bluuebunny/crossref_metadata_2025_split huggingface dataset:
EPOCHS. IV. SED Modeling Assumptions and Their Impact on the Stellar Mass Function at 6.5 ≤ z ≤ 13.5 Using PEARLS and Public JWST Observations
Authors: Harvey Thomas , Conselice Christopher J. , Adams Nathan J. , Austin Duncan , Juodžbalis Ignas , Trussler James , Li Qiong , Ormerod Katherine , Ferreira Leonardo , Lovell Christopher C. , Duan Qiao , Westcott Lewi , Harris Honor , Bhatawdekar Rachana , Coe Dan , Cohen Seth H. , Caruana Joseph , Cheng Cheng , Driver Simon P. , Frye Brenda , Furtak Lukas J. , Grogin Norman A. , Hathi Nimish P. , Holwerda Benne W. , Jansen Rolf A. , Koekemoer Anton M. , Marshall Madeline A. , Nonino Mario , Vijayan Aswin P. , Wilkins Stephen M. , Windhorst Rogier , Willmer Christopher N. A. , Yan Haojing , Zitrin Adi 
Published: December 2024

Abstract
We utilize deep JWST Near Infrared Camera (NIRCam) observations for the first direct constraints on the Galaxy Stellar Mass Function (GSMF) at z > 10. Our EPOCHS v1 sample includes 1120 galaxy candidates at 6.5 < z < 13.5 taken from a consistent reduction and analysis of publicly available deep JWST NIRCam data covering the Prime Extragalactic Areas for Reionization Science, CEERS, GLASS, JADES GOOD-S, NGDEEP, and SMACS0723 surveys, totaling 187 arcmin2. We investigate the impact of spectral energy distribution fitting methods, assumed star formation histories (SFHs), dust laws, and priors on galaxy masses and the resultant GSMF. While our fiducial GSMF agrees with the literature at z < 13.5, we find that the assumed SFH model has a large impact on the GSMF and stellar mass density (SMD), finding a 0.75 dex increase in the SMD at z = 10.5 between a flexible nonparametric and standard parametric SFH. Overall, we find a flatter SMD evolution at z ≥ 9 than some studies predict, suggesting a rapid buildup of stellar mass in the early Universe. We find no incompatibility between our results and those of standard cosmological models, as suggested previously, although the most massive galaxies may require a high star formation efficiency. We find that the “little red dot” galaxies dominate the z = 7 GSMF at high masses, necessitating a better understanding of the relative contributions of active galactic nucleus and stellar emission. We show that assuming a theoretically motivated top-heavy initial mass function (IMF) reduces stellar mass by 0.5 dex without affecting fit quality, but our results remain consistent with existing cosmological models with a standard IMF.
Constraining the Galactic Structure Using Time Domain Gravitational Wave Signal from Double White Dwarfs Detected by Space Gravitational Wave Detectors
Authors: Zhang Siqi , Deng Furen , Lu Youjun , Yu Shenghua 
Published: December 2024

Abstract
The gravitational wave (GW) signals from a large number of double white dwarfs (DWDs) in the Galaxy are expected to be detected by space GW detectors, e.g., the Laser Interferometer Space Antenna (LISA), Taiji, and Tianqin in the millihertz band. In this paper, we present an alternative method by directly using the time-domain GW signal detected by space GW detectors to constrain the anisotropic structure of the Galaxy. The information of anisotropic distribution of DWDs is naturally encoded in the time-domain GW signal because of the variation of the detectors’ directions and consequently the pattern functions due to their annual motion around the Sun. The direct use of the time-domain GW signal enables simple calculations, such as utilizing an analytical method to assess the noise arising from the superposition of random phases of DWDs and using appropriate weights to improve the constraints. We investigate the possible constraints on the scale of the Galactic thin disk and bulge that may be obtained from LISA and Taiji by using this method with mock signals obtained from population synthesis models. We further show the different constraining capabilities of the low-frequency signal (foreground) and the high-frequency signal (resolvable sources) via the Markov Chain Monte Carlo method, and find that the scale height and length of the Galactic thin disk and the scale radius of the bulge can be constrained to a fractional accuracy of ∼30%, 30%, 40% (or 20%, 10%, 40%) by using the low-frequency (or high-frequency) signal detected by LISA or Taiji.
Radiatively Active Clouds and Magnetic Effects Explored in a Grid of Hot Jupiter GCMs
Authors: Kennedy Thomas D. , Rauscher Emily , Malsky Isaac , Roman Michael T. , Beltz Hayley 
Published: December 2024

