bluuebunny/crossref_metadata_2025_split huggingface dataset:
Drought stress increases the expression of barley defence genes with negative consequences for infesting cereal aphids
Authors: Leybourne Daniel J , Valentine Tracy A , Binnie Kirsty , Taylor Anna , Karley Alison J , Bos Jorunn I B 
Published: January 2022

Abstract
Crops are exposed to myriad abiotic and biotic stressors with negative consequences. Two stressors that are expected to increase under climate change are drought and infestation with herbivorous insects, including important aphid species. Expanding our understanding of the impact drought has on the plant–aphid relationship will become increasingly important under future climate scenarios. Here we use a previously characterized plant–aphid system comprising a susceptible variety of barley, a wild relative of barley with partial aphid resistance, and the bird cherry-oat aphid to examine the drought–plant–aphid relationship. We show that drought has a negative effect on plant physiology and aphid fitness, and provide evidence to suggest that plant resistance influences aphid responses to drought stress. Furthermore, we show that the expression of thionin genes, plant defensive compounds that contribute to aphid resistance, increase in susceptible plants exposed to drought stress but remain at constant levels in the partially resistant plant, suggesting that they play an important role in determining the success of aphid populations. This study highlights the role of plant defensive processes in mediating the interactions between the environment, plants, and herbivorous insects.
Regulation of lignin biosynthesis by an atypical bHLH protein CmHLB inChrysanthemum
Authors: Zhao Wenqian , Ding Lian , Liu Jiayou , Zhang Xue , Li Song , Zhao Kunkun , Guan Yunxiao , Song Aiping , Wang Haibin , Chen Sumei , Jiang Jiafu , Chen Fadi 
Published: January 2022

AbstractStem mechanical strength is one of the most important agronomic traits that affects the resistance of plants against insects and lodging, and plays an essential role in the quality and yield of plants. Several transcription factors regulate mechanical strength in crops. However, mechanisms of stem strength formation and regulation remain largely unexplored, especially in ornamental plants. In this study, we identified an atypical bHLH transcription factor CmHLB (HLH PROTEIN INVOLVED IN LIGNIN BIOSYNTHESIS) in chrysanthemum, belonging to a small bHLH sub-family — the PACLOBUTRAZOL RESISTANCE (PRE) family. Overexpression of CmHLB in chrysanthemum significantly increased mechanical strength of the stem, cell wall thickness, and lignin content, compared with the wild type. In contrast, CmHLB RNA interference lines exhibited the opposite phenotypes. RNA-seq analysis indicated that CmHLB promoted the expression of genes involved in lignin biosynthesis. Furthermore, we demonstrated that CmHLB interacted with Chrysanthemum KNOTTED ARABIDOPSIS THALIANA7 (CmKNAT7) through the KNOX2 domain, which has a conserved function, i.e. it negatively regulates secondary cell wall formation of fibres and lignin biosynthesis. Collectively, our results reveal a novel role for CmHLB in regulating lignin biosynthesis by interacting with CmKNAT7 and affecting stem mechanical strength in Chrysanthemum.
Does oxygen affect ageing mechanisms of Pinus densiflora seeds? A matter of cytoplasmic physical state
Authors: Gerna Davide , Ballesteros Daniel , Arc Erwann , Stöggl Wolfgang , Seal Charlotte E , Marami-Zonouz Nicki , Na Chae Sun , Kranner Ilse , Roach Thomas 
Published: January 2022

Abstract
During desiccation, the cytoplasm of orthodox seeds solidifies into an intracellular glass with highly restricted diffusion and molecular mobility. Temperature and water content govern seed ageing rates, while oxygen (O2) can promote deteriorative reactions. However, whether the cytoplasmic physical state affects involvement of O2 in seed ageing remains unresolved. We aged Pinus densiflora seeds by controlled deterioration (CD) at 45 °C and distinct relative humidity (RH), resulting in cells with a glassy (11% and 30% RH) or fluid (60% and 80% RH) cytoplasm. Hypoxic conditions (0.4% O2) during CD delayed seed deterioration, lipid peroxidation, and decline of antioxidants (glutathione, α-tocopherol, and γ-tocopherol), but only when the cytoplasm was glassy. In contrast, when the cytoplasm was fluid, seeds deteriorated at the same rate regardless of O2 availability, while being associated with limited lipid peroxidation, detoxification of lipid peroxide products, substantial loss of glutathione, and resumption of glutathione synthesis. Changes in metabolite profiles provided evidence of other O2-independent enzymatic reactions in a fluid cytoplasm, including aldo-keto reductase and glutamate decarboxylase activities. Biochemical profiles of seeds stored under seed bank conditions resembled those obtained after CD regimes that maintained a glassy cytoplasm. Overall, O2 contributed more to seed ageing when the cytoplasm was glassy, rather than fluid.
Observations of the initial formation and evolution of spiral galaxies at 1 &lt; z &lt; 3 in the CANDELS fields
Authors: Margalef-Bentabol Berta , Conselice Christopher J , Haeussler Boris , Casteels Kevin , Lintott Chris , Masters Karen , Simmons Brooke 
Published: January 2022

