bluuebunny/crossref_metadata_2025_split huggingface dataset:
Comparative toxicology of syringe exchange and postmortem blood samples in the District of Columbia: Trends and affinity analysis
Authors: Turley Ben , Evans Alexandra , Benzio Katharine 
Published: August 2023

Abstract
This cross-sectional analysis aimed to understand the similarities and differences between drugs detected in syringes collected from syringe service providers in the District of Columbia and fatal overdose deaths captured by the State Unintentional Drug Overdose Reporting System. Substance exposures for these fatal and non-fatal drug use outcomes have not been previously compared. Substance distributions were examined and a paired significance test was used to compare changes over time. Affinity analysis was employed to reveal substance co-occurrences. Between September 2020 and September 2022, 1,118 postmortem blood samples (PBSs) and 3,646 syringes exchange samples (SESs) were processed, with fatal overdoses increasing 24.1%. Polysubstance use was more commonly found in postmortem blood (82.5%) than in syringe samples (48.6%). Of samples containing opioids, 94.8% of blood samples and 86.3% of syringes contained fentanyl, fentanyl analogs or fentanyl precursors/metabolites. PBSs had double the frequency of co-occurring stimulants and opioids (43.9%) as SESs (21.8%). Major changes in occurrence frequency over time were found for opioid and stimulant exposure in both groups, especially in the increased occurrence of fluorofentanyl (&gt;400%), methamphetamine (&gt;90%) and xylazine (&gt;60%), while the incidence of fentanyl, heroin and metabolite morphine declined. These results indicate that while fatal use and syringe exchange populations have distinct substance exposures, which may contribute to differences in mortality rate, their substance distributions have similar change magnitudes. This study highlights the utility of using multiple data sources to provide a comprehensive description of drug use patterns and discusses the limitations in reporting data from each source.
Urban ash management and emerald ash borer (Coleoptera: Buprestidae): facts, myths, and an operational synthesis
Authors: Sadof Clifford S , McCullough Deborah G , Ginzel Matthew D 
Published: August 2023

Abstract
Survival of North American species of ash (Oleaceae: Fraxinus spp. L.) is threatened by emerald ash borer (EAB), Agrilus planipennis (Fairmaire), a phloem-feeding beetle that destroys the vascular system of its host. In forested sites where ash is a dominant overstory species, mortality caused by EAB can substantially alter conditions, with potentially cascading effects on ecosystems. In urban forests, ash trees were often abundant and provided an array of ecosystem services because of their rapid growth, capacity to withstand stressful urban conditions and prior to EAB, low pest load. Annualized costs of managing EAB on urban ash trees over the next 30 yr in the United States has been estimated to approach $1.8 billion. Numerous cost-benefit analyses have demonstrated that it is more cost effective to retain mature ash trees with systemic insecticides than to replace these trees in urban areas. Effective protection of urban ash trees depends on deployment of systemic insecticides before EAB injury disrupts the vascular system that transports insecticide to the canopy. Given the ongoing spread of EAB, timely management is critical for protecting urban ash canopies. Over the last 2 decades, we have encountered persistent myths that have hindered the adoption of protective measures to preserve urban ash in communities recently infested by EAB. Here we review these myths and counter them with research-based evidence that supports and justifies an ash management program. Finally, we use the 5 basic tenets of IPM to outline an approach for managing EAB in urban forests.
The analysis of fecal calprotectin as a diagnostic marker for anastomotic leakage after rectal cancer surgery: a pilot study
Authors: Hiraki Masatsugu , Tanaka Toshiya , Sato Hirofumi , Miyake Shuusuke , Kubo Hiroshi , Shinkai Yukio , Sadashima Eiji , Kitahara Kenji 
Published: July 2023

