bluuebunny/crossref_metadata_2025_split huggingface dataset:
Dynamics and thermal sensitivity of rRNA maturation paths in plants
Authors: Shanmugam Thiruvenkadam , Streit Deniz , Schroll Frank , Kovacevic Jelena , Schleiff Enrico 
Published: September 2021

Abstract
Ribosome biogenesis is a constitutive fundamental process for cellular function. Its rate of production depends on the rate of maturation of precursor rRNA (pre-rRNA). The rRNA maturation paths are characterized by four dominant rate-limiting intermediates with cell type variation of the processivity rate. We have identified that high temperature stress in plants, while halting the existing pre-rRNA maturation schemes, also transiently triggers an atypical pathway for 35S pre-rRNA processing. This pathway leads to production of an aberrant pre-rRNA, reminiscent of yeast 24S, encompassing 18S and 5.8S rRNAs that do not normally co-occur together at subunit levels; this response is elicited specifically by high and not low temperatures. We show this response to be conserved in two other model crop plant species (rice and tomato). This pathway persists even after returning to normal growth conditions for 1 h, and is reset between 1 h and 6 h after stress treatment, probably due to resumption of normal 35S pre-rRNA synthesis and processing. The heat-induced ITS2 cleavage-derived precursors and stalled P-A2-like precursors were heterogeneous in nature, with a fraction containing polymeric (A) tails. Furthermore, high temperature treatment and subsequent fractionation resulted in polysome and pre-rRNA depletion.
Portal Venous Thrombosis in a Special Operations Paratrooper: A Case Report
Authors: Bridwell Rachel E , Clerkin Sean , Walker Nathaniel R , Long Brit , Goss Sarah 
Published: September 2021

ABSTRACT
Portal vein thrombosis is the thrombotic occlusion of the extrahepatic portal system, which can propagate towards the vena caval system. Although rare, it occurs primarily in those with cirrhosis, intra-abdominal infections, malignancy, or hypercoagulable disorders. This report describes the first reported case of a soldier within special operations without identifiable risk factors who was found to have a completely occlusive portal vein thrombosis after approximately 10 days of insidious abdominal pain. This case emphasizes the importance of considering this rare but dangerous pathology among this highly screened and capable special operations population.
A systematic review on distribution and antifungal resistance pattern ofCandidaspecies in the Indian population
Authors: Verma Rashi , Pradhan Dibyabhaba , Hasan Ziaul , Singh Harpreet , Jain Arun Kumar , Khan Luqman Ahmad 
Published: September 2021

AbstractThe emergence of antifungal drug resistance in Candida species has led to increased morbidity and mortality in immunocompromised patients. Understanding species distribution and antifungal drug resistance patterns is an essential step for novel drug development. A systematic review was performed addressing this challenge in India with keywords inclusive of ‘Candida’, ‘Antifungal Drug Resistance’, ‘Candidemia’, ‘Candidiasis’ and ‘India’. A total of 106 studies (January 1978–March 2020) from 20 Indian states were included. Of over 11,429 isolates, Candida albicans was the major species accounting for 37.95% of total isolates followed by C. tropicalis (29.40%), C. glabrata (11.68%) and C. parapsilosis (8.36%). Rates of antifungal resistance were highest in non-albicans Candida (NAC) species - C. haemuloni (47.16%), C. krusei (28.99%), C. lipolytica (28.89%) and C. glabrata (20.69%). Approximately 10.34% isolates of C. albicans were observed to be drug resistant. Candida species were frequently resistant to certain azoles (ketoconazole-22.2%, miconazole–22.1% and fluconazole–21.8%). In conclusion, the present systematic review illustrates the overall distribution and antifungal resistance pattern of Candida species among the Indian population that could be helpful in the future for the formation of treatment recommendations for the region but also elsewhere.Lay SummaryA total of 106 studies were reviewed to define the prevalence, distribution and antifungal resistance pattern of Candida species in India. The presented data could become the point of reference for all reported findings on Candida species in India.
Characterizing mass, momentum, energy, and metal outflow rates of multiphase galactic winds in the FIRE-2 cosmological simulations
Authors: Pandya Viraj , Fielding Drummond B , Anglés-Alcázar Daniel , Somerville Rachel S , Bryan Greg L , Hayward Christopher C , Stern Jonathan , Kim Chang-Goo , Quataert Eliot , Forbes John C , Faucher-Giguère Claude-André , Feldmann Robert , Hafen Zachary , Hopkins Philip F , Kereš Dušan , Murray Norman , Wetzel Andrew 
Published: September 2021

