Professional appraisal of online information about children’s footwear measurement and fit : readability, usability and quality

Parents increasingly use the internet to seek health information, share information and for purchasing textiles and footwear. This shift in footwear purchasing habits raises concern about how (and if) parents are getting their children's feet measured, and what support strategies are in place to support the fit of footwear. In response to this, some companies and healthcare organisations have developed resources to support home measurement of foot size, and link these measures to footwear selection, measurement and fitting. The aim of this research was to undertake an appraisal of web-based resources about measurement and fit of children's footwear, focussing specifically on readability, usability and quality. Search terms relating to children's foot measurement were compiled and online searching was undertaken. Search results were saved and screened for relevance. Existing resources were categorised based on their source e.g. a footwear company or a health website. The 15 most commonly identified resources were reviewed by a professional panel for readability, content, usability and validity. One researcher also assessed the accessibility and reading ease of the resources. Online resources were predominantly from commercial footwear companies (54%). Health information sources from professional bodies made up 4.2% of the resources identified. The top 15 resources had appropriate reading ease scores for parents (SMOG Index 4.3-8.2). Accessibility scores (the product of the number of times it appeared in search results and its ranking in the results) were highest for commercial footwear companies. The panel scores for readability ranged from 2.7 to 9 out of 10, with a similar range for content, usability and validity. Information for parents seeking to purchase footwear for their children is readily available online but this was largely dominated by commercial footwear companies. The quality and usability of this information is of a moderate standard; notable improvements could be made to the validity of the task the child is asked to undertake and the measures being taken. Improvements in these resources would improve the data input to the selection of footwear and therefore have a beneficial impact on footwear fit in children. [Abstract copyright: © The Author(s). 2020.

International approaches to paediatric podiatry curricula : it's the same, but different

Pre-registration / entry-level programmes of study provide the core knowledge, skills and abilities required for clinical practice. These programmes are where students are introduced to specialist domains of practice and begin to shape their professional interests. The aim of this research was to describe paediatric curricula within pre-registration and entry level podiatry programmes across comparable universities and offer a contemporary synthesis of international practices. An exploratory, cross-sectional, online survey was undertaken across a three-month period. Representatives from podiatry programmes delivering pre-registration or entry level podiatry degrees in which graduates are eligible for Professional and Statutory Body registration within their country (deemed at a Bachelor degree or higher), were invited to participate. The survey was administered online using Online Surveys. Descriptive statistics were used to describe the data due to the exploratory nature of the research question and design. There were responses from seven (54% of 13) universities in the United Kingdom (UK), nine (100% of nine) universities in Australia and four (50% of eight) of the invited universities external to the UK and Australia (New Zealand, Malta, Ireland, South Africa). There was some variation in curriculum content, but all universities reported to cover ontogeny and developmental milestones and general paediatric orthopaedic conditions. There was further discrepancy with the number of hours dedicated to paediatric podiatry within the curricula (ranging from  26 h). The findings from this study highlight some disparity in the delivery of training for students relating to paediatrics. The data suggests that there is a need for international coordination in establishing priorities for the paediatric curricula. This will ensure consistency in baseline knowledge, modes of training, amount and nature of curriculum delivery during undergraduate or entry level podiatry training

Multiwavelength observations of the 2015 nova in the Local Group irregular dwarf galaxy IC 1613

A nova in the Local Group irregular dwarf galaxy IC 1613 was discovered on 2015 September 10 and is the first nova in that galaxy to be spectroscopically confirmed. We conducted a detailed multi-wavelength observing campaign of the eruption with the Liverpool Telescope, the LCO 2m telescope at Siding Spring Observatory, and Swift, the results of which we present here. The nova peaked at $M_V=-7.93\pm0.08$ and was fast-fading, with decline times of $t_{2(V)}=13\pm2$ and $t_{3(V)}=26\pm2$ days. The overall light curve decline was relatively smooth, as often seen in fast-fading novae. Swift observations spanned 40 days to 332 days post-discovery, but no X-ray source was detected. Optical spectra show the nova to be a member of the hybrid spectroscopic class, simultaneously showing Fe II and N II lines of similar strength during the early decline phase. The spectra cover the eruption from the early optically thick phase, through the early decline and into the nebular phase. The H$\gamma$ absorption minimum from the optically thick spectrum indicates an expansion velocity of $1200\pm200$ km s$^{-1}$. The FWHM of the H$\alpha$ emission line between 10.54 and 57.51 days post-discovery shows no significant evolution and remains at $\sim1750$ km s$^{-1}$, although the morphology of this line does show some evolution. The nova appears close to a faint stellar source in archival imaging, however we find the most likely explanation for this is simply a chance alignment

