bluuebunny/crossref_metadata_2025_split huggingface dataset:
Case Report: Isosulfan Blue–Related Anaphylaxis
Authors: Adams Jacob , Goc Jonathan , Zeien Justin , Patel Alpesh , Gambardella Josephine 
Published: January 2023

ABSTRACT
Anaphylaxis is an acute multisystem syndrome typically resulting from the sudden release of mast cell and basophil-derived mediators into the circulatory system. Isosulfan blue dye is a rare, but known, mediator of anaphylaxis with an incidence between 0.16% and 2% of cases. We report two cases of anaphylaxis attributed to the use of isosulfan blue dye in the intraoperative setting. Both of the patients we report had grade 3 anaphylactic reactions requiring vasopressors to correct significant hypotension. Both patients required overnight monitoring in the intensive care unit with the second patient also requiring continued vasopressor support.
Characterizing Methods for Surveying Partner Nation Medical Capabilities
Authors: Stone Alexandra , Regalbuto Eric , Wilson Ramey L 
Published: January 2023

ABSTRACT

Introduction
Medical capability surveys provide information about how U.S. forces can coordinate with partner nations to leverage partners’ capabilities to deliver care to sick or injured U.S. service members. Rotating forces routinely conduct these surveys. Currently, medical capability surveys are conducted based on individual unit requirements and personnel expertise and stored locally on component-specific sites or individual computers. The lack of a systematic approach and a centralized survey depot may undermine the ability to access previous surveys, leading to redundant surveys and conflicting information, and may have critical implications for force health protection. Partner nation facilities could have capabilities that may be leveraged to care for U.S. service members when U.S. medical care is unavailable. A lack of understanding of medical capabilities at partner nation facilities may undermine the ability to plan missions that mitigate risks.

Materials and Methods
This paper presents the results of 12 semi-structured focus groups with representatives from the U.S. Africa Command Surgeon’s office, the U.S. Transportation Command Patient Movement Requirements Center-East, and 9 U.S. Africa Command service components, sub-unified commands, and force providers. The focus group discussions considered questions on the following four topics: (1) methods for conducting surveys, (2) guidance about how to conduct surveys, (3) nodes of care and ancillary services included in surveys, and (4) how medical capability surveys are used to inform medical planning. The team conducted thematic analysis to identify emergent themes and subthemes.

Results
The team identified five primary, overarching themes: (1) guidance for conducting medical capability surveys, (2) methods and tools for conducting surveys, (3) content and focus of medical capability surveys, (4) archiving and sharing surveys, and (5) uses of medical capability surveys.

Conclusions
Implementing guidance and standardized templates for conducting medical capability surveys could improve the accuracy and completeness of surveys. Templates would likely increase the likelihood that surveyors collect relevant information on key medical capabilities. Training, along with guidance and templates, would provide a common understanding of how to conduct surveys. The lack of a DoD Global Health Engagement collaborative depot for storing and sharing surveys may undermine the ability to access previous surveys to inform future surveys and, thereby, results in inefficiencies in how surveys are conducted. The DoD should consider establishing a collaborative depot for medical capability surveys along with guidance or requirements for uploading surveys. Guidance, templates, training, and a collaborative depot could improve the effectiveness and efficiency of medical planning and thereby increase mission readiness.
Policy Recommendations for Increasing the Use of Evidence-Based Psychotherapy for Posttraumatic Stress Disorder in the Military Health System
Authors: McLean Carmen P , Cook Jeffrey , Riggs David S , Peterson Alan L , Young-McCaughan Stacey , Haddock Christopher K , Rosen Craig S 
Published: January 2023

