bluuebunny/crossref_metadata_2025_split huggingface dataset:
A Response to Mohja Kahf
Authors: Majaj Lisa Suhair 
Published: July 2024

Abstract
This response, written from a Palestinian American perspective, takes seriously Mohja Kahf’s call to hold ourselves responsible for making visible Indigenous realities instead of eliding them; for recognizing implicit, even if unwilled, complicity; and for thinking and acting decolonially. Bringing attention to the contradictions inherent in the political and personal stances of Arab Americans who critique settler colonialism in Palestine but fail to attend to the colonialism defining their own locations in North America, it affirms the need to see and act on processes of erasure—including those we may have unwittingly participated in—across different colonial contexts. Drawing on the intellectual framing of reciprocal intercommunalism and its imperatives for inter-group solidarities and ethical humanism, as well as on personal experience, it discusses points of connection between US and Palestinian settler colonialisms: not only the parallel histories of colonization and expulsion but also the discursive processes used to justify these legacies of destruction. Making these connections visible helps us to not only position ourselves more responsibly in relation to Indigenous histories but also develop a theoretical lexicon and intellectual framework for decolonial struggles applicable more widely. One example of this is the concept of memoricide—the physical destruction and discursive silencing of history and memory—and the correlating decolonial strategy of de-memoricide: asserting the reality of the erased past and in so doing helping to shape a different future. The response concludes with attention to Kahf’s poem “Samidun on the West Bank of the Mississippi,” which brilliantly evokes and portrays strategies of intercommunalism, self-critique, and the stance of inquiry and receptiveness necessary for true decolonial solidarity.
Misaligned precessing jets are choked by the accretion disc wind
Authors: Lu Wenbin , Matsumoto Tatsuya , Matzner Christopher D 
Published: July 2024

ABSTRACT
We analytically and numerically study the hydrodynamic propagation of a precessing jet in the context of tidal disruption events (TDEs) where the star’s angular momentum is misaligned with the black hole spin. We assume that a geometrically thick accretion disc undergoes Lense–Thirring precession around the black hole spin axis and that the jet is aligned with the instantaneous disc angular momentum. At large spin-orbit misalignment angles $\theta _{\it LS}$, the duty cycle along a given angle that the jet sweeps across is much smaller than unity. The faster jet and slower disc wind alternately fill a given angular region, which leads to strong shock interactions between the two. We show that precessing jets can only break out of the wind confinement if $\theta _{\it LS}$ is less than a few times the jet opening angle $\theta _{\rm j}$. The very small event rate of observed jetted TDEs is then explained by the condition of double alignment: both the stellar angular momentum and the observer’s line of sight are nearly aligned with the black hole spin. In most TDEs with $\theta _{\it LS}\gg \theta _{\rm j}$, the jets are initially choked by the disc wind and may only break out later when the disc eventually aligns itself with the spin axis due to the viscous damping of the precession. Such late-time jets may produce delayed radio rebrightening as seen in many optically bright TDEs. Our model is also applicable to jets associated with (stellar mass) black hole-neutron star mergers where the black hole’s spin is misaligned with the orbital angular momentum.
Constraining the duration of ram pressure stripping features in the optical from the direction of jellyfish galaxy tails
Authors: Salinas Vicente , Jaffé Yara L , Smith Rory , Shinn Jong-Ho , Crossett Jacob P , Gullieuszik Marco , González-Torà Gemma , Piraino-Cerda Franco , Poggianti Bianca , Vulcani Benedetta , Biviano Andrea , Lourenço Ana C C , Bilton Lawrence E , Kelkar Kshitija , Calderón-Castillo Paula 
Published: July 2024

