bluuebunny/crossref_metadata_2025_split huggingface dataset:
Quantifying the impact of AGN feedback on the large-scale matter distribution using two- and three-point statistics
Authors: Saha Bipradeep , Bose Sownak 
Published: October 2024

ABSTRACT
Feedback from active galactic nuclei (AGN) plays a critical role in shaping the matter distribution on scales comparable to and larger than individual galaxies. Upcoming surveys such as Euclid and Legacy Survey of Space and Time aim to precisely quantify the matter distribution on cosmological scales, making a detailed understanding of AGN feedback effects essential. Hydrodynamical simulations provide an informative framework for studying these effects, in particular by allowing us to vary the parameters that determine the strength of these feedback processes and, consequently, to predict their corresponding impact on the large-scale matter distribution. We use the EAGLE simulations to explore how changes in subgrid viscosity and AGN heating temperature affect the matter distribution, quantified via two- and three-point correlation functions, as well as higher order cumulants of the matter distribution. We find that varying viscosity has a small impact ($\approx 10~{{\ \rm per\ cent}}$) on scales larger than $1\,{\it h}^{-1}$ Mpc, while changes to the AGN heating temperature lead to substantial differences, with up to 70 per cent variation in gas clustering on small scales ($\lesssim 1\,{\it h}^{-1}$ Mpc). By examining the suppression of the power spectrum as a function of time, we identify the redshift range $z = 1.5{-}1$ as a key epoch where AGN feedback begins to dominate in these simulations. The three-point function provides complementary insight to the more familiar two-point statistics, and shows more pronounced variations between models on the scale of individual haloes. On the other hand, we find that effects on even larger scales are largely comparable.
K2-370 b: a strongly irradiated sub-Neptune transiting a very active solar-type star
Authors: Sozzetti A , Damasso M , Fernández Fernández J , Mortier A , John A Anna , Cubillos P E , Wilson T G , Pinamonti M , Nielsen L , Bonomo A S , Freckelton A V , Cameron A Collier , Armstrong D , Vanderburg A , Bayliss D , Dumusque X , Ghedina A , Keniger M A F , Latham D W , López Morales M , Malavolta L , Osborn A , Pepe F , Rabino R , Strøm P A , Udry S , Wheatley P 
Published: October 2024

ABSTRACT
We report on the detailed characterization of K2-370 b, a transiting sub-Neptune on a 2.14-d orbit around the chromospherically active G-type dwarf HD 284521 ($T_\mathrm{eff} = 5662\pm 44$ K, $\lt \log R^\prime _{\rm HK}\gt =-4.49$). The system parameters are derived based on a global fit to K2, TESS and CHEOPS photometry, and HARPS-N and HARPS radial velocities (RVs). A Gaussian process regression analysis is performed simultaneously to the orbital fit of the RVs of K2-370 to effectively model the strong stellar rotation signal with a period of $13.5\pm 0.05$ d and measure the planetary RV signal with semi-amplitude $K_{\rm b}=5.6\pm 0.7$ m s$^{-1}$. We find that K2-370 b has a radius of $2.67\pm 0.05$ ${\rm R}_{\rm{\oplus }}$ and a mass of $11.1\pm 1.4$ ${\rm M}_{\rm{\oplus }}$. With an estimated equilibrium temperature $T_\mathrm{eq}\sim 1480$ K, K2-370 b is the second-hottest sub-Neptune with a highly precise mass determination around primaries with $T_\mathrm{eff}\gt 5500$ K. The resulting density of $3.2\pm 0.4$ g cm$^{-3}$ implies that K2-370 b either retains a significant ($\sim 2~{{\ \rm per\ cent}}$ by mass) H-rich atmosphere or its interior contains a high ($\sim 40~{{\ \rm per\ cent}}$) water–mass fraction.
Sensitivity of Bayesian 21 cm power spectrum estimation to foreground model errors
Authors: Burba Jacob , Bull Philip , Wilensky Michael J , Kennedy Fraser , Garsden Hugh , Glasscock Katrine A 
Published: October 2024

