bluuebunny/crossref_metadata_2025_split huggingface dataset:
Unstable cosmic ray nuclei constrain low-diffusion zones in the Galactic disc
Authors: Jacobs Hanno , Mertsch Philipp , Phan Vo Hong Minh 
Published: September 2023

ABSTRACT
Observations of the vicinity of a variety of galactic gamma-ray sources have indicated a local suppression of diffusivity of cosmic rays (CRs) by up to three orders of magnitude. However, the impact of these low-diffusion zones on global properties of CR transport is, however, only poorly understood. Here, we argue that CR nuclear ratios, like the boron-to-carbon ratio and relative abundances of Beryllium isotopes are sensitive to the filling fraction of such low-diffusion zones and hence their measurements can be used to constrain the typical sizes and ages of such regions. We have performed a careful parameter study of a CR transport model that allows for different diffusion coefficients κdisc and κhalo in the galactic disc and halo, respectively. Making use of preliminary data from the AMS-02 experiment on the ratio of Beryllium isotopes, we find a 3.5σ preference for a suppression of the diffusion coefficient in the disc with a best-fitting value of $\kappa _{\mathrm{disc}}/\kappa _{\mathrm{halo}} = 0.20^{+0.10}_{-0.06}$. We forecast that with upcoming data from the HELIX balloon experiment, the significance could increase to 6.8σ. Adopting a coarse-graining approach, we find that such a strong suppression could be realized if the filling fraction of low-diffusion zones in the disc was $\sim 66~{{\ \rm per\ cent}}$. We conclude that the impact of regions of suppressed diffusion might be larger than usually assumed and ought to be taken into account in models of Galactic CR transport.
The impact of cosmic rays on thermal and hydrostatic stability in galactic haloes
Authors: Tsung Tsun Hin Navin , Oh S Peng , Bustard Chad 
Published: September 2023

ABSTRACT
We investigate how cosmic rays (CRs) affect thermal and hydrostatic stability of circumgalactic (CGM) gas, in simulations with both CR streaming and diffusion. Local thermal instability can be suppressed by CR-driven entropy mode propagation, in accordance with previous analytic work. However, there is only a narrow parameter regime where this operates, before CRs overheat the background gas. As mass dropout from thermal instability causes the background density and hence plasma β ≡ Pg/PB to fall, the CGM becomes globally unstable. At the cool disc-to-hot−halo interface, a sharp drop in density boosts Alfven speeds and CR gradients, driving a transition from diffusive to streaming transport. CR forces and heating strengthen, while countervailing gravitational forces and radiative cooling weaken, resulting in a loss of both hydrostatic and thermal equilibrium. In lower β haloes, CR heating drives a hot, single-phase diffuse wind with velocities v ∝ (theat/tff)−1, which exceeds the escape velocity when theat/tff ≲ 0.4. In higher β haloes, where the Alfven Mach number is higher, CR forces drive multi-phase winds with cool, dense fountain flows and significant turbulence. These flows are CR dominated due to ‘trapping’ of CRs by weak transverse B-fields, and have the highest mass loading factors. Thus, local thermal instability can result in winds or fountain flows where either the heat or momentum input of CRs dominates.
The IRX–β relation in kpc-sized star-forming regions in nearby galaxies
Authors: Duffy Laura , Molina Mallory , Eracleous Michael , Ciardullo Robin , Yan Renbin , Gronwall Caryl , Ajgaonkar Nikhil , Boquien Médéric , Zhou Shuang , Li Cheng 
Published: September 2023

ABSTRACT
The effect of dust attenuation on a galaxy’s light depends on a number of physical properties, such as geometry and dust composition, both of which can vary across the faces of galaxies. To investigate this variation, we continue analysis on star-forming regions in 29 galaxies studied previously. We analyse these regions using Swift/UV Optical Telescope and Wide-field Infrared Survey Explorer images, as well as Sloan Digital Sky Survey/Mapping Nearby Galaxies at Apache Point Observatory emission line maps to constrain the relationship between the infrared excess (IRX) and the ultraviolet spectral index, β, for each star-forming region. This relationship can be used to constrain which dust attenuation law is appropriate for the region. We find that the value of Dn(4000) for a region is correlated with both IRX and β, and that the gas-phase metallicity is strongly correlated with the IRX. This correlation between metallicity and IRX suggests that regardless of aperture, metal-rich regions have steeper attenuation curves. We also find that integrated galactic light follows nearly the same IRX–β relationship as that found for kpc-sized star-forming regions. This similarity may suggest that the attenuation law followed by the galaxy is essentially the same as that followed by the regions, although the relatively large size of our star-forming regions complicates this interpretation because optical opacity and attenuation curves have been observed to vary within individual galaxies.
Diffuse gamma-ray emission around the Rosette Nebula
Authors: Liu Jia-hao , Liu Bing , Yang Rui-zhi 
Published: September 2023