Abstract
A prospective pilot study was conducted on 11 patients with rectal cancer to investigate fecal calprotectin (FC) as a diagnostic tool for detecting anastomotic leakage (AL) after low anterior resection. Among the 11 patients, 1 patient (9.1%) experienced AL (Clavien-Dindo Grade IIIa). During the post-operative course until post-operative day (POD) 5, the white blood cell count of the patient with AL was within the normal range. The C-reactive protein level in the AL and non-AL groups showed a similar time course. On the other hand, the FC level in patient with AL dramatically increased on POD5, while the FC level of the non-AL group remained relatively stable. There was no significant correlation between the preoperative FC level and the tumor circumference rate, tumor size, depth of invasion or stage. This pilot study showed the possibility of FC as a useful diagnostic tool for the detection of AL after low anterior resection for rectal cancer.
A MeerKAT-meets-LOFAR study of Abell 1413: a moderately disturbed non-cool-core cluster hosting a ~500 kpc ‘mini’-halo
Authors: Riseley C J , Biava N , Lusetti G , Bonafede A , Bonnassieux E , Botteon A , Loi F , Brunetti G , Cassano R , Osinga E , Rajpurohit K , Röttgering H J A , Shimwell T , Timmerman R , van Weeren R J 
Published: August 2023

ABSTRACT
Many relaxed cool-core clusters host diffuse radio emission on scales of hundreds of kiloparsecs: mini-haloes. However, the mechanism responsible for generating them, as well as their connection with central active galactic nuclei, is elusive and many questions related to their physical properties and origins remain unanswered. This paper presents new radio observations of the galaxy cluster Abell 1413 performed with MeerKAT (L-band; 872 to 1712 MHz) and LOFAR HBA (120 to 168 MHz) as part of a statistical and homogeneous census of mini-haloes. Abell 1413 is unique among mini-halo clusters as it is a moderately disturbed non-cool-core cluster. Our study reveals an asymmetric mini-halo up to 584 kpc in size at 1283 MHz, twice as large as first reported at similar frequencies. The spectral index is flatter than previously reported, with an integrated value of α = −1.01 ± 0.06, shows significant spatial variation, and a tentative radial steepening. We studied the point-to-point X-ray/radio surface brightness correlation to investigate the thermal/non-thermal connection: our results show a strong connection between these components, with a superlinear slope of $b = 1.63^{+0.10}_{-0.10}$ at 1283 MHz and $b = 1.20^{+0.13}_{-0.11}$ at 145 MHz. We also explore the X-ray surface brightness/radio spectral index correlation, finding a slope of $b = 0.59^{+0.11}_{-0.11}$. Both investigations support the evidence of spectral steepening. Finally, in the context of understanding the particle acceleration mechanism, we present a simple theoretical model which demonstrates that hybrid scenarios – secondary electrons (re-)accelerated by turbulence – reproduce a superlinear correlation slope.
High-resolution VLBI astrometry of pulsar scintillation screens with the θ - θ transform
Authors: Baker Daniel , Brisken Walter , van Kerkwijk Marten H , van Lieshout Rik , Pen Ue-Li 
Published: August 2023

ABSTRACT
The recent development of $\theta - \theta$ techniques in pulsar scintillometry has opened the door for new high-resolution imaging techniques of the scattering medium. By solving the phase retrieval problem and recovering the wavefield from a pulsar dynamic spectrum, the Doppler shift, time delay, and phase offset of individual images can be determined. However, the results of phase retrieval from a single dish are only known up to a constant phase rotation, which introduces extra parameters when doing astrometry using very long baseline interferometry. We present an extension to previous $\theta - \theta$ methods using the interferometric visibilities between multiple stations to calibrate the wavefields. When applied to existing data for PSR B0834+06, we measure the effective screen distance and lens orientation with five times greater precision than was possible in previous work.
Dynamical friction and feedback on galactic bars in the general fast–slow regime
Authors: Chiba Rimpei 
Published: August 2023

ABSTRACT
Current theories of dynamical friction on galactic bars are based either on linear perturbation theory, which is valid only in the fast limit where the bar changes its pattern speed rapidly, or on adiabatic theory, which is applicable only in the slow limit where the bar’s pattern speed is near-constant. In this paper, we study dynamical friction on galactic bars spinning down at an arbitrary speed, seamlessly connecting the fast and slow limits. We treat the bar–halo interaction as a restricted N-body problem and solve the collisionless Boltzmann equation using the fast-angle-averaged Hamiltonian. The phase-space distribution and density wakes predicted by our averaged model are in excellent agreement with full 3D simulations. In the slow regime where resonant trapping occurs, we show that, in addition to the frictional torque, angular momentum is transferred directly due to the migration of the trapped phase-space: trapped orbits comoving with the resonance typically gain angular momentum, while untrapped orbits leaping over the trapped island lose angular momentum. Due to the negative gradient in the distribution function, gainers typically outnumber the losers, resulting in a net negative torque on the perturber. Part of this torque due to the untrapped orbits was already identified by Tremaine and Weinberg, who named the phenomenon dynamical feedback. Here, we derive the complete formula for dynamical feedback, accounting for both trapped and untrapped orbits. Using our revised formula, we show that dynamical feedback can account for up to 30 per cent of the total torque on the Milky Way’s bar.
The exploration of the soft X-ray excess in FSRQ 4C+21.35 during the 2014 X-ray flare
Authors: Zhao Keqin , Yin Hongxing , Hu Shaoming , Huang Shifeng , Qiao Erlin , Cheng Huaqing , Chen Xu , Xu Jingran 
Published: August 2023

