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Aims This study explores perspectives of on-pack alcohol warning labels, and how they might influence alcohol purchase and/or consumption behavior to inform culturally appropriate label design for effective behavior change. Methods New Zealand participants ≥18 years, who reported having purchased and consumed alcoholic beverages in the last month were recruited via a market research panel and grouped into 10 focus groups (n  = 53) by ethnicity (general population, Māori, and Pacific peoples), age group, and level of alcohol consumption. Participants were shown six potential alcohol health warning labels, with design informed by relevant literature, label framework, and stakeholder feedback. Interviews were transcribed and analyzed via qualitative (directed) content analysis. Results Effective alcohol labels should be prominent, featuring large red and/or black text with a red border, combining text with visuals, and words like "WARNING" in capitals. Labels should contrast with bottle color, be easily understood, and avoid excessive text and confusing imagery. Participants preferred specific health outcomes, such as heart disease and cancer, increasing message urgency and relevance. Anticipated behavior change included reduced drinking and increased awareness of harms, but some may attempt to mitigate warnings by covering or removing labels. Contextual factors, including consistent design and targeted labels for different beverages and populations, are crucial. There was a strong emphasis on collective health impacts, particularly among Māori and Pacific participants. Conclusions Our findings indicate that implementing alcohol warning labels, combined with comprehensive strategies like retail and social marketing campaigns, could effectively inform and influence the behavior of New Zealand's varied drinkers. [ABSTRACT FROM AUTHOR]

Severe acute respiratory syndrome coronavirus 2 (SARS-CoV-2), the virus responsible for coronavirus disease of 2019 (COVID-19), has caused havoc around the world. While several COVID-19 vaccines and drugs have been authorized for use, these antiviral drugs remain beyond the reach of most low- and middle-income countries. Rapid viral evolution is reducing the efficacy of vaccines and monoclonal antibodies and contributing to the deaths of some fully vaccinated persons. Others with normal immunity may have chosen not to be vaccinated and remain at risk if they contract the infection. Vaccines may not protect some immunodeficient patients from SARS-CoV-2, who are also at increased risk of chronic COVID-19 infection, a dangerous stalemate between the virus and a suboptimal immune response. Intra-host viral evolution could rapidly lead to the selection and dominance of vaccine and monoclonal antibody-resistant clades of SARS-CoV-2. There is thus an urgent need to develop new treatments for COVID-19. The NZACE2-Pātari project, comprising modified soluble angiotensin-converting enzyme 2 (ACE2) molecules, seeks to intercept and block SARS-CoV-2 infection of the respiratory mucosa. In vitro data presented here show that soluble wild-type ACE2 molecules retain the ability to effectively block the Spike (S) glycoprotein of SARS-CoV-2 variants including the ancestral Wuhan, delta (B.1.617.2) and omicron (B.1.1.529) strains. This therapeutic strategy may prove effective if implemented early during the nasal phase of the infection and may act synergistically with other antiviral drugs such as Paxlovid to further mitigate disease severity. This article shows that soluble wild-type ACE2 receptors can block the binding of the SARS-CoV-2 to ACE2. This is an antiviral strategy that is resistant to viral evolution. In the future, it may be used against new variants of SARS-CoV-2. [ABSTRACT FROM AUTHOR]

We examined the importance of understanding and incorporating cultural context within Aotearoa/New Zealand when engaging in clinical research and practice. This paper reports on the qualitative findings of a mixed methods study aimed at determining what effect a cardiac risk reduction exercise and lifestyle management programme, embedded within a kaupapa Māori methodological approach, had on Māori participants. This methodology saw participants able to redevelop a western model cardiac risk reduction programme by introducing a Māori worldview. Our study revealed how the kaupapa Māori approach empowered participants to examine and evaluate not only their own health and lifestyle choices, but those of family and the wider community. Combining biomedical and kaupapa Māori components into the programme was found to benefit participants' mental, physical, spiritual and family well-being. [ABSTRACT FROM AUTHOR]

