Optical spectra of quasars in the context of Eigenvector-1

R. Zamanov

Bologna Dec. 5, 2002

in collaboration with:

P. Marziani (Padova, I)J.W. Sulentic (Alabama, USA)M. Calvani (Padova, I)R. Bachev (Alabama, USA)

D. Dultzin-Hacyan (UNAM, Mexico)

CONTENT:

• Eigenvector-1 correlations• Optical FeII emission of AGNs• Average quasar spectra in the context of

Eigenvector-1 diagram• “Blue outliers” among AGNs – objects in which

the [OIII] lines are blue shifted relatively to the H with 300-1000 km/s.

• White dwarfs with spectra similar to quasars and physical drivers of this similarity

The main constuituents of an

Active Galactic Nucleus

Central massive Black Hole (MBH~106-109 M)

Geometrically Thin Accretion Disk (d 3 Rg 105Rg)

Thick molecular torus (d 1 pc)

Line emitting gas (clouds?) (d0.1 pc in low luminosity AGN; d 104 Rg)

Radio Jet along Disk Axis

(from Padovani & Urry 1992)

Massive Black Hole

Molecular Torus

Relativistic Jet

AccretionDisk

FeII emission

Average Quasar Spectrum: Francis et al. 1991

However the quasar spectra are not similar!

Composite Quasar Composite Quasar Spectra from the Sloan Spectra from the Sloan Digital Sky SurveyDigital Sky Survey (Vanden Berk et al., (Vanden Berk et al., 20012001 AJAJ 122122, , 549549).).

Eigenvector-1 correlation space

During the last decade, several investigations of AGNs During the last decade, several investigations of AGNs emission lines emphasized the importance of a set of emission lines emphasized the importance of a set of correlations conventionally called “Eigenvector-1”. They are correlations conventionally called “Eigenvector-1”. They are related to the principal component analysis of the spectral related to the principal component analysis of the spectral properties of the Palomar-Green quasars performed by properties of the Palomar-Green quasars performed by Boroson & Green (1992). This correlation space provide and Boroson & Green (1992). This correlation space provide and optimal discrimination between different type of quasars and optimal discrimination between different type of quasars and could play a role for AGNs similar to H-R diagram in regard to could play a role for AGNs similar to H-R diagram in regard to stars (Sulentic, Calvani, Marziani 2001, stars (Sulentic, Calvani, Marziani 2001, The Messenger 104, The Messenger 104, 2525). ). Physical drivers of Eigenvector-1 can be: Physical drivers of Eigenvector-1 can be:

(i) the source luminosity-to-mass ratio (L/M) convolved (i) the source luminosity-to-mass ratio (L/M) convolved with the orientation (Marziani et al. with the orientation (Marziani et al. 20012001, , ApJApJ 558558, , 553553) or) or

(ii) the fraction of the Edington luminosity at which the (ii) the fraction of the Edington luminosity at which the source emits (L/Lsource emits (L/LEddEdd) and the black hole mass (Boroson ) and the black hole mass (Boroson 20022002, , ApJApJ 565565, , 7878).).

FWHM(H)[LIL kinematics]

ratio R(FeII)=EW(FeII)/EW(H)

[LIL em. Regions physical conditions]

soft-X photon index Soft

[SED]

3D parameter space for Boroson & Green 1992 + Marziani et al. 1996 sample

from Sulentic, Marziani, Dultzin-Hacyan, 2000, ARA&A 38, 521

Interpretation of the Eigenvector 1 correlation space

AGN “MAIN SEQUENCE”

Outliers Outliers are allBAL QSOs

Population A

Population B

skmMM

LHFWHM su

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where Q is the number of hydrogen ionizing photons.

,10

103.34

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62

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The reverberation mapping studies (Kaspi et al. 2000) :

Ionization parameter (Marziani et. 2001):

The FeII-H (optical Eigenvector-1) diagram. The theoretical lines for the range of masses and L/M ratios expected for low redshift quasars (Zamanov & Marziani 2002, ApJ 571, L77).