ABSTRACT
Many aspects concerning the formation of spiral and disc galaxies remain unresolved, despite their discovery and detailed study over the past 150 yr. As such, we present the results of an observational search for proto-spiral galaxies and their earliest formation, including the discovery of a significant population of spiral-like and clumpy galaxies at z &gt; 1 in deep Hubble Space Telescope CANDELS imaging. We carry out a detailed analysis of this population, characterizing their number density evolution, masses, star formation rates (SFR), and sizes. Overall, we find a surprisingly high overall number density of massive $M_{*} \gt 10^{10}\, \mathrm{M}_{\odot }$ spiral-like galaxies (including clumpy spirals) at z &gt; 1 of $0.18\, {\rm per}\, \mathrm{arcmin}^{-2}$. We measure and characterize the decline in the number of these systems at higher redshift using simulations to correct for redshift effects in identifications, finding that the true fraction of spiral-like galaxies grows at lower redshifts as ∼ (1 + z)−1.1. This is such that the absolute numbers of spirals increases by a factor of ∼10 between z = 2.5 and z = 0.5. We also demonstrate that these spiral-like systems have large sizes at z &gt; 2, and high SFRs, above the main-sequence, These galaxies represent a major mode of galaxy formation in the early Universe, perhaps driven by the spiral structure itself. We finally discuss the origin of these systems, including their likely formation through gas accretion and minor mergers, but conclude that major mergers are an unlikely cause.
Dark Energy Survey Year 3 results: galaxy clustering and systematics treatment for lens galaxy samples
Authors: Rodríguez-Monroy M , Weaverdyck N , Elvin-Poole J , Crocce M , Carnero Rosell A , Andrade-Oliveira F , Avila S , Bechtol K , Bernstein G M , Blazek J , Camacho H , Cawthon R , De Vicente J , DeRose J , Dodelson S , Everett S , Fang X , Ferrero I , Ferté A , Friedrich O , Gaztanaga E , Giannini G , Gruendl R A , Hartley W G , Herner K , Huff E M , Jarvis M , Krause E , MacCrann N , Mena-Fernández J , Muir J , Pandey S , Park Y , Porredon A , Prat J , Rosenfeld R , Ross A J , Rozo E , Rykoff E S , Sanchez E , Sanchez Cid D , Sevilla-Noarbe I , Tabbutt M , To C , Wagoner E L , Wechsler R H , Aguena M , Allam S , Amon A , Annis J , Bacon D , Baxter E , Bertin E , Bhargava S , Brooks D , Burke D L , Carrasco Kind M , Carretero J , Castander F J , Choi A , Conselice C , Costanzi M , da Costa L N , Pereira M E S , Desai S , Diehl H T , Flaugher B , Fosalba P , Frieman J , García-Bellido J , Giannantonio T , Gruen D , Gschwend J , Gutierrez G , Hinton S R , Hollowood D L , Honscheid K , Huterer D , Jain B , James D J , Kuehn K , Kuropatkin N , Lima M , Maia M A G , March M , Marshall J L , Melchior P , Menanteau F , Miller C J , Miquel R , Mohr J J , Morgan R , Palmese A , Paz-Chinchón F , Pieres A , Plazas Malagón A A , Roodman A , Scarpine V , Serrano S , Smith M , Soares-Santos M , Suchyta E , Tarle G , Thomas D , Varga T N ,   (DES Collaboration)
Published: January 2022

