bluuebunny/crossref_metadata_2025_split huggingface dataset:
Anatrophic nephrolithotomy and pyelolithotomy for dual staghorn calculi in bifid collecting system
Authors: Ealing Isaac , Calopedos Ross , Basto Marnique , Palma Catalina , Boulas John 
Published: November 2022

Abstract
A bifid ureter is an atypical anatomical variation that occurs with an incidence of 1–10%. This anomaly is in a continuum of duplex collecting systems and most commonly involves a common distal ureter. This is usually asymptomatic and is predominantly an incidental diagnosis, nevertheless, is a potential risk factor for urolithiasis formation. Current surgical management of larger staghorn calculi favours percutaneous nephrolithotomy (PCNL) over traditional open surgery, however for multiple calculi and complex anatomy PCNL would require multiple punctures, with increased risk of bleeding, pleural injury, sepsis and ultimately failed stone clearance. We describe the case of a 71-year-old female with multiple calculi in bifid anatomy. A single open approach, aided with cold-ischaemia was successfully utilized in this context.
Assessment of Training Load, Sleep, Injuries, and Operational Physical Performance During Basic Military Qualification
Authors: Laroche Marie-Andrée , Chassé Étienne , Théoret Daniel , Lalonde François , Comtois Alain-Steve 
Published: November 2022

ABSTRACT

Introduction
Optimizing training load (TL) and sleep is essential to maximize physical performance and prevent musculoskeletal injuries (MSKIs) for Canadian forces recruits during the 10-week basic military qualification (BMQ) course. The purpose of this study was to assess the TL, sleep duration, the occurrence of MSKIs during the BMQ, and the operation fitness performance during the BMQ.

Materials and Methods
Forty Canadian recruits, eight females and 32 males, (age 24 ± 5 years; height 176.4 ± 10.4 cm), were monitored with an accelerometer (GENEActiv) on their wrist between weeks 1 and 9 to evaluate the TL and sleep duration. During weeks 2 and 10, the recruits completed an operational fitness evaluation. Injury surveillance was performed over 10 weeks.

Results
TL intensity was significantly different (P = 0.0001) from week to week. The weekly average total time of moderate and vigorous physical activity was 189.7 ± 48.1 min and 44.7 ± 15.2 min, respectively. The average sleep duration was 5.4 ± 0.4 h per night and decreased to 4.2 h ± 0.4 during field exercises. A significant difference in sleep duration was observed between recruits with and without a MSKI. The recruits accumulated a total of 95 days under medical restrictions with an average of 3.8 consecutive days. The VO2peak estimated from the Fitness for Operational Requirements of Canadian Armed Forces Employment job–based simulation test significantly improved from weeks 2 to 10 (pre, 47.1 ± 6.3; post: 50.2 ± 5.8; P = 0.001).

Conclusions
TL is of high magnitude and varies from week to week. The reported mean sleep duration per week may perhaps negatively impact the occurrence of MSKI. No significant improvement was detected in operational fitness by the end of the BMQ.
The radio signal of PSR B0950 + 08 is detected over the whole pulse phase
Authors: Wang Zhengli , Lu Jiguang , Jiang Jinchen , Lin Jie , Lee Kejia , Liang Enwei , Xu Renxin 
Published: November 2022

ABSTRACT
Pulsars are known as the ‘lighthouses’ of the Universe. Periodic pulses with a duty cycle of $\sim 10{{\ \rm per\ cent}}$ are detected when the radio beam of a rotating pulsar sweeps across the telescope. In this report, 160-min data of a nearby pulsar, PSR B0950 + 08, observed with the Five-hundred-meter Aperture Spherical radio Telescope (FAST) are analysed. Thanks to the extremely high sensitivity of FAST, it is found that the radiation of PSR B0950 + 08 can be detected over the entire pulse period. To investigate the radiative characteristics of the pulsar’s ‘bridge emission’, a function, Θ(n), is defined to reveal the weak radiation there. It is suggested that the narrow peaks of both the main pulses and interpulses could be radiated at low altitude, while other weak emission (e.g. the ‘bridges’) comes from the upper magnetosphere, though its radiative mechanism is still a matter of debate. The measured mean pulse behaviours are consistent with previous results in the phase of strong emission of this pulsar, and both the frequency-independent separation between the interpulse and main pulse and the narrow pulse width may support a double-pole model. In order to understand the magnetospheric geometry of this pulsar, further polarization-calibrated observation with FAST and a proper determination of the baseline emission, especially during the weak emission phase, are surely required.
Radiative feedback on supermassive star formation: the massive end of the Population III initial mass function
Authors: Toyouchi Daisuke , Inayoshi Kohei , Li Wenxiu , Haiman Zoltán , Kuiper Rolf 
Published: November 2022

