bluuebunny/crossref_metadata_2025_split huggingface dataset:
Use of the Mucorales qPCR on blood to screen high-risk hematology patients is associated with better survival
Authors: Bellanger Anne-Pauline , Gbaguidi-Haore Houssein , Berceanu Ana , Gouzien Laura , El Machhour Chaima , Bichard Damien , Lanternier Fanny , Scherer Emeline , Millon Laurence ,   French Mycoses Study Group, Chouaki T , Damiani C , Pihet M , Bonhomme J , Nourrisson C , Poirier P , Dalle F , Desbois N , Bouteille B , Durieux M F , Morio F , Hasseine L , Sasso M , Paugam A , Mariani P , Bougnoux M E , Merabet L , Alanio A , Bretagne S , Minoza A , Perraud E , Nicolas M , Toubas D , Huguenin A , Gangneux J P , Raberin H , Mahinc C , Letscher-Bru V , Favennec L , Cassaing S , Bailly E , Chachaty E , Eloy O , Sitbon K , Hermoso D Garcia 
Published: March 2024

Abstract
Our objective was to determine whether the twice-weekly screening of high-risk hematology patients by Mucorales qPCR on serum affects the prognosis of mucormycosis. Results from all serum Mucorales qPCR tests performed on patients from the hematology unit from January 2017 to December 2022 were analyzed. Patients with positive results were classified as having proven, probable or ‘PCR-only’ mucormycosis. One-month mortality for the local cohort was compared with that of a national cohort of cases of mucormycosis collected by the French surveillance network for invasive fungal disease (‘Réseau de surveillances des infections fongiques invasives en France’ (RESSIF)) from 2012 to 2018. From 2017 to 2022, 7825 serum Mucorales qPCR tests were performed for patients from the hematology unit; 107 patients with at least one positive Mucorales qPCR (164 positive samples) were identified. Sixty patients (70 positive samples, median Cq = 40) had no radiological criteria for mucormycosis and were considered not to have invasive fungal disease (70/7825, 0.9% false positives). It was not possible to classify disease status for six patients (12 positive samples, median Cq = 38). Forty-one patients (82 positive samples, median Cq = 35) had a final diagnosis of mucormycosis. In comparison with the RESSIF cohort, the local cohort was independently associated with a 48% lower one-month all-cause mortality rate (age-, sex-, and primary disease-adjusted hazard ratio = 0.52; 95% confidence interval: 0.29–0.94; P 0.03). Proactive screening for invasive mold diseases in high-risk hematology patients, including twice-weekly Mucorales qPCR on serum, was associated with mucormycosis higher survival.
Origin of the correlation between stellar kinematics and globular cluster system richness in ultradiffuse galaxies
Authors: Pfeffer Joel , Janssens Steven R , Buzzo Maria Luisa , Gannon Jonah S , Bastian Nate , Bekki Kenji , Brodie Jean P , Couch Warrick J , Crain Robert A , Forbes Duncan A , Kruijssen J M Diederik , Romanowsky Aaron J 
Published: March 2024

ABSTRACT
Observational surveys have found that the dynamical masses of ultradiffuse galaxies (UDGs) correlate with the richness of their globular cluster (GC) system. This could be explained if GC-rich galaxies formed in more massive dark matter haloes. We use simulations of galaxies and their GC systems from the E-MOSAICS project to test whether the simulations reproduce such a trend. We find that GC-rich simulated galaxies in galaxy groups have enclosed masses that are consistent with the dynamical masses of observed GC-rich UDGs. However, simulated GC-poor galaxies in galaxy groups have higher enclosed masses than those observed. We argue that GC-poor UDGs with low stellar velocity dispersions are discs observed nearly face on, such that their true mass is underestimated by observations. Using the simulations, we show that galactic star formation conditions resulting in dispersion-supported stellar systems also leads to efficient GC formation. Conversely, conditions leading to rotationally supported discs lead to inefficient GC formation. This result may explain why early-type galaxies typically have richer GC systems than late-type galaxies. This is also supported by comparisons of stellar axis ratios and GC-specific frequencies in observed dwarf galaxy samples, which show GC-rich systems are consistent with being spheroidal, while GC-poor systems are consistent with being discs. Therefore, particularly for GC-poor galaxies, rotation should be included in dynamical mass measurements from stellar dynamics.
Nature of the diffuse emission sources in the H i supershell in the galaxy IC 1613
Authors: Yarovova Anastasiya D , Moiseev Alexei V , Gerasimov Ivan S , Vučetić Milica M , Egorov Oleg V , Ilić Dragana , Mereminskiy Ilya A , Pakhomov Yury V , Sholukhova Olga N 
Published: March 2024

