A Hard Extended X-Ray Source in the IC 443 Supernova Remnant Resolved by Chandra : A Fast Ejecta Fragment or a New Pulsar Wind Nebula?

2005 ◽  
Vol 624 (1) ◽  
pp. L41-L44 ◽  
Author(s):  
A. M. Bykov ◽  
F. Bocchino ◽  
G. G. Pavlov
Keyword(s):  
Supernova Remnant ◽  
X Ray ◽  
Pulsar Wind

scholarly journals Deciphering the nature of the pulsar wind nebula CTB 87 with XMM–Newton

2019 ◽  
Vol 491 (2) ◽  
pp. 3013-3021 ◽  
Author(s):  
B Guest ◽  
S Safi-Harb ◽  
A MacMaster ◽  
R Kothes ◽  
B Olmi ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Thermal Emission ◽  
Plasma Temperature ◽  
Evolutionary Stage ◽  
Reverse Shock ◽  
X Ray ◽  
Upper Limit ◽  
Supernova Shell ◽  
Pulsar Wind ◽  
Hydrodynamical Simulations

ABSTRACT CTB 87 (G74.9+1.2) is an evolved supernova remnant (SNR) which hosts a peculiar pulsar wind nebula (PWN). The X-ray peak is offset from that observed in radio and lies towards the edge of the radio nebula. The putative pulsar, CXOU J201609.2+371110, was first resolved with Chandra and is surrounded by a compact and a more extended X-ray nebula. Here, we use a deep XMM–Newton observation to examine the morphology and evolutionary stage of the PWN and to search for thermal emission expected from a supernova shell or reverse shock interaction with supernova ejecta. We do not find evidence of thermal X-ray emission from the SNR and place an upper limit on the electron density of 0.05 cm−3 for a plasma temperature kT ∼ 0.8 keV. The morphology and spectral properties are consistent with a ∼20-kyr-old relic PWN expanding into a stellar wind-blown bubble. We also present the first X-ray spectral index map from the PWN and show that we can reproduce its morphology by means of 2D axisymmetric relativistic hydrodynamical simulations.

scholarly journals X-RAY OBSERVATIONS OF THE SUPERNOVA REMNANT CTB 87 (G74.9+1.2): AN EVOLVED PULSAR WIND NEBULA

2013 ◽  
Vol 774 (1) ◽  
pp. 33 ◽  
Author(s):  
H. Matheson ◽  
S. Safi-Harb ◽  
R. Kothes
Keyword(s):  
Supernova Remnant ◽  
X Ray ◽  
Pulsar Wind

scholarly journals Radio study of the extended TeV source VER J1907+062

2019 ◽  
Vol 491 (4) ◽  
pp. 5732-5739
Author(s):  
L Duvidovich ◽  
A Petriella ◽  
E Giacani
Keyword(s):  
Atomic Hydrogen ◽  
Molecular Clouds ◽  
Supernova Remnant ◽  
Molecular Gas ◽  
Radio Observations ◽  
Very Large Array ◽  
X Ray ◽  
New Radio ◽  
Γ Ray ◽  
Pulsar Wind

ABSTRACT This paper aims to provide new insights on the origin of the TeV source VER J1907+062 through new high-quality radio observations. We used the Karl G. Jansky Very Large Array (VLA) to observe the whole extension of VER J1907+062 at 1.5 GHz with a mosaicking technique and the PSR J1907+0602 in a single pointing at 6 GHz. These data were used together with 12CO and atomic hydrogen observations obtained from public surveys to investigate the interstellar medium in the direction of VER J1907+062. The new radio observations do not show any evidence of a pulsar wind nebula (PWN) driven by the pulsars present in the field and no radio counterpart to the proposed X-ray PWN powered by PSR J1907+0602 is seen in the new VLA image at 6 GHz down to a noise level of 10 $\mu$Jy beam−1. Molecular clouds were discovered over the eastern, southern, and western borders of the radio shell of G40.5−0.5, suggesting an association with this supernova remnant. We explored several scenarios for the origin of VER J1907+062. We propose as the most probable scenario one in which the TeV emission is produced by two separated γ-ray sources located at different distances: one of leptonic origin and associated with a PWN powered by PSR J1907+0602 at ∼3.2 kpc and another of hadronic origin and produced by the interaction between G40.5−0.5 and the surrounding molecular gas at ∼8.7 kpc.

