bluuebunny/crossref_metadata_2025 huggingface dataset:
Assessing the safety profile of voriconazole use in suspected COVID-19-associated pulmonary aspergillosis–a two-centre observational study
Authors: Costa-Pinto Rahul , Klink Sarah , Rotherham Hannah , Perera Padeepa , Finlay Liam , Urbancic Karen , Vaz Karl , Trubiano Jason , Bellomo Rinaldo
Published: June 2023

The decision to use voriconazole for suspected COVID-19-associated pulmonary aspergillosis (CAPA) is based on clinical judgement weighed against concerns about its potential toxicity. We assessed the safety profile of voriconazole for patients with suspected CAPA by conducting a retrospective study of patients across two intensive care units. We compared changes in any liver enzymes or bilirubin and any new or increasing corrected QT interval (QTc) prolongation following voriconazole use to patient baseline to indicate possible drug effect.

In total, 48 patients with presumed CAPA treated with voriconazole were identified. Voriconazole therapy was administered for a median of 8 days (interquartile range [IQR] 5–22) and the median level was 1.86 mg/L (IQR 1.22–2.94). At baseline, 2% of patients had a hepatocellular injury profile, 54% had a cholestatic injury profile, and 21% had a mixed injury profile. There were no statistically significant changes in liver function tests over the first 7 days after voriconazole initiation. At day 28, there was a significant increase in alkaline phospahte only (81–122 U/L, P = 0.006), driven by changes in patients with baseline cholestatic injury. In contrast, patients with baseline hepatocellular or mixed injury had a significant decrease in alanine transaminase and aspartate transaminase. Baseline QTc was 437 ms and remained unchanged after 7 days of voriconazole therapy even after sensitivity analysis for concomitantly administered QT prolonging agents.

Therefore, at the doses used in this study, we did not detect evidence of significant liver or cardiac toxicity related to voriconazole use. Such information can be used to assist clinicians in the decision to initiate such treatment.
Evidence of anti-Hcp100 antibodies in COVID-19 critically ill patients with detectable anti-histoplasmin antibodies in a highly endemic area for histoplasmosis
Authors: Toscanini María A , Barberis Fernanda , Benedetti Fernanda , Rodríguez Laboccetta Carolina , Videla Garrido Agustín , Fernández Briceño Víctor , Posse Gladys B , Capece Paula , Nusblat Alejandro D , Cuestas María L
Published: June 2023

Patients with severe COVID-19 are at increased risk for invasive fungal infections, which are underestimated. Histoplasmosis reactivation in endemic areas should not be overlooked in this population. In a previous study, seroconversion to anti-histoplasmin antibodies by ELISA was detected in 6/39 (15.4%) patients with severe COVID-19. In this work, samples were further investigated to detect seroconversion to antibodies against the Histoplasma capsulatum 100-kDa antigen (Hcp100) by ELISA. Seroconversion to anti-Hcp100 antibodies was detected in 7/39 patients, of whom 6 also seroconverted anti-histoplasmin antibodies. These results reinforce previous findings that show histoplasmosis as an underdiagnosed fungal entity complicating COVID-19.
TESS and CHEOPS discover two warm sub-Neptunes transiting the bright K-dwarf HD 15906
Authors: Tuson A , Queloz D , Osborn H P , Wilson T G , Hooton M J , Beck M , Lendl M , Olofsson G , Fortier A , Bonfanti A , Brandeker A , Buchhave L A , Collier Cameron A , Ciardi D R , Collins K A , Gandolfi D , Garai Z , Giacalone S , Gomes da Silva J , Howell S B , Patel J A , Persson C M , Serrano L M , Sousa S G , Ulmer-Moll S , Vanderburg A , Ziegler C , Alibert Y , Alonso R , Anglada G , Bárczy T , Barrado Navascues D , Barros S C C , Baumjohann W , Beck T , Benz W , Billot N , Bonfils X , Borsato L , Broeg C , Cabrera J , Charnoz S , Conti D M , Csizmadia Sz , Cubillos P E , Davies M B , Deleuil M , Delrez L , Demangeon O D S , Demory B-O , Dragomir D , Dressing C D , Ehrenreich D , Erikson A , Essack Z , Farinato J , Fossati L , Fridlund M , Furlan E , Gill H , Gillon M , Gnilka C L , Gonzales E , Güdel M , Günther M N , Hoyer S , Isaak K G , Jenkins J M , Kiss L L , Laskar J , Latham D W , Law N , Lecavelier des Etangs A , Curto G Lo , Lovis C , Luque R , Magrin D , Mann A W , Maxted P F L , Mayor M , McDermott S , Mecina M , Mordasini C , Mortier A , Nascimbeni V , Ottensamer R , Pagano I , Pallé E , Peter G , Piotto G , Pollacco D , Pritchard T , Ragazzoni R , Rando N , Ratti F , Rauer H , Ribas I , Ricker G R , Rieder M , Santos N C , Savel A B , Scandariato G , Schwarz R P , Seager S , Ségransan D , Shporer A , Simon A E , Smith A M S , Steller M , Stockdale C , Szabó Gy M , Thomas N , Torres G , Tronsgaard R , Udry S , Ulmer B , Van Grootel V , Vanderspek R , Venturini J , Walton N A , Winn J N , Wohler B
Published: June 2023

