bluuebunny/crossref_metadata_2025_split huggingface dataset:
In vitro cross-resistance to doravirine in a panel of HIV-1 clones harbouring multiple NNRTI resistance mutations
Authors: Saladini Francesco , Giammarino Federica , Hosseini Behnaz A , Giannini Alessia , Boccuto Adele , Dragoni Filippo , Vicenti Ilaria , Shafer Robert W , Zazzi Maurizio 
Published: September 2020

Abstract

Objectives
Doravirine is a recently licensed HIV-1 NNRTI with improved efficacy, pharmacokinetics and safety profile compared with efavirenz and limited cross-resistance with rilpivirine and etravirine. In this in vitro study, cross-resistance to doravirine was analysed in a representative panel of NNRTI-resistant clones.

Methods
In vitro phenotypic susceptibility to doravirine was assessed in 10 clinically derived infectious clones with intermediate- to high-level resistance to rilpivirine, etravirine, efavirenz and nevirapine, and in NL4-3 site-directed mutants harbouring K103N, Y181C, M230L or K103N/Y181C NNRTI mutations.

Results
Although none of the infectious clones harboured any of the major doravirine resistance-associated mutations (RAMs) included in the IAS-USA reference list, doravirine fold change (FC) values were comparable to or higher than those calculated for other NNRTIs, particularly etravirine and rilpivirine. As expected, single NNRTI mutations K103N and Y181C did not impair doravirine susceptibility (FC 1.4 and 1.8, respectively), while reduced activity was observed with the single M230L or double K103N/Y181C mutations (FC 7.6 and 4.9, respectively). Median FC values increased significantly with increasing numbers of NNRTI RAMs (P = 0.005) and were &gt;10 in 4/4 and 1/4 clones harbouring four and three NNRTI RAMs, respectively. FC values correlated well with predicted susceptibility as inferred by Stanford HIV Drug Resistance Database (HIVdb) and ANRS algorithms (both P &lt; 0.001).

Conclusions
Substantial cross-resistance to doravirine was detected in NNRTI-resistant viruses harbouring complex mutational patterns, even in the absence of major IAS-USA doravirine RAMs. Therefore, based on the simple IAS-USA reference list, doravirine resistance may be underestimated in viruses harbouring multiple NNRTI mutations.
The Opposites and Unity: A Study of Chinese Taoist Thought Found in Hermann Hesse’s The Glass Bead Game
Authors: Tang Xianyun , Zheng Boren 
Published: September 2020

Abstract
Hermann Hesse was keenly aware of the spiritual and social crises of war-torn Europe. He explored possible solutions to these problems in his writing and was interested in drawing on the resources of oriental philosophies. Of particular importance was the thought of Chinese Taoism. Hesse frequently mentioned his understanding of the Taoist philosophies of Laozi (老子) and Zhuangzi (庄子) in letters to his friends, and Taoist ideas such as ‘Tao’ (道) or ‘One’ and ‘polar opposites and unity’ recur across his work. This article will trace Hesse’s understanding of the Taoist thought of Laozi and Zhuangzi, and analyse the influence of Chinese Taoism on Hesse’s masterpiece, The Glass Bead Game (1943).
The use of the t-test in Shakespeare scholarship
Authors: Rizvi Pervez 
Published: September 2020

Abstract
In a recent article, the New Oxford Shakespeare scholar Hugh Craig used the t-test in statistics to compare the uses of one hundred function words across plays, authors, genres, characters, and periods in Shakespeare’s era. Craig drew some strong conclusions; for example, that authorship is a greater differentiator between plays than genre. Using both theoretical arguments and the results of further experiments, this note challenges Craig’s analysis, showing that he applied the t-test even when it is not clear that its premises are satisfied, failed to apply necessary controls, and, moreover, that his reasoning contains a fundamental error which invalidates his interpretation of the results.
Be X-ray binaries in the SMC as indicators of mass-transfer efficiency
Authors: Vinciguerra Serena , Neijssel Coenraad J , Vigna-Gómez Alejandro , Mandel Ilya , Podsiadlowski Philipp , Maccarone Thomas J , Nicholl Matt , Kingdon Samuel , Perry Alice , Salemi Francesco 
Published: September 2020