ABSTRACT
We present a study of the nearby low-metallicity dwarf galaxy IC 1613, focusing on the search for massive stars and related feedback processes, as well as for faint supernova remnants (SNR) in late stages of evolution. We obtained the deepest images of IC 1613 in the narrow-band H α, He ii and [S ii] emission lines and new long-slit spectroscopy observations using several facilities (6-m BTA, 2.5m SAI MSU, and 150RTT telescopes), in combination with the multiwavelength archival data from MUSE/VLT, VLA, XMM–Newton, and Swift/XRT. Our deep narrow-band photometry identifies several faint shells in the galaxy, and we further investigate their physical characteristics with the new long-slit spectroscopy observations and the archival multiwavelength data. Based on energy balance calculations and assumptions about their possible nature, we propose that one of the shells is a possible remnant of a supernova explosion. We study five out of eight Wolf–Rayet (WR) star candidates previously published for this galaxy using the He ii emission line mapping, MUSE/VLT archival spectra, and new long-slit spectra. Our analysis discards the considered WR candidates and finds no new ones. We found P Cyg profiles in H α line in two stars, which we classify as Luminous Blue Variable (LBV) star candidates. Overall, the galaxy IC 1613 may have a lower rate of WR star formation than previously suggested.
Magnetic field transport in geometrically thick discs: multidimensional effects on the field strength and inclination angle
Authors: Yamamoto Ryoya , Takasao Shinsuke 
Published: March 2024

ABSTRACT
We theoretically investigate the magnetic flux transport in geometrically thick accretion discs which may form around black holes. We utilize a two-dimensional (2D) kinematic mean-field model for poloidal field transport which is governed by both inward advection and outward diffusion of the field. Assuming a steady state, we analytically show that the multidimensional effects prevent the field accumulation towards the centre and reduce the field inclination angle. We also numerically investigate the radial profile of the field strength and the inclination angle for two geometrically thick discs for which (quasi-)analytical solutions exist: radiatively inefficient accretion flows (RIAFs) and super-Eddington accretion flows. We develop a 2D kinematic mean-field code and perform simulations of flux transport to study the multidimensional effects. The numerical simulations are consistent with our analytical prediction. We also discuss a condition for the external field strength that RIAF can be a magnetically arrested disc. This study could be important for understanding the origin of a large-scale magnetic field that drives jets and disc winds around black holes.
Phase space distribution functions and energy distributions of dark matter particles in haloes
Authors: Gross Axel , Li Zhaozhou , Qian Yong-Zhong 
Published: March 2024

ABSTRACT
For a spherical dark matter halo with isotropic velocity distribution, the phase space distribution function (DF), the energy distribution, and the density profile form a set of self-consistent description of its equilibrium state, and knowing one is sufficient to determine the other two. The Navarro–Frenk–White density profile (NFW profile) is known to be a good approximation to the spherically averaged density distribution in simulated haloes. The DARKexp energy distribution is also known to compare well with the simulated energy distribution. We present a quantitative assessment of the NFW and DARKexp fits to the simulated DF and energy distribution for a wide range of haloes in a dark-matter-only simulation from the IllustrisTNG Project. As expected, we find that the NFW fits work well except at low energy when the density at small radii deviates from the NFW profile. Further, the NFW and DARKexp fits have comparable accuracy in the region where both fit well, but the DARKexp fits are better at low energy because they require matching of the central gravitational potential. We also find an approximate relation between the energy scale parametrizing the DARKexp energy distribution and that defined by the characteristic density and radius of the NFW profile. This relation may be linked to the relaxation process during halo formation.
Chandra and HST studies of the X-ray sources in the globular cluster NGC 362
Authors: Kumawat Gourav , Heinke Craig O , Cohn Haldan N , Lugger Phyllis M 
Published: March 2024

