bluuebunny/crossref_metadata_2025_split huggingface dataset:
Feeding potential of adult Systena frontalis (Coleoptera: Chrysomelidae) on leaves of Hydrangea paniculata (Cornales: Hydrangeaceae)
Authors: Lane Eleanor L , Del Pozo-Valdivia Alejandro I 
Published: August 2023

Abstract
Systena frontalis (F.) (Coleoptera: Chrysomelidae), also known as the red-headed flea beetle, is a defoliating pest of a variety of crop systems, such as ornamentals and food crops. Leaf consumption by this beetle renders ornamental nursery plants, such as hydrangeas (Hydrangea paniculata Siebold, Hydrangeaceae), unsaleable. In Virginia, this insect has become a major pest at commercial nurseries, and their feeding potential on affected crops has not been quantified. In this study, the extent of their damage to individual leaves and host preference between leaf ages were determined. The rate of defoliation on mature and young hydrangea leaves was measured over 24 and 48 h and between different numbers of adults. A single adult caused up to 10% damage to a young leaf or 5% to a whole mature leaf in 24 h. Without choice, there was a higher percent damage to young leaves. When the size of leaves was controlled by cut-out mature leaves, the area damaged was still higher in young leaves when compared with mature leaves. Adult feeding between mature or young leaves was further investigated by choice assays on a caged plant and within a containerized system. In these choice assays, adults inflicted higher percent damage on mature leaves in both caged plant assays and containerized direct choice assays. The choice assays were more similar to field conditions than the nonchoice assays. This demonstrates that S. frontalis showed a preference for mature leaves over young leaves within hydrangeas.
Middle eastern energy and climate ambitions: Vision 2030 in the Kingdom of Saudi Arabia and the influence of the legal environmental principles
Authors: Alomari Mohammad A , Heffron Raphael J 
Published: August 2023

Abstract
Environmental principles with their various forms, natures and different legal roles across jurisdictions are gaining increasing attention in energy and climate scholarship. The trend in the literature has been to discuss these principles in the context of developed countries, considering, for example, the impact of and significant literature on the polluter-pays principle. This article offers an original review with a contribution in discussing the new Middle Eastern energy and climate ambitions of the Kingdom of Saudi Arabia (KSA). These goals are contained within the promising policy document known as Vision 2030, and this review explores these energy and climate ambitions in the legal context of environmental principles. The study reviews the literature on the environmental principles in the Middle Eastern context of the Kingdom of Saudi Arabia and utilizes doctrinal and socio-legal methods (including expert interviews) to explore the practice of Vision 2030. This article advocates that, with the advent of the Kingdom of Saudi Arabia Vision 2030, the application of these principles can fill an existing lacuna in legal scholarship and advance governance in the areas of energy and climate change.
Penicillium and Talaromyces spp. emerging pathogens in dogs since 1990s
Authors: Monpierre Lorra , Soetart Nicolas , Valsecchi Isabel , Brément Thomas , Brunelat Philippe , Drut Amandine , David Manon , Roux Cécile , Hubert Floriane , Razafimandimby Bienvenue , Jouvion Grégory , Miclard Julien , Chermette René , Botterel Françoise , Guillot Jacques 
Published: August 2023

Abstract
Penicillium and Talaromyces spp. are environmental saprophytic molds rarely encountered as infectious agents in humans and animals. This article summarizes the clinical features, treatment, and outcomes of proven infections caused by Penicillium or Talaromyces in four dogs in France. Two dogs had disseminated infections, while the other two had a localized form. All dogs had positive histopathological results showing the presence of hyaline septate hyphae and a positive fungal culture with typical Penicillium conidiophores. Talaromyces georgiensis (n = 1), Penicillium labradorum (n = 2), and Penicillium from section Ramosa series Raistrickiorum (n = 1), were identified based on Internal Transcribed Spacer (ITS) Sanger sequencing. The dogs were initially treated with ketoconazole or itraconazole. Second-line treatment was initiated in three dogs, but after several relapses, the prognosis remained poor. Since the 1990s, 18 cases of Penicillium or Talaromyces infections in dogs have been described worldwide. This series of four reports brings new cases to those already reported in the literature, which are probably underestimated in the world.
Photometry and astrometry with JWST – III. A NIRCam-Gaia DR3 analysis of the open cluster NGC 2506
Authors: Nardiello D , Bedin L R , Griggio M , Salaris M , Scalco M , Cassisi S 
Published: August 2023