Harris Williams Collection - Accession 1234

The C. Harris Williams Collection consists of newspaper clippings and photographs pertaining to the 1952 Rock Hill Centennial Celebration. C. Harris Williams (1912-1960) was a Rock Hill, SC resident, owner of the Williams Gulf Station in Rock Hill, and was a member of the Brothers of the Brush. Most of the photographs in the collection are of Mr. Williams and fellow members of the Brothers of the Bush participating in the 1952 Rock Hill Centennial events and include images of skits, parades, Rock Hill citizens, and Rock Hill Main Street and Downtown. There is also an original photograph of a cotton scene on Main Street in Rock Hill in the early 1900s (possibly 1911). The collection also includes several newspaper clippings related to the Centennial Celebration.https://digitalcommons.winthrop.edu/manuscriptcollection_findingaids/1995/thumbnail.jp

Ultra-brief non-expert-delivered defusion and acceptance exercises for food cravings: A partial replication study

Food cravings are a common barrier to losing weight. This paper presents a randomised comparison of non-expert group-delivered ultra-brief defusion and acceptance interventions against a distraction control. Sixty-three participants were asked to carry a bag of chocolates for a week whilst trying to resist the temptation to eat them. A behavioural rebound measure was administered. Each intervention out-performed control in respect of consumption, but not cravings. These techniques may have a place in the clinical management of food cravings. We provide tentative evidence that the mechanism of action is through decreased reactivity to cravings, not through reduced frequency of cravings

First steps : parent health behaviours related to children’s foot health

Good foot health throughout childhood is important but remains poorly understood with few studies exploring this topic. The aim of this study was to define parents’ knowledge, practices and health-related perceptions of children’s feet. A qualitative design was adopted. Semi-structured, one-to-one interviews were carried out with parents of children aged five years and under, recruited from South East and North West of England. Interviews explored parents’ views, beliefs and understanding of foot health in infancy and early childhood. Transcripts of the interviews were analysed using thematic analysis. Eighteen interviews were conducted. Seven themes were identified relating to (1) parents belief and knowledge about children’s foot health; (2) how parents use and share foot health information; (3) activities for supporting foot health and development; (4) footwear choices, beliefs and influences; (5) the way they access health professionals; (6) the way they search for foot health information and (7) developing practice(s) to support parents. The study provides the first insight into how parents view foot health in early infancy and childhood. The findings highlight the key foot health beliefs important to parents, how they learn about and what influences their decision-making about caring for children’s feet, the way parents receive and seek information, and how they access support for foot health concerns. The findings highlight the need for accurate, clear and consistent foot health messages, and the important role health professionals have in signposting parents towards reliable and informative sources on foot health

Customer satisfaction as a performance measurement and management tool in English social housing

Customer satisfaction measurement is argued to be the ultimate arbiter of the success of public organisations (Hill et al 2007). Despite being a regulatory requirement for English social housing providers to measure customer satisfaction throughout the 2000’s and remaining relevant after sector de-regulation in 2010 (Williams 2013), it is surprising there is little academic literature underpinning quality of service and customer satisfaction within English social housing. This study meets this gap by presenting the first academic research exploring the empirical evidence underpinning the relationship between customer satisfaction and service quality orientated business performance in the UK social housing sector

A Luminous Red Nova in M31 and its Progenitor System

We present observations of M31LRN 2015 (MASTER OT J004207.99+405501.1), discovered in M31 in January 2015, and identified as a rare and enigmatic luminous red nova (LRN). Spectroscopic and photometric observations obtained by the Liverpool Telescope showed the LRN becoming extremely red as it faded from its M(V) = -9.4 +/- 0.2 peak. Early spectra showed strong Halpha emission that weakened over time as a number of absorption features appeared, including Na I D and Ba II. At later times strong TiO absorption bands were also seen. A search of archival Hubble Space Telescope data revealed a luminous red source to be the likely progenitor system, with pre-outburst Halpha emission also detected in ground-based data. The outburst of M31LRN 2015 shows many similarities, both spectroscopically and photometrically, with that of V838 Mon, the best studied LRN. We finally discuss the possible progenitor scenarios