ABSTRACT
We report the soft X-ray excess feature and an opposite tendency between the optical/UV and X-ray bands during the flare that occurred in 2014 in flat-spectrum radio quasar (FSRQ) 4C+21.35 with the observations by Swift-XRT and Swift-UVOT. These unusual phenomena are rarely reported in FSRQs. The flare was covered from the optical to the X-ray while no prominent activity in the γ-ray was observed, which could be an indication of weaker jet activity during the flare. We carry out the spectral energy distribution ranging from the optical to X-ray based on four models which are the warm corona model (Model-1), the relativistic reflection model (Model-2), the corona with the jet model (Model-3), and the relativistic reflection with the jet model (Model-4). We find some extreme variation of the parameters in Model-2 and Model-4 and they are unable to explain the correlations between the optical/UV and X-ray bands. Model-1 and Model-3 can obtain reasonable parameters and provide an explanation for the observed opposite tendency between the optical/UV and X-ray bands. However, considering the weak jet activity during the X-ray flare, Model-1 is much preferred for describing the soft X-ray excess, hard X-ray emission, as well as the opposite tendency between the optical/UV and X-rays. Based on Model-1, it is suggested that the flare in 2014 is probably due to the variation of the geometry of the corona, which is expected to be more strictly tested with further observations in the future.
Towards a reliable prediction of the infrared spectra of cosmic fullerenes and their derivatives in the JWST era
Authors: Xu Jianzhi , Li Aigen , Li Xiaohu , Hou Gao-Lei 
Published: August 2023

ABSTRACT
Fullerenes, including C60, C70, and C60+, are widespread in space through their characteristic infrared vibrational features (C60+ also reveals its presence in the interstellar medium through its electronic transitions) and offer great insights into carbon chemistry and stellar evolution. The potential existence of fullerene-related species in space has long been speculated and recently put forward by a set of laboratory experiments of C60+, C60H+, C60O+, C60OH+, C70H+, and [C60-Metal]+ complexes. The advent of the JWST provides a unique opportunity to search for these fullerene-related species in space. To facilitate JWST search, analysis, and interpretation, accurate knowledge of their vibrational properties is essential. Here, we compile a VibFullerene database and conduct a systematic theoretical study on those species. We derive a set of range-specific scaling factors for vibrational frequencies to account for the deficiency of density functional theory calculations in predicting accurate frequencies. Scaling factors with low root-mean-square and median errors for the frequencies are obtained, and their performance is evaluated, from which the best-performing methods are recommended for calculating the infrared spectra of fullerene derivatives that balance the accuracy and the computational cost. Finally, the recommended vibrational frequencies and intensities of fullerene derivatives are presented for future JWST detection.
The evolution of relative frequencies of ONe and CO SNe Ia
Authors: Bogomazov A I , Tutukov A V 
Published: August 2023