Objective To determine the physical and mental health of very old people (aged 80+) with anaemia. Methods Individual level meta-analysis from five cohorts of octogenarians (n = 2,392): LiLACS NZ Māori, LiLACS NZ non-Māori, Leiden 85-plus Study, Newcastle 85+ Study, and TOOTH. Mixed models of change in functional ability, cognitive function, depressive symptoms, and self-rated health over time were separately fitted for each cohort. We combined individual cohort estimates of differences according to the presence of anaemia at baseline, adjusting for age at entry, sex, and time elapsed. Combined estimates are presented as differences in standard deviation units (i.e. standardised mean differences–SMDs). Results The combined prevalence of anaemia was 30.2%. Throughout follow-up, participants with anaemia, on average, had: worse functional ability (SMD −0.42 of a standard deviation across cohorts; CI -0.59,-0.25); worse cognitive scores (SMD -0.27; CI -0.39,-0.15); worse depression scores (SMD -0.20; CI -0.31,-0.08); and lower ratings of their own health (SMD -0.36; CI -0.47,-0.25). Differential rates of change observed were: larger declines in functional ability for those with anaemia (SMD −0.12 over five years; CI -0.21,-0.03) and smaller mean difference in depression scores over time between those with and without anaemia (SMD 0.18 over five years; CI 0.05,0.30). Conclusion Anaemia in the very old is a common condition associated with worse functional ability, cognitive function, depressive symptoms, and self-rated health, and a more rapid decline in functional ability over time. The question remains as to whether anaemia itself contributes to worse outcomes or is simply a marker of chronic diseases and nutrient deficiencies. [ABSTRACT FROM AUTHOR]

Background: multi-morbidity is associated with poor outcomes and increased healthcare utilisation. We aim to identify multi-morbidity patterns and associations with potentially inappropriate prescribing (PIP), subsequent hospitalisation and mortality in octogenarians. Methods: life and Living in Advanced Age; a Cohort Study in New Zealand (LiLACS NZ) examined health outcomes of 421 Māori (indigenous to New Zealand), aged 80-90 and 516 non-Māori, aged 85 years in 2010. Presence of 14 chronic conditions was ascertained from self-report, general practice and hospitalisation records and physical assessments. Agglomerative hierarchical cluster analysis identified clusters of participants with co-existing conditions. Multivariate regression models examined the associations between clusters and PIP, 48-month hospitalisations and mortality. Results: six clusters were identified for Māori and non-Māori, respectively. The associations between clusters and outcomes differed between Māori and non-Māori. In Māori, those in the complex multi-morbidity cluster had the highest prevalence of inappropriately prescribed medications and in cluster 'diabetes' (20% of sample) had higher risk of hospitalisation and mortality at 48-month follow-up. In non-Māori, those in the 'depression-arthritis' (17% of the sample) cluster had both highest prevalence of inappropriate medications and risk of hospitalisation and mortality. Conclusions: in octogenarians, hospitalisation and mortality are better predicted by profiles of clusters of conditions rather than the presence or absence of a specific condition. Further research is required to determine if the cluster approach can be used to target patients to optimise resource allocation and improve outcomes. [ABSTRACT FROM AUTHOR]

High spectral resolution and signal-to-noise optical spectra, obtained at the Very Large Telescope (VLT), are presented for three post–asymptotic giant branch (AGB) candidates selected from the Edinburgh–Cape (EC) Faint Blue Object Survey. The stellar atmospheric parameters and chemical compositions, derived using sophisticated non-local thermodynamic equilibrium calculations, reveal that EC 14102-1337 and EC 20068-7324 are both in an evolved post–horizontal branch (HB) evolutionary state. However, EC 11507-2253 is most likely a post-AGB star. [ABSTRACT FROM AUTHOR]