ABSTRACT
The Rosette Nebula is a young stellar cluster and molecular cloud complex, located at the edge of the southern shell of a middle-aged supernova remnant Monoceros Loop (G205.5+0.5). We revisited the GeV gamma-ray emission towards the Rosette Nebula using more than 13 yr of Fermi-LAT data. We tested several spatial models and found that compared to the result using the CO gas template only, the inclusion of the H ii gas template can significantly improve the likelihood fit. We performed spectral analysis using the new spatial template. With both the gamma-ray observation and CO+H ii gas data, we derived the cosmic ray spectrum of different components in the vicinity of the Rosette Nebula. We found the gamma-ray emissions from Rosette Nebula are substantially harder than previously reported, which may imply that Rosette Nebula is another example of a gamma-ray emitting young massive star cluster.
Identifying strongly lensed gravitational waves with the third-generation detectors
Authors: Gao Zijun , Liao Kai , Yang Lilan , Zhu Zong-Hong 
Published: September 2023

ABSTRACT
The joint detection of gravitational wave (GW) signals by a network of instruments will increase the detecting ability of faint and far GW signals with higher signal-to-noise ratios (SNRs), which could improve the ability of detecting the lensed GWs as well, especially for the third-generation (3G) detectors, e.g. Einstein Telescope (ET) and Cosmic Explorer (CE). However, identifying strongly lensed gravitational waves (SLGWs) is still challenging. We focus on the identification ability of 3G detectors in this article. We predict and analyse the SNR distribution of SLGW signals and prove only 50.6 per cent of SLGW pairs detected by ET alone can be identified by lens Bayes factor (LBF), which is a popular method at present to identify SLGWs. For SLGW pairs detected by CEET network, owing to the superior spatial resolution, this number rises to 87.3 per cent. Moreover, we get an approximate analytical relation between SNR and LBF. We give clear SNR limits to identify SLGWs and estimate the expected yearly detection rates of galaxy-scale lensed GWs that can get identified with 3G detector network.
RASS-MCMF: a full-sky X-ray selected galaxy cluster catalogue
Authors: Klein Matthias , Hernández-Lang Daniel , Mohr Joseph J , Bocquet Sebastian , Singh Aditya 
Published: September 2023

ABSTRACT
We present the RASS-MCMF catalogue of 8449 X-ray selected galaxy clusters over 25 000 deg2 of extragalactic sky. The accumulation of deep multiband optical imaging data, the development of the Multi-Component Matched Filter (MCMF) cluster confirmation algorithm, and the release of the DESI Legacy Survey DR10 catalogue makes it possible – for the first time, more than 30 yr after the launch of the ROSAT X-ray satellite – to identify the majority of the galaxy clusters detected in the second ROSAT All-Sky-Survey (RASS) source catalogue (2RXS). The resulting 90 per cent pure RASS-MCMF catalogue is the largest intracluster medium (ICM)-selected cluster sample to date. RASS-MCMF probes a large dynamic range in cluster mass spanning from galaxy groups to the most massive clusters. The cluster redshift distribution peaks at $z$ ∼ 0.1 and extends to redshifts $z$ ∼ 1. Out to $z$ ∼ 0.4, the RASS-MCMF sample contains more clusters per redshift interval (dN/dz) than any other ICM-selected sample. In addition to the main sample, we present two subsamples with 6912 and 5506 clusters, exhibiting 95 per cent and 99 per cent purity, respectively. We forecast the utility of the sample for a cluster cosmological study, using realistic mock catalogues that incorporate most observational effects, including the X-ray exposure time and background variations, the existence likelihood selection and the impact of the optical cleaning with the algorithm MCMF. Using realistic priors on the observable–mass relation parameters from a DES-based weak lensing analysis, we estimate the constraining power of the RASS-MCMF×DES sample to be of 0.026, 0.033, and 0.15 (1σ) on the parameters Ωm, σ8, and $w$, respectively.
MaNGA DynPop – II. Global stellar population, gradients, and star-formation histories from integral-field spectroscopy of 10K galaxies: link with galaxy rotation, shape, and total-density gradients
Authors: Lu Shengdong , Zhu Kai , Cappellari Michele , Li Ran , Mao Shude , Xu Dandan 
Published: September 2023

