bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Impact of Clear Speech on the Perceptual and Acoustic Properties of Fricative–Vowel Sequences in Speakers With Dysarthria
Authors: Martel-Sauvageau Vincent , Breton Myriam , Chabot Alexandra , Langlois Mélanie 
Published: March 2021

Purpose
Studies have reported that clear speech has the potential to influence suprasegmental and segmental aspects of speech, in both healthy and dysarthric speakers. While the impact of clear speech has been studied on the articulation of individual segments, few studies have investigated its effects on coarticulation with multisegment sequences such as fricative–vowel.

Objectives
The goals of this study are to investigate, in healthy and dysarthric speech, the impact of clear speech on (a) the perception of anticipatory vowel coarticulation in fricatives and (b) the acoustic characteristics of this effect.

Method
Ten speakers with dysarthria secondary to idiopathic Parkinson's disease were recruited as well as 10 age- and sex-matched healthy speakers. A sentence reading task was performed in natural and clear speaking conditions. The sentences contained words with the initial fricatives /s/ and /ʃ/ preceded by /ə/ and followed by the vowels /i/, /y/, /u/, or /a/. For the perceptual measurements, five listeners were recruited and were asked to predict the upcoming word by listening only to the isolated fricative. Acoustic analyses consisted of spectral moment analysis (M1–M4) on averaged time series.

Results
Perceptual findings report that identification rates were improved with clear speech for the speakers with dysarthria, but only for the fricative–/i/ sequences. Error pattern analysis indicates that this improvement is associated with an increase in the roundness parameter (lip spreading) identification. Acoustic results are unclear for M1 and M3 but suggest that M2 and M4 differentiation between the rounded versus unrounded vowel contexts is increased with clear speech for the speakers with dysarthria.

Discussion
Taken together, these findings suggest that clear speech may improve lip coordination in dysarthric speakers with Parkinson's disease. However, the impact of clear speech on the acoustic measures of fricative spectral moments is somewhat limited. This suggests that these metrics, when taken individually, do not capture the entire complexity of fricative–vowel coarticulation.
Spatial distribution of the aromatic and aliphatic carbonaceous nanograin features in the protoplanetary disk around HD 100546
Authors: Habart E. , Boutéraon T. , Brauer R. , Ysard N. , Pantin E. , Marchal A. , Jones A. P. 
Published: March 2021

Context. Carbonaceous nanograins are present at the surface of protoplanetary disks around Herbig Ae/Be stars, where most of the ultraviolet energy from the central star is dissipated. Efficiently coupled to the gas, they are unavoidable to understand the physics and chemistry of these disks. Furthermore, nanograins are able to trace the outer flaring parts of the disk and possibly the gaps from which the larger grains are missing. However, their evolution through the disks, from internal to external regions, is only poorly understood so far.
Aims. Our aim is to examine the spatial distribution and evolution of the nanodust emission in the emblematic (pre-)transitional protoplanetary disk HD 100546. This disk shows many structures (annular gaps, rings, and spirals) and reveals very rich carbon nanodust spectroscopic signatures (aromatic, aliphatic) in a wide spatial range of the disk (~20−200 au).
Methods. We analysed adaptive optics spectroscopic observations in the 3–4 μm range (angular resolution of ~0.1′′) and imaging and spectroscopic observations in the 8–12 μm range (angular resolution of ~0.3′′). The hyperspectral cube was decomposed into a sum of spatially coherent dust components using a Gaussian decomposition algorithm. We compared the data to model predictions using the heterogeneous dust evolution model for interstellar solids (THEMIS), which is integrated in the radiative transfer code POLARIS by calculating the thermal and stochastic heating of micro- and nanometre-sized dust grains for a given disk structure.
Results. We find that the aromatic features at 3.3, 8.6, and 11.3 μm, and the aliphatic features between 3.4 and 3.5 μm are spatially extended; each band shows a specific morphology dependent on the local physical conditions. The aliphatic-to-aromatic band ratio, 3.4/3.3, increases with the distance from the star from ~0.2 (at 0.2′′ or 20 au) to ~0.45 (at 1′′ or 100 au), suggesting UV processing. In the 8–12 μm observed spectra, several features characteristic of aromatic particles and crystalline silicates are detected. Their relative contribution changes with the distance to the star. The model predicts that the features and adjacent continuum are due to different combinations of grain sub-populations, in most cases with a high dependence on the intensity of the UV field. The model reproduces the spatial emission profiles of the bands well, except for the inner 20-40 au, where the observed emission of the 3.3 and 3.4 μm bands is, unlike the predictions, flat and no longer increases with the UV field.
Conclusions. With our approach that combines observational data in the near- to mid-IR and disk modelling, we deliver constraints on the spatial distribution of nano-dust particles as a function of the disk structure and radiation field.
Asteroid spectral taxonomy using neural networks
Authors: Penttilä A. , Hietala H. , Muinonen K. 
Published: March 2021