ABSTRACT
In this work, we present the galaxy clustering measurements of the two DES lens galaxy samples: a magnitude-limited sample optimized for the measurement of cosmological parameters, maglim, and a sample of luminous red galaxies selected with the redmagic algorithm. maglim/redmagic sample contains over 10 million/2.5 million galaxies and is divided into six/five photometric redshift bins spanning the range z ∈ [0.20, 1.05]/z ∈ [0.15, 0.90]. Both samples cover 4143 $\deg ^2$ over which we perform our analysis blind, measuring the angular correlation function with an S/N ∼ 63 for both samples. In a companion paper, these measurements of galaxy clustering are combined with the correlation functions of cosmic shear and galaxy–galaxy lensing of each sample to place cosmological constraints with a 3 × 2pt analysis. We conduct a thorough study of the mitigation of systematic effects caused by the spatially varying survey properties and we correct the measurements to remove artificial clustering signals. We employ several decontamination methods with different configurations to ensure the robustness of our corrections and to determine the systematic uncertainty that needs to be considered for the final cosmology analyses. We validate our fiducial methodology using lognormal mocks, showing that our decontamination procedure induces biases no greater than 0.5σ in the (Ωm, b) plane, where b is the galaxy bias.
The nozzle shock in tidal disruption events
Authors: Bonnerot Clément , Lu Wenbin 
Published: January 2022

ABSTRACT
Tidal disruption events (TDEs) occur when a star gets torn apart by the strong tidal forces of a supermassive black hole, which results in the formation of a debris stream that partly falls back towards the compact object. This gas moves along inclined orbital planes that intersect near pericentre, resulting in a so-called ‘nozzle shock’. We perform the first dedicated study of this interaction, making use of a two-dimensional simulation that follows the transverse gas evolution inside a given section of stream. This numerical approach circumvents the lack of resolution encountered near pericentre passage in global three-dimensional simulations using particle-based methods. As it moves inward, we find that the gas motion is purely ballistic, which near pericentre causes strong vertical compression that squeezes the stream into a thin sheet. Dissipation takes place at the resulting nozzle shock, inducing a rise in pressure that causes the collapsing gas to bounce back, although without imparting significant net expansion. As it recedes to larger distances, this matter continues to expand while remaining thin despite the influence of pressure forces. This gas evolution specifies the strength of the subsequent self-crossing shock, which we find to be more affected by black hole spin than previously estimated. We also evaluate the impact of general relativistic effects, viscous dissipation, magnetic fields, and radiative processes on the nozzle shock. This study represents an important step forward in the theoretical understanding of TDEs, bridging the gap between our robust knowledge of the fallback rate and the more complex following stages, during which most of the emission occurs.
Scattering and sublimation: a multiscale view of µm-sized dust in the inclined disc of HD 145718
Authors: Davies Claire L , Rich Evan A , Harries Tim J , Monnier John D , Laws Anna S E , Andrews Sean M , Bae Jaehan , Wilner David J , Anugu Narsireddy , Ennis Jacob , Gardner Tyler , Kraus Stefan , Labdon Aaron , le Bouquin Jean-Baptiste , Lanthermann Cyprien , Schaefer Gail H , Setterholm Benjamin R , ten Brummelaar Theo ,   G-LIGHTS collaboration
Published: January 2022

ABSTRACT
We present multi-instrument observations of the disc around the Herbig Ae star, HD 145718, employing geometric and Monte Carlo radiative transfer models to explore the disc orientation, the vertical and radial extent of the near-infrared (NIR) scattering surface, and the properties of the dust in the disc surface and sublimation rim. The disc appears inclined at 67–71°, with position angle, PA = −1.0 to 0.6°, consistent with previous estimates. The NIR scattering surface extends out to ${\sim}75\,$ au and we infer an aspect ratio, hscat(r)/r ∼ 0.24 in J band; ∼0.22 in H band. Our Gemini Planet Imager images and VLTI + CHARA NIR interferometry suggest that the disc surface layers are populated by grains ≳λ/2π in size, indicating these grains are aerodynamically supported against settling and/or the density of smaller grains is relatively low. We demonstrate that our geometric analysis provides a reasonable assessment of the height of the NIR scattering surface at the outer edge of the disc and, if the inclination can be independently constrained, has the potential to probe the flaring exponent of the scattering surface in similarly inclined (i ≳ 70°) discs. In re-evaluating HD 145718’s stellar properties, we found that the object’s dimming events – previously characterized as UX Or and dipper variability – are consistent with dust occultation by grains larger, on average, than found in the ISM. This occulting dust likely originates close to the inferred dust sublimation radius at $0.17\,$ au.
AGN light echoes and the accretion disc self-gravity limit
Authors: Lobban Andrew , King Andrew 
Published: January 2022

