bluuebunny/crossref_metadata_2025_split huggingface dataset:
Neural Responses and Perceptual Sensitivity to Sound Depend on Sound-Level Statistics
Authors: Herrmann Björn , Augereau Thomas , Johnsrude Ingrid S. 
Published: June 2020

AbstractSensitivity to sound-level statistics is crucial for optimal perception, but research has focused mostly on neurophysiological recordings, whereas behavioral evidence is sparse. We use electroencephalography (EEG) and behavioral methods to investigate how sound-level statistics affect neural activity and the detection of near-threshold changes in sound amplitude. We presented noise bursts with sound levels drawn from distributions with either a low or a high modal sound level. One participant group listened to the stimulation while EEG was recorded (Experiment I). A second group performed a behavioral amplitude-modulation detection task (Experiment II). Neural activity depended on sound-level statistical context in two different ways. Consistent with an account positing that the sensitivity of neurons to sound intensity adapts to ambient sound level, responses for higher-intensity bursts were larger in low-mode than high-mode contexts, whereas responses for lower-intensity bursts did not differ between contexts. In contrast, a concurrent slow neural response indicated prediction-error processing: The response was larger for bursts at intensities that deviated from the predicted statistical context compared to those not deviating. Behavioral responses were consistent with prediction-error processing, but not with neural adaptation. Hence, neural activity adapts to sound-level statistics, but fine-tuning of perceptual sensitivity appears to involve neural prediction-error responses.
Induction of IRAK-M in melanoma induces caspase-3 dependent apoptosis by reducing TRAF6 and calpastatin levels
Authors: Geng Degui , Ciavattone Nicholas , Lasola Jackline Joy , Shrestha Rojesh , Sanchez Amelia , Guo Jitao , Vlk Alexandra , Younis Rania , Wang Lucy , Brown Alex J. , Zhang Yuji , Velasco-Gonzalez Cruz , Tan Aik-Choon , Davila Eduardo 
Published: June 2020

AbstractMelanoma represents the most serious type of skin cancer. Although recent years have seen advances using targeted and immunotherapies, most patients remain at high risk for tumor recurrence. Here we show that IRAK-M, a negative regulator of MyD88 signaling, is deficient or low in melanoma and expression levels correlate with patient survival. Inducing IRAK-M expression using genetic approaches or epigenetic modifiers initiates apoptosis by prompting its interaction with TRAF6 via IRAK-M’s C-terminal domain. This complex recruits and degrades calpastatin which stimulates calpain activity and triggers caspase-3-dependent but caspase-8,−9-independent apoptosis. Using a drug screen, we identified compounds that induced IRAK-M expression. Administration of IRAK-M-inducing drugs reduced tumor growth in mice but was ineffective against IRAK-M knock-down tumors. These results uncover a previously uncharacterized apoptosis pathway, emphasize IRAK-M as a potential therapeutic target and suggest that the anticancer activity of certain drugs could do so through their ability to induce IRAK-M expression.
Teaching Preschoolers With Autism to Use Different Speech-Generating Device Display Formats During Play: Intervention and Secondary Factors
Authors: Gevarter Cindy , Horan Keri , Sigafoos Jeff 
Published: June 2020

Purpose
Children with autism spectrum disorder (ASD) and complex communication needs are increasingly taught to use tablet-based speech-generating devices (SGDs). An important issue in designing such interventions is the selection of an appropriate format for displaying vocabulary. The purpose of this study was to determine (a) whether young children with ASD can be taught to use different SGD vocabulary display formats and (b) whether there are differences across the formats on a range of secondary measures (e.g., preference and generalization).

Method
Five preschoolers with ASD (and prior experience with simpler aided augmentative and alternative communication) were taught to use grid and visual scene display SGDs during a play-based intervention. Acquisition of functional responding was assessed using a single-case experimental design. Secondary variables included error types, antecedents for communication, preference, and generalization.

Results
All participants increased their use of functional target vocabulary using both the grid and the simple visual scene display. Of the five participants, three showed similar performance with both formats, whereas two had slightly higher rates of functional responding with the grid. Individualized differences across participants and formats were apparent across secondary variables (e.g., preference, error types, generalization).

