bluuebunny/crossref_metadata_2025 huggingface dataset:
Fat mass and obesity-associated protein inhibit the pathology of rheumatoid arthritis through the NSUN2/SFRP1/Wnt/β-catenin signal axis
Authors: Huang Yurong , Xu Pengfei , Liao Faxue , Ca Huibo , Wang Xiaomei , Wang Xiao , Chang Jun , Miao Chenggui
Published: January 2024

Objectives

The purpose of this study is to investigate whether fat mass and obesity-associated protein (FTO) and NOL1/NOP2/Sun domain family member 2 (NSUN2) mediated RNA methylation is associated with RA pathology.

Methods

We studied the anti-rheumatoid arthritis (RA) mechanism mediated by FTO and NSUN2 in RA samples and collagen-induced arthritis (CIA) rats using real time qPCR (RT-qPCR), western blot, immunofluorescence, and other methods.

Key findings

The expression of NSUN2 was significantly increased in both RA patients and CIA rats compared with normal controls. Knockdown of NSUN2 blocked the Wnt/β-catenin signaling pathway and inhibited RA pathological factors such as MMP3, fibronectin, and interleukins. FTO overexpression inhibited RA by inhibiting the expression of NSUN2, up-regulating the level of SFRP1 protein, and blocking the Wnt/β-catenin signaling pathway. NSUN2 overexpression interfered with the inhibitory effects of FTO on the Wnt/β-catenin signaling pathway and RA pathology, which further verified that FTO inhibited RA through the NSUN2/SFRP1/Wnt/β-catenin signal axis.

Conclusions

FTO and NSUN2 are important factors of RA, and this work provides new potential diagnostic biomarkers and therapeutic targets for RA. We also reveal a gene expression regulation pattern of the interaction between m6A and m5C. revealing the pathogenesis of RA from the perspective of RNA methylation.
Oligo/polysaccharides from Cyathula officinalis and Achyranthes bidentata: a review of structures and bioactivities
Authors: Chai Jun-Hong , He Ting-Ting , Jiang Si-Liang , Zhu Xin-Hua , Zhang Qing-Yu , Ji Ming-Chi , Liang Jun , Xia Yong-Gang
Published: January 2024

Objectives

Oligo-/polysaccharides from Cyathula officinalis Kuan (COPs) and Achyranthes bidentata Blume (ABPs) have attracted researchers’ attention in the fields of healthy food supplements and traditional Chinese medicine (Niúxī) due to their multiple bioactivities combined with their nontoxic and highly biocompatible nature. The purpose of this paper was to provide a systematic and comprehensive overview of the extraction, purification, and structural analysis methods, chemical characteristics, biological activities, and structure bioactivity relationship. Furthermore, the possible development trends and perspectives for future research, and traditional uses of Niúxī are also summarized.

Methods

All the information was gathered from a library search and scientific databases.

Key findings

Although COPs and ABPs are derived from different plants, they have similar structural features in type, structure, and glycosidic linkage patterns and biological activities in vivo and in vitro. However, there are differences in monosaccharide compositions, which can be used as an identification mark.

Conclusions

As traditional Chinese herbal medicine, C. officinalis and A. bidentata have similar pharmacological activities. The COPs and ABP possess wide pharmacological effects such as antitumor, antioxidant, anti-osteoporosis, and anti-inflammatory. Meanwhile, the biological activity and structure–activity relationship of purified COPs and ABPs are less studied, future research should focus on them.
Phloretin: a comprehensive review of its potential against diabetes and associated complications
Authors: Shelke Vishwadeep , Kale Ajinath , Kulkarni Yogesh A , Gaikwad Anil Bhanudas
Published: January 2024

Objectives

Phloretin is ubiquitous in apples (Malus domestica) and other fruits and has potential antidiabetic properties. Considering the preclinical potential of phloretin, its transition to clinical observations has unintentionally been neglected, particularly within the diabetic population. Furthermore, a comprehensive understanding of its pharmacokinetics remains elusive. This review seeks to offer valuable insights into phloretin’s physical properties, pharmacokinetics, and pharmacodynamics, aiming to unveil opportunities for additional research on its therapeutic potential in the context of diabetes.

Key findings

All pharmacokinetic reports of phloretin confirm that the utilization of phloretin gets enhanced during diabetic conditions. Phloretin targets pathomechanisms such as glucose transporter 4 (GLUT4) and peroxisome proliferator’s activity-activated receptor-γ (PPAR-γ) to decrease insulin resistance in diabetic conditions. Moreover, phloretin targets inflammatory, oxidative, and apoptotic signaling to minimize the progression of diabetes-associated macro- and microvascular complications.

The pleiotropic antidiabetic action of phloretin is mainly dependent on its pharmacokinetics. Nevertheless, further investigation into the altered pharmacokinetics of phloretin during diabetic conditions is essential. Additionally, the results derived from clinical studies utilized apples, apple extract, and supplements containing phloretin. Greater emphasis should be placed on future clinical studies to assess the potential of phloretin as a standalone compound.
Modelling urban/rural fractions in low- and middle-income countries
Authors: Wu Yunhan , Wakefield Jon
Published: January 2024