High spectral resolution and signal-to-noise ratio observations of five high Galactic latitude early-type stars taken from the Edinburgh–Cape (EC) Faint Blue Object Survey are presented. These were required to complete a magnitude range-limited survey of young B-type objects with . Of the five stars, four were rejected on the grounds that they are either subluminous (subdwarf or horizontal branch), were part of a binary system or possessed colours later than the cut-off employed. The remaining star in the data set, EC 19596-5356, is found to exhibit normal young B-type stellar properties. A kinematic analysis reveals that an origin in the Galactic disc appears likely for all the stars in the sample. Some statistics are drawn about the number density of young stars in the Galactic halo. [ABSTRACT FROM AUTHOR]

We compare existing high spectral resolution (R = λ/Δλ ∼ 40 000) Ca II K observations (λair = 3933.66 Å) towards 88 mainly B-type stars, and new observations taken using the Intermediate dispersion Spectrograph and Imaging System (ISIS) on the William Herschel Telescope at R ∼ 10 000 towards three stars taken from the Palomar­Green Survey, with 21-cm H I emission-line profiles, in order to search for optical absorption towards known intermediate- and high-velocity cloud complexes. Given certain assumptions, limits to the gas phase abundance of Ca II are estimated for the cloud components. We use the data to derive the following distances from the Galactic plane (z). (i) Tentative lower z-height limits of 2800 and 4100 pc towards complex C using lack of absorption in the spectra of HD341617 and PG0855+294, respectively. (ii) A weak lower z-height of 1400 pc towards complex WA-WB using lack of absorption in EC 09470–1433 and a weak lower limit of 2470 pc using lack of absorption in EC 09452–1403. (iii) An upper z-height of 2470 pc towards a southern intermediate-velocity cloud (IVC) with vLSR = −55 km s-1 using PG2351+198. (iv) Detection of a possible IVC in CaII absorption at vLSR = +52 km s-1 using EC 20104–2944. No associated H i in emission is detected. At this position, normal Galactic rotation predicts velocities of up to ∼ +25 km s-1. The detection puts an upper z-height of 1860 pc to the cloud. (v) Tentative H I and Ca II K detections towards an IVC at ∼ +70 km s-1 in the direction of high-velocity cloud (HVC) complex WE, sightline EC 06387–8045, indicating that the IVC may be at a z-height lower than 1770 pc. (vi) Detection of Ca II K absorption in the spectrum of PG 0855+294 in the direction of IV20, indicating that this IVC has a z-height smaller than 4100 pc. (vii) A weak lower z-height of 4300 pc towards a small HVC with vLSR = +115 km s-1 at l, b = 200°, + 52°, using lack of absorption in the Ca II K spectrum of PG 0955+291. [ABSTRACT FROM AUTHOR]

High-resolution echelle spectroscopic observations of 13 high-latitude early-type stars are presented. These stars comprise the final part of a complete magnitude range limited sample based on low-resolution spectroscopy of targets drawn from the Palomar–Green survey. The magnitude range under consideration is , corresponding to an approximate distance limit for main-sequence B-type objects of . Three stars are found to be apparently normal, young stars, based on their positions on the diagram, normal abundance patterns and relatively large projected rotational velocities. A further star, PG 1209+263, was found to belong to the chemically peculiar (CP) silicon star class of objects. The remainder are evolved subluminous stars lying on post-horizontal branch (post-HB) tracks, with the exception of PG 2120+062, which appears to be in a post-asymptotic giant branch evolutionary stage. For the young stars in the sample, we have derived distance and age estimates through comparison of the atmospheric parameters with recent theoretical evolutionary models. We discuss formation scenarios by comparing times-of-flight and evolutionary time-scales. It is found that all stars could have formed in the Galactic disc and been ejected from there soon after their birth, with the exception of PG 1209+263. The adopted proper motion is found to be a crucial factor in the kinematical analysis. We also present some number densities for young B-type halo stars, which indicate that they are extremely scarce objects. [ABSTRACT FROM AUTHOR]

