bluuebunny/crossref_metadata_2025_split huggingface dataset:
Whole genome characterization of Trichophyton indotineae isolated in Singapore
Authors: Teo Jeanette W P , Cheng Janet W S , Chew Ka Lip , Lin Raymond T P 
Published: February 2024

Abstract
Complete genome sequences from two Trichophyton indotineae isolates were obtained from a 23-year-old male presenting with tinea cruris after an overseas recreational water exposure and from a 53-year-old female patient with unknown travel history. Analysis of the squalene epoxidase gene and the cyp51 gene family showed an absence of mutations, correlating with phenotypic drug susceptibility. The Single Nucleotide Polymorphisms (SNPs) distance between both isolates was 92. Within the T. indotineae cluster, SNPs ranged from 7 to 182, suggesting a high genetic relatedness with other South Asian isolates. This study suggests that the prevalence of T. indotineae is under-reported and more widespread than previously thought.
The EBLM Project– XI. Mass, radius, and effective temperature measurements for 23 M-dwarf companions to solar-type stars observed with CHEOPS
Authors: Swayne M I , Maxted P F L , Triaud A H M J , Sousa S G , Deline A , Ehrenreich D , Hoyer S , Olofsson G , Boisse I , Duck A , Gill S , Martin D , McCormac J , Persson C M , Santerne A , Sebastian D , Standing M R , Acuña L , Alibert Y , Alonso R , Anglada G , Bárczy T , Barrado Navascues D , Barros S C C , Baumjohann W , Baycroft T A , Beck M , Beck T , Benz W , Billot N , Bonfils X , Borsato L , Bourrier V , Brandeker A , Broeg C , Carmona A , Charnoz S , Collier Cameron A , Cortés-Zuleta P , Csizmadia Sz , Cubillos P E , Davies M B , Deleuil M , Delfosse X , Delrez L , Demangeon O D S , Demory B -O , Dransfield G , Erikson A , Fortier A , Forveille T , Fossati L , Fridlund M , Gandolfi D , Gillon M , Güdel M , Günther M N , Hara N , Hébrard G , Heidari N , Hellier C , Helling Ch , Isaak K G , Kerschbaum F , Kiefer F , Kiss L L , Kunovac V , Lalitha S , Lam K W F , Laskar J , Lecavelier des Etangs A , Lendl M , Magrin D , Marafatto L , Martioli E , Miller N J , Mordasini C , Moutou C , Nascimbeni V , Ottensamer R , Pagano I , Pallé E , Peter G , Piazza D , Piotto G , Pollacco D , Queloz D , Ragazzoni R , Rando N , Rauer H , Ribas I , Santos N C , Scandariato G , Ségransan D , Simon A E , Smith A M S , Southworth R , Stalport M , Szabó Gy M , Thomas N , Udry S , Ulmer B , Van Grootel V , Venturini J , Walton N A , Willett E , Wilson T G 
Published: February 2024

ABSTRACT
Observations of low-mass stars have frequently shown a disagreement between observed stellar radii and radii predicted by theoretical stellar structure models. This ‘radius inflation’ problem could have an impact on both stellar and exoplanetary science. We present the final results of our observation programme with the CHaracterising ExOPlanet Satellite (CHEOPS) to obtain high-precision light curves of eclipsing binaries with low-mass stellar companions (EBLMs). Combined with the spectroscopic orbits of the solar-type companions, we can derive the masses, radii, and effective temperatures of 23 M-dwarf stars. We use the pycheops data analysis software to analyse their primary and secondary occultations. For all but one target, we also perform analyses with Transiting Exoplanet Survey Satellite (TESS) light curves for comparison. We have assessed the impact of starspot-induced variation on our derived parameters and account for this in our radius and effective temperature uncertainties using simulated light curves. We observe trends in inflation with both metallicity and orbital separation. We also observe a strong trend in the difference between theoretical and observational effective temperatures with metallicity. There is no such trend with orbital separation. These results are not consistent with the idea that the observed inflation in stellar radius combines with lower effective temperature to preserve the luminosity predicted by low-mass stellar models. Our EBLM systems provide high-quality and homogeneous measurements that can be used in further studies of radius inflation.
Effect of magnetically dependent heating on the behaviour of magnetoacoustic waves in coronal plasma with thermal misbalance
Authors: Agapova D V , Belov S A , Zavershinskii D I 
Published: February 2024