Our data set :

The data set includes CCD spectra of 216 Seyfert 1 galaxies and low-redshift quasars (z0.8). Spectra were obtained for studies of H region with 2 meter class telescopes: ESO (1.5m), San Pedro Martir (2.2m), Calar Alto (2.2m), KPNO (2.2m), Asiago (1.82m).

The spectra were taken with:- similar instrumental setups yielding resolution FWHM 4-7 A, - similar (rest frame) wavelength coverage (4300 - 5100 AA), - typical S/N 20 –50 in the continuum, only spectra with S/N > 12

have been used.

The sample has an average absolute B magnitude MB -23.72.0 .

FeII emission in the optical spectra

Before to analyse the HBefore to analyse the H and [OIII] lines we need to and [OIII] lines we need to subtract FeII emission. subtract FeII emission.

The template based on I The template based on I Zw1 spectrum (Boroson & Zw1 spectrum (Boroson & Green 1992) allows us to Green 1992) allows us to satisfactorily subtract the satisfactorily subtract the FeIIFeIIoptopt emission to about emission to about 98% of the the spectra of 98% of the the spectra of the whole sample.the whole sample.

In the figure is shown the In the figure is shown the successful rendering of the successful rendering of the FeIIFeIIoptopt emission by our emission by our template, once scaled and template, once scaled and broadened, for three broadened, for three objects with very different objects with very different like width. like width.

Examples of Examples of subtraction of FeII subtraction of FeII complex around Hcomplex around H and [OIII] lines. Left and [OIII] lines. Left panels represent the panels represent the continuum continuum subtracted spectra subtracted spectra and best FeII fit. Left and best FeII fit. Left panels represent fit panels represent fit to the Hto the H broad broad component. The component. The difficulties of FeII difficulties of FeII subtraction are subtraction are coming from S/N coming from S/N ratio, wavelength ratio, wavelength coverage, coverage, presence/absence of presence/absence of HeII4686, HeI 4471, HeII4686, HeI 4471, etc. etc.

from Marziani, Sulentic, Zamanov, et al., 2003, ApJS, accepted

FWHM : FWHM : FeIIFeIIoptopt – H – Hβ correlationβ correlation

•Pop. APop. A. (FWHM < 4000 km/s ): (FWHM < 4000 km/s ): There is a tight correlation There is a tight correlation between the FWHM of Hbetween the FWHM of HββBCBC and FeII, namely 1:1. This and FeII, namely 1:1. This implies that both emissions came from the same BLR. implies that both emissions came from the same BLR.

• Pop. BPop. B.. (FWHM > 4000 km/s): (FWHM > 4000 km/s): Even in this case the Even in this case the correlation seems real, but FWMH(Hcorrelation seems real, but FWMH(HββBCBC) exceeds the FeII) exceeds the FeIIoptopt one. one.

R Pearson = 0.693, N =69, P

= 8.5e-9

RPearson = 0.882, N = 43, P = 7.3e-9

from Bongardo, Zamanov, Marziani, Calvani, Sulentic, 2002, astro-ph/0211418

A special case: A special case:

IRAS 07598+6508IRAS 07598+6508This intriguing object shows a This intriguing object shows a FIR excess and its location in FIR excess and its location in the E1 diagram is peculiar. It the E1 diagram is peculiar. It is interesting to note that is interesting to note that FWHM(HFWHM(HββBCBC) = 5000 ± 400 km ) = 5000 ± 400 km ss-1-1 and FWHM(FeII and FWHM(FeIIλ4570λ4570) = ) = 2000 ± 1300 km s2000 ± 1300 km s-1-1. The good . The good S/N ratio and the strength of S/N ratio and the strength of the FeIIthe FeIIoptopt emission, along emission, along with the large EWwith the large EW(H(HββBCBC) make ) make this result especially striking. this result especially striking. The strong blueward The strong blueward asymmetry of the BC of asymmetry of the BC of HHβ β suggest that the broadening suggest that the broadening is due to Balmer emission is due to Balmer emission associated to associated to (1)(1) the highly the highly blueshifted CIV at 1549 Å blueshifted CIV at 1549 Å emission and emission and (2)(2) a narrower a narrower unshifted component unshifted component associated to low ionization associated to low ionization emissionemission..