ABSTRACTFew service members with posttraumatic stress disorder (PTSD) receive evidence-based psychotherapy (EBP) in the military health system (MHS). Efforts to increase EBP implementation have focused on provider training but have not adequately addressed organizational barriers. Thus, although behavioral health providers are trained in EBPs, clinic-, facility-, and system-level barriers preclude widespread EBP implementation. Building on work examining barriers to EBP use for PTSD across eight military treatment facilities, we propose recommendations for increasing the implementation of EBPs for PTSD and improving the quality of behavioral health care in MHS outpatient behavioral health clinics. Increasing the use of EBPs for PTSD will require that their use is supported and prioritized through MHS policy. We recommend that psychotherapy appointments are scheduled at least once weekly, as clinically indicated, as this frequency of care is prerequisite for EBP delivery. We propose several recommendations designed to increase system capacity for weekly psychotherapy, including improved triaging of potential patients, incentivizing and supporting group psychotherapy, matching the modality (i.e., group vs. individual) and frequency of treatment to patients’ needs, and using behavioral health technicians as clinician extenders. Additional recommendations include providing ongoing support for EBP implementation (e.g., protected time to participate in EBP consultation) and matching patients to providers based on patient’s clinical needs and treatment preferences. The barriers to EBP implementation that these recommendations target are interrelated. Therefore, adopting multiple policy recommendations is likely necessary to yield a meaningful and sustained increase in the implementation of EBPs for PTSD in the MHS.
Geomagnetic storm forecasting from solar coronal holes
Authors: Nitti Simona , Podladchikova Tatiana , Hofmeister Stefan J , Veronig Astrid M , Verbanac Giuliana , Bandić Mario 
Published: January 2023

ABSTRACT
Coronal holes (CHs) are the source of high-speed streams (HSSs) in the solar wind, whose interaction with the slow solar wind creates corotating interaction regions (CIRs) in the heliosphere. Whenever the CIRs hit the Earth, they can cause geomagnetic storms. We develop a method to predict the strength of CIR/HSS-driven geomagnetic storms directly from solar observations using the CH areas and associated magnetic field polarity. First, we build a data set comprising the properties of CHs on the Sun, the associated HSSs, CIRs, and orientation of the interplanetary magnetic field (IMF) at L1, and the strength of the associated geomagnetic storms by the geomagnetic indices Dst and Kp. Then, we predict the Dst and Kp indices using a Gaussian process model, which accounts for the annual variation of the orientation of Earth’s magnetic field axis. We demonstrate that the polarity of the IMF at L1 associated with CIRs is preserved in around 83 per cent of cases when compared to the polarity of their CH sources. Testing our model over the period 2010–2020, we obtained a correlation coefficient between the predicted and observed Dst index of R = 0.63/0.73, and Kp index of R = 0.65/0.67, for HSSs having a polarity towards/away from the Sun. These findings demonstrate the possibility of predicting CIR/HSS-driven geomagnetic storms directly from solar observations and extending the forecasting lead time up to several days, which is relevant for enhancing space weather predictions.
The contribution of magnetized galactic outflows to extragalactic Faraday rotation
Authors: Arámburo-García Andrés , Bondarenko Kyrylo , Boyarsky Alexey , Neronov Andrii , Scaife Anna , Sokolenko Anastasia 
Published: January 2023

ABSTRACT
Galactic outflows driven by star formation and active galactic nuclei blow bubbles into their local environments, causing galactic magnetic fields to be carried into intergalactic space. We explore the redshift-dependent effect of these magnetized bubbles on the Faraday rotation measure (RM) of extragalactic radio sources. Using the IllustrisTNG cosmological simulations, we separate the contribution from magnetic bubbles from that of the volume-filling magnetic component expected to be due to the seed field originating in the early universe. We use this separation to extract the redshift dependence of each component and to compare IllustrisTNG model predictions with observation measurements of the NRAO VLA sky survey (NVSS). We find that magnetized bubbles provide a sizeable contribution to the extragalactic RM, with redshift-independent 〈|RM|〉 ≃ 13 rad/m2 for sources at redshifts z ≥ 2. This is close to the mean residual RM of 16 rad/m2 found from NVSS data in this redshift range. Using the IllustrisTNG simulations, we also evaluate a simple model for the contribution to residual RM from individual host galaxies and show that this contribution is negligible at high-redshift. While the contribution from magnetic bubbles in the IllustrisTNG model is currently compatible with observational measurements of residual RM, the next-generation RM sky surveys, which will be free from the wrapping uncertainty, have larger statistics and better sensitivity should be able to observe predicted flat contribution from magnetic bubbles at large redshifts. This should allow to experimentally probe magnetic bubbles and check models of galaxy feedback in cosmological simulations.
An environmental analysis of the fast transient AT2018cow and implications for its progenitor and late-time brightness
Authors: Sun Ning-Chen , Maund Justyn R , Shao Yali , Janiak Ida A 
Published: January 2023

