slide1
Download
Skip this Video
Download Presentation
Introduction

Loading in 2 Seconds...

play fullscreen
1 / 16

Introduction - PowerPoint PPT Presentation


  • 78 Views
  • Uploaded on

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

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about 'Introduction' - avent


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.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
slide1
Multiwavelenth Observations Of Strong Flares From The TevBlazar 1ES 1959+650Reporter:倪嘉阳Arthor:H.Krawczynski, S.B. Hughes2013.10.08
introduction
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)
slide4
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

slide6
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
slide7
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
slide8
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
conclusion
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
ad