bluuebunny/crossref_metadata_2025_split huggingface dataset:
‘Meeting Together in an Equal and Friendly Manner’: The Workplace Literary Culture of Lancashire Mutual Improvement Societies
Authors: Weiss Lauren 
Published: May 2023

Abstract
This article traces the progress of mutual improvement in the coalfields around Aspull beginning in the 1870s and culminating with the opening of the Garswood Hall Collieries Institute in 1893. It analyses this process in relation to Patrick Joyce’s account of the development of industrial paternalism in Lancashire. It shows how mutual improvement societies were formed primarily on the initiative of individual workers, with some assistance from local religious groups, rather than being employer-led. It also demonstrates how the Aspull Society acted as the starting point for a network of similar societies across the local area. By tracing the careers of a number of individuals closely associated with mutual improvement societies, this article shows that such societies did enable occupational and social mobility, thereby demonstrating the virtues of self-help to workers and employers alike. Next, the article traces the factors which led to the opening of the Garswood Hall Collieries Institute and argues that the formation of the Institute exemplifies the delicate social choreography on which the successful practice of paternalism in an industrial context depended. It demonstrates that local autonomous activity on the part of individual miners was combined with the use of local newspapers and delegations to employers to create the conditions for an appropriate paternalist response in the form of the ‘gift’ of the Institute to the community. The Institute thus became a demonstration of the employers’ fitness to exercise local leadership and a symbol of education as a means of achieving class harmony within the existing social hierarchy. It concludes by observing that in the case of the Garswood Hall Collieries Institute the vision of class harmony which it offered its members nonetheless remained vulnerable to the economic realities of the relationship between capital and labour.
A blue depression in the optical spectra of M dwarfs
Authors: Jones Hugh R A , Pavlenko Yakiv , Lyubchik Yuri , Bessell Mike , Allard Nicole , Pinfield David J 
Published: May 2023

ABSTRACT
A blue depression is found in the spectra of M dwarfs from 4000 to 4500 Å. This depression shows an increase towards lower temperatures, though it is particularly sensitive to gravity and metallicity. It is the single strongest and most sensitive feature in the optical spectra of M dwarfs. The depression appears as centred on the neutral calcium resonance line at 4227 Å and leads to nearby features being weaker by about two orders of magnitude than predicted. We consider a variety of possible causes for the depression, including temperature, gravity, metallicity, dust, damping constants, and atmospheric stratification. We also consider relevant molecular opacities that might be the cause identifying AlH, SiH, and NaH in the spectral region. However, none of these solutions are satisfactory. In the absence of a more accurate determination of the broadening of the calcium line perturbed by molecular hydrogen, we find a promising empirical fit using a modified Lorentzian line profile for the calcium resonance line. Such fits provide a simplistic line-broadening description for this calcium resonance line and potentially other unmodelled resonance lines in cool high-pressure atmospheres. Thus, we claim that the most plausible cause of the blue depression in the optical spectra of M dwarfs is a lack of appropriate treatment of line broadening for atomic calcium. The broad wings of the calcium resonance line develop at temperatures below about 4000 K and are analogous to the neutral sodium and potassium features, which dominate the red optical spectra of L dwarfs.
The dark side of FIRE: predicting the population of dark matter subhaloes around Milky Way-mass galaxies
Authors: Barry Megan , Wetzel Andrew , Chapman Sierra , Samuel Jenna , Sanderson Robyn , Arora Arpit 
Published: May 2023