ABSTRACT
The magnetic nature of coronal heating has been actively investigated within the framework of theoretical models and statistical analysis of observational data for decades. At present, a rather wide range of possible mechanisms has been proposed in the literature that requires additional verification. In this paper, we investigate the possibility of analysing the magnetic nature of coronal heating by means of magnetoacoustic (MA) waves propagating in coronal structures. To address this issue, we perform the analysis of fast and slow waves using a magnetic slab geometry. Applying the assumption of strong magnetic structuring, we derive the dispersion relation, which allows us to study the properties of MA waves. To analyse the dependence of phase velocity and wave decrement/increment on wavenumber, we numerically solved the obtained equations using the parameters corresponding to ‘warm’ coronal loop. It is shown that oscillations on the fundamental harmonic in a plasma with a weak magnetic field, where the effect of phase velocity dispersion is most pronounced, are best suited for diagnostics of magnetic heating using slow MA waves. In turn, the geometry remains the primary source for fast MA wave dispersion. Magnetic heating can either suppress or increase the damping of fast and slow MA waves. Moreover, the amplification of fast MA waves accompanied by damping of slow MA waves can be achieved. This issue is of interest in the context of the excitation of the decayless kink oscillations in the solar coronal loops.
Localization of gamma-ray bursts using AstroSat Mass Model
Authors: Saraogi Divita , Aditya J Venkata , Bhalerao Varun , Bala Suman , Balasubramanian Arvind , Mate Sujay , Chattopadhyay Tanmoy , Gupta Soumya , Prasad Vipul , Waratkar Gaurav , Navaneeth P K , Gopalakrishnan Rahul , Bhattacharya Dipankar , Dewangan Gulab , Vadawale Santosh 
Published: February 2024

ABSTRACT
The Cadmium Zinc Telluride Imager (CZTI) aboard AstroSat has good sensitivity to gamma-ray bursts (GRBs), with close to 600 detections including about 50 discoveries undetected by other missions. However, CZTI was not designed to be a GRB monitor and lacks localization capabilities. We introduce a new method of localizing GRBs using ‘shadows’ cast on the CZTI detector plane due to absorption and scattering by satellite components and instruments. Comparing the observed distribution of counts on the detector plane with simulated distributions with the AstroSat Mass Model, we can localize GRBs in the sky. Our localization uncertainty is defined by a two-component model, with a narrow Gaussian component that has close to 50 per cent probability of containing the source, and the remaining spread over a broader Gaussian component with an 11.3 times higher σ. The width (σ) of the Gaussian components scales inversely with source counts. We test this model by applying the method to GRBs with known positions and find good agreement between the model and observations. This new ability expands the utility of CZTI in the study of GRBs and other rapid high-energy transients.
Devolatilization of extrasolar planetesimals by 60Fe and 26Al heating
Authors: Eatson Joseph W , Lichtenberg Tim , Parker Richard J , Gerya Taras V 
Published: February 2024

ABSTRACT
Whilst the formation of Solar system planets is constrained by meteoritic evidence, the geophysical history of low-mass exoplanets is much less clear. The bulk composition and climate states of rocky exoplanets may vary significantly based on the composition and properties of the planetesimals they form. An important factor influenced by planetesimal composition is water content, where the desiccation of accreting planetesimals impacts the final water content of the resultant planets. While the inner planets of the Solar system are comparatively water-poor, recent observational evidence from exoplanet bulk densities and planetary formation models suggests that rocky exoplanets engulfed by substantial layers of high-pressure ices or massive steam atmospheres could be widespread. Here, we quantify variations in planetesimal desiccation due to potential fractionation of the two short-lived radioisotopes 26Al and 60Fe relevant for internal heating on planetary formation time-scales. We focus on how order of magnitude variations in 60Fe can affect the water content of planetesimals, and how this may alter the formation of extrasolar ocean worlds. We find that heating by 26Al is the dominant cause of planetesimal heating in any Solar system analogue scenario, thus validating previous works focussing only on this radioisotope. However, 60Fe can become the primary heating source in the case of high levels of supernova enrichment in massive star-forming regions. These diverging scenarios can affect the formation pathways, bulk volatile budget, and climate diversity of low-mass exoplanets.
Via Machinae 2.0: Full-sky, model-agnostic search for stellar streams in Gaia DR2
Authors: Shih David , Buckley Matthew R , Necib Lina 
Published: February 2024