ABSTRACT
In the third paper of this series aimed at developing the tools for analysing resolved stellar populations using the cameras on board of the James Webb Space Telescope (JWST), we present a detailed multiband study of the 2 Gyr Galactic open cluster NGC 2506. We employ public calibration data sets collected in multiple filters to: (i) derive improved effective Point Spread Functions (ePSFs) for 10 NIRCam filters; (ii) extract high-precision photometry and astrometry for stars in the cluster, approaching the main sequence (MS) lower mass of ∼0.1 M⊙; and (iii) take advantage of the synergy between JWST and Gaia DR3 to perform a comprehensive analysis of the cluster’s global and local properties. We derived a MS binary fraction of ∼57.5 per cent, extending the Gaia limit (∼0.8 M⊙) to lower masses (∼0.4 M⊙) with JWST. We conducted a study on the mass functions (MFs) of NGC 2506, mapping the mass segregation with Gaia data, and extending MFs to lower masses with the JWST field. We also combined information on the derived MFs to infer an estimate of the cluster present-day total mass. Lastly, we investigated the presence of white dwarfs (WDs) and identified a strong candidate. However, to firmly establish its cluster membership, as well as that of four other WD candidates and of the majority of faint low-mass MS stars, further JWST equally deep observations will be required. We make publicly available catalogues, atlases, and the improved ePSFs.
Constraining the assembly time of the stellar haloes of nearby Milky Way-mass galaxies through AGB populations
Authors: Harmsen Benjamin , Bell Eric F , D’Souza Richard , Monachesi Antonela , de Jong Roelof S , Smercina Adam , Jang In Sung , Holwerda Benne W 
Published: August 2023

ABSTRACT
The star formation histories (SFHs) of galactic stellar haloes offer crucial insights into the merger history of the galaxy and the effects of those mergers on their hosts. Such measurements have revealed that while the Milky Way’s most important merger was 8–10 Gyr ago, M31’s largest merger was more recent, within the last few Gyr. Unfortunately, the required halo SFH measurements are extremely observationally expensive outside of the Local Group. Here, we use asymptotic giant branch (AGB) stars brighter than the tip of the red giant branch (RGB) to constrain stellar halo SFHs. Both stellar population models and archival data sets show that the AGB/RGB ratio constrains the time before which 90 per cent of the stars formed, t90. We find AGB stars in the haloes of three highly inclined roughly Milky Way-mass galaxies with resolved star measurements from the Hubble Space Telescope; this population is most prominent in the stellar haloes of NGC 253 and NGC 891, suggesting that their stellar haloes contain stars born at relatively late times, with inferred t90 ∼ 6 ± 1.5 Gyr. This ratio also varies from region to region, tending towards higher values along the major axis and in tidal streams or shells. By combining our measurements with previous constraints, we find a tentative anticorrelation between halo age and stellar halo mass, a trend that exists in models of galaxy formation but has never been elucidated before, i.e. the largest stellar haloes of Milky Way-mass galaxies were assembled more recently.
Characterizing the calibration systematics in radio interferometry due to partially modelled extended emission
Authors: Jackson Jason P , Grobler Trienko L 
Published: August 2023