ABSTRACT
Supermassive stars with masses of M* ≃ 104–105 M⊙ are invoked as possible seeds of high-redshift supermassive black holes, but it remains under debate whether their protostar indeed acquires sufficient mass via gas accretion overcoming radiative feedback. We investigate protostellar growth in dynamically heated atomic cooling haloes (ACHs) found in recent cosmological simulations, performing three-dimensional radiation hydrodynamical simulations that consider stellar evolution under variable mass accretion. We find that one of the ACHs feeds the central protostar at rates exceeding a critical value, above which the star evolves in a cool bloating phase and hardly produces ionizing photons. Consequently, the stellar mass reaches M* ≳ 104 M⊙ unimpeded by radiative feedback. In the other ACH, where the mass supply rate is lower, the star evolves almost as a hot main-sequence star, emitting intense ionizing radiation. Then, the stellar mass growth is terminated around 500 M⊙ by photoevaporation of the circumstellar disc. Our simulations provide a formula of the final stellar mass determined either by stellar feedback or their lifetime as a function of the mass supply rate from the parent cloud. Combining the results with the statistical properties of star-forming clouds in high-redshift quasar progenitor haloes, we construct a top-heavy mass distribution of primordial stars over M* ≃ 100–105 M⊙, approximately following a power-law spectrum of ${\propto} M_\ast ^{-1.3}$. Their black hole remnants would be further fed via the dense debris disc, powering ‘milliquasars’ with a bolometric luminosity of Lbol ≳ 1043 erg s−1.
Does absorption against AGN reveal supermassive black hole accretion?
Authors: Rose Tom , McNamara B R , Combes F , Edge A C , Fabian A C , Gaspari M , Russell H , Salomé P , Tremblay G , Ferland G 
Published: November 2022

ABSTRACT
Galaxies often contain large reservoirs of molecular gas that shape their evolution. This can be through cooling of the gas – which leads to star formation, or accretion on to the central supermassive black hole – which fuels active galactic nucleus (AGN) activity and produces powerful feedback. Molecular gas has been detected in early-type galaxies on scales of just a few tens to hundreds of solar masses by searching for absorption against their compact radio cores. Using this technique, ALMA has found absorption in several brightest cluster galaxies, some of which show molecular gas moving towards their galaxy’s core at hundreds of km s−1. In this paper, we constrain the location of this absorbing gas by comparing each galaxy’s molecular emission and absorption. In four galaxies, the absorption properties are consistent with chance alignments between the continuum and a fraction of the molecular clouds visible in emission. In four others, the properties of the absorption are inconsistent with this scenario. In these systems, the absorption is likely produced by a separate population of molecular clouds in close proximity to the galaxy core and with high inward velocities and velocity dispersions. We thus deduce the existence of two types of absorber, caused by chance alignments between the radio core and: (i) a fraction of the molecular clouds visible in emission, and (ii) molecular clouds close to the AGN, in the process of accretion. We also present the first ALMA observations of molecular emission in S555, Abell 2390, RXC J1350.3+0940, and RXC J1603.6+1553 – with the latter three having $M_{\rm {mol}} \gt 10^{10}\, \rm {M}_{\odot }$.
The ALMA REBELS survey: the dust-obscured cosmic star formation rate density at redshift 7
Authors: Algera Hiddo S B , Inami Hanae , Oesch Pascal A , Sommovigo Laura , Bouwens Rychard J , Topping Michael W , Schouws Sander , Stefanon Mauro , Stark Daniel P , Aravena Manuel , Barrufet Laia , da Cunha Elisabete , Dayal Pratika , Endsley Ryan , Ferrara Andrea , Fudamoto Yoshinobu , Gonzalez Valentino , Graziani Luca , Hodge Jacqueline A , Hygate Alexander P S , de Looze Ilse , Nanayakkara Themiya , Schneider Raffaella , van der Werf Paul P 
Published: November 2022

