Quality Services, Better Outcomes: A Quality Framework for Achieving Outcomes.

The Childhood Development Initiative (CDI) is an innovative, community based response to a comprehensive consultation process undertaken in Tallaght West. Working with a wide range of locally established service providers, CDI is delivering services to children and families which meet identified needs. Etch of these is being rigorously evaluated, and considerable attention is being given to quality assurance, promotion of reflective practice, and professional training and support. The insights gained, and techniques developed during this process are central to delivering high quality services with the view to improving our understanding of what enables children to meet their potential, gain their developmental milestones within appropriate timeframes and become healthy and active citizens. This Workbook describes key processes relating to practice, organisational culture and systems change which support the implementation of evidence-based and evidence-informed programmes and practices. From CDI's experience, implementing evidence-based programmes not only requires specific structures and processes in place to support programme implementation and fidelity (e.g. training, coaching, and supervision) but also necessities a focus on the more generic aspects of delivering quality services (e.g. engaging in reflective practice in order to promote and maintain fidelity to a programme). The Workbook also addresses some fundamental areas in relation to monitoring and evaluation as a way of determining whether an intervention was effective or not. In effect, this Workbook hopes to explain the 'what', 'why', 'how' and 'did we?' of evidence-based practice. The Workbook is intended to provide readers with a comprehensive introduction to both the shared language and concepts underpinning the science and practice of implementation. It complements the 'What Works Process' guide published by the Centre for Effective Services (CES, 2011) which supports services in assessing how effective they are in improving outcomes for children and helps them to think about what works

What are some Best-in-Class Examples of Corporate Cultures and Values Brought-to-Life in Workplace Behaviors that drove Clear Business Results?

Prominent workplace culture and values have been proven to strengthen employee loyalty time and again, yet there is still a need to understand how these nebulous ideas translate into real business practices. Culture can be the driving force in connecting employees directly to the mission of the company, and therefore creating results for all company stakeholders including employees, customers, and shareholders. But in order to produce these outcomes, companies must create values that represent the workplace culture they want to achieve and have merit and teeth, which requires what the Harvard Business Review refers to as “guts”

Spectral properties of stars and stellar populations

I present the results of an investigation into the spectral properties of stars and galaxies. Firstly I investigate methods for automatic MKK classification of stellar spectra, providing both a comparative study of some of the standard methods of automatic classification and a demonstration of a state-of-the-art machine learning technique — Support Vector M achines. Using this technique I obtain a classification accuracy of δ = 1.7.One of the limitations in the classification of stellar spectra is the lack of good training data at high resolution. With this and also the application of population synthesis in mind, I present a high resolution (λ/Δλ = 250000) library of 6410 synthetic stellar spectra which I have generated from the Kurucz model atmospheres. The library covers the wavelength range 3000 - 10 000 with 54 values of effective temperature in the range 5250 - 50 000 K, 11 values of log surface gravity between 0.0 and 5.0 and 19 metallicities in the range - 5 .0 to 1.0. By com paring the new synthetic spectra with the STELIB library of observed spectra (Le Borgne et al., 2003) I demonstrate their suitability for the application of population synthesis.I then extend this library by supplementing the Kurucz spectra with other synthetic spectra, to form a library for population synthesis similar to that of Lejeune et al. (1998) but at higher resolution (2 ). I also investigate two methods of empirical population synthesis however I find that even with modern computational resources these methods are not suitable for the number and size of current spectra.Finally I measure the Lick indices for a sample of Sloan Digital Sky Survey spectra and use these in conjunction with the 2dF groups catalogue to investigate the change in these parameters with the local density of galaxies. I find no strong trends in any of the Lick indices with group velocity dispersion

