bluuebunny/crossref_metadata_2025_split huggingface dataset:
Improvement of image quality of dentomaxillofacial region in ultra-high-resolution CT: a phantom study
Authors: Sakai Yuki , Okamura Kazutoshi , Kitamoto Erina , Shirasaka Takashi , Kato Toyoyuki , Chikui Toru , Ishigami Kousei 
Published: November 2024

Abstract

Objectives
The purpose of this study was to compare the image quality of ultra-high-resolution CT (U-HRCT) with that of conventional multidetector row CT (convCT) and demonstrate its usefulness in the dentomaxillofacial region.

Methods
Phantoms were helically scanned with U-HRCT and convCT scanners using clinical protocols. In U-HRCT, phantoms were scanned in super-high-resolution (SHR) mode, and hybrid iterative reconstruction (HIR) and filtered-back projection (FBP) techniques were performed using a bone kernel (FC81). The FBP technique was performed using the same kernel as in convCT (reference). Two observers independently evaluated the 54 resulting images using a 5-point scale (5 = excellent diagnostic image quality; 4 = above average; 3 = average; 2 = subdiagnostic; and 1 = unacceptable). The system performance function (SPF) was calculated for a comprehensive evaluation of the image quality using the task transfer function and noise power spectrum. Statistical analysis using the Kruskal-Wallis test was performed to compare the image quality among the 3 protocols.

Results
The observers assigned higher scores to images acquired with the SHRHIR and SHRFBP protocols than to those acquired with the reference (P &lt; 0.0001 and P &lt; 0.0001, respectively). The relative SPF value at 1.0 cycles/mm in SHRHIR and SHRFBP compared to the reference protocol were 151.5% and 45.6%, respectively.

Conclusions
Through phantom experiments, this study demonstrated that U-HRCT can provide superior-quality images compared to conventional CT in the dentomaxillofacial region. The development of a better image reconstruction method is required to improve image quality and optimize the radiation dose.
Semi-Picking: A semi-supervised arrival time picking for microseismic monitoring based on the TransUGA network combined with SimMatch
Authors: Wang Qianfang , Sheng Guanqun , Tang Xingong , Xie Kai 
Published: November 2024

SUMMARY
An accurate and efficient method for picking the first arrival of microseismic signals is crucial for processing microseismic monitoring data. However, the weak magnitude and low signal-to-noise ratio (SNR) of these signals make picking arrivals challenging. Recent advancements in deep learning-based methods for picking the first arrivals of microseismic signals have effectively addressed the inefficiencies and inaccuracies of traditional methods. Nevertheless, these methods often require many training samples, and the substantial size and labelling effort significantly hinder the development of deep learning-based first-arrival picking methods. This study introduces Semi-Picking: a semi-supervised method for picking the first arrival of microseismic signals, utilizing the TransUGA network and SimMatch. This approach automatically labels microseismic signals following sample augmentation by establishing a semi-supervised learning framework, significantly reducing the time required for sample labelling. Initially, the TransUNet model is enhanced by incorporating the Self-Supervised Predictive Convolutional Attention Block (SSPCAB) module to create a Deep-TransUNet architecture, which more effectively separates signal from noise in microseismic signals with low SNR and improves the accuracy of first-arrival picking. Subsequently, the data sets for this study are compiled from microseismic traces collected from field monitoring records. Finite-difference forward modelling is applied to the microseismic data to train the network, and hyperparameter tuning is performed to optimize the UGATIT and Deep-TransUNet architecture. The outcomes of the arrival-picking experiments, conducted under conditions of low SNR using both synthetic and real microseismic records, demonstrated that Semi-Picking offers robust resistance to incorrect labels. This resilience stems from the synergistic use of the semi-supervised learning framework and self-attention mechanisms. The proposed method demonstrates superiority over the TransUNet, the SSPCAB-TransUNet, the UNet++ and the traditional short-term average/long-term average method, respectively, with the picking error rate of the Semi-Picking Net being less than 0.1 s. The proposed method outperforms the commonly used deep learning-based approaches for picking the first arrivals of microseismic signals, exhibiting superior performance.
Governance challenges to protect globally important ecosystem services of the Antarctic and Southern Ocean
Authors: Stoeckl Natalie , Adams Vanessa , Baird Rachel , Boothroyd Anne , Costanza Robert , Finau Glenn , Fulton Elizabeth A , Hatton MacDonald Darla , King Matt A , Kubiszewski Ida , Leane Elizabeth , Melbourne-Thomas Jess , Nielsen Hanne E F , Ooi Can-Seng , Raghavan Mala , Senigaglia Valeria , Tian Jing , Yamazaki Satoshi 
Published: November 2024