ABSTRACT
We analyse a Chandra observation of the rich globular cluster NGC 362, finding 33 X-ray sources within 1 arcmin (1.2 half-mass radii) of the cluster centre. Spectral analysis of the brightest source (X1) shows blackbody-like emission, indicating it is likely a quiescent low-mass X-ray binary; we find a possible counterpart that falls in the sub-subgiant region. We use Hubble Space Telescope ultraviolet (UV) Globular Cluster Survey photometry to identify 15 potential optical/UV counterparts to these X-ray sources, including two background active galactic nuclei. We identify no likely cataclysmic variables (CVs), probably due to crowding in optical filters in the core, though we predict of order 8 CVs among the detected X-ray sources. We identify three other sub-subgiants and two red straggler counterparts, which are likely powered by coronal activity, along with five other potential coronally active binary counterparts to three X-ray sources. Finally, we note two unusual counterpart candidates that lie to the red of the red giant branch in V606 − I814, and shift well to the blue of the red giant branch in ultraviolet colour–magnitude diagrams. These systems seem to contain a red giant with a distorted evolutionary history, plus a bright blue light source, either a blue straggler star (an Algol-like system) or an accreting white dwarf (a long-period CV, or a symbiotic star).
Simulating emission line galaxies for the next generation of large-scale structure surveys
Authors: Pei Wenxiang , Guo Qi , Li Ming , Wang Qiao , Han Jiaxin , Hu Jia , Su Tong , Gao Liang , Wang Jie , Luo Yu , Wei Chengliang 
Published: March 2024

ABSTRACT
We investigate emission line galaxies across cosmic time by combining the modified L-Galaxies semi-analytical galaxy formation model with the JiuTian cosmological simulation. We improve the tidal disruption model of satellite galaxies in L-Galaxies to address the time dependence problem. We utilize the public code cloudy to compute emission line ratios for a grid of H ii region models. The emission line models assume the same initial mass function as that used to generate the spectral energy distribution of semi-analytical galaxies, ensuring a coherent treatment for modelling the full galaxy spectrum. By incorporating these emission line ratios with galaxy properties, we reproduce observed luminosity functions for H α, H β, [O ii], and [O iii] in the local Universe and at high redshifts. We also find good agreement between model predictions and observations for autocorrelation and cross-correlation functions of [O ii]-selected galaxies, as well as their luminosity dependence. The bias of emission line galaxies depends on both luminosity and redshift. At lower redshifts, it remains constant with increasing luminosity up to around $\sim 10^{42.5}\, {\rm erg\, s^{-1}}$ and then rises steeply for higher luminosities. The transition luminosity increases with redshift and becomes insignificant above z = 1.5. Generally, galaxy bias shows an increasing trend with redshift. However, for luminous galaxies, the bias is higher at low redshifts, as the strong luminosity dependence observed at low redshifts diminishes at higher redshifts. We provide a fitting formula for the bias of emission line galaxies as a function of luminosity and redshift, which can be utilized for large-scale structure studies with future galaxy surveys.
The mass–metallicity and fundamental metallicity relations in non-AGN and AGN-host galaxies
Authors: Li Song-Lin , Grasha Kathryn , Krumholz Mark R , Wisnioski Emily , Sutherland Ralph S , Kewley Lisa J , Chen Yan-Mei , Li Zefeng 
Published: March 2024

ABSTRACT
Galaxies’ stellar masses, gas-phase oxygen abundances (metallicity), and star formation rates (SFRs) obey a series of empirical correlations, most notably the mass–metallicity relation (MZR) and fundamental metallicity relation (FZR), which relates oxygen abundance to a combination of stellar mass and SFR. However, due to the difficulty of measuring oxygen abundances and SFRs in galaxies that host powerful active galactic nuclei (AGN), to date it is unknown to what extent AGN-host galaxies also follow these correlations. In this work, we apply Bayesian methods to the MaNGA integral field spectrographic (IFS) survey that allow us to measure oxygen abundances and SFRs in AGN hosts, and use these measurements to explore how the MZR and FZR differ between galaxies that do and do not host AGN. We find similar MZRs at stellar masses above $10^{10.5} \, \mathrm{M}_\odot$, but that at lower stellar masses AGN hosts show up to $\sim 0.2$ dex higher oxygen abundances. The offset in the FZR is significantly smaller, suggesting that the larger deviation in the MZR is a result of AGN-host galaxies having systematically lower SFRs at fixed stellar mass. However, within the AGN-host sample there is little correlation between SFR and oxygen abundance. These findings support a scenario in which an AGN can halt efficient gas accretion, which drives non-AGN host galaxies to both higher SFR and lower oxygen abundance, resulting in the galaxy evolving off the star-forming main sequence (SFMS). As a consequence, as the SFR declines for an individual system its metallicity remains mostly unchanged.
Supernova remnant properties and luminosity functions in NGC 7793 using MUSE IFS
Authors: Kopsacheili Maria , Jiménez-Palau Cristina , Galbany Lluís , Boumis Panayotis , González-Díaz. Raúl 
Published: March 2024

