We compare two XMM-Newton observations of the Narrow-Line Seyfert 1 galaxy 1H 0707–495 separated by two years, and discuss the results in terms of the partialcovering phenomenon. The second longer observation once again displays a sharp (< 200 eV) spectral drop above 7 keV; however, in comparison to the first observation, the edge depth and energy have changed significantly. In addition to chan...

We report results on the broad iron emission line of the Seyfert galaxy MCG–6-30-15, obtained from the second long ASCA observation in 1997. The time-averaged profile of the broad line is very similar to that seen with ASCA in 1994, so confirming the detailed model fit then obtained. A bright flare is seen in the light curve, during which the continuum was soft. At that time the emission line p...

MOTIVATION Datasets resulting from metabolomics or metabolic profiling experiments are becoming increasingly complex. Such datasets may contain underlying factors, such as time (time-resolved or longitudinal measurements), doses or combinations thereof. Currently used biostatistics methods do not take the structure of such complex datasets into account. However, incorporating this structure int...

We present preliminary Chandra results on z ≈ 0.2 clusters A665, A2163 and A2218, and a z = 0.05 cluster A754. For A754, A665 and A2163, we have derived first high-resolution projected gas temperature maps. All three show strong spatial temperature variations in the inner r < 0.5 − 1 h−1 50 Mpc regions, indicating ongoing mergers. The maps reveal a probable shock in front of a moving cluster co...

SS433 is a unique star located at the center of supernova remnant called W50, and is a close proximity binary star system which consists of a compact star and a normal star. Jets of material are directed outwards from the vicinity of the compact star symmetrically to the east and west. The radiation of non-thermal X-rays considered to have been formed by the jets is detected at both of X-ray lo...

Anticipatory Stigmergic Collision Avoidance (ASCA) is a reciprocal collision avoidance model in which agents interact by indicating intended future paths to other agents in their local environment. Other agents can then incorporate that information to guide their path planning decisions. Additionally, constraints such as restricted movements and noise are incorporated. Our evaluation showed tha...

The INTEGRAL satellite, during its regular scanning observations of the Galactic plane, has discovered several new X-ray sources emitting above 20 keV. The nature of the great majority of them is still unknown. Here we report on the likely low energy counterpart, observed with ASCA in 1994 and 1997, of one of these sources, IGR J16195–4945. The ASCA source is faint (F2−10keV∼10 −11 erg cm s), h...

The connection between the coronal lines and the warm absorber is examined systematically. In an earlier work it was found that the coronal line emitting plasma and the warm absorber gas share the same density and temperature. If there is a connection between the warm absorber gas and the forbidden high-ionization line (FHIL) plasma, one can use the profiles of coronal lines to derive the kinem...

We investigate how the fraction of broad-line sources in the AGN population changes with X-ray luminosity and redshift. We first construct the rest-frame hard-energy (2 − 8 keV) X-ray luminosity function (HXLF) at z = 0.1 − 1 using Chandra Lockman Hole-Northwest wide-area data, Chandra Deep Field-North 2 Ms data, other Chandra deep field data, and the ASCA Large Sky Survey data. We find that br...