Abstract
Antarctica and the Southern Ocean (A&SO) has a unique environment that plays an important role in the Earth’s life-support systems. It has no indigenous human population but hosts around 5000 researchers and is visited by more than 100 000 tourists per year. In this paper, we describe the biophysical processes that create the region’s ecosystem services, outlining their related governance systems within the Antarctic Treaty System (ATS), and show the global distribution of the ecosystem service beneficiaries. These services clearly support populations across the world but are endangered by anthropogenic activities, which the current place-based ATS is not empowered to control. We discuss whether it is possible to use insights from Elinor Ostrom’s work on managing the commons, including her eight core design principles and the idea of Common Asset Trusts, to better harness efforts to protect ALL of the region’s ecosystem services. We note that many existing arrangements associated with the ATS are already well-aligned with Ostrom’s design principles but need to be expanded to better protect the globally important ecosystem services produced by A&SO.
Natural Boosting and the Immunogenicity of the XBB.1.5 Monovalent Vaccine in the Coronavirus Disease 2019 Endemic Era: A Longitudinal Observational Study
Authors: Kang Hyun Myung , Kim Hye-Jin , Jung Jiwon , Ahn Jin Young , Song Kyoung-Ho , Baek Jin Yang , Choi Ju-yeon , Lee Young Jae , Jeong Hyeonji , Kim Su-Hwan , Park Soyoung , Jang Hye Min , Rhie Gi-eun , Kim Eu Suk , Choi Jun Yong , Kim Sung-Han , Kang Eun-Suk , Peck Kyong Ran , Jeong Hye Won , Ko Jae-Hoon 
Published: November 2024

Abstract

Background
With the transition from the coronavirus disease 2019 (COVID-19) pandemic into endemicity, changes in group immunity and the effect of updated XBB.1.5 monovalent vaccine (MonoV) need to be investigated.

Methods
A multicenter vaccine cohort was followed for 3 years, and the investigation period was classified into the pre-Omicron, Omicron, and endemic eras. Thirteen sampling points were assessed, including pre- and post-MonoV administration. Specimens were classified as vaccinated, molecularly or serologically diagnosed breakthrough infection (BI), natural boosting (NB), or waned.

Results
A total of 327 healthcare workers contributed 2645 blood samples from March 2021 to December 2023. The log10 anti-spike protein antibody (SAb) levels, elevated by vaccination, declined linearly in the pre-Omicron era, were maintained during the Omicron era due to BIs, and increased in the endemic era (slope = 0.02, P = .02) without additional vaccination. NB cases increased significantly across the epidemiologic eras. The incidence rate ratios were 2.72 (P &lt; .001) for Omicron/pre-Omicron and 3.39 (P &lt; .001) for endemic/Omicron. Plaque reduction neutralization test (PRNT) titers against circulating strains (XBB.1.5 and XBB.1.9.1) in the NB group maintained previous levels, but ratios to wild-type PRNT and fold changes exhibited significantly enhanced activity. The XBB.1.5 MonoV increased PRNT by 5.8-fold against XBB.1.5 and 6.6-fold against JN.1, showing stronger enhancement against subsequent epidemic strains than the bivalent vaccine.

Conclusions
Group immunity in the COVID-19 endemic era exhibited maintained SAb levels and adjusted neutralizing activities through BI and NB. The XBB.1.5 MonoV significantly enhanced neutralizing activity against the vaccine strain and robust immunity against the subsequent epidemic JN.1 strain.
Measuring Users’ Trust in VIA Responses: The Age and Response Forms Perspective
Authors: Kang Rui , Rau Pei-Luen Patrick 
Published: November 2024