We report the discovery of two warm sub-Neptunes transiting the bright (G = 9.5 mag) K-dwarf HD 15906 (TOI 461, TIC 4646810). This star was observed by the Transiting Exoplanet Survey Satellite (TESS) in sectors 4 and 31, revealing two small transiting planets. The inner planet, HD 15906 b, was detected with an unambiguous period but the outer planet, HD 15906 c, showed only two transits separated by ∼ 734 d, leading to 36 possible values of its period. We performed follow-up observations with the CHaracterising ExOPlanet Satellite (CHEOPS) to confirm the true period of HD 15906 c and improve the radius precision of the two planets. From TESS, CHEOPS, and additional ground-based photometry, we find that HD 15906 b has a radius of 2.24 ± 0.08 R⊕ and a period of 10.924709 ± 0.000032 d, whilst HD 15906 c has a radius of 2.93$^{+0.07}_{-0.06}$ R⊕ and a period of 21.583298$^{+0.000052}_{-0.000055}$ d. Assuming zero bond albedo and full day-night heat redistribution, the inner and outer planet have equilibrium temperatures of 668 ± 13 K and 532 ± 10 K, respectively. The HD 15906 system has become one of only six multiplanet systems with two warm (≲ 700 K) sub-Neptune sized planets transiting a bright star (G ≤ 10 mag). It is an excellent target for detailed characterization studies to constrain the composition of sub-Neptune planets and test theories of planet formation and evolution.
Halting migration in magnetospherically sculpted protoplanetary discs
Authors: Yu Tze Yeung Mathew , Hansen Brad , Hasegawa Yasuhiro
Published: June 2023

We present a physically motivated model for the manner in which a stellar magnetic field sculpts the inner edge of a protoplanetary disc, and examines the consequence for the migration and stopping of sub-Neptune and super-Earth planets. This model incorporates a transition zone exterior to the inner truncation of the disc, where the surface density profile is modified by the diffusion of the stellar magnetic field into the disc. This modification results in a migration trap at the outer edge of the transition zone. We performed simulations of single-planet migration, considering a range of stellar magnetic field strengths and magnetic diffusion profiles. Our simulations show a tight relationship between the final locations of planets and the total magnetic budget available for the disc from their host star. We found that a stellar magnetic field between 67 and 180 G and a power-law index between 3 and 2.75 can reasonably reproduce the location at which the observed occurrence rate of close-in super-Earth and sub-Neptune populations changes slope.
An escaping outflow in a galaxy with an intermediate-mass black hole
Authors: Zheng Zhiyuan , Shi Yong , Bian Fuyan , Yu Xiaoling , Wang Junfeng , Chen Jianhang , Li Xin , Gu Qiusheng
Published: June 2023

While in massive galaxies active galactic nucleus (AGN) feedback plays an important role, the role of AGN feedback is still under debate in dwarf galaxies. With well spatially resolved data obtained from the Multi-Unit Spectroscopic Explorer, we identify a spatially extended ($\rm \sim 3\,\, kpc$) and fast ($V_{80} \sim 471\,\, \rm km\,\,s^{-1}$) AGN-driven outflow in a dwarf galaxy: Sloan Digital Sky Survey J022849.51-090153.8 with $M_{*} \sim 10^{9.6}\,\,{\rm {\rm M}_{\odot }}$ that host an intermediate-mass black hole of $M_{\rm BH} \sim 10^5\,\,{\rm {\rm M}_{\odot }}$ and LAGN/LEdd ∼ 0.15. Through the measurement of the rotation curve, we estimate the escape velocity of the halo and the ratio of the outflow velocity to the halo escape velocity to be 1.09 ± 0.04, indicating that the outflow is capable of escaping not only the galaxy disc but the halo. The outflow size of our AGN is found to be larger than AGN in massive galaxies at the given AGN [O iii] luminosity, while the size of the photoionized narrow-line region is comparable. These results suggest the important role of AGN feedback through outflows in dwarf galaxies when their central intermediate-mass black holes accrete at high-Eddington ratios.
Rapid X-ray variability of the gamma-ray binary LS I +61°303
Authors: López-Miralles J , Motta Sara E , Migliari S , Jaron F
Published: June 2023

The gamma-ray binary LS I +61°303 has been widely monitored at different wavelengths since its discovery more than 60 yr ago. However, the nature of the compact object and the peculiar behaviour of the system are still largely debated. Aimed at investigating the rapid X-ray variability of LS I  +61°303, we have analysed all the archival Rossi X-ray Timing Explorer/Proportional Counter Array (RXTE/PCA) data of the source, taken between 1996 and 2011. The timing analysis yields a periodicity of P ∼ 26.6 ± 0.3 d, which is statistically compatible with several periodicities reported in the literature for LS I +61°303. Using this period, we performed a data phase-resolved analysis to produce a set of phase-bin-averaged energy spectra and power density spectra. These power density spectra are dominated by weak red noise below 0.1 Hz, and show no signal above this frequency. The amplitude of the red noise varies mildly with the phase, and shows a maximum that coincides with a dip of the X-ray flux and a softer photon index. Aside from low-frequency noise, this analysis does not provide any statistically significant periodic or quasi-periodic timing feature in the RXTE/PCA data of LS I  +61°303.
On the stability of relativistic two-component AGN jets
Authors: Sinnis Charalampos , Millas Dimitrios , Vlahakis Nektarios
Published: June 2023

