COMA X RAY FREE

The spectrum is not consistent with the existence of a hard X-ray tail at the flux level reported by Bazzano el al. The Fe K-beta line blend is also weakly detected. Head back to the surgeon and hang up the pictures in this order: 4, 3, 2, 1. Head upstairs to the X-Ray Room and grab the X-ray Images. Once inside, continue to the left to find the note near the back. The Fe K-alpha line blend is strongly detected, from which we infer 0.18-0.36 solar abundance in the X-ray emitting gas. After waking up in The Coma, exit the old storage room and go to the cafeteria at the far left side of the hall. Using the best-fitting parameters, the gas is found to be a significant fraction (25 percent) of the total cluster mass. Coma is the richest nearby cluster, with relatively dense and hot IC gas, and only a small degree of apparent ellipticity. Because the principal ray passes through the origin of the aperture coordinate system, s equals zero. This analysis reduces the total cluster mass by a factor of 3-5 below the optically derived virial mass. Coma cluster (Abell 1656, z0.0235) has been the first target in the MITO cosmological project, selected for its good visibility, the high observational efficiency and the high-quality of the existing X-ray measurements. The size or magnitude of each aberration is indicated by the subscripted weights A 1, A 2 and B 1 to B 5, and these weighted aberration terms add together to indicate the total aberration in the point image. To model the spectrum more accurately, we have performed fits of polytropic models and find that the gas is well fitted by an equation of state with polytropic index ranging between 1.38 and 1.6. The spectrum is not well fitted by an isothermal bremsstrahlung model with an Fe line. By comparing to ROSAT observations of the 0.2- 0.4 keV soft excess, we find that the overall excess luminosity is easily reproduced for g)$$ is the axion-photon (axion-neutron) coupling constant.The HEAO 1 A-2 and OSO 8 observations of the Coma Cluster of galaxies in the 2-60 keV energy band are presented. Spherical aberration can be considered as a variation of the focal length with the aperture. The cluster contains thousands of galaxies enveloped by a vast 100 million-degree Celsius gas cloud. This Chandra image shows the central region - about 1.5 million light years across - of the Coma Cluster.

COMA X RAY FREE

If the paraxial magnification is equal to the real ray marginal magnification, then an optical system would be free of coma. Coma Cluster: Gas Clouds Strike A Delicate Balance Credit: NASA/CXC/SAO/A.Vikhlinin et al. We study the morphology of the soft excess by numerically propagating axions through stochastic, multi-scale magnetic field models that are consistent with observations of Faraday rotation measures from Coma. Coma aberration can be considered as a variation of magnification with respect to the aperture. We provide a detailed self-contained review of the cluster soft X-ray excess, the proposed astrophysical explanations and the problems they face, and explain how a 0.1- 1 keV axion background naturally arises at reheating in many string theory models of the early universe. Around 1.5 million light-years across, Comas central region around galaxy NGC 4889 (left) and NGC 4874 contains a diffuse cloud of hot gas (at 10 to 20 million degrees) that is held by the clusters enormous gravity, (more from CXC). We show that the soft X-ray excess in the Coma cluster can be explained by a cosmic background of relativistic axion-like particles (ALPs) converting into photons in the cluster magnetic field. Vikhlinin et al, 2001 CXC, SAO, NASA Larger x-ray image.

Coma x ray