Abstract
When interacting with voice intelligent assistants (VIAs), users of different age groups usually react differently to the devices’ responses. This research focused on two influencing factors of users’ trust—user age and VIA response forms, and devised an experiment followed up with voluntary semi-structured interviews with 100 younger adult users (aged 22 to 59), 100 older adult users (aged 66 to 79) and 100 child users (aged 6 to11) to (i) quantify the varying degrees of trust across distinct age groups in the different presentation forms used to convey the same response content from VIAs, (ii) identify how the type of question posed influences on the levels of trust exhibited by users of different age groups in VIA response forms and (iii) explore the underlying rationales and motivations behind user perceptions and attitudes towards the diverse presentation forms of VIA responses, accounting for variations across different age demographics. In this paper, seven VIA response forms was studied, i.e. picture, text, hyperlink, ‘picture + text’, ‘picture + hyperlink’, ‘text + hyperlink’, and ‘picture + text + hyperlink’. Results indicate that users from different age groups demonstrate varying degrees of trust in the same responses when presented in different forms, expanding the research on users’ trust from the distinctive perspectives of user ages and response forms, while providing manufacturers with insights into consumer psychology.
Flexible modelling of time-varying exposures and recurrent events to analyse training load effects in team sports injuries
Authors: Zumeta-Olaskoaga Lore , Bender Andreas , Lee Dae-Jin 
Published: November 2024

Abstract
We present a flexible modelling approach to analyse time-varying exposures and recurrent events in team sports injuries. The approach is based on the piece-wise exponential additive mixed model where the effects of past exposures (i.e. high-intensity training loads) may accumulate over time and present complex forms of association. In order to identify a relevant time window at which past exposures have an impact on the current risk, we propose a penalty approach. We conduct a simulation study to evaluate the performance of the proposed model, under different true weight functions and different levels of heterogeneity between recurrent events. Finally, we illustrate the approach with a case study application involving an elite male football team participating in the Spanish LaLiga competition. The cohort includes time-loss injuries and external training load variables tracked by Global Positioning System devices, during the seasons 2017–2018 and 2018–2019.
NGTS-31b and NGTS-32b: two inflated hot Jupiters orbiting subgiant stars
Authors: Vines Jose I , Jenkins James S , Anderson David R , Alves Douglas R , Moyano Maximiliano , Acton Jack S , Apergis Ioannis , Barkaoui Khalid , Bayliss Daniel , Bouchy Francois , Bryant Edward M , Burleigh Matthew R , Casewell Sarah L , Christiansen Jessie L , Collins Karen A , Eigmüller Philipp , Falk Ben , Gill Samuel , Gillen Edward , Goad Michael R , Günther Maximilian N , Henderson Beth A , Kendall Alicia , Lendl Monika , McCormac James , Nielsen Louise D , Osborn Ares , Ramsay Gavin , Ricker George R , Rowden Pamela , Rudat Alexander , Saha Suman , Seager Sara , Smith Alexis M S , Tan Thiam-Guan , Tilbrook Rosanna H , Udry Stéphane , West Richard , Wheatley Peter J , Winn Joshua N , Zivave Tafadzwa 
Published: November 2024

ABSTRACT
We present the discoveries of NGTS-31b(= TOI-2721), and NGTS-32b, two hot Jupiters from the Next Generation Transit Survey (NGTS) transiting slightly evolved stars. The orbital periods, radii, and masses are 4.16 and 3.31 d, 1.61 and 1.42 $R_{J}$, and 1.12 and 0.57 $M_{J}$, respectively. Both planets have an incident stellar flux significantly above the threshold where inflation occurs, with both planets showing signs of inflation. These planets have widely different equilibrium temperatures than other hot Jupiters of similar mass and radius, with NGTS-31b having a significantly lower temperature, and NGTS-32b being hotter. This dichotomy raises the question of how prevalent the roles of other inflation mechanisms are in the radius anomaly phenomena and will help further constrain different inflationary models.
Polycyclic aromatic hydrocarbons in exoplanet atmospheres: a detectability study
Authors: Arenales-Lope Rosa , Molaverdikhani Karan , Dubey Dwaipayan , Ercolano Barbara , Grübel Fabian , Rab Christian 
Published: November 2024

ABSTRACT
In this paper, we explore the detectability of polycyclic aromatic hydrocarbons (PAHs) under diverse planetary conditions, aiming to identify promising targets for future observations of planetary atmospheres. Our primary goal is to determine the minimum detectable mass fractions of PAHs on each studied planet. We integrate the one-dimensional self-consistent model petitcode with petitradtrans, a radiative transfer model, to simulate the transmission spectra of these planets. Subsequently, we employ the pandexo noise simulator using the NIRSpec PRISM instrument aboard the JWST to assess the observability. Then, we conduct a Bayesian analysis through the multinest code. Our findings illustrate that variations in C/O ratios and planet temperatures significantly influence the transmission spectra and the detectability of PAHs. Our results show that planets with [Fe/H] = 0 and 1, C/O = 0.55, and temperatures around 1200 K are the most promising for detecting PAHs, with detectable mass fractions as low as 10$^{-7}$, or one thousandth of the interstellar medium abundance level. For colder planets with lower metallicities and C/O ratios, as well as hotter planets with carbon-rich atmospheres, PAHs can be detected at abundances around 10$^{-6}$. These results aid our strategy for selecting targets to study PAHs in the atmospheres of exoplanets.
Elevated UV luminosity density at Cosmic Dawn explained by non-evolving, weakly mass-dependent star formation efficiency
Authors: Feldmann Robert , Boylan-Kolchin Michael , Bullock James S , Çatmabacak Onur , Faucher-Giguère Claude-André , Hayward Christopher C , Kereš Dušan , Lazar Alexandres , Liang Lichen , Moreno Jorge , Oesch Pascal A , Quataert Eliot , Shen Xuejian , Sun Guochao 
Published: November 2024