Conclusions
Both simple grid and visual scene displays may be viable options when teaching functional use of SGDs to children with ASD who have prior aided augmentative and alternative communication experience. Analyzing secondary variables beyond device acquisition (e.g., generalization, preference) may have implications for individualizing intervention.
Transparent conductive silver nanowires films on glass substrate
Authors: Zhong Jianjun , Wang Yuehui 
Published: June 2020

Silver nanowires (AgNWs) with the length and diameter of 25–35 μm and 25–35 nm, respectively, were prepared via a polyol reduction process using FeCl3 and NaBr as reaction inhibitors. The molar ratio of FeCl3 to NaBr has an influence on the yield of the product, but has little influence on the morphology of the product. Transparent conductive AgNWs films were fabricated on a glass slide and the optoelectronic and electrothermal properties of the film were investigated. The experimental results reveal that AgNWs heated at 25–170°C remained intact, and fused into discontinuous segments after heated at 200°C; and AgNWs films have good conductivities (51.2 to 20.5 Ω sq−1), excellent transmittance values (96.3 to 95.7%), and low surface roughness values (12.7 to 18.3 nm). The transparent AgNWs film heaters show fast heat response to reach its steady‐state temperature and good electro‐thermal conversion behaviour at low input voltages.
Microstructure and mechanical properties of Zr‐modified Al–7Si–0.35Mg–0.2Ti cast alloy
Authors: Zhang Zhuang , Du Xiaodong , Zhuang Pengcheng , Chai Rong , Wang Changjian , Zhang Hao 
Published: June 2020

In this research, four specimens of hypo‐eutectic Al–7Si–0.35Mg–0.2Ti–xZr (x = 0, 0.1, 0.2, 0.3 wt%) cast alloys were fabricated via a traditional casting method. The effect of different concentrations of Zr on the microstructure and mechanical properties of cast alloys was investigated through metallographic observation, SEM analysis, TEM observations, tensile strength testing, and Vickers hardness test. The results show that the plate‐like shape eutectic Si phase is gradually transformed into fine fibrous eutectic Si phase, and is more evenly distributed as the content of Zr increased. The α‐Al matrix grains are transformed from dendrites to isometric grains, of which the grains sizes became smaller. The results of the tensile test show that with the addition of 0.2% Zr, Al–7Si–0.35Mg–0.2Ti alloys obtain the best tensile properties. The ultimate tensile strength and elongation values are 221 MPa and 11%, the number of which is increased by 14.5 and 71.9% than base alloy, respectively. Additionally, the alloy's yield strength, Vickers hardness, and other comprehensive mechanical properties have also improved significantly.
Controlled functionalisation of graphene oxide using ethylene diamine: a one‐pot synthesis approach for chromium sorption
Authors: Govindankutty Gopika , Hareendran Shreya , Sathish Asha , Kamaraj Nithya 
Published: June 2020

Introduction of ethylene diamine into the layers of graphene oxide was achieved through direct compounding method. Graphene oxide intercalated with ethylene diamine was characterised by Fourier transform‐infrared spectroscopy (FT‐IR), X‐ray diffraction (XRD), thermo gravimetric analysis (TGA) and scanning electron microscopy–energy dispersive X‐ray spectroscopy (SEM‐EDX) techniques. The efficiency of the material in adsorbing chromium was evaluated through batch scale studies by optimising parameters like pH, concentration and contact time. The material renders a monolayer adsorption capacity of 69.93 mg/g, at pH 1 within 60 min time period for a minimal dosage of 0.05 g. The ethylene diamine modified graphene oxide thus appeals to be a promising adsorbent for environmental applications.
Anisotropy of random motions of gas in Messier 33
Authors: Chemin Laurent , Braine Jonathan , Combes Françoise , Kam Zacharie S. , Carignan Claude 
Published: June 2020

