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In a self-similar paradigm of structure formation, the thermal pressure of the hot intra-cluster gas follows a universal distribution once the profile of each cluster is normalised based on the proper mass and redshift dependencies. The reconstruction of such a universal pressure profile requires an individual estimate of the mass of each cluster. In this context, we present a method to jointly fit, for the first time, the universal pressure profile and individual cluster \\(M_{500}\\) masses over a sample of galaxy clusters, properly accounting for correlations between the profile shape and amplitude, and masses scaling the individual profiles. We demonstrate the power of the method and show that a consistent exploitation of the universal pressure profile and cluster mass estimates when modelling the thermal pressure in clusters is necessary to avoid biases. In particular, the method, informed by a cluster mass scale, outputs individual cluster masses with same accuracy and better precision than input masses. Using data from the {\\guillemotleft}Cluster HEritage project with XMM-Newton: Mass Assembly and Thermodynamics at the Endpoint of structure formation{\\guillemotright}, we investigate a sample of \\(\\sim 25\\) galaxy clusters spanning mass and redshift ranges of \\(2 \\lesssim M_{500}/10^{14} \\; \\mathrm{M}_{\\odot} \\lesssim 14\\) and \\(0.07 < z < 0.6\\).

Within the self-similar framework of structure formation, the thermal pressure of the hot intra-cluster medium follows a universal distribution that is independent of the cluster mass scale. Once normalised to the proper mass and redshift dependencies, this pressure distribution becomes common to all clusters. Reconstructing such a universal pressure profile requires individual estimates of each cluster’s mass. In this work, we present a methodology to simultaneously fit the universal pressure profile alongside the masses of individual clusters in a sample, while properly accounting for correlations between the profile’s shape, its amplitude, and cluster masses. We apply this method to a sub-sample of clusters from the CHEX-MATE project and demonstrate the strong impact that the assumed pressure profile has on the measured signal. This effect propagates into the thermal Sunyaev-Zel’dovich (tSZ) power spectrum and, in turn, influences the determination of cosmological parameters.

BirdLife International´s Important Bird and Biodiversity Areas (IBA) Programme has identified, documented and mapped over 13,000 sites of international importance for birds. IBAs have been influential with governments, multilateral agreements, businesses and others in: (1) informing governments’ efforts to expand protected area networks (in particular to meet their commitments through the Convention on Biological Diversity); (2) supporting the identification of Ecologically or Biologically Significant Areas (EBSAs) in the marine realm, (3) identifying Wetlands of International Importance under the Ramsar Convention; (4) identifying sites of importance for species under the Convention on Migratory Species and its sister agreements; (5) identifying Special Protected Areas under the EU Birds Directive; (6) applying the environmental safeguards of international finance institutions such as the International Finance Corporation; (7) supporting the private sector to manage environmental risk in its operations; and (8) helping donor organisations like the Critical Ecosystems Partnership Fund (CEPF) to prioritise investment in site-based conservation. The identification of IBAs (and IBAs in Danger: the most threatened of these) has also triggered conservation and management actions at site level, most notably by civil society organisations and local conservation groups. IBA data have therefore been widely used by stakeholders at different levels to help conserve a network of sites essential to maintaining the populations and habitats of birds as well as other biodiversity. The experience of IBA identification and conservation is shaping the design and implementation of the recently launched Key Biodiversity Areas (KBA) Partnership and programme, as IBAs form a core part of the KBA network.