In low- and middle-income countries, household surveys are the most reliable data source to examine health and demographic indicators at the subnational level, an exercise in small area estimation. Model-based unit-level models are favoured for producing the subnational estimates at fine scale, such as the admin-2 level. Typically, the surveys employ stratified 2-stage cluster sampling with strata consisting of an urban/rural designation crossed with administrative regions. To avoid bias and increase predictive precision, the stratification should be acknowledged in the analysis. To move from the cluster to the area requires an aggregation step in which the prevalence surface is averaged with respect to population density. This requires estimating a partition of the study area into its urban and rural components, and to do this we experiment with a variety of classification algorithms, including logistic regression, Bayesian additive regression trees, and gradient boosted trees. Pixel-level covariate surfaces are used to improve prediction. We estimate spatial HIV prevalence in women of age 15–49 in Malawi using the stratification/aggregation method we propose.
Augmenting predictive models in forensic psychiatry with Cultural Consensus Theory
Authors: van den Bergh Don , Schuringa Erwin , Wagenmakers Eric-Jan
Published: January 2024

Forensic psychiatric hospitals regularly monitor the mental health and forensic risk factors of their patients. As part of this monitoring, staff score patients on various items. Common practice is to aggregate these scores across staff members. However, this is suboptimal because it assumes that assessors are interchangeable and that patients are independent. An improvement over averaging scores is the use of Cultural Consensus Theory (CCT), which imposes a hierarchical model across patients, staff members, and items. While accounting for differences between patients and staff members, CCT estimates a ‘true’ score for each patient on each item based on the consensus among staff members. Here, we apply a CCT model to data from a Dutch maximum-security forensic psychiatric centre and use the inferences to predict violent behaviour in patients. The CCT model outpredicts several alternatives, such as random forest and boosted regression trees, albeit by a small margin. We discuss practical limitations and directions for how future monitoring of patients could be adapted to maximize the added value of a CCT-based approach.
Successful management strategy for giant primary hepatic rhabdomyosarcoma in 15-year-old male: a case report
Authors: Brimo Alsaman Muhamad Zakaria , Ghanem Roaa , Nahas Mohamad Ali , Chatty Eyad M , Hasan Hasan A , Othman Zeinab Nabil , Horoub Rafat
Published: January 2024

Primary hepatic rhabdomyosarcoma is an exceedingly rare type of sarcomas. A 15-year-old boy was admitted to the hospital with abdominal pain. Serial investigation showed a giant heterogeneous mass, with a diameter of 15 cm, located in the right lobe of the liver (segment 4a, 4b, 5, 6, 7, 8), with clear margins, non-homogeneous density in computerized tomography and the Positron Emission Tomography Scan Multi Slice revealed a peripherally slightly metabolically active hepatic mass (205 × 134 × 208 mm). Histopathological examination and the Immunohistochemical showed embryonal rhabdomyosarcoma. The management strategy involved multiple cycles of ifosfamide and doxorubicin and monitoring the tumor size, until the tumor size was suitable for the surgery. The management of hepatic rhabdomyosarcoma is a surgical challenge due to the late onset of symptoms, a limited number of reported cases, and poor prognosis. Surgical excision is the treatment of choice for primary hepatic rhabdomyosarcoma and combination between chemotherapy, surgery showed good results.
Nuss procedure for the treatment of pectus excavatum with dyspnea following oropharyngeal cancer surgery: a case report
Authors: Masai Kyohei , Nakai Taketo , Okubo Yu , Kaseda Kaoru , Hishida Tomoyuki , Asakura Keisuke
Published: January 2024

Pectus excavatum (PE) causes cardiopulmonary dysfunction depending on the degree and form of the depression. The patient was a 74-year-old woman with a history of PE. Fourteen years ago, a total glossolaryngectomy was performed for oropharyngeal cancer. Two years later, the patient gradually experienced difficulty in breathing. Computed tomography (CT) revealed severe PE and right main bronchial stenosis. We performed a Nuss procedure for PE repair to surgically release the stenosis of the right main bronchus. Postoperative chest CT showed improvement in the sternal depression and right main bronchial stenosis. Furthermore, shortness of breath was relieved postoperatively. Oropharyngeal cancer surgery may cause tracheal support disruption, leading to leftward shift and severe stenosis of the right main bronchus due to sternum depression. This is an important report regarding respiratory distress caused by a combination of PE and post-oropharyngeal cancer surgery.
Surgical resection of isolated portohepatic melanoma metastases—a case report
Authors: Sidhu Tejminder S , Jhamb Shaurya , Ben David Matan M
Published: January 2024

Metastatic melanoma is a significant public health issue in Australia and New Zealand. Although melanoma commonly metastasises to the liver, isolated hepatic metastases are rare, with isolated metastasis to portohepatic lymph nodes being scarce. As such, the optimal management strategy for this subset of patients remains unclear. Here, we present a case of a patient with isolated portohepatic metastases management with a combination neoadjuvant immunotherapy and surgical resection.
The ascorbate–glutathione cycle coming of age
Authors: Foyer Christine H , Kunert Karl
Published: January 2024

Concepts regarding the operation of the ascorbate–glutathione cycle and the associated water/water cycle in the processing of metabolically generated hydrogen peroxide and other forms of reactive oxygen species (ROS) are well established in the literature. However, our knowledge of the functions of these cycles and their component enzymes continues to grow and evolve. Recent insights include participation in the intrinsic environmental and developmental signalling pathways that regulate plant growth, development, and defence. In addition to ROS processing, the enzymes of the two cycles not only support the functions of ascorbate and glutathione, they also have ‘moonlighting’ functions. They are subject to post-translational modifications and have an extensive interactome, particularly with other signalling proteins. In this assessment of current knowledge, we highlight the central position of the ascorbate–glutathione cycle in the network of cellular redox systems that underpin the energy-sensitive communication within the different cellular compartments and integrate plant signalling pathways.
Competitiveness of reutericyclin producing and nonproducing Limosilactobacillus reuteri in food and intestinal ecosystems: a game of rock, paper, and scissors?
Authors: Lin Xiaoxi B , Liu Tingting , Schmaltz Robert , Ramer-Tait Amanda E , Walter Jens W , Gänzle Michael G
Published: January 2024