ABSTRACT
A variety of observational campaigns seek to test dark matter models by measuring dark matter subhaloes at low masses. Despite their predicted lack of stars, these subhaloes may be detectable through gravitational lensing or via their gravitational perturbations on stellar streams. To set measurable expectations for subhalo populations within Lambda cold dark matter, we examine 11 Milky Way (MW)-mass haloes from the FIRE-2 baryonic simulations, quantifying the counts and orbital fluxes for subhaloes with properties relevant to stellar stream interactions: masses down to $10^{6}\, \text{M}_\odot$, distances ≲50 kpc of the galactic centre, across z = 0 − 1 (tlookback = 0–8 Gyr). We provide fits to our results and their dependence on subhalo mass, distance, and lookback time, for use in (semi)analytical models. A typical MW-mass halo contains ≈16 subhaloes $\gt 10^{7}\, \text{M}_\odot$ (≈1 subhalo $\gt 10^{8}\, \text{M}_\odot$) within 50 kpc at z ≈ 0. We compare our results with dark matter-only versions of the same simulations: because they lack a central galaxy potential, they overpredict subhalo counts by 2–10×, more so at smaller distances. Subhalo counts around a given MW-mass galaxy declined over time, being ≈10× higher at z = 1 than at z ≈ 0. Subhaloes have nearly isotropic orbital velocity distributions at z ≈ 0. Across our simulations, we also identified 4 analogues of Large Magellanic Cloud satellite passages; these analogues enhance subhalo counts by 1.4–2.1 times, significantly increasing the expected subhalo population around the MW today. Our results imply an interaction rate of ∼5 per Gyr for a stream like GD-1, sufficient to make subhalo–stream interactions a promising method of measuring dark subhaloes.
Systematics in asteroseismic modelling: application of a correlated noise model for oscillation frequencies
Authors: Li Tanda , Davies Guy R , Nielsen Martin , Cunha Margarida S , Lyttle Alexander J 
Published: May 2023

ABSTRACT
The detailed modelling of stellar oscillations is a powerful approach to characterizing stars. However, poor treatment of systematics in theoretical models leads to misinterpretations of stars. Here, we propose a more principled statistical treatment for the systematics to be applied to fitting individual mode frequencies with a typical stellar model grid. We introduce a correlated noise model based on a Gaussian process (GP) kernel to describe the systematics given that mode frequency systematics are expected to be highly correlated. We show that tuning the GP kernel can reproduce general features of frequency variations for changing model input physics and fundamental parameters. Fits with the correlated noise model better recover stellar parameters than traditional methods that either ignore the systematics or treat them as uncorrelated noise.
Multiwavelength variability of γ-ray emitting narrow-line Seyfert 1 galaxies
Authors: Yao Su , Komossa S 
Published: May 2023

ABSTRACT
As one of the drivers of feedback in active galactic nuclei (AGNs), the jets launched from supermassive black holes (SMBHs) are important for understanding the co-evolution of SMBHs and their host galaxies. However, the formation of AGN jets is far from clear. The discovery of γ-ray narrow-line Seyfert 1 (NLS1) galaxies during the past two decades has provided us with a new means of studying the link between jets and accretion processes and the formation of jets. Here, we explore the coupling of jet and accretion discs in seven bright γ-ray NLS1 galaxies by studying simultaneous optical/ultraviolet and X-ray observations of these systems taken by Swift. The results show that, except for 1H 0323+342 in which the X-rays are significantly contributed from the accretion disc, the observed X-ray emission of the other sources is dominated by the jet, and accretion process makes little contribution if not absent. Although the origin of the X-ray emission is different, the broad-band spectral shape characterized by αox and the X-ray flux is found to follow the same evolutionary trend in 1H 0323+342, PMN J0948+0022, and PKS 1502+036. For the remaining sources, the trend is not observed or the sampling is not dense enough.
NGC 1436: the making of a lenticular galaxy in the Fornax Cluster
Authors: Loni Alessandro , Serra Paolo , Sarzi Marc , Józsa Gyula I G , Anta Pablo M Galán-de , Zabel Nikki , Kleiner Dane , Maccagni Filippo M , Molnár Daniel , Ramatsoku Mpati , Loi Francesca , Corsini Enrico M , Pisano D J , Kamphuis Peter , Davis Timothy A , de Blok W J G , Dettmar Ralf J , Falcon-Barroso Jesus , Iodice Enrichetta , Lara-López Maritza A , Loubser S Ilani , Morokuma-Matsui Kana , Peletier Reynier , Pinna Francesca , Poci Adriano , Smith Matthew W L , Trager Scott C , van de Ven Glenn 
Published: May 2023