ABSTRACT
We characterize mass, momentum, energy, and metal outflow rates of multiphase galactic winds in a suite of FIRE-2 cosmological ‘zoom-in’ simulations from the Feedback in Realistic Environments (FIRE) project. We analyse simulations of low-mass dwarfs, intermediate-mass dwarfs, Milky Way-mass haloes, and high-redshift massive haloes. Consistent with previous work, we find that dwarfs eject about 100 times more gas from their interstellar medium (ISM) than they form in stars, while this mass ‘loading factor’ drops below one in massive galaxies. Most of the mass is carried by the hot phase (&gt;105 K) in massive haloes and the warm phase (103−105 K) in dwarfs; cold outflows (&lt;103 K) are negligible except in high-redshift dwarfs. Energy, momentum, and metal loading factors from the ISM are of order unity in dwarfs and significantly lower in more massive haloes. Hot outflows have 2−5 × higher specific energy than needed to escape from the gravitational potential of dwarf haloes; indeed, in dwarfs, the mass, momentum, and metal outflow rates increase with radius whereas energy is roughly conserved, indicating swept up halo gas. Burst-averaged mass loading factors tend to be larger during more powerful star formation episodes and when the inner halo is not virialized, but we see effectively no trend with the dense ISM gas fraction. We discuss how our results can guide future controlled numerical experiments that aim to elucidate the key parameters governing galactic winds and the resulting associated preventative feedback.
Stellar migration and chemical enrichment in the milky way disc: a hybrid model
Authors: Johnson James W , Weinberg David H , Vincenzo Fiorenzo , Bird Jonathan C , Loebman Sarah R , Brooks Alyson M , Quinn Thomas R , Christensen Charlotte R , Griffith Emily J 
Published: September 2021

ABSTRACT
We develop a hybrid model of galactic chemical evolution that combines a multiring computation of chemical enrichment with a prescription for stellar migration and the vertical distribution of stellar populations informed by a cosmological hydrodynamic disc galaxy simulation. Our fiducial model adopts empirically motivated forms of the star formation law and star formation history, with a gradient in outflow mass loading tuned to reproduce the observed metallicity gradient. With this approach, the model reproduces many of the striking qualitative features of the Milky Way disc’s abundance structure: (i) the dependence of the [O/Fe]–[Fe/H] distribution on radius Rgal and mid-plane distance |z|; (ii) the changing shapes of the [O/H] and [Fe/H] distributions with Rgal and |z|; (iii) a broad distribution of [O/Fe] at sub-solar metallicity and changes in the [O/Fe] distribution with Rgal, |z|, and [Fe/H]; (iv) a tight correlation between [O/Fe] and stellar age for [O/Fe] &gt; 0.1; (v) a population of young and intermediate-age α-enhanced stars caused by migration-induced variability in the Type Ia supernova rate; (vi) non-monotonic age–[O/H] and age–[Fe/H] relations, with large scatter and a median age of ∼4 Gyr near solar metallicity. Observationally motivated models with an enhanced star formation rate ∼2 Gyr ago improve agreement with the observed age–[Fe/H] and age–[O/H] relations, but worsen agreement with the observed age–[O/Fe] relation. None of our models predict an [O/Fe] distribution with the distinct bimodality seen in the observations, suggesting that more dramatic evolutionary pathways are required. All code and tables used for our models are publicly available through the Versatile Integrator for Chemical Evolution (VICE; https://pypi.org/project/vice).
1/f noise analysis for FAST H i intensity mapping drift-scan experiment
Authors: Hu Wenkai , Li Yichao , Wang Yougang , Wu Fengquan , Zhang Bo , Zhu Ming , Zuo Shifan , Lagache Guilaine , Ma Yin-Zhe , Santos Mario G , Chen Xuelei 
Published: September 2021

