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To better understand barriers to participation in mail-out bowel cancer screening programs, two survey studies tested the relationship between psychological distress and self-reported bowel cancer screening.First, a nationally representative sample of Australians N = 5421 completed measures of bowel cancer screening and psychological distress (using the Kessler Psychological Distress Scale; K10). Second, N = 479 completed a survey measuring participation in the National Bowel Cancer Screening Program (NBCSP) and psychological distress using the Depression, Anxiety and Stress Scale. In both studies, logistic regressions were conducted to test relationships between psychological distress and self-reported screening participation.Study one found that psychological distress had a significant quadratic effect on having ever screened for bowel cancer, where screening rates were similar for those with low, moderate, or high levels of distress, but were lower for those with very high levels of distress. In study two, depression scores had a negative linear relationship with NBCSP participation (higher depression levels were associated with lower screening participation), and anxiety had a quadratic effect whereby NBCSP participation rates were higher with increasing levels of anxiety except in the severe category, where participation was significantly lower.Findings indicate that psychological distress has a complex relationship with screening, and those with extreme levels of distress consistently show lower participation rates. Special efforts to encourage screening may be required for those experiencing extreme psychological distress and mental health disorders.

To examine the relationships between need for control and self-reliance and barriers to bowel cancer screening to better understand the reasons for lower bowel cancer screening adherence in males and younger individuals.Participants (n = 506) aged between 54 and 75 years old completed an online survey measuring demographic information, the four-factor Barriers to Home Bowel Cancer Screening Scale (BB-CanS) and a measure of Need for Control and Self-Reliance (NCSR). Model fit statistics were compared for seven path models testing the relationships between NCSR and BB-CanS factors and the moderating and mediating effects of age and gender.Models where age and gender were included as moderators showed the best fit. When compared to females and those under 60 years of age, stronger positive associations between NCSR and BB-CanS factors were evident among males (βsubavoidance/sub = 0.539, p lt; 0.001); βsubdisgust/sub = 0.558, p lt; 0.001; βsubdifficulty/sub = 0.489, p lt; 0.001; βsubautonomy/sub = 0.619, p = 0.002) and those over 60 years of age (βsubavoidance/sub = 0.400, p lt; 0.001); βsubdisgust/sub = 0.462, p lt; 0.001; βsubdifficulty/sub = 0.447, p lt; 0.001; βsubautonomy/sub = 0.378, p lt; 0.001.When encouraging males and people aged 60 years and over to participate in bowel cancer screening, public health messages may benefit from conveying preventative health behaviour and cancer screening participation as actions that reflect self-control and self-reliance.

The present study aimed to provide the first psychometric evaluation of the newly developed, digitally animated assessment instrument: the Interactive Child Distress Screener ( ICDS). The latent factor structure of the novel ICDS was first established using exploratory factor analysis (EFA) on 15 pairs of animated items using a community sample ( N = 266) of child–parent dyads. EFA results support a two-factor structure representing two broad domains of internalizing and externalizing difficulties ( r = .52) and comprised 12 items. The reliability of the factors was strong with ordinal alpha and omega coefficients above .84 and .87, respectively, for each of the subscales. Convergent validity for the overall sample was supported with established child and parent-reported measures of internalizing and externalizing problems; however, the ICDS factors demonstrated convergence greater in magnitude with other child-reported measures such as the Me and My School Survey. Satisfaction and utility ratings by children indicated that the digital format was highly acceptable.

Planet formation is often considered in the context of one circumstellar disk around one star. Yet stellar binary systems are ubiquitous, and thus a substantial fraction of all potential planets must form and evolve in more complex, dynamical environments. We present the results of a five-year astrometric monitoring campaign studying 45 binary star systems that host Kepler planet candidates. The planet-forming environments in these systems would have literally been shaped by the binary orbits that persist to the present day. Crucially, the mutual inclinations of star-planet orbits can only be addressed by a statistical sample. We describe in detail our sample selection and Keck/NIRC2 laser guide star adaptive optics observations collected from 2012 to 2017. We measure orbital arcs, with a typical accuracy of ~0.1 mas/yr, that test whether the binary orbits tend to be aligned with the edge-on transiting planet orbits. We rule out randomly-distributed binary orbits at 4.7$\sigma$, and we show that low mutual inclinations are required to explain the observed orbital arcs. If the stellar orbits have a field binary-like eccentricity distribution, then the best match to our observed orbital arcs is a distribution of mutual inclinations ranging from 0-30 degrees. We discuss the implications of such widespread planet-binary alignment in the theoretical context of planet formation and circumstellar disk evolution., Comment: Accepted to MNRAS