Abstract
Cloud formation and magnetic effects are both expected to significantly impact the structures and observable properties of hot Jupiter atmospheres. For some hot Jupiters, thermal ionization and condensation can coexist in a single atmosphere, and both processes are important. We present a grid of general circulation models across a wide range of irradiation temperatures with and without incorporating the effects of magnetism and cloud formation to investigate how these processes work in tandem. We find that clouds are present in the atmosphere at all modeled irradiation temperatures, while magnetic effects are negligible for planets with irradiation temperatures cooler than 2000 K. At and above this threshold, clouds and magnetic fields shape atmospheres together, with mutual feedback. Models that include magnetism, through their influence on the temperature structure, produce more longitudinally symmetric dayside cloud coverage and more equatorially concentrated clouds on the nightside and morning terminator. To indicate how these processes would affect observables, we generate bolometric thermal and reflected phase curves from these models. The combination of clouds and magnetic effects increases thermal phase-curve amplitudes and decreases peak offsets more than either process does individually.
Rising Near-ultraviolet Spectra in Stellar Megaflares
Authors: Kowalski Adam F. , Osten Rachel A. , Notsu Yuta , Tristan Isaiah I. , Segura Antigona , Maehara Hiroyuki , Namekata Kosuke , Inoue Shun 
Published: December 2024

Abstract
Flares from M dwarf stars can attain energies up to 104 times larger than solar flares but are generally thought to result from similar processes of magnetic energy release and particle acceleration. Larger heating rates in the low atmosphere are needed to reproduce the shape and strength of the observed continua in stellar flares, which are often simplified to a blackbody model from the optical to the far-ultraviolet (FUV). The near-ultraviolet (NUV) has been woefully undersampled in spectral observations despite this being where the blackbody radiation should peak. We present Hubble Space Telescope NUV spectra in the impulsive phase of a flare with E
TESS ≈ 7.5 × 1033 erg and a flare with E
TESS ≈ 1035 erg and the largest NUV flare luminosity observed to date from an M star. The composite NUV spectra are not well represented by a single blackbody that is commonly assumed in the literature. Rather, continuum flux rises toward shorter wavelengths into the FUV, and we calculate that an optical T = 104 K blackbody underestimates the short-wavelength NUV flux by a factor of ≈6. We show that rising NUV continuum spectra can be reproduced by collisionally heating the lower atmosphere with beams of E ≳ 10 MeV protons or E ≳ 500 keV electrons and flux densities of 1013 erg cm−2 s−1. These are much larger than the canonical values describing accelerated particles in solar flares.
A Spectro-temporal View of Normal Branch Oscillations in Cygnus X-2 as Seen by NICER and NuSTAR
Authors: Sudha Malu , Ludlam Renee M. , Altamirano Diego , Cackett Edward M. , Hare Jeremy 
Published: December 2024

Abstract
We report the spectro-temporal study of the neutron star low mass X-ray binary Cygnus X-2 using NICER and NuSTAR data while the source was in the normal branch (NB). We detect a normal branch oscillation (NBO) feature at ∼5.41 Hz that appears in the middle portion of the NB branch. We note that the NBO appeared only in the 0.5–3 keV energy range, with maximum strength in the 1–2 keV energy band, but was absent in the 3–10 keV energy band of NuSTAR and NICER data. The energy spectrum of the source exhibits an emission feature at ∼1 keV, previously identified as the Fe L transition in the outer region of the accretion disk. Upon considering both the Fe L and NBO features, we suggest that the originating location of the Fe L line and the NBOs may coincide and perhaps be due to the same underlying mechanism. Therefore, lags seen in the frequency-/energy-dependent lag spectra of Cygnus X-2 could be considered to be arising from a region of photoionized material far from the central source. We study the frequency and energy-dependent lag spectra of the source, which exhibited a few millisecond hard lag at the NBO frequency (12–15 ms) and a switch from hard to soft lags at 1 keV. The rms spectrum peaks at 1 keV, and the covariance spectrum clearly resembles a thermal spectrum. We discuss the spectro-temporal behavior of the NBO and attempt to constrain its location of origin.
Magnetic Field Geometry and Anisotropic Scattering Effects on Solar Radio Burst Observations
Authors: Clarkson Daniel L. , Kontar Eduard P. 
Published: December 2024