ABSTRACT
Power spectrum estimators are an important tool in efforts to detect the 21 cm brightness temperature fluctuations from neutral hydrogen at early times. An initial detection will likely be statistical in nature, meaning that it will not be possible to make a coherent map of the brightness temperature fluctuations; instead, only their variance will be measured against a background of noise and residual systematic effects. Optimal quadratic estimator-based methods often apply an inverse covariance weighting to the data. However, inaccurate covariance modelling can lead to reduced sensitivity and, in some cases, severe signal loss. We recently proposed a Bayesian method to jointly estimate the 21 cm fluctuations, their power spectrum, and foreground emission. Instead of requiring a fixed a priori estimate of the covariance, we estimate the covariance as part of the inference. Choices of parametrization, particularly of the foregrounds, are subject to model errors and could lead to biases and other ill effects if not properly controlled. In this paper, we investigate the effects of inaccurate foreground models on 21 cm power spectrum recovery. Using simulated visibilities, we find that, even in the most extreme scenarios tested, our approach is capable of recovering 21 cm delay power spectrum estimates consistent with a known input signal for delays $\gtrsim 300$ ns ($\sim$88 per cent of the available Fourier modes). This is true even when using foreground models derived from modified foreground catalogues containing spatial and spectral perturbations at the quoted level of uncertainty on our foreground catalogues.
Local stability of differential rotation in magnetized radiation zones and the solar tachocline
Authors: Dymott R W , Barker A J , Jones C A , Tobias S M 
Published: October 2024

ABSTRACT
We study local magnetohydrodynamical instabilities of differential rotation in magnetized, stably stratified regions of stars and planets using a Cartesian Boussinesq model. We consider arbitrary latitudes and general shears (with gravity direction misaligned from this by an angle $\phi$), to model radial ($\phi =0$), latitudinal ($\phi =\pm 90^\circ$), and mixed differential rotations, and study both non-diffusive [including magnetorotational instability (MRI) and Solberg–Høiland instability] and diffusive instabilities [including Goldreich–Schubert–Fricke (GSF) and MRI with diffusion]. These instabilities could drive turbulent transport and mixing in radiative regions, including the solar tachocline and the cores of red giant stars, but their dynamics are incompletely understood. We revisit linear axisymmetric instabilities with and without diffusion and analyse their properties in the presence of magnetic fields, including deriving stability criteria and computing growth rates, wave vectors, and energetics, both analytically and numerically. We present a more comprehensive analysis of axisymmetric local instabilities than prior work, exploring arbitrary differential rotations and diffusive processes. The presence of a magnetic field leads to stability criteria depending upon angular velocity rather than angular momentum gradients. We find MRI operates for much weaker differential rotations than the hydrodynamic GSF instability, and that it typically prefers much larger length-scales, while the GSF instability is impeded by realistic strength magnetic fields. We anticipate MRI to be more important for turbulent transport in the solar tachocline than the GSF instability when $\phi \gt 0$ in the Northern (and vice versa in the Southern) hemisphere, though the latter could operate just below the convection zone when MRI is absent for $\phi \lt 0$.
Ice origins of OCS and chemistry of CS2-bearing ice mantles
Authors: Martín-Doménech Rafael , Öberg Karin I , Muñoz Caro Guillermo M , Carrascosa Héctor , Fuente Asunción , Rajappan Mahesh 
Published: October 2024

ABSTRACT
Understanding the formation of carbonyl sulfide (OCS) in interstellar ices is key to constrain the sulfur chemistry in the interstellar medium (ISM), since it is the only ice S-bearing molecule securely detected thus far. Two general pathways for OCS formation have been proposed: sulfurization of CO (CO + S) and oxidation of CS (CS + O), but their relative contribution in interstellar ices remains unconstrained. We have evaluated the contribution of both pathways to OCS formation upon energetic processing in isotopically labelled CO$_2$:CS$_2$ and CO:CS$_2$ ice samples at 7$-$50 K. Our results indicated that formation of OCS through the CS + O pathway was more favourable than through the CO + S pathway, as previously suggested by theoretical calculations. In addition, its relative contribution increased at higher temperatures. Therefore, this pathway could play a role in the ice formation of OCS, especially in warm regions where CO is expected to be preferentially in the gas phase. At the same time, we have explored the chemistry of CS$_2$-bearing, CO$_2$-, CO-, and also H$_2$O-rich ices, that could be relevant to the sulfur interstellar chemistry. We observed formation of a variety of S-bearing products in addition to OCS, including SO$_2$, C$_3$S$_2$, and S$_2$. However, a significant fraction of sulfur was not detected at the end of the experiments, and could be locked in long, undetectable sulfur allotropes, one of the potential carriers of the missing sulfur in the dense ISM.
Long-term evolution of spin and other properties of neutron star low-mass X-ray binaries: implications for millisecond X-ray pulsars
Authors: Kar Abhijnan , Ojha Pulkit , Bhattacharyya Sudip 
Published: October 2024