We present high-resolution Ca ii K interstellar observations towards 88 mainly B-type stars, of which 74 are taken from the Edinburgh–Cape or Palomar–Green surveys, and 81 have . The majority of the data come from previously existing spectroscopy, although also included are 18 new observations of stars with echelle spectra taken with UVES on the Very Large Telescope UT2 (Kueyen). Some 49 of the sample stars have distance estimates above the Galactic plane , and are thus good probes of the halo interstellar medium. Of the 362 interstellar Ca K components that we detect, 75 (21 per cent) have absolute values of their LSR velocity values exceeding 40 km s−1. In terms of the deviation velocity for the sightlines with distance estimates, 46/273 (17 per cent) of components have velocity values exceeding those predicted by standard Galactic rotation by more than 40 km s−1. Combining this data set with previous observations, we find that the median value of the reduced equivalent width (REW) of stars with is ∼ , similar to that observed in extragalactic sightlines by Bowen. Using data of all z distances, the REW at infinity is found to be ∼ , with the scaleheight ( l) of the Ca ii K column density distribution being ≈ and reduced column density at infinity of log[ N(Ca ii K) cm−2]∼12.24. This implies that ∼30 per cent of Ca ii K absorption occurs at distances exceeding ∼1 kpc. For nine sightlines with distance exceeding 1 kpc and with a companion object within 5°, we find that all but two have values of Ca ii reduced equivalent width the same to within ∼20 per cent, when the REW of the nearest object is extrapolated to the distance of the further of the pair, and assuming . For 29 of our sightlines with and a H i detection from the Leiden–Dwingeloo survey (beamsize of 0.5°), we find log( N(Ca ii K)/ N(H i)) ranging from −7.4 to −8.4. Values of the Ca ii K abundance relative to neutral hydrogen (log[ N(Ca ii K) cm−2] – log[ N(H i) cm−2]) are found to be more than ∼0.5 dex higher in stars with distances exceeding ≈100 pc, when compared with the (log[ N(Ca ii K) cm−2]– log[ N(Htot) cm−2]) values found in nearby sightlines such as those in . Finally, stellar Ca ii K equivalent widths of the sample are determined for 26 objects. [ABSTRACT FROM AUTHOR]

Absolute and differential abundance analyses have been performed from high-resolution, high signal-to-noise ratio optical (Keck I) spectra for three evolved Galactic halo stars, namely PG 1704 + 222, HD 341617 and LS IV -04 01. Their derived atmospheric parameters indicate that all three objects are undergoing a post-asymptotic giant branch (post-AGB) phase of evolution. A differential abundance analysis reveals HD 341617 as having a mild carbon deficiency of 0.74 dex, possibly due to the star having evolved off the AGB before the onset of the third dredge-up. Although such carbon underabundances are typical of hot post-AGB objects, the same trend is not observed in PG 1704 + 222, where the carbon abundance is found to be consistent with those derived for nitrogen and oxygen. Hence, a dredge-up scenario need not be invoked to explain the chemical composition of PG 1704 + 222. For LS IV -04 01 no iron deficiency is apparent relative to magnesium and silicon, and hence a gas-dust separation event in the AGB progenitor need not be invoked for this star. [ABSTRACT FROM AUTHOR]

Abstract 19 B-type stars, selected from the Palomar–Green Survey, have been observed at infrared wavelengths to search for possible infrared excesses, as part of an ongoing programme to investigate the nature of early-type stars at high Galactic latitudes. The resulting infrared fluxes, along with Strömgren photometry, are compared with theoretical flux profiles to determine whether any of the targets show evidence of circumstellar material, which may be indicative of post-main-sequence evolution. Eighteen of the targets have flux distributions in good agreement with theoretical predictions. However, one star, PG 2120+062, shows a small near-infrared excess, which may be due either to a cool companion of spectral type F5–F7, or to circumstellar material, indicating that it may be an evolved object such as a post-asymptotic giant branch star, in the transition region between the asymptotic giant branch and planetary nebula phase, with the infrared excess due to recent mass loss during giant branch evolution. [ABSTRACT FROM AUTHOR]