Online classification for time-domain astronomy

The advent of synoptic sky surveys has spurred the development of techniques for real-time classification of astronomical sources in order to ensure timely follow-up with appropriate instruments. Previous work has focused on algorithm selection or improved light curve representations, and naively convert light curves into structured feature sets without regard for the time span or phase of the light curves. In this paper, we highlight the violation of a fundamental machine learning assumption that occurs when archival light curves with long observational time spans are used to train classifiers that are applied to light curves with fewer observations. We propose two solutions to deal with the mismatch in the time spans of training and test light curves. The first is the use of classifier committees where each classifier is trained on light curves of different observational time spans. Only the committee member whose training set matches the test light curve time span is invoked for classification. The second solution uses hierarchical classifiers that are able to predict source types both individually and by sub-group, so that the user can trade-off an earlier, more robust classification with classification granularity. We test both methods using light curves from the MACHO survey, and demonstrate their usefulness in improving performance over similar methods that naively train on all available archival data.Comment: Astroinformatics workshop, IEEE International Conference on Data Mining 201

VAST: An ASKAP Survey for Variables and Slow Transients

The Australian Square Kilometre Array Pathfinder (ASKAP) will give us an unprecedented opportunity to investigate the transient sky at radio wavelengths. In this paper we present VAST, an ASKAP survey for Variables and Slow Transients. VAST will exploit the wide-field survey capabilities of ASKAP to enable the discovery and investigation of variable and transient phenomena from the local to the cosmological, including flare stars, intermittent pulsars, X-ray binaries, magnetars, extreme scattering events, interstellar scintillation, radio supernovae, and orphan afterglows of gamma-ray bursts. In addition, it will allow us to probe unexplored regions of parameter space where new classes of transient sources may be detected. In this paper we review the known radio transient and variable populations and the current results from blind radio surveys. We outline a comprehensive program based on a multi-tiered survey strategy to characterise the radio transient sky through detection and monitoring of transient and variable sources on the ASKAP imaging timescales of 5 s and greater. We also present an analysis of the expected source populations that we will be able to detect with VAST

Ultra- and Hyper-compact HII regions at 20 GHz

We present radio and infrared observations of 4 hyper-compact HII regions and 4 ultra-compact HII regions in the southern Galactic plane. These objects were selected from a blind survey for UCHII regions using data from two new radio surveys of the southern sky; the Australia Telescope 20 GHz survey (AT20G) and the 2nd epoch Molonglo Galactic Plane Survey (MGPS-2) at 843 MHz. To our knowledge, this is the first blind radio survey for hyper- and ultra-compact HII regions. We have followed up these sources with the Australia Telescope Compact Array to obtain H70-alpha recombination line measurements, higher resolution images at 20 GHz and flux density measurements at 30, 40 and 95 GHz. From this we have determined sizes and recombination line temperatures as well as modeling the spectral energy distributions to determine emission measures. We have classified the sources as hyper-compact or ultra-compact on the basis of their physical parameters, in comparison with benchmark parameters from the literature. Several of these bright, compact sources are potential calibrators for the Low Frequency Instrument (30-70 GHz) and the 100-GHz channel of the High Frequency Instrument of the Planck satellite mission. They may also be useful as calibrators for the Australia Telescope Compact Array, which lacks good non-variable primary flux calibrators at higher frequencies and in the Galactic plane region. Our spectral energy distributions allow the flux densities within the Planck bands to be determined, although our high frequency observations show that several sources have excess emission at 95 GHz (3 mm) that can not be explained by current models.Comment: 13 pages, 7 figures, accepted for publication in MNRA

Using the VO to Study the Time Domain

Just as the astronomical "Time Domain" is a catch-phrase for a diverse group of different science objectives involving time-varying phenomena in all astrophysical regimes from the solar system to cosmological scales, so the "Virtual Observatory" is a complex set of community-wide activities from archives to astroinformatics. This workshop touched on some aspects of adapting and developing those semantic and network technologies in order to address transient and time-domain research challenges. It discussed the VOEvent format for representing alerts and reports on celestial transient events, the SkyAlert and ATELstream facilities for distributing these alerts, and the IVOA time-series protocol and time-series tools provided by the VAO. Those tools and infrastructure are available today to address the real-world needs of astronomers.Comment: Contribution to the proceedings of IAU Symposium 285, "New Horizons in Time Domain Astronomy": http://www.physics.ox.ac.uk/IAUS285/, 6 page