We demonstrate an implicit space mapping (ISM) method for microwave filter design that is enhanced and assisted by a tuning procedure. This procedure helps us to select design variables as well as suitable preassigned parameters for an ISM implementation. It also aids us in the convergence of our ISM algorithm. We investigated and solved a microstrip notch filter using this technique. This show...

The issue of information security management (ISM) had been widely studied with different approaches and from different perspectives. To have the right security objectives is the primary step to achieving an effective security program. Based on the contingency theory, a conceptual model of factors that determine ISM objectives was proposed. To validate this model, a webbased survey with open-en...

We present a preliminary study of using the template of an ensemble of evolving shells we developed for M 82 (Yao 2009). we apply the model to represent various stages of starburst evolution in a well known sample of nearby luminous infrared galaxies (LIRGs). In this way, we attempt to interpret the relationship between the degree of molecular excitation and ratio of far-infrared (FIR) to CO lu...

3 The Copernicus Era 19 3.1 Cloudy Sightlines: ζ Oph . . . . . . . . . . . . . . . . . . . . . . . . . . . . 20 3.2 Intercloud Material . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 23 3.3 Deuterium . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 24 3.4 The Distribution of Nearby Clouds . . . . . . . . . . . . . . . . . . . . . . . 25 3.5 Molecular Hy...

There are two existing avenues to interpreting the diffuse ISM: the theorist’s approach in which real data is interpreted numerically in the context of simulations, and the observer’s approach in which objects are found and categorized by eye. We are pioneering a middle way, following the fast-growing science of machine vision to extract shape information from complex maps of the diffuse Galact...

Aliphatic hydrocarbons exhibit an absorption feature at 3.4 m, observed toward sources that sample diffuse regions of the interstellar medium (ISM). The absorbers responsible for this feature are assumed to reside in some component of interstellar dust, but the physical nature of the particles (size, shape, structure, etc.) is uncertain. Observations of interstellar polarization provide discrim...

We present optical observations and 2D hydrodynamic modeling of an isolated shocked ISM cloud. Hα images taken in 1992.6 and 2003.7 of a small optical emission cloud along the southwestern limb of the Cygnus Loop were used to measure positional displacements of ∼ 0. 1 yr for surrounding Balmer dominated emission filaments and 0. 025 − . 055 yr for internal cloud emission features. These measure...