An Improved Method for Estimating the Masses of Stars with Transiting Planets

To determine the physical parameters of a transiting planet and its host star from photometric and spectroscopic analysis, it is essential to independently measure the stellar mass. This is often achieved by the use of evolutionary tracks and isochrones, but the mass result is only as reliable as the models used. The recent paper by Torres et al (2009) showed that accurate values for stellar masses and radii could be obtained from a calibration using T_eff, log g and [Fe/H]. We investigate whether a similarly good calibration can be obtained by substituting log rho - the fundamental parameter measured for the host star of a transiting planet - for log g, and apply this to star-exoplanet systems. We perform a polynomial fit to stellar binary data provided in Torres et al (2009) to obtain the stellar mass and radius as functions of T_eff, log rho and [Fe/H], with uncertainties on the fit produced from a Monte Carlo analysis. We apply the resulting equations to measurements for seventeen SuperWASP host stars, and also demonstrate the application of the calibration in a Markov Chain Monte Carlo analysis to obtain accurate system parameters where spectroscopic estimates of effective stellar temperature and metallicity are available. We show that the calibration using log rho produces accurate values for the stellar masses and radii; we obtain masses and radii of the SuperWASP stars in good agreement with isochrone analysis results. We ascertain that the mass calibration is robust against uncertainties resulting from poor photometry, although a good estimate of stellar radius requires good-quality transit light curve to determine the duration of ingress and egress.Comment: 5 pages, 2 figures, accepted for publication in A&

The impact of COVID-19 lockdown measures on older residents' social connections and everyday wellbeing within housing schemes that provide care and support in England and Wales

The COVID-19 pandemic and the lockdown measures imposed as a result affected the lives of people in all parts of society across the world. In 2020, during the first UK national lockdown, older adults (aged 70 years and over) were told to ‘shield’ within their homes, as they were regarded as being at higher risk of serious COVID-19 infection compared to other age groups. This paper explores older adults' experiences of COVID-19 lockdown measures whilst living in housing with care schemes for older people. The purpose is to examine the impact of the lockdown measures on scheme life including social connections amongst residents and their general everyday wellbeing during this time. We present qualitative findings based on interviews with 72 residents who took part in longitudinal and cross-sectional interviews across 26 housing with care schemes. Data were analysed using a thematic framework approach to examine specifically their experiences of living in housing with care schemes during the 2020 UK lockdown. The paper highlights that COVID-19 restrictions had a detrimental impact on the social connections and interactions of older residents living in housing with care schemes, as well as on their feelings of autonomy and independence. Despite this, residents adapted and coped with self-isolation restrictions and sought out positive ways to maintain social contact with others inside and outside to the scheme. We further highlight the tensions that providers of housing for older adults faced in promoting residents' autonomy and connectedness whilst also trying to provide a safe living environment and protect residents from risk of COVID-19 infection. Our findings apply not only to a pandemic situation but to the broader understanding of how housing with care for older adults must navigate between autonomy and support

Globular Cluster Abundances from High-Resolution, Integrated-Light Spectroscopy. III. The Large Magellanic Cloud: Fe and Ages

In this paper we refine our method for the abundance analysis of high resolution spectroscopy of the integrated light of unresolved globular clusters (GCs). This method was previously demonstrated for the analysis of old ($>$10 Gyr) Milky Way GCs. Here we extend the technique to young clusters using a training set of 9 GCs in the Large Magellanic Cloud (LMC). Depending on the signal-to-noise ratio of the data, we use 20-100 Fe lines per cluster to successfully constrain the ages of old clusters to within a $\sim$5 Gyr range, the ages of $\sim$2 Gyr clusters to a 1-2 Gyr range, and the ages of the youngest clusters (0.05-1 Gyr) to a $\sim$200 Myr range. We also demonstrate that we can measure [Fe/H] in clusters with any age less than 12 Gyrs with similar or only slightly larger uncertainties (0.1-0.25 dex) than those obtained for old Milky Way GCs (0.1 dex); the slightly larger uncertainties are due to the rapid evolution in stellar populations at these ages. In this paper, we present only Fe abundances and ages. In the next paper in this series, we present our complete analysis of the $\sim 20$ elements for which we are able to measure abundances. For several of the clusters in this sample, there are no high resolution abundances in the literature from individual member stars; our results are the first detailed chemical abundances available. The spectra used in this paper were obtained at Las Campanas with the echelle on the du Pont Telescope and with the MIKE spectrograph on the Magellan Clay Telescope.Comment: 34 pages, accepted for publication in Ap