ABSTRACT
A neutron star (NS) accreting matter from a companion star in a low-mass X-ray binary (LMXB) system can spin up to become a millisecond pulsar (MSP). Properties of many such MSP systems are known, which is excellent for probing fundamental aspects of NS physics when modelled using the theoretical computation of NS LMXB evolution. Here, we systematically compute the long-term evolution of NS, binary, and companion parameters for NS LMXBs using the stellar evolution code mesa. We consider the baryonic to gravitational mass conversion to calculate the NS mass evolution and show its cruciality for the realistic computation of some parameters. With computations using many combinations of parameter values, we find the general nature of the complex NS spin frequency ($\nu$) evolution, which depends on various parameters, including accretion rate, fractional mass-loss from the system, and companion star magnetic braking. Further, we utilize our results to precisely match some main observed parameters, such as $\nu$, orbital period ($P_{\rm orb}$), etc., of four accreting millisecond X-ray pulsars (AMXPs). By providing the $\nu$, $P_{\rm orb}$, and the companion mass spaces for NS LMXB evolution, we indicate the distribution and plausible evolution of a few other AMXPs. We also discuss the current challenges in explaining the parameters of AMXP sources with brown dwarf companions and indicate the importance of modelling the transient accretion in LMXBs as a possible solution.
Shear-driven magnetic buoyancy in the solar tachocline: dependence of the mean electromotive force on diffusivity and latitude
Authors: Duguid Craig D , Bushby Paul J , Wood Toby S 
Published: October 2024

ABSTRACT
The details of the dynamo process that is responsible for driving the solar magnetic activity cycle are still not fully understood. In particular, while differential rotation provides a plausible mechanism for the regeneration of the toroidal (azimuthal) component of the large-scale magnetic field, there is ongoing debate regarding the process that is responsible for regenerating the Sun’s large-scale poloidal field. Our aim is to demonstrate that magnetic buoyancy, in the presence of rotation, is capable of producing the necessary regenerative effect. Building upon our previous work, we carry out numerical simulations of a local Cartesian model of the tachocline, consisting of a rotating, fully compressible, electrically conducting fluid with a forced shear flow. An initially weak, vertical magnetic field is sheared into a strong, horizontal magnetic layer that becomes subject to magnetic buoyancy instability. By increasing the Prandtl number we lessen the back reaction of the Lorentz force on to the shear flow, maintaining stronger shear and a more intense magnetic layer. This in turn leads to a more vigorous instability and a much stronger mean electromotive force, which has the potential to significantly influence the evolution of the mean magnetic field. These results are only weakly dependent upon the inclination of the rotation vector, i.e. the latitude of the local Cartesian model. Although further work is needed to confirm this, these results suggest that magnetic buoyancy in the tachocline is a viable poloidal field regeneration mechanism for the solar dynamo.
Determining star formation rates in AGN hosts from strong optical emission lines
Authors: de Mellos Maitê S Z , Riffel Rogemar A , Schimoia Jaderson S , Rembold Sandro B , Riffel Rogério , Storchi-Bergmann Thaisa , Wylezalek Dominika , Ilha Gabriele S , Albán Marco , Dors Oli L , Gatto Lara , Krabbe Angela C , Mallmann Nicolas D , Trevisan Marina 
Published: October 2024

ABSTRACT
The influence of Active Galactic Nuclei (AGN) on star formation within their host galaxies remains a topic of intense debate. One of the primary challenges in quantifying the star formation rate (SFR) within AGN hosts arises from the prevalent assumption in most methodologies, which attribute gas excitation to young stars alone. However, this assumption does not consider the contribution of the AGN to the ionization of the gas in their environment. To address this issue, we evaluate the use of strong optical emission lines to obtain the SFR surface density ($\Sigma {{\rm SFR_{AGN}}}$) in regions predominantly ionized by an AGN, using a sample of 293 AGN hosts from the MaNGA survey, with SFR measurements available through stellar population fitting. We propose calibrations involving the H$\alpha$ and [O iii]$\lambda$5007 emission lines, which can be used to determine $\Sigma {{\rm SFR_{AGN}}}$, resulting in values consistent with those estimated through stellar population fitting.
Exploring faint white dwarfs and the luminosity function with Subaru HSC and SDSS in Stripe 82
Authors: Qiu Tian , Takada Masahiro , Yasuda Naoki , Tokiwa Akira , Kashiyama Kazumi , Suzuki Yoshihisa , Hotokezaka Kenta 
Published: October 2024

