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

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)

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

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

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

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

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 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 )

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

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

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

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