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Introduction

Multiwavelenth Observations O f S trong F lares F rom The Tev Blazar 1ES 1959+650 Reporter: 倪嘉阳 Arthor:H.Krawczynski , S.B. Hughes 2013.10.08. Introduction. Detection of strong TeV γ -ray flares from the BL Lac object 1ES 1959+650

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Introduction

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  1. Multiwavelenth Observations Of Strong Flares From The TevBlazar 1ES 1959+650Reporter:倪嘉阳Arthor:H.Krawczynski, S.B. Hughes2013.10.08

  2. Introduction • Detection of strong TeVγ-ray flares from the BL Lac object 1ES 1959+650 • Intensive target of opportunity radio, optical, X-ray, and TeVγ-ray observations • There was six well-established TeVBlazars at that time(see table 1)

  3. 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

  4. 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

  5. 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

  6. 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

  7. Gamma-ray observations • Whipple 10 m Cerenkov telescope • The HEGRA system of five Cerenkov telescopes

  8. 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

  9. Detailed light curves • Divide the data into four epochs • Epoch 1(May 16-25;MJD 52410-52419): γ-ray and X-ray fluxes seem to be correlated • Epoch 2(May 26-June 21;MJD 52420-52446) • the strong ophanγ-ray flare on June 4,shown in more detail • Epoch 3(July 5-19;MJD 52460-52474) • Epoch 4(July 31-August 14;MJD 52486-52500)

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

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

  12. 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 1959+650, together with a simple one-zone SSC model

  13. 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

  14. Correlations between emission parameters and black hole mass indicators

  15. 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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