scholarly journals Discovery of a New X‐Ray Filled Radio Supernova Remnant around the Pulsar Wind Nebula in 3EG J1809−2328

2008 ◽  
Vol 681 (1) ◽  
pp. 320-324 ◽  
Author(s):  
Mallory S. E. Roberts ◽  
Crystal L. Brogan
Keyword(s):  
Supernova Remnant ◽  
X Ray ◽  
Pulsar Wind

THE PUZZLING JET AND PULSAR WIND NEBULA OF IGR J11014-6103

2014 ◽  
Vol 28 ◽  
pp. 1460172 ◽  
Author(s):  
LUCIA PAVAN ◽  
POL BORDAS ◽  
GERD PÜHLHOFER ◽  
MIROSLAV D. FILIPOVIC ◽  
AIN DE HORTA ◽  
...  
Keyword(s):  
Neutron Star ◽  
Supernova Remnant ◽  
Helical Structure ◽  
Core Collapse ◽  
Radio Observations ◽  
X Ray ◽  
Core Collapse Supernova ◽  
The Core ◽  
Pulsar Wind

IGR J11014-6103 is a hard X-ray source discovered by INTEGRAL. Follow-up X-ray and radio observations revealed an elongated pulsar wind nebula formed by a neutron star escaping supersonically its parent supernova remnant SNR MSH 11-61A. The pulsar also emits highly collimated jets extending perpendicularly to the direction of motion. The jet has a continuous helical structure extending up to more than 10 parsecs. IGR J11014-6103 is a laboratory to study jet ejection in the wind of a pulsar and to constrain the core collapse supernova mechanism responsible for the observed pulsar kick velocity in excess of 1000 km/s.

scholarly journals On the origin of jet-like features in bow shock pulsar wind nebulae

2019 ◽  
Vol 490 (3) ◽  
pp. 3608-3615 ◽  
Author(s):  
B Olmi ◽  
N Bucciantini
Keyword(s):  
Supernova Remnant ◽  
High Energy ◽  
Field Structure ◽  
Bow Shock ◽  
Pulsar Wind Nebulae ◽  
Magnetic Field Structure ◽  
X Ray ◽  
Class A ◽  
Pulsar Wind ◽  
High Energy Particles

ABSTRACT Bow shock pulsar wind nebulae are a large class of non-thermal synchrotron sources associated to old pulsars that have emerged from their parent supernova remnant and are directly interacting with the interstellar medium. Within this class a few objects show extended X-ray features, generally referred as ‘jets’, that defies all the expectations from the canonical MHD models, being strongly misaligned respect to the pulsar direction of motion. It has been suggested that these jets might originate from high energy particles that escape from the system. Here we investigate this possibility, computing particle trajectories on top of a 3D relativistic MHD model of the flow and magnetic field structure, and we show not only that beamed escape is possible, but that it can easily be asymmetric and charge separated, which as we will discuss are important aspects to explain known objects.

scholarly journals Discovery of a jet-like structure with overionized plasma in the SNR IC 443

2018 ◽  
Vol 615 ◽  
pp. A157 ◽  
Author(s):  
Emanuele Greco ◽  
Marco Miceli ◽  
Salvatore Orlando ◽  
Giovanni Peres ◽  
Eleonora Troja ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Supernova Explosion ◽  
Original Position ◽  
Core Collapse ◽  
Complex Environment ◽  
Energy Bands ◽  
X Ray ◽  
Spatially Resolved ◽  
Pulsar Wind ◽  
The Relationship

