3-11 July 2007
Merida, Mexico
Mexico/General timezone
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OG 2.2

Place

Location: Merida, Mexico
Room: Uxmal + Tulum (Holiday Inn)
Date: 6 Jul 08:30 - 10:06

Timetable | Contribution List

Displaying 8 contributions out of 8
Type: Oral Session: OG 2.2
Track: OG.2.2
Observations with H.E.S.S. in 2004-2005 revealed a new source of very high-energy (VHE) gamma-rays above 100 GeV -- HESS J1825-137 -- extending mainly to the south of the energetic pulsar PSR B1823-13. While the direction of the VHE gamma-ray emission with respect to the pulsar is similar to that of the asymmetric X-ray PWN G18.0-0.2 in this system, the RMS extension of HESS J1825--137 is >0.2 ... More
Presented by Dr. Stefan FUNK on 6/7/2007 at 14:06
Type: Oral Session: OG 2.2
Track: OG.2.2
In this work we study the individual contribution to diffuse $\gamma$-ray emission from the secondary products in hadronic interactions generated by cosmic rays (CRs), in addition to the contribution of neutral-pions via the decay into two gamma rays. For that purpose we employ the Monte Carlo particle collision code DPMJET3.04 to determine the multiplicity spectra of various secondary p ... More
Presented by Prof. Martin POHL on 6/7/2007 at 14:54
Type: Oral Session: OG 2.2
Track: OG.2.2
The H.E.S.S. source J1809-193 was discovered in 2006 in data of the Galactic Plane survey, followed by several re-observations. It shows a hard gamma-ray spectrum and the emission is clearly extended. Its vicinity to PSR J1809-1917, a high spin-down luminosity pulsar powerful enough to drive the observed gamma-ray emission, makes it a plausible candidate for a Pulsar Wind Nebula. On the other ... More
Presented by Nukri KOMIN on 6/7/2007 at 13:54
Type: Oral Session: OG 2.2
Track: OG.2.2
Nonlinear kinetic theory of cosmic ray acceleration in supernova remnants is used to investigate the properties of Kepler's SNR and, in particular, to predict the gamma-ray spectrum expected from this SNR. Observations of the non-thermal radio and X-ray emission spectra as well as theoretical constraints for the total supernova explosion energy are used to constrain the astronomical and part ... More
Presented by Dr. Leonid KSENOFONTOV on 6/7/2007 at 13:30
Type: Oral Session: OG 2.2
Track: OG.2.2
The H.E.S.S. 2004-2005 survey of the Galactic Plane at energies above 200 GeV had revealed a number of pulsar wind nebulae candidates, including the remarkable source HESS J1825-137. Spatially resolved spectral measurements of this source gave the first evidence of an energy-dependent morphology which was interpreted as being due to the cooling of relic electrons cumulated throughout pul ... More
Presented by Dr. anne LEMIERE on 6/7/2007 at 13:42
Type: Oral Session: OG 2.2
Track: OG.2.2
The binary system LS 5039 was serendipously with the High Energy Stereoscopic system (H.E.S.S.) during the scan of the inner galactic plane in 2004. Deeper observations were carried out in 2005, and brought clear evidence for TeV emission perodicity. This is the highest energy periodic source known so far. The observed flux modulation is attributed to a modulated absorption of the VHE gamma ... More
Presented by Mr. Mathieu DE NAUROIS on 6/7/2007 at 14:30
Type: Oral Session: OG 2.2
Track: OG.2.2
Many of the recently discovered galactic very high-energy gamma-ray sources are associated with Pulsar Wind Nebulae (PWN), which is the most populous source category at TeV energies. Extended synchrotron nebulae seen from these objects in the X-ray band is a footprint of the relativistic winds, generated by the young energetic pulsars, which interact with the matter ejected by the supernova ex ... More
Presented by Dr. Alexander KONOPELKO on 6/7/2007 at 14:18
Type: Oral Session: OG 2.2
Track: OG.2.2
PSR B 1259-63/SS2883 is a binary system consisting of a 48ms radio pulsar orbiting a Be star with a period of 3.4y in a highly eccentric orbit (e = 0.87). The system was first detected in very-high-energy (VHE) gamma-rays by H.E.S.S. around the last periastron passage in March 2004 (March 7, 2004). These observations established PSR B1259-63/SS2883 as the first variable galactic source in the ... More
Presented by Mr. Matthias KERSCHHAGGL on 6/7/2007 at 14:42
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