A number of observations of astrophysical jets, at different scales, have shown that jets are often non-uniform outflows in their cross-section. Their structure is believed to play an important role in their overall stability. In this work, we combine analytical methods and numerical simulations to investigate the stability of non-uniform jets originating from active galactic nuclei. We adopt a standard ‘spine and sheath’ model, using a fast, light inner spine and a heavier, slower outer sheath. In the first part of this work, we conduct a linear stability analysis, finding the time-scales for the growth of the instabilities and the corresponding eigenfunctions. We focus on the nature of the physical processes that dominate and drive the destabilization of configurations. In the second part, we examine the evolution of the perturbed jets through relativistic 3D numerical simulations using the pluto code. Starting with the eigenfunctions found in the first part as initial conditions, we derive instability growth times and evolution which are in good agreement with the linear analysis.
Environments of red nuggets at z ∼ 0.7 from the VIPERS survey
Authors: Siudek M , Lisiecki K , Krywult J , Donevski D , Haines C P , Karska A , Małek K , Moutard T , Pollo A
Published: June 2023

Red ultra-compact massive galaxies, called red nuggets were formed at high redshifts (z ∼ 2–3). Survivors of red nuggets, known as relics, observed at lower redshifts (z < 2) are believed to remain almost unchanged since their formation. For the first time, we verify the environmental properties of red nuggets at intermediate redshift (0.5 < z < 0.9) using 42 red, massive (log(Mstar/M⊙) ≥ 10.9), and ultra compact (Re < 1.5 kpc) from the VIMOS Public Extragalactic Redshift Survey (VIPERS). We found that the increasing fraction of red galaxies, when moving to denser environments, is driven by the red massive normal-size galaxies. Red nuggets, similarly to red intermediate-mass (10.4 ≲ log (Mstar/M⊙) < 10.9) ultra-compact galaxies, are found in various types of environments, with consistent (within 1σ) fractions across all local densities. Analysis of red nugget stellar ages suggests that relics are preferably found in high-density regions while quiescent red nuggets are overabundant in low-density environments. We speculate that red nuggets have survived to lower redshifts via two channels: i) in low-density environments, where the fraction of red nuggets decreases as time passes due to (very) limited merger activity, ii) in high-density environments, where the number of red nuggets drops at higher redshift due to merger activity and is preserved at lower redshift as the high velocities of clusters prevent them from being cannibalized. Even more, the fraction of red nuggets in clusters may increase due to the addition of red massive normal-size galaxies deprived of their envelopes with cosmic time.
Probing quasar viewing angle with the variability structure function
Authors: Tang Ji-Jia , Wolf Christian , Tonry John , Lai Samuel , Yong Suk Yee , Steyn Zachary
Published: June 2023

Given the anisotropic emission from quasar accretion discs, their viewing angle affects estimates of the quasar luminosity, black hole mass, and Eddington ratio. Discs appear overluminous when viewed pole-on and underluminous when viewed at high inclination. In radio-quiet quasars, the viewing angle is usually unknown, although spectroscopic indicators have been proposed. Here, we use a recently discovered universality in the variability structure function (SF) of quasar light curves (LCs), where all quasars show the same SF when clocks run in units of orbital time-scale. As an offset from the mean relation can be caused by incorrect orbital time-scales and thus incorrect luminosities, we correlate these offsets with suggested inclination indicators. We derive SFs from NASA/Asteroid Terrestrial-impact Last Alert System (ATLAS) LCs spanning ∼6 yr of observation, using a sample of 183 luminous quasars with measured H β lines as well as 753 quasars with C iv and Mg ii lines. Starting from the proposed orientation indicators, we expect quasars with narrower H β lines and with more blueshifted C iv lines to be viewed more pole-on and thus appear overluminous. In contrast, our SF analysis finds that presumed pole-on discs appear underluminous, consistently for both line indicators. We discuss possible explanations for the behaviour of quasars with highly blueshifted C iv lines irrespective of inclination angle, including dusty outflows that might render the accretion disc underluminous and flatter disc temperature profiles with longer orbital time-scales than in thin-disc models but reach no satisfying conclusion.
Flaring latitudes in ensembles of low-mass stars
Authors: Ilin Ekaterina , Angus Ruth , Luger Rodrigo , Morris Brett M , Jehn Florian U
Published: June 2023

The distribution of small-scale magnetic fields in stellar photospheres is an important ingredient in our understanding of the magnetism of low-mass stars. Their spatial distribution connects the field generated in the stellar interior with the outer corona and the large scale field, and thereby affects the space weather of planets. Unfortunately, we lack techniques that can locate them on most low-mass stars. One strategy is to localize field concentrations using the flares that occur in their vicinity. We explore a new method that adapts the spot simulation software fleck to study the modulation of flaring times as a function of active latitude. We use empirical relations to construct flare light curves similar to those available from Kepler and the Transiting Exoplanet Survey Satellite (TESS), search them for flares, and use the waiting times between flares to determine the location of active latitudes. We find that the mean and standard deviations of the waiting time distribution provide a unique diagnostic of flaring latitudes as a function of the number of active regions. Latitudes are best recovered when stars have three or less active regions that flare repeatedly, and active latitude widths below 20 deg; when either increases, the information about the active latitude location is gradually lost. We demonstrate our technique on a sample of flaring G dwarfs observed with the Kepler satellite, and furthermore suggest that combining ensemble methods for spots and flares could overcome the limitations of each individual technique for the localization of surface magnetic fields.
How the dynamical properties of globular clusters impact their γ-ray and X-ray emission
Authors: de Menezes Raniere , Di Pierro Federico , Chiavassa Andrea
Published: June 2023