The formation of giant planets is best studied through direct imaging by observing planets both during and after formation. Giant planets are expected to form either by core accretion, which is typically associated with low initial entropy (cold-start models) or by gravitational instability, which corresponds to a high initial entropy of the gas (hot-start models). Thus, constraining the initial entropy provides insight into the planet formation mechanism and determines the resultant brightness evolution. We find that, by observing planets in nearby moving groups of known age both through direct imaging and astrometry with Gaia, it will be possible to constrain the initial entropy of giant planets. We simulate a set of planetary systems in stars in nearby moving groups identified by BANYAN $\Sigma$ and assume a model for planet distribution consistent with radial velocity detections. We find that Gaia should be able to detect approximately 50% of planets in nearby moving groups greater than ~0.3 M$_\text{J}$. Using 5$\sigma$ contrast limits of current and future instruments, we calculate the flux uncertainty, and using models for the evolution of the planet brightness, we convert this to an initial entropy uncertainty. We find that, for future instruments such as MICADO and METIS on E-ELT and VIKiNG with VLTI, the entropy uncertainty is less than 0.5 $k_{B}$/baryon, showing that these instruments should be able to distinguish between hot and cold-start models., Comment: Final version, submitted to MNRAS

To accurately assess children’s emotional and behavioral distress via self-report, we must design instruments that are meaningful to them. This study was an essential first step in co-designing digitally animated assessment items for a new self-reported screening instrument for children: “name Blinded for Review”. Twenty children aged five to 11 years participated in semi-structured small group interviews to discuss 15 pairs of contrasting emotional and behavioral constructs (EBC’s). Interview questions were designed to determine how children comprehend, express, and recognize these EBC’s and were correlated to the following five categories to aid the development of the animated items: lexical understanding, visual expression, narrative settings, behavioral actions, and audio cues. Data were analyzed by cataloguing common responses for each EBC across the five categories and examining whether age-specific response typologies were apparent. Except for lexical labeling abilities, results indicated a distinct lack of age-related differences in children’s comprehension of physical and expressive displays of EBC’s between age group levels. This highlights the importance of audio-visual depictions of EBC’s over written text. Typology tables for each of the construct pairs were produced describing corresponding visual demonstrations, narrative contexts, behavioral actions, and audio cues shared by all children. These typologies provide insight into the child’s perspective of socio-emotional and behavioral archetypes and were utilized to inform the development of animated items for a novel screening tool. This study utilized co-design methodologies and produced datasets that may inform the development of mental health tools, interventions, or activities for children concerning emotional and behavioral concepts.

Objective: As cancer survival rates continue to increase, so will the demand for care from family and friends, particularly in more isolated settings. This study aims to examine the needs of cancer caregivers in regional and remote Australia. Methods: A total of 239 informal (i.e., non-professional) cancer caregivers (e.g., family/friends) from regional and remote Queensland, Australia, completed the Comprehensive Needs Assessment Tool for Cancer Caregivers (CNAT-C). The frequencies of individuals reporting specific needs were calculated. Logistic regression analyses assessed the association between unmet needs and demographic characteristics and cancer type. Results: The most frequently endorsed needs were lodging near hospital (77%), information about the disease (74%), and tests and treatment (74%). The most frequent unmet needs were treatment near home (37%), help with economic burden (32%), and concerns about the person being cared for (32%). Younger and female caregivers were significantly more likely to report unmet needs overall (OR = 2.12, OR = 0.58), and unmet healthcare staff needs (OR = 0.35, OR = 1.99, respectively). Unmet family and social support needs were also significantly more likely among younger caregivers (OR = 0.35). Caregivers of breast cancer patients (OR = 0.43) and older caregivers (OR = 0.53) were significantly less likely to report unmet health and psychology needs. Proportions of participants reporting needs were largely similar across demographic groups and cancer type with some exceptions. Conclusions: Caregiver health, practical issues associated with travel, and emotional strain are all areas where regional and remote caregivers require more support. Caregivers’ age and gender, time since diagnosis and patient cancer type should be considered when determining the most appropriate supportive care.