ABSTRACT
We investigate the 1/f noise of the Five-hundred-meter Aperture Spherical Telescope (FAST) receiver system using drift-scan data from an intensity mapping pilot survey. All the 19 beams have 1/f fluctuations with similar structures. Both the temporal and the 2D power spectrum densities are estimated. The correlations directly seen in the time series data at low frequency f are associated with the sky signal, perhaps due to a coupling between the foreground and the system response. We use singular value decomposition (SVD) to subtract the foreground. By removing the strongest components, the measured 1/f noise power can be reduced significantly. With 20 modes subtraction, the knee frequency of the 1/f noise in a 10-MHz band is reduced to $1.8 \times 10^{-3}\, {\rm Hz}$, well below the thermal noise over 500-s time-scale. The 2D power spectra show that the 1/f-type variations are restricted to a small region in the time-frequency space and the correlations in frequency can be suppressed with SVD modes subtraction. The residual 1/f noise after the SVD mode subtraction is uncorrelated in frequency, and a simple noise diode frequency-independent calibration of the receiver gain at 8-s interval does not affect the results. The 1/f noise can be important for H i intensity mapping, we estimate that the 1/f noise has a knee frequency (fk) ∼ 6 × 10−4 Hz, and time and frequency correlation spectral indices (α) ∼ 0.65, (β) ∼ 0.8 after the SVD subtraction of 30 modes. This can bias the H i power spectrum measurement by 10 per cent.
Gravitational-wave cosmology with extreme mass-ratio inspirals
Authors: Laghi Danny , Tamanini Nicola , Del Pozzo Walter , Sesana Alberto , Gair Jonathan , Babak Stanislav , Izquierdo-Villalba David 
Published: September 2021

ABSTRACTThe Laser Interferometer Space Antenna (LISA) will open the mHz frequency window of the gravitational-wave (GW) landscape. Among all the new GW sources expected to emit in this frequency band, extreme mass-ratio inspirals (EMRIs) constitute a unique laboratory for astrophysics and fundamental physics. Here, we show that EMRIs can also be used to extract relevant cosmological information, complementary to both electromagnetic (EM) and other GW observations. By using the loudest EMRIs (S/N &gt; 100) detected by LISA as dark standard sirens, statistically matching their sky localization region with mock galaxy catalogues, we find that constraints on H0 can reach ∼1.1 per cent (∼3.6 per cent) accuracy, at the 90 per cent credible level, in our best(worst)- case scenario. By considering a dynamical dark energy (DE) cosmological model, with ΛCDM parameters fixed by other observations, we further show that in our best(worst)- case scenario ∼5.9 per cent (∼12.3 per cent) relative uncertainties at the 90 per cent credible level can be obtained on w0, the DE equation of state parameter. Besides being relevant in their own right, EMRI measurements will be affected by different systematics compared to both EM and ground-based GW observations. Cross-validation with complementary cosmological measurements will therefore be of paramount importance, especially if convincing evidence of physics beyond ΛCDM emerges from future observations.
CLMM: a LSST-DESC cluster weak lensing mass modeling library for cosmology
Authors: Aguena M , Avestruz C , Combet C , Fu S , Herbonnet R , Malz A I , Penna-Lima M , Ricci M , Vitenti S D P , Baumont L , Fan H , Fong M , Ho M , Kirby M , Payerne C , Boutigny D , Lee B , Liu B , McClintock T , Miyatake H , Sifón C , von der Linden A , Wu H , Yoon M ,   The LSST Dark Energy Science Collaboration, Chisari Elisa , Clowe Douglas , Dell’Antonio Ian 
Published: September 2021

ABSTRACT
We present the v1.0 release of CLMM, an open source python library for the estimation of the weak lensing masses of clusters of galaxies. CLMM is designed as a stand-alone toolkit of building blocks to enable end-to-end analysis pipeline validation for upcoming cluster cosmology analyses such as the ones that will be performed by the Vera C. Rubin Legacy Survey of Space and Time-Dark Energy Science Collaboration (LSST-DESC). Its purpose is to serve as a flexible, easy-to-install, and easy-to-use interface for both weak lensing simulators and observers and can be applied to real and mock data to study the systematics affecting weak lensing mass reconstruction. At the core of CLMM are routines to model the weak lensing shear signal given the underlying mass distribution of galaxy clusters and a set of data operations to prepare the corresponding data vectors. The theoretical predictions rely on existing software, used as backends in the code, that have been thoroughly tested and cross-checked. Combined theoretical predictions and data can be used to constrain the mass distribution of galaxy clusters as demonstrated in a suite of example Jupyter Notebooks shipped with the software and also available in the extensive online documentation.
Spurious heating of stellar motions in simulated galactic discs by dark matter halo particles
Authors: Ludlow Aaron D , Fall S Michael , Schaye Joop , Obreschkow Danail 
Published: September 2021