ABSTRACT
Cosmic dust is an essential component shaping both the evolution of galaxies and their observational signatures. How quickly dust builds up in the early Universe remains an open question that requires deep observations at (sub-)millimetre wavelengths to resolve. Here, we use Atacama Large Millimeter Array observations of 45 galaxies from the Reionization Era Bright Emission Line Survey (REBELS) and its pilot programs, designed to target [C ii] and dust emission in UV-selected galaxies at z ∼ 7, to investigate the dust content of high-redshift galaxies through a stacking analysis. We find that the typical fraction of obscured star formation fobs = SFRIR/SFRUV+IR depends on stellar mass, similar to what is observed at lower redshift, and ranges from fobs ≈ 0.3 − 0.6 for galaxies with log10(M⋆/M⊙) = 9.4–10.4. We further adopt the z ∼ 7 stellar mass function from the literature to extract the obscured cosmic star formation rate density (SFRD) from the REBELS survey. Our results suggest only a modest decrease in the SFRD between 3 ≲ z ≲ 7, with dust-obscured star formation still contributing ${\sim}30{{\ \rm per\ cent}}$ at z ∼ 7. While we extensively discuss potential caveats, our analysis highlights the continued importance of dust-obscured star formation even well into the epoch of reionization.
Machine learning classification of CHIME fast radio bursts – I. Supervised methods
Authors: Luo Jia-Wei , Zhu-Ge Jia-Ming , Zhang Bing 
Published: November 2022

ABSTRACT
Observationally, the mysterious fast radio bursts (FRBs) are classified as repeating ones and apparently non-repeating ones. While repeating FRBs cannot be classified into the non-repeating group, it is unknown whether the apparently non-repeating FRBs are actually repeating FRBs whose repetitions are yet to be discovered, or whether they belong to another physically distinct type from the repeating ones. In a series of two papers, we attempt to disentangle this mystery with machine learning methods. In this first paper, we focus on an array of supervised machine learning methods. We train the machine learning algorithms with a fraction of the observed FRBs in the first CHIME/FRB catalogue, telling them which ones are apparently non-repeating and which ones are repeating. We then let the trained models predict the repetitiveness of the rest of the FRB data with the observed parameters, and we compare the predictions with the observed repetitiveness. We find that the models can predict most FRBs correctly, hinting towards distinct mechanisms behind repeating and non-repeating FRBs. We also find that the two most important distinguishing factors between non-repeating and repeating FRBs are brightness temperature and rest-frame frequency bandwidth. By applying the trained models back to the entire first CHIME catalogue, we further identify some potentially repeating FRBs currently reported as non-repeating. We recommend a list of these bursts as targets for future observing campaigns to search for repeated bursts in a combination with the results presented in Paper II using unsupervised machine learning methods.
The Three Hundred Project: Connection between star formation quenching and dynamical evolution in and around simulated galaxy clusters
Authors: Hough Tomás , Cora Sofía A , Haggar Roan , Vega-Martinez Cristian , Kuchner Ulrike , Pearce Frazer , Gray Meghan , Knebe Alexander , Yepes Gustavo 
Published: November 2022

ABSTRACT
In this work, we combine the semi-analytic model of galaxy formation and evolution sag with the 102 relaxed simulated galaxy clusters from the three hundred project, and we study the link between the quenching of star formation (SF) and the physical processes that galaxies experience through their dynamical history in and around clusters. We classify galaxies in four populations based on their orbital history: recent and ancient infallers, and backsplash and neighbouring galaxies. We find that ∼85 per cent of the current population of quenched galaxies located inside the clusters are ancient infallers with low or null content of hot and cold gas. The fraction of quenched ancient infallers increases strongly between the first and second pericentric passage, due to the removal of hot gas by the action of ram-pressure stripping (RPS). The majority of them quenches after the first pericentric passage, but a non-negligible fraction needs a second passage, specially galaxies with $M_\star \le 10^{10.5} \, {\rm M_\odot }$. Recent infallers represent ∼15 per cent of the quenched galaxies located inside the cluster and, on average, they contain a high proportion of hot and cold gas; moreover, pre-processing effects are responsible for quenching the recent infallers prior to infall onto the main cluster progenitor. The ∼65 per cent of quenched galaxies located around clusters are backsplash galaxies, for which the combination of RPS acting during a pre-processing stage and inside the cluster is necessary for the suppression of SF in this population.
Spectroscopic follow-up of a subset of the Gaia/IPHAS catalogue of Hα-excess sources
Authors: Fratta M , Scaringi S , Monguió M , Pala A F , Drew J E , Knigge C , Iłkiewicz K A , Gandhi P 
Published: November 2022