A bone of contention: A dynamic ultrasound assessment of the role of the radial head in the arthrokinematics of the proximal radioulnar joint

INTRODUCTION: The arthrokinematics of the proximal radioulnar joint (PRUJ) are believed to follow the convex-concave rule, meaning that when the convex radial head articulates with the concave radial notch on the ulna, rolling and gliding occur in opposite directions during forearm pronation and supination. Previous research using helical computerized tomography (CT) identified that the sequence of joint actions is in contrast with this rule, which would indicate a posterior glide of the radius on the ulna during pronation movement and the converse during supination. OBJECTIVES: The aims of this study are to determine the arthrokinematics of the PRUJ while being assessed via ultrasound (US) imaging and to assess the impact the direction of joint mobilization has on active and passive range of motion (ROM) during forearm supination and pronation at the PRUJ. METHODS: A convenience sample of 53 healthy individuals were recruited. The arthrokinematics of the PRUJ were observed via US cine-loops. A linear US transducer was applied in the transverse plane and placed over the radial head during all testing conditions. A metronome standardized the rate of forearm pronation and supination at 1Hz (60 bpm) during US cine-loops acquisition. Radial head motion was assessed in two different elbow positions during US and joint range of motion assessment. The elbow was flexed to 90° with a neutral forearm position and fully extended with a neutral forearm position. The glenohumeral joint was stabilized during all testing conditions. A repeated measures design randomizing joint mobilization direction to the radial head was utilized to assess forearm pronation and supination via inclinometer data measured in degrees. Joint glides were applied to the radial head according to the convex-concave rule to facilitate forearm supination and pronation. An anteromedial glide to facilitate forearm supination and a posterolateral glide to facilitate forearm pronation. A metronome standardized the rate of joint mobilization at a rate 2Hz (120 bpm). A bubble inclinometer assessed active and passive PRUJ ROM at the wrist during all testing conditions. RESULTS:US imaging cine-loops showed the radial head rolled anteromedially during pronation and posterolaterally during supination, with no translation/gliding evident. Multivariate analysis revealed that the direction of joint mobilization had a significant impact on ROM F(1,47.0)= 6.964, p=.011, partial η2 =.129), with anterior mobilization increasing pronation and posterior mobilization increasing supination. Supination ROM was significantly increased F1(1, 47.0) = 78.03, p CONCLUSION: Our findings are in conflict with the convex-concave rule, which is frequently used by physical therapists to improve joint motion. Should we now reconsider applying this rule to improve joint ROM at the PRUJ

Operation and performance of the OSSE instrument

The Oriented Scintillation Spectrometer Experiment (OSSE) on the Arthur Holly Compton Gamma Ray Observatory is described. An overview of the operation and control of the instrument is given, together with a discussion of typical observing strategies used with OSSE and basic data types produced by the instrument. Some performance measures for the instrument are presented that were obtained from pre-launch and in-flight data. These include observing statistics, continuum and line sensitivity, and detector effective area and gain stability

Rossiter-McLaughlin Effect Measurements for WASP-16, WASP-25 and WASP-31

We present new measurements of the Rossiter-McLaughlin (RM) effect for three WASP planetary systems, WASP-16, WASP-25 and WASP-31, from a combined analysis of their complete sets of photometric and spectroscopic data. We find a low amplitude RM effect for WASP-16 (Teff = 5700 \pm 150K), suggesting that the star is a slow rotator and thus of an advanced age, and obtain a projected alignment angle of lambda = -4.2 degrees +11.0 -13.9. For WASP-25 (Teff = 5750\pm100K) we detect a projected spin-orbit angle of lambda = 14.6 degrees \pm6.7. WASP-31 (Teff = 6300\pm100K) is found to be well-aligned, with a projected spin-orbit angle of lambda = 2.8degrees \pm3.1. A circular orbit is consistent with the data for all three systems, in agreement with their respective discovery papers. We consider the results for these systems in the context of the ensemble of RM measurements made to date. We find that whilst WASP-16 fits the hypothesis of Winn et al. (2010) that 'cool' stars (Teff < 6250K) are preferentially aligned, WASP-31 has little impact on the proposed trend. We bring the total distribution of the true spin-orbit alignment angle, psi, up to date, noting that recent results have improved the agreement with the theory of Fabrycky & Tremaine (2007) at mid-range angles. We also suggest a new test for judging misalignment using the Bayesian Information Criterion, according to which WASP-25 b's orbit should be considered to be aligned.Comment: 20 pages, 14 tables, 10 figures. Accepted to MNRA