The ecological relationships among antimicrobial producing, resistant, and sensitive strains have been proposed to follow rock-paper-scissors dynamics, but evidence is mainly based on Gram-negative bacteriocins in vitro. The ecological relevance of antimicrobials in vivo or in situ has not been systematically studied. This study therefore aimed to analyze binary and ternary competitions among reutericyclin-producing strain Limosilactobacillus reuteri TMW1.656, its reutericyclin-resistant, nonproducing isogenic derivative L. reuteri TMW1.656∆rtcN, and the reutericyclin-sensitive, nonproducing L. reuteri TMW1.656∆rtcN∆rtcT in vitro (liquid culture and static plate), in situ (sourdough fermentation), and in vivo (gut of germ-free mice). In liquid culture, L. reuteri TMW1.656 had a higher fitness than TMW1.656∆rtcN and TMW1.656∆rtcN∆rtcT. Limosilactobacillus reuteri TMW1.656∆rtcN∆rtcT had a higher fitness than TMW1.656∆rtcN. On agar plates, L. reuteri TMW1.656 had a higher fitness than TMW1.656∆rtcN∆rtcT. In situ, reutericyclin production and resistance had no influence on the fitness of the strains. In vivo, TMW1.656 had an advantage over TMW1.656∆rtcN and TMW1.656∆rtcN∆rtcT. Ternary competitions showed reutericyclin production was ecologically beneficial in all ecosystems. The findings support the ecological importance of reutericyclin in a variety of environments/niches, providing an explanation for the acquisition of the reutericyclin gene cluster in L. reuteri and its contribution to the ecological fitness of Streptococcus mutans.
Detection of Scedosporium spp.: Colonizer or pathogen? A retrospective analysis of clinical significance and management in a large tertiary center
Authors: Reinhold Ilana , Quiblier Chantal , Blaser Frank , Bögeholz Jan , Imkamp Frank , Schuurmans Macé M , Soyka Michael B , Zbinden Reinhard , Mueller Nicolas J
Published: January 2024

Infections with Scedosporium spp. are emerging in the past two decades and are associated with a high mortality rate. Microbiological detection can be associated with either colonization or infection. Evolution from colonization into infection is difficult to predict and clinical management upon microbiological detection is complex. Microbiological samples from 2015 to 2021 were retrospectively analyzed in a single tertiary care center. Classification into colonization or infection was performed upon first microbiological detection. Clinical evolution was observed until July 2023. Further diagnostic procedures after initial detection were analyzed. Among 38 patients with microbiological detection of Scedosporium spp., 10 were diagnosed with an infection at the initial detection and two progressed from colonization to infection during the observation time. The main sites of infection were lung (5/12; 41.6%) followed by ocular sites (4/12; 33.3%). Imaging, bronchoscopy or biopsies upon detection were performed in a minority of patients. Overall mortality rate was similar in both groups initially classified as colonization or infection [30.7% and 33.3%, respectively (P = 1.0)]. In all patients where surgical debridement of site of infection was performed (5/12; 42%); no death was observed. Although death occurred more often in the group without eradication (3/4; 75%) compared with the group with successful eradication (1/8; 12.5%), statistical significance could not be reached (P = 0.053). As therapeutic management directly impacts patients’ outcome, a multidisciplinary approach upon microbiological detection of Scedosporium spp. should be encouraged. Data from larger cohorts are warranted in order to analyze contributing factors favoring the evolution from colonization into infection.
Magnetic field amplification in cosmological zoom simulations from dwarf galaxies to galaxy groups
Authors: Pakmor Rüdiger , Bieri Rebekka , van de Voort Freeke , Werhahn Maria , Fattahi Azadeh , Guillet Thomas , Pfrommer Christoph , Springel Volker , Talbot Rosie Y
Published: January 2024

Magnetic fields are ubiquitous in the Universe. Recently, cosmological simulations of galaxies have successfully begun to incorporate magnetic fields and their evolution in galaxies and their haloes. However, so far they have mostly focused on Milky Way-like galaxies. Here, we analyse a sample of high-resolution cosmological zoom simulations of disc galaxies in haloes with mass ${M}_\rm {200c}$ from $10^{10}$ to $10^{13}\, \rm {M}_\odot$, simulated with the Auriga galaxy formation model. We show that with sufficient numerical resolution the magnetic field amplification and saturation is converged. The magnetic field strength reaches equipartition with turbulent energy density for galaxies in haloes with ${M}_\rm {200c}\gtrsim 10^{11.5}\, \mathrm{M_\odot }$. For galaxies in less massive haloes, the magnetic field strength saturates at a fraction of equipartition that decreases with decreasing halo mass. For our lowest mass haloes, the magnetic field saturates significantly below 10  per cent of equipartition. We quantify the resolution we need to obtain converged magnetic field strengths and discuss our resolution requirements also in the context of the IllustrisTNG cosmological box simulations. We show that, at z = 0, rotation-dominated galaxies in our sample exhibit for the most part an ordered large-scale magnetic field, with fewer field reversals in more massive galaxies. Finally, we compare the magnetic fields in our cosmological galaxies at z = 0 with simulations of isolated galaxies in a collapsing halo set-up. Our results pave the way for detailed studies of cosmic rays and other physical processes in similar cosmological galaxy simulations that crucially depend on the strength and structure of magnetic fields.
Modeling quasar proximity zones in a realistic cosmological environment with a self-consistent light curve
Authors: Zhou Yihao , Chen Huanqing , Matteo Tiziana Di , Ni Yueying , Croft Rupert A C , Bird Simeon
Published: January 2024