ABSTRACT
We present an update to Via Machinae, an automated stellar stream-finding algorithm based on the deep learning anomaly detector ANODE. Via Machinae identifies stellar streams within Gaia, using only angular positions, proper motions, and photometry, without reference to a model of the Milky Way potential for orbit integration or stellar distances. This new version, Via Machinae 2.0, includes many improvements and refinements to nearly every step of the algorithm, that altogether result in more robust and visually distinct stream candidates than our original formulation. In this work, we also provide a quantitative estimate of the false positive rate of Via Machinae 2.0 by applying it to a simulated Gaia-mock catalogue based on galaxia, a smooth model of the Milky Way that does not contain substructure or stellar streams. Finally, we perform the first full-sky search for stellar streams with Via Machinae 2.0, identifying 102 streams at high significance within the Gaia Data Release 2, of which only 10 have been previously identified. While follow-up observations for further confirmation are required, taking into account the false positive rate presented in this work, we expect approximately 90 of these stream candidates to correspond to real stellar structures.
Stellar populations of massive early-type galaxies observed by MUSE
Authors: Parikh Taniya , Saglia Roberto , Thomas Jens , Mehrgan Kianusch , Bender Ralf , Maraston Claudia 
Published: February 2024

ABSTRACT
Stellar population studies of massive early-type galaxies (ETGs) suggest that the stellar initial mass function may not be universal. In particular, the centres of ETGs seem to contain an excess of low-mass dwarf stars compared to our own Galaxy. Through high-resolution data from MUSE (Multi Unit Spectroscopic Explorer), we carry out a detailed study of the stellar populations of eight massive ETGs. We use full spectrum fitting to determine ages, element abundances, and initial mass function (IMF) slopes for spatially binned spectra. We measure flat gradients in age and [Mg/Fe] ratio, as well as negative gradients in metallicity and [Na/Fe]. We detect IMF gradients in some galaxies, with the centres hosting bottom-heavy IMFs and mass excess factors between 1.5 and 2.5 compared to a Kroupa IMF. The IMF slope below 0.5 M$_\odot$varies for our galaxy sample between 1 and 2.8, with negative radial gradients, while the IMF slope between 0.5 and 1M$_\odot$ has a steep value of $\sim$3 with mildly positive gradients for most galaxies. For M87, we find excellent agreement with the dynamical mass-to-light ratio (M/L) as a function of radius. For the other galaxies, we find systematically higher M/L from stellar populations compared to orbit-based dynamical analysis of the same data. This discrepancy increases with NaI strength, suggesting a combination of calibration issues of this line and correlated uncertainties.
Reassessing the constraints from SH0ES extragalactic Cepheid amplitudes on systematic blending bias
Authors: Sharon Amir , Kushnir Doron , Yuan Wenlong , Macri Lucas , Riess Adam 
Published: February 2024

ABSTRACT
The SH0ES collaboration Hubble constant determination is in a ∼5σ difference with the Planck value, known as the Hubble tension. The accuracy of the Hubble constant measured with extragalactic Cepheids depends on robust stellar-crowding background estimation. Riess et al. (R20) compared the light-curve amplitudes of extragalactic and MW Cepheids to constrain an unaccounted systematic blending bias, $\gamma =-0.029\pm 0.037\, \rm {mag}$, which cannot explain the required, $\gamma =0.24\pm 0.05\, \rm {mag}$, to resolve the Hubble tension. Further checks by Riess et al. demonstrate that a possible blending is not likely related to the size of the crowding correction. We repeat the R20 analysis, with the following main differences: (1) we limit the extragalactic and MW Cepheids comparison to periods $P\lesssim 50\, \rm {d}$, since the number of MW Cepheids with longer periods is minimal; (2) we use publicly available data to recalibrate amplitude ratios of MW Cepheids in standard passbands; (3) we remeasure the amplitudes of Cepheids in NGC 5584 and NGC 4258 in two Hubble Space Telescope filters (F555W and F350LP) to improve the empirical constraint on their amplitude ratio A555/A350. We show that the filter transformations introduce an ${\approx }0.04\, \rm {mag}$ uncertainty in determining γ, not included by R20. While our final estimate, $\gamma =0.013\pm 0.057\, \rm {mag}$, is consistent with the value derived by R20 and is consistent with no bias, the error is somewhat larger, and the best-fitting value is shifted by ${\approx }0.04\, \rm {mag}$ and closer to zero. Future observations, especially with JWST, would allow better calibration of γ.
Long-term orbital evolution of dimorphos boulders and implications on the origin of meteorites
Authors: Fenucci M , Carbognani A 
Published: February 2024

