C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST18:16:34

2018A&A...617A...5D - Astronomy and Astrophysics, volume 617A, 5-5 (2018/9-1)

Disentangling hadronic from leptonic emission in the composite SNR G326.3-1.8.


Abstract (from CDS):

Context. G326.3-1.8 (also known as MSH 15-56) has been detected in radio as middle-aged composite supernova remnant (SNR) consisting of an SNR shell and a pulsar wind nebula (PWN) that has been crushed by the SNR reverse shock. Previous γ-ray studies of SNR G326.3-1.8 revealed bright and extended emission with uncertain origin. Understanding the nature of the γ-ray emission allows probing the population of high-energy particles (leptons or hadrons), but can be challenging for sources of small angular extent.
Aims. With the recent Fermi Large Area Telescope data release Pass 8, which provides increased acceptance and angular resolution, we investigate the morphology of this SNR to disentangle the PWN from the SNR contribution.In particular, we take advantage of the new possibility to filter events based on their angular reconstruction quality.
Methods. We performed a morphological and spectral analysis from 300MeV to 300GeV. We used the reconstructed events with the best angular resolution (PSF3 event type) to separately investigate the PWN and the SNR emissions, which is crucial to accurately determine the spectral properties of G326.3-1.8 and understand its nature.
Results. The centroid of the γ-ray emission evolves with energy and is spatially coincident with the radio PWN at high energies (E>3GeV). The morphological analysis reveals that a model considering two contributions from the SNR and the PWN reproduces the γ-ray data better than a single-component model. The associated spectral analysis using power laws shows two distinct spectral features, a softer spectrum for the remnant (Γ=2.17±0.06) and a harder spectrum for the PWN (Γ=1.79±0.12), consistent with hadronic and leptonic origin for the SNR and the PWN, respectively. Focusing on the SNR spectrum, we use one-zone models to derive some physical properties, and we find in particular, that the emission is best explained with a hadronic scenario in which the high target density is provided by radiative shocks in HI clouds struck by the SNR.

Abstract Copyright: © ESO 2018

Journal keyword(s): astroparticle physics - cosmic rays - ISM: supernova remnants - gamma rays: ISM

Simbad objects: 4

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Number of rows : 4

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
1 IC 443 SNR 06 18 02.7 +22 39 36           ~ 1101 1
2 Kes 25 SNR 15 53 00.000 -56 10 00.00           ~ 115 0
3 SNR G034.6-00.5 SNR 18 56 10.650 +01 13 21.30           ~ 826 2
4 NAME Cyg Loop SNR 20 51.0 +30 40           ~ 823 0

    Equat.    Gal    SGal    Ecl

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