The X-ray and γ-ray emission of globular clusters (GCs) is attributed to their large fraction of compact binary systems, especially those with millisecond pulsars (MSPs). We analyse a population of 124 Galactic GCs to investigate how their dynamical properties affect the formation and evolution of compact binary systems and how this can be translated into the clusters’ observed X-ray and γ-ray emission. We use mainly Chandra X-ray Observatory and Fermi Large Area Telescope observations to achieve our goals and start by detecting 39 GCs in γ rays, seven of which are not listed in previous Fermi-LAT catalogs. Additionally, we find that the total number of X-ray sources within a GC and its γ-ray luminosity are linearly correlated with the stellar encounter rate, indicating that compact binary systems are mainly formed via close stellar encounters. We also find an unexpected rise in the number of X-ray sources for GCs with low rates of stellar encounters, suggesting that there is a dynamical threshold where the formation of X-ray sources is dominated by stellar encounters. Furthermore, we use the Heggie-Hills law to find that subsequent stellar encounters in these compact binaries will, on average, make the binaries even harder, with basically no possibility of binary ionization. Finally, we find that all GCs are point-like sources in γ rays, indicating that the MSPs are concentrated in the clusters’ cores, likely due to dynamical friction.
On the frequencies of circumbinary discs in protostellar systems
Authors: Elsender Daniel , Bate Matthew R , Lakeland Ben S , Jensen Eric L N , Lubow Stephen H
Published: June 2023

We report the analysis of circumbinary (CB) discs formed in a radiation hydrodynamical simulation of star cluster formation. We consider both pure binary stars and pairs within triple and quadruple systems. The protostellar systems are all young (ages < 105 yrs). We find that the systems that host a CB disc have a median separation of ≈11 au, and the median characteristic radius of the discs is ≈64 au. We find that 89 per cent of pure binaries with semimajor axes a < 1 au have a CB disc, and the occurrence rate of CB discs is bimodal with log-separation in pure binaries with a second peak at a ≈ 50 au. Systems with a > 100 au almost never have a CB disc. The median size of a CB disc is between ≈5 and 6 a depending on the order of the system, with higher order systems having larger discs relative to binary separation. We find the underlying distributions of mutual inclination between CB discs and binary orbits from the simulation are in good agreement with those of observed CB discs.
Uncovering the geometry of the hot X-ray corona in the Seyfert galaxy NGC 4151 with IXPE
Authors: Gianolli V E , Kim D E , Bianchi S , Agís-González B , Madejski G , Marin F , Marinucci A , Matt G , Middei R , Petrucci P-O , Soffitta P , Tagliacozzo D , Tombesi F , Ursini F , Barnouin T , De Rosa A , Di Gesu L , Ingram A , Loktev V , Panagiotou C , Podgorny J , Poutanen J , Puccetti S , Ratheesh A , Veledina A , Zhang W , Agudo I , Antonelli L A , Bachetti M , Baldini L , Baumgartner W H , Bellazzini R , Bongiorno S D , Bonino R , Brez A , Bucciantini N , Capitanio F , Castellano S , Cavazzuti E , Chen C-T , Ciprini S , Costa E , Del Monte E , Di Lalla N , Di Marco A , Donnarumma I , Doroshenko V , Dovčiak M , Ehlert S R , Enoto T , Evangelista Y , Fabiani S , Ferrazzoli R , García J A , Gunji S , Heyl J , Iwakiri W , Jorstad S G , Kaaret P , Karas V , Kislat F , Kitaguchi T , Kolodziejczak J J , Krawczynski H , La Monaca F , Latronico L , Liodakis I , Maldera S , Manfreda A , Marscher A P , Marshall H L , Massaro F , Mitsuishi I , Mizuno T , Muleri F , Negro M , Ng C-Y , O’Dell S L , Omodei N , Oppedisano C , Papitto A , Pavlov G G , Peirson A L , Perri M , Pesce-Rollins M , Pilia M , Possenti A , Ramsey B D , Rankin J , Roberts O J , Romani R W , Sgrò C , Slane P , Spandre G , Swartz D A , Tamagawa T , Tavecchio F , Taverna R , Tawara Y , Tennant A F , Thomas N E , Trois A , Tsygankov S S , Turolla R , Vink J , Weisskopf M C , Wu K , Xie F , Zane S
Published: June 2023

We present an X-ray spectropolarimetric analysis of the bright Seyfert galaxy NGC 4151. The source has been observed with the Imaging X-ray Polarimetry Explorer (IXPE) for 700 ks, complemented with simultaneous XMM–Newton (50 ks) and NuSTAR (100 ks) pointings. A polarization degree Π = 4.9 ± 1.1 per cent and angle Ψ = 86° ± 7° east of north (68 per cent confidence level) are measured in the 2–8 keV energy range. The spectropolarimetric analysis shows that the polarization could be entirely due to reflection. Given the low reflection flux in the IXPE band, this requires, however, a reflection with a very large (>38 per cent) polarization degree. Assuming more reasonable values, a polarization degree of the hot corona ranging from ∼4 to ∼8 per cent is found. The observed polarization degree excludes a ‘spherical’ lamppost geometry for the corona, suggesting instead a slab-like geometry, possibly a wedge, as determined via Monte Carlo simulations. This is further confirmed by the X-ray polarization angle, which coincides with the direction of the extended radio emission in this source, supposed to match the disc axis. NGC 4151 is the first active galactic nucleus with an X-ray polarization measure for the corona, illustrating the capabilities of X-ray polarimetry and IXPE in unveiling its geometry.
Prominence detection and chromosphere feature on the prototype RS CVn of active binary systems
Authors: Cao Dongtao , Gu Shenghong , Wolter U , Mittag M , Schmitt J H M M , Gao Dongyang , Hu Shaoming
Published: June 2023