ABSTRACT
By using recent observations of the Dydimos−Dimorphos system from the Hubble Space Telescope, 37 boulders with a size of 4 to 7 m ejected from the system during the impact with the DART spacecraft were identified. In this work, we studied the orbital evolution of a swarm of boulders with a similar size to that of the detected ones. By using recent estimates for the ejection velocity of the boulders, we numerically propagated the dynamics of the swarm for 20 kyr in the future. We found that the ejection velocities and the non-gravitational effects are not strong enough to change the secular evolution significantly. The minimum orbit intersection distance (MOID) with the Earth will be reached in about 2.5 kyr, but it will not fall below 0.02 au. On the contrary, the Mars MOID will be very small in four instances, two near 6 kyr and the other two near 15 kyr. Therefore, there may be a chance for them to impact Mars in the future. Given the rarefaction of the Martian atmosphere, we expect the boulders to arrive intact on the ground and excavate a small impact crater. The results presented here provide a further indication that some meteorites found on Earth originated in collisions of ∼100 m near-Earth asteroids with projectiles of ∼1 m in size.
Torque wiggles – a robust feature of the global disc–planet interaction
Authors: Cimerman Nicolas P , Rafikov Roman R , Miranda Ryan 
Published: February 2024

ABSTRACT
Gravitational coupling between planets and protoplanetary discs is responsible for many important phenomena such as planet migration and gap formation. The key quantitative characteristic of this coupling is the excitation torque density – the torque (per unit radius) imparted on the disc by planetary gravity. Recent global simulations and linear calculations found an intricate pattern of low-amplitude, quasi-periodic oscillations in the global radial distribution of torque density in the outer disc, which we call torque wiggles. Here, we show that torque wiggles are a robust outcome of global disc–planet interaction and exist despite the variation of disc parameters and thermodynamic assumptions (including β-cooling). They result from coupling of the planetary potential to the planet-driven density wave freely propagating in the disc. We developed analytical theory of this phenomenon based on approximate self-similarity of the planet-driven density waves in the outer disc. We used it, together with linear calculations and simulations, to show that (a) the radial periodicity of the wiggles is determined by the global shape of the planet-driven density wave (its wrapping in the disc) and (b) the sharp features in the torque density distribution result from constructive interference of different azimuthal (Fourier) torque contributions at radii where the planetary wake crosses the star–planet line. In the linear regime, the torque wiggles represent a weak effect, affecting the total (integrated) torque by only a few per cent. However, their significance increases in the non-linear regime, when a gap (or a cavity) forms around the perturber’s orbit.
Hierarchical reconstruction of the cosmic web, the H-Spine method
Authors: Aragon-Calvo M A 
Published: February 2024

ABSTRACT
The cosmic web consists of a nested hierarchy of structures: voids, walls, filaments, and clusters. These structures interconnect and can encompass one another, collectively shaping an intricate network. Here we introduce the Hierarchical Spine (H-Spine) method, a framework designed to hierarchically identify and characterize voids, walls, and filaments. Inspired by the geometrical and dynamical constraints imposed by anisotropic gravitational collapse, the H-Spine method captures the geometry and interconnectivity between cosmic structures as well as their nesting relations, offering a more complete description of the cosmic web compared to single-scale or multiscale approaches. To illustrate the method’s utility, we present the distribution of densities and sizes of voids, walls, and filaments identified in a three-level hierarchical space. This analysis demonstrates how each level within the hierarchy unveils distinctive densities and scales inherent to cosmic web elements.
ALPACA: a new semi-analytical model for metal absorption lines emerging from clumpy galactic environments
Authors: Li Zhihui , Gronke Max , Steidel Charles C 
Published: February 2024

