fabian et al. (1989) The Origins, Applications and Mysteries of the Fluorescent Iron Line p.3/29
4 First Broad Iron Line from AGN MCG Seyfert Type-1 Nandra, Pounds, Stewart, Fabian, Rees (1989) 2-day EXOSAT observation Not interpreted as relativistic broadening The Origins, Applications and Mysteries of the Fluorescent Iron Line p.4/29
5 ASCA Revolution MCG Tanaka et al. (1995) ASCA 4-day observation Beginning of detailed matching to models The Origins, Applications and Mysteries of the Fluorescent Iron Line p.5/29
6 X-ray Observatories [ Reynolds & Nowak (2003) ] The Origins, Applications and Mysteries of the Fluorescent Iron Line p.6/29
7 Kα Fluorescence L M K Kα 33% 66% 6.4 kev >7.1 kev The Origins, Applications and Mysteries of the Fluorescent Iron Line p.7/29
8 X-ray Reflection Spectrum [Reynolds, Ph.D. Thesis (1996)] Incident Flux: F N E Γ (where Γ = 2 here); Cosmic Abundances: H+, He++, neutral metals; Kα = kev (Fe I to Fe XXV ); Kβ = 7.1 kev (Fe I ); Abs.Edge = kev (Fe I to Fe XXV ); The Origins, Applications and Mysteries of the Fluorescent Iron Line p.8/29
9 Accretion Disk Models a M H r g R r g /c = GM/c 3 t dyn α t therm α (H/R) 2 t visc [ t dyn = 310 a + (r/r g ) 3/2] M 10 7 M sec. T M 1/4, L = η Mc 2 The Origins, Applications and Mysteries of the Fluorescent Iron Line p.9/29
10 Accretion Disk Models Thermal, black-body spectrum from disk; Inverse Compton (IC) scattering up-scatters thermal γ s into power-law X-ray; X-rays Kα in disk; IC cut-off at E 100keV when E γ E e T corona IC cools corona The Origins, Applications and Mysteries of the Fluorescent Iron Line p.9/29
11 Corona Models [Nowak astro-ph/ ] The Origins, Applications and Mysteries of the Fluorescent Iron Line p.10/29
12 Types of Accretors AGN GBHC s M = M 1 100M T M 1/ K 10 7 K Spectra Opt./UV BB + P-L tail X-ray BB + P-L tail t dyn minutes to hours t dyn = milliseconds t obs 1ks t therm t visc The Origins, Applications and Mysteries of the Fluorescent Iron Line p.11/29
13 Numerical Models for Fitting Thin disk, cosmic abundances... The Origins, Applications and Mysteries of the Fluorescent Iron Line p.12/29
14 Numerical Models for Fitting Thin disk, cosmic abundances... a BH spin: 0 < a The Origins, Applications and Mysteries of the Fluorescent Iron Line p.12/29
15 Numerical Models for Fitting Thin disk, cosmic abundances... a i BH spin: 0 < a Inclination angle: i The Origins, Applications and Mysteries of the Fluorescent Iron Line p.12/29
16 Numerical Models for Fitting Thin disk, cosmic abundances... a i BH spin: 0 < a Inclination angle: i β Emissivity (β): I e r β e The Origins, Applications and Mysteries of the Fluorescent Iron Line p.12/29
17 Numerical Models for Fitting Thin disk, cosmic abundances... a i BH spin: 0 < a Inclination angle: i β ξ Emissivity (β): I e r β e Ionization Parameter ξ The Origins, Applications and Mysteries of the Fluorescent Iron Line p.12/29
18 Relativistic Effects (a = 0) [Fabian, Iwasawa, Reynolds, Young (2000)] The Origins, Applications and Mysteries of the Fluorescent Iron Line p.13/29
19 Dependence on BH Spin [Reynolds & Nowak (2003)] β = 3 The Origins, Applications and Mysteries of the Fluorescent Iron Line p.14/29
20 Dependence on Inclination [Reynolds & Nowak (2003)] β = 0.5, a = The Origins, Applications and Mysteries of the Fluorescent Iron Line p.15/29
21 Dependence on Emissivity [Reynolds & Nowak (2003)] a = 0.5 The Origins, Applications and Mysteries of the Fluorescent Iron Line p.16/29