Abstract
The fine structures of solar radio bursts reveal complex dynamics in the corona, yet the observed characteristics of these subsecond bursts are additionally complicated by radio wave scattering in the turbulent solar corona. We examine the impact of anisotropic turbulence in radio wave propagation simulations with nonradial magnetic field structures in shaping the morphology, time characteristics, and source positions of fine structures. The apparent sources are found to move along the direction of the magnetic field lines and not along the density gradient, whereas the major axis of the scattered source is perpendicular to the local magnetic field (the scattering anisotropy axis). Using a dipolar magnetic field structure of an active region, we reproduce observed radio fine-structure source motion parallel to the solar limb associated with a coronal loop and provide a natural explanation for puzzling observations of solar radio burst position motions with the Low Frequency Array. Furthermore, the anisotropy aligned with a dipolar magnetic field causes the apparent-source images to bifurcate into two distinct components, with characteristic sizes smaller than in unmagnetized media. The temporal broadening induced by scattering reduces the observed frequency drift rate of fine structures, depending on the contribution of scattering to the time profile. The findings underscore the role of magnetic field geometry and anisotropic scattering for the interpretation of solar radio bursts and highlight that anisotropic scattering produces more than a single source.
Magnetic Flux Transport in Advection-dominated Accretion Flow toward the Formation of a Magnetically Arrested Disk
Authors: Li Jia-Wen , Cao Xinwu 
Published: December 2024

Abstract
Magnetically arrested disks (MADs) have attracted much attention in recent years. The formation of MADs is usually attributed to the accumulation of a sufficient amount of dynamically significant poloidal magnetic flux. In this work, the magnetic flux transport within an advection-dominated accretion flow (ADAF) and the formation of an MAD are investigated. The structure and dynamics of an inner MAD connected with an outer ADAF are derived by solving a set of differential equations with suitable boundary conditions. We find that an inner MAD is eventually formed at a region about several 10 R
S outside the horizon. Due to the presence of a strong large-scale magnetic field, the radial velocity of the accretion flow is significantly decreased. The angular velocity of the MAD region is highly sub-Keplerian with Ω ∼ (0.4–0.5)ΩK, and the corresponding ratio of gas to magnetic pressure is about β ≲ 1. Also, we find that an MAD is unlikely to be formed through the inward flux advection process when the external magnetic field strength is weak enough with β
out ≳ 100 around R
out ∼ 1000 R
s. Based on a rough estimate, we find that the jet power of a black hole, with mass M
BH and spin a
*, surrounded by an ADAF with an inner MAD region is about 2 orders of magnitude larger than that of a black hole surrounded by a normal ADAF. This may account for the powerful jets observed in some Fanaroff–Riley type I galaxies with a very low Eddington ratio.
A Compilation of Optical Starlight Polarization Catalogs
Authors: Panopoulou G. V. , Markopoulioti L. , Bouzelou F. , Millar-Blanchaer M. A. , Tinyanont S. , Blinov D. , Pelgrims V. , Johnson S. , Skalidis R. , Soam A. 
Published: December 2024

Abstract
Polarimetry of stars at optical and near-infrared wavelengths is an invaluable tool for tracing interstellar dust and magnetic fields. Recent studies have demonstrated the power of combining stellar polarimetry with distances from the Gaia mission, in order to gain accurate, 3D information on the properties of the interstellar magnetic field and the dust distribution. However, access to optical polarization data is limited, as observations are conducted by different investigators, with different instruments, and are made available in many separate publications. To enable a more widespread accessibility of optical polarimetry for studies of the interstellar medium, we compile a new catalog of stellar polarization measurements. The data are gathered from 81 separate publications spanning two decades since the previous, widely used agglomeration of catalogs by C. Heiles. The compilation contains a total of 55,742 measurements of stellar polarization. We combine this database with stellar distances based on the Gaia Early Data Release 3, thereby providing polarization and distance data for 42,482 unique stars. We provide two separate data products: an extended catalog (containing all polarization measurements) and a unique source catalog (containing a subset of sources excluding duplicate measurements). We propose the use of a common tabular format for the publication of stellar polarization catalogs to facilitate accessibility and increase discoverability in the future.
Simulating a Steady-state Heliosphere
Authors: Heerikhuisen Jacob , Zirnstein Eric J. , Pogorelov Nikolai V. 
Published: December 2024