ABSTRACT
Ram pressure stripping is perhaps the most efficient mechanism for removing gas and quenching galaxies in dense environments, as they move through the intergalactic medium. Extreme examples of on-going ram pressure stripping are known as jellyfish galaxies, characterized by a tail of stripped material that can be directly observed in multiple wavelengths. Using the largest homogeneous broad-band optical jellyfish candidate sample in local clusters known to date, we measure the angle between the direction of the tails visible in the galaxies, and the direction towards the host cluster centre. We find that 33 per cent of the galaxy tails point away from the cluster centre, 18 per cent point towards the cluster centre, and 49 per cent point elsewhere. Moreover, we find stronger signatures of ram pressure stripping happening on galaxies with a tail pointing away and towards the cluster centre, and larger velocity dispersion profiles for galaxies with tails pointing away. These results are consistent with a scenario where ram pressure stripping has a stronger effect for galaxies following radial orbits on first infall. The results also suggest that in many cases, radially infalling galaxies are able to retain their tails after pericenter and continue to experience significant on-going ram pressure stripping. We further constrain the lifespan of the optical tails from the moment they first appear to the moment they disappear, by comparing the observed tail directions with matched N-body simulations through Bayesian parameter estimation. We obtain that galaxy tails appear for the first time at $\sim 1.16$R$_{200}$ and disappear $\sim 660$ Myr after pericenter.
The beyond-halo mass effects of the cosmic web environment on galaxies
Authors: Wang Kuan , Avestruz Camille , Guo Hong , Wang Wei , Wang Peng 
Published: July 2024

ABSTRACT
Galaxy properties primarily depend on their host halo mass. Halo mass, in turn, depends on the cosmic web environment. We explore if the effect of the cosmic web on galaxy properties is entirely transitive via host halo mass, or if the cosmic web has an effect independent of mass. The secondary galaxy bias, sometimes referred to as ‘galaxy assembly bias’, is the beyond-mass component of the galaxy–halo connection. We investigate the link between the cosmic web environment and the secondary galaxy bias in simulations. We measure the secondary galaxy bias through the following summary statistics: projected two-point correlation function, $w_{\mathrm{p}}(r_{\mathrm{p}})$, and counts-in-cylinders statistics, $P(N_{\mathrm{CIC}})$. First, we examine the extent to which the secondary galaxy bias can be accounted for with a measure of the environment as a secondary halo property. We find that the total secondary galaxy bias preferentially places galaxies in more strongly clustered haloes. In particular, haloes at fixed mass tend to host more galaxies when they are more strongly associated with nodes or filaments. This tendency accounts for a significant portion, but not the entirety, of the total secondary galaxy bias effect. Secondly, we quantify how the secondary galaxy bias behaves differently depending on the host halo proximity to nodes and filaments. We find that the total secondary galaxy bias is relatively stronger in haloes more associated with nodes or filaments. We emphasize the importance of removing halo mass effects when considering the cosmic web environment as a factor in the galaxy–halo connection.
Turbocharging constraints on dark matter substructure through a synthesis of strong lensing flux ratios and extended lensed arcs
Authors: Gilman Daniel , Birrer Simon , Nierenberg Anna , Oh Maverick S H 
Published: July 2024

ABSTRACT
Strong gravitational lensing provides a purely gravitational means to infer properties of dark matter haloes and thereby constrain the particle nature of dark matter. Strong lenses sometimes appear as four lensed images of a background quasar accompanied by spatially resolved emission from the quasar host galaxy encircling the main deflector (lensed arcs). We present methodology to simultaneously reconstruct lensed arcs and relative image magnifications (flux ratios) in the presence of full populations of subhaloes and line-of-sight haloes. To this end, we develop a new approach for multiplane ray tracing that accelerates lens mass and source light reconstruction by factors of $\sim\!\! 100\!\!-\!\!1000$. Using simulated data, we show that simultaneous reconstruction of lensed arcs and flux ratios isolates small-scale perturbations to flux ratios by dark matter substructure from uncertainties associated with the main deflector mass profile on larger angular scales. Relative to analyses that use only image positions and flux ratios to constrain the lens model, incorporating arcs strengthens likelihood ratios penalizing warm dark matter with a suppression scale $m_{\rm {hm}} / {\rm M}_{\odot }$ in the ranges of $\left[10^7 \!\!-\!\! 10^{7.5}\right]$, $\left[10^{7.5} \!\!-\!\! 10^{8}\right]$, $\left[10^8 \!\!-\!\! 10^{8.5}\right]$, and $\left[10^{8.5} \!\!-\!\! 10^{9}\right]$ by factors of 1.3, 2.5, 5.6, and 13.1, respectively, for a cold dark matter ground truth. The 95 per cent exclusion limit improves by 0.5 dex in $\log _{10} m_{\rm {hm}}$. The enhanced sensitivity to low-mass haloes enabled by these methods pushes the observational frontier of substructure lensing to the threshold of galaxy formation, enabling stringent tests of any theory that alters the properties of dark matter haloes.
Tribocharged solids in protoplanetary discs: internal and external discharge time-scales
Authors: Becker T , Völke G , Steinpilz T , Onyeagusi F C , Teiser J , Wurm G 
Published: July 2024

