ASCA Observations of NLS1s

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ASCA Observations of NLS1s

• BH Mass from X-ray Variability
• and X-ray Spectrum
• K. Hayashida, K. Mori
• (Osaka University)

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Narrow Line Seyfert 1 (NLS1)

• Seyfert Type 1 whose Broad Emission Line Width is
  Narrow. (???)

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Statistical Properties
Narrow Hb Width
Rapid / Large Ampl. X-ray Variability
Steep Soft X-ray Spectrum
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BH Mass Estimation of NLS1

• X-ray Variability
• Application of the Method developed in Hayashida
  et al., 1998,ApJ500,p.642.
• Black Body Fit to Soft Component
• Classical Method in (X-ray) Astronomy

Preliminary Results were appeared in Hayashida,
1998(IAU Sympo 188), and Hayashida, 1999 (Adv. in
Space Res.).
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Mass Estimation from Variability

• Assumptions
• X-ray Variability of BHs (from SBHC to AGNs) is
  Similar to Each Other.
• Variability Time Scale is Proportional to System
  Size, i.e., BH Mass.
• Cyg X-1 BH 10 Mo
• Use Normalized Power Spectrum Density (NPSD)

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How to make a Normalized Power Spectral
Density(NPSD)

• Two BGD Subtracted Light Curves
• Short bin size16-256s
• Long bin size5760sec
• Short-gtNPSD for High Freq Long-gtNPSD for Low
  Freq.
• Normalized by Average Intensity2
• Combine Two NPSDs
• NPSD points are missed around 2x104 Hz.

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Time Scale and NPSD (1/2)
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Time Scale and NPSD (2/2)
Source B
Source A
fp(f)-plot Power per Log Frequency
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fP(f)-Plot BLS1 Cyg X-1
Cyg X-1
AGNs(BLS1)
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Lx vs Mvar for BLS1s
H0 75km/s/Mpc Lbol/Lx(2-10) 27.2 Is assumed
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Motivations/Supports

• Similarity between AGN and SBHC (White, et al.,
  1984, Inoue, 1989)
• NPSD of Cyg X-1 is stable at higher frequency
  part (Knee Frequency shifts.) (Belloni and
  Hasinger, 1990.)
• NPSD of GBHCs coincide at higher frequency parts.
  (Miyamoto et al., 1992)
• NPSD of X1608

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Constancy of NPSD
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NLS1 ASCA Sample

• 14NLS1
• Zw1, Ton S180, PHL1092, PKS0558-504, 1H0707-495,
  RE103439, NGC4051, PG1211143, Mrk766,
  PG1244226, IRAS13224-3809, PG1404226, Mrk478,
  Ark564.
• 9BLS1 s for Comparison
• MCG-6-30-15, NGC5548, Mrk841, Mkn509, 3C120,
  NGC3227) from ASCA
• MCG-6-30-15, NGC4151,NGC5506,ESO-G103,NGC5548
  from Ginga

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ASCA Light Curves of NLS1
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NPSDs of NLS1s
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1H0707-495 (1995Mar-gt1998May)

• Intensity Drop by factor of 6.
• NPSDs unchanged.

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f P(f) Plot NLS1 (ASCA)
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Lx vs Mvar (NLS1)
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Hb FWHM vs Mvar
BLS1 107-108Mo NLS1 105-107Mo
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Calibration Mass from BL width vs Mvar
Mrev and Mph from Wandel, A. et al., 1999
(astro-ph/9905224) )Mrev for NGC4051 is
preliminary (ct6.5days).
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Mvar v.s. Excess Variance
(Excess Variance from Turner et al., 1999)
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Summary-1

• We estimated BH masses of NLS1s from X-ray
  Variabiliy.
• BH Masses in NLS1s from X-ray variability
  distribute from 105 to 107 Mo, while those in
  BLS1 range 107-108Mo.
• Calibration to Mrev were Shown.

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X-ray Spectrum of NLS1s
2nd Method
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Problems on BB Fitting

• How perfect is the underlying Power Law ?
• Spectral Features / Warm Absorber / 1keV Feature.
• Is Blackbody fit perfect ? (Color Temp/Effective
  Temp)
• Calibration Uncertainty of ASCA (excess NH?)
• SIS-CCD Degradation Effect (Dark Frame Error etc.)

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kTBB vs Soft Excess Ratio
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BB Fit -gtArea-gtBH Size
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BB area size -gtBH size around 105-106Mo

• The soft component of NLS1s have simiar Emission
  Region Size BB luminosity.
• The soft component of the BLS1s (if they have
  similar one) are difficult to be detected.
• Does the BB area really correspond to the central
  BH ?

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MBBfit vs Mvar
1st vs 2nd
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MBBfit(0.5Rs) vs Mvar
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Can we reconcile the Contradiction ?

• For MBBfit lt Mvar
• Inclination Effect
• cos Factor MBBfit gives under-estimate
• Tc gt Te Effect
• MBBfit gives under-estimate, too.

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Extreme NLS1 Class/State ?

• For MBBfit gtMvar
• X-ray Variability of Extremely Enhanced Soft
  Components gt Variability Amplitude is Also
  Enhanced ?
• Mvar underestimation

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0.5Rs lt-gt Kerr BH lt-gt Slim Disk Solution
ADAF (Slim Disk)
Standard Disk
ADAF
From Mineshige et al., 1999 see also Abramowicz
1995.
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Summary-2

• Soft Component of NLS1s was fitted with a BB
  model with kT of 0.1-0.2keV.
• BH mass estimated about 105Mo (r3Rs) or
  105-106Mo (r0.5Rs) .
• Lbb exceeds LEdd for r3Rs, but not for r0.5Rs.
• MBBfit was compared with Mvar Contradiction of 2
  order of magnitudes was found. Possible
  reconciliation was discussed.

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Long Term Variability of NLS1s(1/2)
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Long Term Variability of NLS1s(2/2)
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NLS1s Personal View

• NLS1s have smaller BH of 105-107 Mo.
• In some of NLS1s, high mass flow rate makes near
  or super Eddington accretion.
• In the extreme high accretion rate
• Variability Amplitude is enhanced.
• Hard X-ray emission is suppressed.
• Mass flow rate changes with time scales of years,
  reflecting the smallness of system.
• NLS1Evolving Stage of Seyferts to BLS1.