ABSTRACT
The nature of the newly discovered fast blue optical transients (FBOTs) is still puzzling astronomers. In this paper, we carry out a comprehensive analysis of the molecular gas, ionized gas, and stellar populations in the environment of the nearby FBOT AT2018cow based on ALMA, VLT/MUSE, and HST/WFC3 observations. A prominent molecular concentration of 6 (± 1) × 106 M⊙ is found in the vicinity of AT2018cow, which has given rise to two active star-forming complexes with ages of 4 ± 1 and ≲2.5 Myr, respectively. Each star-forming complex has a stellar mass of 3 × 105 M⊙, and has photoionized a giant H ii region with Hα luminosity even comparable to that of the 30 Dor mini-starburst region. AT2018cow is spatially coincident with one of the star-forming complexes; however, it is most likely to reside in its foreground since it has a much smaller extinction than the complex. Its progenitor could have been formed in a different star-forming event, and the non-detection of the associated stellar population constrains the progenitor’s age to be ≳10 Myr and initial mass to be ≲20 M⊙. We further find the late-time brightness of AT2018cow is unlikely to be a stellar object. Its brightness has slightly declined from 2 to 4 yr after explosion and is most likely to originate from AT2018cow itself due to some powering mechanism still working at such late times.
Star formation at the smallest scales: a JWST study of the clump populations in SMACS0723
Authors: Claeyssens Adélaïde , Adamo Angela , Richard Johan , Mahler Guillaume , Messa Matteo , Dessauges-Zavadsky Miroslava 
Published: January 2023

ABSTRACT
We present the clump populations detected in 18 lensed galaxies at redshifts 1--8.5 within the lensing cluster field SMACS0723. The recent JWST Early Release Observations of this poorly known region of the sky have revealed numerous point-like sources within and surrounding their host galaxies, undetected in the shallower Hubble Space Telescope images. We use JWST multi-and photometry and the lensing model of this galaxy cluster to estimate the intrinsic sizes and magnitudes of the stellar clumps. We derive optical restframe effective radii from &lt;10 to hundreds pc and masses ranging from ∼105 to 109 M ⊙, overlapping with massive star clusters in the local universe. Clump ages range from 1 Myr to 1 Gyr. We compare the crossing time to the age of the clumps and determine that between 45 and 60 per cent of the detected clumps are consistent with being gravitationally bound. On average, the dearth of Gyr old clumps suggests that the dissolution time scales are shorter than 1 Gyr. We see a significant increase in the luminosity (mass) surface density of the clumps with redshift. Clumps in reionization era galaxies have stellar densities higher than star clusters in the local universe. We zoom in into single galaxies at redshift &lt;6 and find for two galaxies, the Sparkler and the Firework, that their star clusters/clumps show distinctive colour distributions and location surrounding their host galaxy that are compatible with being accredited or formed during merger events. The ages of some of the compact clusters are between 1 and 4 Gyr, e.g. globular cluster precursors formed around 9--12 Gyr ago. Our study, conducted on a small sample of galaxies, shows the potential of JWST observations for understanding the conditions under which star clusters form in rapidly evolving galaxies.
The rotation rate of solar active and ephemeral regions – II. Temporal variations of the rotation rates
Authors: Kutsenko Alexander S , Abramenko Valentina I , Litvishko Daria V 
Published: January 2023