We present a study of high-resolution spectra of RS Canum Venaticorum (RS CVn), a prototype of active binary systems. Our data were obtained from 1998 to 2017 using different telescopes. We analyse the chromospheric activity indicators $\rm{Ca~{\small II}}$ IRT, Hα, $\rm{Na~{\small I}}$ D1, D2 doublet, $\rm{He~{\small I}}$ D3, and Hβ using a spectral subtraction technique. The chromospheric emission stems mainly from the K2 IV primary star, while the F5 V secondary star only shows weak emission features in a few of our spectra. We find excess absorption features in the subtracted Hα lines and other activity indicators from spectra taken near primary eclipse, which we ascribe to prominence-like material associated with the primary star. We estimate size limits of these tentative prominences based on the geometry of the binary system, and investigate the physical properties of the strongest prominence. An optical flare, characterized by $\rm{He~{\small I}}$ D3 line emission, together with stronger emission in other activity lines, was detected. The flare energy is roughly comparable to strong flares observed on other RS CVn-type stars. The chromospherically active longitudes of RS CVn most frequently appear near the two quadratures of the system and display changes between observing runs, which indicates an ongoing evolution of its active regions.
High-z galaxies with JWST and local analogues – it is not only star formation
Authors: Brinchmann Jarle
Published: June 2023

I present an analysis of the JWST NIRSpec data of SMACS 0723 released as Early Release Observations. As part of this three new redshifts are provided, bringing the total of reliable redshifts to 14. I propose a modification to the direct abundance determination method that reduces sensitivity to flux calibration uncertainties by a factor of ∼3 and show that the resulting abundances are in good agreement with Bayesian photoionization models of the rest-frame optical spectrum. I also show that 6355 is most likely a narrow-line active galactic nucleus (AGN) with $M_*\lt 10^9\, \mathrm{M}_\odot$ at z = 7.66 and argue that 10 612 might also have an AGN contribution to its flux through comparison to photoionization models and low-redshift analogues. Under the assumption that the lines come from star formation, I find that the galaxies have gas depletion times of ∼107 yr, comparable to similar galaxies locally. I also identify a population of possibly shock-dominated galaxies at z < 3, whose near-IR emission lines plausibly come nearly all from shocks and discuss their implications. I close with a discussion of the potential for biases in the determination of the mass–metallicity relation using samples defined by detected [O iii]4363 and show using low-z galaxies that this can lead to biases of up to 0.5 dex with a systematic trend with mass.
LOFAR observations of gravitational wave merger events: O3 results and O4 strategy
Authors: Gourdji K , Rowlinson A , Wijers R A M J , Broderick J W , Shulevski A
Published: June 2023

The electromagnetic counterparts to gravitational wave (GW) merger events hold immense scientific value, but are difficult to detect due to the typically large localization errors associated with GW events. The Low-Frequency Array (LOFAR) is an attractive GW follow-up instrument owing to its high sensitivity, large instantaneous field of view, and ability to automatically trigger on events to probe potential prompt emission within minutes. Here, we report on 144-MHz LOFAR radio observations of three GW merger events containing at least one neutron star that were detected during the third GW observing run. Specifically, we probe 9 and 16 per cent of the location probability density maps of S190426c and S200213t, respectively, and place limits at the location of an interesting optical transient (PS19hgw/AT2019wxt) found within the localization map of S191213g. While these GW events are not particularly significant, we use multi-epoch LOFAR data to devise a sensitive wide-field GW follow-up strategy to be used in future GW observing runs. In particular, we improve on our previously published strategy by implementing direction-dependent calibration and mosaicing, resulting in nearly an order of magnitude increase in sensitivity and more uniform coverage. We achieve a uniform 5σ sensitivity of 870 μJy beam−1 across a single instantaneous LOFAR pointing’s 21 deg2 core, and a median sensitivity of 1.1 mJy beam−1 when including the full 89 deg2 hexagonal beam pattern. We also place the deepest transient surface density limits yet on time-scales of the order of month for surveys between 60 and 340 MHz (0.017 deg−2 above 2.0 mJy beam−1 and 0.073 deg−2 above 1.5 mJy beam−1).
Variability and evolution of the optical polarization of a sample of gamma-ray blazars
Authors: Otero-Santos J , Acosta-Pulido J A , González J Becerra , Raiteri C M , Carnerero M I , Segura N Castro , González-Martín O , Luashvili A
Published: June 2023

We present a polarization variability analysis of a sample of 26 γ-ray blazars monitored by the Steward Observatory between 2008 and 2018 in the optical band. We investigate the properties and long-term variability of their optical polarization, searching for differences between blazar types. We observe that BL Lac objects are typically less polarized and less variable than flat spectrum radio quasars (FSRQs). Moreover, BL Lacs display a distribution of their polarization angle typically oriented in a preferential direction, contrary to the rather random distribution of FSRQs. For the latter blazar type, as well as those sources showing a bright stellar emission, we take into account the depolarizing effect introduced by the broad line region and the host galaxy on the measured polarization degree. In this sample, we also observe that BL Lacs present an uncorrelated evolution of the flux and the polarization. Contrary, FSRQs show a correlation before the depolarization correction, that is lost however after considering this effect. In addition, we study the behaviour of the polarization angle, searching for angle rotations in its long-term evolution. We derive that the FSRQs studied here show rotations more frequently than BL Lac objects by a factor ∼1.5. During these periods, we also observe a systematic decrease of the polarization fraction, as well as a marginal flux increase, not significant however to connect rotations with optical flares. We interpret these results within the extended shock-in-jet scenario, able to explain the overall features observed here for the polarization of the blazar sample.
The relationship between the incidence of X-ray selected AGN in nearby galaxies & star-formation rate
Authors: Birchall Keir L , Watson M G , Aird J , Starling R L C
Published: June 2023

