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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 1851992

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



  • 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)

Introduction 1851992

  • 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

Data sets and data reduction

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

Introduction 1851992

  • 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

Introduction 1851992

  • 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

Introduction 1851992

  • Gamma-ray observations

  • Whipple 10 m Cerenkov telescope

  • The HEGRA system of five Cerenkov telescopes

Results of the multiwavelenth campaign

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

Detailed light curves

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)

Flux correlations in different energy bands

Flux correlations in different energy bands

the correlation between simultaneously measured γ-ray and X-ray fluxes during the full campaign

X ray hardness intensity correlation

X-ray hardness-intensity correlation

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

Spectral energy distribution and ssc modeling

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

The orphan ray flare in the frame of ssc models

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

Correlations between emission parameters and black hole mass indicators

Correlations between emission parameters and black hole mass indicators



  • 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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