ABSTRACT
State-of-the-art techniques to identify Hα emission-line sources in narrow-band photometric surveys consist of searching for  Hα excess with reference to nearby objects in the sky (position-based selection). However, while this approach usually yields very few spurious detections, it may fail to select intrinsically faint and/or rare Hα-excess sources. In order to obtain a more complete representation of the heterogeneous emission-line populations, we recently developed a technique to find outliers relative to nearby objects in the colour–magnitude diagram (CMD-based selection). By combining position-based and CMD-based selections, we built an updated catalogue of Hα-excess candidates in the Northern Galactic Plane. Here, we present spectroscopic follow-up observations and classification of 114 objects from this catalogue that enables us to test our novel selection method. Out of the 70 spectroscopically confirmed Hα-emitters in our sample, 15 were identified only by the CMD-based selection, and would have been thus missed by the classic position-based technique. In addition, we explore the distribution of our spectroscopically confirmed emitters in the Gaia CMD. This information can support the classification of emission-line sources in large surveys such as the upcoming WEAVE and 4-m Multi-Object Spectroscopic Telescope, especially if augmented with the introduction of other colours.
An accurate set of H3O+ − H2 collisional rate coefficients for non-LTE modelling of warm interstellar clouds
Authors: Demes Sándor , Lique François , Faure Alexandre , van der Tak Floris F S 
Published: November 2022

ABSTRACT
Hydronium (H3O+) was first detected in 1986 in interstellar molecular clouds. It was reported in many Galactic diffuse and dense regions, as well as in extragalactic sources. H3O+ plays a major role both in interstellar oxygen and water chemistry. However, despite the large number of H3O+ observations, its collisional excitation was investigated only partially. In this work, we study the state-to-state rotational (de-)excitation of ortho- and para-H3O+ in collisions both with ortho- and para-H2. The cross sections are calculated within the close-coupling formalism using a highly accurate potential energy surface developed for this system. The rate coefficients are computed up to a kinetic temperature of 300 K. Transitions between the lowest 21 rotation-inversion states were studied for para-H3O+, and the lowest 11 states for ortho-H3O+, i.e. all levels with rotational energies below 430 K (∼300 cm−1) are considered. In order to estimate the impact of the new rate coefficients on the astrophysical models for H3O+, radiative transfer calculations were also carried out. We have examined how the new collisional data affect the line intensities with respect to older data previously used for the interpretation of observations. By analysing all detected transitions we find that our new, accurate rate coefficients have a significant impact (typically within a factor of 2) on radiation temperatures, allowing more accurate estimation of column densities and relative abundances of hydronium, especially in warm molecular clouds, paving the path towards better interpretation of interstellar water and oxygen chemistry.
Collective effects in an incompressible electronic liquid
Authors: Miao Jian-Jian , Jin Hui-Ke , Zhou Yi 
Published: November 2022

ABSTRACT
Starting from Landau’s kinetic equation, we show that an electronic liquid in d = 2, 3 spatial dimensions depicted by a Landau-type effective theory will become incompressible on condition that the Landau parameters satisfy either (i) $1+F_{1}^{s}/d=0$ or (ii) $F_{0}^{s}\rightarrow +\infty$. Condition (i) is the Pomeranchuk instability in the current channel and suggests a quantum spin liquid (QSL) state with a spinon Fermi surface; while condition (ii) means that the strong repulsion in the charge channel leads to a conventional charge and thermal insulator. In the collisionless regime (ωτ ≫ 1) and the hydrodynamic regime (ωτ ≪ 1), the zero and first sound modes have been studied and classified by symmetries, including the longitudinal and transverse modes in d = 2, 3 and the higher angular momentum modes in d = 3. The sufficient (and/or necessary) conditions of these collective modes have been revealed. It has been demonstrated that some of these collective modes will behave in quite different manners under incompressibility condition (i) or (ii). Possible nematic QSL states and a hierarchy structure for gapless QSL states have been proposed in d = 3.
Subgenomic RNA Abundance Relative to Total Viral RNA Among Severe Acute Respiratory Syndrome Coronavirus 2 Variants
Authors: Su Maxwell , Ping Sara , Nguyen Phuong-Vi , Rojas Alejandra , Hussaini Laila , Carmola Ludy Registre , Taz Azmain , Sullivan Julie , Martin Greg S , Piantadosi Anne , Martinez Magaly , Lam Wilbur A , Anderson Evan J , Waggoner Jesse J 
Published: November 2022