ABSTRACT
We study the evolutionary path of the Fornax Cluster galaxy NGC 1436, which is known to be currently transitioning from a spiral into a lenticular morphology. This galaxy hosts an inner star-forming disc and an outer quiescent disc, and we analyse data from the MeerKAT Fornax Survey, ALMA, and the Fornax 3D survey to study the interstellar medium and the stellar populations of both disc components. Thanks to the combination of high resolution and sensitivity of the MeerKAT data, we find that the H i is entirely confined within the inner star-forming disc, and that its kinematics is coincident with that of the CO. The cold gas disc is now well settled, which suggests that the galaxy has not been affected by any environmental interactions in the last ∼1 Gyr. The star-formation history derived from the Fornax 3D data shows that both the inner and outer discs experienced a burst of star formation ∼5 Gyr ago, followed by rapid quenching in the outer disc and by slow quenching in the inner disc, which continues forming stars to this day. We claim that NGC 1436 has begun to effectively interact with the cluster environment 5 Gyr ago, when a combination of gravitational and hydrodynamical interactions caused the temporary enhancement of the star-formation rate. Furthermore, due to the weaker gravitational binding H i was stripped from the outer disc, causing its rapid quenching. At the same time, accretion of gas onto the inner disc stopped, causing slow quenching in this region.
A test of invariance of dark matter halo surface density using multiwavelength mock galaxy catalogues
Authors: Gopika K , Desai Shantanu , Paranjape Aseem 
Published: May 2023

ABSTRACT
A large number of observations have shown that the dark matter halo surface density, given by the product of halo core radius and core density, is nearly constant for a diverse suite of galaxies. Although this invariance of the halo surface density is violated at galaxy cluster and group scales, it is still an open question on whether the aforementioned constancy on galactic scales can be explained within Lambda cold dark matter (ΛCDM). For this purpose, we probe the variation of halo surface density as a function of mass using multiwavelength mock galaxy catalogues from ΛCDM simulations, where the adiabatic contraction of dark matter haloes in the presence of baryons has been taken into account. We find that these baryonified ΛCDM haloes were best fitted with a generalized Navarro–Frenk–White profile, and the halo surface density from these haloes has a degeneracy with respect to both the halo mass and the virial concentration. We find that the correlation with mass when averaged over concentration is consistent with a constant halo surface density. However, a power-law dependence as a function of halo mass also cannot be ruled out.
Imprint of magnetic obliquity in apparent spin-down of radio pulsars
Authors: Biryukov Anton , Beskin Gregory 
Published: May 2023

ABSTRACT
Numerical simulations predict that the spin-down rate of a single rotation-powered neutron star depends on the angle α between its spin and magnetic axes as $P\dot{P} \propto \mu ^2 (k_0 + k_1\sin ^2\alpha)$, where P is the star spin period, μ is its magnetic moment, while k0 ∼ k1 ∼ 1. Here, we describe a simple observational test for this prediction based on the comparison of spin-down rates of 50 nearly orthogonal (with α close to 90 deg) and 27 nearly aligned (with α close to 0 deg) pulsars. We found, that the apparent pulsar spin-down is consistent with the theory if assumed, that magnetic moments of orthogonal rotators are systematically larger than those of aligned ones for ∼0.15...0.2 dex. Also, as a by-product of the analysis, we provide yet another constraint on the average braking index of radio pulsars as 1 ≤ n ≤ 4 with formal significance not worse than 99 per cent.
DMPP-3: confirmation of short-period S-type planet(s) in a compact eccentric binary star system, and warnings about long-period RV planet detections
Authors: Stevenson Adam T , Haswell Carole A , Barnes John R , Barstow Joanna K , Ross Zachary O B 
Published: May 2023