ABSTRACT
Calibration is the process by which we try to remove atmospheric and instrumental errors that corrupt the observations made by interferometers. Calibration is however an imperfect process and when we calibrate with an incomplete sky model systematics or artefacts manifest in our final images. One of the more striking artefacts that can appear in images are ghost sources. This paper explores these ghost artefacts in greater depth. We are particularly interested in the systematics or artefacts that are created if we partially model extended emission. A theoretical model that utilizes an east–west layout is developed (and empirically validated) that can give insight into the systematics so formed. The results from this study reveal that when we only partially model extended emission then the calibration systematics that form can manifest as extended emission in images. The aforementioned systematics alter the original extended source in various ways; the flux density of the extended source is modified and becomes comparable to the flux density of the source in the calibration sky model and its profile is slightly modified (it becomes more point like). More importantly, we found that the shorter baselines that are more sensitive to extended emission are in general more affected by the calibration systematics than the longer baselines are. In related works, it was found that the number of antennas greatly influence the brightness of the created systematics. For the use case, we investigate in the paper, however, we found this to not be the case.
FOREVER22: the first bright galaxies with Population III stars at redshifts z ≃ 10–20 and comparisons with JWST data
Authors: Yajima Hidenobu , Abe Makito , Fukushima Hajime , Ono Yoshiaki , Harikane Yuichi , Ouchi Masami , Hashimoto Takuya , Khochfar Sadegh 
Published: August 2023

ABSTRACT
We study the formation of the first galaxies in overdense regions modelled by the FORmation and EVolution of galaxies in Extremely overdense Regions motivated by SSA22 (FOREVER22) simulation project. Our simulations successfully reproduce the star formation rates and the MUV–Mstar relations of candidate galaxies at z ∼ 10–14 observed by the JWST. We suggest that the observed galaxies are hosted by dark matter haloes with Mh ≳ 1010 M⊙ and are in short-period starburst phases. On the other hand, even simulated massive galaxies in overdense regions cannot reproduce the intense star formation rates and the large stellar masses of observed candidates at z ∼ 16. Also, we show that the contribution of Population III stars to the ultraviolet (UV) flux decreases as the stellar mass increases and it is a few per cent for galaxies with Mstar ∼ 107 M⊙. Therefore, a part of the observed flux by JWST could be the light from Population III stars. Our simulations suggest that the UV flux can be dominated by Population III stars and the UV slope shows β ≲ −3 if future observations would reach galaxies with Mstars ∼ 105 M⊙ at z ∼ 20 of which the mass fraction of Population III stars can be greater than 10 per cent.
Evidence for late-time dust formation in the ejecta of supernova SN 1995N from emission-line asymmetries
Authors: Wesson R , Bevan A M , Barlow M J , De Looze I , Matsuura M , Clayton G , Andrews J 
Published: August 2023

ABSTRACT
We present a study of the dust associated with the core-collapse supernova SN 1995N. Infrared emission detected 14–15 yr after the explosion was previously attributed to thermally echoing circumstellar material (CSM) associated with the supernova (SN) progenitor. We argue that this late-time emission is unlikely to be an echo, and is more plausibly explained by newly formed dust in the SN ejecta, indirectly heated by the interaction between the ejecta and the CSM. Further evidence in support of this scenario comes from emission-line profiles in spectra obtained 22 yr after the explosion; these are asymmetric, showing greater attenuation on the red wing, consistent with absorption by dust within the expanding ejecta. The spectral energy distribution and emission-line profiles at epochs later than ∼5000 d are both consistent with the presence of about 0.4 M⊙ of amorphous carbon dust. The onset of dust formation is apparent in archival optical spectra, taken between 700 and 1700 d after the assumed explosion date. As this is considerably later than most other instances where the onset of dust formation has been detected, we argue that the explosion date must be later than previously assumed.
BCG alignment with the locations of cluster members and the large-scale structure out to 10 R200
Authors: Smith Rory , Hwang Ho Seong , Kraljic Katarina , Calderón-Castillo Paula , Jackson Thomas M , Pasquali Anna , Shin Jihye , Ko Jongwan , Yoo Jaewon , Kim Hyowon , Kim Jae-Woo 
Published: August 2023