Context. IC 443 is a supernova remnant (SNR) located in a quite complex environment since it interacts with nearby clouds. Indications for the presence of overionized plasma have been found though the possible physical causes of overionization are still debated. Moreover, because of its peculiar position and proper motion, it is not clear if the pulsar wind nebula (PWN) within the remnant is the relic of the IC 443 progenitor star or just a rambling one seen in projection on the remnant. Aims. Here we address the study of IC 443 plasma in order to clarify the relationship PWN-remnant, the presence of overionization and the origin of the latter. Methods. We analyzed two XMM-Newton observations producing background-subtracted, vignetting-corrected and mosaicked images in two different energy bands and we performed a spatially resolved spectral analysis of the X-ray emission. Results. We identified an elongated (jet-like) structure with Mg-rich plasma in overionization. The head of the jet is interacting with a molecular cloud and the jet is aligned with the position of the PWN at the instant of the supernova explosion. Interestingly, the direction of the jet of ejecta is somehow consistent with the direction of the PWN jet. Conclusions. Our discovery of a jet of ejecta in IC 443 enlarge the sample of core-collapse SNRs with collimated ejecta structures. IC 443’s jet is the first one which shows overionized plasma, possibly associated with the adiabatic expansion of ejecta. The match between the jet’s direction and the original position of the PWN strongly supports the association between the neutron star and IC 443.

scholarly journals An X-ray Pulsar, Metal-rich Ejecta, and Shocked Ambient Medium in the Supernova Remnant G292.0+1.8

2004 ◽  
Vol 218 ◽  
pp. 199-202
Author(s):  
John P. Hughes ◽  
Robert B. Friedman ◽  
Patrick Slane ◽  
Sangwook Park
Keyword(s):  
High Resolution ◽  
Supernova Remnant ◽  
Ambient Medium ◽  
Compact Object ◽  
Optical Counterpart ◽  
Reverse Shock ◽  
X Ray ◽  
Pulsar Wind ◽  
Circumstellar Medium

We report the discovery of pulsed X-ray emission from the compact object CXOU J112439.1-591620 within the Galactic supernova remnant G292.0+1.8 using the High Resolution Camera on the Chandra X-Ray Observatory. The X-ray period is consistent with the extrapolation of the radio period and spindown rate of PSR J1124−5916. The X-ray pulse is single peaked and broad. There is no optical counterpart to a limit of MV ∼ 26. The pressure in the pulsar wind nebula is considerably less than that in the reverse-shock-heated ejecta and circumstellar medium, indicating that the reverse shock has not yet begun to interact with the nebula.

scholarly journals Discovery of recombining plasma inside the extended gamma-ray supernova remnant HB9

2019 ◽  
Vol 489 (3) ◽  
pp. 4300-4310 ◽  
Author(s):  
A Sezer ◽  
T Ergin ◽  
R Yamazaki ◽  
H Sano ◽  
Y Fukui
Keyword(s):  
Supernova Remnant ◽  
Gamma Ray ◽  
Radio Continuum ◽  
Continuum Emission ◽  
Large Area ◽  
Imaging Spectrometer ◽  
X Ray ◽  
East Region ◽  
X Ray Imaging ◽  
Collisional Ionization

ABSTRACT We present the results from the Suzaku X-ray Imaging Spectrometer observation of the mixed-morphology supernova remnant (SNR) HB9 (G160.9+2.6). We discovered recombining plasma (RP) in the western Suzaku observation region and the spectra here are well described by a model having collisional ionization equilibrium (CIE) and RP components. On the other hand, the X-ray spectra from the eastern Suzaku observation region are best reproduced by the CIE and non-equilibrium ionization model. We discuss possible scenarios to explain the origin of the RP emission based on the observational properties and concluded that the rarefaction scenario is a possible explanation for the existence of RP. In addition, the gamma-ray emission morphology and spectrum within the energy range of 0.2–300 GeV are investigated using 10 yr of data from the Fermi Large Area Telescope (LAT). The gamma-ray morphology of HB9 is best described by the spatial template of radio continuum emission. The spectrum is well fit to a log-parabola function and its detection significance was found to be 25σ. Moreover, a new gamma-ray point source located just outside the south-east region of the SNR’s shell was detected with a significance of 6σ. We also investigated the archival H i and CO data and detected an expanding shell structure in the velocity range of $-10.5$ and $+1.8$ km s−1 that is coinciding with a region of gamma-ray enhancement at the southern rim of the HB9 shell.

scholarly journals An X-ray characterization of the central region of the supernova remnant G332.5-5.6

2015 ◽  
Vol 583 ◽  
pp. A84 ◽  
Author(s):  
A. E. Suárez ◽  
J. A. Combi ◽  
J. F. Albacete-Colombo ◽  
S. Paron ◽  
F. García ◽  
...  
Keyword(s):  
Central Region ◽  
Supernova Remnant ◽  
X Ray
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