Aims. We explore the performance of neural networks in automatically classifying asteroids into their taxonomic spectral classes. We particularly focus on what the methodology could offer the ESA Gaia mission.
Methods. We constructed an asteroid dataset that can be limited to simulating Gaia samples. The samples were fed into a custom-designed neural network that learns how to predict the samples’ spectral classes and produces the success rate of the predictions. The performance of the neural network is also evaluated using three real preliminary Gaia asteroid spectra.
Results. The overall results show that the neural network can identify taxonomic classes of asteroids in a robust manner. The success in classification is evaluated for spectra from the nominal 0.45–2.45 μm wavelength range used in the Bus-DeMeo taxonomy, and from a limited range of 0.45–1.05 μm following the joint wavelength range of Gaia observations and the Bus-DeMeo taxonomic system.
Conclusions. The obtained results indicate that using neural networks to execute automated classification is an appealing solution for maintaining asteroid taxonomies, especially as the size of the available datasets grows larger with missions like Gaia.
Activity of the Jupiter co-orbital comet P/2019 LD2(ATLAS) observed with OSIRIS at the 10.4 m GTC
Authors: Licandro J. , de León J. , Moreno F. , de la Fuente Marcos C. , de la Fuente Marcos R. , Cabrera-Lavers A. , Lara L. , de Souza-Feliciano A. , De Prá M. , Pinilla-Alonso N. , Geier S. 
Published: March 2021