ABSTRACT
Accretion disc theory predicts that an AGN disc becomes self-gravitating and breaks up into stars at an outer radius Rsg ≃ 12 light-days, with effectively no free parameter. We present evidence that the longest observed AGN light echoes are all close to 12 d in the AGN rest frames. These observations give a stringent test of the AGN disc theory. Further monitoring should offer insight into the formation angular momentum of the gas forming the disc. For distant AGN, observed lags significantly longer than 12 d give lower limits on their redshifts.
Multicomponent DHOST analysis in galaxy clusters
Authors: Laudato Enrico , Salzano Vincenzo , Umetsu Keiichi 
Published: January 2022

ABSTRACT
Extended theories of gravity with additional scalar degrees of freedom have recently acquired increasing interest due to the presence of a screening mechanism that allows suppressing at small scales (e.g. the Solar system scale) every modification restoring general relativity (GR). In this work, we consider a second-order extended theory of gravity belonging to the family of degenerate high-order scalar-tensor theories (DHOST) characterized by a partial breaking of the Vainshtein screening mechanism. We study this model in two different scenarios as a description of dark energy (DE) only and as a description of both dark matter (DM) and DE. Such scenarios have been tested here by analysing a sample of 16 high-mass galaxy clusters targeted by the cluster lensing and supernova survey with Hubble program using two complementary probes, namely X-ray and strong- and weak-gravitational lensing observations. In mass modelling, we adopt a multicomponent approach including hot gas and galactic stellar contributions. For the majority of the clusters in our sample, results show mild Bayesian evidence in favour of the DHOST model as a description of DE over GR. This model also appears to alleviate the discrepancy present in GR between X-ray hydrostatic and lensing mass estimates. For the second scenario, where gravity acts as both DE and DM due to the partial breaking of the Vainshtein screening mechanism at cluster scales, the model is statistically disfavoured compared to GR.
Quenching of satellite galaxies of Milky Way analogues: reconciling theory and observations
Authors: Font Andreea S , McCarthy Ian G , Belokurov Vasily , Brown Shaun T , Stafford Sam G 
Published: January 2022

ABSTRACT
The vast majority of low-mass satellite galaxies around the Milky Way and M31 appear virtually devoid of cool gas and show no signs of recent or ongoing star formation. Cosmological simulations demonstrate that such quenching is expected and is due to the harsh environmental conditions that satellites face when joining the Local Group (LG). However, recent observations of Milky Way analogues in the SAGA survey present a very different picture, showing the majority of observed satellites to be actively forming stars, calling into question the realism of current simulations and the typicality of the LG. Here, we use the ARTEMIS suite of high-resolution cosmological hydrodynamical simulations to carry out a careful comparison with observations of dwarf satellites in the LG, SAGA, and the Local Volume (LV) survey. We show that differences between SAGA and the LG and LV surveys, as well as between SAGA and the ARTEMIS simulations, can be strongly reduced by considering differences in the host mass distributions and (more importantly) observational selection effects, specifically that low-mass satellites which have only recently been accreted are more likely to be star forming, have a higher optical surface brightness, and are therefore more likely to be included in the SAGA survey. This picture is confirmed using data from the deeper LV survey, which shows pronounced quenching at low masses, in accordance with the predictions of ΛCDM-based simulations.
A forward-modelling method to infer the dark matter particle mass from strong gravitational lenses
Authors: He Qiuhan , Robertson Andrew , Nightingale James , Cole Shaun , Frenk Carlos S , Massey Richard , Amvrosiadis Aristeidis , Li Ran , Cao Xiaoyue , Etherington Amy 
Published: January 2022

