Long Slit Spectroscopy of Gas in the Cores of X-Ray Luminous Clusters.
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Long Slit Spectroscopy of Gas in the Cores of X-Ray Luminous Clusters.

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Published by s.n in S.l .
Written in English

Book details:

Edition Notes


SeriesUS Space Telescope Science Institute Preprint Series -- 49
ContributionsHu, E., Cowie, L., Wang, Z.
ID Numbers
Open LibraryOL21750401M

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The X-ray image of Cygnus A reveals a great deal of structure, including cocoon shocks and X-ray jets that do not coincide with its radio ations of the X-ray data will be discussed. In particular, theyhave been used to estimate the mean jet power. X-ray emission from the jets is best explained by a synchrotron model. Major gas-rich mergers of galaxies are expected to play an important role in triggering and fueling luminous active galactic nuclei (AGNs). The mechanism of AGN fueling during mergers, however, remains poorly understood. We present deep multi-band (u/r/z) imaging and long-slit spectroscopy of four double-peaked [OIII] emitting AGNs. @article{osti_, title = {Emission Lines in the Near-infrared Spectra of the Infrared Quintuplet Stars in the Galactic Center}, author = {Najarro, F. and Geballe, T. R. and Figer, D. F. and Fuente, D. de la}, abstractNote = {We report the detection of a number of emission lines in the – μ m spectra of four of the five bright-infrared dust-embedded stars at the center of Cited by: 6. Long-slit spectroscopy described by Ciardullo et al. reveals strong emission in [S II] , and [N II] , unfavorably coinciding with diagnostic emission lines of XPNe. The accuracy that can be obtained from an interpolation of the background along the slit on both sides next to the target appears to be limited.

A spatial distribution is a spatial frequency of occurrence or extent of an existence or existences such as entities, sources, or objects. A space is a volume large enough to accommodate a thing. There is an “extensive 1/4 keV emission in the Galactic halo”, an “observed 1/4 keV [X-ray emission originating] in a Local Hot Bubble (LHB) that surrounds the Sun. and an isotropic. We find a total HI mass of x 10^7 Msun, and a X-ray mass of x 10^9 Msun. The HI mass is smaller than the previous single dish observation. The HI is mainly located at south of the optical center of M86, while the hot X-ray plasm spreads out . The study of galaxies across cosmic time encompasses the main constituents of the universe across 90 percent of its history, from the formation and evolution of structures such as galaxies, clusters of galaxies, and the “cosmic web” of intergalactic matter, to the stars, gas, dust, supermassive black holes, and dark matter of which they are composed. The regions in blue are x-ray data from the Chandra X-ray Observatory orbiting the Earth, with a shock wave (bottom right) where a jet has collided with the surrounding gas medium. The remaining visible light data are from the m optical telescope at La Silla, Chile.

We have studied unbarred S0 galaxies, NGC and NGC , the members of the X-ray bright group Leo II, by means of 3D spectroscopy, long-slit spectroscopy, and imaging, with the aim to identify epoch and mechanisms of their transformation from spirals. Long-slit spectra for 14 objects chosen among the ones with the most luminous and extended line-emitting regions were collected at the m telescope at ESO La Silla (Chile), in order to compare the gas and the stellar kinematics, and study the characteristics of the emission (equivalent widths, line ratios). Preliminary results for 6 objects. The present volume is the record of a recent topical conference on the interplay between heating and cooling processes in galaxies and clusters of galaxies. The volume documents recent progress in our understanding of the dense central regions of these objects. X-ray Study of Distant Clusters of Galaxies: Structure and Evolution: Ota, Naomi; Mitsuda, Kazuhisa: Gas Temperature Profile of the Medium-Distant Galaxy Cluster Abell Observed with XMM-Newton: Reiprich, Thomas H. X-ray Absorption Features of the Intergalactic Medium: Sasaki, Shin; Ikari, Ayako.