P ROBING THE MAGNETIC FIELD OF 3C 279 by Sebastian Kiehlmann on behalf of the Quasar Movie Project team Max Planck Institute for Radio Astronomy, Auf dem.

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Presentation transcript:

P ROBING THE MAGNETIC FIELD OF 3C 279 by Sebastian Kiehlmann on behalf of the Quasar Movie Project team Max Planck Institute for Radio Astronomy, Auf dem Hügel 69, Bonn, Germany

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN i.Polarization of 3C 279 ii.The 180° ambiguity iii.Polarization of 3C 279 iv.Conclusions I

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN II. Polarization of 3C Fig. 1a: Optical, linear polarization degree of 3C 279

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN II. Polarization of 3C Fig. 1b: Optical, linear polarization degree and EVPA of 3C 279 Optical electric vector position angle (EVPA) degree of linear polarization

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN II. Polarization of 3C Fig. 1b: Optical, linear polarization degree and EVPA of 3C 279 objectEVPA rotationtime interval explanationreference OJ °7 d Helical motion in a helical magnetic field Kikuchi et al., 1988 BL Lac240 °5 dMarscher et al., 2008 PKS °50 dMarscher et al., C 279  300 °60 dLarionov et al., C 279  208 °12 dBent jetAbdo et al., 2010 γ- ray flaring

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN Assumption: smooth variation Question: – Valid assumption? – Reliability? III. The 180° ambiguity 4 Fig. 2a: Sketched EVPA curve Fig. 2b: Sketched modified EVPA curve

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN Method 1: III. The 180° ambiguity III.a Smoothing methods 5 Method 2:

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN III. The 180° ambiguity III.c Test 2: assumption of smoothness 6 Fig. 4a: Sketched cells of the random walk process

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN III. The 180° ambiguity III.c Test 2: assumption of smoothness 7 Fig. 4b: Sketched cells of the random walk process

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN III. The 180° ambiguity III.c Test 2: assumption of smoothness 8 Fig. 5a: Random EVPA variation

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN III. The 180° ambiguity III.c Test 2: assumption of smoothness 9 Fig. 5b: Random EVPA variation, smoothed 1,000,000 simulations Method 1:Method 2: > 99.5 %> 98.5 % 43 %

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN III. The 180° ambiguity III.c Test 2: assumption of smoothness 10 Fig. 5b: Random EVPA variation, smoothed 1,000,000 simulations Method 1:Method 2: > 99.5 %> 98.5 % 43 % 1 %

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN III. The 180° ambiguity III.c Test 2: assumption of smoothness 11 Fig. 5c: Random EVPA variation, smoothed, p-t-p variation 1,000,000 simulations Method 1:Method 2: > 99.5 %> 98.5 % 43 % 1 %

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN III. The 180° ambiguity III.c Test 2: assumption of smoothness 12 Fig. 5c: Random EVPA variation, smoothed, p-t-p variation 1,000,000 simulations Method 1:Method 2: > 99.5 %> 98.5 % 43 % 1 %

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN Method 1:Method 2: > 99.5 %> 98.5 % 43 % 0 % 0.1 %0.3 % 76 %98 % 18 °/d15 °/d 1 % III. The 180° ambiguity III.c Test 2: assumption of smoothness 13 Fig. 5c: Random EVPA variation, smoothed, p-t-p variation 1,000,000 simulations

↓ Random walk simulation ↓ ↓ 3C 279 observation (optical) ↓

↓ Random walk simulation ↓ ↓ 3C 279 observation (optical) ↓

↓ Random walk simulation ↓ ↓ 3C 279 observation (optical) ↓

↓ Random walk simulation ↓ ↓ 3C 279 observation (optical) ↓

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN IV. Polarization of 3C 279 IV.a EVPA smoothness 15 Fig. 6a: 3C 279 optical polarization EpochEVPA I↓32(5)no

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN 15 Fig. 6b: 3C 279 optical polarization EpochEVPA I↓32(5)no II↑ IV. Polarization of 3C 279 IV.a EVPA smoothness

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN 15 Fig. 6c: 3C 279 optical polarization EpochEVPA I↓32(5)no II↑ III↓ IV. Polarization of 3C 279 IV.a EVPA smoothness

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN 15 Fig. 6d: 3C 279 optical polarization EpochEVPA I↓32(5)no II↑ III↓ IV↑ IV. Polarization of 3C 279 IV.a EVPA smoothness

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN 15 Fig. 6e: 3C 279 optical polarization EpochEVPA I↓32(5)no II↑ III↓ IV↑ V↑ IV. Polarization of 3C 279 IV.a EVPA smoothness

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN 15 Fig. 6f: 3C 279 optical polarization EpochEVPA I↓32(5)no II↑ 2-6yes III↓ IV↑ V↑ VI↑ IV. Polarization of 3C 279 IV.a EVPA smoothness

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN 15 Fig. 6g: 3C 279 optical polarization EpochEVPA I↓32(5)no II↑ 2-6yes III↓ IV↑ V↑ VI↑ VII↓10.5(8)yes IV. Polarization of 3C 279 IV.a EVPA smoothness

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN 16 Fig. 7a: Sketched jet model Fig. 8: 3C 279 LCs (V+R) and opt. pol. IV. Polarization of 3C 279 IV.b Interpretation

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN 17 IV. Polarization of 3C 279 IV.b Interpretation Fig. 7b: Sketched jet model Fig. 8: 3C 279 LCs (V+R) and opt. pol.

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN 18 IV. Polarization of 3C 279 IV.c Gamma-ray-flaring Fig. 9: 3C 279 γ-ray light curve, optical light curves and polarization

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN 19 Fig. 10: 3C 279 mm and optical EVPA IV. Polarization of 3C 279 IV.d mm polarization

S EBASTIAN K IEHLMANN, D IPL.-P HYS. M AX -P LANCK I NSTITUT FÜR R ADIOASTRONOMIE, B ONN V. Conclusions 20 → no globally bending jet → helical motion in a helical magnetic field

Special thanks to the QMP collaborators: T. Savolainen (PI), S.G. Jorstad, F. Schinzel, K.V. Sokolovsky, I. Agudo, M. Aller, L. Berdnikov, V. Chavushyan, L. Fuhrmann, M. Gurwell, R. Itoh, J. Heidt, Y.Y. Kovalev, T. Krajci, O. Kurtanidze, A. Lähteenmäki, V.M. Larionov, J. León-Tavares, A.P. Marscher, K. Nilson, the AAVSO, the Yale SMARTS project and all the observers. Acknowledgements: SK was supported for this research through a stipend from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Max Planck Institute for Radio Astronomy in cooperation with the Universities of Bonn and Cologne. Data from the Steward Observatory spectropolarimetric monitoring project were used. This program is supported by Fermi Guest Investigator grants NNX08AW56G, NNX09AU10G, and NNX12AO93G. We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research.