060627 zamanov

OHP, june 2006: 

From Symbiotic stars to Quasars Radoslav K. Zamanov OHP, june 2006

in collaboration with: M.F. Bode (Liverpool, UK) P. Marziani (Padova, Italy) C.H.F. Melo (ESO & Chile) R. Bachev (Bulgaria) R.Konstantinova-Antova (Bulgaria) J.W. Sulentic (Alabama, USA) M. Calvani (Padova, Italy) A. Gomboc (Ljubliana, Slovenia): 

in collaboration with: M.F. Bode (Liverpool, UK) P. Marziani (Padova, Italy) C.H.F. Melo (ESO & Chile) R. Bachev (Bulgaria) R.Konstantinova-Antova (Bulgaria) J.W. Sulentic (Alabama, USA) M. Calvani (Padova, Italy) A. Gomboc (Ljubliana, Slovenia)

Slide3: 

Symbiotic stars are interacting binaries consisting of a red giant transferring mass onto a white dwarf.

Slide4: 

We are investigating the projected rotational velocities of the mass donors (red giants). Our aims are: To check theoretical prediction that the red giants in these binaries are co-rotating (for objects with known periods). To perform comparative analysis and to check if they are faster rotators (comparing with isolated giants and those in wide binary systems). To give clues for binary periods, individual mass loss rates, select candidates for X-ray observations.

Slide5: 

Observations: 40 symbiotic stars have been observed with the 2.2m telescope (ESO, La Silla) + FEROS spectrograph at resolution 48000. Our sample: All objects from the Symbiotic star catalogue with 12h<R.A.<24h, Dec. < +20, and brighter than V< 12.5 mag. From literature -12 northern symbiotic

Slide6: 

Examples of the CCF and the fitting gaussian. AS 316: v sin i = 9.8 ± 1.5 km/s Rapid rotator V417 Cen: v sin i = 75 ± 7.5 km/s R Aqr: only upper limit can be given (v sin i < 3.5 km/s) To measure the projected rotational velocity (v sin i) we used the CCF method and numerical template. The width of the CCF is connected (calibrated for FEROS) with the v sin i.

Slide7: 

The rotational period of the red giant versus the orbit period for 16 symbiotic stars in our sample with known orbital periods (all they are S-type). The solid line represents synchronization (Porb=Prot). Among these 16 objects there are two, which deviate considerably from co-rotation: CD-43 14304 and RS Oph. There are doubts that v sin i of CD-43 14304 could be wrong. RS Oph seems to be the only symbiotic system which is not synchronized.

Slide8: 

Results: 238 K2III-K5III stars have vsini in the interval from less than 1.0 km/s up to 6.7 km/s with mean vsini =1.70 km/s (median= 1.50 km/s) and standartd deviation of the sample = 0.90 km/s. The K giants of 8 S-type symbiotic stars with mass donors K2III-K5III have vsini in the interval from 4.5 up to 8.9 km/s with mean vsini=7.42 km/s (median=7.15 km/s) and stddev= 1.54 km/s. The Koslmogorov-Smirnov test gives a probability of 10-6 (K-S statistics =0.60) that both distributions are coming from the same parent population. This means that the K-giant mass donors of symbiotic stars rotate faster than isolated K-giants. Isolated giants spectral classes K2-K5 III K2-K5 III giants in symbiotic stars (238 objects from catalogues of v sin i) (7 objects, our measurements)

Slide9: 

Isolated M giants: 1.8 km/s < v sin i < 18.1 km/s, mean vsini =5.54 km/s (median=3.10 km/s), stddev=5.22 km/s. M-giants in symbiotics: 3.0 < v sin i < 52 km/s, mean vsin i=9.07 km/s (median=7.72 km/s), stddev=8.81 km/s. The Kolmogorov-Smirnov test gives a probability of 0.0074 (K-S statistic =0.54) that both distributions are coming from the same parent population. This means that from statistical point of view the M giants mass donors of symbiotic stars rotate faster than isolated M-giants (at confidence level 99%). Isolated giants spectral classes M0-M7 III M0-M7 III giants in symbiotic stars (12 objects from catalogues of v sin i) (28 objects, our measurements mostly)

Slide10: 

Reasons for faster rotation of the giants in symbiotic systems: - synchronization, if the time spent by the mass-losing star on the giant branch is longer than the synchronization time. In all symbiotic systems with orbital period Porb ≤ 100 years tidal interaction overcomes the angular momentum loss by the wind (Soker 2002). - accretion during the MS phase of the present red giant: the more massive star in the system, the present WD, had transferred material at the stage when it had been red giant. - backflowing material: hot component prevents part of the mass blown by the giant from acquiring the escape velocity for the binary system. This fraction of mass may acquire angular momentum, and if it is accreted back by the giant, it spins-up its envelope. - angular momentum dredge-up when convective envelope approaches the core region of the giant. - planet engulfment during the giant phase.

Slide11: 

FUTURE WORK: To strengthen our results, more data on M type isolated giants and more v sin i measurements of K type mass donors in symbiotics are desirable. 1. 17 more symbiotics have been observed with the same FEROS+2.2m 2. We intend to expand our sample with northern and fainter symbiotic stars. ELODIE at Bulgarian Observatory “Rozhen” can play important role.