Context. The ellipsoid of random motions of the gaseous medium in galactic disks is often considered isotropic, as appropriate if the gas is highly collisional. However, the collisional or collisionless behavior of the gas is a subject of debate. If the gas is clumpy with a low collision rate, then the often observed asymmetries in the gas velocity dispersion could be hints of anisotropic motions in a gaseous collisionless medium.
Aims. We study the properties of anisotropic and axisymmetric velocity ellipsoids from maps of the gas velocity dispersion in nearby galaxies. This data allow us to measure the azimuthal-to-radial axis ratio of gas velocity ellipsoids, which is a useful tool to study the structure of gaseous orbits in the disk. We also present the first estimates of perturbations in gas velocity dispersion maps by applying an alternative model that considers isotropic and asymmetric random motions.
Methods. High-quality velocity dispersion maps of the atomic medium at various angular resolutions of the nearby spiral galaxy Messier 33, are used to test the anisotropic and isotropic velocity models. The velocity dispersions of hundreds of individual molecular clouds are also analyzed.
Results. The HI velocity dispersion of M 33 is systematically larger along the minor axis, and lower along the major axis. Isotropy is only possible if asymmetric motions are considered. Fourier transforms of the H I velocity dispersions reveal a bisymmetric mode which is mostly stronger than other asymmetric motions and aligned with the minor axis of the galaxy. Within the anisotropic and axisymmetric velocity model, the stronger bisymmetry is explained by a radial component that is larger than the azimuthal component of the ellipsoid of random motions, thus by gaseous orbits that are dominantly radial. The azimuthal anisotropy parameter is not strongly dependent on the choice of the vertical dispersion. The velocity anisotropy parameter of the molecular clouds is observed highly scattered.
Conclusions. Perturbations such as HI spiral-like arms could be at the origin of the gas velocity anisotropy in M 33. Further work is necessary to assess whether anisotropic velocity ellispsoids can also be invoked to explain the asymmetric gas random motions of other galaxies.
Global photometric properties of (162173) Ryugu
Authors: Tatsumi E. , Domingue D. , Schröder S. , Yokota Y. , Kuroda D. , Ishiguro M. , Hasegawa S. , Hiroi T. , Honda R. , Hemmi R. , Le Corre L. , Sakatani N. , Morota T. , Yamada M. , Kameda S. , Koyama T. , Suzuki H. , Cho Y. , Yoshioka K. , Matsuoka M. , Honda C. , Hayakawa M. , Hirata N. , Hirata N. , Yamamoto Y. , Vilas F. , Takato N. , Yoshikawa M. , Abe M. , Sugita S. 
Published: June 2020

Context.The Hayabusa2 spacecraft launched by Japan Aerospace Exploration Agency has been conducting observations of the asteroid (162173) Ryugu since June 2018. The Telescopic Optical Navigation Camera (ONC-T) onboard Hayabusa2 has obtained thousands of images under a variety of illumination and viewing conditions.Aims.Our objective is to examine and validate the camera calibration, derive a photometric correction for creating global albedo maps, and to interpret the photometric modeling results to characterize the surface of Ryugu.Methods.We observed (162173) Ryugu with the Gemini-South telescope, and combined these measurements with other published ground-based observations of the asteroid. The ground-based observations were compared with the data obtained by ONC-T in order to validate the radiometric calibration mutually. We used a combination of the Hapke disk-integrated and disk-resolved model equations to simultaneously analyze the combined ground- and spacecraft-based data.Results.The average spectrum of Ryugu was classified as Cb-type following the SMASSII taxonomy and C/F-type following the Tholen taxonomy based on spacecraft observations. We derived Hapke model parameters for all seven color filters, which allowed us to photometrically correct images to within an error of <10% for ~80% of the image pixels used in the modeling effort. Using this model, we derived a geometric albedo of 4.0 ± 0.5% (vband) for Ryugu. The average reflectance factor at the standard illumination condition was 1.87 ± 0.14% in thevband. Moreover we measured a phase reddening of (2.0 ± 0.7) × 10−3μm−1deg−1for Ryugu, similar to that observed for the asteroid (101955) Bennu.Conclusions.The global color map showed that the general trend was for darker regions to also be redder regions, however there were some distinct exceptions to this trend. For example, Otohime Saxum was bright and red while Kibidango crater was dark and blue. The darkness and flatness of Ryugu’s reflectance might be caused by a high abundance of organic materials.
Using radio triangulation to understand the origin of two subsequent type II radio bursts
Authors: Jebaraj I. C. , Magdalenić J. , Podladchikova T. , Scolini C. , Pomoell J. , Veronig A. M. , Dissauer K. , Krupar V. , Kilpua E. K. J. , Poedts S. 
Published: June 2020

