We present the first images of the pulsar wind nebula (PWN) MSH 15−52 in the hard X-ray band (> ∼8 keV), as measured with the Nuclear Spectroscopic Telescope Array (NuSTAR). Overall, the morphology of the PWN as measured by NuSTAR in the 3–7 keV band is similar to that seen in Chandra high-resolution imaging. However, the spatial extent decreases with energy, which we attribute to synchrotron e...

We study the physical properties derived from interstellar cloud complexes having a fractal structure. We first generate fractal clouds with a given fractal dimension and associate each clump with a maximum in the resulting density field. Then, we discuss the effect that different criteria for clump selection has on the derived global properties. We calculate the masses, sizes and average densi...

Recent H i surveys of the Large Magellanic Cloud (LMC) with the Australia Telescope Compact Array (Kim et al. 1998) and the Parkes multibeam receiver (Staveley-Smith et al. 2003) have focussed, respectively, on the small-scale (< 20) structure of the interstellar medium (ISM) and the large-scale (> 1) structure of the galaxy. Using a Fourier-plane technique, we have merged both data sets provid...

Context. Supernova remnants (SNR) are one of the main sources galactic cosmic rays acceleration. This acceleration, believed to happen at blast wave front, leads an energy loss shock front. results in apparent proximity between and contact discontinuity. Aims. In this article, we study effect that turbulent-like density perturbations interstellar medium (ISM) have on evolution young SNRs. We fo...

We use the standard, adiabatic shell evolution to predict the size distribution N (R) for populations of SN-driven superbubbles in a uniform ISM. We derive N (R) for simple cases of superbubble creation rate and mechanical luminosity function. We then compare our predictions for N (R) with the largely complete H i hole catalogue for the SMC, with a view toward the global structure of the ISM in...

We use the standard, adiabatic shell evolution to predict the size distribution N(R) for populations of SN-driven superbubbles in a uniform ISM. We derive N(R) for simple cases of superbubble creation rate and mechanical luminosity function. We then compare our predictions for N(R) with the largely complete H i hole catalogue for the SMC, with a view toward the global structure of the ISM in th...

We extract and analyze the decision factors of introducing image information system by ISM (Interpretive Structural Modeling) method to determine the criteria and structure for system selection. As a result, 15 factors were extracted, and the structure and relation among factors became clear.

We investigate the structure of self-gravitating polytropic stellar systems. We present a method which allows to obtain approximate analytical solutions, ψn+ǫ(x), of the nonlinear Poisson equation with the polytropic index n+ ǫ, given the solution ψn(x) with the polytropic index n, for any positive or negative ǫ such that |ǫ| ≪ 1. Application of this method to the spherically symmetric stellar ...

VLA observations of large-scale HI and OH absorption in the merging galaxy of NGC6240 are presented with 1 arcsec resolution. HI absorption is found across large areas of the extended radio continuum structure with a strong concentration towards the double-nucleus. The OH absorption is confined to the nuclear region. The HI and OH observations identify fractions of the gas disks of the two gala...