Search: onr:"swepub:oai:DiVA.org:lnu-33979" > HESS J1818-154, a n...
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001 | oai:DiVA.org:lnu-33979 | |
003 | SwePub | |
008 | 140424s2014 | |||||||||||000 ||eng| | |
009 | oai:DiVA.org:su-102980 | |
024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:lnu:diva-339792 URI |
024 | 7 | a https://doi.org/10.1051/0004-6361/2013229142 DOI |
024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-1029802 URI |
040 | a (SwePub)lnud (SwePub)su | |
041 | a engb eng | |
042 | 9 SwePub | |
072 | 7 | a ref2 swepub-contenttype |
072 | 7 | a art2 swepub-publicationtype |
100 | 1 | a Abramowski, A.4 aut |
245 | 1 0 | a HESS J1818-154, a new composite supernova remnant discovered in TeV gamma rays and X-rays |
264 | c 2014-02-06 | |
264 | 1 | b EDP Sciences,c 2014 |
338 | a print2 rdacarrier | |
500 | a AuthorCount:219; | |
520 | a Composite supernova remnants (SNRs) constitute a small subclass of the remnants of massive stellar explosions where non-thermal radiation is observed from both the expanding shell-like shock front and from a pulsar wind nebula (PWN) located inside of the SNR. These systems represent a unique evolutionary phase of SNRs where observations in the radio, X-ray, and gamma-ray regimes allow the study of the co-evolution of both these energetic phenomena. In this article, we report results from observations of the shell-type SNR G15.4+0.1 performed with the High Energy Stereoscopic System (H. E. S. S.) and XMM-Newton. A compact TeV gamma-ray source, HESS J1818-154, located in the center and contained within the shell of G15.4+0.1 is detected by H. E. S. S. and featurs a spectrum best represented by a power-law model with a spectral index of -2.3 +/- 0.3(stat) +/- 0.2(sys) and an integral flux of F(>0.42 TeV) = (0.9 +/- 0.3(stat) +/- 0.2(sys)) x 10(-12) cm(-2) s(-1). Furthermore, a recent observation with XMM-Newton reveals extended X-ray emission strongly peaked in the center of G15.4+0.1. The X-ray source shows indications of an energy-dependent morphology featuring a compact core at energies above 4 keV and more extended emission that fills the entire region within the SNR at lower energies. Together, the X-ray and VHE gamma-ray emission provide strong evidence of a PWN located inside the shell of G15.4+0.1 and this SNR can therefore be classified as a composite based on these observations. The radio, X-ray, and gamma-ray emission from the PWN is compatible with a one-zone leptonic model that requires a low average magnetic field inside the emission region. An unambiguous counterpart to the putative pulsar, which is thought to power the PWN, has been detected neither in radio nor in X-ray observations of G15.4+0.1. | |
650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
653 | a X-rays: individuals: G15.4+0.1 | |
653 | a gamma rays: general | |
653 | a methods: observational | |
653 | a supernovae: individual: HESS J1818-154 | |
653 | a X-rays: general | |
653 | a Astropartikelfysik | |
653 | a Astroparticle Physics | |
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773 | 0 | t Astronomy and Astrophysicsd : EDP Sciencesg 562, s. 562-q 562<562-x 0004-6361x 1432-0746 |
856 | 4 | u https://www.aanda.org/articles/aa/pdf/2014/02/aa22914-13.pdf |
856 | 4 | u https://doi.org/10.1051/0004-6361/201322914y Fulltext |
856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:lnu:diva-33979 |
856 | 4 8 | u https://doi.org/10.1051/0004-6361/201322914 |
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