We study quasar proximity zones in a simulation that includes a self-consistent quasar formation model and realistic intergalactic medium (IGM) environments. The quasar host halo is 1013 M⊙ at z = 6, more massive than typical halos studied in previous work. Between 6 < z < 7.5, the quasar luminosity varies rapidly, with a mean magnitude of MUV, mean = −24.8 and the fluctuation reaching up to two orders of magnitude. Using this light curve to post-process the dense environment around the quasar, we find that the proximity zone size (Rp) ranges between 0.5 and 5 pMpc. We show that the light curve variability causes a similar degree of scatter in Rp as does the density fluctuation, both of which result in a standard deviation of ∼0.3 pMpc. The Rp traces the light curve fluctuations closely but with a time delay of ∼104 yr, breaking the correspondence between the Rp and the contemporaneous MUV. This also indicates that we can only infer quasar activity within the past ∼104 yr instead of the integrated lifetime from Rp in the later part of cosmic reionization. Compared with the variable light curve, a constant light curve underestimates the Rp by 13 per cent at the dim end (MUV ∼ −23.5), and overestimates the Rp by 30 per cent at the bright end (MUV ∼ −26). By calculating the Rp generated by a number of quasars, we show that variable light curves predict a wider Rp distribution than lightbulb models, and readily explain the extremely small Rp values that have been observed.
Warm dark matter constraints from the JWST
Authors: Dayal Pratika , Giri Sambit K
Published: January 2024

Warm dark matter (WDM) particles with masses (∼ kilo electronvolt) offer an attractive solution to the small-scale issues faced by the cold dark matter (CDM) paradigm. The delay of structure formation in WDM models and the associated dearth of low-mass systems at high redshifts makes this an ideal time to revisit WDM constraints in light of the unprecedented datasets from the JWST. Developing a phenomenological model based on the halo mass functions in CDM and WDM models, we calculate high redshift ($z \gtrsim 6$), the stellar mass functions (SMF) and the associated stellar mass density (SMD) and the maximum stellar mass allowed in a given volume. We find that: (i) WDM as light as 1.5 keV is already disfavoured by the low-mass end of the SMF (stellar mass $M_* \sim 10^7\,\rm M_\odot$) although caution must be exerted given the impact of lensing uncertainties; (ii) 1.5 keV WDM models predict SMD values that show a steep decrease from 108.8 to $10^{2}\,\rm M_\odot \rm cMpc^{-3}$ from z ∼ 4 to 17 for $M_* \gtrsim 10^8\,\rm M_\odot$; and (iii) the 1.5 keV WDM model predicts a sharp and earlier cut-off in the maximum stellar masses for a given number density (or volume) as compared to CDM or heavier WDM models. For example, with a number density of $10^{-3}\,\rm {cMpc^{-3}}$, 1.5 (3) KeV WDM models do not predict bound objects at $z \gtrsim 12$ (18). Forthcoming JWST observations of multiple blank fields can therefore be used as a strong probe of WDM at an epoch inaccessible by other means.
Pisces VII/Triangulum III – M33’s second dwarf satellite galaxy
Authors: Collins Michelle L M , Karim Noushin , Martinez-Delgado David , Monelli Matteo , Tollerud Erik J , Donatiello Giuseppe , Navabi Mahdieh , Charles Emily , Boschin Walter
Published: January 2024

Pisces VII/Triangulum III (Pisc VII) was discovered in the DESI Legacy Imaging Survey and was shown to be a Local Group dwarf galaxy with follow-up imaging from the 4-m Telescopio Nazionale Galileo. However, this imaging was unable to reach the horizontal branch of Pisc VII, preventing a precision distance measurement. The distance bound from the red giant branch population placed Pisc VII as either an isolated ultra-faint dwarf galaxy or the second known satellite galaxy of Triangulum (M33). Using deep imaging from Gemini GMOS-N, we have resolved the horizontal branch of Pisc VII, and measure a distance of $D=916^{+65}_{-53}$ kpc, making Pisc VII a likely satellite of M33. We also remeasure its size and luminosity from this deeper data, finding $r_{\rm half}=186^{+58}_{-32}$ pc, MV = −6.0 ± 0.3, and $L=2.2^{+0.7}_{-0.5}\times 10^4\, {\rm L}_\odot$. Given its position in the M33 halo, we argue that Pisc VII could support the theory that M33 is on its first infall to the Andromeda system. We also discuss the presence of blue plume and helium burning stars in the colour–magnitude diagram of Pisc VII that are consistent with ages of ∼1.5 Gyr. If these are truly members of the galaxy, it would transform our understanding of how reionization affects the faintest galaxies. Future deep imaging and dynamics could allow significant insight into both the stellar populations of Pisc VII and the evolution of M33.
Hot Jupiter formation in dense star clusters
Authors: Benkendorff L , Flammini Dotti F , Stock K , Cai Maxwell X , Spurzem R
Published: January 2024