We present the results of a medium resolution optical spectroscopic survey of 92 cool ($3,000 \lesssim T_{\rm eff} \lesssim 4,500\,$K) southern TESS candidate planet hosts, and describe our spectral fitting methodology used to recover stellar parameters. We quantify model deficiencies at predicting optical fluxes, and while our technique works well for $T_{\rm eff}$, further improvements are needed for [Fe/H]. To this end, we developed an updated photometric [Fe/H] calibration for isolated main sequence stars built upon a calibration sample of 69 cool dwarfs in binary systems, precise to $\pm0.19\,$dex, from super-solar to metal poor, over $1.51 < {\rm Gaia}~(B_P-R_P) < 3.3$. Our fitted $T_{\rm eff}$ and $R_\star$ have median precisions of 0.8% and 1.7%, respectively and are consistent with our sample of standard stars. We use these to model the transit light curves and determine exoplanet radii for 100 candidate planets to 3.5% precision and see evidence that the planet-radius gap is also present for cool dwarfs. Our results are consistent with the sample of confirmed TESS planets, with this survey representing one of the largest uniform analyses of cool TESS candidate planet hosts to date., Accepted version. 33 Pages, 12 Figures, 9 Tables

Hi-5 is the L'-band (3.5-4.0 $\mu$m) high-contrast imager of Asgard, an instrument suite in preparation for the visitor focus of the VLTI. The system is optimized for high-contrast and high-sensitivity imaging within the diffraction limit of a single UT/AT telescope. It is designed as a double-Bracewell nulling instrument producing spectrally-dispersed (R=20, 400, or 2000) complementary nulling outputs and simultaneous photometric outputs for self-calibration purposes. In this paper, we present an update of the project with a particular focus on the overall architecture, opto-mechanical design of the warm and cold optics, injection system, and development of the photonic beam combiner. The key science projects are to survey (i) nearby young planetary systems near the snow line, where most giant planets are expected to be formed, and (ii) nearby main sequence stars near the habitable zone where exozodiacal dust that may hinder the detection of Earth-like planets. We present an update of the expected instrumental performance based on full end-to-end simulations using the new GRAVITY+ specifications of the VLTI and the latest planet formation models., Comment: 16 pages, 9 figures, SPIE 2022 "Astronomical Telescopes and Instrumentation" manuscript 12183-16

OBJECTIVES: To measure rates of detection via screening, perceived self-imposed delays in seeking medical attention, and support seeking in a sample of regional and remote people with a cancer diagnosis and to test whether an association exists between these behaviours and minimising problems and resignation, a need for self-control and reliance and fatalism. Correlations and binary logistic regressions were conducted to test the associations between demographic characteristics, attitudes and behaviours. RESULTS: Females were more likely to have had their cancer detected via screening (OR = 10.02, CI = 3.49 - 28.78). Younger participants (r = -.103, p =.009) were slightly more likely to seek at least one form of support and online support was sought more often by younger patients (r = -.269, p < .001), females (r = .152 , p

Empathy is essential for social functioning and is relevant to a host of clinical conditions. This COSMIN review evaluated the empirical support for empathy self-report measures used with autistic and nonautistic adults. Given autism is characterized by social differences, it is the subject of a substantial proportion of empathy research. Therefore, this review uses autism as a lens through which to scrutinize the psychometric quality of empathy measures. Of the 19 measures identified, five demonstrated “High-Quality” evidence for “Insufficient” properties and cannot be recommended. The remaining 14 had noteworthy gaps in evidence and require further evaluation before use with either group. Without tests of measurement invariance or differential item functioning, the extent to which observed group differences represent actual trait differences remains unknown. Using autism as a test case highlights an alarming tendency for empathy measures to be used to characterize, and potentially malign vulnerable populations before sufficient validation.

The suicide rate of farmers is approximately double that of the general Australian population, yet farmers employ fewer help-seeking behaviours (Arnautovska et al. in Soc Psychiatry Psychiatr Epidemiol 49:593–599, 2014; Brew et al. in BMC Public Health 16:1–11, 2016). Therefore, it is crucial to understand if, and how health services and system might influence farmer help-seeking. To shed light on this, the current study employed qualitative semi-structured interviews with 10 farmers, 10 farmers’ partners and 8 medical practitioners. Thematic analysis, guided by Braun and Clarke’s (Qual Res Psychol 3:77–101, 2006) techniques, was used to analyse the data. Three themes were devised concerning the interaction between farmers and health services, including ‘health service interactions’, ‘services are provided within a complex system’ and ‘emerging technologies: the users, practitioners, and systems’. The findings underscore the importance of interactions between a farmer and a service provider, with farmers wanting their provider to have an understanding of farming life. Help-seeking was also shaped by access, availability, and practitioner constancy. Lastly, a complex relationship between digital mental health services and farmer help-seeking was reported, with factors related to the farmers, the practitioners and the infrastructure/systems discussed. The outcomes have implications for health service and policy reform, developing and providing interventions for farmers to promote health services interaction as a way of mental health help-seeking.