Abstract A preliminary search for stars that may have formed coevally with the apparently young halo B-type star PHL 346 has been performed with the 2dF multifibre spectrograph on the Anglo-Australian Telescope (AAT). Candidates were selected for spectroscopy from APM scans of B and R Schmidt plates centred on PHL 346. A total of 476 stars of spectral type A or F were found; radial velocity estimates and more accurate spectral type assignments narrowed the number of possible coeval candidates to 6 A-type and 14 F-type stars. A statistical analysis of these results using a comparison with a control field suggests that the number of A-type or F-type candidate stars around PHL 346 is not unexpected, and that they need not be associated with PHL 346. A number of ways to improve the project are suggested. [ABSTRACT FROM AUTHOR]

Abstract The absorption-line spectra of early B-type supergiants show significant broadening that implies that an additional broadening mechanism (characterized here as ‘macroturbulence’) is present in addition to rotational broadening. Using high-resolution spectra with signal-to-noise ratios of typically 500, we have attempted to quantify the relative contributions of rotation and macroturbulence, but even with data of this quality significant problems were encountered. However, for all our targets, a model where macroturbulence dominates and rotation is negligible is acceptable; the reverse scenario leads to poor agreement between theory and observation. Additionally, there is marginal evidence for the degree of broadening increasing with line strength, possibly a result of the stronger lines being formed higher in the atmosphere. Acceptable values of the projected rotational velocity are normally less than or equal to 50 km s-1 , which may also be a typical upper limit for the rotational velocity. Our best estimates for the projected rotational velocity are typically 10–20 km s -1 and hence compatible with this limit. These values are compared with those predicted by single star evolutionary models, which are initially rapidly rotating. It is concluded that either these models underestimate the rate of rotational breaking or some of the targets may be evolving through a blue loop or are binaries. [ABSTRACT FROM AUTHOR]

Local thermodynamic equilibrium (LTE) absolute and differential abundances are presented for a peculiar metal-rich B-type star, HD 135485. These suggest that HD 135485 has a general enrichment of ∼0.5 dex in all the metals observed (C, N, O, Ne, Mg, Al, Si, P, S, Cl, Ar, Sc, Ti, Cr, Mn, Fe and Sr), except for nickel. The helium enhancement and hence hydrogen deficiency can account for ≤ 0.2 dex of this enhancement of metals, with the additional enhancement probably being representative of the progenitor gas. However, some of the metals appear to have greater enhancements, which may have occurred during the star's evolution. The significantly larger nitrogen abundance coupled with a modest helium enhancement observed in HD 135485 indicates that carbon–nitrogen (CN) processed material has possibly contaminated the stellar surface. Neon and carbon enhancements may indicate that helium core flashes have also occurred in HD 135485. Some of the iron-group elements (viz. Mn and Ni) appear to have similar abundance patterns to that of silicon Ap stars, but it is uncertain how these abundance patterns formed if they were not present in the progenitor gas. From a kinematical investigation it is unclear whether this star formed in a metal-rich region as implied by its chemical composition. From its position in the Hertzsprung–Russell diagram, HD 135485 would appear to be an evolved star lying close to or on the horizontal branch. [ABSTRACT FROM AUTHOR]

We present a model-atmosphere analysis for the bright (V∼13) star ZNG-1, in the globular cluster M10. From high-resolution (R∼40 000) optical spectra we confirm ZNG-1 to be a post-asymptotic giant branch (post-AGB) star. The derived atmospheric parameters are T[sub eff]=26 500±1000 K and log g=3.6±0.2 dex. A differential abundance analysis reveals a chemical composition typical of hot post-AGB objects, with ZNG-1 being generally metal poor, although helium is approximately solar. The most interesting feature is the large carbon underabundance of more than 1.3 dex. This carbon deficiency, along with an observed nitrogen enhancement relative to other elements, may suggest that ZNG-1 evolved off the AGB before the third dredge-up occurred. Also, iron depletions observed in other similar stars suggest that gas–dust fractionation in the AGB progenitor could be responsible for the observed composition of these objects. However, we need not invoke either scenario since the chemical composition of ZNG-1 is in good agreement with abundances found for a Population II star of the same metallicity. [ABSTRACT FROM AUTHOR]

