460 citations · 1.3k across the 36 of their papers we have counts for
13 papers · 1 filter
Observations of ionized carbon towards the -ray-bright supernova remnant RX J1713.7-3946
A. R. Thakur, G. P. Rowell, R. Higgins +7
The origin of Galactic Cosmic Rays (CRs), particularly at sub-GeV energies, remains uncertain due to their difficulty in being traced. One possible tracer of low-energy CRs is ioni…
A deep spectromorphological study of the -ray emission surrounding the young massive stellar cluster Westerlund 1
F. Aharonian, H. Ashkar, M. Backes +156
Young massive stellar clusters are extreme environments and potentially provide the means for efficient particle acceleration. Indeed, they are increasingly considered as being res…
Modelling the Gamma-Ray Morphology of HESS J1804-216 from Two Supernova Remnants in a Hadronic Scenario
K. Feijen, S. Einecke, G. Rowell +3
HESS J1804-216 is one of the brightest yet most mysterious TeV gamma-ray sources discovered to date. Previous arc-minute scale studies of the interstellar medium (ISM) surrounding…
Arc-minute-scale studies of the interstellar gas towards HESSJ1804216: Still an unidentified TeV -ray source
K. Feijen, G. Rowell, S. Einecke +5
The Galactic TeV -ray source HESSJ1804216 is currently an unidentified source. In an attempt to unveil its origin, we present here the most detailed study of interstellar…
Radio Emission from Interstellar Shocks: Young Type Ia Supernova Remnants and the Case of N 103B in the Large Magellanic Cloud
R. Z. E. Alsaberi, L. A. Barnes, M. D. Filipovic +19
Here we present a radio continuum study based on new and archival data from the Australia Telescope Compact Array towards N 103B, a young (<=1000 yrs) spectroscopically confirmed t…
A Supernova Remnant Counterpart for HESS J1832-085
Nigel I. Maxted, M. D. Filipovic, N. Hurley-Walker +18
We examine the new Galactic supernova remnant (SNR) candidate, G23.11+0.18, as seen by the Murchison Widefield Array (MWA) radio telescope. We describe the morphology of the candid…
Discovery of a Pulsar-powered Bow Shock Nebula in the Small Magellanic Cloud Supernova Remnant DEMS5
Rami Z. E. Alsaberi, C. Maitra, M. D. Filipovi'c +32
We report the discovery of a new Small Magellanic Cloud Pulsar Wind Nebula (PWN) at the edge of the Supernova Remnant (SNR)-DEM S5. The pulsar powered object has a cometary morphol…
A Morphological Study of the Supernova Remnant RX J0852.0-4622 (Vela Jr.)
Nigel I. Maxted, M. D. Filipovic, H. Sano +14
We conduct a multi-wavelength morphological study of the Galactic supernova remnant RXJ0852.0-4622 (also known as Vela Jr., Vela Z and G266.2-1.2). RX J0852.0-4622 is coincident wi…
Natal molecular cloud of SNR Kes 41. Complete characterisation
Leonardo Supán, Gabriela Castelletti, Alberto D. Supanitsky +3
Using high-resolution data of the CO and CO (=1-0}) line emission from The Mopra Southern Galactic Plane CO Survey in conjunction with neutral hydrogen observation…
Searching for an interstellar medium association for HESS J1534-571
Nigel I. Maxted, C. Braiding, G. F. Wong +9
The Galactic supernova remnant HESS J1534-571 (also known as G323.7-1.0) has a shell-like morphology in TeV gamma-ray emission and is a key object in the study of cosmic ray origin…
Multi-frequency observations of a superbubble in the LMC: The case of LHA 120-N 70
A. Y. De Horta, E. R. Sommer, M. D. Filipović +8
We present a detailed study of new Australia Telescope Compact Array (ATCA) and XMM-Newton observations of LHA 120-N 70 (hereafter N 70), a spherically shaped object in the Large M…
AGN behind the SMC selected from radio and X-ray surveys
R. Sturm, D. Drašković, M. D. Filipović +8
The XMM-Newton survey of the Small Magellanic Cloud (SMC) revealed 3053 X-ray sources with the majority expected to be active galactic nuclei (AGN) behind the SMC. However, the hig…
Swings between rotation and accretion power in a millisecond binary pulsar
A. Papitto, C. Ferrigno, E. Bozzo +20
It is thought that neutron stars in low-mass binary systems can accrete matter and angular momentum from the companion star and be spun-up to millisecond rotational periods. During…