1 / 16

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

avent
Télécharger la présentation

Introduction

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related