ABSTRACT
In this study, we use MUSE Integral Field Spectroscopy (IFS), along with multiline diagnostics, for the optical identification of supernova remnants (SNRs) in the galaxy NGC 7793. We find in total 238 SNR candidates, 225 of them new identifications, increasing significantly the number of known SNRs in this galaxy. The velocity dispersion of the candidate SNRs was calculated, giving a mean value of $\rm 27\, km\, s^{-1}$. We construct the H $\rm {\alpha }$, [S ii], [O iii], and [S ii]–H $\rm {\alpha }$ luminosity functions, and for the first time, the [N ii], [N iI]–H $\rm {\alpha }$, [N ii]–[S ii], [O iii]–[S ii], and [O iii]–[N ii] luminosity functions of the candidate SNRs. Shock models, along with the observed multiline information were used, in order to estimate shock velocities. The $\rm \sim 65{{\ \rm per\ cent}}$ of the SNRs present velocities &lt; 300 $\rm km\, s^{-1}$. There is a clear correlation between shock velocity and [O iii]/H $\rm {\beta }$ ratio, and a less clear but still evident correlation in the relation between shock velocity and the [S ii]/H $\rm {\alpha }$, [N ii]/H $\rm {\alpha }$ ratios. We also use the [S ii]6716/31 ratio of the SNR candidates to calculate their post-shock density, assuming different temperatures. The median value of the density of our sample is $\rm \sim 80\, cm^{-3}$, for a temperature of $\rm T = 10^4\, K$. No correlation between shock velocity and density, or density and SNRs with [S ii]/H $\rm {\alpha }$ &gt; 0.4 and [S ii]/H $\rm {\alpha }$ &lt; 0.4 is observed.
Constraints on the origin of the radio synchrotron background via angular correlations
Authors: Todarello Elisa , Regis Marco , Bianchini Federico , Singal Jack , Branchini Enzo , Cowie Fraser J , Heston Sean , Horiuchi Shunsaku , Lucero Danielle , Offringa Andre 
Published: March 2024

ABSTRACT
The origin of the radio synchrotron background (RSB) is currently unknown. Its understanding might have profound implications in fundamental physics or might reveal a new class of radio emitters. In this work, we consider the scenario in which the RSB is due to extragalactic radio sources and measure the angular cross-correlation of Low-Frequency Array (LOFAR) images of the diffuse radio sky with matter tracers at different redshifts, provided by galaxy catalogues and cosmic microwave background lensing. We compare these measured cross-correlations to those expected for models of RSB sources. We find that low-redshift populations of discrete sources are excluded by the data, while higher redshift explanations are compatible with available observations. We also conclude that at least 20 per cent of the RSB surface brightness level must originate from populations tracing the large-scale distribution of matter in the Universe, indicating that at least this fraction of the RSB is of extragalactic origin. Future measurements of the correlation between the RSB and tracers of high-redshift sources will be crucial to constraining the source population of the RSB.
Differences in the properties of disrupted and surviving satellites of Milky-Way-mass galaxies in relation to their host accretion histories
Authors: Grimozzi Salvador E , Font Andreea S , De Rossi María Emilia 
Published: March 2024