ABSTRACT
We present a new semi-analytical formalism for modelling metal absorption lines that emerge from a clumpy galactic environment, ALPACA. We predict the “down-the-barrel” (DTB) metal absorption line profiles and the equivalent width (EW) of absorption at different impact parameters (b) as a function of the clump properties, including clump kinematics, clump volume filling factor, clump number density profile, and clump ion column densities. With ALPACA, we jointly model the stacked DTB C ii λ1334 spectrum of a sample of z ∼ 3 Lyman break galaxies and the EW versus b profile of a sample of z ∼ 2 star-forming galaxy–galaxy pairs. ALPACA successfully reproduced two data sets simultaneously, and the best fit prefers a low clump volume filling factor (∼3 × 10−3). The radial velocities of the clumps are a superposition of a rapidly accelerated outflow with a maximum velocity of $\sim 400 \, {\mathrm{km}\, \mathrm{s}^{-1}}$ and a velocity dispersion of $\sigma \sim 120 \, {\mathrm{km}\, \mathrm{s}^{-1}}$. The joint modelling reveals a physical scenario where the absorption observed at a particular velocity is contributed by the clumps distributed over a fairly broad range of radii. We also find that the commonly adopted Sobolev approximation is at best only applicable within a narrow range of radii where the clumps are undergoing rapid acceleration in a non-volume-filling clumpy medium. Lastly, we find that the clump radial velocity profile may not be fully constrained by the joint modelling and spatially resolved Ly α emission modelling may help break the degeneracy.
Multimass modelling of milky way globular clusters – II. Present-day black hole populations
Authors: Dickson N , Smith P J , Hénault-Brunet V , Gieles M , Baumgardt H 
Published: February 2024

ABSTRACT
Populations of stellar-mass black holes (BHs) in globular clusters (GCs) influence their dynamical evolution and have important implications on one of the main formation channels for gravitational wave sources. Inferring the size of these populations remains difficult, however. In this work, multimass models of 34 Milky Way GCs, first presented in Dickson et al., are used to explore the present-day BH populations. Direct constraints on both the total and visible mass components provided by several observables allow these models to accurately determine the distribution of the dark mass (including BHs) within clusters, as we demonstrate in a proof-of-concept fitting of the models to mock observations extracted from Monte Carlo cluster models. New constraints on the BH population retained to the present-day in each cluster are inferred from our models. We find that BH mass fractions ranging from 0 to 1 per cent of the total mass are typically required to explain the observations, except for ω Cen, for which we infer a mass fraction above 5 per cent, in agreement with previous works. Relationships between the dark remnant populations and other cluster parameters are examined, demonstrating a clear anticorrelation between the amount of BHs and mass segregation between visible stars, as well as a correlation between remnant mass fractions and the dynamical age of clusters. Our inferred BH populations are in good agreement overall with other recent studies using different methodologies, but with notable discrepancies for individual clusters.
FAUST XII. Accretion streamers and jets in the VLA 1623–2417 protocluster
Authors: Codella C , Podio L , De Simone M , Ceccarelli C , Ohashi S , Chandler C J , Sakai N , Pineda J E , Segura-Cox D M , Bianchi E , Cuello N , López-Sepulcre A , Fedele D , Caselli P , Charnley S , Johnstone D , Zhang Z E , Maureira M J , Zhang Y , Sabatini G , Svoboda B , Jiménez-Serra I , Loinard L , Mercimek S , Murillo N , Yamamoto S 
Published: February 2024

ABSTRACT
The ALMA interferometer has played a key role in revealing a new component of the Sun-like star forming process: the molecular streamers, i.e. structures up to thousands of au long funnelling material non-axisymmetrically to discs. In the context of the FAUST ALMA LP, the archetypical VLA1623-2417 protostellar cluster has been imaged at 1.3 mm in the SO(56–45), SO(66–55), and SiO(5–4) line emission at the spatial resolution of 50 au. We detect extended SO emission, peaking towards the A and B protostars. Emission blue-shifted down to 6.6 km s−1 reveals for the first time a long (∼ 2000 au) accelerating streamer plausibly feeding the VLA1623 B protostar. Using SO, we derive for the first time an estimate of the excitation temperature of an accreting streamer: 33 ± 9 K. The SO column density is ∼ 1014 cm−2, and the SO/H2 abundance ratio is ∼ 10−8. The total mass of the streamer is 3 × 10−3M⊙, while its accretion rate is 3–5 × 10−7M⊙ yr−1. This is close to the mass accretion rate of VLA1623 B, in the 0.6–3 × 10−7M⊙ yr−1 range, showing the importance of the streamer in contributing to the mass of protostellar discs. The highest blue- and red-shifted SO velocities behave as the SiO(5–4) emission, the latter species detected for the first time in VLA1623-2417: the emission is compact (100–200 au), and associated only with the B protostar. The SO excitation temperature is ∼ 100 K, supporting the occurrence of shocks associated with the jet, traced by SiO.