We present the identification and analysis of an X-ray selected AGN sample that lie within the local (z < 0.35) galaxy population. From a parent sample of 22 079 MPA-JHU (based on SDSS DR8) galaxies, we identified 917 galaxies with central, excess X-ray emission (from 3XMM-DR7) likely originating from an AGN. We measured the host galaxies’ star formation rates and classified them as either star-forming or quiescent based on their position relative to main sequence of star formation. Only 72 per cent of the X-ray selected sample were identified as AGN using BPT selection; this technique is much less effective in quiescent hosts, only identifying 50 per cent of the X-ray AGN. We also calculated the growth rates of the black holes powering these AGN in terms of their specific accretion rate (∝ LX/M*) and found quiescent galaxies, on average, accrete at a lower rate than star-forming galaxies. Finally, we measured the sensitivity function of 3XMM so we could correct for observational bias and construct probability distributions as a function of accretion rate. AGN were found in galaxies across the full range of star formation rates ($\log _{10} \, \mathrm{SFR/M_\odot \ yr^{-1}} = -3\ \mathrm{to}\ 2$) in both star-forming and quiescent galaxies. The incidence of AGN was enhanced by a factor 2 (at a 3.5σ significance) in star-forming galaxies compared to quiescent galaxies of equivalent stellar mass and redshift, but we also found a significant population of AGN hosted by quiescent galaxies.
Lopsided galaxies in a cosmological context: a new galaxy–halo connection
Authors: Varela-Lavin Silvio , Gómez Facundo A , Tissera Patricia B , Besla Gurtina , Garavito-Camargo Nicolás , Marinacci Federico , Laporte Chervin F P
Published: June 2023

Disc galaxies commonly show asymmetric features in their morphology, such as warps and lopsidedness. These features can provide key information regarding the recent evolution of a given disc galaxy. In the nearby Universe, up to ∼30 per cent of late-type galaxies display a global non-axisymmetric lopsided mass distribution. However, the origin of this perturbation is not well understood. In this work, we study the origin of lopsided perturbations in simulated disc galaxies extracted from the TNG50 simulation of the IllustrisTNG project. We statistically explore different excitation mechanisms for this perturbation, such as direct satellite tidal interactions and distortions of the underlying dark matter distributions. We also characterize the main physical conditions that lead to lopsided perturbations. 50 per cent of our sample galaxy have lopsided modes m = 1 greater than ∼0.12. We find a strong correlation between internal galaxy properties, such as central stellar surface density and disc radial extension with the strength of lopsided modes. The majority of lopsided galaxies have lower central surface densities and more extended discs than symmetric galaxies. As a result, such lopsided galaxies are less self-gravitationally cohesive, and their outer disc region is more susceptible to different types of external perturbations. However, we do not find strong evidence that tidal interactions with satellite galaxies are the main driving agent of lopsided modes. Lopsided galaxies tend to live in asymmetric dark matter haloes with high spin, indicating strong galaxy–halo connections in late-type lopsided galaxies.
Classifying IGR J15038−6021 as a magnetic CV with a massive white dwarf
Authors: Tomsick John A , Kumar Snehaa Ganesh , Coughenour Benjamin M , Shaw Aarran W , Mukai Koji , Hare Jeremy , Clavel Maïca , Krivonos Roman , Fornasini Francesca M , Gerber Julian , Joens Alyson
Published: June 2023

Cataclysmic variables (CVs) are binary systems consisting of a white dwarf (WD) accreting matter from a companion star. Observations of CVs provide an opportunity to learn about accretion discs, the physics of compact objects, classical novae, and the evolution of the binary and the WD that may ultimately end in a Type Ia supernova (SN). As Type Ia SNe involve a WD reaching the Chandrasekhar limit or merging WDs, WD mass measurements are particularly important for elucidating the path from CV to Type Ia SN. For intermediate polar (IP) type CVs, the WD mass is related to the bremsstrahlung temperature of material in the accretion column, which typically peaks at X-ray energies. Thus, the IPs with the strongest hard X-ray emission, such as those discovered by the INTEGRAL satellite, are expected to have the highest masses. Here, we report on XMM–Newton, Nuclear Spectroscopic Telescope Array (NuSTAR), and optical observations of IGR J15038−6021. We find an X-ray periodicity of 1678 ± 2 s, which we interpret as the WD spin period. From fitting the 0.3–79 keV spectrum with a model that uses the relationship between the WD mass and the post-shock temperature, we measure a WD mass of $1.36^{+0.04}_{-0.11}$ M⊙. This follows an earlier study of IGR J14091−6108, which also has a WD with a mass approaching the Chandrasekhar limit. We demonstrate that these are both outliers among IPs in having massive WDs and discuss the results in the context of WD mass studies as well as the implications for WD mass evolution.
SIRT1 regulates DNA damage signaling through the PP4 phosphatase complex
Authors: Rasti George , Becker Maximilian , Vazquez Berta N , Espinosa-Alcantud Maria , Fernández-Duran Irene , Gámez-García Andrés , Ianni Alessandro , Gonzalez Jessica , Bosch-Presegué Laia , Marazuela-Duque Anna , Guitart-Solanes Anna , Segura-Bayona Sandra , Bech-Serra Joan-Josep , Scher Michael , Serrano Lourdes , Shankavaram Uma , Erdjument-Bromage Hediye , Tempst Paul , Reinberg Danny , Olivella Mireia , Stracker Travis H , de la Torre Carolina , Vaquero Alejandro
Published: June 2023