Context.The existence of comets with heliocentric orbital periods close to that of Jupiter (i.e., co-orbitals) has been known for some time. Comet 295P/LINEAR (2002 AR2) is a well-known quasi-satellite of Jupiter. However, their orbits are not long-term stable, and they may eventually experience flybys with Jupiter at very close range, close enough to trigger tidal disruptions like the one suffered by comet Shoemaker-Levy 9 in 1992.Aims.Our aim was to study the observed activity and the dynamical evolution of the Jupiter transient co-orbital comet P/2019 LD2(ATLAS) and its dynamical evolution.Methods.We present results of an observational study of P/2019 LD2carried out with the 10.4 m Gran Telescopio Canarias (GTC) that includes image analyses using a Monte Carlo dust tail fitting code to characterize its level of cometary activity, and spectroscopic studies to search for gas emission. We also presentN-body simulations to explore its past, present, and future orbital evolution.Results.Images of P/2019 LD2obtained on May 16, 2020, show a conspicuous coma and tail, but the spectrum obtained on May 17, 2020, does not exhibit any evidence of CN, C2, or C3emission. The comet brightness in a 2.6′′ aperture diameter isr′ = 19.34 ± 0.02 mag, with colors (g′−r′) = 0.78 ± 0.03, (r′−i′) = 0.31 ± 0.03, and (i′−z′) = 0.26 ± 0.03. The temporal dependence of the dust loss rate of P/2019 LD2can be parameterized by a Gaussian function having a full width at half maximum of 350 days, with a maximum dust mass loss rate of 60 kg s−1reached on August 15, 2019. The total dust loss rate from the beginning of activity until the GTC observation date (May 16, 2020) is estimated at 1.9 × 109kg. Comet P/2019 LD2is now an ephemeral co-orbital of Jupiter, following what looks like a short arc of a quasi-satellite cycle that started in 2017 and will end in 2028. On January 23, 2063, it will experience a very close encounter with Jupiter at perhaps 0.016 au; its probability of escaping the solar system during the next 0.5 Myr is estimated to be 0.53 ± 0.03.Conclusions.Photometry and tail model results show that P/2019 LD2is a kilometer-sized object, in the size range of the Jupiter-family comets, with a typical comet-like activity most likely linked to sublimation of crystalline water ice and clathrates. Its origin is still an open question. Our numerical studies give a probability of this comet having been captured from interstellar space during the last 0.5 Myr of 0.49 ± 0.02 (average and standard deviation), 0.67 ± 0.06 during the last 1 Myr, 0.83 ± 0.06 over 3 Myr, and 0.91 ± 0.09 during the last 5 Myr.
The GAPS programme at TNG
Authors: Rainer M. , Borsa F. , Pino L. , Frustagli G. , Brogi M. , Biazzo K. , Bonomo A. S. , Carleo I. , Claudi R. , Gratton R. , Lanza A. F. , Maggio A. , Maldonado J. , Mancini L. , Micela G. , Scandariato G. , Sozzetti A. , Buchschacher N. , Cosentino R. , Covino E. , Ghedina A. , Gonzalez M. , Leto G. , Lodi M. , Martinez Fiorenzano A. F. , Molinari E. , Molinaro M. , Nardiello D. , Oliva E. , Pagano I. , Pedani M. , Piotto G. , Poretti E. 
Published: March 2021

Context. Transiting ultra-hot Jupiters are ideal candidates for studying the exoplanet atmospheres and their dynamics, particularly by means of high-resolution spectra with high signal-to-noise ratios. One such object is KELT-20b. It orbits the fast-rotating A2-type star KELT-20. Many atomic species have been found in its atmosphere, with blueshifted signals that indicate a day- to night-side wind.
Aims. We observe the atmospheric Rossiter-McLaughlin effect in the ultra-hot Jupiter KELT-20b and study any variation of the atmospheric signal during the transit. For this purpose, we analysed five nights of HARPS-N spectra covering five transits of KELT-20b.
Methods. We computed the mean line profiles of the spectra with a least-squares deconvolution using a stellar mask obtained from the Vienna Atomic Line Database (Teff = 10 000 K, log g = 4.3), and then we extracted the stellar radial velocities by fitting them with a rotational broadening profile in order to obtain the radial velocity time-series. We used the mean line profile residuals tomography to analyse the planetary atmospheric signal and its variations. We also used the cross-correlation method to study a previously reported double-peak feature in the FeI planetary signal.
Results. We observed both the classical and the atmospheric Rossiter-McLaughlin effect in the radial velocity time-series. The latter gave us an estimate of the radius of the planetary atmosphere that correlates with the stellar mask used in our work (Rp+atmo∕Rp = 1.13 ± 0.02). We isolated the planetary atmospheric trace in the tomography, and we found radial velocity variations of the planetary atmospheric signal during transit with an overall blueshift of ≈10 km s−1, along with small variations in the signal depth, and less significant, in the full width at half maximum (FWHM). We also find a possible variation in the structure and position of the FeI signal in different transits.
Conclusions. We confirm the previously detected blueshift of the atmospheric signal during the transit. The FWHM variations of the atmospheric signal, if confirmed, may be caused by more turbulent condition at the beginning of the transit, by a variable contribution of the elements present in the stellar mask to the overall planetary atmospheric signal, or by iron condensation. The FeI signal show indications of variability from one transit to the next.
BAO angular scale atzeff= 0.11 with the SDSS blue galaxies
Authors: de Carvalho E. , Bernui A. , Avila F. , Novaes C. P. , Nogueira-Cavalcante J. P. 
Published: March 2021

