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Multiwavelenth Observations Of Strong Flares From The Tev Blazar 1ES 1959+650 Reporter: 倪嘉阳 Arthor:H.Krawczynski, S.B. Hughes 2013.10.08.

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Presentation on theme: "Multiwavelenth Observations Of Strong Flares From The Tev Blazar 1ES 1959+650 Reporter: 倪嘉阳 Arthor:H.Krawczynski, S.B. Hughes 2013.10.08."— Presentation transcript:

1 Multiwavelenth Observations Of Strong Flares From The Tev Blazar 1ES Reporter: 倪嘉阳 Arthor:H.Krawczynski, S.B. Hughes

2 Introduction Detection of strong TeV γ-ray flares from the BL Lac object 1ES Intensive target of opportunity radio, optical, X-ray, and TeV γ-ray observations There was six well-established TeV Blazars at that time(see table 1)

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4 Long flaring phases can be recognized in three sources Mrk 501 flared in 1997 but showed only modest fluxes thereafter Flaring phases offer ideal opportunities to study these objects

5 Data sets and data reduction Radio observations  UMRAO at 4.8 and 14.5 GHz between 2002 May and August 9  Additional flux density measurements: VLA of the NRAO

6 Optical observations (two optical data sets)  0.4m telescope at Boltwood Observatory, using V, R, and I broadband filters  0.7m telescope at the Abastmani Observatory in Georgia, using an R filter for all observations

7 X-ray observations  3-25 keV data from the PCA on board the RXTE satellite  Standard procedure to reduce the data to get the light curves and spectra

8 Gamma-ray observations  Whipple 10 m Cerenkov telescope  The HEGRA system of five Cerenkov telescopes

9 Results of the multiwavelenth campaign Analyse of every figure For analyzing the X-ray flux variability, compute the e- folding times: Shortest e-folding times Analyze photon index variations

10 Detailed light curves Divide the data into four epochs Epoch 1(May 16-25;MJD ): γ-ray and X-ray fluxes seem to be correlated Epoch 2(May 26-June 21;MJD ) the strong ophan γ-ray flare on June 4,shown in more detail Epoch 3(July 5-19;MJD ) Epoch 4(July 31-August 14;MJD )

11 Flux correlations in different energy bands the correlation between simultaneously measured γ-ray and X-ray fluxes during the full campaign

12 X-ray hardness-intensity correlation The correlation between 3- 25keV X-ray photon index and the 10 keV flux

13 Spectral energy distribution and SSC modeling X-ray emission: synchrotron self-Compton(SSC) mechanism Γ-ray emission: inverse Compton scattering of synchrotron photons The radio-to-γ-ray SED of 1ES , together with a simple one-zone SSC model

14 The orphan γ-ray flare in the frame of SSC models It is not possible to produce an orphan γ-ray flare by moving the high-energy cutoff of accelerated electrons to higher energies Adding a low energy electron population succeeds in producing an orphan γ-ray flare Postulating a second, dense electron population within a small emission region

15 Correlations between emission parameters and black hole mass indicators

16 conclusion Presenting evidence for an “orphan” γ-ray flare without an X-ray counterpart There are several ways to explain the orphan flare Multiple-Component SSC Models External Compton Models Magnetic Field Aligned along Jet axis Proton Models It cannot be explained with conventional one- zone SSC model


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