ABSTRACT
Be X-ray binaries (BeXRBs) consist of rapidly rotating Be stars with neutron star (NS) companions accreting from the circumstellar emission disc. We compare the observed population of BeXRBs in the Small Magellanic Cloud (SMC) with simulated populations of BeXRB-like systems produced with the compas population synthesis code. We focus on the apparently higher minimal mass of Be stars in BeXRBs than in the Be population at large. Assuming that BeXRBs experienced only dynamically stable mass transfer, their mass distribution suggests that at least $\sim 30{{\ \rm per\ cent}}$ of the mass donated by the progenitor of the NS is typically accreted by the B-star companion. We expect these results to affect predictions for the population of double compact object mergers. A convolution of the simulated BeXRB population with the star formation history of the SMC shows that the excess of BeXRBs is most likely explained by this galaxy’s burst of star formation ∼20–40 Myr ago.
Active gas features in three HSC-SSP CAMIRA clusters revealed by high angular resolution analysis of MUSTANG-2 SZE and XXL X-ray observations
Authors: Okabe Nobuhiro , Dicker Simon , Eckert Dominique , Mroczkowski Tony , Gastaldello Fabio , Lin Yen-Ting , Devlin Mark , Romero Charles E , Birkinshaw Mark , Sarazin Craig , Horellou Cathy , Kitayama Tetsu , Umetsu Keiichi , Sereno Mauro , Mason Brian S , ZuHone John A , Honda Ayaka , Akamatsu Hiroki , Chiu I-Non , Kohno Kotaro , Lin Kai-Yang , Medezinski Elinor , Miyazaki Satoshi , Mitsuishi Ikuyuki , Nishizawa Atsushi J , Oguri Masamune , Ota Naomi , Pacaud Florian , Pierre Marguerite , Sievers Jonathan , Smolčić Vernesa , Stanchfield Sara , Tanaka Keigo , Yamamoto Ryoichi , Yang Chong , Yoshida Atsushi 
Published: September 2020

ABSTRACT
We present results from simultaneous modelling of high angular resolution GBT/MUSTANG-2 90 GHz Sunyaev–Zel’dovich effect (SZE) measurements and XMM-XXL X-ray images of three rich galaxy clusters selected from the HSC-SSP Survey. The combination of high angular resolution SZE and X-ray imaging enables a spatially resolved multicomponent analysis, which is crucial to understand complex distributions of cluster gas properties. The targeted clusters have similar optical richnesses and redshifts, but exhibit different dynamical states in their member galaxy distributions: a single-peaked cluster, a double-peaked cluster, and a cluster belonging to a supercluster. A large-scale residual pattern in both regular Compton-parameter y and X-ray surface brightness distributions is found in the single-peaked cluster, indicating a sloshing mode. The double-peaked cluster shows an X-ray remnant cool core between two SZE peaks associated with galaxy concentrations. The temperatures of the two peaks reach ∼20–30 keV in contrast to the cool core component of ∼2 keV, indicating a violent merger. The main SZE signal for the supercluster is elongated along a direction perpendicular to the major axis of the X-ray core, suggesting a minor merger before core passage. The SX and y distributions are thus perturbed at some level, regardless of the optical properties. We find that the integrated Compton y parameter and the temperature for the major merger are boosted from those expected by the weak-lensing mass and those for the other two clusters show no significant deviations, which is consistent with predictions of numerical simulations.
Overdensity of SMGs in fields containing z ∼ 0.3 galaxies: magnification bias and the implications for studies of galaxy evolution
Authors: Dunne L , Bonavera L , Gonzalez-Nuevo J , Maddox S J , Vlahakis C 
Published: September 2020

ABSTRACT
We report a remarkable overdensity of high-redshift submillimetre galaxies (SMG), 4–7 times the background, around a statistically complete sample of twelve 250 μm selected galaxies at z = 0.35, which were targeted by ALMA in a study of gas tracers. This overdensity is consistent with the effect of lensing by the haloes hosting the target z = 0.35 galaxies. The angular cross-correlation in this sample is consistent with statistical measures of this effect made using larger sub-mm samples. The magnitude of the overdensity as a function of radial separation is consistent with intermediate scale lensing by haloes of the order of $7\times 10^{13}\mbox{ $\rm M_{\odot }$ }$, which should host one or possibly two bright galaxies and several smaller satellites. This is supported by observational evidence of interaction with satellites in four out of the six fields with SMG, and membership of a spectroscopically defined group for a fifth. We also investigate the impact of these SMG on the reported Herschel fluxes of the z = 0.35 galaxies, as they produce significant contamination in the 350 and 500 μm Herschel bands. The higher than random incidence of these boosting events implies a significantly larger bias in the sub-mm colours of Herschel sources associated with z &lt; 0.7 galaxies than has previously been assumed, with fboost = 1.13, 1.26, 1.44 at 250, 350, and 500 μm . This could have implications for studies of spectral energy distributions, source counts, and luminosity functions based on Herschel samples at z = 0.2–0.7.
Turbulence-induced deviation between baryonic field and dark matter field in the spatial distribution of the Universe
Authors: Yang Hua-Yu , He Ping , Zhu Weishan , Feng Long-Long 
Published: September 2020