Abstract
Ever since the discovery of the solar wind, it has been understood that our solar system resides within a bubble of solar wind plasma that originates from the Sun. Due to its vast size, the geometry of this bubble, known as the heliosphere, remains a topic of conjecture and debate. Three-dimensional simulations, employing magnetohydrodynamics coupled to neutral particles, provide a key way of understanding the global flow dynamics on macroscopic scales. While many of these models suggest a comet-like shape with a single heliotail for the heliosphere, others have suggested geometries with two distinct outflows of solar wind plasma. In this paper we show how numerical simulations with the same boundary conditions may evolve differently, depending on factors such as initial conditions and run time. We find that the eventual steady state is the same comet-like shape, even for less than optimal choices of the initial condition.
Environmental Features of in Situ and Laboratory Simulations and Their Potential Impact on the Development of Teamwork Skills for Novice Trauma Professionals
Authors: Lapierre Alexandra , Lavoie Patrick , Arbour Caroline 
Published: December 2024

Background
The effect of environmental fidelity on the development of teamwork skills in health care simulations is unclear. This preliminary descriptive study explored how in situ and laboratory environments impact the development of teamwork skills among novice trauma professionals.

Method
Four teams of six novice trauma professionals participated in two in situ or two laboratory simulations. Environmental features such as noise, interruptions, and the presence of nonparticipating individuals were assessed. Teamwork skills were evaluated from video recordings with the Team Emergency Assessment Measure (TEAM).

Results
In situ simulations involved higher levels of noise, more interruptions, and the presence of nonparticipating individuals compared with laboratory simulations. Teamwork skills in the in situ setting were rated as poor, with no improvement between simulations. In contrast, in the laboratory setting, teamwork skills were rated as good, with a 10-point improvement.

Conclusion

Preliminary results suggest that the in situ environment may hinder the development of teamwork skills. Further research with larger samples is needed to explore these effects and guide educators in choosing optimal training environments for novice trauma health care professionals.

[
J Contin Educ Nurs.
2025;56(1):34–40.]
Consensus Based Indian Guidelines for the Management of Pemphigus Vulgaris and Pemphigus Foliaceous
Authors: De Dipankar , Mehta Hitaishi , Shah Shikha , Ajithkumar Kidangazhiathmana , Barua Shyamanta , Chandrashekar Laxmisha , Chatterjee Manas , Gupta Vishal , Khandpur Sujay , Khullar Geeti , Kolalapudi Seetharam Anjaneyulu , Kumar Sheetanshu , Neema Shekhar , Pandhi Deepika , Poojary Shital , Rai Reena , Rajagopalan Murlidhar , Rao Raghavendra , Shah Bela , Singal Archana , Thakur Vishal , Vinay Keshavamurthy , Aggrawal Ashutosh , De Arka , Mukherjee Soham , Prinja Shankar , Mahajan Rahul , Handa Sanjeev 
Published: December 2024

Abstract
Pemphigus is an autoimmune blistering disorder characterized by the presence of intraepidermal blisters and erosions, primarily affecting the mucosa and/or skin. There are no established Indian guidelines for the management of pemphigus, and Western guidelines cannot be directly applied due to differences in clinicodemographic profiles, comorbidities, and resource limitations. These guidelines aim to provide Indian dermatologists with evidence-based and consensus-driven recommendations for the management of pemphigus vulgaris (PV) and pemphigus foliaceous (PF), taking into account the unique challenges posed by the Indian healthcare setting. The guidelines focus on the comprehensive management of PV and PF, addressing diagnosis, treatment, monitoring, and follow-up. It is intended for dermatologists working in both outpatient and inpatient settings across India. The first draft of the guidelines was prepared by the writing group and then reviewed by 19 national experts in pemphigus management, including inputs from allied specialties. Areas with limited evidence or anticipated variation in recommendations were subjected to rounds of voting, with responses categorized as “strongly agree,” “agree,” “neutral,” “disagree,” or “strongly disagree.” Suggestions were incorporated, and statements were revised until a mean agreement score of 4 or higher was reached across 16 key areas after four voting rounds. These guidelines offer a structured approach to managing pemphigus in India, addressing the need for region-specific recommendations that account for unique challenges such as resource constraints and specific comorbidities in Indian patients. They serve as a valuable resource for dermatologists treating pemphigus in a range of clinical settings.
Biologics and Small Molecules for Inflammatory Nail Disorders: A Narrative Review
Authors: Forman Carrie A. , Lipner Shari R. 
Published: December 2024