Direct imaging in the infrared at the diffraction limit of large telescopes is a unique probe of the properties of young planetary systems. We survey 55 single class I and class II stars in Taurus in the L' filter using natural and laser guide star adaptive optics and the near-infrared camera (NIRC2) of the Keck II telescope, in order to search for planetary mass companions. We use both reference star differential imaging and kernel phase techniques, achieving typical 5-sigma contrasts of ~6 magnitudes at separations of 0.2" and ~8 magnitudes beyond 0.5". Although we do not detect any new faint companions, we constrain the frequency of wide separation massive planets, such as HR 8799 analogues. We find that, assuming hot-start models and a planet distribution with power-law mass and semi-major axis indices of -0.5 and -1, respectively, less than 20% of our target stars host planets with masses >2 MJ at separations >10 AU., 16 pages, 14 figures, accepted for publication in MNRAS

In the current era of Gaia and large, high signal to noise stellar spectroscopic surveys, there is an unmet need for a reliable library of fundamentally calibrated stellar effective temperatures based on accurate stellar diameters. Here we present a set of precision diameters and temperatures for a sample of 6 dwarf, 5 sub-giant, and 5 giant stars observed with the PIONIER beam combiner at the VLTI. Science targets were observed in at least two sequences with five unique calibration stars each for accurate visibility calibration and to reduce the impact of bad calibrators. We use the standard PIONIER data reduction pipeline, but bootstrap over interferograms, in addition to employing a Monte-Carlo approach to account for correlated errors by sampling stellar parameters, limb darkening coefficients, and fluxes, as well as predicted calibrator angular diameters. The resulting diameters were then combined with bolometric fluxes derived from broadband Hipparcos-Tycho photometry and MARCS model bolometric corrections, plus parallaxes from Gaia to produce effective temperatures, physical radii, and luminosities for each star observed. Our stars have mean angular diameter and temperatures uncertainties of 0.8% and 0.9% respectively, with our sample including diameters for 10 stars with no pre-existing interferometric measurements. The remaining stars are consistent with previous measurements, with the exception of a single star which we observe here with PIONIER at both higher resolution and greater sensitivity than was achieved in earlier work., Comment: Published in MNRAS, 22 pages, 7 figures

We present science cases and instrument design considerations for the BIFROST instrument that will open the short-wavelength (Y/J/H-band), high spectral dispersion (up to R=25,000) window for the VLT Interferometer. BIFROST will be part of the Asgard Suite of instruments and unlock powerful venues for studying accretion & mass-loss processes at the early/late stages of stellar evolution, for detecting accreting protoplanets around young stars, and for probing the spin-orbit alignment in directly-imaged planetary systems and multiple star systems. Our survey on GAIA binaries aims to provide masses and precision ages for a thousand stars, providing a legacy data set for improving stellar evolutionary models as well as for Galactic Archaeology. BIFROST will enable off-axis spectroscopy of exoplanets in the 0.025-1" separation range, enabling high-SNR, high spectral resolution follow-up of exoplanets detected with ELT and JWST. We give an update on the status of the project, outline our key technology choices, and discuss synergies with other instruments in the proposed Asgard Suite of instruments., 19 pages, 7 figures, SPIE 2022 "Astronomical Telescopes and Instrumentation" manuscript 12183-66

The Hi-5 instrument, a proposed high-contrast L' band (3.5-4.0 μm) nulling interferometer for the visitor focus of the Very Large Telescope Interferometer (VLTI), will characterize young extra-solar planetary systems and exozodiacal dust around nearby main-sequence stars. Thanks to VLTI's angular resolution (λ=B = 5 mas for the longest UT baseline), it will fill the gap between young giant exoplanets discovered by ongoing single-aperture direct imaging surveys and exoplanet populations discovered by radial velocity surveys. In this paper, we investigate the exoplanet detection yield of Hi-5. First, we present the latest catalog of stars identified as members of young stellar associations within 150 pc of the Sun thanks to the BANYAN algorithm and other searches for young moving group members. Realistic exoplanet populations are then generated around these stars and processed with the SCIFYsim tool, the end-to-end simulator for the Hi-5 instrument. Then, two formation models are used to estimate the giant planet's luminosity. The first is the New Generation Planetary Population Synthesis (NGPPS), also known as the Bern model, and the second is a statistical model based on gravitational instability (hot-start model - AMES-Dusty model). We show that Hi-5 is insensitive to cold-start planets but can detect giant hot-start planets. With ATs, more than 40 planets could be detected assuming 20 nights of observations. With its unique capabilities, Hi-5 is also able to constrain in mass the observed systems. Hi-5 is sensitive to planets with a mass > 2 Mjup around the snow line.

