bluuebunny/crossref_metadata_2025_split huggingface dataset:
Characterizing History of Health Sciences Organizations at Academic Health Sciences Centers
Authors: Alpi Kristine M , Johnson Jordan R , Langford Meg E 
Published: February 2023

Abstract
Questions of how to sustain interest in the history of medicine and broader health sciences (HOM/HS) in a changing institutional environment, and how to collaborate with stakeholders to offer activities to do so, are on the radar for many academic health sciences centers and their libraries. This essay is an initial exploratory study of non-curricular HOM/HS efforts at United States medical schools ranked in the top thirty in primary care or research. In 2019, we collected public information pertinent to any presence of an on-campus HOM/HS community and the group’s structure, including funding, activities, and the library’s involvement with the group. Seventeen of forty-five institutions in the sample presented information about an institutional HOM/HS group. All posted a mission statement. Their funding varied in nature; some collected fees from members, while others relied on university support. Half were student-led. Most groups hosted regular lecture series, with fifteen groups hosting at least one annually. Six groups sponsored publications or awards. These findings indicate that several institutions with active programs offer potential models and lessons for sustaining HOM/HS communities. Beyond providing a physical or digital space in which HOM/HS groups connect, libraries play an active role in fostering some of these communities.
Developing a new biologic toxin binder for reducing AFB1 toxicity in laying hens
Authors: Nasiri Poroj Shohreh , Fazeli Mohammad Reza , Larypoor Mohaddeseh , Shariatmadari Farid 
Published: February 2023

Abstract
Aflatoxin (AFs)-contaminated diet in feeding domestic animals is one of the biggest health concerns for humans. Therefore, various methods have been developed to detoxify AFs. In the present study, adding Saccharomyces cerevisiae probiotic yeast and titanium dioxide nanoparticles (TiO2-NPs) reduces the toxicity of AF B1 (AFB1) in laying hens was studied. After preparing the laying hens, they were fed with a diet containing AFB1 for 14 days and supplemented with S. cerevisiae and TiO2-NPs. Weight changes, serum levels of albumin, globulin, total protein, aspartate transaminase (AST), and alanine transaminase (ALT) were measured over 14 days. Also, on day 14, after killing the animals, their liver tissue was extracted, and the AFB1 content was measured by high-performance liquid chromatography (HPLC) and studied histopathologically using hematoxylin-eosin staining. The results showed that adding S. cerevisiae strain and TiO2-NPs to the diet of chicks with aflatoxicosis prevented weight loss, detoxified the liver, increased total protein, decreased albumin, and globulin content. Histopathological images showed damage to the liver tissue of laying hens fed diets containing AFB1. However, S. cerevisiae and TiO2-NPs were able to prevent liver damage. In general, it was concluded that adding S. cerevisiae along with TiO2-NPs could be a good optiofor reducing AFB1 toxicity in laying hens.
Cryptococcosis in domestic and wild animals: A review
Authors: Bermann Carolina dos Santos , Braga Caroline Quintana , Ianiski Lara Baccarin , Botton Sônia de Avila , Pereira Daniela Isabel Brayer 
Published: February 2023

AbstractCryptococcosis is a fungal disease of public health relevance that affects numerous animal species and humans, causing respiratory and neurological impairment. Hence, we conducted a systematic review that included publications from 1975 to 2021 and covered 132 articles that addressed reports of cryptococcosis in domestic and wild animals, its main clinical manifestations, pathological findings, etiology, diagnosis, and therapeutic protocols. We found that the highest number of reports of cryptococcosis is in domestic species, especially cats. Among the wild and/or exotic animals, koalas and ferrets are the most affected, being important carriers of Cryptococcus spp. Pulmonary and neurological involvement is predominant in all species, although nonspecific clinical manifestations have been reported in various species, making clinical suspicion and diagnosis difficult. The countries with the most reports are Australia, the United States, Brazil, and Canada, with C. gattii VGI and VGII standing out. The therapies were based on azoles, amphotericin B, and 5-flucytosine, although there is no standard treatment protocol. Although, several diagnostic methods have been described, in a significant number of reports the diagnosis was made after a necropsy. Professionals are warned about diverse and nonspecific clinical manifestations in different animal species, which underlines the importance of cryptococcosis in the differential diagnosis in clinical practice. Furthermore, it is necessary to encourage the use of laboratory and molecular tools to improve the diagnosis of cryptococcosis. We also emphasize the urgent need for standardized therapeutic protocols to guide veterinary clinicians.
Occurrence and molecular characterization ofEnterocytozoon bieneusiin wild and domestic animal species in Portugal
Authors: Figueiredo Ana M , Dashti Alejandro , Santín Mónica , Köster Pamela C , Torres Rita T , Fonseca Carlos , Mysterud Atle , Carvalho João , Sarmento Pedro , Neves Nuno , Hipólito Dário , Palmeira Josman D , Teixeira Daniela , Lima Cátia , Calero-Bernal Rafael , Carmena David 
Published: February 2023