Hot Jupiters (HJ) are defined as Jupiter-mass exoplanets orbiting around their host star with an orbital period < 10 d. It is assumed that HJ do not form in-situ but ex-situ. Recent discoveries show that star clusters contribute to the formation of HJ. We present direct N-body simulations of planetary systems in star clusters and analyse the formation of HJ in them. We combine two direct N-body codes: nbody6++gpu for the dynamics of dense star clusters with 32 000 and 64 000 stellar members and lonelyplanets used to follow 200 identical planetary systems around solar mass stars in those star clusters. We use different sets with three, four, or five planets and with the innermost planet at a semimajor axis of 5 or 1 au and follow them for 100 Myr in our simulations. The results indicate that HJs are generated with high efficiency in dense star clusters if the innermost planet is already close to the host star at a semimajor axis of 1 au. If the innermost planet is initially beyond a semimajor axis of 5 au, the probability of a potential HJ ranges between 1.5 and 4.5 per cent. Very dense stellar neighbourhoods tend to eject planets rather than forming HJs. A correlation between HJ formation and angular momentum deficit is not witnessed. Young HJs (tage < 100 Myr) have only been found, in our simulations, in planetary systems with the innermost planet at a semimajor axis of 1 au.
The 2022–2023 accretion outburst of the young star V1741 Sgr
Authors: Kuhn Michael A , Hillenbrand Lynne A , Connelley Michael S , Rich R Michael , Staels Bart , Carvalho Adolfo S , Lucas Philip W , Fremling Christoffer , Karambelkar Viraj R , Lee Ellen , Ahumada Tomás , Ishida Emille E O , De Kishalay , de Souza Rafael S , Kasliwal Mansi M
Published: January 2024

V1741 Sgr (= SPICY 71482/Gaia22dtk) is a Classical T Tauri star on the outskirts of the Lagoon Nebula. After at least a decade of stability, in mid-2022, the optical source brightened by ∼3 mag over 2 months, remained bright until early 2023, then dimmed erratically over the next 4 months. This event was monitored with optical and infrared spectroscopy and photometry. Spectra from the peak (October 2022) indicate an EX Lup-type (EXor) accretion outburst, with strong emission from H i, He i, and Ca ii lines and CO bands. At this stage, spectroscopic absorption features indicated a temperature of T ∼ 4750 K with low-gravity lines (e.g. Ba ii and Sr ii). By April 2023, with the outburst beginning to dim, strong TiO absorption appeared, indicating a cooler T ∼ 3600 K temperature. However, once the source had returned to its pre-outburst flux in August 2023, the TiO absorption and the CO emission disappeared. When the star went into outburst, the source’s spectral energy distribution became flatter, leading to bluer colours at wavelengths shorter than ∼1.6 $\mu$m and redder colours at longer wavelengths. The brightening requires a continuum emitting area larger than the stellar surface, likely from optically thick circumstellar gas with cooler surface layers producing the absorption features. Additional contributions to the outburst spectrum may include blue excess from hotspots on the stellar surface, emission lines from diffuse gas, and reprocessed emission from the dust disc. Cooling of the circumstellar gas would explain the appearance of TiO, which subsequently disappeared once this gas had faded and the stellar spectrum reemerged.
MUSEQuBES: mapping the distribution of neutral hydrogen around low-redshift galaxies
Authors: Dutta Sayak , Muzahid Sowgat , Schaye Joop , Mishra Sapna , Chen Hsiao-Wen , Johnson Sean , Wisotzki Lutz , Cantalupo Sebastiano
Published: January 2024

We present a detailed study of cool, neutral gas traced by Lyα around 4595 z < 0.5 galaxies using stacks of background quasar spectra. The galaxies are selected from our MUSEQuBES low-z survey along with data from the literature. These galaxies, with a median stellar mass of ${\rm log}_{10}(M_*/\rm {\rm M}_{\odot })$ =10.0, are probed by 184 background quasars giving rise to 5054 quasar-galaxy pairs. The median impact parameter is b = 1.5 pMpc (median b/Rvir = 10.4) with 204 (419) quasar-galaxy pairs probing b/Rvir < 1(2). We find excess absorption out to at least ≈15Rvir transverse distance and ≈±600 $\rm km~s^{-1}$ along the line of sight. We show that the median stacked profile for the full sample, dominated by the pairs with b > Rvir, can be explained by a galaxy-absorber two-point correlation function with r0 = 7.6 pMpc and γ = −1.57. There are strong indications that the inner regions (≲Rvir) of the rest equivalent width profile are better explained by a log-linear (or a Gaussian) relation, whereas the outer regions are well described by a power-law, consistent with galaxy-absorber large-scale clustering. Using a sub-sample of 339 galaxies (442 quasar-galaxy pairs, median b/Rvir = 1.6) with star formation rate measurements, we find that the Lyα absorption is significantly stronger for star-forming galaxies compared to passive galaxies, but only within the virial radius. The Lyα absorption at b ≈ Rvir for a redshift-controlled sample peaks at $M_* \sim 10^9~ {\rm {\rm M}_{\odot }}~ (M_{\rm halo} \sim 10^{11}~ \rm {\rm M}_{\odot })$.
Characterization of K2-167 b and CALM, a new stellar activity mitigation method
Authors: de Beurs Zoë L , Vanderburg Andrew , Thygesen Erica , Rodriguez Joseph E , Dumusque Xavier , Mortier Annelies , Malavolta Luca , Buchhave Lars A , Shallue Christopher J , Zieba Sebastian , Kreidberg Laura , Livingston John H , Haywood R D , Latham David W , López-Morales Mercedes , Silva André M
Published: January 2024