from Bongardo, Zamanov, Marziani, Calvani, Sulentic, 2002, astro-ph/0211418

The most straightforward implication is that the FeIIThe most straightforward implication is that the FeIIoptopt emission mechanism is probably the same in almost all AGN emission mechanism is probably the same in almost all AGN and that FeIIand that FeIIoptopt is mainly from the zone of the BLR where Hβ is mainly from the zone of the BLR where Hβ is also emitted. In fact the FWHM of FeIIis also emitted. In fact the FWHM of FeIIoptopt in Pop. B objects in Pop. B objects seems to be narrower than that of Hβ. It I possible that seems to be narrower than that of Hβ. It I possible that FeIIFeIIoptopt emission in Population B sources comes from the emission in Population B sources comes from the outer part of Hβ emitting region, where the ionization outer part of Hβ emitting region, where the ionization degree is lower.degree is lower.

Average quasar spectra

Prediction of unification models on spectral properties of Seyfert 1

and quasars:

One point somewhere here

We present median AGN spectra for fixed regions of the We present median AGN spectra for fixed regions of the E1 (optical) parameter space [FWHM(Hβ) vs. equivalent E1 (optical) parameter space [FWHM(Hβ) vs. equivalent width ratio Rwidth ratio RFeiiFeii=W(Fe II λ4570)/W(Hβ)]. We suggest that =W(Fe II λ4570)/W(Hβ)]. We suggest that

an E1-driven approach to median/average spectra an E1-driven approach to median/average spectra emphasizes significant differences between AGNs and emphasizes significant differences between AGNs and offers more insights into AGN physics than a single-offers more insights into AGN physics than a single-population median/average spectrum derived from a population median/average spectrum derived from a large and heterogeneous sample of sources. large and heterogeneous sample of sources.

Optical parameter plane of E1. The lines indicate the adopted binning.

from Sulentic, Marziani, Zamanov, et al. , 2002, ApJ 566, L71

Average quasar spectra along E1 sequence Sulentic, Marziani, Zamanov, et al. 2002 ApJ 566, L71

Optical parameter plane of E1. This is the largest sample yet displayed in an E1 context. The lines indicate the adopted binning.

Composite quasar spectra following the spectral beams Composite quasar spectra following the spectral beams defined in Eigenvector-1 diagram. Left panel: before FeII defined in Eigenvector-1 diagram. Left panel: before FeII subtraction. Right panel: same composite spectra with FeII subtraction. Right panel: same composite spectra with FeII emission subtracted.emission subtracted.

Continuum subtracted HContinuum subtracted H composite line profiles for the composite line profiles for the different E1 parameter bins. The different E1 parameter bins. The solid colored lines show the Hsolid colored lines show the H BC after subtraction of NC. A BC after subtraction of NC. A Lorenztian fit (red line) is Lorenztian fit (red line) is superposed on the NLSy1, A1, superposed on the NLSy1, A1, and A2 profiles. The individual and A2 profiles. The individual components of a double components of a double Gaussian (green lines) and Gaussian (green lines) and resultant fit are shown for B1 resultant fit are shown for B1 and B1+. and B1+. We find that the Hβ We find that the Hβ broad component line profile broad component line profile changes along the E1 sequence changes along the E1 sequence in FWHM, centroid shift, and in FWHM, centroid shift, and profile asymmetry. While objects profile asymmetry. While objects with FWHM(Hβwith FWHM(HβBCBC)<4000 km s)<4000 km s-1-1

are well fitted by a Lorentz are well fitted by a Lorentz function, AGNs with function, AGNs with FWHM(HβFWHM(HβBCBC)>4000 km s)>4000 km s-1-1 are are

better fitted if two broad-line better fitted if two broad-line components are used: a components are used: a ``classical'' broad-line ``classical'' broad-line component and a very component and a very broad/redshifted component. broad/redshifted component.