Context. Eruptive events such as coronal mass ejections (CMEs) and flares accelerate particles and generate shock waves which can arrive at Earth and can disturb the magnetosphere. Understanding the association between CMEs and CME-driven shocks is therefore highly important for space weather studies.
Aims. We present a study of the CME/flare event associated with two type II bursts observed on September 27, 2012. The aim of the study is to understand the relationship between the observed CME and the two distinct shock wave signatures.
Methods. The multiwavelength study of the eruptive event (CME/flare) was complemented with radio triangulation of the associated radio emission and modelling of the CME and the shock wave employing MHD simulations.
Results. We found that, although temporal association between the type II bursts and the CME is good, the low-frequency type II (LF-type II) burst occurs significantly higher in the corona than the CME and its relationship to the CME is not straightforward. The analysis of the EIT wave (coronal bright front) shows the fastest wave component to be in the southeast quadrant of the Sun. This is also the quadrant in which the source positions of the LF-type II were found to be located, probably resulting from the interaction between the shock wave and a streamer.
Conclusions. The relationship between the CME/flare event and the shock wave signatures is discussed using the temporal association, as well as the spatial information of the radio emission. Further, we discuss the importance and possible effects of the frequently non-radial propagation of the shock wave.
Observed sizes of planet-forming disks trace viscous spreading
Authors: Trapman L. , Rosotti G. , Bosman A. D. , Hogerheijde M. R. , van Dishoeck E. F. 
Published: June 2020

Context. The evolution of protoplanetary disks is dominated by the conservation of angular momentum, where the accretion of material onto the central star is fed by the viscous expansion of the outer disk or by disk winds extracting angular momentum without changing the disk size. Studying the time evolution of disk sizes therefore allows us to distinguish between viscous stresses or disk winds as the main mechanism of disk evolution. Observationally, estimates of the size of the gaseous disk are based on the extent of CO submillimeter rotational emission, which is also affected by the changing physical and chemical conditions in the disk during the evolution.
Aims. We study how the gas outer radius measured from the extent of the CO emission changes with time in a viscously expanding disk. We also investigate to what degree this observable gas outer radius is a suitable tracer of viscous spreading and whether current observations are consistent with viscous evolution.
Methods. For a set of observationally informed initial conditions we calculated the viscously evolved density structure at several disk ages and used the thermochemical code DALI to compute synthetic emission maps, from which we measured gas outer radii in a similar fashion as observations.
Results. The gas outer radii (RCO, 90%) measured from our models match the expectations of a viscously spreading disk: RCO, 90% increases with time and, for a given time, RCO, 90% is larger for a disk with a higher viscosity αvisc. However, in the extreme case in which the disk mass is low (Mdisk ≤ 10−4 M⊙) and αvisc is high (≥10−2), RCO, 90% instead decreases with time as a result of CO photodissociation in the outer disk. For most disk ages, RCO, 90% is up to ~12× larger than the characteristic size Rc of the disk, and RCO, 90%/Rc is largest for the most massive disk. As a result of this difference, a simple conversion of RCO, 90% to αvisc overestimates the true αvisc of the disk by up to an order of magnitude. Based on our models, we find that most observed gas outer radii in Lupus can be explained using viscously evolving disks that start out small (Rc(t = 0) ≃ 10 AU) and have a low viscosity (αvisc = 10−4−10−3).
Conclusions. Current observations are consistent with viscous evolution, but expanding the sample of observed gas disk sizes to star-forming regions, both younger and older, would better constrain the importance of viscous spreading during disk evolution.
Masses for the seven planets in K2-32 and K2-233
Authors: Lillo-Box J. , Lopez T. A. , Santerne A. , Nielsen L. D. , Barros S. C. C. , Deleuil M. , Acuña L. , Mousis O. , Sousa S. G. , Adibekyan V. , Armstrong D. J. , Barrado D. , Bayliss D. , Brown D. J. A. , Demangeon O. D. S. , Dumusque X. , Figueira P. , Hojjatpanah S. , Osborn H. P. , Santos N. C. , Udry S. 
Published: June 2020