ABSTRACT
This is the second paper of the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) Dynamics and stellar Population (DynPop) series, which analyses the global stellar population, radial gradients, and non-parametric star-formation history of ∼10K galaxies from the MaNGA Survey final data release 17 and relates them with dynamical properties of galaxies. We confirm the correlation between the stellar population properties and the stellar velocity dispersion σe, but also find that younger galaxies are more metal-poor at fixed σe. Stellar age, metallicity, and mass-to-light ratio (M*/L) all decrease with increasing galaxy rotation, while their radial gradients become more negative (i.e. lower value at the outskirts). The exception is the slow rotators, which also appear to have significantly negative metallicity gradients, confirming the mass–metallicity gradient correlation. Massive disc galaxies in the green valley, on the $(\sigma _{\rm e},\rm age)$ plane, show the most negative age and metallicity gradients, consistent with their old central bulges surrounded by young star-forming discs and metal-poor gas accretion. Galaxies with high σe, steep total mass-density slope, low dark matter fraction, high M*/L, and high metallicity have the highest star-formation rate at earlier times, and are currently quenched. We also discover a population of low-mass star-forming galaxies with low rotation but physically distinct from the massive slow rotators. A catalogue of these stellar population properties is provided publicly.
Cosmological simulations of a momentum coupling between dark matter and quintessence
Authors: Palma Daniela , Candlish Graeme N 
Published: September 2023

ABSTRACT
Dark energy is frequently modelled as an additional dynamical scalar field component in the Universe, referred to as ‘quintessence’, which drives the late-time acceleration. Furthermore, the quintessence field may be coupled to dark matter and/or baryons, leading to a fifth force. In this paper, we explore the consequences for non-linear cosmological structure formation arising from a momentum coupling between the quintessence field and dark matter only. The coupling leads to a modified Euler equation, which we implement in an N-body cosmological simulation. We then analyse the effects of the coupling on the non-linear power spectrum and the properties of the dark matter haloes. We find that, for certain quintessence potentials, a positive coupling can lead to significantly reduced structure on small scales and somewhat enhanced structure on large scales, as well as reduced halo density profiles and increased velocity dispersions.
Radiation hydrodynamical self-similar accretion disc winds
Authors: Fukue J 
Published: September 2023

ABSTRACT
Self-similar supersonic winds from an accretion disc around a central object are examined with/without radiation fields under the fully self-similar treatment of two-dimensional outflows. The thermal pressure and viscosity are ignored for simplicity. In the case without radiation fields, many solutions are not outflowing winds, but bound flows, except for limited cases which satisfy the escape condition with sufficiently large initial launch speed and rotational one. In the case with radiation fields, the radiation force acts as a driving force, and therefore, the winds blow easier. However, several solutions are unphysical, since the radiative energy density becomes negative. As a result, depending on the rotational motion and boundary conditions, the radiatively driven self-similar cold disc winds are divided into three types; bound solutions lacking launch speed or radiative acceleration, unphysical ones with a negative energy density, and escaping winds confined in the conical region or extending in the whole space as a special type.
Shaping the unseen: the influence of baryons and environment on low-mass, high-redshift dark matter haloes in the SIEGE simulations
Authors: Pascale R , Calura F , Lupi A , Rosdahl J , Lacchin E , Meneghetti M , Nipoti C , Vanzella E , Vesperini E , Zanella A 
Published: September 2023