ABSTRACT
The cosmic baryonic fluid at low redshifts is similar to a fully developed turbulence. In this work, we use simulation samples produced by the hybrid cosmological hydrodynamical/N-body code, to investigate on what scale the deviation of spatial distributions between baryons and dark matter is caused by turbulence. For this purpose, we do not include the physical processes such as star formation, supernovae (SNe), and active galactic nucleus (AGN) feedback into our code, so that the effect of turbulence heating for IGM can be exhibited to the most extent. By computing cross-correlation functions rm(k) for the density field and rv(k) for the velocity field of both baryons and dark matter, we find that deviations between the two matter components for both density field and velocity field, as expected, are scale-dependent. That is, the deviations are the most significant at small scales and gradually diminish on larger and larger scales. Also, the deviations are time-dependent, i.e. they become larger and larger with increasing cosmic time. The most emphasized result is that the spatial deviations between baryons and dark matter revealed by velocity field are more significant than that by density field. At z = 0, at the $1{{\ \rm per\ cent}}$ level of deviation, the deviation scale is about $3.7\, {h^{-1} {\rm Mpc}}$ for density field, while as large as $23\, {h^{-1} {\rm Mpc}}$ for velocity field, a scale that falls within the weakly non-linear regime for the structure formation paradigm. Our results indicate that the effect of turbulence heating is indeed comparable to that of these processes such as SN and AGN feedback.
On the first δ Sct–roAp hybrid pulsator and the stability of p and g modes in chemically peculiar A/F stars
Authors: Murphy Simon J , Saio Hideyuki , Takada-Hidai Masahide , Kurtz Donald W , Shibahashi Hiromoto , Takata Masao , Hey Daniel R 
Published: September 2020

ABSTRACT
Strong magnetic fields in chemically peculiar A-type (Ap) stars typically suppress low-overtone pressure modes (p modes) but allow high-overtone p modes to be driven. KIC 11296437 is the first star to show both. We obtained and analysed a Subaru spectrum, from which we show that KIC 11296437 has abundances similar to other magnetic Ap stars, and we estimate a mean magnetic field modulus of 2.8 ± 0.5 kG. The same spectrum rules out a double-lined spectroscopic binary, and we use other techniques to rule out binarity over a wide parameter space, so the two pulsation types originate in one δ Sct–roAp hybrid pulsator. We construct stellar models depleted in helium and demonstrate that helium settling is second to magnetic damping in suppressing low-overtone p modes in Ap stars. We compute the magnetic damping effect for selected p and g modes, and find that modes with frequencies similar to the fundamental mode are driven for polar field strengths ≲4 kG, while other low-overtone p modes are driven for polar field strengths up to ∼1.5 kG. We find that the high-order g modes commonly observed in γ Dor stars are heavily damped by polar fields stronger than 1–4 kG, with the damping being stronger for higher radial orders. We therefore explain the observation that no magnetic Ap stars have been observed as γ Dor stars. We use our helium-depleted models to calculate the δ Sct instability strip for metallic-lined A (Am) stars, and find that driving from a Rosseland mean opacity bump at ∼5 × 104 K caused by the discontinuous H-ionization edge in bound-free opacity explains the observation of δ Sct pulsations in Am stars.
Physical conditions of five O vi absorption systems towards PG 1522+101
Authors: Sankar Sriram , Narayanan Anand , Savage Blair D , Khaire Vikram , Rosenwasser Benjamin E , Charlton Jane , Wakker Bart P 
Published: September 2020

