5,563 research outputs found

    ASCA Temperature Maps of Three Clusters of Galaxies Abell 1060, AWM7, and the Centaurus Cluster

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    We present two-dimensional temperature maps of three bright clusters of galaxies Abell 1060, AWM7, and the Centaurus cluster, based on multi-pointing observations with the ASCA GIS. The temperatures are derived from hardness ratios by taking into account the XRT response. For the Centaurus cluster, we subtracted the central cool component using the previous ASCA and ROSAT results, and the metallicity gradients observed in AWM7 and the Centaurus cluster were included in deriving the temperatures. The intracluster medium in Abell 1060 and AWM7 is almost isothermal from the center to outer regions with a temperature of 3.3 and 3.9 keV, respectively. The Centaurus cluster exhibits remarkable hot regions within about 30' from the cluster center showing a temperature increase of +0.8 keV from the surrounding level of 3.5 keV, and outer cool regions with lower temperatures by -1.3 keV. These results imply that a strong merger has occurred in the Centaurus in the recent 2-3 Gyr, and the central cool component has survived it. In contrast, the gas in Abell 1060 was well-mixed in an early period, which probably has prevented the development of the central cool component. In AWM7, mixing of the gas should have occurred in a period earlier than the epoch of metal enrichment.Comment: 18 pages, 8 figures (including color), Latex(PASJadd.sty, PASJ95.sty), accepted for publication in PASJ. Postscript is also available at http://www-x.phys.metro-u.ac.jp/~furusho/papers.htm

    Detection of Excess Hard X-ray Emission from the Group of Galaxies HCG62

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    From the group of galaxies HCG62, we detected an excess hard X-ray emission in energies above 4\sim 4 keV with \A SCA. The excess emission is spatially extended up to 10\sim10' from the group center, and somewhat enhanced toward north. Its spectrum can be represented by either a power-law of photon index 0.8-2.7, or a Bremsstrahlung of temperature >6.3>6.3 keV. In the 2-10 keV range, the observed hard X-ray flux, (1.0±0.3)×1012(1.0\pm0.3)\times10^{-12} erg cm2^{-2} s1^{-1}, implies a luminosity of (8.0±2.0)×1041(8.0\pm2.0)\times10^{41} erg s1^{-1} for a Hubble constant of 50 km s1^{-1} Mpc1^{-1}. The emission is thus too luminous to be attributed to X-ray binaries in the memb er galaxies. We discuss possible origin of the hard X-ray emission.Comment: 6 pages, 3 Postscript figures, uses emulateapj.sty. Accepted for publication in the Astrophysical Journal Letter

    Chandra X-Ray Spectral Analysis of Cooling Flow Clusters, 2A 0335+096 and Abell 2199

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    We report on a spatially resolved analysis of Chandra X-ray data on a nearby typical cooling flow cluster of galaxies 2A 0335+096, together with A 2199 for a comparison. As recently found in the cores of other clusters, the temperature around the central part of 2A 0335+096 is 1.3--1.5 keV, which is higher than that inferred from the cooling flow picture. Furthermore, the absorption column density is almost constant against the radius in 2A 0335+096; there is no evidence of excess absorption up to 200--250 kpc. This indicates that no significant amount of cold material, which has cooled down, is present. These properties are similar to those of A 2199. Since the cooling time in the central part is much shorter than the age of the clusters, a heating mechanism, which weakens the effect of radiative cooling, is expected to be present in the central part of both clusters of galaxies. Both 2A 0335+096 and A 2199 have radio jets associated with their cD galaxy. We discuss the possibility of heating processes caused by these radio jets by considering the thermal conduction and the sound velocity together with the observed disturbance of the ICM temperature and density. We conclude that the observed radio jets can produce local heating and/or cooling, but do not sufficiently reduce the overall radiative cooling. This implies that much more violent jets, whose emission has now decayed, heated up the cooling gas >109>10^9 years ago.Comment: 13 pages, 7 figures, to appear in PASJ 55 No.

    Suppression of Magnetic Order by Pressure in BaFe2As2

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    We performed the dc resistivity and the ZF 75As-NMR measurement of BaFe2As2 under high pressure. The T-P phase diagram of BaFe2As2 determined from resistivity anomalies and the ZF 75As-NMR clearly revealed that the SDW anomaly is quite robust against P.Comment: 2 pages, 2 figure

    Chiral phase transition of bulk Abelian gauge theories in the Randall-Sundrum brane world

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    The chiral phase transition of strong-coupling Abelian gauge theories is investigated in the brane world. It is assumed that gauge boson propagates in an extra dimension, i.e. bulk gauge theories. The phase structure is analytically evaluated by using the low-energy effective theories. We also numerically solve the ladder Schwinger-Dyson equation for the full fermion propagator including Kaluza-Klein (KK) excitation modes of the gauge field. It is found that the chiral phase transition is of the second order, and the critical value of the coupling constant is obtained. The extra dimension has a large influence on the chiral phase transition for the Randall-Sundrum (RS) brane world. It is studied how the number of KK modes affect the chiral phase transition.Comment: 18 pages, 7 figures, REVTe

    Reflection Component in the Hard X-Ray Emission from the Seyfert 2 Galaxy Mrk 1210

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    The Seyfert 2 galaxy Mrk 1210 was found to exhibit a flat hard X-ray component by ASCA, although ASCA could not distinguish whether it is an absorbed direct component or a reflected one. We then observed Mrk 1210 with BeppoSAX, and found that the X-ray spectral properties are quite different from those of ASCA, as have been confirmed with XMM-Newton; the flux is significantly higher than that in the ASCA observation, and a clear absorption cut-off appears below 5 keV. A bright hard X-ray emission is detected up to 100 keV. The reflection component is necessary to describe the BeppoSAX PDS spectrum, and represents the ASCA hard component very well. Therefore, the hard component in the ASCA spectrum is a reflected one, whose intensity is almost constant over 6 years. This indicates that a dramatic spectral variability is attributed to a large change of the absorption column density by a factor of >5, rather than the variability of the nuclear emission. The change in the absorption-column density means that the torus is not homogeneous, but has a blobby structure with a typical blob size of < 0.001Comment: 9 pages, 5 figures, accepted for Pablications for the Astronomical Society of Japa
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