The Role of Project Modularity in Information Systems Development

Recent surveys have shown that ISD project success rates are particularly low. Organizations are applying a wide array of information systems development methodologies (ISDMs) -- both plan-based and agile, such as waterfall, scrum and XP -- to improve information systems development (ISD) performance. However, as ISD projects often have different characteristics such as size, scope and complexity, prior studies have been focused on helping organizations better choose an ISDM for projects. Nevertheless, prior research has not taken into consideration the notion of problem modularity of ISD projects. In this study, we utilize the NK fitness landscapes model to computationally examine via computer simulations the effects of problem modularity alongside various project environmental factors, and aim to answer the question: under various environmental factors, which ISDM should an ISD team adopt under various degree of problem modularity

Halo-to-Halo Similarity and Scatter in the Velocity Distribution of Dark Matter

We examine the Velocity Distribution Function (VDF) in dark matter halos from Milky Way to cluster mass scales. We identify an empirical model for the VDF with a wider peak and a steeper tail than a Maxwell--Boltzmann distribution, and discuss physical explanations. We quantify sources of scatter in the VDF of cosmological halos and their implication for direct detection of dark matter. Given modern simulations and observations, we find that the most significant uncertainty in the VDF of the Milky Way arises from the unknown radial position of the solar system relative to the dark matter halo scale radius.Comment: Accepted to ApJ. Figure 3 and 5 and Section 4 newly added. 6 pages, 6 figures, typeset using emulateap

RHAPSODY-G simulations II - Baryonic growth and metal enrichment in massive galaxy clusters

We study the evolution of the stellar component and the metallicity of both the intracluster medium and of stars in massive ($M_{\rm vir}\approx 6\times 10^{14}$ M$_{\odot}/h$) simulated galaxy clusters from the Rhapsody-G suite in detail and compare them to observational results. The simulations were performed with the AMR code RAMSES and include the effect of AGN feedback at the sub-grid level. AGN feedback is required to produce realistic galaxy and cluster properties and plays a role in mixing material in the central regions and regulating star formation in the central galaxy. In both our low and high resolution runs with fiducial stellar yields, we find that stellar and ICM metallicities are a factor of two lower than in observations. We find that cool core clusters exhibit steeper metallicity gradients than non-cool core clusters, in qualitative agreement with observations. We verify that the ICM metallicities measured in the simulation can be explained by a simple "regulator" model in which the metallicity is set by a balance of stellar yield and gas accretion. It is plausible that a combination of higher resolution and higher metal yield in AMR simulation would allow the metallicity of simulated clusters to match observed values; however this hypothesis needs to be tested with future simulations. Comparison to recent literature highlights that results concerning the metallicity of clusters and cluster galaxies might depend sensitively on the scheme chosen to solve the hydrodynamics.Comment: 22 pages, 11 figures, 2 tables. Accepted for publication on MNRA

Rhapsody-G simulations: galaxy clusters as baryonic closed boxes and the covariance between hot gas and galaxies

Within a sufficiently large cosmic volume, conservation of baryons implies a simple `closed box' view in which the sum of the baryonic components must equal a constant fraction of the total enclosed mass. We present evidence from Rhapsody-G hydrodynamic simulations of massive galaxy clusters that the closed-box expectation may hold to a surprising degree within the interior, non-linear regions of haloes. At a fixed halo mass, we find a significant anti-correlation between hot gas mass fraction and galaxy mass fraction (cold gas + stars), with a rank correlation coefficient of -0.69 within $R_{500c}$. Because of this anti-correlation, the total baryon mass serves as a low-scatter proxy for total cluster mass. The fractional scatter of total baryon fraction scales approximately as $0.02 (\Delta_c/100)^{0.6}$, while the scatter of either gas mass or stellar mass is larger in magnitude and declines more slowly with increasing radius. We discuss potential observational tests using cluster samples selected by optical and hot gas properties; the simulations suggest that joint selection on stellar and hot gas has potential to achieve 5% scatter in total halo mass.Comment: 10 pages, 6 figures, 3 tables; replaced to match published versio

The Role of Online Peer-to-Peer Lending in Crisis Response: Evidence from Kiva

Online peer-to-peer (P2P) lending, a new form of microfinance, has been touted as to its prominent potential for reducing world poverty. Although a growing body of research has been devoted to examining online P2P lending, how such platforms actually make a difference in curbing poverty has yet to be fully explored. The Ebola outbreak of 2014 provides us a unique empirical opportunity to explore such broader impacts of online P2P lending. We investigate how the demand and supply sides of P2P lending platforms react to an unpredictable crisis. Employing a difference-in-difference identification strategy with data from Kiva.org, we conduct country- and loan-level estimations. Results show upward trends on both demand and supply sides of P2P lending; borrowers request more financial capital and lenders are more active in their lending behaviors in the post-crisis period. We extend online P2P lending literature by investigating the influences of “off-platform shocks on within-platform behaviors