ABSTRACT
We present the analysis of five O vi absorbers identified across a redshift path of z ∼ (0.6−1.3) towards the background quasar PG 1522+101 with information on five consecutive ionization stages of oxygen from O ii to O vi. The combined HST and Keck spectra cover UV, redshifted extreme-UV, and optical transitions from a multitude of ions spanning ionization energies in the range of ∼(13−300) eV. Low-ionization (C ii, O ii, Si ii, Mg ii) and very high-ionization species (Ne viii, Mg x) are non-detections in all the absorbers. Three of the absorbers have coverage of He i, in one of which it is a &gt;3σ detection. The kinematic structures of these absorbers are extracted from C iv detected in HIRES spectra. The farthest absorber in our sample also contains the detections of Ne v and Ne vi. Assuming co-spatial absorbing components, the ionization models show the medium to be multiphased with small-scale density–temperature inhomogeneities that are sometimes kinematically unresolved. In two of the absorbers, there is an explicit indication of the presence of a warm gas phase (T ≳ 105 K) traced by O vi. In the remaining absorbers, the column densities of the ions are consistent with a non-uniform photoionized medium. The subsolar [C/O] relative abundances inferred for the absorbers point at enrichment from massive Type II supernovae. Despite metal enrichment, the inferred wide range for [O/H] ∼ [−2.1, +0.2] amongst the absorbers along with their anticorrelation with the observed H i suggest poor small-scale mixing of metals with hydrogen in the regions surrounding galaxies and the IGM.
Joint galaxy–galaxy lensing and clustering constraints on galaxy formation
Authors: Renneby Malin , Henriques Bruno M B , Hilbert Stefan , Nelson Dylan , Vogelsberger Mark , Angulo Raúl E , Springel Volker , Hernquist Lars 
Published: September 2020

ABSTRACT
We compare predictions for galaxy–galaxy lensing profiles and clustering from the Henriques et al. public version of the Munich semi-analytical model (SAM) of galaxy formation and the IllustrisTNG suite, primarily TNG300, with observations from KiDS + GAMA and SDSS-DR7 using four different selection functions for the lenses (stellar mass, stellar mass and group membership, stellar mass and isolation criteria, and stellar mass and colour). We find that this version of the SAM does not agree well with the current data for stellar mass-only lenses with $M_\ast \gt 10^{11}\, \mathrm{ M}_\odot$. By decreasing the merger time for satellite galaxies as well as reducing the radio-mode active galactic nucleus accretion efficiency in the SAM, we obtain better agreement, both for the lensing and the clustering, at the high-mass end. We show that the new model is consistent with the signals for central galaxies presented in Velliscig et al. Turning to the hydrodynamical simulation, TNG300 produces good lensing predictions, both for stellar mass-only (χ2 = 1.81 compared to χ2 = 7.79 for the SAM) and locally brightest galaxy samples (χ2 = 3.80 compared to χ2 = 5.01). With added dust corrections to the colours it matches the SDSS clustering signal well for red low-mass galaxies. We find that both the SAMs and TNG300 predict $\sim 50\, {{\ \rm per\ cent}}$ excessive lensing signals for intermediate-mass red galaxies with 10.2 &lt; log10M*[M⊙] &lt; 11.2 at $r \approx 0.6\, h^{-1}\, \text{Mpc}$, which require further theoretical development.
A revision of the vdB 130 cluster stellar content based on Gaia DR2 data: interstellar extinction toward the Cyg OB1 supershell
Authors: Sitnik T G , Rastorguev A S , Tatarnikova A A , Tatarnikov A M , Egorov O V , Tatarnikov A A 
Published: September 2020

ABSTRACT
Two star-forming regions are studied: the young embedded open cluster vdB 130 and the protocluster neighbourhood observed in the head and tail of the cometary molecular cloud located in the wall of the expanding supershell surrounding the Cyg OB1 association. The Gaia DR2 catalogue is employed to verify the stellar composition of the vdB 130 cluster whose members were earlier selected using the UCAC4 catalogue. The new sample of vdB 130 members contains 68 stars with close proper motions (within 1 mas yr−1) and close trigonometric parallaxes (ranging from 0.50–0.70 mas). The relative parallax error is shown to increase with distance to objects and depend on their magnitude. At a distance of 1.5–2 kpc it is of about 3–7 per cent and 20–30 per cent for bright and faint stars, respectively. The cluster is not older than ∼10 Myr. New spectroscopic and photometric observations carried out on Russian telescopes are combined with Gaia DR2 to search for optical components in the protocluster region – a new starburst. An analysis of 20 stars in the vicinity of the protocluster revealed no concentration of either proper motions or parallaxes. According to spectroscopic, photometric and trigonometric estimates, the distances to these stars range from 0.4–2.5 kpc, and colour excess is shown to increase with a distance D (kpc) in accordance with the law E(B − V) ≃ 0.6 × D mag.
Morphometric analysis of brightest cluster galaxies
Authors: Cougo J , Rembold S B , Ferrari F , Kaipper A L P 
Published: September 2020