ABSTRACT
We use zoom-in, hydrodynamical, cosmological N-body simulations tracing the formation of the first stellar clumps from the SImulating the Environments where Globular clusters Emerged project, to study key structural properties of dark matter haloes when the Universe was only $0.92\, {\rm Gyr}$ old. The very high resolution (maximum physical resolution $0.3\, {h}^{-1}\, {\rm pc}$ at z = 6.14, smallest dark matter particle mass $164\, {\rm M}_{\odot }$) allows us to reach the very low mass end of the stellar-to-halo mass relation ($M_{\rm vir}=10^{7.5{\!-\!}9.5}\, {\rm M}_{\odot }$) to study the processes that mould dark matter haloes during the first stages of structure formation. We investigate the role of baryonic cooling and stellar feedback, modelled from individual stars, in shaping haloes, and of environmental effects as accretion of dark matter along cosmic filaments and mergers. We find that the onset of star formation (typically for $\log M_{\rm vir}/\, {\rm M}_{\odot }\simeq 7.6$) causes the inner cusp in the haloes’ density profile to flatten into a core with constant density and size proportionally to the halo virial mass. Even at these mass scales, we confirm that baryons make haloes that have formed stars rounder in the central regions than haloes that have not formed stars yet, with median minor-to-major 〈q〉 and intermediate-to-major 〈s〉 axes 0.66 and 0.84, respectively. Our morphological analysis shows that, at z = 6.14, haloes are largely prolate in the outer parts, with the major axis aligned along filaments of the cosmic web or towards smaller sub-haloes, with the degree of elongation having no significant dependence on the halo mass.
Interpreting Sunyaev–Zel’dovich observations with MillenniumTNG: mass and environment scaling relations
Authors: Hadzhiyska Boryana , Ferraro Simone , Pakmor Rüdiger , Bose Sownak , Delgado Ana Maria , Hernández-Aguayo César , Kannan Rahul , Springel Volker , White Simon D M , Hernquist Lars 
Published: September 2023

ABSTRACT
Sunyaev–Zel’dovich (SZ) measurements can dramatically improve our understanding of the intergalactic medium and the role of feedback processes in galaxy formation, allowing us to calibrate important astrophysical systematics in cosmological constraints from weak lensing galaxy clustering surveys. However, the signal is only measured in a two-dimensional projection, and its correct interpretation relies on understanding the connection between observable quantities and the underlying intrinsic properties of the gas, in addition to the relation between the gas and the underlying matter distribution. One way to address these challenges is through the use of hydrodynamical simulations such as the high-resolution, large-volume MillenniumTNG suite. We find that measurements of the optical depth, τ, and the Compton-y parameter, Y, receive large line-of-sight contributions that can be removed effectively by applying a compensated aperture photometry filter. In contrast with other τ probes (e.g. X-rays and fast radio bursts), the kinematic SZ-inferred τ receives most of its signal from a confined cylindrical region around the halo due to the velocity decorrelation along the line of sight. Additionally, we perform fits to the Y–M and τ–M scaling relations and report best-fitting parameters adopting the smoothly broken power law formalism. We note that subgrid physics modelling can broaden the error bar on these by 30 per cent for intermediate-mass haloes (${\sim }10^{13} \, {\rm M}_{\odot }$). The scatter of the scaling relations can be captured by an intrinsic dependence on concentration and an extrinsic dependence on tidal shear. Finally, we comment on the effect of using galaxies rather than haloes in observations, which can bias the inferred profiles by ∼20 per cent for L* galaxies.
Heating and cooling in stellar coronae: coronal rain on a young Sun
Authors: Daley-Yates Simon , Jardine Moira M , Johnston Craig D 
Published: September 2023