Hi-5 is an ERC-funded project hosted at KU Leuven and a proposed visitor instrument for the VLTI. Its primary goal is to image the snow line region around young planetary systems using nulling interferometry in the L’ band, between 3.5 and 4.1 μm, where the contrast between exoplanets and their host stars is very advantageous. The breakthrough is the use of a photonic chip based beam combiner, which only recently allowed the required theoretical raw contrast of 10−3 in this spectral range. The VLTI long baseline interferometry enables to reach high angular resolution (4.2 mas at 3.8 μm wavelength with the Auxiliary Telescopes (ATs)), while high contrast detection is achieved using nulling interferometry. This polarisation requires a high degree of optical symmetry between the four pupils of the VLTI, only possible with precise phase, dispersion and intensity control systems. The instrument is currently in its design phase. In this paper, the warm optics design and the injection system up to the photonic chip are presented. The different properties of the design are presented including the optics used, the characteristics of the four beams and the current drawbacks. Particular attention is devoted to the optical alignment and the tolerance analysis in order to estimate the precision required for the alignment procedure and therefore to choose adapted optical mountings.

Beam combiners are important components of an optical/infrared astrophysical interferometer, with many variants as to how to optimally combine two or more beams of light to fringe-track and obtain the complex fringe visibility. One such method is the use of an integrated optics chip that can instantaneously provide the measurement of the visibility without temporal or spatial modulation of the optical path. Current asymmetric planar designs are complex, resulting in a throughput penalty, and so here we present developments into a three dimensional triangular tricoupler that can provide the required interferometric information with a simple design and only three outputs. Such a beam combiner is planned to be integrated into the upcoming $\textit{Pyxis}$ interferometer, where it can serve as a high-throughput beam combiner with a low size footprint. Results into the characterisation of such a coupler are presented, highlighting a throughput of 85$\pm$7% and a flux splitting ratio between 33:33:33 and 52:31:17 over a 20% bandpass. We also show the response of the chip to changes in optical path, obtaining an instantaneous complex visibility and group delay estimate at each input delay., 20 pages, 10 figures, resubmitted to JATIS after addressing reviewer comments

Large spectroscopic surveys of the Milky Way need to be calibrated against a sample of benchmark stars to ensure the reliable determination of atmospheric parameters. We present new fundamental stellar parameters of seven giant and subgiant stars that will serve as benchmarks. The aim is to reach a precision of 1% in the effective temperature. This precision is essential for accurate determinations of the full set of fundamental parameters and abundances of stars observed by the surveys. We observed HD121370 (etaBoo), HD161797 (muHer), HD175955, HD182736, HD185351, HD188512 (betaAql), and HD189349 using the high angular resolution optical interferometric instrument PAVO/CHARA. The limb-darkening corrections were determined from 3D model atmospheres based on the STAGGER grid. The Teff were determined directly from the Stefan-Boltzmann relation, with an iterative procedure to interpolate over tables of bolometric corrections. We estimated surface gravities from comparisons to Dartmouth stellar evolution model tracks. The spectroscopic observations were collected from the ELODIE and FIES spectrographs. We estimated metallicities ([Fe/H]) from a 1D non-local thermodynamic equilibrium (NLTE) abundance analysis of unblended lines of neutral and singly ionised iron. For six of the seven stars we measure Teff to better than 1%. For one star, HD189349, the uncertainty in Teff is 2% due to an uncertain bolometric flux. We do not recommend this star as a benchmark until this measurement can be improved. Median uncertainties for all stars in logg and [Fe/H]} are 0.034dex and 0.07dex, respectively. All the fundamental stellar parameters were based on consistently combining interferometric observations, 3D limb-darkening modelling and spectroscopic analysis. This paper follows our previous papers including dwarfs and metal-poor stars., 14 pages, 8 figures, 9 tables, tables A.1.-A.7. will be submitted electronically, accepted for publication in A&A. arXiv admin note: text overlap with arXiv:2006.05411