We present high-resolution spectroscopic observations of 21 B-type stars, selected from the Edinburgh–Cape Blue Object Survey. Model atmosphere analyses confirm that 14 of these stars are young, main-sequence B-type objects with Population I chemical compositions. The remaining seven are found to be evolved objects, including subdwarfs, horizontal branch and post-AGB objects. A kinematical analysis shows that all 14 young main-sequence stars could have formed in the disc and subsequently been ejected into the halo. These results are combined with the analysis of a previous subsample of stars taken from the Survey. Of the complete sample, 31 have been found to be young, main-sequence objects, with formation in the disc, and subsequent ejection into the halo, again being found to be a plausible scenario. [ABSTRACT FROM AUTHOR]

Background In New Zealand (NZ) approximately 10,000 people experience an acute coronary syndrome (ACS) annually. Little is known about the diets of people who present with first ACS. Methods The Multi-Ethnic NZ study of Acute Coronary Syndromes (MENZACS) is a multi-centre, longitudinal cohort study of patients with first-time ACS. At baseline, patients complete a validated short food frequency questionnaire (FFQ) asking about dietary intakes in the 12 months preceding their event. Participants are followed up for rehospitalisation and mortality. Results Here we present the dietary intakes of the 2,015 participants enrolled into MENZACS. We excluded 90 participants who did not start the FFQ and 42 participants who had extreme energy intakes. For men (n = 1489), the median energy intake was 8637 kJ, and the median percentage of energy from carbohydrate, protein, fat, and saturated fat were 40.3%, 17.9%, 34.7% and 17.8%, respectively. For women (n = 394), the median energy intake was 7499 kJ, and the median percentage of energy from carbohydrate, protein, fat and saturated fat were 40.3%, 18.4%, 35.6%, and 18.0%, respectively. Conclusions Both men and women reported high saturated fat intakes in the year preceding their first ACS. Future work will examine dietary predictors of rehospitalisation and mortality, as well as analyse baseline blood samples for Lipoprotein(a) and lipidomics. Key messages Patients in hospital with first time ACS are able to complete a short food frequency questionnaire, with little missing data. [ABSTRACT FROM AUTHOR]

ABSTRACTWe present new, high-resolution, high signal-to-noise ratio, optical and 21-cm HI observations of the faint blue halo star HD 100340. A differential abundance analysis with respect to the Galactic disc star HR 2387 shows no significant peculiarities. We find that HD 100340 lies at a distance of 3 kpc, and a kinematical analysis strongly supports a `runaway star' origin. We also present improved cloud models for three intermediate velocity clouds seen in Ca II K or H I towards HD 100340. [ABSTRACT FROM AUTHOR]

We present a parallax measurement for the very cool degenerate WD 0346+246, the serendipitous discovery of which was reported by Hambly et al. We find an absolute parallax of 36±5 mas, yielding a distance estimate of 28±4 pc. The resulting absolute visual magnitude of the object is M[sub V]=16.8±0.3, making it the second-lowest luminosity white dwarf currently known. We use the distance estimate and measured proper motion to show that the object has kinematics consistent with membership of the Galactic halo. WD 0346+246 is therefore by far the coolest and least luminous of only a handful of plausible halo white dwarf candidates. As such, the object has relevance to the ongoing debate concerning the results of microlensing experiments and the nature of any baryonic dark matter component to the Galactic halo residing in stellar remnants. [ABSTRACT FROM AUTHOR]