from Sulentic, Marziani, Zamanov, et al. , 2002, ApJ 566, L71

The Lorentz profileThe Lorentz profile is consistent with emissionis consistent with emission

from an extended accretionfrom an extended accretion disk. This reinforces thedisk. This reinforces the

suggestion that the LILsuggestion that the LIL spectra in population Aspectra in population A sources sources arise from aarise from a disk. The situation isdisk. The situation is less clear for less clear for populationpopulation B sources, where theB sources, where the Eddington ratio may beEddington ratio may be

much lower. There ismuch lower. There is good evidence that sometimesgood evidence that sometimes only only one of theone of the two emission components istwo emission components is present in present in population Bpopulation B sources (a pure BLRsources (a pure BLR or a pure veryor a pure very broad broad line region [VBLR]). line region [VBLR]).

Can theCan the double-Gaussian model that isdouble-Gaussian model that is needed to needed to fit populationfit population B (and radio-loud) profilesB (and radio-loud) profiles be physically be physically justified? Severaljustified? Several lines of evidence pointlines of evidence point toward the toward the existence ofexistence of a VBLR at thea VBLR at the inner edge of the inner edge of the BLR (Corbin BLR (Corbin 1997, ApJS 113, 245 and ApJ 485, 517). 1997, ApJS 113, 245 and ApJ 485, 517). Emission from Emission from this regionthis region may be thought ofmay be thought of as a sort ofas a sort of inner large inner large covering factorcovering factor "boundary layer" where gas"boundary layer" where gas begins to begins to become opticallybecome optically thick.thick.

[OIII] “blue outliers” among the AGNs

Forbidden [OIII] emission arises in the NLR of AGNs. This Forbidden [OIII] emission arises in the NLR of AGNs. This emission has now been partly resolved in the nearest AGN, emission has now been partly resolved in the nearest AGN, where the geometry of the line-emitting gas has been found where the geometry of the line-emitting gas has been found to be far from spherically symmetric. This suggest that to be far from spherically symmetric. This suggest that measures of the integrated [OIII] emission may correlate measures of the integrated [OIII] emission may correlate with source orientation to the line of sight. At the same time with source orientation to the line of sight. At the same time it is generally believed that radial velocity measures of the it is generally believed that radial velocity measures of the narrow emission lines (e.g narrow component of Hnarrow emission lines (e.g narrow component of H and [OIII] and [OIII] 4959, 4959, 5007) provide a reliable measure of the systemic, or 5007) provide a reliable measure of the systemic, or rest-frame, velocity. rest-frame, velocity.

Several observations, however, indicate that the Several observations, however, indicate that the NLSy1 prototype I Zw1 shows an blue shift of the [OIII] lines NLSy1 prototype I Zw1 shows an blue shift of the [OIII] lines VV -500 km/s relatively to other rest frame indicators (HI -500 km/s relatively to other rest frame indicators (HI 21cm, molecular CO emission).21cm, molecular CO emission).

We measured the radial velocity difference (We measured the radial velocity difference (V) V) between the Hbetween the H and [OIII] and [OIII] 4959, 4959, 5007 lines in 187 objects 5007 lines in 187 objects (our sample 215 objects, 7 with no detectable [OIII] (our sample 215 objects, 7 with no detectable [OIII] emission, 16 with poorly defined Hemission, 16 with poorly defined H peak). peak).

Histogram showing the Histogram showing the distribution of the radial distribution of the radial velocity difference velocity difference between [OIII]between [OIII]5007 and 5007 and top of Htop of H. As it is visible . As it is visible in most of the objects |in most of the objects |V| < 300 km sV| < 300 km s-1-1. . However there are some However there are some objects, with objects, with V down to V down to -1000 km s-1000 km s-1-1..