ABSTRACT
We use idealized N-body simulations of equilibrium stellar discs embedded within course-grained dark matter (DM) haloes to study the effects of spurious collisional heating on disc structure and kinematics. Collisional heating artificially increases the vertical and radial velocity dispersions of disc stars, as well as the thickness and size of discs; the effects are felt at all galacto-centric radii. The integrated effects of collisional heating are determined by the mass of DM halo particles (or equivalently, by the number of particles at fixed halo mass), their local density and characteristic velocity dispersion, but are largely insensitive to the stellar particle mass. The effects can therefore be reduced by increasing the mass resolution of DM in cosmological simulations, with limited benefits from increasing the baryonic (or stellar) mass resolution. We provide a simple empirical model that accurately captures the effects of spurious collisional heating on the structure and kinematics of simulated discs, and use it to assess the importance of disc heating for simulations of galaxy formation. We find that the majority of state-of-the-art zoom simulations, and a few of the highest-resolution, smallest-volume cosmological runs, are in principle able to resolve thin stellar discs in Milky Way-mass haloes, but most large-volume cosmological simulations cannot. For example, DM haloes resolved with fewer than ≈106 particles will collisionally heat stars near the stellar half-mass radius such that their vertical velocity dispersion increases by ≳ 10 per cent of the halo’s virial velocity in approximately one Hubble time.
A radiation transfer model for the Milky Way. II The global properties and large scale structure
Authors: Natale Giovanni , Popescu Cristina C , Rushton Mark , Yang Ruizhi , Thirlwall Jordan J , Pricopi Dumitru 
Published: September 2021

Abstract
We obtained an axi-symmetric model for the large-scale distribution of stars and dust in the Milky Way (MW) using a radiative transfer code that can account for the existing near-infrared (NIR)/mid-infrared/submm all-sky emission maps of our Galaxy. We find that the MW has a star-formation rate of SFR = 1.25 ± 0.2 M⊙/yr, a stellar mass M* = (4.9 ± 0.3) × 1010 M⊙, and a specific SFR that is relatively constant with radius (except for the inner 1 kpc). We identified an inner radius Rin = 4.5 kpc beyond which the stellar emissivity and dust distribution fall exponentially. For R &lt; Rin the emissivities fall linearly towards the centre. The old stellar populations in the disk have an exponential scalelength that increases monotonically from $h_{\rm s}^{\rm disk}(K)=2.2\pm 0.6$ kpc in the NIR, to $h_{\rm s}^{\rm disk}(B)=3.2\pm 0.9$ kpc at the shorter optical bands, and a scaleheight that varies with radial distance, from $z_{\rm s}^{\rm disk}(0) =140\pm 20$ pc in the centre to $z_{\rm s}^{\rm disk}(R_{\odot }) =300\pm 20$ pc at the solar radius. The young stellar populations have a scalelength of $h_{\rm s}^{\rm tdisk}=3.2\pm 0.9$ kpc and a scaleheight that varies from $z_{\rm s}^{\rm tdisk}(0)=50\pm 10$ pc in the centre to $z_{\rm s}^{\rm tdisk}(R_{\odot })=90\pm 10$ pc at the solar radius. We discovered an inner stellar disk within the central 4.5 kpc, which we associate with the extended long bar of the MW. Most of the obscured star formation happens within this inner thin disk. The diffuse dust is mainly distributed in a disk with scalelength $h_{\rm d}^{\rm disk}=5.2\pm 0.8$ kpc and scaleheight $z_{\rm d}^{\rm disk}=0.14\pm 0.02$ kpc. We give the first derivation of the MW attenuation curve and present it as a functional fit to the model data. We find the MW to lie in the Green Valley of the main sequence relation for spiral galaxies.
The influence of the environment on the spin evolution of low-mass stars – I. External photoevaporation of circumstellar discs
Authors: Roquette J , Matt S P , Winter A J , Amard L , Stasevic S 
Published: September 2021