ABSTRACT
Systematic studies of the rotation rate of sunspot groups using white light images yield controversial results on the variations of the rotation rate: sunspot groups were found to either accelerate or decelerate systematically. This disagreement might be related to shortcomings of the method used to probe the rotation rate of sunspot groups. In contrast to previous works, in this study we use magnetic field maps to analyse the variations of the rotation rate of active regions. We found that an active region may exhibit either acceleration or deceleration during the emergence, while the rotation rate remains almost unchanged during decay. Hence, we suppose that there is no systematic geometrical inclination to the radial direction of the apex of the subsurface magnetic flux loop forming an active region. A thorough comparison of the rotation rate of unipolar and bi/multipolar active regions revealed no significant changes in the rotation rate of decaying active regions. In contrast to previous works, we presume the rotation rate to remain constant (within the expected uncertainties) during the evolution of an active region after emergence.
Dissecting the active galactic nucleus in Circinus – IV. MUSE-NFM observations unveil a tuning-fork ionized outflow morphology
Authors: Kakkad D , Stalevski M , Kishimoto M , Knežević S , Asmus D , Vogt F P A 
Published: January 2023

ABSTRACT
We present the ionized gas outflow morphology in the Circinus galaxy using the narrow-field mode (NFM) of the Multi Unit Spectroscopic Explorer (MUSE) instrument onboard the Very Large Telescope (VLT). The NFM observations provide a spatial resolution of ∼0.1 arcsec, corresponding to a physical scale of ∼2 pc, one of the highest spatial resolution achievable using ground-based adaptive optics-assisted observations in the optical wavelengths. The MUSE observations reveal a collimated clumpy outflow profile originating near the active galactic nucleus (AGN) location and extending up to 1.5 arcsec (∼30 pc) in the north-west direction. The collimated structure then fragments into two filaments, giving the entire outflowing gas a ‘tuning-fork’ morphology. These structures remain undetected in the lower spatial resolution MUSE wide-field mode data. We explain the origin of this tuning-fork structure to the interaction of the outflow with a dense clump in the interstellar medium (ISM) as the outflow propagates outwards. The origin of the collimated structure itself could be from jet–ISM interactions on small scales. These observations also provide evidence to the origin of the ionized gas filaments previously observed in the Circinus galaxy out to kiloparsec scales. We find instantaneous and time-averaged mass outflow rates of 10−2 and 10−4 M⊙ yr−1, respectively. Based on the star formation rate in the Circinus galaxy reported in the literature, the observed ionized outflows are not expected to regulate star formation within the ∼100 pc scales probed by the NFM data.
A comparison of numerical methods for computing the reionization of intergalactic hydrogen and helium by a central radiating source
Authors: Leong Ka-Hou , Meiksin Avery , Lai Althea , To K H 
Published: January 2023

ABSTRACT
We compare numerical methods for solving the radiative transfer equation in the context of the photoionization of intergalactic gaseous hydrogen and helium by a central radiating source. Direct integration of the radiative transfer equation and solutions using photon packets are examined, both for solutions to the time-dependent radiative transfer equation and in the infinite-speed-of-light approximation. The photon packet schemes are found to be more generally computationally efficient than a direct integration scheme. While all codes accurately describe the growth rate of hydrogen and helium ionization zones, it is shown that a fully time-dependent method is required to capture the gas temperature and ionization structure in the near zone of a source when an ionization front expands at a speed close to the speed of light. Applied to quasi-stellar objects in the Epoch of Reionization (EoR), temperature differences as high as 5 × 104 K result in the near zone for solutions of the time-dependent radiative transfer equation compared with solutions in the infinite-speed-of-light approximation. Smaller temperature differences are found following the nearly full photoionization of helium in gas in which the hydrogen was already ionized and the helium was singly ionized. Variations found in the temperature and ionization structure far from the source, where the gas is predominantly neutral, may affect some predictions for 21-cm EoR experiments.
Star formation histories of UV-luminous galaxies at z ≃ 6.8: implications for stellar mass assembly at early cosmic times
Authors: Whitler Lily , Stark Daniel P , Endsley Ryan , Leja Joel , Charlot Stéphane , Chevallard Jacopo 
Published: January 2023