ABSTRACT
We present additional HARPS radial velocity observations of the highly eccentric (e ∼ 0.6) binary system DMPP-3AB, which comprises a K0V primary and a low-mass companion at the hydrogen burning limit. The binary has a 507 d orbital period and a 1.2 au semimajor axis. The primary component harbours a known 2.2 M⊕ planet, DMPP-3A b, with a 6.67-d orbit. New HARPS measurements constrain periastron passage for the binary orbit and add further integrity to previously derived solutions for both companion and planet orbits. Gaia astrometry independently confirms the binary orbit and establishes the inclination of the binary is 63.89 ± 0.78°. We performed dynamical simulations that establish that the previously identified ∼800 d RV signal cannot be attributed to an orbiting body. The additional observations, a deviation from strict periodicity, and our new analyses of activity indicators suggest the ∼800 d signal is caused by stellar activity. We conclude that there may be long-period planet ‘detections’ in other systems, which are similar misinterpreted stellar activity artefacts. Without the unusual eccentric binary companion to the planet-hosting star, we could have accepted the ∼800 d signal as a probable planet. Further monitoring of DMPP-3 will reveal which signatures can be used to most efficiently identify these imposters. We also report a threshold detection (0.2 per cent FAP) of a ∼2.26 d periodicity in the RVs, potentially attributed to an Earth-mass S-type planet interior to DMPP-3A b.
One EURO for Uranus: the Elliptical Uranian Relativity Orbiter mission
Authors: Iorio Lorenzo , Girija Athul Pradeepkumar , Durante Daniele 
Published: May 2023

ABSTRACT
Recent years have seen increasing interest in sending a mission to Uranus, visited so far only by Voyager 2 in 1986. Elliptical Uranian Relativity Orbiter is a preliminary mission concept investigating the possibility of dynamically measuring the planet’s angular momentum by means of the Lense–Thirring effect affecting a putative Uranian orbiter. It is possible, at least in principle, to separate the relativistic precessions of the orbital inclination to the celestial equator and of the longitude of the ascending node of the spacecraft from its classical rates of the pericentre induced by the multipoles of the planet’s gravity field by adopting an appropriate orbital configuration. For a wide and elliptical $2000\times 100\, 000\, \mathrm{km}$ orbit, the gravitomagnetic signatures amount to tens of milliarcseconds per year, while, for a suitable choice of the initial conditions, the peak-to-peak amplitude of the range-rate shift can reach the level of ≃ 1.5 × 10−3 mm s−1 in a single pericentre passage of a few hours. By lowering the apocentre height to $10\, 000\, \mathrm{km}$, the Lense–Thirring precessions are enhanced to the level of hundreds of milliarcseconds per year. The uncertainties in the orientation of the planetary spin axis and in the inclination are major sources of systematic bias; it turns out that they should be determined with accuracies as good as ≃0.1–1 and ≃1–10 mas, respectively.
Discovery of double Hall pattern associated with collisionless magnetic reconnection in dusty plasmas
Authors: Yang Shu-Di , Wang Liang , Dong Chuanfei 
Published: May 2023

ABSTRACT
Magnetic reconnection is prevalent in magnetized plasmas in space and laboratories. Despite significant investigations on reconnection in electron–ion plasmas, studies of reconnection in magnetized plasmas with negatively charged dust grains are quite sparse. Here, we report the first fully kinetic simulations of collisionless reconnection in a three-species (i.e. electron, proton, and negatively charged dust grain) dusty plasma, through which the discovery of double Hall pattern is made. The double Hall pattern consists of a traditional Hall quadruple current in between the ion and electron diffusion region and a reversed Hall current in between the boundary of the ion and dust diffusion region. The analysis of the reconnection rate is also given. This study may be applicable to explain observations of planetary magnetospheres and the astrophysical objects, and may be realized in the laboratory studies of dusty plasmas.
Non-parametric reconstruction of photon escape fraction from reionization
Authors: Mitra Sourav , Chatterjee Atrideb 
Published: May 2023

ABSTRACT
One of the most crucial yet poorly constrained parameters in modelling the ionizing emissivity is the escape fraction of photons from star-forming galaxies. Several theoretical and observational studies have been conducted over the past few years, but consensus regarding its redshift evolution has yet to be achieved. We present here the first non-parametric reconstruction of this parameter as a function of redshift from a data-driven reionization model using a Gaussian Process Regression method. Our finding suggests a mild redshift evolution of escape fraction with a mean value of $4~{{\ \rm per\ cent}},7~{{\ \rm per\ cent}},\sim 10~{{\ \rm per\ cent}}$ at $z$ = 2, 6, 12. However, a constant escape fraction of $6-10~{{\ \rm per\ cent}}$ at $z$ ≳ 6 is still allowed by current data and also matches other reionization-related observations. With the detection of fainter high-redshift galaxies from upcoming observations of JWST, the approach presented here will be a robust tool to put the most stringent constraint on escape fraction as well as reionization histories.
DNA binding specificity of all four Saccharomyces cerevisiae forkhead transcription factors
Authors: Cooper Brendon H , Dantas Machado Ana Carolina , Gan Yan , Aparicio Oscar M , Rohs Remo 
Published: May 2023