Vulval intraepithelial neoplasia is a skin disorder affecting the vulva that, if left untreated, can become cancerous. Currently, the standard treatment for patients with vulval intraepithelial neoplasia is surgery, but this approach does not guarantee cure and can be disfiguring, causing physical and psychological problems, particularly in women of reproductive age. We aimed to assess the activity, safety, and feasibility of two topical treatments—cidofovir and imiquimod—as an alternative to surgery in female patients with vulval intraepithelial neoplasia. We recruited female patients (age 16 years or older) from 32 centres to an open-label, randomised, phase 2 trial. Eligibility criteria were biopsy-proven vulval intraepithelial neoplasia grade 3 and at least one lesion that could be measured accurately. We randomly allocated patients to topical treatment with either 1% cidofovir (supplied as a gel in a 10 g tube, to last 6 weeks) or 5% imiquimod (one 250 mg sachet for every application), to be self-applied three times a week for a maximum of 24 weeks. Randomisation (1:1) was done by stratified minimisation via a central computerised system, with stratification by hospital, disease focality, and presentation stage. The primary endpoint was a histologically confirmed complete response at the post-treatment assessment visit 6 weeks after the end of treatment (a maximum of 30 weeks after treatment started). Analysis of the primary endpoint was by intention to treat. Secondary outcomes were toxic effects (to assess safety) and adherence to treatment (to assess feasibility). We present results after all patients had reached the primary endpoint assessment point at 6 weeks; 2-year follow-up of complete responders continues. This trial is registered with Current Controlled Trials, ISRCTN 34420460. Between Oct 21, 2009, and Jan 11, 2013, 180 participants were enrolled to the study; 89 patients were randomly allocated cidofovir and 91 were assigned imiquimod. At the post-treatment assessment visit, a complete response had been achieved by 41 (46%; 90% CI 37·0–55·3) patients allocated cidofovir and by 42 (46%; 37·2–55·3) patients assigned imiquimod. After 6 weeks of treatment, 156 (87%) patients (78 in each group) had adhered to the treatment regimen. Five patients in the cidofovir group and seven in the imiquimod group either withdrew or were lost to follow-up before the first 6-week safety assessment. Adverse events of grade 3 or higher were reported in 31 (37%) of 84 patients allocated cidofovir and 39 (46%) of 84 patients assigned imiquimod; the most frequent grade 3 and 4 events were pain in the vulva, pruritus, fatigue, and headache. Cidofovir and imiquimod were active, safe, and feasible for treatment of vulval intraepithelial neoplasia and warrant further investigation in a phase 3 setting. Both drugs are effective alternatives to surgery for female patients with vulval intraepithelial neoplasia after exclusion of occult invasive disease. Cancer Research UK.

© 2018 Springer Science+Business Media, LLC, part of Springer Nature The high-frequency telescope for LiteBIRD is designed with refractive and reflective optics. In order to improve sensitivity, this paper suggests the new optical configurations of the HFT which have approximately 7 times larger focal planes than that of the original design. The sensitivities of both the designs are compared, and the requirement of anti-reflection (AR) coating on the lens for the refractive option is derived. We also present the simulation result of a sub-wavelength AR structure on both surfaces of silicon, which shows a band-averaged reflection of 1.1–3.2% at 101–448 GHz.

The epoch of reionisation is a key phase in cosmic history, characterised by the ionisation of the intergalactic medium by the first luminous sources. In this work, we constrain the reionisation history of the Universe using data from the cosmic microwave background, more specifically the latest Planck Public Release 4 (PR4) dataset. We investigate a wide range of reionisation models, from simple parametric descriptions to more flexible non-parametric approaches, systematically evaluating their impact on the inferred constraints. Special attention is given to implicit priors introduced by each model and their influence on the derived reionisation optical depth, \\(\\tau\\). To achieve this, we employ both Bayesian and frequentist methods to derive robust constraints. We obtain consistent estimates of \\(\\tau\\) across models, highlighting the robustness of the constraints on the integrated optical depth derived from the Planck PR4 data. Averaging across models, the posterior means and best-fit values, respectively, yield \\(\\tau = 0.0576 \\pm 0.0060\\) and \\(\\tau = 0.0581\\), highlighting the presence of small volume effects. Based on our analysis, we estimate that an additional uncertainty, associated with the modelling of reionisation, contributes an error of approximately \\(\\sigma_\\tau\\!\\sim\\!0.0006\\). Beyond the integrated optical depth, our analysis reveals that the inferred ionisation fraction as a function of redshift is highly model-dependent. While current CMB data do not favour significant early ionisation, they are consistent with a modest contribution from ionised gas at very early times (\\(z>15\\)). Although indicative upper bounds can be placed on such contributions, these limits remain strongly dependent on the assumed model.