AbstractThe phylum Microsporidia encompasses a diverse group of obligate, intracellular, and spore-forming organisms able to infect a wide range of animal hosts. Among them, Enterocytozoon bieneusi is the most frequently reported species in humans and animals. Little is known about the presence and epidemiology of E. bieneusi in wildlife. We investigated E. bieneusi occurrence and genetic diversity in wild and domestic mammals, through molecular-detection methods, from different regions across Portugal. A total of 756 samples were collected from 288, 242, and 226 wild carnivores, wild ungulates, and domestic animals, respectively. Overall, eight specimens were E. bieneusi-positive (1.1%, 8/756) obtained from five wild (Iberian lynx, Iberian wolf, red fox, stone marten, and wild boar) and one domestic (sheep) host. Nucleotide sequence analysis identified four genotypes of E. bieneusi, Type IV, Wildboar3, BEB6, and PtEbIX. Three of those genotypes belong to Groups 1 (Type IV and Wildboar3) and 2 (BEB6), which are known to contain genotypes capable of infecting a variety of hosts, including humans, highlighting their public health importance. PtEbIX belongs to the dog-specific Group 11. This study represents the first, largest, and most comprehensive molecular-based epidemiology survey carried out in Portugal in wild and domestic animals to date and the first worldwide identification of E. bieneusi in wolf species. Our study showed that wild carnivores and ungulates may act as reservoirs of zoonotic genotypes of E. bieneusi, establishing their role in maintaining the sylvatic cycle of this parasite while representing a potential source of infection for humans and domestic animals.
Gaussian processes for glitch-robust gravitational-wave astronomy
Authors: Ashton Gregory 
Published: February 2023

ABSTRACTInterferometric gravitational-wave observatories have opened a new era in astronomy. The rich data produced by an international network enable detailed analysis of the curved space-time around black holes. With nearly 100 signals observed so far and thousands expected in the next decade, their population properties enable insights into stellar evolution and the expansion of our Universe. However, the detectors are afflicted by transient noise artefacts known as ‘glitches’ which contaminate the signals and bias inferences. Of the 90 signals detected to date, 18 were contaminated by glitches. This feasibility study explores a new approach to transient gravitational-wave data analysis using Gaussian processes, which model the underlying physics of the glitch-generating mechanism rather than the explicit realization of the glitch itself. We demonstrate that if the Gaussian process kernel function can adequately model the glitch morphology, we can recover the parameters of simulated signals. Moreover, we find that the Gaussian processes kernels used in this work are well suited to modelling long-duration glitches which are most challenging for existing glitch-mitigation approaches. Finally, we show how the time-domain nature of our approach enables a new class of time-domain tests of General Relativity, performing a re-analysis of the inspiral-merger-ringdown test on the first observed binary black hole merger. Our investigation demonstrates the feasibility of the Gaussian processes as an alternative to the traditional framework but does not yet establish them as a replacement. Therefore, we conclude with an outlook on the steps needed to realize the full potential of the Gaussian process approach.
CMZoom III: Spectral line data release
Authors: Callanan Daniel , Longmore Steven N , Battersby Cara , Hatchfield H Perry , Walker Daniel L , Henshaw Jonathan , Keto Eric , Barnes Ashley , Ginsburg Adam , Kauffmann Jens , Kruijssen J M Diederik , Lu Xing , Mills Elisabeth A C , Pillai Thushara , Zhang Qizhou , Bally John , Butterfield Natalie , Contreras Yanett A , Ho Luis C , Immer Katharina , Johnston Katharine G , Ott Juergen , Patel Nimesh , Tolls Volker 
Published: February 2023