ABSTRACT
In this population synthesis work, we study a variety of possible origin channels of supernovae type Ia (SNe Ia). Among them mergers of carbon–oxygen (CO) and oxygen–neon (ONe) white dwarfs (WDs) under the influence of gravitational waves are considered as the primary channel of SNe Ia formation. We estimated frequencies of mergers of WDs with different chemical compositions and distributions of masses of merging WDs. We computed the dependence of the ratio of merger frequencies of ONe and CO WDs as primaries in corresponding binaries on time. The scatter of masses of considered sources (up to the factor 1.5–2) of SNe Ia is important and should be carefully studied with other sophisticated methods from theoretical point of view. Our ‘game of parameters’ potentially explains the increased dimming of SNe Ia in the redshift range z ≈ 0.5–1 by the changes in the ratio of ONe and CO WDs, i.e. to describe the observed accelerated expansion of the Universe in terms of the evolution of properties of SNe Ia instead of cosmological explanations. This example shows the extreme importance of theoretical studies of problems concerning SNe Ia, because evolutionary scenario and parameter games in nature potentially lead to confusions in their empirical standardization and, therefore, they can influence on cosmological conclusions.
MIGHTEE-H i: the MH i – M* relation over the last billion years
Authors: Pan Hengxing , Jarvis Matt J , Santos Mario G , Maddox Natasha , Frank Bradley S , Ponomareva Anastasia A , Prandoni Isabella , Kurapati Sushma , Baes Maarten , Piña Pavel E Mancera , Rodighiero Giulia , Meyer Martin J , Davé Romeel , Sharma Gauri , Rajohnson Sambatriniaina H A , Adams Nathan J , Bowler Rebecca A A , Sinigaglia Francesco , van der Hulst Thijs , Hatfield Peter W , Sekhar Srikrishna , Collier Jordan D 
Published: August 2023

ABSTRACT
We study the $M_{\rm H\, {\small {I}}}-M_{\star }$ relation over the last billion years using the MIGHTEE-H i sample. We first model the upper envelope of the $M_{\rm H\, {\small {I}}}-M_{\star }$ relation with a Bayesian technique applied to a total number of 249 H i-selected galaxies, without binning the data sets, while taking account of the intrinsic scatter. We fit the envelope with both linear and non-linear models, and find that the non-linear model is preferred over the linear one with a measured transition stellar mass of log10(M⋆/M⊙) = 9.15 ± 0.87, beyond which the slope flattens. This finding supports the view that the lack of H i gas is ultimately responsible for the decreasing star formation rate observed in the massive main-sequence galaxies. For spirals alone, which are biased towards the massive galaxies in our sample, the slope beyond the transition mass is shallower than for the full sample, indicative of distinct gas processes ongoing for the spirals/high-mass galaxies from other types with lower stellar masses. We then create mock catalogues for the MIGHTEE-H i detections and non-detections with two main galaxy populations of late- and early-type galaxies to measure the underlying $M_{\rm H\, {\small {I}}}-M_{\star }$ relation. We find that the turnover in this relation persists whether considering the two galaxy populations as a whole or separately. We note that an underlying linear relation could mimic this turnover in the observed scaling relation, but a model with a turnover is strongly preferred. Measurements on the logarithmic average of H i masses against the stellar mass are provided as a benchmark for future studies.
Nucleosynthesis in outflows of compact objects and detection prospects of associated kilonovae
Authors: Ekanger Nick , Bhattacharya Mukul , Horiuchi Shunsaku 
Published: August 2023

ABSTRACT
We perform a comparative analysis of nucleosynthesis yields from binary neutron star (BNS) mergers, black hole-neutron star (BHNS) mergers, and core-collapse supernovae (CCSNe) with the goal of determining which are the most dominant sources of r-process enrichment observed in stars. We find that BNS and BHNS binaries may eject similar mass distributions of robust r-process nuclei post-merger (up to third peak and actinides, A ∼ 200−240), after accounting for the volumetric event rates. Magnetorotational (MR) CCSNe likely undergo a weak r-process (up to A ∼ 140) and contribute to the production of light element primary process (LEPP) nuclei, whereas typical thermal, neutrino-driven CCSNe only synthesize up to first r-process peak nuclei (A ∼ 80−90). We also find that the upper limit to the rate of MR CCSNe is $\lesssim 1~{{\ \rm per\ cent}}$ the rate of typical thermal CCSNe; if the rate was higher, then weak r-process nuclei would be overproduced. Although the largest uncertainty is from the volumetric event rate, the prospects are encouraging for confirming these rates in the next few years with upcoming surveys. Using a simple model to estimate the resulting kilonova light curve from mergers and our set of fiducial merger parameters, we predict that ∼7 BNS and ∼2 BHNS events will be detectable per year by the Vera C. Rubin Observatory (LSST), with prior gravitational wave (GW) triggers.
Mapping gravity in stellar nurseries – establishing the effectiveness of 2D acceleration maps
Authors: He Zhen-Zhen , Li Guang-Xing , Burkert Andreas 
Published: August 2023

