scholarly journals Hard X-Ray Radiation in the Coma Cluster Spectrum

1999 ◽  
Vol 513 (1) ◽  
pp. L21-L24 ◽  
Author(s):  
Roberto Fusco-Femiano ◽  
Daniele Dal Fiume ◽  
Luigina Feretti ◽  
Gabriele Giovannini ◽  
Paola Grandi ◽  
...  
Keyword(s):  
2016 ◽  
Vol 68 (5) ◽  
pp. 85 ◽  
Author(s):  
Toru Sasaki ◽  
Kyoko Matsushita ◽  
Kosuke Sato ◽  
Nobuhiro Okabe
Keyword(s):  

1979 ◽  
Vol 3 (5) ◽  
pp. 332-341 ◽  
Author(s):  
O. B. Slee ◽  
P. J. Quinn

The completion of the Uhuru (Forman et al. 1978) and Ariel V (Cooke et al. 1978) surveys of the sky for X-ray emission has resulted in many proposed identifications with individual galaxies and clusters of galaxies. The X-ray positions are not usually accurate enough to enable a positive identification to be made of the X-ray sources with optical or radio objects, and hence the identification is often based on statistical arguments — viz., the unexpected occurrence of unusual galaxies, radio sources or clusters of galaxies within or near the X-ray error boxes. There is usually no significant information available on the angular size of the X-ray emitter but in two or three cases (e.g. Perseus cluster, Coma cluster and Virgo cluster) the angular resolution is good enough to identify a broad component with dimensions approaching those of the whole cluster. This extended X-ray emission has been ascribed to either inverse Compton scattering of the 3° microwave background by relativistic electrons in the intra-cluster medium or to thermal-bremsstrahlung emission by an optically thin plasma at - 10s K.


2003 ◽  
Vol 594 (2) ◽  
pp. 732-740 ◽  
Author(s):  
Ping‐Hung Kuo ◽  
Chorng‐Yuan Hwang ◽  
Wing‐Huen Ip

1984 ◽  
Vol 280 ◽  
pp. 15 ◽  
Author(s):  
G. Des Forets ◽  
R. Dominguez-Tenreiro ◽  
D. Gerbal ◽  
G. Mathez ◽  
A. Mazure ◽  
...  

1968 ◽  
Vol 46 (10) ◽  
pp. S409-S413 ◽  
Author(s):  
Walter H. G. Lewin ◽  
George W. Clark ◽  
William B. Smith

A complete X-ray survey of the northern sky has been made in the energy range 20–100 keV. Spectra are given for Cyg X-1 and Tau X-1. Intensity ratios (Cyg X-1/Tau X-1) of 0.84 ± 0.10 and 1.30 ± 0.25 were derived in the 20–70 keV range from data obtained on July 19, 1966 and February 13, 1967, respectively. Observations on Sco X-1 and the Coma cluster show upper limits which are quite different from results reported by other groups.


2008 ◽  
Vol 687 (2) ◽  
pp. 968-975 ◽  
Author(s):  
A. A. Lutovinov ◽  
A. Vikhlinin ◽  
E. M. Churazov ◽  
M. G. Revnivtsev ◽  
R. A. Sunyaev
Keyword(s):  
X Ray ◽  

2011 ◽  
Vol 732 (2) ◽  
pp. 85 ◽  
Author(s):  
R. Fusco-Femiano ◽  
M. Orlandini ◽  
M. Bonamente ◽  
A. Lapi
Keyword(s):  

2007 ◽  
Vol 470 (3) ◽  
pp. 835-841 ◽  
Author(s):  
D. Eckert ◽  
A. Neronov ◽  
T. J.-L. Courvoisier ◽  
N. Produit
Keyword(s):  
X Ray ◽  

2004 ◽  
Vol 414 (3) ◽  
pp. L41-L44 ◽  
Author(s):  
M. Rossetti ◽  
S. Molendi
Keyword(s):  

2002 ◽  
Vol 579 (2) ◽  
pp. 587-591 ◽  
Author(s):  
Yoel Rephaeli ◽  
Duane Gruber
Keyword(s):  

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