22 Dependence on Ionization from [Reynolds & Nowak (2003)], calculated by [Ballantyne et al. (2001)] The Origins, Applications and Mysteries of the Fluorescent Iron Line p.17/29
23 Appearance of Disk s Temperature a = 0.01 i = 85 i = 45 i = 5 The Origins, Applications and Mysteries of the Fluorescent Iron Line p.18/29
24 Appearance of Disk s Temperature a = i = 85 i = 45 i = 5 The Origins, Applications and Mysteries of the Fluorescent Iron Line p.19/29
25 Reverberation a = 0.998, i = 30, h flare = 7.5r g [Reynolds et al. (1999)], [Young & Reynolds (2000)], [Young (2003)] The Origins, Applications and Mysteries of the Fluorescent Iron Line p.20/29
26 Reverberation a = 0.998, i = 30, h flare = 10r g [Reynolds The Origins, Applications and Mysteries of the Fluorescent Iron Line p.21/29
27 Variability Problem F Kα varies without F cont variation Mrk 841, Seyfert-1, t var 10hours, [Petrucci et al. (2002)] F cont varies without F Kα MCG , Seyfert-1, [Vaughan & Fabian (2004)] F Kα varies with F cont (kinda): IRAS , Seyfert-2, highly-ionized disk, [Iwasawa et al. (2004)] No long-term EW/F cont correlation: Sampling of 7 Seyfert-1 AGN, [Markowitz, Edelson, Vaughan (2003)] Short-term (30 days) and Long-term (1000 days) RXTE obs. s Correlations between Γ and F cont The Origins, Applications and Mysteries of the Fluorescent Iron Line p.22/29
28 F Kα Variation Mrk 841, Seyfert-1 [Petrucci et al. (2002)] The Origins, Applications and Mysteries of the Fluorescent Iron Line p.23/29
29 F cont Variation MCG , Seyfert-1 [Vaughan & Fabian (2004)] The Origins, Applications and Mysteries of the Fluorescent Iron Line p.24/29
30 Variation Resolutions: Disk Properties F Kα diminished in Radio-loud AGN Anti-correlation with increasing ionization effects [Ballantyne et al. (2002)]; Photon Bubble Instability, [Gammie (1998)], [Ballantyne et al. (2004)] varying density structure t dyn ; can explain Mrk 841 variability; Disk asymmetries modulations from orbit w/o modulating source Spiral density/ionization profile [Karas et al. (2001), Hartnell & Blackman (2002)]; MHD Turbulence (non-rel., ZEUS, a = 0) [Armitage & Reynolds (2003)]; F Kα from material within ISCO [Reynolds & Begelman (1997)], [Reynolds et al. (2004)]; Ang. Mom. Transfer from material within ISCO [Gammie (1999)], [Reynolds et al. (2004)]; The Origins, Applications and Mysteries of the Fluorescent Iron Line p.25/29
31 Variation Resolutions: Source Properties [Miniutti & Fabian (2004)] Source asymmetry disk bias; Rel. effects magnify bias; a = The Origins, Applications and Mysteries of the Fluorescent Iron Line p.26/29
32 Variation Resolutions: Source Geometry The Origins, Applications and Mysteries of the Fluorescent Iron Line p.27/29
33 Variation Resolutions: Source Geometry [Iwasawa, Miniutti & Fabian (astro-ph/ )] Rotating point source, r = 6r g, h = 9r g, i = 20, a = M sim = M M Hα 1.68 ± M NGC 3516 Seyfert-1 The Origins, Applications and Mysteries of the Fluorescent Iron Line p.28/29
34 Conclusions and the Future better spectroscopy + better models = real measurements more sophisticated models = more possibilities XEUS (ESA), Constellation-X (NASA), MAXIM Measure iron-line for furthest known AGN Resolve inner horizon Greater time-resolved spectroscopy The Origins, Applications and Mysteries of the Fluorescent Iron Line p.29/29
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