From White dwarfs to Quasars : 

From White dwarfs to Quasars

Slide13: 

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?) (d0.1 pc in low luminosity AGN; d 104 Rg) Radio Jet along Disk Axis (from Padovani & Urry 1992) Massive Black Hole Molecular Torus Relativistic Jet Accretion Disk

Slide14: 

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

Slide15: 

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.

Slide16: 

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)= 97090 km s-1 (Zamanov & Marziani, 2002, ApJ 571, 77)

Slide17: 

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.

Slide18: 

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 .

Slide19: 

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.

Slide20: 

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 symbiotic stars (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, 303, 308

Slide21: 

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 two symbiotic stars 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

Slide22: 

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 !

[OIII] “blue outliers” among the AGNs: 

[OIII] “blue outliers” among the AGNs

Slide24: 

However the quasar spectra are not similar! Composite Quasar Spectra from the Sloan Digital Sky Survey (Van den Berk et al., 2001 AJ 122, 549).

Slide25: 

Examples of subtraction of FeII complex around H and [OIII] lines. Left panels represent the continuum subtracted spectra and best FeII fit. Left panels represent fit to the H broad component. The difficulties of FeII subtraction are coming from S/N ratio, wavelength coverage, presence/absence of HeII4686, HeI 4471, etc. from Marziani, Sulentic, Zamanov, et al., 2003, ApJS, 145, 199

Slide26: 

H spectral region of the “blue outliers” after the deredshift and subtraction of the FeII template. Spectra are normalized with respect to the normal continuum and arbitrary constant added. Solid curves correspond to the subtraction of IZw1-based empirical template, and dot-dashed curves to the subtraction of a theoretical template (Sigut & Pradham 2003, ApJ 145, 15). Vertical lines indicate the position of H, [OIII]4959 and [OIII]5007. The difference in radial velocities between [OIII] lines and H is obvious. from Zamanov, Marziani, Sulentic, et al., 2002, ApJ 576, L9

Slide27: 

Forbidden [OIII] emission arises in the NLR of AGNs. This emission has now been partly resolved in the nearest AGN, where the geometry of the line-emitting gas has been found to be far from spherically symmetric. This suggest that measures of the integrated [OIII] emission may correlate with source orientation to the line of sight. At the same time it is generally believed that radial velocity measures of the narrow emission lines (e.g narrow component of H and [OIII] 4959, 5007) provide a reliable measure of the systemic, or rest-frame, velocity. Several observations, however, indicate that the NLSy1 prototype I Zw1 shows an blue shift of the [OIII] lines V -500 km/s relatively to other rest frame indicators (HI 21cm, molecular CO emission). We measured the radial velocity difference (V) between the H and [OIII] 4959, 5007 lines in 187 objects (our sample 215 objects, 7 with no detectable [OIII] emission, 16 with poorly defined H peak).

Slide28: 

Histogram showing the distribution of the radial velocity difference between [OIII]5007 and top of H. As it is visible in most of the objects |V| < 300 km s-1. However there are some objects, with V down to -1000 km s-1. The values range from –950 to +280 km/s with average <V>= -30 km/s and sample standard deviation 135 km/s. Typical measurement error is 50 km/s. from Zamanov, Marziani, Sulentic, et al., 2002, ApJ 576, L9

Slide29: 

Radial velocity difference between H and [OIII]5007 versus the FWHM(H BC). Vertical dotted line marks the boundary of the NLSy1 galaxies. Vertical dashed line separates population A and B sources. In our sample of 215 objects we detected 7 objects with V  -300 km s-1. from Zamanov, Marziani, Sulentic, et al., 2002, ApJ 576, L9

Slide30: 

Location of the outliers in the FWHM(HBC) versus W(FeII)/W (HBC) diagram (the optical E1 diagram). They are not randomly distributed (2D_KS test gives probability 0.990 – 0.999). from Zamanov, Marziani, Sulentic, et al., 2002, ApJ 576, L9

Slide31: 

A sketch representing “blue outlier”. The [OIII] lines originate from the wind, the disk is visible face-on, and the receding part of the wind is obscured from the disk. In calculations we adopted cone half-opening angle 850, with the line of sight oriented at 150, with respect to the cone axis. The receding part of the flow is assumed to be fully obscured by an optically thick disk.

Slide32: 

Upper panels: CIV 1549 and [OIII]5007 profiles of Ton 28. Lower panels: CIV 1549 and [OIII]5007 outflow model profiles, for optically thin gas moving at approximately the local escape velocity. from Zamanov, Marziani, Sulentic, et al., 2002, ApJ 576, L9

Slide33: 

For our sample, we calculated the masses using reverberation mapping studies(Kaspi et al. 2000). Our sample covers: magnitude range 20 < MB <27 BH mass 7 < log(M/M) <10 a well defined strip of L/LEdd = 0.02 - 1.00. The blue outliers are located between objects with highest L/LEdd ratio. L/LEdd of “blue outliers”

Slide34: 

The luminosity-to-mass ratio versus the mass of the BH. If the blue outliers are oriented nearly pole-on the effect of orientation could play a role. It could be as high as M0.4. Even in these case the blue outliers remain between objects accreting at higher Eddington ratio. (Bear in mind that a lot of other objects also have to be moved in the same way).

Slide35: 

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”.

In future:: 

Search for blue-shifted [OIII] among higher redshift quasars (IR data). Searching for orientation indicators. Exploration of the connection between the L/M ratio and blue shifts. In future:

Slide37: 

THE END