Quasi-Periodicity in the Parsec-Scale Quasi-Periodicity in the Parsec-Scale JetJet

of the Quasar 3C345of the Quasar 3C345- A High Resolution Study using VSOP and VLBA -- A High Resolution Study using VSOP and VLBA -

In collaboration with:

J.A. ZensusA. Witzel

T.P. KrichbaumA.P. Lobanov

E. Ros

Content of the TalkContent of the Talk

The Quasar 3C345OverviewObservationsKinematic study of the jetFlux density study of the jetMerging of GalaxiesThe model

Outlook

The Quasar 3C345The Quasar 3C345- Overview -- Overview -

z=0.595, m=16 arcsec scalescompact region at the base of a 4''jet; diffuse steep-spectrum

halo mas scales

VLBI monitoring since 1979 Þ long time study core-jet structure

core (D): unresolved, optically thick, flat spectrum, stationary (Bartel et al. 1986)jet: 11 components (C1-C11), different curved trajectories, variable superluminal speed (2-20c)

D C9 C8 C7

C5 C4 C3

4 Epochs: 1.6GHz VSOP

4 Epochs: 5GHz VSOP

7 Epochs: 22GHz VLBA

9+5 Epochs: 43GHz VLBA

Jet Kinematics: Core -ShiftJet Kinematics: Core -Shift

Jet Kinematics: Trajectory of Jet Kinematics: Trajectory of C7C7

Jet Kinematics: Trajectories of C8, Jet Kinematics: Trajectories of C8, C9C9

Jet Kinematics: Trajectories of C10, Jet Kinematics: Trajectories of C10, C11C11

Jet KinematicsKinematics: Trajectories

9 years later

Jet Kinematics: Ejection Position Jet Kinematics: Ejection Position AngleAngle

T = 8-10 years

P.A.ej = 2.6° ± 0.3° /year

Jet Parameters: Min. Lorentz FactorJet Parameters: Min. Lorentz Factor

Jet Parameters: Constant Lorentz Jet Parameters: Constant Lorentz FactorFactor

Jet Parameters: Increasing Jet Parameters: Increasing gg

Flux Density Evolution: Flux Density Evolution: C7/C8/C10/C11C7/C8/C10/C11

Trajectory part of Flux Density Trajectory part of Flux Density PeaksPeaks

Evolution of the Flux Density Evolution of the Flux Density PeaksPeaks

Merging of Galaxies Merging of Galaxies Þ Þ Binary Black Binary Black Holes? Holes?

Binary Black Hole ModelBinary Black Hole Model

Binary Black Hole ModelBinary Black Hole ModelBinary Black Hole model of Lobanov & Roland

2002:C7: Kinematic and flux density evolution

C5-to-C8: Obs: D P.A.ej = 28° ± 14° BBH: D P.A.ej = 27°

peak-to-peak: Obs: D P.A.ej = 26° ± 7° BBH: D P.A.ej = 30°

Results1 Three new ejected jet components C9, C10 and C11. 2 Different component trajectories but similarity of

the C5 and C8 trajectory: Equivalent points areabout 8-10 years later for C8 than for C5.

3 Component ejection angles vary: Quasi-periodicity of 8-10 years. Long-term variation of P.A.ej = 2.6° ± 0.3° / year

4 Acceleration of the jet components. Lorentz factor rises from 3 to 16.

5 Doppler factor rises from 5 to 30. 6 Angle to the line of sight changes down to: 3.5° > Q > 0.2°.7 Component flux density peaks due to Doppler boosting.8 Component flux density peaks show quasi-periodicity

with a period of about 9 years.9 Observations match with Binary Black Hole model

of Lobanov & Roland 2002: Orbital period in observers frame: 8.5 years. Precession period in observers frame: 125 years (2.9° / year)

Outlook1. Continue VLBI monitoring to pursue our intensive study of this

particular quasar.

3. Test the stationarity of the core:Phase-referencing program started with the VLBA to the nearby

quasar NRAO 512 (~ 0.5° apart) at 7 mm and 3 mm in 2002. 4. Test Binary Black Hole model with jet components C8 and C9.

2. Several observations have been made at l = 3 mm to supplement our extensive study at core distances smaller than 100 marcsec.

Flare Model, Lobanov & Flare Model, Lobanov & ZensusZensus

Lobanov & Zensus 1999

Spectral Index MapsSpectral Index Maps

ComponentsComponents

Core -ShiftCore -Shift

5/22Ghz: 0.182mas 5/43GHz: 0.254mas

Flux Density Evolution of C9Flux Density Evolution of C9

1.6

Precision of the TrajectoriesPrecision of the Trajectories

1.6

Precision of the TrajectoriesPrecision of the Trajectories

Dx @ 0.3 mas r @ 14 pc r @ 3 pc

1.6

Precision of the TrajectoriesPrecision of the Trajectories

Dx @ 0.4 mas

r @ 49 pc

r @ 3 pc

1.6

Precision of the TrajectoriesPrecision of the Trajectories

Small changes in the observed trajectories lead to

big differences in derived jet parameters! ÞNeed high-precision trajectories

The inner jet (C10-C7) of The inner jet (C10-C7) of 3C3453C345