We present the XMM-Newton results of the galaxy clusters 2A 0335$+$096 and A496. From an investigation of 2-dimensional ICM profiles, we obtained new features related to dynamical activities in the ICM. In 2A 0335$+$096, we found a spiral cool tail around the central cold core, which is trailing from the opposite side of the cold front observed by Chandra. The deprojected temperature of the tail is 1.7 keV. The spiral feature apparently shows a turnaround motion of the core. We suggest that the cool tail feature represents evidence for turbulent viscous stripping of the remaining subcluster core. For A496, we found another cold front $4^{\prime}$ south of the X-ray emission peak. From the pressure profile across the cold front, we derived an upper limit to the Mach number of a gas body of 0.2. Regarding the temperature distribution in the outer region, we found non-uniformity on the cluster scale for both clusters, which suggests that both clusters experienced a merger in the past. We argue that the gas dynamical motions seen in the central regions of both clusters can be attributed to the past merger.

We present here the results of the observation of CTB 37A obtained with the Xray Imaging Spectrometer onboard the Suzaku satellite. The X-ray spectrum of CTB 37A is well fitted by two components, a single-temperature ionization equilibrium component (VMEKAL) with solar abundances, an electron temperature of kT e ∼ 0.6 keV, absorbing column density of N H ∼ 3 × 10 22 cm −2 and a power-law component with photon index of Γ ∼ 1.6. The X-ray spectrum of CTB 37A is characterized by clearly detected K-shell emission lines of Mg, Si, S, and Ar. The plasma with solar abundances supports the idea that the X-ray emission originates from the shocked interstellar material. The ambient gas density, and age of the remnant are estimated to be ∼1f −1/2 cm −3 and ∼3×10 4 f 1/2 yr, respectively. The center-filling X-ray emission surrounded by a shell-like radio structure and other X-ray properties indicate that this remnant would be a new member of mixed-morphology supernova remnant class.

We present here the results of an X‐ray analysis of Galactic supernova remnant G346.6−0.2 observed with Suzaku. K‐shell emission lines of Mg, Si, S, Ca and Fe are detected clearly for the first time. Strong emission lines of Si and S imply that the X‐ray emission nature of G346.6−0.2 is ejecta‐dominated. The ejecta‐dominated emission is well fitted by a combined model consisting of a thermal plasma in non‐equilibrium ionization and a non‐thermal component, which can be regarded as synchrotron emission with a photon index of Γ∼ 0.6. An absorbing column density of NH∼ 2.1 × 1022 cm−2 is obtained from the best fit, implying a high‐density medium, high electron temperature of kTe∼ 1.2 keV and ionization time‐scale of net∼ 2.9 × 1011 cm−3 s, indicating that this remnant may be far from full ionization equilibrium. The relative abundances from the ejecta show that the remnant originates from a Type Ia supernova explosion.

A hard-x-ray telescope is successfully produced for balloon observations by making use of depth-graded multilayers, or so-called supermirrors, with platinum-carbon (Pt/C) layer pairs. It consists of four quadrant units assembled in an optical configuration with a diameter of 40 cm and a focal length of 8 m. Each quadrant is made of 510 pieces of coaxially and confocally aligned supermirrors that significantly enhance the sensitivity in an energy range of 20-40 keV. The configuration of the telescope is similar to the x-ray telescope onboard Astro-E, but with a longer focal length. The reflectivity of supermirrors is of the order of 40% in the energy range concerned at a grazing angle of 0.2 deg. The effective area of a fully assembled telescope is 50 cm2 at 30 keV. The angular resolution is 2.37 arc min at half-power diameter 8.0 keV. The field of view is 12.6 arc min in the hard-x-ray region, depending somewhat on x-ray energies. We discuss these characteristics, taking into account the figure errors of reflectors and their optical alignment in the telescope assembly. This hard-x-ray telescope is unanimously afforded in the International Focusing Optics Collaboration for muCrab Sensitivity balloon experiment.

Two nearby clusters of galaxies, A 194 (z = 0.018) and A 1060 (z = 0.0114), have been analyzed for their X-ray point-source properties with XMM-Newton EPIC-PN data. A multi-band source detection technique was applied to both of the clusters, resulting in 46 sources from the A 194 field and 32 sources from the A 1060 field, respectively. The cumulative log(N )-log(S) for a flux limit of F X ≥ 1 × 10 −14 erg cm −2 s −1 was calculated and compared with that of the Lockman Hole. A ∼ 3 σ excess of X-ray sources was found for the cluster regions. Considering the higher fraction observed in optical studies from the clusters, we estimate that the cluster source density is 6-times higher than the blank-field source density, and 15-times higher than the local group. Our X-ray selected sources have luminosity values of 10 39.6 ≤ L X ≤ 10 41.4 erg s −1 , in which X-ray emission from LMXBs, hot halos and starburst galaxies becomes noticeable. The significance of the source-density excess gradually vanishes for sources with L X ≥ 10 40.5 erg s −1 , at which point the source density becomes comparable to that of the blankfield level. Considering this confined low-luminosity range and the X-ray to optical luminosity ratios (L X /L B ), the observed overdensity is ascribed to AGN fueling by its infall into cluster environment for L X ≤ 10 40.5 erg s −1 in the X-ray luminosity function. However, the quenching of AGN activity by the deep cluster potential explains why the excess of the source density vanishes for brighter sources.