ABSTRACT
Gravity is the driving force of star formation. Although gravity is caused by the presence of matter, its role in complex regions is still unsettled. One effective way to study the pattern of gravity is to compute the accretion it exerts on the gas by providing gravitational acceleration maps. A practical way to study acceleration is by computing it using 2D surface density maps, yet whether these maps are accurate remains uncertain. Using numerical simulations, we confirm that the accuracy of the acceleration maps a2D(x, y) computed from 2D surface density are good representations for the mean acceleration weighted by mass. Due to the underestimations of the distances from projected maps, the magnitudes of accelerations will be overestimated $|\mathbf {a}_{\rm 2D}(x,y)| \approx 2.3 \pm 1.8 \,\, |\mathbf {a}_{\rm 3D}^{\rm proj}(x,y)|$, where $\mathbf {a}_{\rm 3D}^{\rm proj}(x,y)$ is mass-weighted projected gravitational acceleration, yet a2D(x, y) and $\mathbf {a}_{\rm 3D}^{\rm proj}(x,y)$ stay aligned within 20°. Significant deviations only occur in regions where multiple structures are present along the line of sight. The acceleration maps estimated from surface density provide good descriptions of the projection of 3D acceleration fields. We expect this technique useful in establishing the link between cloud morphology and star formation, and in understanding the link between gravity and other processes such as the magnetic field. A version of the code for calculating surface density gravitational potential is available at https://github.com/zhenzhen-research/phi_2d.
The clustering properties of high-redshift passive galaxies
Authors: Magliocchetti M , Santini P , Merlin E , Pentericci L 
Published: August 2023

ABSTRACT
We investigate the clustering properties of 3 &lt; z &lt; 5 candidate passive galaxies from the Merlin et al. (2019) sample residing in the GOODS-North (35 sources) and GOODS-South (33 sources) fields. Within the large uncertainties due to the paucity of sources we do not detect clustering signal in GOODS-North, while this is present in GOODS-South, highlighting the importance of the effects of cosmic variance. The estimated correlation length in GOODS-South is $r_0=12^{+4}_{-5}$ Mpc, while the estimated minimum mass for a halo capable to host one of such high-redshift quenched galaxies is log10(Mmin/M⊙) = 13.0 ± 0.3, once also the constraints from their space density are taken into account. Both values are compatible with the results from GOODS-North. Putting the above findings in a cosmological context, these suggest no evolution of the dark matter content of the hosts of passive galaxies during the past 12.5 Gyr, i.e. during more than 90 per cent of the age of the Universe. We discuss possible scenarios for the observed trend.
The innermost jet in the hidden ultra-luminous X-ray source Cygnus X-3
Authors: Yang Jun , García Federico , del Palacio Santiago , Spencer Ralph , Paragi Zsolt , Castro Segura Noel , Gong Biping , Cao Hongmin , Chen Wen 
Published: August 2023

ABSTRACT
Cygnus X-3 is a high-mass X-ray binary with a compact object accreting matter from a Wolf–Rayet donor star. Recently, it has been revealed by the Imaging X-ray Polarimetry Explorer (IXPE) as a hidden Galactic ultra-luminous X-ray (ULX) source with a luminosity above the Eddington limit, along the direction of a narrow (opening angle $\lesssim 32^{\circ }$) funnel. In between the IXPE observations, we observed Cyg X-3 with the European very long baseline interferometry (VLBI) Network at 22 GHz and the NICER X-ray instrument. To probe possible relations between the X-ray funnel and the potential radio jet from the ULX, we analysed the simultaneous multiwavelength data. Our high-resolution VLBI image reveals an elongated structure with a position angle of −3.2 ± 0.4 °, accurately perpendicular to the direction of the linear X-ray polarization. Because Cyg X-3 was in the radio quiescent state on 2022 November 10, we identify the mas-scale structure as the innermost radio jet. The finding indicates that the radio jet propagates along and within the funnel. Moreover, the jet is marginally resolved in the transverse direction. This possibly results from the strong stellar winds and the rapid orbital motion of the binary system.