The values range from –The values range from –950 to +280 km/s with 950 to +280 km/s with average <average <V>= -30 km/s V>= -30 km/s and sample standard and sample standard deviation deviation 135 km/s. 135 km/s. Typical measurement Typical measurement error is error is 50 km/s.50 km/s.

from Zamanov, Marziani, Sulentic, et al., 2002, ApJ 576, L9

HH spectral region of the spectral region of the “blue outliers” after the “blue outliers” after the deredshift and subtraction deredshift and subtraction of the FeII template. Spectra of the FeII template. Spectra are normalized with respect are normalized with respect to the normal continuum to the normal continuum and arbitrary constant and arbitrary constant added. Solid curves added. Solid curves correspond to the correspond to the subtraction of IZw1-based subtraction of IZw1-based empirical template, and dot-empirical template, and dot-dashed curves to the dashed curves to the subtraction of a theoretical subtraction of a theoretical template (Sigut & Pradham template (Sigut & Pradham 2002, astro-ph/0206096). 2002, astro-ph/0206096). Vertical lines indicate the Vertical lines indicate the position of Hposition of H, [OIII], [OIII]4959 4959 and [OIII]and [OIII]5007. The 5007. The difference in radial difference in radial velocities between [OIII] velocities between [OIII] lines and Hlines and H is obvious. is obvious.

from Zamanov, Marziani, Sulentic, et al., 2002, ApJ 576, L9

Radial velocity Radial velocity difference between Hdifference between H and [OIII]and [OIII]5007 versus 5007 versus the FWHM(Hthe FWHM(H BC). BC). Vertical dotted line Vertical dotted line marks the boundary of marks the boundary of the NLSy1 galaxies. the NLSy1 galaxies. Vertical dashed line Vertical dashed line separates population A separates population A and B sources. and B sources.

In our sample of In our sample of 215 objects we detected 215 objects we detected 7 objects with 7 objects with V V -300 -300 km skm s-1-1. .

from Zamanov, Marziani, Sulentic, et al., 2002, ApJ 576, L9

Location of the outliers Location of the outliers in the FWHM(Hin the FWHM(HBCBC) versus ) versus W(FeII)/W (HW(FeII)/W (HBCBC) diagram ) diagram (the optical E1 diagram). (the optical E1 diagram). They are not randomly They are not randomly distributed (2D_KS test distributed (2D_KS test gives probability 0.990 – gives probability 0.990 – 0.999). 0.999).

from Zamanov, Marziani, Sulentic, et al., 2002, ApJ 576, L9

[OIII][OIII]5007 shifts with respect to5007 shifts with respect to the top of the top of H H ( ( underlying galaxy underlying galaxy systemic velocitysystemic velocity ? ?)) . As it is visible the NLR kinematics is changing . As it is visible the NLR kinematics is changing along E1 sequencealong E1 sequence

Low W([OIII]5007)

High EW[OIII]5007)

Low EW([OIII]5007)

From Marziani, Zamanov, Calvani, et al.From Marziani, Zamanov, Calvani, et al. 200 2003, Mem SAIt, in press). 3, Mem SAIt, in press).

A sketch representing A sketch representing “blue outlier”. The [OIII] “blue outlier”. The [OIII] lines originate from the lines originate from the wind, the disk is visible wind, the disk is visible face-on, and the receding face-on, and the receding part of the wind is part of the wind is obscured from the disk.obscured from the disk.

In calculations we adopted In calculations we adopted cone half-opening angle cone half-opening angle 858500, with the line of sight , with the line of sight oriented at 15oriented at 1500, with , with respect to the cone axis. respect to the cone axis. The receding part of the The receding part of the flow is assumed to be fully flow is assumed to be fully obscured by an optically obscured by an optically thick disk.thick disk.

Upper panels:Upper panels: CIV CIV 1549 and 1549 and [OIII][OIII]5007 profiles 5007 profiles of Ton 28. of Ton 28.

Lower panels:Lower panels: CIV CIV 1549 and 1549 and [OIII][OIII]5007 outflow 5007 outflow model profiles, for model profiles, for optically thin gas optically thin gas moving at moving at approximately the approximately the local escape velocity. local escape velocity.

from Zamanov, Marziani, Sulentic, et al., 2002, ApJ 576, L9

For our sample, we calculated For our sample, we calculated the masses using reverberation the masses using reverberation mapping studies(Kaspi et al. mapping studies(Kaspi et al. 2000). Our sample covers:2000). Our sample covers:

• magnitude range 20 < Mmagnitude range 20 < MBB <27 <27• BH mass 7 < log(M/MBH mass 7 < log(M/M) <10 ) <10 • a well defined strip ofa well defined strip of

L/LL/LEddEdd = 0.02 - 1.00. = 0.02 - 1.00.

