bluuebunny/crossref_metadata_2025_split huggingface dataset:
The origin of the observed Ly α EW distribution of dwarf galaxies at z ∼ 2
Authors: Snapp-Kolas Christopher , Siana Brian , Gburek Timothy , Alavi Anahita , Emami Najmeh , Richard Johan , Stark Daniel P , Scarlata Claudia , Lemaux Brian C , Zamorani Giovanni , Bardelli Sandro , Hathi Nimish , Cassata Paolo 
Published: September 2023

ABSTRACT
We present a rest-UV-selected sample of 32 lensed galaxies at z ∼ 2 observed with joint Keck/LRIS rest-UV and Keck/MOSFIRE rest-optical spectra behind the clusters Abell 1689, MACS J0717, and MACS J1149. The sample pushes towards the faintest UV luminosities observed ($-19 \le {M_{\rm UV}} \le -17$) at this redshift. The fraction of dwarf galaxies identified as Ly α emitters ($\rm EW \ge 20$ Å) is ${X_{\rm LAE}}=33^{+17}_{-12}\,{\rm per\, cent}$. We use the Balmer lines and UV continuum to estimate both the intrinsic EW and the Ly α escape fraction to determine their relative importance in dictating the observed EW distribution. Fainter galaxies (MUV &gt; −19) show larger intrinsic EWs and escape fractions than brighter galaxies. Only galaxies with intrinsic EWs greater than 40 Å have escape fractions larger than 5 per cent. We find little to no anticorrelation between the escape fraction and dust in dwarf galaxies. The volumetric escape fraction of our sample is $f_{\rm esc}^{\rm Ly\alpha } = 4.6^{+2.0}_{-1.4}\,{\rm per\, cent}$ in agreement with measurements found elsewhere in the literature. 60 per cent of the total integrated Ly α luminosity density comes from galaxies with EWobs &gt; 20 Å.
On the similarity of rotational motion of dust particles in the inner atmosphere of comets
Authors: Ivanovski Stavro L , Zakharov V V , Moreno F , Bykov N Y , Muñoz O , Fulle M , Rotundi A , Corte V Della , Rodionov A V 
Published: September 2023

ABSTRACT
In situ measurements of individual dust grain parameters in the immediate vicinity of a cometary nucleus are being carried by the Rosetta spacecraft at comet 67P/Churyumov–Gerasimenko. For interpretation of these observational data, a model of dust grain motion as realistic as possible is requested. In particular, the results of Stardust mission and analysis of samples of interplanetary dust have shown that these particles are highly non-spherical. In many cases precise simulations of non-spherical grain’s dynamics is either impossible or computationally too expensive. In such situation it is proposed to use available experimental or numerical data obtained for other conditions and rescale them considering similarity of the physical process. In the present paper we focus on the derivation of scaling laws of rotational motion applicable for any shape of particles. We use a set of universal, dimensionless parameters characterizing the dust motion in the inner cometary coma. The scaling relations for translational and rotational motion of dust grains in a cometary environment are proposed. The scaled values are compared with numerically computed ones in our previous works.
A new method for spatially resolving the turbulence-driving mixture in the ISM with application to the Small Magellanic Cloud
Authors: Gerrard Isabella A , Federrath Christoph , Pingel Nickolas M , McClure-Griffiths Naomi M , Marchal Antoine , Joncas Gilles , Clark Susan E , Stanimirović Snežana , Lee Min-Young , van Loon Jacco Th , Dickey John , Dénes Helga , Ma Yik Ki , Dempsey James , Lynn Callum 
Published: September 2023