ABSTRACT
Particles regularly tribocharge in collisions. Here, we study how long charges can persist on such particles in the environment of a protoplanetary disc. We set up three complementary experiments to quantify discharge time-scales. We first directly measure the time dependency of charge on triboelectrically charged objects. For this aspect, we performed two long-time experiments under different environmental conditions. We find that the charge persists on the tribocharged bodies on time-scales between minutes and years. Discharge might be mediated by external ions or internally, by conduction. To constrain the latter, we also determined the specific electric resistance of dust samples as simulants for dust aggregates in protoplanetary discs. In this third experiment, we see an increase in resistivity at decreasing ambient pressure up to the limit of the instrument. These findings are consistent with the assumption that water on all relevant surfaces including dust grains within the pore space of aggregates is the main driver of discharge. Under disc conditions, the charge might persist for weeks to years. This leaves net-charged isolated grains in dense parts of the mid-plane of protoplanetary discs charged in between collisions.
AGN-driven outflows in clumpy media: multiphase structure and scaling relations
Authors: Ward S R , Costa T , Harrison C M , Mainieri V 
Published: July 2024

ABSTRACT
Small-scale winds driven from accretion discs surrounding active galactic nuclei (AGN) are expected to launch kpc-scale outflows into their host galaxies. However, the ways in which the structure of the interstellar medium (ISM) affects the multiphase content and impact of the outflow remain uncertain. We present a series of numerical experiments featuring a realistic small-scale AGN wind with velocity $5\times 10^3 \!-\! 10^4\rm {\ km\ s^{-1}}$ interacting with an isolated galaxy disc with a manually controlled clumpy ISM, followed at sub-pc resolution. Our simulations are performed with arepo and probe a wide range of AGN luminosities ($L_{\rm {AGN}}{=} 10^{43-47}\rm {\ erg\ s^{-1}}$) and ISM substructures. In homogeneous discs, the AGN wind sweeps up an outflowing, cooling shell, where the emerging cold phase dominates the mass and kinetic energy budgets, reaching a momentum flux $\dot{p} \approx 7\ L/c$. However, when the ISM is clumpy, outflow properties are profoundly different. They contain small, long-lived ($\gtrsim 5\ \rm {Myr}$), cold ($T{\lesssim }10^{4.5}{\rm {\ K}}$) cloudlets entrained in the faster, hot outflow phase, which are only present in the outflow if radiative cooling is included in the simulation. While the cold phase dominates the mass of the outflow, most of the kinetic luminosity is now carried by a tenuous, hot phase with $T \gtrsim 10^7 \, \rm K$. While the hot phases reach momentum fluxes $\dot{p} \approx (1 - 5)\ L/c$, energy-driven bubbles couple to the cold phase inefficiently, producing modest momentum fluxes $\dot{p} \lesssim L/c$ in the fast-outflowing cold gas. These low momentum fluxes could lead to the outflows being misclassified as momentum-driven using common observational diagnostics. We also show predictions for scaling relations between outflow properties and AGN luminosity and discuss the challenges in constraining outflow driving mechanisms and kinetic coupling efficiencies using observed quantities.
HD152843 b & c: the masses and orbital periods of a sub-Neptune and a superpuff Neptune
Authors: Nicholson B A , Aigrain S , Eisner N L , Cretignier M , Barragán O , Kaye L , Taylor J , Owen J , Mortier A , Affer L , Boschin W , Buchhave L A , Cameron A Collier , Damasso M , Fabrizio L Di , DiTomasso V , Dumusque X , Ghedina A , Latham D W , López-Morales M , Lorenzi V , Fiorenzano A F Martínez , Molinari E , Pedani M , Pinamonti M , Rice K , Sozzetti A 
Published: July 2024