Abstract
Severe acute respiratory syndrome coronavirus 2 (SARS-CoV-2) subgenomic RNA (sgRNA) may indicate actively replicating virus, but sgRNA abundance has not been systematically compared between SARS-CoV-2 variants. sgRNA was quantified in 169 clinical samples by real-time reverse-transcription polymerase chain reaction, demonstrating similar relative abundance among known variants. Thus, sgRNA detection can identify individuals with active viral replication regardless of variant.
Generating 3D architectured nature-inspired materials and granular media using diffusion models based on language cues
Authors: Buehler Markus J 
Published: November 2022

Abstract
A variety of image generation methods have emerged in recent years, notably DALL-E 2, Imagen and Stable Diffusion. While they have been shown to be capable of producing photorealistic images from text prompts facilitated by generative diffusion models conditioned on language input, their capacity for materials design has not yet been explored. Here, we use a trained Stable Diffusion model and consider it as an experimental system, examining its capacity to generate novel material designs especially in the context of 3D material architectures. We demonstrate that this approach offers a paradigm to generate diverse material patterns and designs, using human-readable language as input, allowing us to explore a vast nature-inspired design portfolio for both novel architectured materials and granular media. We present a series of methods to translate 2D representations into 3D data, including movements through noise spaces via mixtures of text prompts, and image conditioning. We create physical samples using additive manufacturing and assess material properties of materials designed via a coarse-grained particle simulation approach. We present case studies using images as starting point for material generation; exemplified in two applications. First, a design for which we use Haeckel’s classic lithographic print of a diatom, which we amalgamate with a spider web. Second, a design that is based on the image of a flame, amalgamating it with a hybrid of a spider web and wood structures. These design approaches result in complex materials forming solids or granular liquid-like media that can ultimately be tuned to meet target demands.
Simple lessons from complex learning: what a neural network model learns about cosmic structure formation
Authors: Jamieson Drew , Li Yin , He Siyu , Villaescusa-Navarro Francisco , Ho Shirley , de Oliveira Renan Alves , Spergel David N 
Published: November 2022

Abstract
We train a neural network model to predict the full phase space evolution of cosmological N-body simulations. Its success implies that the neural network model is accurately approximating the Green’s function expansion that relates the initial conditions of the simulations to its outcome at later times in the deeply nonlinear regime. We test the accuracy of this approximation by assessing its performance on well-understood simple cases that have either known exact solutions or well-understood expansions. These scenarios include spherical configurations, isolated plane waves, and two interacting plane waves: initial conditions that are very different from the Gaussian random fields used for training. We find our model generalizes well to these well-understood scenarios, demonstrating that the networks have inferred general physical principles and learned the nonlinear mode couplings from the complex, random Gaussian training data. These tests also provide a useful diagnostic for finding the model’s strengths and weaknesses, and identifying strategies for model improvement. We also test the model on initial conditions that contain only transverse modes, a family of modes that differ not only in their phases but also in their evolution from the longitudinal growing modes used in the training set. When the network encounters these initial conditions that are orthogonal to the training set, the model fails completely. In addition to these simple configurations, we evaluate the model’s predictions for the density, displacement, and momentum power spectra with standard initial conditions for N-body simulations. We compare these summary statistics against N-body results and an approximate, fast simulation method called COLA (COmoving Lagrangian Acceleration). Our model achieves percent level accuracy at nonlinear scales of k∼1Mpc−1h, representing a significant improvement over COLA.