Abstract
Quantifying the nucleotide preferences of DNA binding proteins is essential to understanding how transcription factors (TFs) interact with their targets in the genome. High-throughput in vitro binding assays have been used to identify the inherent DNA binding preferences of TFs in a controlled environment isolated from confounding factors such as genome accessibility, DNA methylation, and TF binding cooperativity. Unfortunately, many of the most common approaches for measuring binding preferences are not sensitive enough for the study of moderate-to-low affinity binding sites, and are unable to detect small-scale differences between closely related homologs. The Forkhead box (FOX) family of TFs is known to play a crucial role in regulating a variety of key processes from proliferation and development to tumor suppression and aging. By using the high-sequencing depth SELEX-seq approach to study all four FOX homologs in Saccharomyces cerevisiae, we have been able to precisely quantify the contribution and importance of nucleotide positions all along an extended binding site. Essential to this process was the alignment of our SELEX-seq reads to a set of candidate core sequences determined using a recently developed tool for the alignment of enriched k-mers and a newly developed approach for the reprioritization of candidate cores.
Hi-TrAC detects active sub-TADs and reveals internal organizations of super-enhancers
Authors: Cao Yaqiang , Liu Shuai , Cui Kairong , Tang Qingsong , Zhao Keji 
Published: May 2023

AbstractThe spatial folding of eukaryotic genome plays a key role in genome function. We report here that our recently developed method, Hi-TrAC, which specializes in detecting chromatin loops among accessible genomic regions, can detect active sub-TADs with a median size of 100 kb, most of which harbor one or two cell specifically expressed genes and regulatory elements such as super-enhancers organized into nested interaction domains. These active sub-TADs are characterized by highly enriched histone mark H3K4me1 and chromatin-binding proteins, including Cohesin complex. Deletion of selected sub-TAD boundaries have different impacts, such as decreased chromatin interaction and gene expression within the sub-TADs or compromised insulation between the sub-TADs, depending on the specific chromatin environment. We show that knocking down core subunit of the Cohesin complex using shRNAs in human cells or decreasing the H3K4me1 modification by deleting the H3K4 methyltransferase Mll4 gene in mouse Th17 cells disrupted the sub-TADs structure. Our data also suggest that super-enhancers exist as an equilibrium globule structure, while inaccessible chromatin regions exist as a fractal globule structure. In summary, Hi-TrAC serves as a highly sensitive and inexpensive approach to study dynamic changes of active sub-TADs, providing more explicit insights into delicate genome structures and functions.
Breeze 2.0: an interactive web-tool for visual analysis and comparison of drug response data
Authors: Potdar Swapnil , Ianevski Filipp , Ianevski Aleksandr , Tanoli Ziaurrehman , Wennerberg Krister , Seashore-Ludlow Brinton , Kallioniemi Olli , Östling Päivi , Aittokallio Tero , Saarela Jani 
Published: May 2023

Abstract
Functional precision medicine (fPM) offers an exciting, simplified approach to finding the right applications for existing molecules and enhancing therapeutic potential. Integrative and robust tools ensuring high accuracy and reliability of the results are critical. In response to this need, we previously developed Breeze, a drug screening data analysis pipeline, designed to facilitate quality control, dose-response curve fitting, and data visualization in a user-friendly manner. Here, we describe the latest version of Breeze (release 2.0), which implements an array of advanced data exploration capabilities, providing users with comprehensive post-analysis and interactive visualization options that are essential for minimizing false positive/negative outcomes and ensuring accurate interpretation of drug sensitivity and resistance data. The Breeze 2.0 web-tool also enables integrative analysis and cross-comparison of user-uploaded data with publicly available drug response datasets. The updated version incorporates new drug quantification metrics, supports analysis of both multi-dose and single-dose drug screening data and introduces a redesigned, intuitive user interface. With these enhancements, Breeze 2.0 is anticipated to substantially broaden its potential applications in diverse domains of fPM.