ABSTRACT
We present an overview and data release of the spectral line component of the SMA Large Program, CMZoom. CMZoom observed 12CO (2–1), 13CO (2–1), and C18O (2–1), three transitions of H2CO, several transitions of CH3OH, two transitions of OCS, and single transitions of SiO and SO within gas above a column density of N(H2) ≥ 1023 cm−2 in the Central Molecular Zone (CMZ; inner few hundred pc of the Galaxy). We extract spectra from all compact 1.3 mm CMZoom continuum sources and fit line profiles to the spectra. We use the fit results from the H2CO 3(0, 3)–2(0, 2) transition to determine the source kinematic properties. We find ∼90 per cent of the total mass of CMZoom sources have reliable kinematics. Only four compact continuum sources are formally self-gravitating. The remainder are consistent with being in hydrostatic equilibrium assuming that they are confined by the high external pressure in the CMZ. We find only two convincing proto-stellar outflows, ruling out a previously undetected population of very massive, actively accreting YSOs with strong outflows. Finally, despite having sufficient sensitivity and resolution to detect high-velocity compact clouds (HVCCs), which have been claimed as evidence for intermediate mass black holes interacting with molecular gas clouds, we find no such objects across the large survey area.
A low-frequency sub-arcsecond view of powerful radio galaxies in rich-cluster environments: 3C 34 and 3C 320
Authors: Mahatma V H , Basu A , Hardcastle M J , Morabito L K , van Weeren R J 
Published: February 2023

ABSTRACT
Models of radio galaxy physics have been primarily based on high frequency (≥1 GHz) observations of their jets, hotspots, and lobes. Without highly resolved low-frequency observations, which provide information on older plasma, our understanding of the dynamics of radio galaxies and their interaction with their environment is limited. Here, we present the first sub-arcsecond (0.3 arcsec) resolution images at 144 MHz of two powerful radio galaxies situated in rich cluster environments, namely 3C 34 and 3C 320, using the International Low Frequency Array Telescope. We detect for the first time at low frequencies a plethora of structures in these objects, including strikingly large filaments across the base of the lobes in both sources, which are spatially associated with dense regions in the ambient medium. For 3C 34, we report a spectral flattening in the region of the central filament, suggesting that the origin of the filaments is related to the presence of large-scale ordered magnetic fields. We also report periodic total intensity and spectral index banding of diffuse emission in the eastern lobe, seen for the first time in radio galaxy lobes. The hotspot complexes are resolved into multiple fragments of varying structure and spectral index; we discuss the implications for particle acceleration and jet termination models. We find at most smooth gradients in the spectral behaviour of the hotspot structure suggesting that particle acceleration, if present, may be occurring throughout the complex, in contrast to simple models, but different jet termination models may apply to both sources.
Observational connection of non-thermal X-ray emission from pulsars with their timing properties and thermal emission
Authors: Chang Hsiang-Kuang , Hsiang Jr-Yue , Chu Che-Yen , Chung Yun-Hsin , Su Tze-Hsiang , Lin Tzu-Hsuan , Huang Chien-You 
Published: February 2023

ABSTRACTThe origin and radiation mechanisms of high-energy emissions from pulsars have remained mysterious since their discovery. Here we report, based on a sample of 68 pulsars, observational connection of non-thermal X-ray emissions from pulsars with their timing properties and thermal emissions, which may provide some constraints on theoretical modeling. Besides strong correlations with the spin-down power $\dot{E}$ and the magnetic field strength at the light cylinder Blc, the non-thermal X-ray luminosity in 0.5–8 keV, Lp, represented by the power-law component in the spectral model, is found to be strongly correlated with the highest possible electric field strength in the polar gap, Epc, of the pulsar. The spectral power index Γp of that power-law component is also found, for the first time in the literature, to strongly correlate with $\dot{E}$, Blc, and Epc, thanks to the large sample. In addition, we found that Lp can be well described by Lp ∝ T5.96 ± 0.64R2.24 ± 0.18, where T and R are the surface temperature and the emitting-region radius of the surface thermal emission, represented by the blackbody component in the spectral model. Γp, on the other hand, can be well described only when timing variables are included and the relation is $\Gamma _{\rm p}= \log (T^{-5.8\pm 1.93}R^{-2.29\pm 0.85}P^{-1.19\pm 0.88}\dot{P}^{0.94\pm 0.44})$ plus a constant. These relations strongly suggest the existence of connections between surface thermal emission and electron–positron pair production in pulsar magnetospheres.
On the origin of UV-dim stars: a population of rapidly rotating shell stars?
Authors: Martocchia S , Bastian N , Saracino S , Kamann S 
Published: February 2023