ABSTRACT
Recent observations with JWST have uncovered unexpectedly high cosmic star formation activity in the early Universe, mere hundreds of millions of years after the big bang. These observations are often understood to reflect an evolutionary shift in star formation efficiency (SFE) caused by changing galactic conditions during these early epochs. We present FIREbox$^{\it HR}$, a high-resolution, cosmological hydrodynamical simulation from the Feedback in Realistic Environments (FIRE) project, which offers insights into the SFE of galaxies during the first billion years of cosmic time. FIREbox$^{\it HR}$ re-simulates the cosmic volume ($L=22.1$ cMpc) of the original FIREbox run with eight times higher mass resolution ($m_{\rm b}\sim {}7800\, M_\odot$), but with identical physics, down to $z\sim {}6$. FIREbox$^{\it HR}$ predicts ultraviolet (UV) luminosity functions in good agreement with available observational data. The simulation also successfully reproduces the observed cosmic UV luminosity density at $z\sim {}6{\!-\!}14$, demonstrating that relatively high star formation activity in the early Universe is a natural outcome of the baryonic processes encoded in the FIRE-2 model. According to FIREbox$^{\it HR}$, the SFE–halo mass relation for intermediate mass haloes ($M_{\rm halo}\sim {}10^9{\!-\!}10^{11}\, {\rm M}_\odot$) does not significantly evolve with redshift and is only weakly mass-dependent. These properties of the SFE–halo mass relation lead to a larger contribution from lower mass haloes at higher z, driving the gradual evolution of the observed cosmic UV luminosity density. A theoretical model based on the SFE–halo mass relation inferred from FIREbox$^{\it HR}$ allows us to explore implications for galaxy evolution. Future observations of UV faint galaxies at $z\gt 12$ will provide an opportunity to further test these predictions and deepen our understanding of star formation during Cosmic Dawn.
The frequency and mass-ratio distribution of binaries in clusters – III. Probabilistic generative modelling of six young open clusters
Authors: Alexander Jason S , Albrow Michael D 
Published: November 2024

ABSTRACT
We apply probabilistic generative modelling of colour–magnitude diagrams to six young Galactic open star clusters and determine their mass functions, binary mass-ratio distributions, and the frequencies of binary stars. We find that younger clusters tend to exhibit a higher incidence of binaries than their older counterparts. The mass-ratio distribution is fairly flat for the clusters, with one exception that exhibits a sharp increase for $q\gtrsim 0.9$. The ratio of the number of cluster binaries for which $q\gt 0.75$ to the number of binaries for which $q\gt 0.5$ (referred to as $FQ_{75}$) ranges from $\sim 0.4 \,{\text{to}}\, 0.8$. This metric increases with the binary-star frequency of a cluster but declines with cluster age. This may be due to non-ionizing three-body dynamical processing of a primordial population of close binaries with initial mass ratios, $q \simeq 1$.
The properties of the interstellar medium in dusty star-forming galaxies at z ∼ 2–4: the shape of the CO spectral line energy distributions
Authors: Taylor Dominic J , Swinbank A M , Smail Ian , Puglisi Annagrazia , Birkin Jack E , Dudzevičiūtė Ugne , Chen Chian-Chou , Ikarashi S , Frias Castillo Marta , Weiß Axel , Li Zefeng , Chapman Scott C , Jansen Jasper , Jiménez-Andrade E F , Morabito Leah K , Murphy Eric J , Rybak Matus , van der Werf P P 
Published: November 2024

