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Radio quiet quasar main sequence - a hidden parameter behind it
B. Czerny, P. Du, J.-M. Wang, C. Wildy
Center for Theoretical Physics PAS Al. Lotników 32/46, 02-668 Warsaw, Poland
Active Galactic Nuclei: What's in a name?June 27 - July 1, 2016
ESO, Garching bei München, Germany
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Stellar Main Sequence
Herzschrung-Herschel diagram started as purely observational, based on some spectral indicators.
We now know that the true govering parameter is the star effective temperature, or, equivalently, the stelar mass
The width of the main sequence is related to age and metallicity
There are outliers, of course (AGB etc.), i.e. evolved stars not located on the main sequence any more
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PCA approach - Eigenvector 1Boroson & Green (1992) found a single parameter which is responsible for most of the dispersion in the observed properties of type 1 AGN.
AGN main sequence
?
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Early ideas on the driving parameter
The natural parameters of the accretion disk are:
Black hole massAccretion rate (Eddington ratio)Spin Inclination
Extinction (?)
Since we concentrate on the type 1 objects, inclination should not be a problem.
The obvious suspect: Eddington ratio
Boroson & Green (1992), Pounds et al. (1995),…. NLS1 concentrating in the right part of the diagram
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Many more sources
Simplified definition of the EV1
EV1 = R_FeII
R_FeII =
EW(FeII)/EW(Hbeta)
Observational progress with SDSS
Shen & Ho (2014)
L/LEdd
M_BH
i
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Where high L/Ledd sources are?
Lijiang data from Pu et al. 2016
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Trends in the 'uncorrected' sample
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Trends overplotted the 'corrected sample'
Lijiang high Eddington ratio objects
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The studied properties are predominantly:
Line kinematic width Line ratios
Logicaly, this should mostly depend on:
Inclination (line kinematic width) Shape of the SED (Spectral Energy Density)
And shape of the SED depends, if we use a simple disk model, on the maximum disk temperature
Starting from the theoretical side...
T_Eff_max^4 ~ M_BH Mdot/M_BH^3 f(spin)
~ L/L_Edd/M_BH f(spin)
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So the simple expectation for the key parameter is
Not just the Eddington ratio
but
the ratio of the Eddington ratio to the black hole mass
with some dispersion due to the spin
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Is it really working?There is a clrear relation between this new main sequence parameter and R_FeII but only for small values of R_FeII.
Data accuracy?
Or the SED peak does not depend on the new parameter for large values of R_FeII.
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An example – broad band modelling of REJ 1034+396
Not just the spin, but also disk corona/hot skin may cause the location of the SED maximum at the same position… But this happens only if the corona is optically thick.
Czerny et al. 2016
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Future work
Tests of dispersion for low values of R_FeII – good interpretation should decrease the dispersion around the main sequence
Better description of HWHM (Hbeta)
Observational determination of the SED maximum for selected quasars