ABSTRACT
The importance of stellar rotation in setting the observed properties of young star clusters has become clearer over the past decade, with rotation being identified as the main cause of the observed extended main sequence turn-off (eMSTO) phenomenon and split main sequences. Additionally, young star clusters are observed to host large fractions of rapidly rotating Be stars, many of which are seen nearly equator-on through decretion discs that cause self-extinction (the so called ‘shell stars’). Recently, a new phenomenon has been reported in the ∼1.5 Gyr star cluster NGC 1783, where a fraction of the main-equence turn-off stars appears abnormally dim in the UV. We investigate the origin of these ‘UV-dim’ stars by comparing the UV colour–magnitude diagrams of NGC 1850 (∼100 Myr), NGC 1783 (∼1.5 Gyr), NGC 1978 (∼2 Gyr), and NGC 2121 (∼2.5 Gyr), massive star clusters in the Large Magellanic Cloud. While the younger clusters show a non-negligible fraction of UV-dim stars, we find a significant drop of such stars in the two older clusters. This is remarkable as clusters older than ∼2 Gyr do not have an eMSTO, thus a large populations of rapidly rotating stars, because their main-sequence turn-off stars are low enough in mass to slow down due to magnetic braking. We conclude that the UV-dim stars are likely rapidly rotating stars with decretion discs seen nearly equator-on (i.e. are shell stars) and discuss future observations that can confirm or refute our hypothesis.
Absence of extended atmospheres in low-mass star radius-gap planets
Authors: Krishnamurthy Vigneshwaran , Hirano Teruyuki , Gaidos Eric , Sato Bunei , Kopparapu Ravi , Barclay Thomas , Garcia-Sage Katherine , Harakawa Hiroki , Hodapp Klaus , Jacobson Shane , Konishi Mihoko , Kotani Takayuki , Kudo Tomoyuki , Kurokawa Takashi , Kuzuhara Masayuki , Lopez Eric , Nishikawa Jun , Omiya Masashi , Schlieder Joshua E , Serizawa Takuma , Tamura Motohide , Ueda Akitoshi , Vievard Sebastien 
Published: February 2023

ABSTRACT
Kepler showed a paucity of planets with radii of 1.5–2 R⊕ around solar mass stars but this radius-gap has not been well studied for low-mass star planets. Energy-driven escape models like photoevaporation and core-powered mass-loss predict opposing transition regimes between rocky and non-rocky planets when compared to models depicting planets forming in gas-poor environments. Here, we present transit observations of three super-Earth sized planets in the radius-gap around low-mass stars using high-dispersion InfraRed Doppler spectrograph on the Subaru 8.2 m telescope. The planets GJ 9827 b and d orbit around a K6V star and TOI-1235 b orbits a M0.5 star. We limit any planet-related absorption in the 1083.3 nm lines of triplet He i by placing an upper-limit on the equivalent width of 14.71, 18.39, and 1.44 mÅ for GJ 9827 b (99 per cent confidence), GJ 9827 d (99 per cent confidence), and TOI-1235 b (95 per cent confidence), respectively. Using a Parker wind model, we cap the mass-loss at &gt;0.25 M⊕ Gyr−1 and &gt;0.2 M⊕ Gyr−1 for GJ 9827 b and d, respectively (99 per cent confidence), and &gt;0.05 M⊕ Gyr−1 for TOI-1235 b (95 per cent confidence) for a representative wind temperature of 5000 K. Our observed results for the three planets are more consistent with the predictions from photoevaporation and/or core-powered mass-loss models than the gas-poor formation models. However, more planets in the radius-gap regime around the low-mass stars are needed to robustly predict the atmospheric evolution in planets around low-mass stars.
Dynamically constraining the length of the Milky way bar
Authors: Lucey Madeline , Pearson Sarah , Hunt Jason A S , Hawkins Keith , Ness Melissa , Petersen Michael S , Price-Whelan Adrian M , Weinberg Martin D 
Published: February 2023