We present constraints on cosmological parameters using maps from the last Planck data release (PR4). In particular, we detail an upgraded version of the cosmic microwave background likelihood, HiLLiPoP, based on angular power spectra and relying on a physical modelling of the foreground residuals in the spectral domain. This new version of the likelihood retains a larger sky fraction (up to 75%) and uses an extended multipole range. Using this likelihood, along with low-l measurements from LoLLiPoP, we derive constraints on \\(\\Lambda\\)CDM parameters that are in good agreement with previous Planck 2018 results, but with 10% to 20% smaller uncertainties. We demonstrate that the foregrounds can be accurately described in spectra domain with only negligible impact on \\(\\Lambda\\)CDM parameters. We also derive constraints on single-parameter extensions to \\(\\Lambda\\)CDM including \\(A_L\\), \\(\\Omega_K\\), \\(N_{eff}\\), and \\(\\sum m_{\\nu}\\). Noteworthy results from this updated analysis include a lensing amplitude value of \\(A_L = 1.039 \\pm 0.052\\), which aligns more closely with theoretical expectations within the \\(\\Lambda\\)CDM framework. Additionally, our curvature measurement, \\(\\Omega_K = -0.012 \\pm 0.010\\), now demonstrates complete consistency with a flat universe, and our measurement of \\(S_8\\) is closer to the measurements derived from large-scale structure surveys (at the 1.6\\(\\sigma\\) level). We also add constraints from PR4 lensing, making the combination the most constraining data set that is currently available from Planck. Additionally we explore adding baryon acoustic oscillation data, which tightens limits on some particular extensions to the standard cosmology.

The Quadratic Maximum Likelihood estimator can be used to reconstruct the Cosmic Microwave Background (CMB) power spectra with minimal error bars. Still, it requires an accurate estimate of the datasets noise covariance matrix in order to be corrected for spurious bias. We describe an extension of this method to cross-correlation, thus removing noise bias and mitigating the impact of systematic effects, providing they are uncorrelated. This estimator is tested on two simulation surveys at large and intermediate angular scales, respectively corresponding to satellite and ground-based CMB experiments. The analysis focuses on polarization maps, over a wide range of noise levels from 0.1 to 50 muK.arcmin. We show how this estimator minimizes the increase of variance due to polarization leakage between E and B modes. We compare this method with the pure pseudo-spectrum formalism which is computationally faster but less optimal, especially on large angular scales.

The utility of routine TEE to exclude LAA thrombus prior to AF ablation in patients treated with NOAC therapy is unclear. This single center retrospective study sought to investigate the incidence of left atrial appendage (LAA) thrombus in patients undergoing routine transesophageal echocardiography (TEE) prior to atrial fibrillation (AF) ablation treated with warfarin or non-vitamin K oral anticoagulant (NOAC) therapy. We included 937 routine pre-AF ablation TEE procedures performed in patients treated with warfarin (n=517) or NOAC (n=420). Patients were anticoagulated without interruption for at least 4 consecutive weeks prior to the TEE. Patients treated with warfarin had lower LAA velocity and underwent TEE earlier in the study period than patients treated with NOAC ( P <0.05). The incidence of LAA thrombus was higher in patients treated with warfarin (1.55%, 8/517) compared to patients treated with NOAC (0.24%, 1/420, P = 0.0473 for difference). No LAA thrombus was identified in NOAC treated patients with a CHA2 DS2 -VASC score <5 and in warfarin treated patients with a CHA2 DS2 -VASC score <2. TEE related complications occurred in 3/937 procedures (0.3%). In conclusion, LAA thrombus is detected rarely during pre-AF ablation TEE. Treatment with a NOAC is associated with a lower incidence of pre AF-ablation LAA thrombus compared to warfarin.

We present a joint cosmological analysis combining data from the Planck satellite, the Atacama Cosmology Telescope, and the South Pole Telescope, constructing a unified likelihood that reproduces the measured temperature and polarisation power spectra by jointly modelling the cosmic microwave background (CMB) signal, galactic and extragalactic foregrounds, and instrumental systematics across all datasets. This approach reduces reliance on external priors and improves the robustness of parameter estimation. Within this joint analysis, \\(\\Lambda\\)CDM parameters exhibit remarkable stability with respect to variations in foreground modelling. Extended cosmological parameters are more sensitive to these assumptions, with uncertainties increasing by up to 35%. Despite this, the combined constraints show no significant deviation from \\(\\Lambda\\)CDM expectations, and several previously reported tensions -- such as the preference for non-zero curvature or the excess of lensing amplitude A_L -- are significantly reduced or resolved. In contrast, the determination of foreground parameters more severely depends on the assumptions made about the underlying models. Overall, this work demonstrates the feasibility and reliability of a fully joint analysis of current CMB experiments, and emphasizes the importance of consistent and accurate foreground modelling for the scientific goals of next-generation, high-sensitivity CMB surveys.