ABSTRACT
Using a sample of &gt;200 clusters, each with typically 100–200 spectroscopically confirmed cluster members, we search for a signal of alignment between the position angle (PA) of the Brightest Cluster Galaxy (BCG) and the distribution of cluster members on the sky about the cluster centre out to projected distances of 3 R200. The deep spectroscopy, combined with corrections for spectroscopic incompleteness, makes our sample ideal to determine alignment signal strengths. We also use an SDSS based skeleton of the filamentary large-scale structure (LSS), and measure BCG alignment with the location of the LSS skeleton segments on the sky out to projected distances of 10 R200. The alignment signal is measured using three separate statistical measures; Rao’s spacing test (U), Kuiper’s V parameter (V), and the Binomial probability test (P). The significance of the BCG alignment signal with both cluster members and LSS segments is extremely high (1 in a million chance or less to be drawn randomly from a uniform distribution). We investigate a wide set of parameters that may influence the strength of the alignment signal. Clusters with more elliptical-shaped BCGs show stronger alignment with both their cluster members and LSS segments. Also, selecting clusters with closely connected filaments, or using a luminosity-weighted LSS skeleton, increases the alignment signal significantly. Alignment strength decreases with increasing projected distance. Combined, these results provide strong evidence for the growth of clusters and their BCGs by preferential feeding along the direction of the filaments in which they are embedded.
QUIJOTE scientific results – X. Spatial variations of Anomalous Microwave Emission along the Galactic plane
Authors: Fernández-Torreiro M , Rubiño-Martín J A , López-Caraballo C H , Génova-Santos R T , Peel M W , Guidi F , Harper S E , Artal E , Ashdown M , Barreiro R B , Casas F J , de la Hoz E , Herranz D , Hoyland R , Lasenby A , Martínez-Gonzalez E , Piccirillo L , Poidevin F , Rebolo R , Ruiz-Granados B , Tramonte D , Vansyngel F , Vielva P , Watson R A 
Published: August 2023

ABSTRACT
Anomalous microwave emission (AME) is an important emission component between 10 and 60 GHz that is not yet fully understood. It seems to be ubiquitous in our Galaxy and is observed at a broad range of angular scales. Here we use the new QUIJOTE-MFI wide survey data at 11, 13, 17, and 19 GHz to constrain the AME in the Galactic plane (|b| &lt; 10°) on degree scales. We built the spectral energy distribution between 0.408 and 3000 GHz for each of the 5309 0.9° pixels in the Galactic plane, and fitted a parametric model by considering five emission components: synchrotron, free–free, AME, thermal dust and CMB anisotropies. We show that not including QUIJOTE-MFI data points leads to the underestimation (up to 50 per cent) of the AME signal in favour of free–free emission. The parameters describing these components are then intercompared, looking for relations that help to understand AME physical processes. We find median values for the AME width, WAME, and for its peak frequency, νAME, respectively of $0.560^{+0.059}_{-0.050}$ and $20.7^{+2.0}_{-1.9}$ GHz, slightly in tension with current theoretical models. We find spatial variations throughout the Galactic plane for νAME, but only with reduced statistical significance. We report correlations of AME parameters with certain ISM properties, such as that between the AME emissivity (which shows variations with the Galactic longitude) and the interstellar radiation field, and that between the AME peak frequency and dust temperature. Finally, we discuss the implications of our results on the possible molecules responsible for AME.
Novel conservative methods for adaptive force softening in collisionless and multispecies N-body simulations
Authors: Hopkins Philip F , Nadler Ethan O , Grudić Michael Y , Shen Xuejian , Sands Isabel , Jiang Fangzhou 
Published: August 2023

ABSTRACT
Modelling self-gravity of collisionless fluids (e.g. ensembles of dark matter, stars, black holes, dust, and planetary bodies) in simulations is challenging and requires some force softening. It is often desirable to allow softenings to evolve adaptively, in any high-dynamic range simulation, but this poses unique challenges of consistency, conservation, and accuracy, especially in multiphysics simulations where species with different ‘softening laws’ may interact. We therefore derive a generalized form of the energy-and-momentum conserving gravitational equations of motion, applicable to arbitrary rules used to determine the force softening, together with consistent associated time-step criteria, interaction terms between species with different softening laws, and arbitrary maximum/minimum softenings. We also derive new methods to maintain better accuracy and conservation when symmetrizing forces between particles. We review and extend previously discussed adaptive softening schemes based on the local neighbour particle density, and present several new schemes for scaling the softening with properties of the gravitational field, i.e. the potential or acceleration or tidal tensor. We show that the ‘tidal softening’ scheme not only represents a physically motivated, translation and Galilean invariant and equivalence-principle respecting (and therefore conservative) method but also imposes negligible time-step or other computational penalties, ensuring that pairwise two-body scattering is small compared to smooth background forces and can resolve outstanding challenges in properly capturing tidal disruption of substructures (minimizing artificial destruction) while also avoiding excessive N-body heating. We make all of this public in the GIZMO code.
On the observability and identification of Population III galaxies with JWST
Authors: Trussler James A A , Conselice Christopher J , Adams Nathan J , Maiolino Roberto , Nakajima Kimihiko , Zackrisson Erik , Austin Duncan , Ferreira Leonardo , Harvey Tom 
Published: August 2023