Abstract

Background:
Inflammatory dermatological conditions, including psoriasis, lichen planus, eczema, and alopecia areata, are frequently accompanied by nail findings and can have a significant impact on quality of life. Biologic and small-molecule medications have been approved over the past several decades in treating patients with these inflammatory nail disorders. They may be used in conjunction with longstanding mainstays of treatment (topical and intralesional corticosteroids, topical vitamin D3 analogs).

Objectives:
Our objectives were to review biologic and small-molecule treatment efficacies for nail psoriasis and alopecia areata-associated nail dystrophy, including Janus kinase inhibitors, apremilast, tumor necrosis factor (TNF) inhibitors, interleukin (IL)-17 inhibitors, and IL-23 inhibitors.

Materials and Methods:
A comprehensive PubMed literature review of clinical research studies, narrative reviews, systematic reviews, and meta-analyses was performed.

Conclusion:
Many biologics and small molecules are effective in treating nail psoriasis and alopecia areata, with each requiring precautions for adverse events. Clinical trials for use of biologics and small molecules for nail lichen planus and atopic dermatitis have not been published to date.
Laser Treatment in Nail Disorders: A Comprehensive Review
Authors: Chandrashekar Byalakere Shivanna , Madura Chandu , Shenoy Chaitra , Chandar Abhijna , Roopa Mysore Seshadri , Narayana Nakka Lakshmi 
Published: December 2024

Abstract

Background:
Laser therapy has emerged as an innovative approach for managing various nail conditions, offering precise targeting, minimal invasiveness, and favorable safety profiles. This review analyzes the literature on laser therapy for nail indications, encompassing onychomycosis, nail psoriasis, nail warts, ingrown toenails, onychodystrophy, nail pigmentation disorders, and nail tumors.

Methods:
PubMed and Google Scholar databases were searched to identify articles on laser therapy using specific key terms related to nail conditions (e.g., onychomycosis, nail psoriasis). Relevant articles were shortlisted based on laser treatment in nail disorders, its mechanisms of action, research outcomes, and clinical applications.

Results:
Nd:YAG or CO2 lasers showed efficacy in onychomycosis by targeting fungal cells. Studies suggest that laser treatments offer comparable results to traditional therapies, often enhancing outcomes when combined with topical agents such as calcipotriol/betamethasone in nail psoriasis. For nail warts, ingrown toenails, onychodystrophy, and nail pigmentation disorders, lasers provide alternative or adjunctive therapies, achieving positive outcomes lesion clearance and symptom improvement. Conclusion: This review underscores the transformative potential of laser therapy in nail disorder management, providing clinicians with innovative treatment alternatives. Nevertheless, further studies are needed to refine protocols, evaluate long-term outcomes and explore its application in specific conditions such as nail tumors.
A rare anatomical perplexity of submandibular cavernous hemangioma with phleboliths
Authors: Patil Karthikeya , Sanjay C. J. , Suresh Namrata , Christopher Varusha Sharon 
Published: December 2024

Abstract
This case report presents a unique instance of a submandibular cavernous hemangioma, a rare vascular tumor, accompanied by phleboliths- –calcified masses within blood vessels. The presence of phleboliths, considered an unusual anatomical variation, accentuates the complexity of the condition. A detailed clinical examination, imaging studies, and histopathological analysis were pivotal in confirming the diagnosis. Understanding the interplay of hemangioma and phleboliths in the submandibular region is crucial for accurate diagnosis and appropriate treatment planning, shedding light on this intricate vascular anomaly, and guiding tailored therapeutic interventions for optimal patient outcomes.

The following core competencies are addressed in this article: Medical knowledge, Patient care.