ABSTRACT
Recent observations of rapidly rotating cool dwarfs have revealed H α line asymmetries indicative of clumps of cool, dense plasma in the stars’ coronae. These clumps may be either long-lived (persisting for more than one stellar rotation) or dynamic. The fastest dynamic features show velocities greater than the escape speed, suggesting that they may be centrifugally ejected from the star, contributing to the stellar angular momentum loss. Many, however, show lower velocities, similar to coronal rain observed on the Sun. We present 2.5D magnetohydrodynamic simulations of the formation and dynamics of these condensations in a rapidly rotating (Prot = 1 d) young Sun. Formation is triggered by excess surface heating. This pushes the system out of thermal equilibrium and triggers a thermal instability. The resulting condensations fall back towards the surface. They exhibit quasi-periodic behaviour, with periods longer than typical periods for solar coronal rain. We find line-of-sight velocities for these clumps in the range of 50 km s−1 (blueshifted) to 250 km s−1 (redshifted). These are typical of those inferred from stellar H α line asymmetries, but the inferred clump masses of 3.6 × 1014 g are significantly smaller. We find that a maximum of ${\simeq}3~{{ \rm per\ cent}}$ of the coronal mass is cool clumps. We conclude that coronal rain may be common in solar-like stars, but may appear on much larger scales in rapid rotators.
RNF8 ubiquitylation of XRN2 facilitates R-loop resolution and restrains genomic instability in BRCA1 mutant cells
Authors: Krishnan Rehna , Lapierre Mariah , Gautreau Brandon , Nixon Kevin C J , El Ghamrasni Samah , Patel Parasvi S , Hao Jun , Yerlici V Talya , Guturi Kiran Kumar Naidu , St-Germain Jonathan , Mateo Francesca , Saad Amine , Algouneh Arash , Earnshaw Rebecca , Shili Duan , Seitova Alma , Miller Joshua , Khosraviani Negin , Penn Adam , Ho Brandon , Sanchez Otto , Hande M Prakash , Masson Jean-Yves , Brown Grant W , Alaoui-Jamali Moulay , Reynolds John J , Arrowsmith Cheryl , Raught Brian , Pujana Miguel A , Mekhail Karim , Stewart Grant S , Hakem Anne , Hakem Razqallah 
Published: September 2023

Abstract
Breast cancer linked with BRCA1/2 mutations commonly recur and resist current therapies, including PARP inhibitors. Given the lack of effective targeted therapies for BRCA1-mutant cancers, we sought to identify novel targets to selectively kill these cancers. Here, we report that loss of RNF8 significantly protects Brca1-mutant mice against mammary tumorigenesis. RNF8 deficiency in human BRCA1-mutant breast cancer cells was found to promote R-loop accumulation and replication fork instability, leading to increased DNA damage, senescence, and synthetic lethality. Mechanistically, RNF8 interacts with XRN2, which is crucial for transcription termination and R-loop resolution. We report that RNF8 ubiquitylates XRN2 to facilitate its recruitment to R-loop-prone genomic loci and that RNF8 deficiency in BRCA1-mutant breast cancer cells decreases XRN2 occupancy at R-loop-prone sites, thereby promoting R-loop accumulation, transcription-replication collisions, excessive genomic instability, and cancer cell death. Collectively, our work identifies a synthetic lethal interaction between RNF8 and BRCA1, which is mediated by a pathological accumulation of R-loops.
FLIBase: a comprehensive repository of full-length isoforms across human cancers and tissues
Authors: Shi Qili , Li Xinrong , Liu Yizhe , Chen Zhiao , He Xianghuo 
Published: September 2023

Abstract
Regulatory processes at the RNA transcript level play a crucial role in generating transcriptome diversity and proteome composition in human cells, impacting both physiological and pathological states. This study introduces FLIBase (www.FLIBase.org), a specialized database that focuses on annotating full-length isoforms using long-read sequencing techniques. We collected and integrated long-read (351 samples) and short-read (12 469 samples) RNA sequencing data from diverse normal and cancerous human tissues and cells. The current version of FLIBase comprises a total of 983 789 full-length spliced isoforms, identified through long-read sequences and verified using short-read exon–exon splice junctions. Of these, 188 248 isoforms have been annotated, while 795 541 isoforms remain unannotated. By overcoming the limitations of short-read RNA sequencing methods, FLIBase provides an accurate and comprehensive representation of full-length transcripts. These comprehensive annotations empower researchers to undertake various downstream analyses and investigations. Importantly, FLIBase exhibits a significant advantage in identifying a substantial number of previously unannotated isoforms and tumor-specific RNA transcripts. These tumor-specific RNA transcripts have the potential to serve as a source of immunogenic recurrent neoantigens. This remarkable discovery holds tremendous promise for advancing the development of tailored RNA-based diagnostic and therapeutic strategies for various types of human cancer.