ABSTRACT
We utilize theoretical models of Population III stellar + nebular spectra to investigate the prospects of observing and accurately identifying Population III galaxies with JWST using both deep imaging and spectroscopy. We investigate a series of different colour cuts, finding that a combination of NIRCam and MIRI photometry through the F444W−F560W, F560W−F770W colours offers the most robust identifier of potential z = 8 Pop III candidates. We calculate that NIRCam will have to reach ∼28.5–30.0 AB mag depths (1–20 h), and MIRI F560W must reach ∼27.5–29.0 AB mag depths (10–100 h) to achieve 5σ continuum detections of M* = 106 M⊙ Pop III galaxies at z = 8. We also discuss the prospects of identifying Pop III candidates through slitless and NIRSpec spectroscopic surveys that target Lyα, Hβ, and/or He ii λ1640. We find small differences in the Hβ rest-frame equivalent width (EW) between Pop III and non-Pop III galaxies, rendering this diagnostic likely impractical. Instead, we find that the detection of high EW He ii λ1640 emission will serve as the definitive Pop III identifier, requiring (ultra-)deep integrations (5–150 h) with NIRSpec/G140M for M* = 106 M⊙ Pop III galaxies at z = 8. However, MIRI F770W detections of Pop III galaxies will require substantial gravitational lensing (μ = 10) and/or fortuitous imaging of exceptionally massive (M* = 107 M⊙) Pop III galaxies. Thus, NIRCam medium-band imaging surveys that can search for high EW He ii λ1640 emitters in photometry may perhaps be a viable alternative for finding Pop III candidates.
The MUSE Ultra Deep Field (MUDF). IV. A pair of X-ray weak quasars at the heart of two extended Lyα nebulae
Authors: Lusso Elisabeta , Nardini Emanuele , Fumagalli Michele , Fossati Matteo , Arrigoni Battaia Fabrizio , Revalski Mitchell , Rafelski Marc , D’Odorico Valentina , Peroux Celine , Cristiani Stefano , Dayal Pratika , Haardt Francesco , Lofthouse Emma K 
Published: August 2023

ABSTRACT
We present the results obtained from follow-up observations of the MUSE Ultra Deep Field (MUDF) at X-ray energies with XMM–Newton. The MUDF is centred on a unique field with two bright, physically associated quasars at z ≃ 3.23, separated by ∼500 kpc in projection. Both quasars are embedded within extended Lyα nebulae (${\gtrsim}100\,{\rm kpc}$ at a surface brightness flux level of ≈6 × 10−19 ${\rm erg\,s^{-1}\,cm^{-2}\,arcsec^{-2}}$), whose elongated morphology is suggestive of an extended filament connecting the quasar haloes. The new X-ray observations presented here allow us to characterize the physical properties (e.g. X-ray slope, luminosities, gas column densities) in the innermost region of the MUDF quasars. We find that both quasars are X-ray underluminous compared to objects at similar ultraviolet luminosities. Based on our X-ray spectral analysis, absorbing columns of NH(z) ≳ 1023 cm−2 appear unlikely therefore such a weakness is possibly intrinsic. When also including literature data, we do not observe any detectable trend between the area of the nebulae and nuclear luminosities at both the rest-frame 2 keV and 2500 Å. The area is also not correlated with the X-ray photon index nor with the integrated band flux in the hard band (2–10 keV). We also do not find any trend between the extended Lyα emission of the nebulae and the nuclear X-ray luminosity. Finally, the properties of the MUDF quasars’ nebulae are consistent with the observed relation between the Lyα integrated luminosity of the nebulae and their area. Our results suggest that the quasar ionization power is not a strong driver of the morphology and size of the nebulae.