Dry etching of ZnO films and plasma-induced damage to optical properties

To study the effects of plasma chemistries on etch characteristics. and plasma-induced damage to the optical properties, dry etching of ZnO films has been carried out using inductively coupled plasmas of Cl-2 /Ar, Cl-2 /H-2 /Ar, and CH4 /H-2 /Ar. The CH4 /H-2 /Ar chemistry showed a faster etch rate and a better surface morphology than the Cl-2-based chemistries. Etched samples in all chemistries showed a substantial decrease in the PL intensity of band-edge luminescence mainly due to the plasma-induced damage. The CH4 /H-2 /Ar chemistry showed the least degradation of the optical properties. (C) 2003 American Vacuum Society. [DOI: 10.1116/1.1563252].open1139sciescopu

Hahn echo and criticality in spin-chain systems

We establish a relation between Hahn spin-echo of a spin-$\frac 1 2$ particle and quantum phase transition in a spin-chain, which couples to the particle. The Hahn echo is calculated and discussed at zero as well as at finite temperatures. On the example of XY model, we show that the critical points of the chain are marked by the extremal values in the Hahn echo, and influence the Hahn echo in surprising high temperature. An explanation for the relation between the echo and criticality is also presented.Comment: 5 pages, 6 figure

ISCASMC: A Web-Based Probabilistic Model Checker

We introduce the web-based model checker iscasMc for probabilistic systems (see http://iscasmc.ios.ac.cn/IscasMC). This Java application offers an easy-to-use web interface for the evaluation of Markov chains and decision processes against PCTL and PCTL specifications. Compared to PRISM or MRMC, iscasMc is particularly efficient in evaluating the probabilities of LTL properties. © 2014 Springer International Publishing Switzerland.We introduce the web-based model checker iscasMc for probabilistic systems (see http://iscasmc.ios.ac.cn/IscasMC). This Java application offers an easy-to-use web interface for the evaluation of Markov chains and decision processes against PCTL and PCTL specifications. Compared to PRISM or MRMC, iscasMc is particularly efficient in evaluating the probabilities of LTL properties. © 2014 Springer International Publishing Switzerland

Rhapsody. I. Structural Properties and Formation History From a Statistical Sample of Re-simulated Cluster-size Halos

We present the first results from the Rhapsody cluster re-simulation project: a sample of 96 "zoom-in" simulations of dark matter halos of 10^14.8 +- 0.05 Msun/h, selected from a 1 (Gpc/h)^3 volume. This simulation suite is the first to resolve this many halos with ~5x10^6 particles per halo in the cluster-mass regime, allowing us to statistically characterize the distribution of and correlation between halo properties at fixed mass. We focus on the properties of the main halos and how they are affected by formation history, which we track back to z=12, over five decades in mass. We give particular attention to the impact of the formation history on the density profiles of the halos. We find that the deviations from the Navarro-Frenk-White (NFW) model and the Einasto model depend on formation time. Late-forming halos tend to have considerable deviations from both models, partly due to the presence of massive subhalos, while early-forming halos deviate less but still significantly from the NFW model and are better described by the Einasto model. We find that the halo shapes depend only moderately on formation time. Departure from spherical symmetry impacts the density profiles through the anisotropic distribution of massive subhalos. Further evidence of the impact of subhalos is provided by analyzing the phase-space structure. A detailed analysis of the properties of the subhalo population in Rhapsody is presented in a companion paper.Comment: 20 pages, 13 figures, replaced to match published versio

Detecting variability in massive astronomical time-series data. II. Variable candidates in the Northern Sky Variability Survey

We present variability analysis of data from the Northern Sky Variability Survey (NSVS). Using the clustering method, which defines variable candidates as outliers from large clusters, we cluster 16,189,040 light curves having data points at more than 15 epochs as variable and non-variable candidates in 638 NSVS fields. Variable candidates are selected depending on how strongly they are separated from the largest cluster and how rarely they are grouped together in eight-dimensional space spanned by variability indices. All NSVS light curves are also cross-correlated with IRAS, AKARI, Two Micron All Sky Survey, Sloan Digital Sky Survey (SDSS), and GALEX objects, as well as known objects in the SIMBAD database. The variability analysis and cross-correlation results are provided in a public online database, which can be used to select interesting objects for further investigation. Adopting conservative selection criteria for variable candidates, we find about 1.8 million light curves as possible variable candidates in the NSVS data, corresponding to about 10% of our entire NSVS sample. Multi-wavelength colors help us find specific types of variability among the variable candidates. Moreover, we also use morphological classification from other surveys such as SDSS to suppress spurious cases caused by blending objects or extended sources due to the low angular resolution of the NSV