The Sirtuin family of NAD+-dependent enzymes plays an important role in maintaining genome stability upon stress. Several mammalian Sirtuins have been linked directly or indirectly to the regulation of DNA damage during replication through Homologous recombination (HR). The role of one of them, SIRT1, is intriguing as it seems to have a general regulatory role in the DNA damage response (DDR) that has not yet been addressed. SIRT1-deficient cells show impaired DDR reflected in a decrease in repair capacity, increased genome instability and decreased levels of γH2AX. Here we unveil a close functional antagonism between SIRT1 and the PP4 phosphatase multiprotein complex in the regulation of the DDR. Upon DNA damage, SIRT1 interacts specifically with the catalytical subunit PP4c and promotes its inhibition by deacetylating the WH1 domain of the regulatory subunits PP4R3α/β. This in turn regulates γH2AX and RPA2 phosphorylation, two key events in the signaling of DNA damage and repair by HR. We propose a mechanism whereby during stress, SIRT1 signaling ensures a global control of DNA damage signaling through PP4.
The 3D chromatin landscape of rhabdomyosarcoma
Authors: Wang Meng , Sreenivas Prethish , Sunkel Benjamin D , Wang Long , Ignatius Myron , Stanton Benjamin Z
Published: June 2023

Rhabdomyosarcoma (RMS) is a pediatric soft tissue cancer with a lack of precision therapy options for patients. We hypothesized that with a general paucity of known mutations in RMS, chromatin structural driving mechanisms are essential for tumor proliferation. Thus, we carried out high-depth in situ Hi-C in representative cell lines and patient-derived xenografts (PDXs) to define chromatin architecture in each major RMS subtype. We report a comprehensive 3D chromatin structural analysis and characterization of fusion-positive (FP-RMS) and fusion-negative RMS (FN-RMS). We have generated spike-in in situ Hi-C chromatin interaction maps for the most common FP-RMS and FN-RMS cell lines and compared our data with PDX models. In our studies, we uncover common and distinct structural elements in large Mb-scale chromatin compartments, tumor-essential genes within variable topologically associating domains and unique patterns of structural variation. Our high-depth chromatin interactivity maps and comprehensive analyses provide context for gene regulatory events and reveal functional chromatin domains in RMS.
Unbundling Property in Welfare
Authors: Cohen-Rimer Yael , Stern Shai
Published: June 2023

In most Western jurisdictions, welfare law utilises means testing to determine whether individuals are eligible for welfare allowances, often using property ownership as one of the eligibility criteria. Crucially, the prevailing conception of property ownership is premised on the notion that property rights are applied equally to all owners in matters relating to the control and management of that property. When this assumption proves not to reflect reality, it can have devastating consequences for those most in need of the support ostensibly provided by welfare law. The present qualitative empirical study examines two cases in which such adverse consequences are felt: in the two largest minority communities in Israel—the Palestinians and the Ultraorthodox Jews (Charedi). The findings show that property ownership in these communities is realised hierarchically, along patriarchal lines, and that family members occupy and manage property in accordance with community customs and traditional norms, often far removed from state laws. Beyond theoretical debates or ethnographic observations, the discrepancies between the state’s ideas of ownership and those recognised by members of the Palestinian and Charedi communities in Israel often result in the denial of financial aid to those who need it most. This article will identify such differences in conception and will describe how they provide an additional explanation for the high levels of poverty in minority communities. Finally, it will examine two private law doctrines that can be used as inspiration to better interpret welfare law and make it more nuanced and culturally sensitive, especially when it encounters people in poverty and marginalised groups.
Sport-related concussion and bodychecking in children and youth: Evaluation, management, and policy implications
Authors: Goulet Kristian , Beno Suzanne
Published: June 2023

Concussions are a common injury both within and outside sport and recreational settings, and they remain a serious concern for children and youth. Any young person suspected of sustaining a concussion should be medically evaluated as soon as possible, and when the injury occurs during sport, the individual must be removed from play immediately to avoid secondary injury. A brief initial period of physical and cognitive rest is followed by supervised, stepwise return-to-learn and return-to-play protocols. All individuals involved in child and youth sports and recreation must be able to recognize risk for, and signs and symptoms of, concussion. They must also ensure that any participant suspected of sustaining a concussion is properly evaluated and managed by qualified medical personnel. Evolving data and literature have strengthened both our pathophysiological understanding of concussion and guidance for clinical management, especially related to acute care, persistent symptoms, and prevention. This statement also re-examines the relationship between bodychecking in hockey and injury rates, and advocates for a change in policy in youth hockey.
Spinal cord injury and prescribed opioids for pain: a scoping review
Authors: Shoup Jo Ann , Welter JoEllen , Binswanger Ingrid A , Hess Florian , Dullenkopf Alexander , Coker Jennifer , Berliner Jeffrey
Published: June 2023

Objective

Spinal cord injury (SCI) is a life-altering neurological condition affecting physical and psycho-social functioning and associated high rates of pain. Thus, individuals with SCI may be more likely to be exposed to prescription opioids. A scoping review was conducted to synthesize published research findings on post-acute SCI and prescription opioid use for pain, identify literature gaps, and propose recommendations for future research.

Methods

We searched 6 electronic bibliographic databases (PubMed [MEDLINE], Ovid [MEDLINE], EMBASE, Cochrane Library, CINAHL, PsychNET) for articles published from 2014 through 2021. Terms for “spinal cord injury” and “prescription opioid use” were used. Included articles were in English and peer reviewed. Data were extracted using an electronic database by 2 independent reviewers. Opioid use risk factors for chronic SCI were identified and a gap analysis was performed.

