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Model | RA(°) | DEC(°) | Semi Major Axis (°) | Semi Minor Axis (°) | Pos.Ang.(°) |
283,990 | 1,355 | 0,300 | 0,190 | 327,000 | |
Pass 6 | 284.015(+/-0.004) | 1.392(+/-0.005) | 0.335(+0.117 -0.086) | 0.207 (+0.023 -0.021) | 330+/- 25 |
Pass 7 | 284.000(+/-0.006) | 1.374(+/-0.006) | 0.332(+0.109/-0.079) | 0.205 (+0.021/-0.017) | 327 +/-22 |
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We fitted the source using pointlike above 300GeV to prevent contamination at low energy.
Here are the summary of the Pass 6 analysis :
The best fit obtained using pointlike gave the following parameters :
Int. Flux (>100MeV) | -1 X Index | Lower Limit (MeV) | Upperlimit(GeV) | TS |
|---|---|---|---|---|
8.19+/-1.71(stat) | 1.65+/-0.06(stat) | 100 | 100 | 49.73 |
Table. 5. Parameters of the best fit obtained using pointlike on Pass6.
Those gave the following SED :
Fig. 10 SED obtained with pointlike using Pass
The We obtained the following SED and best fit are those obtained using Pass 7 :
Fig. 10 11 : SED obtained using gtlike above 300 MeV. The best fit is show in yellow.
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IRFS | Int. Flux (>100MeV) | -1 X Index | Lower limit (MeV) | Upper limit (GeV) | TS | gal |
|---|---|---|---|---|---|---|
Pass 7 | 5.67+/-0.65+/-3.2 | 1.65+/-0.27+/-0.31 | 100 | 100 | 28.1 | 1.09 |
Table. 56. Parameters of the best fit obtained using gtlike.
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Adam constructed a time-dependent one-zone SED model with constant expansion velocity, and assuming a distance of 9 kpc. The modeling only need an IC component.
Fig. 11 12 show the SED modeling constructed by Adam. Blue point are those obtained with HESS data and the green one using ASCA observation. IC components : stellar (dot), IR (medium-dashed) and scattering on
CMB (long-dashed)
Preliminary fit:
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This efficiency is consistent with what is expected from Ackerman et al. 2011 (the order of magnitude of the percent) as is shown in the following picture : 
Fig. 12 13 ?-ray Luminosity of the Pulsar Wind Nebulae as a function of the spin-down
luminosity of the associated pulsar. All the pulsar wind nebulae detected by Fermi are
associated with young and energetic pulsars. Pulsar wind nebulae detected by Fermi are
marked with red stars. Blue squares represent pulsars for which GeV ?-ray emission
seems to come from the neutron star magnetosphere, and not from the nebula.
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I would like to show 3 figures which are th Fig. 4, 8 and 1112.
The draft is coming soon.
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