ABSTRACT
We present the characterization of the two transiting planets around HD 152843 (TOI 2319, TIC 349488688) using an intensive campaign of HARPS-N radial velocities, and two sectors of TESS data. These data reveal a unique and fascinating system: HD 152843 b and c have near equal masses of around 9 $M_{\hbox{$\oplus $}}$ but differing radii of $3.05 \pm 0.11$$R_{\hbox{$\oplus $}}$ and $5.94 _{ - 0.16 } ^ { + 0.18 }$$R_{\hbox{$\oplus $}}$, respectively, and orbital periods of $11.62071 _{ - 0.000106 } ^ { + 9.6e-05 }$ and $19.502104 _{ - 8.5e-05 } ^ { + 7.4e-05 }$ d. This indicates that HD 152843 c is in the lowest fifth-percentile in density of the known exoplanet population, and has the longest orbital period among these low-density planets. Further, HD 152843 c’s radius places it in the ‘Saturn valley’, the observed lack of planets larger than Neptune, but smaller than Saturn. The orbital periods of these planets indicate they are near a $5:3$ mean motion resonance, indicating the possibility of transit timing variations, and hints at the possibility of interaction with a third planet at some point in the evolution of this system. Further, the brightness of the host star and the low density of HD 152843 c make it a key target for atmospheric characterization.
Constraints from Fermi observations of long gamma-ray bursts on cosmological parameters
Authors: Wang Huifeng , Liang Nan 
Published: July 2024

ABSTRACT
In this paper, we compile a Fermi sample of the long gamma-ray bursts (GRB) observations from 15 years of GBM catalogue with identified redshift, in which the GOLD sample contains 123 long GRBs at $z\le 5.6$ and the FULL sample contains 151 long GRBs with redshifts at $z\le 8.2$. The Amati relation (the $E_{\rm p,i}$–$E_{\rm iso}$ correlation) is calibrated at $z\lt 1.4$ by a Gaussian Process from the latest observational Hubble data with the cosmic chronometers method so that GRBs at high-redshift $z\ge 1.4$ can be used to constrain cosmological models via the Markov chain Monte Carlo (MCMC) method. From the cosmology-independent GRBs with the GOLD sample at $z\ge 1.4$ and the Pantheon + sample of type Ia supernovae (SNe Ia) at $0.01\lt z\le 2.3$, we obtain $\Omega _{\rm m} = 0.354\pm 0.018, H_0 = 73.05\pm 0.2\, \rm {km\,s^{-1}\,Mpc^{-1}}$ for the flat Lambda cold dark matter ($\Lambda$CDM) model; $w_0 = -1.22^{+0.18}_{-0.15}$ for the flat wCDM model; and $w_{a} = -1.12^{+0.45}_{-0.83}$ for the flat Chevallier–Polarski–Linder model at the 1$\sigma$ confidence level. Our results with the GOLD and FULL sample are almost identical, which are more stringent than the previous results with GRBs.
The variable radio jet of the accreting neutron star the Rapid Burster
Authors: van den Eijnden J , Robins D , Sharma R , Sánchez-Fernández C , Russell T D , Degenaar N , Miller-Jones J C A , Maccarone T 
Published: July 2024

ABSTRACT
The Rapid Burster is a unique neutron star low-mass X-ray binary system, showing both thermonuclear v-I and accretion-driven Type-II X-ray bursts. Recent studies have demonstrated how coordinated observations of X-ray and radio variability can constrain jet properties of accreting neutron stars – particularly when the X-ray variability is dominated by discrete changes. We present a simultaneous very large array, Swift, and INTErnational Gamma-Ray Astrophysics Laboratory observing campaign of the Rapid Burster to investigate whether its jet responds to Type-II bursts. We observe the radio counterpart of the X-ray binary at its faintest-detected radio luminosity, while the X-ray observations reveal prolific, fast X-ray bursting. A time-resolved analysis reveals that the radio counterpart varies significantly between observing scans, displaying a fractional variability of $38 \pm 5$ per cent. The radio faintness of the system prevents the robust identification of a causal relation between individual Type-II bursts and the evolution of the radio jet. However, based on a comparison of its low-radio luminosity with archival Rapid Burster observations and other accreting neutron stars, and on a qualitative assessment of the X-ray and radio light curves, we explore the presence of a tentative connection between bursts and jet: i.e. the Type-II bursts may weaken or strengthen the jet. The former of those two scenarios would fit with magnetorotational jet models; we discuss three lines of future research to establish this potential relation between Type-II bursts and jets more confidently.
Pro-environmental voting: What it is, how to measure it, and its determinants among contemporary European voters
Authors: Mannoni Elisabetta 
Published: July 2024