ABSTRACT
From the chemodynamical properties of tidal debris in the Milky Way, it has been inferred that the dwarf satellites that have been disrupted had different chemical abundances from their present-day counterparts of similar mass that survive today, specifically, they had lower [Fe/H] and higher [Mg/Fe]. Here we use the Artemis simulations to study the relation between the chemical abundances of disrupted progenitors of MW-mass galaxies and their stellar mass, and the evolution of the stellar mass–metallicity relations (MZR) of this population with redshift. We find that these relations have significant scatter, which correlates with the accretion redshifts (zacc) of satellites, and with their cold gas fractions. We investigate the MZRs of dwarf populations accreted at different redshifts and find that they have similar slopes, and also similar with the slope of the MZR of the surviving population (≈0.32). However, the entire population of disrupted dwarfs displays a steeper MZR, with a slope of ≈0.48, which can be explained by the changes in the mass spectrum of accreted dwarf galaxies with redshift. We find strong relations between the (mass-weighted) 〈zacc〉 of the disrupted populations and their global chemical abundances (〈[Fe/H]〉 and 〈[Mg/Fe]〉), which suggests that chemical diagnostics of disrupted dwarfs can be used to infer the types of merger histories of their hosts. For the case of the MW, our simulations predict that the bulk of the disrupted population was accreted at 〈zacc〉 ≈ 2, in agreement with other findings. We also find that disrupted satellites form and evolve in denser environments, closer to their hosts, than their present-day counterparts.
The morphology of the redshifted 21-cm signal from the Cosmic Dawn
Authors: Ghara Raghunath , Bag Satadru , Zaroubi Saleem , Majumdar Suman 
Published: March 2024

ABSTRACT
The spatial fluctuations in the tomographic maps of the redshifted 21-cm signal from the Cosmic Dawn (CD) crucially depend on the size and distribution of the regions with gas temperatures larger than the radio background temperature. In this article, we study the morphological characteristics of such emission regions and their absorption counterparts using the shape diagnostic tool surfgen2. Using simulated CD brightness temperature cubes of the 21-cm signal, we find that the emission regions percolate at stages with the filling factor of the emission regions $\mathrm{FF}_{\rm emi}\gtrsim 0.15$. Percolation of the absorption regions occurs for $\mathrm{FF}_{\rm abs}\gtrsim 0.05$. The largest emission and absorption regions are topologically complex and highly filamentary for most parts of the CD. The number density of these regions as a function of the volume shows the power-law nature with the power-law indexes $\approx -2$ and $-1.6$ for the emission and absorption regions, respectively. Overall, the planarity, filamentarity, and genus increase with the increase of the volume of both emission and absorption regions.
Diffuse low-grade glioma: What is the optimal linear measure to assess tumor growth?
Authors: Dos Santos Thomas , Deverdun Jeremy , Chaptal Thierry , Darlix Amélie , Duffau Hugues , Van Dokkum Liesjet Elisabeth Henriette , Coget Arthur , Carrière Mathilde , Denis Eve , Verdier Margaux , Menjot de Champfleur Nicolas , Le Bars Emmanuelle 
Published: March 2024

Abstract

Background
Radiological follow-up of diffuse low-grade gliomas (LGGs) growth is challenging. Approximative visual assessment still predominates over objective quantification due to the complexity of the pathology. The infiltrating character, diffuse borders and presence of surgical cavities demand LGG-based linear measurement rules to efficiently and precisely assess LGG evolution over time.

Methods
We compared optimized 1D, 2D, and 3D linear measurements with manual volume segmentation as a reference to assess LGG tumor growth in 36 patients with LGG (340 magnetic resonance imaging scans), using the clinically important mean tumor diameter (MTD) and the velocity diameter expansion (VDE). LGG-specific progression thresholds were established using the high-grade gliomas-based RECIST, Macdonald, and RANO criteria, comparing the sensitivity to identify progression/non-progression for each linear method compared to the ground truth established by the manual segmentation.

Results
3D linear volume approximation correlated strongly with manually segmented volume. It also showed the highest sensitivity for progression detection. The MTD showed a comparable result, whereas the VDE highlighted that caution is warranted in the case of small tumors with multiple residues. Novel LGG-specific progression thresholds, or the critical change in estimated tumor volume, were increased for the 3D (from 40% to 52%) and 2D methods (from 25% to 33%) and decreased for the 1D method (from 20% to 16%). Using the 3D method allowed a ~5-minute time gain.

Conclusions
While manual volumetric assessment remains the gold standard for calculating growth rate, the 3D linear method is the best time-efficient standardized alternative for radiological evaluation of LGGs in routine use.