ABSTRACT
Turbulence plays a crucial role in shaping the structure of the interstellar medium. The ratio of the three-dimensional density contrast ($\sigma _{\rho /\rho _0}$) to the turbulent sonic Mach number ($\mathcal {M}$) of an isothermal, compressible gas describes the ratio of solenoidal to compressive modes in the turbulent acceleration field of the gas, and is parameterized by the turbulence driving parameter: $b=\sigma _{\rho /\rho _0}/\mathcal {M}$. The turbulence driving parameter ranges from b = 1/3 (purely solenoidal) to b = 1 (purely compressive), with b = 0.38 characterizing the natural mixture (1/3 compressive, 2/3 solenoidal) of the two driving modes. Here, we present a new method for recovering $\sigma _{\rho /\rho _0}$, $\mathcal {M}$, and b, from observations on galactic scales, using a roving kernel to produce maps of these quantities from column density and centroid velocity maps. We apply our method to high-resolution ${\rm H}\,\rm{\small I}$ emission observations of the Small Magellanic Cloud (SMC) from the GASKAP-HI survey. We find that the turbulence driving parameter varies between b ∼ 0.3 and 1.0 within the main body of the SMC, but the median value converges to b ∼ 0.51, suggesting that the turbulence is overall driven more compressively (b &gt; 0.38). We observe no correlation between the b parameter and ${\rm H}\,\rm{\small I}$ or H α intensity, indicating that compressive driving of ${\rm H}\,\rm{\small I}$ turbulence cannot be determined solely by observing ${\rm H}\,\rm{\small I}$ or H α emission density, and that velocity information must also be considered. Further investigation is required to link our findings to potential driving mechanisms such as star-formation feedback, gravitational collapse, or cloud–cloud collisions.
A kinematic study of the disc-outflow system around a high-mass protostar G59.783+0.065 probed by methanol and water masers
Authors: Nakamura M , Motogi K , Nakamura H , Yonekura Y , Fujisawa K 
Published: September 2023

ABSTRACT
Class II CH3OH masers are used as a convenient tracer of disc-like structures in high-mass star formation. However, more than half of them show a complex distribution in Very Long Baseline Interferometry (VLBI) maps. The origin of such a complex distribution is still unknown. We conducted VLBI monitoring observations to unveil the origin of a complex class II CH3OH maser in the high-mass star-forming region G59.783+0.065. We observed the CH3OH maser at 6.7 GHz and the H2O maser at 22 GHz to probe detailed circumstellar kinematics and structures by the Japanese VLBI network and the VLBI Exploration of Radio Astrometry. We found similar bipolar distributions in both masers, specifically two clusters located 2000 au apart along the east–west direction. We detected a linear distribution of CH3OH masers in the western cluster. A position–velocity diagram shows that the western CH3OH masers trace a rotating disc-wind or infalling component inside an edge-on disc-like structure. In contrast to the simple bipolar expanding motions of the H2O masers, the CH3OH masers exhibited complex motions despite their spatial coincidence. Some of the eastern CH3OH masers showed bipolar expansions similar to the H2O masers, while others displayed random or even inward motions. Such complex kinematics and their close association with the H2O maser could occur at the boundary between outflow and inflow. We suggest that the complex distribution of class II CH3OH masers, like G59.783+0.065 arises from several distinct circumstellar structures that simultaneously achieve maser excitation.
The SAMI galaxy survey: impact of black hole activity on galaxy spin–filament alignments
Authors: Barsanti Stefania , Colless Matthew , D’Eugenio Francesco , Oh Sree , Bryant Julia J , Casura Sarah , Croom Scott M , Mai Yifan , Ristea Andrei , van de Sande Jesse , Welker Charlotte , Zovaro Henry R M 
Published: September 2023

ABSTRACT
The activity of central supermassive black holes might affect the alignment of galaxy spin axes with respect to the closest cosmic filaments. We exploit the Sydney–AAO Multi-object Integral-field Galaxy Survey to study possible relations between black hole activity and the spin–filament alignments of stars and ionized gas separately. To explore the impact of instantaneous black hole activity, active galaxies are selected according to emission-line diagnostics. Central stellar velocity dispersion (σc) is used as a proxy for black hole mass and its integrated activity. We find evidence for the gas spin–filament alignments to be influenced by AGN, with Seyfert galaxies showing a stronger perpendicular alignment at fixed bulge mass with respect to galaxies, where ionization is consequence of low-ionization nuclear emission-line regions (LINERs) or old stellar populations (retired galaxies). On the other hand, the greater perpendicular tendency for the stellar spin–filament alignments of high-bulge mass galaxies is dominated by retired galaxies. Stellar alignments show a stronger correlation with σc compared to the gas alignments. We confirm that bulge mass (Mbulge) is the primary parameter of correlation for both stellar and gas spin–filament alignments (with no residual dependency left for σc), while σc is the most important property for secular star formation quenching (with no residual dependency left for Mbulge). These findings indicate that Mbulge and σc are the most predictive parameters of two different galaxy evolution processes, suggesting mergers trigger spin–filament alignment flips and integrated black hole activity drives star formation quenching.
Determining the ratio of the jet to the unbeamed luminosities for γ-ray blazars
Authors: Pei Zhiyuan , Li Ziyan , Huang Xiulin , Qian Yanjun , Huang Danyi , Li Chengfeng , Liao Jiru , Ye Xiao , Liang Jingchao , Chen Guohai , Fan Junhui 
Published: September 2023

