ASCA Observations of NLS 1 s BH Mass

ASCA Observations of NLS 1 s BH Mass from X-ray Variability and X-ray Spectrum Kiyoshi Hayashida (Osaka University)

AGN=Accretion onto Super Massive BH n Huge Amount of Emission (L=10411047 erg/s) from Small Region <1 Rs=3 x(M/MQ) km= 10 -7 (M/106 Mo) pc <1”=190 pc @z=0. 01 (H 0=75) <Radio Observation->1 marcsec <(X-ray) Variabiliuty v=R/t. . R<ct

Time Scale vs BH Mass

Mass of Black Hole Steller BH Mass in Binary System => Mass Function + Inclination n BH Mass in AGNs – Dynamical Mass (e. g. BLR M=v 2 r/G) – Blue Bump = Accretion Disk Spectrum – X-ray Variability n

Significance of BH Mass Emission Mechanisim – Eddington Luminosity LEdd= 1. 3 x 1038 (M/Mo) erg/s n Cosmological Evolution – d. M/dt=L/e c 2={(L/Ledd) /e} (M/Mo)x 1. 3 x 1038 <M/(d. M/dt)=4. 5 x 107 (e/0. 1) / (L/Ledd) yr n

Mass Estimation from X-ray Variability From Normalized Power Spectrum n 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 n

ASCA Light Curves of BLS 1

How to make a Normalized Power Spectral Density(NPSD) n Two BGD Subtracted Light Curves – Short: bin size=16256 s – Long: bin size=5760 sec n n Short->NPSD for High Freq Long->NPSD for Low Freq. – Normalized by Average Intensity^2 Combine Two NPSDs – NPSD points are missed around 2 x 104 Hz.

Time Scale and NPSD (1/2)

Time Scale and NPSD (2/2) Source A Source B fp(f)-plot : Power per Log Frequency

f. P(f)-Plot: BLS 1 + Cyg X-1

Lx vs Mvar for BLS 1 s

Motivations/Supports Similarity between AGN and SBHC (White, et al. , 1984, Inoue, 1989) n NPSD of Cyg X-1 is stable at higher frequency part (Knee Frequency shifts. ) (Belloni and Hasinger, 1990. ) n NPSD of GBHCs coincide at higher frequency parts. (Miyamoto et al. , 1992) n NPSD of X 1608 n

Constancy of NPSD

Application/Extension NGC 4258(Ishisaki et al. ) n M 81 (Iyomoto et al. , 1999) n LLAGN and Sy 2 (Awaki et al. 1999) n NGC 4395 (Iwasawa et al. , 1999) n

Narrow Line Seyfert 1 (NLS 1) n Seyfert Type 1 whose Broad Emission Line Width is Narrow. (? ? ? ) 2021/12/19

X-ray Studies with ROSAT Prototype=IRAS 13224 -3809 n Steep Soft X-ray Index G=4. 4± 0. 2 n Rapid & Large Amplitude Variability n Common for NLS 1 at Some Level Boller et al. , 1997

ASCA Studies n Two Components Spectrum : – Soft Component ~BB k. T=0. 10. 2 ke. V – Hard Tail above 2 ke. V

Statistical Properties (Strong Fe. II Line) Narrow Hb FWHM Steep Soft Xray Spectrum (Steep Hard X-ray Index) (Spectral Feature at 1 ke. V) n Rapid / Large Amplitude X-ray Variability See Boller et al. , 1996, Leighly, K. , 1999, Turner et al. , 1999 and reference therein.

BH Mass Estimation of NLS 1 X-ray Variability – Application of the Method developed in Hayashida et al. , 1998. n Black Body Fit to Soft Component – Classical Method in (X-ray) Astronomy n Preliminary Results were appeared in Hayashida, 1998(IAU Sympo 188), and Hayashida, 1999 (Adv. In Space Research).