Objective This study aimed to compare stress, burnout, stressors, and protective factors among regional‐ and metropolitan‐based Australian medical doctors. Method A mixed methods design was utilized with 252 Australian medical doctors completing an online questionnaire package. A subsample also completed qualitative interviews. Results Stress was significantly higher among doctors compared with population norms. Over half of doctors reported burnout on one or more dimensions. The strongest unique predictors were being female, working late, and work–family conflict. Qualitatively, 12 stressors (e.g., training and competition, workload, and time management) and 9 protective subthemes (e.g., being well resourced, clinical interest) emerged across system‐level, clinical environment‐level, and individual factor and personal response themes. Conclusions Stress and burnout among doctors are alarmingly high and both system/organization‐level (e.g., communication systems, workload, flexible work arrangements) and individual‐level (e.g., fostering resilience/coping strategies) predictors are implicated by our results. These may be useful targets for future interventions.

The aim of this study was to understand the ‘farming life’ factors that affect the mental health help-seeking of farmers. Semi-structured interviews were completed with 10 farmers, 10 farmers’ partners, and eight General Practitioners (GPs), covering mental health help-seeking. Interview data were then analysed using thematic analysis resulting in three themes: Lifestyle and culture, farming priorities, and the challenges of farming. The findings showed that the lifestyle and culture of farming values traits such as stoicism and self-reliance, which is ingrained in farmers’ identities and appears antithetical to mental health help-seeking. The farming priorities theme highlighted that farmers are time-poor and believe mental health help-seeking to be time-consuming and an interference to their work, which is their primary priority. Lastly, this research revealed that farming challenges, such as financial volatility, increase the need for help, but can also reduce the ability to seek help. Implications of the findings highlight a need to carefully engage with farming cultures more broadly when seeking to support the mental health of the farming community.

Giant planets are expected to form at orbital radii that are relatively large compared to transit and radial velocity detections (>1 AU). As a result, giant planet formation is best observed through direct imaging. By simulating the formation of giant (0.3-5$M_{J}$) planets by core accretion, we predict planet magnitude in the near infrared (2-4 $��$m) and demonstrate that, once a planet reaches the runaway accretion phase, it is self-luminous and is bright enough to be detected in near infrared wavelengths. Using planet distribution models consistent with existing radial velocity and imaging constraints, we simulate a large sample of systems with the same stellar and disc properties to determine how many planets can be detected. We find that current large (8-10m) telescopes have, at most a 0.2% chance of detecting a core accretion giant planet in the L' band and 2% in the K band for a typical solar type star. Future instruments such as METIS and VIKiNG have higher sensitivity and are expected to detect exoplanets at a maximum rate of 2% and 8% respectively., 12 pages, 13 figures, final revision submitted to MNRAS

The aim of the present study was to investigate the mediating role of patience in the relationship between mindfulness and pain among patients with cardiovascular disease. A cross-sectional design was employed. One hundred and ten patients with cardiovascular diseases were conveniently sampled from the clinic of Imam Reza in the city of Shiraz in Iran. Participants completed self-report measures of mindfulness, patience, and pain. Structural equation modeling was performed with Amos 16.0. Results indicated that mindfulness and patience had a significant inverse relationship with pain. There was also a significant positive relationship between patience and mindfulness. Estimated indirect effects showed that patience partly mediated the relationship between mindfulness and pain. These results show that among cardiovascular patients, increases in mindfulness are associated with reductions in pain as a function of increased patience. Therefore, patience is plausibly a key mechanism for understanding the impact of mindfulness on pain reduction.

Alcohol-linked sponsorship of sport represents a significant and growing investment as a popular strategy for brand communication. The current study confirms a relationship between exposure and hazardous consumption and provides insight into this relationship by examining the mediators responsible. Specifically, brand-image transfer (i.e., the mirroring of positive image attributes from the sponsored event to the sponsoring brand) and implied endorsement (i.e., the consumer assumes that the team or athlete favors the sponsor by virtue of the sponsorship relationship) were tested as mechanisms that explain these effects. The study involved a cross-sectional online survey across 8 sports that examined this relationship between exposure to alcohol-brand sport sponsorship and associated alcohol consumption in young Australian sport consumers (N = 2,033). Findings support a link between alcohol-sponsorship exposure in sport and alcohol consumption, mediated by image transfer and implied endorsement. Implications for sponsors, sports, and regulators concerned with consumer protection and national health are discussed.