ABSTRACT
The spectacular observational phenomena lying in blazars can be well explained and described by the relativistic beaming effect that the emission in the jet is highly boosted along the line of sight to observers. Aiming to reveal the intrinsic emission core dominance in γ-ray loud blazars, we collect a large sample including 226 blazars with available superluminal motion data and radio core-dominance parameters at 5 GHz, and calculate a crucial parameter, R⊥, defined as the ratio of the luminosity in the jet to the unbeamed luminosity when the viewing angle comes up to 90°. R⊥ is a better parameter than the well-known core-dominance parameter, R, to reveal more intrinsic physical properties behind the prominent observational characteristics within blazars. We primarily ascertain the updated median value of R⊥ = 0.032 at 5 GHz, illustrating around 97 per cent of the total radio emission are dominated by the jets in γ-ray loud blazars. We also make further discussion on the physical difference in BL Lacertae objects and flat-spectrum radio quasars.
The spectroscopic orbit of Polaris and its pulsation properties
Authors: Torres Guillermo 
Published: September 2023

ABSTRACT
Polaris is the nearest and brightest classical Cepheid, and pulsates with a period of about 4 d. It has long been known as a single-lined spectroscopic binary with an orbital period of 30 yr. Historical photometric and spectroscopic records indicate that, until recently, the pulsation period has been increasing at a rate of about 4.5 s yr−1, and that the amplitude of the pulsation declined for most of the 20th century, but more recently halted its decline and began to increase. Here, we report an analysis of the more than 3600 individual radial velocity measurements of Polaris available from the literature over the past 126 yr. We find that the pulsation period is now becoming shorter, and that the amplitude of the velocity variations has stopped increasing, and may be getting smaller again. We also find tantalizing evidence that these changes in pulsation behaviour over the last century may be related to the binary nature of the system, as they seem to occur near each periastron passage, when the secondary comes within 29 stellar radii of the Cepheid in its eccentric orbit. This suggests the companion may be perturbing the atmosphere of the Cepheid and altering its pulsation properties at each encounter. After removal of the pulsation component of the velocities, we derive a much improved spectroscopic orbit for the binary that should serve as the basis for a more accurate determination of the dynamical masses, which are still rather uncertain.
A linearized approach to radial velocity extraction
Authors: Shahaf S , Zackay B 
Published: September 2023

ABSTRACT
High-precision radial velocity (RV) measurements are crucial for exoplanet detection and characterization. Efforts to achieve ∼10 cm s–1 precision have been made over the recent decades, with significant advancements in instrumentation, data reduction techniques, and statistical inference methods. However, despite these efforts, RV precision is currently limited to ∼50 cm s–1. This value exceeds state-of-the-art spectrographs’ expected instrumental noise floor and is mainly attributed to RV signals induced by stellar variability. In this work, we propose a factorization method to overcome this limitation. The factorization is particularly suitable for controlling the effect of localized changes in the stellar emission profile, assuming some smooth function of a few astrophysical parameters governs them. We use short-time Fourier transforms (STFTs) to infer the RV in a procedure equivalent to least-squares minimization in the wavelength domain and demonstrate the effectiveness of our method in treating arbitrary temperature fluctuations on the star’s surface. The proposed prescription can be naturally generalized to account for other effects, either intrinsic to the star, such as magnetic fields, or extrinsic to it, such as telluric contamination. As a proof-of-concept, we empirically derive a set of factorization terms describing the solar centre-to-limb variation and apply them to a set of realistic SOAP-GPU spectral simulations. We discuss the method’s capability to mitigate variability-induced RV signals and its potential extensions to serve as a tomographic tool.
Low-degree solar rotational splitting from 45 yr of BiSON observations
Authors: Howe Rachel , Chaplin W J , Elsworth Y P , Hale S J , Nielsen M B 
Published: September 2023