We report precise radial velocity (RV) observations of HD 212657 (= K2-167), a star shown by K2 to host a transiting sub-Neptune-sized planet in a 10 d orbit. Using Transiting Exoplanet Survey Satellite (TESS) photometry, we refined the planet parameters, especially the orbital period. We collected 74 precise RVs with the HARPS-N spectrograph between August 2015 and October 2016. Although this planet was first found to transit in 2015 and validated in 2018, excess RV scatter originally limited mass measurements. Here, we measure a mass by taking advantage of reductions in scatter from updates to the HARPS-N Data Reduction System (2.3.5) and our new activity mitigation method called CCF Activity Linear Model (CALM), which uses activity-induced line shape changes in the spectra without requiring timing information. Using the CALM framework, we performed a joint fit with RVs and transits using exofastv2 and find Mp = $6.3_{-1.4}^{+1.4}$  $\, M_{\hbox{$\oplus $}}$ and Rp = $2.33^{+0.17}_{-0.15}$  $\, R_{\hbox{$\oplus $}}$, which places K2-167 b at the upper edge of the radius valley. We also find hints of a secondary companion at a ∼22 d period, but confirmation requires additional RVs. Although characterizing lower mass planets like K2-167 b is often impeded by stellar variability, these systems especially help probe the formation physics (i.e. photoevaporation, core-powered mass-loss) of the radius valley. In the future, CALM or similar techniques could be widely applied to FGK-type stars, help characterize a population of exoplanets surrounding the radius valley, and further our understanding of their formation.
PLATO on the shoulders of TESS: analysing mono-transit planet candidates in TESS data as a prior knowledge for PLATO observations
Authors: Magliano Christian , Covone Giovanni , Nascimbeni Valerio , Inno Laura , Vines Jose I , Kostov Veselin , Fiscale Stefano , Granata Valentina , Montalto Marco , Pagano Isabella , Piotto Giampaolo , Saggese Vito
Published: January 2024

The Transiting Exoplanet Survey Satellite (TESS) and the upcoming mission PLAnetary Transits and Oscillations of stars (PLATO) represent two space-based missions with complementary objectives in the field of exoplanet science. While TESS aims at detecting and characterizing exoplanets around bright and nearby stars on a relative short-period orbit, PLATO will discover a wide range of exoplanets including rocky planets within the habitable zones of their stars. We analyse mono-transit events in TESS data around stars that will or could be monitored by the PLATO mission, offering a unique opportunity to bridge the knowledge gap between the two missions and gain deeper insights into exoplanet demographics and system architectures. We found 48 TESS mono-transit events around stars contained in the all-sky PLATO Input Catalog; of these, at least four will be imaged on the first long-pointing PLATO field, LOPS2. We uniformly vetted this sample to rule out possible false positive detections thus removing 10 signals from the original sample. We developed an analytic method which allows us to estimate both the orbital period and inclination of a mono-transit planet candidate using only the shape of the transit. We derived the orbital period and inclination estimates for 30 TESS mono-transit planet candidates. Finally, we investigated whether these candidates are amenable targets for a CHaracterising ExOPlanets Satellite observing campaign.
Observational evidence for local vertical constraining of H i by molecular cloud complexes
Authors: Nandakumar Meera , Roy Nirupam , Jog Chanda J , Menten Karl M
Published: January 2024

A massive molecular cloud complex represents local gravitational potential that can constrain the vertical distribution of surrounding stars and gas. This pinching effect results in the local corrugation of the scale height of stars and gas which is in addition to the global corrugation of the mid-plane of the disc. For the first time, we report observational evidence for this pinching on the H i vertical structures in the Galactic region (20° < l < 40°), also called W41–W44 region. The H i vertical distribution is modelled by a double Gaussian profile that physically represents a narrow dense gas distribution confined to the mid-plane embedded in a wider diffuse H i. We find that the estimate of the H i scale height distribution of wider components shows corrugated structures at the locations of molecular complexes, as theoretically predicted in literature. While the narrow component is less affected by the pinching, we found a hint of the disc being disrupted by the active dynamics in the local environment of the complex, for example, supernova explosions. Molecular complexes of mass of several $10^6 \rm M_{\odot } $, associated with the mini-starburst region W43 and the supernova remnant W41 show the strongest evidence for the pinching; here a broad trough, with an average width of ∼400 pc and height ∼300 pc, in the disc thickness of the wider component is prominently visible. Searching for similar effect on the stars as well as in the location of other complexes in the Milky Way and other galaxies will be useful to establish this phenomenon more firmly.
Mixing Sinc kernels to improve interpolations in smoothed particle hydrodynamics without pairing instability
Authors: Cabezón Rubén M , García-Senz Domingo
Published: January 2024

The smoothed particle hydrodynamic technique is strongly based on the proper choice of interpolation functions. This statement is particularly relevant for the study of subsonic fluxes and turbulence, where inherent small errors in the averaging procedures introduce excessive damping on the smallest scales. To mitigate these errors, we can increase both the number of interpolating points and the order of the interpolating kernel function. However, this approach leads to a higher computational burden across all fluid regions. Ideally, the development of a single kernel function capable of effectively accommodating varying numbers of interpolating points in different fluid regions, providing good resolution and minimal errors would be highly desirable. In this work, we revisit and extend the main properties of a family of interpolators called Sinc kernels and compare them with the widely used family of Wendland kernels. We show that a linear combination of low- and high-order Sinc kernels generates good-quality interpolators, which are resistant to pairing instability while maintaining good sampling properties in a wide range of neighbour interpolating points, 60 ≤ nb ≤ 400. We show that a particular case of this linear mix of Sincs produces a well-balanced and robust kernel that improves previous results in the Gresho–Chan vortex experiment even when the number of neighbours is not large, while yielding a good convergence rate. Although such a mixing technique is ideally suited for Sinc kernels owing to their excellent flexibility, it can be easily applied to other interpolating families such as the B-splines and Wendland kernels.
Elastic and inelastic cross-sections for 12C + CO2 and 13C + CO2 scattering at superthermal energies
Authors: Gacesa Marko
Published: January 2024

