Home > Publications database > Deeper H.E.S.S. observations of Vela Junior (RX J0852.0−4622): Morphology studies and resolved spectroscopy |
Report/Journal Article | PUBDB-2019-00149 |
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2018
EDP Sciences
Les Ulis
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Please use a persistent id in citations: doi:10.1051/0004-6361/201630002 doi:10.3204/PUBDB-2019-00149
Report No.: arXiv:1611.01863
Abstract: Aims. We study γ-ray emission from the shell-type supernova remnant (SNR) RX J0852.0−4622 to better characterize its spectral properties and its distribution over the SNR.Methods. The analysis of an extended High Energy Spectroscopic System (H.E.S.S.) data set at very high energies (E > 100 GeV) permits detailed studies, as well as spatially resolved spectroscopy, of the morphology and spectrum of the whole RX J0852.0−4622 region. The H.E.S.S. data are combined with archival data from other wavebands and interpreted in the framework of leptonic and hadronic models. The joint Fermi-LAT-H.E.S.S. spectrum allows the direct determination of the spectral characteristics of the parent particle population in leptonic and hadronic scenarios using only GeV-TeV data.Results. An updated analysis of the H.E.S.S. data shows that the spectrum of the entire SNR connects smoothly to the high-energy spectrum measured by Fermi-LAT. The increased data set makes it possible to demonstrate that the H.E.S.S. spectrum deviates significantly from a power law and is well described by both a curved power law and a power law with an exponential cutoff at an energy of Ecut = (6.7 ± 1.2stat ± 1.2syst) TeV. The joint Fermi-LAT-H.E.S.S. spectrum allows the unambiguous identification of the spectral shape as a power law with an exponential cutoff. No significant evidence is found for a variation of the spectral parameters across the SNR, suggesting similar conditions of particle acceleration across the remnant. A simple modeling using one particle population to model the SNR emission demonstrates that both leptonic and hadronic emission scenarios remain plausible. It is also shown that at least a part of the shell emission is likely due to the presence of a pulsar wind nebula around PSR J0855−4644.Key words: astroparticle physics / gamma rays: general / acceleration of particles / cosmic rays / ISM: supernova remnants★ A FITS image of the region of interest and two text files describingthe H.E.S.S. spectrum of RX J0852.0–4622 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/612/A7† Deceased.
Keyword(s): gamma ray: emission ; model: hadronic ; particle: acceleration ; HESS ; spectral ; one-particle ; supernova ; pulsar ; GLAST ; VHE
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Deeper H.E.S.S. Observations of Vela Junior (RX J0852.0-4622) : Morphology Studies and Resolved Spectroscopy
[10.3204/PUBDB-2017-00446]
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