ABSTRACT
We study the build-up of the stellar mass of brightest cluster galaxies (BCGs) at z &lt; 0.1 as a function of their morphological type. Morphometric parameters for 1216 BCGs were obtained from the SDSS DR12 r-band images with the code morfometryka. We show that the morphometric parameters are efficient to separate BCGs into cD galaxies, conventional ellipticals, disc-dominated BCGs, and merging objects. We propose a simple classification scheme using two concentration indices, C1 and C2, and the spirality σψ. We then investigate how the stellar masses of BCGs and the velocity dispersions of their parent haloes relate to their morphological properties. We find that BCGs with larger envelope contributions are more massive than BCGs in other classes and more common in massive clusters. The stellar mass and the halo velocity dispersion correlate for all classes, suggesting that environmental effects are important for BCGs of any morphology. At fixed parent halo mass, we detect a continuous mass excess up to $\sim 60{{\ \rm per\ cent}}$ from pure E galaxies to extreme cD galaxies, while the inner regions of such cDs present only $\sim 40{{\ \rm per\ cent}}$ of the mass of an E galaxy. We interpret our findings in a scenario where different BCGs have developed their mass through an asymmetric combination of distinct processes, so that present-time cD galaxies have grown in mass mainly through minor merging and tidal stripping from satellite galaxies, while elliptical BCGs evolve mainly through processes like major merging.
On the magnetoionic environments of fast radio bursts
Authors: Wang Wei-Yang , Zhang Bing , Chen Xuelei , Xu Renxin 
Published: September 2020

ABSTRACT
Observations of the Faraday rotation measure, combined with the dispersion measure, can be used to infer the magnetoionic environment of a radio source. We investigate the magnetoionic environments of fast radio bursts (FRBs) by deriving their estimated average magnetic field strengths along the line of sight 〈B∥〉 in their host galaxies and comparing them with those of Galactic pulsars and magnetars. We find that for those FRBs with RM measurements, the mean 〈B∥〉 are $1.77^{+9.01}_{-1.48}\, \rm \mu G$ and $1.74^{+14.82}_{-1.55}\, \rm \mu G$ using two different methods, which is slightly larger but not inconsistent with the distribution of Galactic pulsars, $1.00^{+1.51}_{-0.60}\, \rm \mu G$. Only six Galactic magnetars have estimated 〈B∥〉. Excluding PSR J1745–2900 that has an anomalously high value due to its proximity with the Galactic Centre, the other five sources have a mean value of $1.70\, \rm \mu G$, which is statistically consistent with the 〈B∥〉 distributions of both Galactic pulsars and FRBs. There is no apparent trend of evolution of magnetar 〈B∥〉 as a function of age or surface magnetic field strength. Galactic pulsars and magnetars close to the Galactic Centre have relatively larger 〈B∥〉 values than other pulsars/magnetars. We discuss the implications of these results for the magnetoionic environments of FRB 121102 within the context of magnetar model and the model invoking a supermassive black hole, and for the origin of FRBs in general.
Specific suppression of D-RNA G-quadruplex–protein interaction with an L-RNA aptamer
Authors: Umar Mubarak I , Kwok Chun Kit 
Published: September 2020

Abstract
G-quadruplexes (G4s) are nucleic acid structure motifs that are of significance in chemistry and biology. The function of G4s is often governed by their interaction with G4-binding proteins. Few categories of G4-specific tools have been developed to inhibit G4–protein interactions; however, until now there is no aptamer tool being developed to do so. Herein, we present a novel L-RNA aptamer that can generally bind to D-RNA G-quadruplex (rG4) structure, and interfere with rG4–protein interaction. Using hTERC rG4 as the target for in vitro selection, we report the shortest L-aptamer being developed so far, with only 25 nucleotides. Notably, this new aptamer, L-Apt.4-1c, adopts a stem–loop structure with the loop folding into an rG4 motif with two G-quartet, demonstrates preferential binding toward rG4s over non-G4s and DNA G-quadruplexes (dG4s), and suppresses hTERC rG4–nucleolin interactions. We also show that inhibition of rG4–protein interaction using L-RNA aptamer L-Apt.4-1c is comparable to or better than G4-specific ligands such as carboxypyridostatin and QUMA-1 respectively, highlighting that our approach and findings expand the current G4 toolbox, and open a new avenue for diverse applications.