In urban South Africa, 16 year old adolescents experience greater health equality than children

Despite the strongly established link between socio-economic status (SES) and health across most stages of the life-course, the evidence for a socio-economic gradient in adolescent health outcomes is less consistent. This paper examines associations between household, school, and neighbourhood SES measures with body composition outcomes in 16 year old South African Black urban adolescents from the 1990 born Birth to Twenty (Bt20) cohort. Multiple regression analyses were applied to data from a sub-sample of the Bt20 cohort (n=346, 53% male) with measures taken at birth and 16 years of age to establish socio-economic, biological and demographic predictors of fat mass, lean mass, and body mass index (BMI). Results were compared with earlier published evidence of health inequality at ages 9-10 years in Bt20. Consistent predictors of higher fat mass and BMI in fully adjusted models were being female, born post term, having a mother with post secondary school education, and having an obese mother. Most measures of SES were only weakly associated with body composition, with an inconsistent direction of association. This is in contrast to earlier findings with Bt20 9-10 year olds where SES inequalities in body composition were observed. Findings suggest targeting obesity interventions at females in households where a mother has a high BMI

Line-profile tomography of exoplanet transits I: The Doppler shadow of HD 189733b

We present a direct method for isolating the component of the starlight blocked by a planet as it transits its host star, and apply it to spectra of the bright transiting planet HD 189733b. We model the global shape of the stellar cross-correlation function as the convolution of a limb-darkened rotation profile and a gaussian representing the Doppler core of the average photospheric line profile. The light blocked by the planet during the transit is a gaussian of the same intrinsic width, whose trajectory across the line profile yields a precise measure of the misalignment angle and an independent measure of v sin I. We show that even when v sin I is less than the width of the intrinsic line profile, the travelling Doppler "shadow" cast by the planet creates an identifiable distortion in the line profiles which is amenable to direct modelling. Direct measurement of the trajectory of the missing starlight yields self-consistent measures of the projected stellar rotation rate, the intrinsic width of the mean local photospheric line profile, the projected spin-orbit misalignment angle, and the system's centre-of-mass velocity. Combined with the photometric rotation period, the results give a geometrical measure of the stellar radius which agrees closely with values obtained from high-precision transit photometry if a small amount of differential rotation is present in the stellar photosphere.Comment: 8 pages, 5 figures, 2 tables; accepted by MNRA

Associations between household and neighbourhood socioeconomic status and systolic blood pressure among urban South African adolescents.

Factors resulting in high risk for cardiovascular disease have been well studied in high income countries, but have been less well researched in low/middle income countries. This is despite robust theoretical evidence of environmental transitions in such countries which could result in biological adaptations that lead to increased hypertension and cardiovascular disease risk. Data from the South African Birth to Twenty cohort, Bone Health sub-sample (n = 358, 47% female), were used to model associations between household socioeconomic status (SES) in infancy, household/neighbourhood SES at age 16 years, and systolic blood pressure (multivariate linear regression) and risk for systolic pre-hypertension (binary logistic regression). Bivariate analyses revealed household/neighbourhood SES measures that were significantly associated with increased systolic blood pressure. These significant associations included improved household sanitation in infancy/16 years, caregiver owning the house in infancy and being in a higher tertile (higher SES) of indices measuring school problems/environment or neighbourhood services/problems/crime at 16 years of age. Multivariate analyses adjusted for sex, maternal age, birth weight, parity, smoking, term birth, height/body mass index at 16 years. In adjusted analyses, only one SES variable remained significant for females: those in the middle tertile of the crime prevention index had higher systolic blood pressure (β = 3.52, SE = 1.61) compared with the highest tertile (i.e. those with the highest crime prevention). In adjusted analyses, no SES variables were significantly associated with the systolic blood pressure of boys, or with the risk of systolic pre-hypertension in either sex. The lack of association between SES and systolic blood pressure/systolic pre-hypertension at age 16 years is consistent with other studies showing an equalization of adolescent health inequalities. Further testing of the association between SES and systolic blood pressure would be recommended in adulthood to see whether the lack of association persists