ABSTRACT
The variety of star formation histories (SFHs) of z ≳ 6 galaxies provides important insights into early star formation, but has been difficult to systematically quantify. Some observations suggest that many z ∼ 6–9 galaxies are dominated by ≳200 Myr stellar populations, implying significant star formation at z ≳ 9, while others find that most reionization era galaxies are ≲10 Myr, consistent with little z ≳ 9 star formation. Here, we quantify the distribution of ages of UV-bright ($-22.5\lesssim M_{\rm \small UV}\lesssim -21$) galaxies colour-selected to lie at z ≃ 6.6–6.9, an ideal redshift range to systematically study the SFHs of reionization era galaxies with ground-based observatories and Spitzer. We infer galaxy properties with two SED modelling codes and compare results, finding that stellar masses are largely insensitive to the model, but the inferred ages can vary by an order of magnitude. We infer a distribution of ages assuming a simple, parametric SFH model, finding a median age of ∼30–70 Myr depending on SED model. We quantify the fractions of ≤10 and ≥250 Myr galaxies, finding that these systems comprise ∼15–30 per cent and ∼20–25 per cent of the population, respectively. With a flexible SFH model, the shapes of the SFHs are consistent with those implied by the simple model (e.g. young galaxies have rapidly rising SFHs). However, stellar masses can differ significantly, with those of young systems sometimes being more than an order of magnitude larger with the flexible SFH. We quantify the implications of these results for z ≳ 9 stellar mass assembly and discuss improvements expected from JWST.
Quasi-periodic behaviour in the radio and γ-ray light curves of blazar PKS 1510–089
Authors: Li Xiao-Pan , Cai Yan , Yang Hai-Yan , Lähteenmäki Anne , Tornikoski Merja , Tammi Joni , Suutarinen Sofia , Yang Hai-Tao , Luo Yu-Hui , Wang Li-Sha 
Published: January 2023

Abstract
We explore the possible quasi-periodic oscillations (QPOs) of the blazar PKS 1510–089, utilizing the ∼38-year Metsähovi flux density observations at 37 GHz and over ten-year Fermi-LAT observations in the 0.1–300 GeV energy range. Both the flux distributions of the radio and γ-ray light curves suggest a log-normal distribution, and power spectral densities (PSDs) of both light curves can be well represented by a bending power-law model. Comparing the results from the Weighted Wavelet Z-transform and Lomb-Scargle Periodogram approaches, a quasi period of 1330 ± 55 days at a 99.80% (&gt;3σ) significance against the red noise background is observed in the radio light curve, whereas no similar modulation is seen in the γ-ray light curve. We briefly discuss the research actuality of blazar QPO phenomena and explain the observed radio QPO as the result of Keplerian motion in a supermassive binary black hole system and periodic modulation induced by the Lense-Thirring precession of the innermost portions of the accretion disk.
A study of convective core overshooting as a function of stellar mass based on two-dimensional hydrodynamical simulations
Authors: Baraffe I , Clarke J , Morison A , Vlaykov D G , Constantino T , Goffrey T , Guillet T , Le Saux A , Pratt J 
Published: January 2023

ABSTRACT
We perform two-dimensional (2D) numerical simulations of core convection for zero-age main-sequence stars covering a mass range from 3 to 20 M⊙. The simulations are performed with the fully compressible time-implicit code music. We study the efficiency of overshooting, which describes the ballistic process of convective flows crossing a convective boundary, as a function of stellar mass and luminosity. We also study the impact of artificially increasing the stellar luminosity for 3 M⊙ models. The simulations cover hundreds to thousands of convective turnover time-scales. Applying the framework of extreme plume events previously developed for convective envelopes, we derive overshooting lengths as a function of stellar masses. We find that the overshooting distance (dov) scales with the stellar luminosity (L) and the convective core radius (rconv). We derive a scaling law $d_{\rm ov} \propto L^{1/3} r_{\rm conv}^{1/2}$, which is implemented in a one-dimensional stellar evolution code and the resulting stellar models are compared to observations. The scaling predicts values for the overshooting distance that significantly increase with stellar mass, in qualitative agreement with observations. Quantitatively, however, the predicted values are underestimated for masses ≳10 M⊙. Our 2D simulations show the formation of a nearly adiabatic layer just above the Schwarzschild boundary of the convective core, as exhibited in recent three-dimensional simulations of convection. The most luminous models show a growth in size with time of the nearly adiabatic layer. This growth seems to slow down as the upper edge of the nearly adiabatic layer gets closer to the maximum overshooting length and as the simulation time exceeds the typical thermal diffusive time-scale in the overshooting layer.