Context. High-precision planetary densities are key pieces of information necessary to derive robust atmospheric properties for extrasolar planets. Measuring precise masses is the most challenging part of this task, especially in multi-planetary systems. The ESO-K2 collaboration focuses on the follow-up of a selection of multi-planetary systems detected by the K2 mission using the HARPS instrument with this goal in mind.
Aims. In this work, we measure the masses and densities of two multi-planetary systems: a four-planet near resonant chain system (K2-32) and a young (~400 Myr old) planetary system consisting of three close-in small planets (K2-233).
Methods. We obtained 199 new HARPS observations for K2-32 and 124 for K2-233 covering a long baseline of more than three years. We performed a joint analysis of the radial velocities and K2 photometry with PASTIS to precisely measure and constrained the properties of these planets, focusing on their masses and orbital properties.
Results. We find that K2-32 is a compact scaled-down version of the Solar System’s architecture, with a small rocky inner planet (Me = 2.1−1.1+1.3 M⊕, Pe ~ 4.35 days) followed by an inflated Neptune-mass planet (Mb = 15.0−1.7+1.8 M⊕, Pb ~ 8.99 days) and two external sub-Neptunes (Mc = 8.1 ± 2.4 M⊕, Pc ~ 20.66 days; Md = 6.7 ± 2.5 M⊕, Pd ~ 31.72 days). K2-32 becomes one of the few multi-planetary systems with four or more planets known where all have measured masses and radii. Additionally, we constrain the masses of the three planets in the K2-233 system through marginal detection of their induced radial velocity variations. For the two inner Earth-size planets we constrain their masses at a 95% confidence level to be smaller than Mb < 11.3 M⊕ (Pb ~ 2.47 days), Mc < 12.8 M⊕ (Pc ~ 7.06 days). The outer planet is a sub-Neptune size planet with an inferred mass of Md = 8.3−4.7+5.2 M⊕ (Md < 21.1 M⊕, Pd ~ 24.36 days).
Conclusions. Our observations of these two planetary systems confirm for the first time the rocky nature of two planets orbiting a young star, with relatively short orbital periods (<7 days). They provide key information for planet formation and evolution models of telluric planets. Additionally, the Neptune-like derived masses of the three planets, K2-32 b, c, d, puts them in a relatively unexplored regime of incident flux and planet mass, which is key for transmission spectroscopy studies in the near future.
No universal connection between the vertical magnetic field and the umbra-penumbra boundary in sunspots
Authors: Löptien B. , Lagg A. , van Noort M. , Solanki S. K. 
Published: June 2020

Context. It has been reported that the boundary between the umbra and the penumbra of sunspots occurs at a canonical value of the strength of the vertical magnetic field, independently of the size of the spot. This critical field strength is interpreted to be the threshold for the onset of magnetoconvection.
Aims. Here we investigate the reasons why this criterion, also called the Jurčák criterion in the literature, does not always identify the boundary between the umbra and the penumbra.
Methods. We performed a statistical analysis of 23 sunspots observed with Hinode/SOT. We compared the properties of the continuum intensity and the vertical magnetic field between filaments and spines and how they vary between spots of different sizes.
Results. We find that the inner boundary of the penumbra is not related to a universal value of the vertical magnetic field. The properties of spines and filaments vary between spots of different sizes. Both components are darker in larger spots and the spines exhibit a stronger vertical magnetic field. These variations of the properties of filaments and spines with the spot size are also the reason for the reported invariance in the averaged vertical magnetic field at 50% of the mean continuum intensity.
Conclusions. The formation of filaments and the onset of magnetoconvection are not related to a canonical value of the strength of the vertical magnetic field. The seemingly unique magnetic field strength is rather an effect of the filling factor of spines and penumbral filaments.