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X-ray Observation of Accretion Disk in AGN

X-ray Observation of Accretion Disk in AGN. K. Hayashida (Osaka University). VSOP…Jet … Blazar. X-ray Observational Study of AGNs. Spectrum Power Law Cold Absorber Iron Line Soft X-ray Excess Reflection Hump Warm Absorber Timing Image Outflow, starburst component etc. MKN509.

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X-ray Observation of Accretion Disk in AGN

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  1. X-ray Observation of Accretion Disk in AGN K. Hayashida (Osaka University)

  2. VSOP…Jet… Blazar X-rayObservational Study of AGNs • Spectrum • Power Law • Cold Absorber • Iron Line • Soft X-ray Excess • Reflection Hump • Warm Absorber • Timing • Image • Outflow, starburst component etc.

  3. MKN509 MKN841 Soft X-ray Excess • Discovery • Mkn509 (HEA1 A2 LED+MED), Singh et al., 1985, ApJ, 297, 633. • Mkn841 (EXOSAT), Arnaud et al., 1985, MNRAS, 217, 105. • Excess Soft X-ray Emission above Extrapolation of Power Law Spectrum determined at High Energy • High Energy Tail of the UV-Bump ? • Lower kT version of Soft (Disk) Component found in Stellar Black Hole Candidates • kT~1keV for SBHC • T∝M -1/4

  4. Correlation with the UV emission • ROSAT • Walter & Fink, 1993, A&A,274, 105 G in Soft X-ray band G in Soft X-ray band (Soft Excess / Power Law) @0.2-0.4keV (UV flux / 2keV Flux)

  5. IUE / ROSAT / Ginga(Walter et al.,1994, A&A,285, 119) Model A Model B

  6. Model A Large Scatter in Ecut Model B Ecut ranges 40-80eV Spectral Shape (Cut-off energy)

  7. Origin of the Soft Excess Component • Thermal Emission from (Optically Thick) Accretion Disk • Inverse Compton Emission by Hot Corona , Cooled Pairs etc. • Seed: UV photons from the Disk • Reprocessing of Hard X-ray photons • (Thin Thermal Emission)

  8. Soft X-ray Excesswith ASCA • NGC4051, Mihara et al. 1994 • PG1211+143, Yaqoob et al., 1994. • NGC5506, Wang et al., 1996 • 3C273, Cappi et al., 1998 • Reynolds, 1997 • 24 Type1 AGNs (RQ+RL) ; Soft Excess in 7 objects • Murakami, 1997. • 10AGNs; Soft Excess (f0.5>0.1) was found in 9 objects • BB kT~0.1keV or Brems~0.2keV

  9. Correlation with UV-flux fse(ASCA0.5keV) Correlates with fse(ROSAT0.1-0.4keV) . BB luminosity >Ledd More Sophisticated model is needed ? fse:Soft Excess Comp/ Power Law Comp at 0.5 keV Soft X-ray Excess (Murakami, 1997)

  10. Seyfert Type 1 whose Broad Emission Line Width is Narrow. (???) Efficient Way to see the Soft Excess …Narrow Line Seyfert 1 (NLS1)

  11. Boller et al., 1997 X-ray Studies with ROSAT • Prototype=IRAS13224-3809 • Steep Soft X-ray Index G=4.4±0.2 • Rapid & Large Amplitude Variability Common for NLS1 at Some Level

  12. ASCA … Spectrum Above 2keV • Two Components Spectrum (e.g. Otani et al.1996) • Soft Component ~BB kT=0.1-0.2keV • Hard Tail above 2 keV • Hard PL Index Steeper (G>2) than BLS1 (Brandt et al., 1997) • See Leighly, 1999.

  13. Models Edge On Pole On Small BH Statistical Properties Narrow Hb Width Rapid / Large Ampl. X-ray Variability Steep Soft X-ray Spectrum

  14. X-ray Spectrum of NLS1s　（ASCA)

  15. kTBB vs Soft Excess Ratio

  16. BB Fit ->Area->BH Size Hayashida，2000, New Astronomy Review,44,419

  17. ASCA Light Curves of NLS1

  18. NGC4151 BLSｙ１NLSy1 Lx vs Mvar（BLSy1 / NLSy1) Hayashida，2000, New Astronomy Review,44,419 Cf Results from Excess Variance By Tuner et al.(1999) & Leighly (1999)

  19. Hb FWHMvs Mvar BLS1: 107-108Mo NLS1: 105-107Mo Hayashida，2000, New Astronomy Review,44,419

  20. MBBfit(0.5Rs) vs Mvar for NLS1 Hayashida，2000, New Astronomy Review,44,419

  21. Can we reconcile the Contradiction ? • For MBBfit < Mvar • Inclination Effect • cos Factor … MBBfit gives under-estimate • Tc > Te Effect • MBBfit gives under-estimate, too. Hayashida，2000, New Astronomy Review,44,419

  22. Accretion Disk ? • If Soft Component is thermal emission from accretion disk, Observations of NLS1 provide important clue to theoretical work. • e.g. SlimDiskModel (Mineshige et al. 2000, PASJ, 52, 499)

  23. Peculiar Spectral Feature around 1keV • Otani et al (1996), Hayashida et al (1997), Leighly et al. (1997) • 0.2-0.3c blue shifted absorption edge ? • 0.5-0.6c blue shifted absorption line ? • Emission line ?