NLS 1 From ASCA Archive 14 NLS 1 Zw 1, Ton S 180, PHL 1092, PKS 0558504, 1 H 0707 -495, RE 1034+39, NGC 4051, PG 1211+143, Mrk 766, PG 1244+226, IRAS 13224 -3809, PG 1404+226, Mrk 478, Ark 564. n 6 BLS 1 s(MCG-6 -30 -15, NGC 5548, Mrk 841, Mkn 509, 3 C 120, NGC 3227) were also analyzed for their X-ray variability. n

ASCA Light Curves of NLS 1

NPSDs of NLS 1 s

1 H 0707 -495 Case (1995 Mar>1998 May) n n Regardless of Intensity Drop by factor of 6, NPSDs agree well. Supporting its use for the Scale Measure.

f P(f) Plot : NLS 1 (ASCA)

Lx vs Mvar (NLS 1)

FWHM vs Mvar BLS 1: 107 -108 Mo NLS 1: 105 -107 Mo

Calibration of Mvar to Mass from BL width Mrev and Mph from Wandel, A. et al. , 1999 (astro-ph/9905224) 19 AGNs *)Mrev for NGC 4051 is preliminary (ct=6. 5 days). 2021/12/19

Mvar v. s. Excess Variance Normalized Excess variance (Nandra et al. , 1997) = Integration of NPSD =(Variability Coefficient)^2 (Ogwara et al. , 1977) 2021/12/19 (Excess Variance from Turner et al. , 1999)

Summary-1 We estimated central BH masses of NLS 1 s from X-ray Variabiliy. n Mass from X-ray variability distributes from 105 to 107 Mo, contrasting the those for BLS 1 ranges 107 -108 Mo. n *) Calibrations/Supports were Shown, supporting the Mvar gives (at least) order ofmagnitude estimation. n

Intermission

X-ray Spectrum of NLS 1 s

Problems on BB Fitting – How perfect is the underlying Power Law ? – Spectral Features / Warm Absorber / 1 ke. V Feature. – Is Blackbody fit perfect ? (Color Temp/Effective Temp) – Calibration Uncertainty of ASCA (excess NH? ) – SIS-CCD Degradation Effect (Dark Frame Error etc. ) 2021/12/19

k. TBB vs Soft Excess Ratio

BB Fit ->Area->BH Size

BB area size ->BH size = around 105 -106 Mo n n n The soft component of NLS 1 s have simiar Emission Region Size & BB luminosity. The soft component of the BLS 1 s (if they have similar one) are difficult to be detected. Does the BB area really correspond to the central BH ?

MBBfit vs Mvar

MBBfit(0. 5 Rs) vs Mvar

Can we reconcile the Contradiction ? n For MBBfit < Mvar – Geometry Effect <cos Factor … MBBfit gives underestimate – Tc > Te Effect < MBBfit gives under-estimate, too. 2021/12/19

Extreme NLS 1 Class/State ? n For MBBfit >Mvar – X-ray Variability of Extremely Enhanced Soft Components => Variability Amplitude is Also Enhanced ? <Break in Variability Scaling ? –c. f. SBHC High/Low State – Dopper Boosting with large q

0. 5 Rs <-> Kerr BH <-> Slim Disk Solution ADAF (Slim Disk) Standard Disk ADAF 2021/12/19 From Mineshige et al. , 1999 see also Abramowicz 1995.

Summary-2 n n Soft Component of NLS 1 s can be fitted with BB model. BB Temperature distributes 0. 1 -0. 2 ke. V BH mass estimated with the assumption r=3 Rs yields super Eddington luminosity, r=0. 5 Rs does not. MBBfit was compared with Mvar; Contradiction of 2 order of magnitudes was found in some sources. Possible reconciliation was discussed.

Long Term Variability of NLS 1 s(1/2)

Long Term Variability of NLS 1 s(2/2) 0. 5 -2 ke. V Flux 2 -10 ke. V Flux

NLS 1 s : Tentative Hypothesis n n n NLS 1 s have smaller BH of 105 -107 Mo. In some of NLS 1 s, high mass flow rate makes near or super Eddington accretion. In the extreme high accretion rate – Variability is enhanced. – Hard X-ray emission is suppressed Mass flow rate (compared to critical rate) changes with time scales of years, reflecting the smallness of MBH. NLS 1=Evolving Stage of AGNs to BLS 1