We report elastic and inelastic cross-sections for fast superthermal 12C(3P) and 13C(3P) atoms scattering on 12CO2. The cross-sections were computed using quantum-mechanical rotationally close-coupling formalism with the electronic interaction described by a newly constructed potential energy surface correlating to the lowest energy asymptote of the complex. State-to-state rotational cross-sections, differential cross-sections, and derived transport properties of interest for energy relaxation are also reported. The computed elastic differential cross-sections are found to be strongly anisotropic, show significant energy dependence, and differ by up to 2 percent between the two isotopes of carbon.
A Gaussian-processes approach to fitting for time-variable spherical solar wind in pulsar timing data
Authors: Niţu Iuliana C , Keith Michael J , Tiburzi Caterina , Brüggen Marcus , Champion David J , Chen Siyuan , Cognard Ismaël , Desvignes Gregory , Dettmar Ralf-Jürgen , Grießmeier Jean-Mathias , Guillemot Lucas , Guo Yanjun , Hoeft Matthias , Hu Huanchen , Jang Jiwoong , Janssen Gemma H , Jawor Jedrzej , Karuppusamy Ramesh , Keane Evan F , Kramer Michael , Künsemöller Jörn , Lackeos Kristen , Liu Kuo , Main Robert A , McKee James W , Porayko Nataliya K , Shaifullah Golam M , Theureau Gilles , Vocks Christian
Published: January 2024

Propagation effects are one of the main sources of noise in high-precision pulsar timing. For pulsars below an ecliptic latitude of 5°, the ionized plasma in the solar wind can introduce dispersive delays of order $100\, \mu \mathrm{s}$ around solar conjunction at an observing frequency of 300 MHz. A common approach to mitigate this assumes a spherical solar wind with a time-constant amplitude. However, this has been shown to be insufficient to describe the solar wind. We present a linear, Gaussian-process piecewise Bayesian approach to fit a spherical solar wind of time-variable amplitude, which has been implemented in the pulsar software run_enterprise. Through simulations, we find that the current EPTA+InPTA data combination is not sensitive to such variations; however, solar wind variations will become important in the near future with the addition of new InPTA data and data collected with the low-frequency LOFAR telescope. We also compare our results for different high-precision timing data sets (EPTA+InPTA, PPTA, and LOFAR) of 3 ms pulsars (J0030+0451, J1022+1001, J2145−0450), and find that the solar-wind amplitudes are generally consistent for any individual pulsar, but they can vary from pulsar to pulsar. Finally, we compare our results with those of an independent method on the same LOFAR data of the three millisecond pulsars. We find that differences between the results of the two methods can be mainly attributed to the modelling of dispersion variations in the interstellar medium, rather than the solar wind modelling.
Magnetic field breakout from white dwarf crystallization dynamos
Authors: Blatman Daniel , Ginzburg Sivan
Published: January 2024

A convective dynamo operating during the crystallization of white dwarfs is one of the promising channels to produce their observed strong magnetic fields. Although the magnitude of the fields generated by crystallization dynamos is uncertain, their timing may serve as an orthogonal test of this channel’s contribution. The carbon–oxygen cores of $M\approx 0.5-1.0\, {\rm M}_{\odot }$ white dwarfs begin to crystallize at an age tcryst ∝ M−5/3, but the magnetic field is initially trapped in the convection zone – deep inside the CO core. Only once a mass of mcryst has crystallized, the convection zone approaches the white dwarf’s helium layer, such that the magnetic diffusion time through the envelope shortens sufficiently for the field to break out to the surface, where it can be observed. This breakout time is longer than tcryst by a few Gyr, scaling as tbreak ∝ tcrystf−1/2, where f ≡ 1 − mcryst/M depends on the white dwarf’s initial C/O profile before crystallization. The first appearance of strong magnetic fields B ≳ 1 MG in volume-limited samples approximately coincides with our numerically computed tbreak(M) – potentially signalling crystallization dynamos as a dominant magnetization channel. However, some observed magnetic white dwarfs are slightly younger, challenging this scenario. The dependence of the breakout process on the white dwarf’s C/O profile implies that magnetism may probe the CO phase diagram, as well as uncertainties during the core helium burning phase in the white dwarf’s progenitor, such as the 12C(α, γ)16O nuclear reaction.
Chemical evolution of local post-starburst galaxies: implications for the mass–metallicity relation
Authors: Leung Ho-Hin , Wild Vivienne , Papathomas Michail , Carnall Adam , Zheng Yirui , Boardman Nicholas , Wang Cara , Johansson Peter H
Published: January 2024