ABSTRACT
We present a novel method for constraining the length of the Galactic bar using 6D phase-space information to directly integrate orbits. We define a pseudo-length for the Galactic bar, named RFreq, based on the maximal extent of trapped bar orbits. We find the RFreq measured from orbits is consistent with the RFreq of the assumed potential only when the length of the bar and pattern speed of said potential is similar to the model from which the initial phase-space coordinates of the orbits are derived. Therefore, one can measure the model’s or the Milky Way’s bar length from 6D phase-space coordinates by determining which assumed potential leads to a self-consistent measured RFreq. When we apply this method to ≈210 000 stars in APOGEE DR17 and Gaia eDR3 data, we find a consistent result only for potential models with a dynamical bar length of ≈3.5 kpc. We find the Milky Way’s trapped bar orbits extend out to only ≈3.5 kpc, but there is also an overdensity of stars at the end of the bar out to 4.8 kpc which could be related to an attached spiral arm. We also find that the measured orbital structure of the bar is strongly dependent on the properties of the assumed potential.
Understanding and predicting cadence effects in the characterization of exoplanet transits
Authors: Hernandez Camero Julio , Ho Cynthia S K , Van Eylen Vincent 
Published: February 2023

ABSTRACT
We investigate the effect of observing cadence on the precision of radius ratio values obtained from transit light curves by performing uniform Markov chain Monte Carlo fits of 46 exoplanets observed by the Transiting Exoplanet Survey Satellite (TESS) in multiple cadences. We find median improvements of almost 50 per cent when comparing fits to 20 and 120 s cadence light curves to 1800 s cadence light curves, and of 37 per cent when comparing 600 s cadence to 1800 s cadence. Such improvements in radius precision are important, for example, to precisely constrain the properties of the radius valley or to characterize exoplanet atmospheres. We also implement a numerical information analysis to predict the precision of parameter estimates for different observing cadences. We tested this analysis on our sample and found that it reliably predicts the effect of shortening observing cadence with errors in the predicted percentage precision of $\lesssim0.5~{{\ \rm per\ cent}}$ for most cases. We apply this method to 157 TESS objects of interest that have only been observed with 1800 s cadence to predict the precision improvement that could be obtained by reobservations with shorter cadences and provide the full table of expected improvements. We report the 10 planet candidates that would benefit the most from reobservations at short cadence. Our implementation of the information analysis for the prediction of the precision of exoplanet parameters, Prediction of Exoplanet Precisions using Information in Transit Analysis, is made publicly available.
The bright supernova 1996cr in the circinus galaxy imaged with VLBI: shell structure with complex evolution
Authors: Bietenholz Michael F , Bartel Norbert , Bauer Franz E , Dwarkadas Vikram V , Mtshweni Leon , Orquera-Rojas Carlos , Ellingsen Simon , Horiuchi Shinji , Tzioumis Anastasios 
Published: February 2023

ABSTRACT
We present broad-band radio flux-density measurements supernova (SN) 1996cr, made with MeerKAT, ATCA, and ALMA, and images made from very long baseline interferometry (VLBI) observations with the Australian Long Baseline Array. The spectral energy distribution of SN 1996cr in 2020, at age t ∼8700 d, is a power-law, with flux density, S ∝ ν−0.588 ± 0.011 between 1 and 34 GHz, but may steepen at &gt;35 GHz. The spectrum has flattened since t = 5370 d (2010). Also since t = 5370 d, the flux density has declined rapidly, with $S_{\rm 9 \, GHz} \propto t^{-2.9}$. The VLBI image at t = 8859 d shows an approximately circular structure with a central minimum reminiscent of an optically-thin spherical shell of emission. For a distance of 3.7 Mpc, the average outer radius of the radio emission at t = 8859 d was (5.1 ± 0.3) × 1017 cm, and SN 1996cr has been expanding with a velocity of 4650 ± 1060 km s−1 between t = 4307 and 8859 d. It must have undergone considerable deceleration before t = 4307 d. Deviations from a circular shell structure in the image suggest a range of velocities up to ∼7000 km s−1, and hint at the presence of a ring- or equatorial-belt-like structure rather than a complete spherical shell.