The blue outliers are located The blue outliers are located between objects with highest between objects with highest L/LL/LEddEdd ratio. ratio.

L/LL/LEdd Edd of “blue of “blue outliers”outliers”

The luminosity-to-mass ratio The luminosity-to-mass ratio versus the mass of the versus the mass of the BH. If the blue outliers BH. If the blue outliers are oriented nearly pole-are oriented nearly pole-on the effect of on the effect of orientation could play a orientation could play a role. It could be as high role. It could be as high as as MM0.4. Even in 0.4. Even in these case the blue these case the blue outliers remain between outliers remain between objects accreting at objects accreting at higher Eddington ratio. higher Eddington ratio.

(Bear in mind that a lot of (Bear in mind that a lot of other objects also have other objects also have to be moved in the same to be moved in the same way).way).

The “blue outliers” among AGNs seems to represent a special case of high L/M ratio, face-on view, and very compact NLR.

They seems to be radio quiet analog of the core dominated radio loud quasars.

(!) Not all radio quiet AGNs visible pole-on are “blue outliers”.

From White dwarfs to Quasars

Figure: UV – region spectral similarity between CH Cyg and I Zw. The middle spectrum is produced by scaling and broadening of the CH Cyg spectrum to imitate the emission lines widths of IZw1.

I Zw 1 – narrow line Seyfert 1 galaxy, widely used as template for all quasars. Mass of the

black hole ~107 M .

CH Cyg – symbiotic with ~1M WD

CH Cyg

CH Cyg (broad.)

I Zw 1

From Zamanov & Marziani, 2002, ApJ 571, 77

Comparison between the optical spectra in the H - H region of the interacting binaries CH Cyg, MWC 560 and the low redshift quasar I Zw 1. A clear similarity between the emission lines is visible. Practically every emission feature visible in the spectrum of IZw1 has corresponding emission line in the spectra of CH Cyg and MWC 560.

The optical emission line spectra of CH Cyg and MWC 560 are subtracted, broadened and scaled to imitate I Zw 1. This standard procedure is widely used for the emission line measurements of AGN, using I Zw 1 itself as a template (Boroson & Green 1992, Marziani et al. 1996). After this processing, good identity is achieved with the spectrum of I Zw 1. Our best fit corresponds to a width FWHM(FeII)= 97090 km s-1 (Zamanov & Marziani, 2002, ApJ 571, 77)

The HI and FeII lines of AGNs are coming from the so-called broad-line region. This poorly understood region is thought to be within 1 pc from the central (supermassive) black hole.

The clear spectral similarity means that in objects like MWC 560 and CH Cyg we are observing a scaled down version of the famous broad line region of quasars.

JETS:

Jet velocity : ~1000-1500 km s-1 in CH Cyg (Taylor et al. 1986, Crocker et al. 2001) and 1000-6000 km s-1 in MWC 560 (Tomov et al. 1992)

Galactic microquasars (accreting stellar mass black holes):0.26c SS 433 (Margon 1984)0.5c Cyg X-3 (Marti et al. 2001) 0.9c GRS 1915+105 (Mirabel & Rodriguez 1999)

Consistent with an overall picture in which the jet velocity is of the same order of the escape velocity (Livio 2001) : Vesc(WD)= 0.02 c .

JET ENERGY :

MWC 560 and CH Cyg: the jets are probably result of the propeller action of a magnetic white dwarf (Mikolajewski et al. 1996) = extraction of rotational energy from the compact object.

Quasars – the jet energy is coming from extraction of energy and angular momentum from a rotating black hole via the Blandford & Znajek (1977) mechanism.