ABSTRACT
We present solar low-degree rotational splitting values based on a new analysis of Sun-as-a-star observations from the Birmingham Solar Oscillations Network, covering a 16 425-d period from 1976 December 31 to 2021 December 20 with a duty cycle of 57 per cent. The splitting values are estimated from the power spectrum using a Markov chain Monte Carlo sampling method, and we also present for comparison the results from an analysis of 100 realizations of synthetic data with the same resolution and gap structure. Comparison of the scatter in the results from the synthetic realizations with their estimated uncertainties suggests that for this data set the formal uncertainty estimates are about 30 per cent too small. An upward bias in the splittings at frequencies above 2200 μHz, where the components are not fully resolved, is seen in both the observed and synthetic data. When this bias is taken into account, our results are consistent with a frequency-independent synodic rotational splitting value of 400 nHz.
Srsf1 and Elavl1 act antagonistically on neuronal fate choice in the developing neocortex by controlling TrkC receptor isoform expression
Authors: Weber A Ioana , Parthasarathy Srinivas , Borisova Ekaterina , Epifanova Ekaterina , Preußner Marco , Rusanova Alexandra , Ambrozkiewicz Mateusz C , Bessa Paraskevi , Newman Andrew G , Müller Lisa , Schaal Heiner , Heyd Florian , Tarabykin Victor 
Published: September 2023

Abstract
The seat of higher-order cognitive abilities in mammals, the neocortex, is a complex structure, organized in several layers. The different subtypes of principal neurons are distributed in precise ratios and at specific positions in these layers and are generated by the same neural progenitor cells (NPCs), steered by a spatially and temporally specified combination of molecular cues that are incompletely understood. Recently, we discovered that an alternatively spliced isoform of the TrkC receptor lacking the kinase domain, TrkC-T1, is a determinant of the corticofugal projection neuron (CFuPN) fate. Here, we show that the finely tuned balance between TrkC-T1 and the better known, kinase domain-containing isoform, TrkC-TK+, is cell type-specific in the developing cortex and established through the antagonistic actions of two RNA-binding proteins, Srsf1 and Elavl1. Moreover, our data show that Srsf1 promotes the CFuPN fate and Elavl1 promotes the callosal projection neuron (CPN) fate in vivo via regulating the distinct ratios of TrkC-T1 to TrkC-TK+. Taken together, we connect spatio-temporal expression of Srsf1 and Elavl1 in the developing neocortex with the regulation of TrkC alternative splicing and transcript stability and neuronal fate choice, thus adding to the mechanistic and functional understanding of alternative splicing in vivo.
Sustained pigmentation causes DNA damage and invokes translesion polymerase Polκ for repair in melanocytes
Authors: Ghazi Madeeha , Khanna Shivangi , Subramaniam Yogaspoorthi , Rengaraju Jeyashri , Sultan Farina , Gupta Iti , Sharma Kanupriya , Chandna Sudhir , Gokhale Rajesh S , Natarajan Vivek T 
Published: September 2023

Abstract
Melanin protects skin cells from ultraviolet radiation-induced DNA damage. However, intermediates of eumelanin are highly reactive quinones that are potentially genotoxic. In this study, we systematically investigate the effect of sustained elevation of melanogenesis and map the consequent cellular repair response of melanocytes. Pigmentation increases γH2AX foci, DNA abasic sites, causes replication stress and invokes translesion polymerase Polκ in primary human melanocytes, as well as mouse melanoma cells. Confirming the causal link, CRISPR-based genetic ablation of tyrosinase results in depigmented cells with low Polκ levels. During pigmentation, Polκ activates replication stress response and keeps a check on uncontrolled proliferation of cells harboring melanin-damaged DNA. The mutational landscape observed in human melanoma could in part explain the error-prone bypass of DNA lesions by Polκ, whose absence would lead to genome instability. Thereby, translesion polymerase Polκ is a critical response of pigmenting melanocytes to combat melanin-induced DNA alterations. Our study illuminates the dark side of melanin and identifies (eu)melanogenesis as a key missing link between tanning response and mutagenesis, mediated via the necessary evil translesion polymerase, Polκ.
Key enzyme in charge of ketone reabsorption of renal tubular SMCT1 may be a new target in diabetic kidney disease
Authors: Guo Zhenhong , Zhong Feifei , Hou Meng , Xie Jinlan , Zhang A Zhong , Li Xinran , Li Yuan , Chang Baocheng , Yang Juhong 
Published: September 2023