ABSTRACT
We present 5080 white dwarf (WD) candidates selected from stars matching between the multiband imaging data sets of the Subaru Hyper Suprime-Cam (HSC) Survey and the Sloan Digital Sky Survey in the Stripe82 region covering about 165 deg$^2$. We select WD candidates from the ‘reduced proper motion’ diagram by combining the apparent magnitude in the range $i=19$–24 and the proper motion measured from the data sets among a baseline of $\sim$14 yr. We refine the WD candidates by fitting blackbody and template WD atmosphere models to HSC photometries for each candidate, enabling the estimation of distance and tangential velocity ($v_{\rm t}$). The deep HSC data allow us to identify low-temperature ($\lt 4000$ K) and faint WD candidates down to absolute magnitude, $M_{\rm bol}\simeq 17$. We evaluate the selection function of our WD candidates using a mock catalogue of spatial and kinematic distributions of WDs in the (thin and thick) disc and halo regions based on a Galactic model. We construct samples of disc and halo WD candidates by selecting WDs with tangential velocity, $40\lt v_{\rm t}/({\rm km}~{\rm s}^{-1})\lt 80$ and $200\lt v_{\rm t}/({\rm km}~{\rm s}^{-1})\lt 500$, respectively. The total number densities of the disc and halo WDs are $(9.33 \pm 0.89) \times 10^{-3}$ pc$^{-3}$ and $(6.34 \pm 2.90) \times 10^{-4}$ pc$^{-3}$. Our luminosity functions (LFs) extend down to fainter absolute magnitudes compared with previous work. The faint WDs could represent the oldest generation of building blocks over the past $\sim$10 billion years of the assembly history of our Milky Way.
Targeted delivery of napabucasin with radiotherapy improves outcomes in diffuse midline glioma
Authors: Gallitto Matthew , Zhang Xu , De Los Santos Genesis , Wei Hong-Jian , Fernández Ester Calvo , Duan Shoufu , Sedor Geoffrey , Yoh Nina , Kokossis Danae , Angel J Carlos , Wang Yi-Fang , White Erin , Kinslow Connor J , Berg Xander , Tomassoni Lorenzo , Zandkarimi Fereshteh , Chio Iok In Christine , Canoll Peter , Bruce Jeffrey N , Feldstein Neil A , Gartrell Robyn D , Cheng Simon K , Garvin James H , Zacharoulis Stergios , Wechsler-Reya Robert J , Pavisic Jovana , Califano Andrea , Zhang Zhiguo , Wu Cheng-Chia 
Published: October 2024

Abstract

Background
Diffuse midline glioma (DMG) is the most aggressive primary brain tumor in children. All previous studies examining the role of systemic agents have failed to demonstrate a survival benefit; the only standard of care is radiation therapy (RT). Successful implementation of radiosensitization strategies in DMG remains an essential and promising avenue of investigation. We explore the use of Napabucasin, an NAD(P)H quinone dehydrogenase 1 (NQO1)-bioactivatable reactive oxygen species (ROS)-inducer, as a potential therapeutic radiosensitizer in DMG.

Methods
In this study, we conduct in vitro and in vivo assays using patient-derived DMG cultures to elucidate the mechanism of action of Napabucasin and its radiosensitizing properties. As penetration of systemic therapy through the blood-brain barrier (BBB) is a significant limitation to the success of DMG therapies, we explore focused ultrasound (FUS) and convection-enhanced delivery (CED) to overcome the BBB and maximize therapeutic efficacy.

Results
Napabucasin is a potent ROS-inducer and radiosensitizer in DMG, and treatment-mediated ROS production and cytotoxicity are dependent on NQO1. In subcutaneous xenograft models, combination therapy with RT improves local control. After optimizing targeted drug delivery using CED in an orthotopic mouse model, we establish the novel feasibility and survival benefit of CED of Napabucasin concurrent with RT.

Conclusions
As nearly all DMG patients will receive RT as part of their treatment course, our validation of the efficacy of radiosensitizing therapy using CED to prolong survival in DMG opens the door for exciting novel studies of alternative radiosensitization strategies in this devastating disease while overcoming limitations of the BBB.
The out-of-plane contact shield and mA-modulation – the effect on fetal absorbed dose
Authors: Larjava Heli R S , Eneh Chibuzor T M , Saikkonen Aleksi , Parkkola Riitta K 
Published: October 2024