ABSTRACT
A fundamental prediction of the cold dark matter (CDM) model of structure formation is the existence of a vast population of dark matter haloes extending to subsolar masses. By contrast, other dark matter models, such as a warm thermal relic (WDM), predict a cutoff in the mass function at a mass which, for popular models, lies approximately between 107 and $10^{10}\, {\rm M}_\odot$. We use mock observations to demonstrate the viability of a forward modelling approach to extract information about low-mass dark haloes lying along the line of sight to galaxy–galaxy strong lenses. This can be used to constrain the mass of a thermal relic dark matter particle, mDM. With 50 strong lenses at Hubble Space Telescope resolution and a maximum pixel signal-to-noise ratio of ∼50, the expected median 2σ constraint for a CDM-like model (with a halo mass cutoff at $10^{7}\, {\rm M}_\odot$) is $m_\mathrm{DM} \gt 4.10 \, \mathrm{keV}$ (50 per cent chance of constraining mDM to be better than 4.10 keV). If, however, the dark matter is a warm particle of $m_\mathrm{DM}=2.2 \, \mathrm{keV}$, our ‘approximate Bayesian computation’ method would result in a median estimate of mDM between 1.43 and 3.21 keV. Our method can be extended to the large samples of strong lenses that will be observed by future telescopes and could potentially rule out the standard CDM model of cosmogony. To aid future survey design, we quantify how these constraints will depend on data quality (spatial resolution and integration time) as well as on the lensing geometry (source and lens redshifts).
Dwarf galaxy luminosity functions and cluster environments
Authors: Hashimoto Yasuhiro , Böhringer Hans , Umetsu Keiichi 
Published: January 2022

ABSTRACT
We report an investigation of the luminosity function (LF) of dwarf galaxies (Mi &lt; −15) inside 33 clusters at z ∼ 0.15–0.3, to address the crucial but unsettled problem of the faint-end slope (FS) in the cluster environments that may hold a key to the missing-satellite problem related to the standard cold dark matter formation scenario. By using a wide field imager mounted on the 8 m-class telescope, Subaru Suprime-Cam, and by selecting clusters in an optimal redshift range, we achieve a crucial balance between the depth and the spatial coverage of observation, that is essential for cluster dwarf studies. The deep and wide observations also provide us with image-by-image local background correction and tailor-made detection incompleteness correction on every cluster and background fields. These two essential but intertwined corrections were unfortunately often ignored in the previous studies. We find, when the accurate background and detection incompleteness corrections are made in a combined manner, that the faint end of the cluster LF shows a relatively flat slope (α ∼ −1.2 to −1.4), comparable to the field LF. We also find: (1) FS becomes steeper at larger cluster-centric distance. (2) Blue dwarf galaxies tend to show steeper FS. (3) Galaxy LFs show steeper slopes inside clusters with high X-ray luminosity although cluster-to-cluster variations are significant. Investigations of the FS are sensitive to various systematics, and variations among individual clusters that we need to address carefully. With a slope of −1.2 to −1.4, our study does not show the excess of dwarfs previously reported in some observational studies. Our findings may indicate the missing-satellite problem remains in galaxy clusters.
Distribution of the diffuse interstellar band λ6614 in the NGC 2264, Rosette Nebula, and S147 regions
Authors: Ma Wen-Jing , Chen Jian-Jun , Li Yin-Bi , Wu Ke-Fei , Zhang Wei , Chen Xiang-lei , Luo A-Li , Ren Juan-Juan , Wu Chao-Jian , Wu Hong 
Published: January 2022

ABSTRACT
Diffuse interstellar bands (DIBs) are absorption features arising from the interstellar medium, for which the carriers remain unclear. In this work, a total of 3115 stars in the regions of NGC 2264, the Rosette Nebula, and S147 are selected from LAMOST-MRS to study the spatial and velocity distributions of the DIB λ6614 carrier. From the spatial distribution, we find that DIB λ6614 carrier clouds appear to be widely and inhomogeneously distributed in the three target regions. They are either closer or further in distance, or much wider than the three nebulae, and there are gaps within them. The radial velocities of the DIB λ6614 carrier clouds are on average about 13, 20, and 10 km s−1 slower than the radial velocities of the nebulae in the NGC 2264, Rosette Nebula, and S147 regions, respectively. Furthermore, there is probably a high-extinction region from 0.6 to 0.8 kpc in the NGC 2264 direction, where the DIB λ6614 carrier vanishes. In the S147 region, the DIB λ6614 cloud is possibly discontinuous, and the tomographic evidence suggests that there are two DIB λ6614 clouds. The first cloud is at 0.3–0.9 kpc, which is in or near the Local Arm, while the second one emerges at about 1.8 kpc from the Sun and may be associated with S147 and in the Perseus Arm.