ABSTRACT
The molecular gas in the interstellar medium (ISM) of star-forming galaxy populations exhibits diverse physical properties. We investigate the $^{12}$CO excitation of 12 dusty luminous star-forming galaxies at $z \sim$ 2–4 by combining observations of the $^{12}$CO from $J_{\rm up} = 1$ to $J_{\rm up} = 8$. The spectral line energy distribution (SLED) has a similar shape to NGC 253, M82, and local ultra-luminous infrared galaxies, with much stronger excitation than the Milky Way inner disc. By combining with resolved dust continuum sizes from high-resolution 870 $\mu$m ALMA observations and dust mass measurements determined from multiwavelength spectral energy distribution fitting, we measure the relationship between the $^{12}$CO SLED and probable physical drivers of excitation: star-formation efficiency, the average intensity of the radiation field $\langle U\rangle$, and the star-formation rate surface density. The primary driver of high-$J_{\rm up}$$^{12}$CO excitation in star-forming galaxies is star-formation rate surface density. We use the ratio of the CO(3–2) and CO(6–5) line fluxes to infer the CO excitation in each source and find that the average ratios for our sample are elevated compared to observations of low-redshift, less actively star-forming galaxies and agree well with predictions from numerical models that relate the ISM excitation to the star-formation rate surface density. The significant scatter in the line ratios of a factor $\approx 3$ within our sample likely reflects intrinsic variations in the ISM properties that may be caused by other effects on the excitation of the molecular gas, such as cosmic ray ionization rates and mechanical heating through turbulence dissipation.
Simultaneous two-colour intensity interferometry with H.E.S.S
Authors: Vogel Naomi , Zmija Andreas , Wohlleben Frederik , Anton Gisela , Mitchell Alison , Zink Adrian , Funk Stefan 
Published: November 2024

ABSTRACT
In recent years, intensity interferometry has been successfully applied to the Imaging Atmospheric Cherenkov Telescopes, H.E.S.S. , MAGIC, and VERITAS. All three telescope systems have proven the feasibility and capability of this method. After our first campaign in 2022, when two of the H.E.S.S. telescopes in Namibia were equipped with our external set-up and the angular diameter of two stars was measured, our set-up was upgraded for a second campaign in 2023, where the goal is to perform simultaneous two-colour measurements. The second campaign not only involves a third equipped telescope, but also each mechanical set-up now includes two interference filters at two different wavelengths (375 and 470 nm) with a broader bandwidth of 10 nm. This enables having simultaneous two-colour measurements, which yield information about the star’s physical size at different wavelengths. This is the first time that simultaneous dual-waveband intensity interferometry measurements have been performed. We report the angular diameter results of four stars, Mimosa ($\beta$ Cru), Eta Centauri ($\eta$ Cen), Nunki (σ Sgr), and Dschubba (δ Sco), where the effects of limb darkening are also taken into account.
A comparison of pre-existing ΛCDM predictions with the abundance of JWST galaxies at high redshift
Authors: Lu Shengdong , Frenk Carlos S , Bose Sownak , Lacey Cedric G , Cole Shaun , Baugh Carlton M , Helly John C 
Published: November 2024

ABSTRACT
Observations with the JWST have revealed a high abundance of bright galaxies at redshift, $z\gtrsim 12$, which has been widely interpreted as conflicting with the Lambda cold dark matter model. In Cowley et al., predictions were made – prior to the JWST observations – for the expected abundance of these galaxies using the Durham semi-analytic galaxy formation model, galform, which is known to produce a realistic population of galaxies at lower redshifts including the present day. Key to this model is the assumption of a ‘top-heavy’ initial mass function of stars formed in bursts (required to explain the number counts and redshift distribution of submillimetre galaxies). Here, we compare the rest-frame ultraviolet luminosity functions derived from JWST observations with those predicted by the Cowley et al. model up to $z=14$ and make further predictions for $z=16$. We find that below $z\sim 10$, the Cowley et al. predictions agree very well with observations, while agreement at $z\gtrsim 12$ requires extending the model to take into account the time-scale for the growth of obscuring dust grains at these very early times and its dependence on gas metallicity. We trace the evolution of these galaxies from $z=14$ to $z=0$ and find that their descendants typically reside in haloes with a median mass $2.5\times 10^{13}\, h^{-1}\, \mathrm{{\rm M}_{\odot }}$. The stellar masses of the descendants range from $3.2\times 10^{6}\, h^{-1}\, \mathrm{{\rm M}_{\odot }}$ to $3.2\times 10^{11}\, h^{-1}\, \mathrm{{\rm M}_{\odot }}$. Although these galaxies were all central galaxies at $z=14$, over half of their descendants end up as satellites in massive haloes.