ABSTRACT
Massive stars are strong sources of far-ultraviolet radiation that can be hostile to the evolution of protoplanetary discs, driving mass-loss by external photoevaporation and shortening disc-dissipation time-scales. Their effect may also reduce the time-scale of angular momentum exchanges between the disc and host star during the early pre-main-sequence phase. To improve our understanding of the environmental influence on the rotational history of stars, we developed a model that considers the influence of the local far-ultraviolet radiation on the spin evolution of low mass stars. Our model includes an assumption of disc locking, which fixes the rotation rate during the star-disc-interaction phase, with the duration of this phase parametrized as a function of the local far-ultraviolet radiation and stellar mass (in the range of 0.1–1.3 M⊙). In this way, we demonstrate how the feedback from massive stars can significantly influence the spin evolution of stars and explain the mass dependence observed in period-mass distributions of young regions like Upper Sco and NGC 2264. The high far-ultraviolet environments of high-mass stars can skew the period distribution of surrounding stars towards fast-rotation, explaining the excess of fast-rotating stars in the open cluster h Per. The proposed link between rotation and the pre-main-sequence environment opens new avenues for interpreting the rotational distributions of young stars. For example, we suggest that stellar rotation may be used as a tracer for the primordial ultraviolet irradiation for stars up to ∼1 Gyr, which offers a potential method to connect mature planetary systems to their birth environment.
Distant probes of rotation measure structure: where is the Faraday rotation towards the Magellanic Leading Arm?
Authors: Jung S Lyla , McClure-Griffiths N M , Hill Alex S 
Published: September 2021

ABSTRACT
Faraday rotation measures (RMs) should be interpreted with caution because there could be multiple magneto-ionized medium components that contribute to the net Faraday rotation along sightlines. We introduce a simple test using Galactic diffuse polarized emission that evaluates whether structures evident in RM observations are associated with distant circumgalactic medium or foreground interstellar medium. We focus on the Magellanic Leading Arm region where a clear excess of RM was previously reported. There are two gaseous objects standing out in this direction: the distant Magellanic Leading Arm and the nearby Antlia supernova remnant (SNR). We recognized narrow depolarized filaments in the $2.3\, \rm GHz$ S-band Polarization All Sky Survey image that overlaps with the reported RM excess. We suggest that there is a steep gradient in Faraday rotation in a foreground screen arising from the Antlia SNR. The estimated strength of the line-of-sight component of the magnetic field is $B_{\parallel }\sim 5\, \rm \mu G$, assuming that the excess of RM is entirely an outcome of the magnetized supernova shell. Our analysis indicates that the overlap between the RM excess and the Magellanic Leading Arm is only a remarkable coincidence. We suggest for future RM grid studies that checking Galactic diffuse polarization maps is a convenient way to identify local Faraday screens.
Broadened profiles of diffuse interstellar bands
Authors: Krełowski J , Galazutdinov G A , Gnaciński P , Hakalla R , Szajna W , Siebenmorgen R 
Published: September 2021

ABSTRACT
The paper describes profile broadening and peak wavelength variation of diffuse interstellar bands (DIBs) measured for 46 lines of sight, probably caused by the physical properties of intervening clouds. The full width at half-maximum of four studied DIBs (5780, 5797, 6196 and 6614 Å) demonstrates strong variability, sometimes doubling the widths of the features. Despite the high magnitude of the effect, our current analysis is restricted to the strongest DIBs because the weaker ones require a much higher signal-to-noise ratio. The profile broadening in the studied DIBs moves the profile’s centres towards longer wavelengths, probably due to the excitation of higher levels of the P branch of the unknown molecular carrier. Moreover, DIBs are broader in clouds with abundantly populated vibrationally excited states of hydrogen molecules; that is, the broadening of DIBs correlates with the rotational temperature estimated on the H2ν= 2 vibrational level. However, objects that demonstrate extremely broadened profiles of DIBs are scarce. The extreme peculiarity of the DIB profiles was detected in Herschel 36. Here we show the gradual growths of the widths of DIBs, confirmed in spectra from different instruments.