Results

Of the 16 articles included in the scoping review, a majority were conducted in the United States (n = 9). Most articles lacked information on income (87.5%), ethnicity (87.5%), and race (75%). Prescription opioid use ranged from 35% to 64% in articles reporting this information (n = 7 articles, n = 3675 participants). Identified risk factors for opioid use included middle age, lower income, osteoarthritis diagnosis, prior opioid use, and lower-level spinal injury. Limited reporting of diversity in study populations, absence of risk of polypharmacy, and limited high quality methodology were identified gaps.

Conclusions

Future research should report data on prescription opioid use in SCI populations, with additional demographics such as race, ethnicity, and income, given their importance to risk outcomes.
Low-dose naltrexone’s utility for non-cancer centralized pain conditions: a scoping review
Authors: Rupp Adam , Young Erin , Chadwick Andrea L
Published: June 2023

Background

At low doses, naltrexone (LDN) has been shown to modulate inflammation through the interruption of microglial cell activation within the central nervous system. One of the most likely contributors to centralized pain is changes in microglial cell processing. Therefore, it has been postulated that LDN can be used to manage patients with pain resulting from central sensitization due to this relationship. This scoping review aims to synthesize the relevant study data for LDN as a novel treatment strategy for various centralized pain conditions.

Methods

A comprehensive literature search was conducted in PubMed, Embase, and Google Scholar, guided by the Scale for Assessment of Narrative Review Articles (SANRA) criteria.

Results

Forty-seven studies related to centralized pain conditions were identified. Many of the studies were case reports/series and narrative reviews, but a few randomized control trials have been conducted. Overall, the body of evidence revealed improvement in patient-reported pain severity and in outcomes related to hyperalgesia, physical function, quality of life, and sleep. Variability in dosing paradigms and the time to patient response was present in the reviewed studies.

Conclusions

Evidence synthesized for this scoping review supports the ongoing use of LDN for the treatment of refractory pain in various centralized chronic pain conditions. Upon review of the currently available published studies, it is apparent that further high-quality, well-powered randomized control trials need to be conducted to establish efficacy, standardization for dosing, and response times. In summary, LDN continues to offer promising results in the management of pain and other distressing symptoms in patients with chronic centralized pain conditions.
Nociceptive flexion reflex in small fibers neuropathy and pain assessments
Authors: Ser Merve Hazal , Yılmaz Basak , Sulu Cem , Gönen Mustafa Sait , Gunduz Aysegul
Published: June 2023

Background

The nociceptive flexion reflex (NFR) is a polysynaptic and multisegmental spinal reflex that develops in response to a noxious stimulus and is characterized by the withdrawal of the affected body part. The NFR possesses two excitatory components: early RII and late RIII. Late RIII is derived from high-threshold cutaneous afferent A-delta fibers, which are prone to injury early in the course of diabetes mellitus (DM) and may lead to neuropathic pain. We investigated NFR in patients with DM with different types of polyneuropathies to analyze the role of NFR in small fiber neuropathy (SFN).

Methods

We included 37 patients with DM and 20 healthy participants of similar age and sex. We performed the Composite Autonomic Neuropathy Scale-31, modified Toronto Neuropathy Scale, and routine nerve conduction studies. We grouped the patients into large fiber neuropathy (LFN), SFN, and no overt neurological symptom/sign groups. In all participants, NFR was recorded on anterior tibial (AT) and biceps femoris (BF) muscles after train stimuli on the sole of the foot, and NFR-RIII findings were compared.

Results

We identified 11 patients with LFN, 15 with SFN, and 11 with no overt neurological symptoms or signs. The RIII response on the AT was absent in 22 (60%) patients with DM and 8 (40%) healthy participants. The RIII response on the BF was absent in 31 (73.8%) patients and 7 (35%) healthy participants (P = .001). In DM, the latency of RIII was prolonged, and the magnitude was reduced. Abnormal findings were seen in all subgroups; however, they were more prominent in patients with LFN compared to other groups.

Conclusions

The NFR-RIII was abnormal in patients with DM even before the emergence of the neuropathic symptoms. The pattern of involvement before neuropathic symptoms was possibly related to an earlier loss of A-delta fibers.
Conditions for the stable adsorption of lipid monolayers to solid surfaces
Authors: Šako Marin , Staniscia Fabio , Schneck Emanuel , Netz Roland R , Kanduč Matej
Published: June 2023

Lipid monolayers are ubiquitous in biological systems and have multiple roles in biotechnological applications, such as lipid coatings that enhance colloidal stability or prevent surface fouling. Despite the great technological importance of surface-adsorbed lipid monolayers, the connection between their formation and the chemical characteristics of the underlying surfaces has remained poorly understood. Here, we elucidate the conditions required for stable lipid monolayers nonspecifically adsorbed on solid surfaces in aqueous solutions and water/alcohol mixtures. We use a framework that combines the general thermodynamic principles of monolayer adsorption with fully atomistic molecular dynamics simulations. We find that, very universally, the chief descriptor of adsorption free energy is the wetting contact angle of the solvent on the surface. It turns out that monolayers can form and remain thermodynamically stable only on substrates with contact angles above the adsorption contact angle, θads. Our analysis establishes that θads falls into a narrow range of around 60∘–70∘ in aqueous media and is only weakly dependent on the surface chemistry. Moreover, to a good approximation, θads is roughly determined by the ratio between the surface tensions of hydrocarbons and the solvent. Adding small amounts of alcohol to the aqueous medium lowers θads and thereby facilitates monolayer formation on hydrophilic solid surfaces. At the same time, alcohol addition weakens the adsorption strength on hydrophobic surfaces and results in a slowdown of the adsorption kinetics, which can be useful for the preparation of defect-free monolayers.