scholarly journals Locating the TeV γ-rays from the shell regions of Cassiopeia A

2013 ◽  
Vol 9 (S296) ◽  
pp. 380-381
Author(s):  
Lab Saha ◽  
Tulun Ergin ◽  
Pratik Majumdar ◽  
Mustafa Bozkurt
Keyword(s):  
Energy Range ◽  
Power Law ◽  
Supernova Remnant ◽  
X Ray ◽  
Cassiopeia A ◽  
Young Supernova Remnant ◽  
Multi Wavelength ◽  
Flux Level ◽  
Γ Rays ◽  
Different Parts

AbstractWe have analyzed Chandra X-ray data from different parts of the shell of young supernova remnant (SNR) in the energy range of 0.7 - 8 keV. We observed that X-ray flux level varies over different shell regions of the source. Implications of X-ray observation will be discussed here. We also analyzed Fermi-LAT data in the energy range 0.5 - 50 GeV for the source. The differential spectrum obtained in this way fits with simple power-law. We also present here multi-wavelength modeling of the source considering archival radio and TeV data along with Chandra and Fermi-LAT data.

scholarly journals HESS J1858+020: A GeV-TeV source possibly powered by cosmic rays from SNR G35.6-0.4

2021 ◽  
Vol 646 ◽  
pp. A114
Author(s):  
Y. Cui ◽  
Y. Xin ◽  
S. Liu ◽  
P. H. T. Tam ◽  
G. Pühlhofer ◽  
...  
Keyword(s):  
Diffusion Coefficient ◽  
Cosmic Rays ◽  
Power Law ◽  
Supernova Remnant ◽  
Observational Evidence ◽  
X Ray ◽  
Multi Wavelength ◽  
Northern Edge ◽  
Cloud Complex ◽  
Hadronic Model

Context. The supernova remnant (SNR) G35.6−0.4 shows a non-thermal radio shell, however, no γ-ray or X-ray counterparts have been found for it thus far. One TeV source, HESS J1858+020, was found near the SNR and this source is spatially associated with some clouds at 3.6 kpc. Aims. To attain a better understanding of the origin of HESS J1858+020, we further investigate the association between SNR cosmic rays (CRs) and the clouds through the Fermi-LAT analysis and hadronic modeling. Methods. We performed the Fermi-LAT analysis to explore the GeV emission in and around the SNR. We explored the SNR physics with previously observed multi-wavelength data. We built a hadronic model using runaway CRs of the SNR to explain the GeV-TeV observation. Results. We found a hard GeV source (SrcX2) that is spatially coincident with both HESS J1858+020 and a molecular cloud complex at 3.6 kpc. In addition, a soft GeV source (SrcX1) was found at the northern edge of the SNR. The GeV spectrum of SrcX2 connects well with the TeV spectrum of HESS J1858+020. The entire γ-ray spectrum ranges from several GeV up to tens of TeV and it follows a power-law with an index of ~2.15. We discuss several pieces of observational evidence to support the middle-aged SNR argument. Using runaway CRs from the SNR, our hadronic model explains the GeV-TeV emission at HESS J1858+020, with a diffusion coefficient that is much lower than the Galactic value.

scholarly journals Multi-year X-Ray Variations of Iron-K and Continuum Emissions in the Young Supernova Remnant Cassiopeia A

2017 ◽  
Vol 836 (2) ◽  
pp. 225 ◽  
Author(s):  
Toshiki Sato ◽  
Yoshitomo Maeda ◽  
Aya Bamba ◽  
Satoru Katsuda ◽  
Yutaka Ohira ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
X Ray ◽  
Cassiopeia A ◽  
Young Supernova Remnant

X-Ray, Optical and UV Observations of the Young Supernova Remnant in the Irregular Galaxy NGC 4449

1983 ◽  
pp. 579-582
Author(s):  
W. P. Blair ◽  
R. P. Kirshner ◽  
P. F. Winkler ◽  
J. C. Raymond ◽  
R. A. Fesen ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Irregular Galaxy ◽  
X Ray ◽  
Young Supernova Remnant

scholarly journals XMM-Newton and Fermi/LAT view on the supernova remnant 3C434.1

2019 ◽  
Vol 631 ◽  
pp. A179
Author(s):  
V. Doroshenko ◽  
D. Malyshev ◽  
G. Pühlhofer ◽  
B. Dincel ◽  
M. Sasaki ◽  
...  
Keyword(s):  
Power Law ◽  
Supernova Remnant ◽  
X Rays ◽  
Significant Excess ◽  
X Ray ◽  
Thermal Origin