Microquasars – black hole - Blandford & Znajek (1977) mechanism

neutron star - ??? (The jets of Crab are the most pure case of extraction of rotational energy, even without accretion).

The jets of CH Cyg and MWC 560 represent probably a low energy (non-relativistic) analog of the jets of quasars and

microquasars, having a similar energy source – the extraction of rotational energy from the central compact object.

We propose to name these objects NANOQUASARS.

NANOQUASARS : white dwarfs with jets and quasar-like spectra , representing the low energy (non-relativistic) analog of quasars and microquasars.

Why “nano” ?

Denomination: quasars microquasars nanoquasars

(greek) = nano (ital.) = enana (spanish) = dwarf (engl.)

Optical spectra demonstrating the spectral similarity and the changes of the FWHM(H). The filled circles refer to NLSy 1 galaxies, which are supposed to have systematically lower black hole masses. The two triangles indicate the nanoquasars (CH Cyg and MWC 560). As it could be expected they are located outside of the AGN population but from the side of NLSy1.

from Zamanov & Marziani, 2003, ASP Conf.Ser, in press

The FeII-H (Eigenvector-1) diagram. The lines are plotted (from top to bottom) for MBH=1.109

M, MBH=5.107 M, and white dwarf mass MWD=1.4 M. The L/M ratio was running in the limits 2.5-4.6 for MBH=1.109 M; 2.5-5.1 for MBH=5.107 M; 3.0-3.9 for white dwarf mass MWD=1.4 M. The ratio (L/M) is in solar units with the solar value (L/M)=1.92 ergs s-1 g-1.

The position of nanoquasars on the diagram reinforces the interpretation of Boroson &Green Eigenvector-1 as a mainly result of L/M ratio. The efficiency of accretion along with some other factors could play some minor role.

from Zamanov & Marziani, 2002, ApJ 571, L77

Similarity of the CIV profile of the nova-like variable RW Sex, with those of broad absorption line quasars.

The high mass X-ray binaries

Can we observe a scaled down version of the quasar broad line region in wind-fed X-ray binaries ?

In the most cases they have additional source of ionization – a hot primary OB star, i.e the ionization conditions are quite different from symbiotics and AGNs.

It will be extremely interesting to detect a stellar mass black hole accreting from the wind of red giant (although very difficult from the evolutionary point of view). A black hole accreting from wind of red giant will (probably) represent good imitation of quasar !

SUMMARY:

1. We are investigating optical E1 on base of the largest sample yet displayed in an E1 context.

2. The average quasar spectra in E1 emphasize the differences between AGNs and offers more insights into physics than a single population spectrum.

3. The FWHM(FeII) is slightly different from FWHM(H) in pop.B, although it is very similar in general.

4. We detected objects in which different system velocity indicators gives inconsistent results. We detected in 3% of our sample that the [OIII] lines are shifted with >300 km/s (“blue outliers”).

5. We found striking similarity between the emission lines of two accreting WDs and quasars. This gives us the unique possibility to consider the optical E1 diagram using objects less massive by a factor of ~107. Our results reinforce the interpretation of E1 as driven mainly by the L/M ratio.

In future:

1. Extension of our sample to higher redshift quasars (IR data).

2. Searching for orientation indicators.

3. Theoretical lines and distributions of objects onto the other Eigenvector-1 plans.

4. We would like to distinguish the influence of MBH and L/M ratio onto the emission line properties.

THE END

Both Radio Loud and Radio Quiet (30% RQ; 70% RL in our sample)Predominantly Radio QuietRadio Loudness

LargerLowerW([OIII])

LargerLowerW(H )

More frequent high amplitude variability

Possible long term variability

and flickeringOptical Variability

Redward Asymmetric

Affected by a Very Broad redshifted component?