On the Progenitors of Local Group Novae. II. The Red Giant Nova Rate of M31

In our preceding paper, Liverpool Telescope data of M31 novae in eruption were used to facilitate a search for their progenitor systems within archival Hubble Space Telescope (HST) data, with the aim of detecting systems with red giant secondaries (RG-novae) or luminous accretion disks. From an input catalog of 38 spectroscopically confirmed novae with archival quiescent observations, likely progenitors were recovered for eleven systems. Here we present the results of the subsequent statistical analysis of the original survey, including possible biases associated with the survey and the M31 nova population in general. As part of this analysis we examine the distribution of optical decline times (t(2)) of M31 novae, how the likely bulge and disk nova distributions compare, and how the M31 t(2) distribution compares to that of the Milky Way. Using a detailed Monte Carlo simulation, we determine that 30 (+13/-10) percent of all M31 nova eruptions can be attributed to RG-nova systems, and at the 99 percent confidence level, >10 percent of all M31 novae are RG-novae. This is the first estimate of a RG-nova rate of an entire galaxy. Our results also imply that RG-novae in M31 are more likely to be associated with the M31 disk population than the bulge, indeed the results are consistent with all RG-novae residing in the disk. If this result is confirmed in other galaxies, it suggests any Type Ia supernovae that originate from RG-nova systems are more likely to be associated with younger populations, and may be rare in old stellar populations, such as early-type galaxies

Extragalactic Novae and Their Progenitors

Novae are binary systems containing a white dwarf (WD) and a less-evolved companion star, either a main-sequence, sub-giant or red giant star. The WD accretes matter from the companion through Roche lobe overflow or via a stellar wind. As material is accreted, the pressure and temperature at the base of the accreted envelope increase until a thermonuclear runaway occurs. This causes a sudden increase in brightness (the outburst), which ranks among the most luminous stellar astrophysical phenomena.Following the outburst, some novae form detectable dust in the ejecta. Observationally, there is a correlation between the dust-formation timescale and the time it takes the nova to fade optically by two magnitudes, which was emphasised in a study of infrared emission from novae in the Andromeda Galaxy (M31). In the first part of this thesis, a simple theoretical model is presented, which considers the higher-energy photons produced by the nova being absorbed by neutral hydrogen in the ejecta, before they can reach the potential dust-formation sites. This new model successfully replicates the observed trend between these two parameters and agrees well with the observational data.The majority of novae are thought to consist of a WD and a main-sequence star, although some systems harbour a sub-giant (SG-novae) or red giant (RG-novae) companion instead. In the Milky Way galaxy, relatively few RG-novae have been confirmed, although in many systems, the evolutionary state of the secondary is simply not known. There is evidence that the progenitors of some Type Ia supernovae (SNe Ia) may be RG-nova systems (e.g. SN PTF11kx), therefore it is important to understand the population of such systems. In this thesis, archival Hubble Space Telescope (HST) data are used to search for RG-novae in M31. Many more novae are discovered in M31 each year (~30) than in the Milky Way (~10). Distance determination is a major complication when studying Galactic novae. However, at the distance of M31 all the novae may be considered to be at the same distance, making M31 an excellent environment for studying nova populations.We conducted a survey of 38 spectroscopically confirmed M31 novae in quiescence. We determined that 11 of these systems had a coincident progenitor candidate whose probability of being a chance alignment with a resolved source in the HST data was ≤5%. As the main sequence and the majority of the sub-giant branch are not resolvable in the HST data, this implies that a significant proportion of these systems contain red giant secondaries. The light curves of several M31 novae are also presented here, some of which use HST data to extend the light curves far deeper than is typically possible for extragalactic systems.A statistical study was then carried out to test the results of the survey and derive an estimate of the proportion of M31 novae associated with a resolved source in the HST data. This includes, for example, models of the spatial distribution, speed class and peak magnitude of the M31 nova population, as well as considering biases introduced by the HST coverage of M31. The initial results suggest about 0.38 of M31 novae are associated with a source in the HST data, a class of objects expected to be dominated by RG-novae. This is a much greater proportion than that observed so far in our Galaxy, and will be important when considering such systems as potential SN Ia candidates. The spatial distribution of novae that have resolved progenitor candidates is consistent with these systems being associated with the M31 disk, rather than the bulge.The method used to locate the progenitors of M31 novae was also used to study three additional systems. The M31 nova, M31N 2008-12a, which appears to be a recurrent nova (RN) with a very short inter-outburst period, produced an outburst in November 2013. This outburst was studied and a candidate progenitor system was found in HST data when it was apparently in quiescence, supporting its classification as a RN with a high accretion rate. The method was also used to explore upper limits on the brightness of the progenitor of SN 2014J, a SN Ia in M82, although no progenitor was found, a RG-nova (or in-fact any type of system) could not be ruled out due to the limitations of the data. For the M31 transient TCP J00403295+4034387, which showed an unusual spectrum, archival HST data were used to show the object was probably a blend of two objects with a very small apparent separation. Finally, the thesis is summarised, and future work on both dust formation and the progenitor search are discussed