Abstract
The effect of patient shielding on fetal radiation dose was evaluated in computed tomography pulmonary angiography with the out-of-plane shield visible in the localizer but absent in the scan range in chest computed tomography (CT). An anthropomorphic phantom with additional prosthetic pregnancy belly was scanned with different CT scanners using clinical imaging protocols and radiophotoluminescence dosemeters (GD-352 M). The out-of-plane shield decreased the fetal absorbed radiation dose with Siemens Somatom go.Up, Canon Aquilion Prime SP and Canon Aquilion One scanners. The decrease was 3.9%–39.4% (0.01–0.09 mGy). With GE Optima the shield increased the fetal dose by 100% (0.23 mGy), with Canon Aquilion One and GE Optima scanners the abdomen dose increase was 17.5% and 36.4%, respectively (0.61 and 1.38 mGy). Applying an out-of-plane shield outside the scanned volume may increase the fetal radiation dose during CT when using tube current modulation, depending on the make and model of the CT scanner.
From Forced Migration to Displacement?
Authors: Owen David 
Published: October 2024

Abstract
Should the multi-disciplinary field of Forced Migration Studies (FMS) re-orient itself around the concept of “displacement”? This short intervention situates this question against the background of the transition from Refugee Studies to FMS, as well as external developments in the realm of protection. It draws attention to how the concept of displacement has become more central to both policy and academic discussion in FMS before considering what difference such a re-orientation might make conceptually, ethically, and politically. It concludes by suggesting that FMS might be conceived as standing between and across two larger fields of enquiry: Migration Studies and Displacement Studies.
Seasonal changes in hydraulic functions of eight temperate tree species: divergent responses to freeze–thaw cycles in spring and autumn
Authors: Li Zhimin , Luo Dandan , Ibrahim Muhammed Mustapha , Luo Xianzhen , Deng Rufang , Wang Chuankuan , Hou Enqing 
Published: October 2024

Abstract
Freeze–thaw cycles (FTCs) are the major seasonal environment stress in the temperate and boreal forests, inducing hydraulic dysfunction and limiting tree growth and distribution. There are two types of FTCs in the field: FTCs with increasing temperature from winter to spring (spring FTCs); and FTCs with decreasing temperature from autumn to winter (autumn FTCs). While previous studies have evaluated the hydraulic function during the growing season, its seasonal changes and how it adapts to different types of FTCs remain unverified. To fill this knowledge gap, the eight tree species from three wood types (ring- and diffuse-porous, tracheid) were selected in a temperate forest undergoing seasonal FTCs. We measured the branch hydraulic traits in spring, summer, autumn, and early, middle and late winter. Ring-porous trees always showed low native hydraulic conductance (Kbranch), and high percentage loss of maximum Kbranch (PLCB) and water potential that loss of 50% maximum Kbranch (P50B) in non-growing seasons (except summer). Kbranch decreased, and PLCB and P50B increased in diffuse-porous trees after several spring FTCs. In tracheid trees, Kbranch decreased after spring FTCs while the P50B did not change. All sampled trees gradually recovered their hydraulic functions from spring to summer. Kbranch, PLCB and P50B of diffuse-porous and tracheid trees were relatively constant after autumn FTCs, indicating almost no effect of autumn FTCs on hydraulic functions. These results suggested that hydraulic functions of temperate trees showed significant seasonal changes, and spring FTCs induced more hydraulic damage (except ring-porous trees) than autumn FTCs, which should be determined by the number of FTCs and trees’ vitality before FTCs. These findings advance our understanding of seasonal changes in hydraulic functions and how they cope with different types of FTC in temperate forests.
Prevalence of unplanned extubation in a tertiary care neonatal intensive care unit
Authors: García Heladia , Ramos-Soto Dulce Ivonne , Miranda-Novales Guadalupe , Luna-Santos Laura 
Published: October 2024

Abstract
Orotracheal intubation and mechanical ventilation (MV) have become routine practices in intensive care units. Unplanned extubation (UE) is one of the most important complications, particularly in premature infants and critically ill newborns. The objective of this study was to determine the prevalence of UE in a tertiary care neonatal intensive care unit (NICU). In this analytical cross-sectional retrospective study, all data, including perinatal data, indications for ventilatory support, days of MV at the time of UE, work shift, month of the event, reintubation, and postextubation complications, were obtained from the manual review of clinical charts. In total, 151 neonates, who received invasive MV, were included in this study. The prevalence of UE was 2.0/100 days of ventilation. The most affected were premature infants, with a gestational age of ≤ 32 weeks (54.7%) and a birth weight of ≤ 1500 g. The main cause for UE was deficient fixation of the endotracheal tube (ETT) (27.7%). Most UE events occurred during night shifts (48.1%). Reintubation was required in 83.3% of newborns. Immediate complications developed in 96.3% of the UE events, including desaturation (57.7%) and bradycardia (36.5%). The prevalence of UE was high, particularly in premature infants, with a high rate of reintubation and immediate complications. Standardized protocols for ETT care must be implemented to reduce these events.