Douple peaked or highly shifted single peaked H profiles

Lorentzian (see Figure), symmetric save for spectral type A3 where a blueward

asymmetry becomes prominentH line profile shape

LowerLargerW(FeII)

Mainly “mini-BAL QSOs”?Preferred occurrence of low-z (and presumably higher z) of BAL QSOs

BAL QSOs

(see poster at this meeting)

Large EW of [OIII]4959,5007 and general radial velocity

agreement with H

[OIII]4959,5007 has low EW and frequent blue shifts with respect to H

Forbidden Narrow Lines

(see Figure)

Only slightly broader than, or equal to FWHM(H).

Larger than FWHM(H) also by a factor of several

HeII4686 emission FWHM

Less than FWHM(H) by 20%.Equal to FWHM(H). FeII4570 emission FWHM

CIV1549 unshifted or shifted to the red as H

Flatter, soft2, no soft X ray excess

Population B

[FWHM(H) 4000 Km s-1]

Large systematic blueshift of CIV1549CIV1549

Steeper, soft3Soft X ray spectra index

Population A

[FWHM(H) < 4000 Km s-1]

skmMM

LHFWHM su

su

/4350)( 15.035.0

where Q is the number of hydrogen ionizing photons. We will use for typical AGN continuum f=0.39, =1.221016 (Laor et al.1997), and for nanoquasars we will adopt (Teff=8500 K) corresponding to f=110-5, =3.481015.

,10

103.34

4.007.116

62

su

su

Hz

e

MM

Lf

ncr

QU

The reverberation mapping studies (Kaspi et al. 2000) :

The ionization parameter (Marziani et. 2001):

Other analogies:

Orientation of the source (FWHM and the orientation)

FWHM in quasars is (probably) connected with the orientation.In a flattened configuration (Marziani et al. 2001) :

)sin()0()( iFWHMHFWHM

where i is the inclination angle.

Face on (MWC 560) FWHM(H)=110 km/sEdge on (CH Cyg) FWHM(H)=200 km/s

This is in qualitative agreement with the expectations for quasars, that a face-on object must have lower FWHM .

Figure. The FeII-H (optical Eigenvector-1) diagram. First theoretical grid proposed (Marziani et al. 2001, ApJ 558, 553). In this grid is the position depends on the L/M ratio and the orientation, supposing that all quasars have equal masses log (M/M)=8.

Immediate results:

Narrow-Line Seyfert 1 Galaxies (NLSy1; FWHM(H) 2000 km s-1) represent an extremum in the parameter space, not a disjoint peculiar class of AGN (and they are NOT Seyfert 2!). Not really FeII strong emitters, NLSy1 are discriminated among radio quiet AGN by their small W(H). Steep spectrum radio-loud sources represent the opposite extremum. No ultra-soft excess has been revealed in core-dominated RL AGN, which show Soft 2.5, therefore better discriminated in the Soft - R(FeII) than in the R(FeII)-FWHM(H)

plane. There is a remarkable continuity and correlation in line parameters between NLSy1 and RQ AGN with broader Balmer lines up to FWHM(H) 4000 km s-1. Perhaps a more significant distinction is between AGN with FWHM(H) 4000 km s-1, which we may call “Population A” and AGN for which FWHM(H) > 4000 (“Population B”). Population A includes 65% of PG quasars but almost no radio loud AGN. Population B encompass RQ quasars that show optical properties rather similar to RL AGN. If EW(FeII) is used instead of R(FeII), Pop. A and B are separated into two disjoint “clouds” of RQ AGN.

Two main (sets of) correlations systematize the spread of observed properties among AGN:

(1) The so-called Eigenvector 1 correlations; Originally identified by Boroson & Green (1992) by a

Principal Component Analysis (PCA) of the specral properties of 82 Palomar-Green quasars, dominated by an anticorrelation between the strength of FeII and [OIII]4959,5007;

E1 involves primarily Low Ionization Lines (LIL)HI Balmer lines, MgII2800, FeII multipletsDoes not depend on the quasar luminosityRelationship between optical parameters and soft X-rays:

Wang et al (1996) Optimal 3 dimensional correlation space

The “Baldwin effect,” Anticorrelation between HIL rest-frame equivalent width

and continuum luminosiyInvolves primarily High Ionization Lines (LIL) CIV 1549, HeII (1640 and 4686), OVI 1034.