ABSTRACT

Objective
A ketogenic diet or mildly increased ketone body levels are beneficial for diabetic kidney disease (DKD) patients. Our previous study has found that sodium-coupled monocarboxylate transporter 1 (SMCT1), a key enzyme in charge of ketone reabsorption, possesses beneficial effects on the function of renal tubular epithelial cells (TECs) in energy crisis. Our present study is to investigate whether SMCT1 is important in maintaining the physiological function of renal tubular and plays a role in DKD.

Methods
We tested the expression of SMCT1 in kidney tissues from DKD patients receiving kidney biopsy as well as diabetes mice. We compared the difference of β-hydroxybutyrate (β-HB) levels in serum, urine and kidney tissues between diabetic mice and control. Using recombinant adeno-associated viral vector containing SMCT1 (encoded by Slc5a8 gene), we tested the effect of SMCT1 upregulation on microalbuminuria as well as its effects on mitochondrial energy metabolism in diabetic mice. Then we investigated the role of SMCT1 and its β-HB reabsorption function in maintaining the physiological function of renal tubular using renal tubule-specific Slc5a8 gene knockout mice. Transcriptomes and proteomics analysis were used to explore the underlying mechanism.

Results
SMCT1 downregulation was found in DKD patients as well as in diabetic mice. Moreover, diabetic mice had a decreased renal β-HB level compared with control, and SMCT1 upregulation could improve microalbuminuria and mitochondrial energy metabolism. In renal tubule–specific Slc5a8 gene knockout mice, microalbuminuria occurred early at 24 weeks of age, accompanied by ATP shortage and metabolic reprogramming in the kidney; however, supplementation with β-HB precursor substance 1,3-butanediol in food alleviated kidney damage as well as energy metabolic reprogramming.

Conclusions
Decreased SMCT1 expression and its ketone reabsorption function play an important role in the occurrence of DKD. SMCT1 may be a new promising target in treating DKD.
Recommended calcium intake in adults and children with chronic kidney disease—a European consensus statement
Authors: Evenepoel Pieter , Jørgensen Hanne Skou , Bover Jordi , Davenport Andrew , Bacchetta Justine , Haarhaus Mathias , Hansen Ditte , Gracia-Iguacel Carolina , Ketteler Markus , McAlister Louise , White Emily , Mazzaferro Sandro , Vervloet Marc , Shroff Rukshana 
Published: September 2023

ABSTRACT
Mineral and bone disorders (MBD) are common in patients with chronic kidney disease (CKD), contributing to significant morbidity and mortality. For several decades, the first-line approach to controlling hyperparathyroidism in CKD was by exogenous calcium loading. Since the turn of the millennium, however, a growing awareness of vascular calcification risk has led to a paradigm shift in management and a move away from calcium-based phosphate binders. As a consequence, contemporary CKD patients may be at risk of a negative calcium balance, which, in turn, may compromise bone health, contributing to renal bone disease and increased fracture risk. A calcium intake below a certain threshold may be as problematic as a high intake, worsening the MBD syndrome of CKD, but is not addressed in current clinical practice guidelines. The CKD-MBD and European Renal Nutrition working groups of the European Renal Association (ERA), together with the CKD-MBD and Dialysis working groups of the European Society for Pediatric Nephrology (ESPN), developed key evidence points and clinical practice points on calcium management in children and adults with CKD across stages of disease. These were reviewed by a Delphi panel consisting of ERA and ESPN working groups members. The main clinical practice points include a suggested total calcium intake from diet and medications of 800–1000 mg/day and not exceeding 1500 mg/day to maintain a neutral calcium balance in adults with CKD. In children with CKD, total calcium intake should be kept within the age-appropriate normal range. These statements provide information and may assist in decision-making, but in the absence of high-level evidence must be carefully considered and adapted to individual patient needs.