We use the stellar fossil record to constrain the stellar metallicity evolution and star-formation histories of the post-starburst (PSB) regions within 45 local PSB galaxies from the MaNGA survey. The direct measurement of the regions’ stellar metallicity evolution is achieved by a new two-step metallicity model that allows for stellar metallicity to change at the peak of the starburst. We also employ a Gaussian process noise model that accounts for correlated errors introduced by the observational data reduction or inaccuracies in the models. We find that a majority of PSB regions (69 per cent at >1σ significance) increased in stellar metallicity during the recent starburst, with an average increase of 0.8 dex and a standard deviation of 0.4 dex. A much smaller fraction of PSBs are found to have remained constant (22 per cent) or declined in metallicity (9 per cent, average decrease 0.4 dex, standard deviation 0.3 dex). The pre-burst metallicities of the PSB galaxies are in good agreement with the mass–metallicity (MZ) relation of local star-forming galaxies. These results are consistent with hydrodynamic simulations, which suggest that mergers between gas-rich galaxies are the primary formation mechanism of local PSBs, and rapid metal recycling during the starburst outweighs the impact of dilution by any gas inflows. The final mass-weighted metallicities of the PSB galaxies are consistent with the MZ relation of local passive galaxies. Our results suggest that rapid quenching following a merger-driven starburst is entirely consistent with the observed gap between the stellar mass–metallicity relations of local star-forming and passive galaxies.
Cassini’s CDA observes a variety of dust populations just outside Saturn’s main rings
Authors: Linti Simon , Khawaja Nozair , Hillier Jon K , Nölle Lenz , Fischer Christian , Hsu Hsiang-Wen , Srama Ralf , Postberg Frank
Published: January 2024

Before the end of its mission, the Cassini spacecraft orbited Saturn in a series of highly inclined elliptical ‘Ring-Grazing’ orbits (RGO). During the RGO, the spacecraft passed repeatedly through the ring plane outside the F ring, near the orbits of Janus and Epimetheus, at an average relative speed of ∼20 km s–1. For the first time, Cassini’s Cosmic Dust Analyser (CDA) directly sampled dust particles from this region. Here, we analyse the compositions of dust grains sampled within ±15 min relative to nine ring plane crossings of the RGO. The compositions of most analysed RGO grains are similar to those of E ring ice grains, implying that the E ring extends to within at least 2.45 Saturn radii (RS) of Saturn. The compositional distribution of these grains point at a similar average period (decades) since ejection from Enceladus as of particles in the outer E ring (beyond 8 RS). Higher fractions of larger grains are found near the orbits of Janus and Epimetheus, which probably represent ejecta from these moons. Most of these grains have compositions similar to the background E ring grains, indicating that E ring material is coating the surfaces of Janus and Epimetheus. We also report the detection of several types of mineral grains on prograde orbits, one of which, a water ice/silicate mixture, has never been observed by CDA elsewhere. These mineral grains appear to have a different origin from the E ring, and may arise from nearby moons, the F ring, or main rings.
Exploring the influence of the ‘Smiley Sun’ on the dynamics of inner solar corona and near-Earth space environment
Authors: Jain Richa N , Choudhary R K , Imamura T
Published: January 2024

The image captured by SDO/AIA (Solar Dynamics Observatory) in the 193 Å ultraviolet channel from 2022 October 25–27, unveiled a remarkable trio of dark coronal holes near the heliocentric equator, forming a distinctive smiling face. Serendipitously, during that period, coronal radio science experiments were being conducted using the Akatsuki spacecraft to investigate turbulence regimes in the inner-middle corona and track the acceleration of solar wind streams. By analysing Doppler frequency residuals, we derived valuable insights into plasma turbulence characteristics, estimated electron density fluctuations and flow speeds using isotropic quasi-static turbulence methods. The analysis consistently unveiled a shallow turbulence spectrum and flow speeds ranging from 180 to 400 km s−1 at heliocentric distances of 3–9 Rs. During this period, the solar wind flow speed, recorded at the L1 point near Earth, was of the order of 600–650 km s−1. This presented a unique opportunity to delve into turbulence within the inner corona and explore the mechanisms responsible for energizing and accelerating high-speed streams emanating from these trans-equatorial coronal holes. The study also suggests the innovative use of spacecraft signals as radio beacons for enhanced forecasting of potential space weather events triggered by Earth-directed high-speed solar wind streams.
Mixed Patterns of Intergenerational DNA Methylation Inheritance in Acropora
Authors: Peterson Christopher R , Scott Carly B , Ghaffari Rashin , Dixon Groves , Matz Mikhail V
Published: January 2024

For sessile organisms at high risk from climate change, phenotypic plasticity can be critical to rapid acclimation. Epigenetic markers like DNA methylation are hypothesized as mediators of plasticity; methylation is associated with the regulation of gene expression, can change in response to ecological cues, and is a proposed basis for the inheritance of acquired traits. Within reef-building corals, gene-body methylation (gbM) can change in response to ecological stressors. If coral DNA methylation is transmissible across generations, this could potentially facilitate rapid acclimation to environmental change. We investigated methylation heritability in Acropora, a stony reef-building coral. Two Acropora millepora and two Acropora selago adults were crossed, producing eight offspring crosses (four hybrid, two of each species). We used whole-genome bisulfite sequencing to identify methylated loci and allele-specific alignments to quantify per-locus inheritance. If methylation is heritable, differential methylation (DM) between the parents should equal DM between paired offspring alleles at a given locus. We found a mixture of heritable and nonheritable loci, with heritable portions ranging from 44% to 90% among crosses. gBM was more heritable than intergenic methylation, and most loci had a consistent degree of heritability between crosses (i.e. the deviation between parental and offspring DM were of similar magnitude and direction). Our results provide evidence that coral methylation can be inherited but that heritability is heterogenous throughout the genome. Future investigations into this heterogeneity and its phenotypic implications will be important to understanding the potential capability of intergenerational environmental acclimation in reef building corals.