We report on XMM-Newton observations of the supernova remnant (SNR) 3C434.1 (G94.0+1.0), the first in X-rays since the ROSAT era. Our analysis confirms the thermal origin of the observed extended X-ray emission, whose morphology appears more complex than previously reported. In particular, part of the shell shows a significantly harder spectrum which is consistent with a power law, and it is, therefore, likely of non-thermal origin. Motivated by these finding, we revisited the GeV observations of the field taken with the Fermi observatory. A significant excess associated with the remnant was detected, which is likely associated with non-thermal X-ray emission from part of the shell. The analysis of the Fermi data resulted in the serendipity discovery of GeV emission from the nearby SNR G093.7-00.2. Finally, we searched for a possible compact remnants within the shell, however, no obvious candidates could be identified due to the fairly large positional uncertainties.

scholarly journals Iron Line Emission from NGC1068

1989 ◽  
Vol 134 ◽  
pp. 167-172
Author(s):  
Katsuji Koyama
Keyword(s):  
Energy Range ◽  
Power Law ◽  
Equivalent Width ◽  
Line Emission ◽  
X Rays ◽  
Iron Line ◽  
X Ray ◽  
Central Engine ◽  
Photon Index ◽  
The Continuum

X-ray emission in the 2–10 keV energy range was observed with the Ginga satellite from the Seyfert 2 galaxy NGC1068. The continuum spectrum can be described by a power-law of photon index about 1.5. An intense iron line at 6.5 keV with an equivalent width of 1.3 keV was clearly noticed. The X-ray flux was about 6 × 10 −12 erg/sec/cm2 or 3 × 1041 erg/sec, assuming a distance of 22 Mpc. The observed spectrum is consistent with the scattering and reprocessing of X-rays by the gas surrounding the central engine. With this picture we estimate that the X-ray flux of the central engine is about 1043 - 1044 erg/sec, a typical value for a Seyfert 1 galaxy.

scholarly journals Asymmetries of Heavy Elements in the Young Supernova Remnant Cassiopeia A

2020 ◽  
Vol 889 (2) ◽  
pp. 144 ◽  
Author(s):  
Tyler Holland-Ashford ◽  
Laura A. Lopez ◽  
Katie Auchettl
Keyword(s):  
Supernova Remnant ◽  
Heavy Elements ◽  
Cassiopeia A ◽  
Young Supernova Remnant

scholarly journals XMM-Newton spectrum of the magnetar CXOU J171405.7–381031

2019 ◽  
Vol 71 (4) ◽  
Author(s):  
Haruka Watanabe ◽  
Aya Bamba ◽  
Shinpei Shibata ◽  
Eri Watanabe
Keyword(s):  
Power Law ◽  
Time Variation ◽  
Supernova Remnant ◽  
Component Model ◽  
Time Variability ◽  
Spectral Parameters ◽  
X Ray ◽  
Two Component ◽  
Photon Index ◽  
Higher Temperature

Abstract We observe the magnetar CXOU J171405.7−381031 with XMM-Newton and obtain the most reliable X-ray spectral parameters for this magnetar. After removing the flux from the surrounding supernova remnant CTB 37B, the radiation of CXOU J171405.7−381031 is best described by a two-component model, consisting of a blackbody and power law. We obtain a blackbody temperature of $0.58^{+0.03}_{-0.03}$ keV, a photon index of $2.15^{+0.62}_{-0.68}$, and an unabsorbed 2–10 keV band flux of $2.33^{+0.02}_{-0.02} \times 10^{-12}$ erg cm−2 s−1. These new parameters enable us to compare CXOU J171405.7−381031 with other magnetars, and it is found that the luminosity, temperature, and photon index of CXOU J171405.7−381031 are aligned with the known trend among the magnetar population with a slightly higher temperature, which could be caused by its young age. All magnetars with a spin-down age of less than 1000 yr show time variation or bursts except for CXOU J171405.7−381031. We explore the time variability for six observations between 2006 and 2015, but there is no variation larger than ∼10%.

The Soft X-Ray Spectra of Cassiopeia a and Tycho's Supernova Remnant

1975 ◽  
Vol 200 ◽  
pp. 158 ◽  
Author(s):  
R. W. Hill ◽  
G. A. Burginyon ◽  
F. D. Seward
Keyword(s):  
Supernova Remnant ◽  
X Ray ◽  
Cassiopeia A

scholarly journals The X-ray structure and mass of the Cassiopeia A supernova remnant

1980 ◽  
Vol 193 (2) ◽  
pp. 175-188 ◽  
Author(s):  
A. C. Fabian ◽  
R. Willingale ◽  
J. P. Pye ◽  
S. S. Murray ◽  
G. Fabbiano
Keyword(s):  
Supernova Remnant ◽  
X Ray ◽  
Cassiopeia A
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