  24. Chandra Observations of BLS１ｓ (NGC3783, NGC5548) • Narrow Absorption Lines from H-like or He-like ions of C, N, O, Ne, Na, Mg, Si, Fe • OVII, OVIII edge were NOT detected. (NGC5548) • V(blueshift)~200-500km/s • V(turb)~100-200km/s NGC5548(LETG;86ks)

  25. Reflection from Ionized Disk Model (Ross & Fabian, 1993, MNRAS,261, 74)

  26. Chandra / XMM Observation of Soft X-ray Excess in NLS1s • Sensitive to Lower Energy Band • Higher Energy Resolution with Gratings • No Strong Absorption / Emission Features in the Soft X-ray Spectra of NLS1s • TonS180 (Chandra) Tuner et al., • PG1404(Chandra) Nandra et al., • Mrk766(XMM)

  27. ACIS/LETG Simlutaneous with ASCA and FUSE +HST (UV) Tuner et al., 2001, ApJ, 548, L13. No significant absorption feature TonS180 Instrumental

  28. Nandra et al., 2001 PG1404 (Chandra MEG)

  29. Nandra et al., 2001 PG1404 (Chandra MEG)

  30. Sorry, No Time (Ability) to Cover • Comparison with • Disk Component in Stellar Black Hole Candidates • X-ray Spectra of Super Eddington Sources in nearby galaxies • Disk Component and Jet Component in micro quasars

  31. Soft X-ray Excess : Summary • Soft X-ray Excess does exist • Correlate with UV • Enhanced in NLS1s • Examination with Theoretical Accretion Disk Model is expected • Correlation / Lag to UV, Hard X-ray would be examined.

  32. Fe K Fluorescence Line • Discovery by ArielV，HEAO-1 • Reflection Hump found by Ginga • Interpretedwith Reflection Model • Line Broadening discovered by ASCA • Disk Line Model

  33. Disk Line Model (e.g. Fabian, 2001, astroph.0103438)

  34. Luminosity Dependence of the Line Intensity (Nandra et al., 1997, ApJ, 487, L91)

  35. XMM Observation of MCG-6-30-15 Williams, Fabain 2001

  36. Line Intensity [phs/s/keV/cm^２] Energy [keV] from Matsumoto Disk Line MCG-6-30-15 Tanaka et al., 1995, Nature, 375, 659 i=30deg, 6rg-40rg

  37. Alternative Model Variability of Continuum / Line(Matsumoto, Inoue, 2000) Line Emission region must be far away from several Rs

  38. Flux Energy Alternative Interpretation Flux(Fobs) Energy Variability Energy Ｄｉｓｋｌｉｎｅ model (Matsumoto, Inoue, 2000) PL Variable Ionized Absorber Variability PL Energy Two warm absorbers to reproduce the σ(E) ξ≈ 50～100 (a dotted line) ξ≈500～1000

  39. Chandra HEG Observation … Narrow Line Component • NGC5548 (Yaqoob, et al.,2001,ApJ,546,759) • Narrow Line • 6.40+-0.03keV • FWHM=4515 (+3525-2645)km/s • *) does not rule out broad component

  40. Disk Lines of Other Elements ? • Warm Absorber -> Disk (Emission) Line • Brandaurdi-Raymont et al., 2001, A&A, 365, L140

  41. Chandra data can be fitted with Warm Absorber Model (Lee,2001, astroph0101065)

  42. Disk Line or Fe-K Line • Fe-K Line is found in most of Radio Quiet AGNs • Eq. Width is anti-correlated with Lx • Broad Line Width and Red Wing are found in several Seyferts, which usually are interpreted with Line emission from several Rs • Little correlation between Line / Continuum is against the simple disk line model • Narrow Line component may be taken into account

  43. What can we suggest to VSOP2? • Disk Emission observed in X-rays … No apparent relation to Jet (VSOP’s Main Topic?) • What discriminates Radio Loud / Radio Quiet AGNs ? • Can VSOP(2) resolve accretion disk ? • CAUTION: Ultimate Higher Angular Resolution will be obtained in X-rays

  44. From http://maxim.gsfc.nasa.gov MAXIM mission (X-ray Interferometer) 100marcsec 0.3marcsec Also Note XMAS project in Japan

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