Abstract
With this research, I introduce the concept of pro-environmental voting, proposing an outcome-oriented rather than motivation-based definition and measurement. By conceptualizing it as an instance of pro-environmental behavior, I define it as voting for a party that takes a pro-environmental stance and for which environmental protection is also relatively salient—regardless of whether that is why the voter supports that party. I suggest measuring it by multiplying, for the party voted, its salience score on environmental protection with the distance between its position on the environment and the average position of all parties in the system on the same issue. Then, I apply this measurement to the recently released ESS10 (2023) data from 26 European countries. Findings primarily reveal that moral obligation and age are key drivers of pro-environmental voting; they also show that younger individuals vote more consistently with their environmental concern than older voters.
The U1 small nuclear RNA enhances drought tolerance in Arabidopsis
Authors: Wang Fan , Li Yang , Yuan Jianbo , Li Cong , Lin Yan , Gu Jinbao , Wang Zhen-Yu 
Published: July 2024

Abstract
Alternative splicing (AS) is an important posttranscriptional regulatory mechanism that improves plant tolerance to drought stress by modulating gene expression and generating proteome diversity. The interaction between the 5′ end of U1 small nuclear RNA (U1 snRNA) and the conserved 5′ splice site of precursor messenger RNA (pre-mRNA) is pivotal for U1 snRNP involvement in AS. However, the roles of U1 snRNA in drought stress responses remain unclear. This study provides a comprehensive analysis of AtU1 snRNA in Arabidopsis (Arabidopsis thaliana), revealing its high conservation at the 5′ end and a distinctive four-leaf clover structure. AtU1 snRNA is localized in the nucleus and expressed in various tissues, with prominent expression in young floral buds, flowers, and siliques. The overexpression of AtU1 snRNA confers enhanced abiotic stress tolerance, as evidenced in seedlings by longer seedling primary root length, increased fresh weight, and a higher greening rate compared with the wild-type. Mature AtU1 snRNA overexpressor plants exhibit higher survival rates and lower water loss rates under drought stress, accompanied by a significant decrease in H2O2 and an increase in proline. This study also provides evidence of altered expression levels of drought-related genes in AtU1 snRNA overexpressor or genome-edited lines, reinforcing the crucial role of AtU1 snRNA in drought stress responses. Furthermore, the overexpression of AtU1 snRNA influences the splicing of downstream target genes, with a notable impact on SPEECHLESS (SPCH), a gene associated with stomatal development, potentially explaining the observed decrease in stomatal aperture and density. These findings elucidate the critical role of U1 snRNA as an AS regulator in enhancing drought stress tolerance in plants, contributing to a deeper understanding of the AS pathway in drought tolerance and increasing awareness of the molecular network governing drought tolerance in plants.
Statin intolerance and the drucebo effect
Authors: Mugawar B , Mcerlean S , O’ Connor P , Kennedy C 
Published: July 2024

Abstract
Hypercholesterolemia is a well-described risk factor for atherosclerotic cardiovascular disease. Statins remain the cornerstone of therapy. Statin intolerance (SI) particularly statin associated muscle symptoms (SAMS) and inappropriate stopping of treatment is associated with increased cardiovascular risk. A significant proportion of reported SAMS relates to expectation of side effects and can be termed the ‘negative drucebo effect’. Patients should be educated about SI, the negative drucebo effect, in addition to the benefits of adherence to the therapy when first prescribed a statin. The aim of this commentary is to discuss the issue of SI, the negative drucebo effect and to suggest some interventions that may be used to address this issue.