Astrophotonics is an emerging field that focuses on the development of photonic components for astronomical instrumentation. With ongoing advancements, astrophotonic solutions are already becoming an integral part of existing instruments. A recent example is the €60M ESO GRAVITY instrument at the Very Large Telescope Interferometer, Chile, that makes heavy use of photonic components. We envisage far-reaching applications in future astronomical instruments, especially those intended for the new generation of extremely large telescopes and in space. With continued improvements in extreme adaptive optics, the case becomes increasingly compelling. The joint issue of JOSA B and Applied Optics features more than 20 state-of-the-art papers in diverse areas of astrophotonics. This introduction provides a summary of the papers that cover several important topics, such as photonic lanterns, beam combiners and interferometry, spectrographs, OH suppression, and coronagraphy.

Purpose The Interactive Child Distress Screener (ICDS) is a novel, digital screening tool that is currently under development and aims to broadly assess self-reported emotional and behavioural distress in children aged five to 11 years. This study implemented a generative participatory codesign and iterative refinement process to qualitatively validate the content of 30 animated assessment items developed for the ICDS by assessing their acceptability and accuracy from the child's perspective. Methods The participants (N = 62) were five to 11-year-old children. Individual interviews were conducted with each child to determine acceptability and validity of animated items and facilitate the co-design refinement process of the animated assessment items. Results Twenty-two out of 30 (73%) items met ≥80% satisfaction and accuracy consensus in their original format, six items (20%) required one round of refinement before meeting consensus, and two items (7%) required two rounds of refinements. Combined acceptability of animated items was high, ranging from 4.1 to 5 out of 5 across all items. Conclusion Participants were able to accurately identify and understand socio-emotional and behavioural constructs when depicted as animated items. Acceptability was high, even in first iterations when accuracy of understanding required refinement. This study highlighted the importance and benefits of iterative participatory design methodology in ensuring assessment items developed for children are understood, accepted and likely to be effective in obtaining accurate self-report., Highlights • Children 5–11 years can identify and understand complex emotions and behaviours presented as animations. • Participatory co-design with children increases assessment item accuracy and acceptability. • Young children reported high acceptability of animated scenarios as assessment items.

We present a hierarchical optical phased array design with adaptive optics capabilities. The design allows for modular control over emitter counts, supporting the large emitter count required for the Breakthrough Starshot optical phased array.

Photometric monitoring of Beta Pictoris in 1981 showed anomalous fluctuations of up to 4% over several days, consistent with foreground material transiting the stellar disk. The subsequent discovery of the gas giant planet Beta Pictoris b and the predicted transit of its Hill sphere to within 0.1 au projected distance of the planet provided an opportunity to search for the transit of a circumplanetary disk in this $21\pm 4$ Myr-old planetary system. Continuous broadband photometric monitoring of Beta Pictoris requires ground-based observatories at multiple longitudes to provide redundancy and to provide triggers for rapid spectroscopic followup. These observatories include the dedicated Beta Pictoris monitoring observatory bRing at Sutherland and Siding Springs, the ASTEP400 telescope at Concordia, and observations from the space observatories BRITE and Hubble Space Telescope. We search the combined light curves for evidence of short period transient events caused by rings and for longer term photometric variability due to diffuse circumplanetary material. We find no photometric event that matches with the event seen in November 1981, and there is no systematic photometric dimming of the star as a function of the Hill sphere radius. We conclude that the 1981 event was not caused by the transit of a circumplanetary disk around Beta Pictoris b. The upper limit on the long term variability of Beta Pictoris places an upper limit of $1.8\times 10^{22}$ g of dust within the Hill sphere. Circumplanetary material is either condensed into a non-transiting disk, is condensed into a disk with moons that has a small obliquity, or is below our detection threshold. This is the first time that a dedicated international campaign has mapped the Hill sphere transit of a gas giant extrasolar planet at 10 au., Comment: 12 pages, 9 figures, 1 table, accepted for publication in A&A. Reduced data and reduction scripts on GitHub at https://github.com/mkenworthy/beta_pic_b_hill_sphere_transit

A space interferometer could reach a sensitivity and angular resolution which is unattainable on Earth due to the distortion and absorption of the atmosphere. It would enable many unique science cases, including the direct imaging and characterisation of temperate terrestrial exoplanets. This ambitious vision relies on the formation flying of individual spacecrafts, and the demonstration of precision metrology measuring positions in to better than 1mm in at least 2 dimensions, and velocities in the range of nm/s. These significant technical challenges are one of the main reasons progress in space interferometry has been seriously hampered in the two last decades. To overcome this obstacle, we propose a novel metrology concept operating in two steps. The coarse positioning of the array elements is achieved through commercially demonstrated components, such as GPS, wide angle cameras and time-of-flight sensors. For the critical fine metrology, multiple longitudinal mode Fabry-Perot lasers in a central spacecraft are split and retro-reflected off each telescope bearing spacecraft. The reflected beams are then coherently combined in the central spacecraft and the resulting fringes are spectrally dispersed. In this manner, the phase difference is measured at the different Fabry-Perot wavelengths, allowing the unambiguous differential position measurements over a couple of mm capture range. We present the concept together with a prototype system in the laboratory.

Optical and infrared interferometry from the ground has had major successes but will soon meet fundamental limitations. Adaptive optics and creative fringe tracking solutions has the potential to greatly increase the reach of interferometry from the ground, but the factor of 107 in thermal infrared background means that space interferometry with small telescopes is a more cost-effective solution at long wavelengths. Additionally, important spectral windows for high angular resolution astrophysics are only open from space. I will briefly outline the limitations of interferometry from the ground, and make the case for space. In addition to reviewing the historical cases of low fringe visibility (complex) imaging, precision astrometry, high contrast mid-infrared interferometry and far infrared interferometry, I will make the case for wavelength-differential and polarimetric interferometry at visible and ultraviolet wavelengths. A major long baseline interferometry mission will require higher technological readiness levels of key technologies, including interspacecraft metrology, fringe tracking in a space environment and high contrast nulling. For some mission concepts, relatively little new subsystem development is required and tolerances are surprisingly loose. I will argue that in order to fast-track the inevitability of space interferometry, some key subsystem development, whole mission simulation and a pathfinder mission are all required in the near future.

In the new era of Extremely Large Telescopes (ELTs) currently under construction, challenging requirements drive spectrograph designs towards techniques that efficiently use a facility's light collection power. Operating in the single-mode (SM) regime, close to the diffraction limit, reduces the footprint of the instrument compared to a conventional high-resolving power spectrograph. The custom built injection fiber system with 3D-printed microlenses on top of it for the replicable high-resolution exoplanet and asteroseismology spectrograph (RHEA) at Subaru in combination with extreme adaptive optics of SCExAO, proved its high efficiency in a lab environment, manifesting up to ∼77% of the theoretical predicted performance.

The instrument group of the Herzberg Astronomy and Astrophysics has been subcontracted by Australian Astronomical Optics (AAO) at Macquarie University to design and build the bench spectrograph for the Gemini High-Resolution Optical SpecTrograph (GHOST) instrument. The GHOST instrument is being developed for the Gemini telescope and is a collaboration between AAO, the Herzberg Astronomy and Astrophysics (HAA) in Canada and the Australian National University (ANU). The instrument is a fiber fed spectrograph with R, Ground-based and Airborne Instrumentation for Astronomy VIII, December 14-18, 2020, Online Only, United States, Series: Proceedings of SPIE

The CHARA Array is the longest baseline optical interferometer in the world. Operated with natural seeing, it has delivered landmark sub-milliarcsecond results in the areas of stellar imaging, binaries, and stellar diameters. However, to achieve ambitious observations of faint targets such as young stellar objects and active galactic nuclei, higher sensitivity is required. For that purpose, adaptive optics are developed to correct atmospheric turbulence and non-common path aberrations between each telescope and the beam combiner lab. This paper describes the AO software and its integration into the CHARA system. We also report initial on-sky tests that demonstrate an increase of scientific throughput by sensitivity gain and by extending useful observing time in worse seeing conditions. Our 6 telescopes and 12 AO systems with tens of critical alignments and control loops pose challenges in operation. We describe our methods enabling a single scientist to operate the entire system., Comment: SPIE, Optical and Infrared Interferometry and Imaging VII, Proceedings Volume 11446, 1144622, Dec 14, 2020 "See, https://doi.org/10.1117/12.2561560"

Space interferometry is the inevitable endpoint of high angular resolution astrophysics, and a key technology that can be leveraged to analyse exoplanet formation and atmospheres with exceptional detail. Here, we present a feasibility study into a small scale formation flying interferometric array, flying in Low Earth Orbit, that will aim to prove the technical concepts involved with space interferometry while still making unique astrophysical measurements. We will detail the design of the mission, as well as present orbital simulations that show that the array should be stable enough to perform interferometry with