Aims.We measure the transverse baryon acoustic oscillations (BAO) signal in the local Universe using a sample of blue galaxies from the Sloan Digital Sky Survey (SDSS) survey as a cosmological tracer.Methods.The method is weakly dependent on a cosmological model and is suitable for 2D analyses in thin redshift bins to investigate the SDSS data in the intervalz ∈ [0.105, 0.115].Results.We detect the transverse BAO signalθBAO= 19.8°±1.05° atzeff = 0.11, with a statistical significance of 2.2σ. Additionally, we perform tests that confirm the robustness of this angular BAO signature. Supported by a large set of log-normal simulations, our error analyses include statistical and systematic contributions. In addition, considering the sound horizon scale calculated by the Planck Collaboration,rsPlanck, and theθBAOvalue obtained here, we obtain a measurement of the angular diameter distanceDA(0.11) =258.31 ± 13.71 h−1Mpc. Moreover, combining thisθBAOmeasurement at low redshift with other BAO angular scale data reported in the literature, we perform statistical analyses for the cosmological parameters of some Lambda cold dark matter type models.
Bouncing and sticking collisions of organic nanoparticles: Atomistic study
Authors: Anders Christian , Urbassek Herbert M. 
Published: March 2021

Context. Whether nanoparticles bounce or stick during collisions determines whether particles grow or fragment, hence shaping collision-induced agglomeration processes. The collision behavior of organic matter may strongly differ from that of silica or ice grains.
Aims. We explore the microscopic processes underlying the bouncing behavior of organic nanoparticles.
Methods. Molecular dynamics simulations based on a reactive potential, which follow molecular motion on an atomistic scale, are used.
Results. For the exemplary case of glycolic acid molecules, warm nanoparticles (250 K) always show sticking, while at low velocities (2.5 m s−1) cold nanoparticles (100 K) exhibit a considerable probability for bouncing. This behavior can be traced back to the distant electrostatic repulsion of the nanoparticles at certain orientations; this prevents a closer approach, during which van der Waals and H-bonded interactions would lead to sticking. At higher temperatures, molecular vibrations and conformational flexibility average over the nanoparticle interaction, such that attraction dominates and bouncing is prevented. Our results are in qualitative agreement with laboratory experiments.
Conclusions. Organic matter distinctly influences the collision behavior of nanoparticles.
Formation of giant planets with large metal masses and metal fractions via giant impacts in a rapidly dissipating disk
Authors: Ogihara Masahiro , Hori Yasunori , Kunitomo Masanobu , Kurosaki Kenji 
Published: March 2021

Context. According to planetary interior models, some giant planets contain large metal masses with large metal-mass fractions. HD 149026b and TOI-849b are characteristic examples of these giant planets. It has been suggested that the envelope mass loss during giant impacts plays a key role in the formation of such giant planets.
Aims. The aim of the present Letter is to propose a mechanism that can explain the origin of such giant planets.
Methods. We investigate the formation of giant planets in a rapidly dissipating disk using N-body simulations that consider pebble accretion.
Results. The results show that although the pebble isolation mass is smaller than the metal mass (≳30 Earth masses) in some giant planets, the interior metal mass can be increased by giant impacts between planets with the isolation mass. Regarding the metal fraction, the cores accrete massive envelopes by runaway gas accretion during the disk-dissipation phase of 1−10 Myr in a disk that evolves without photoevaporation. Although a large fraction of the envelope can be lost during giant impacts, the planets can reaccrete the envelope after impacts in a slowly dissipating disk. Here, we demonstrate that, by photoevaporation in a rapidly dissipating disk, the runaway gas accretion is quenched in the middle, resulting in the formation of giant planets with large metal-mass fractions.
Conclusions. The origins of HD 149026b and TOI-849b, which are characterized by their large metal-mass fractions, can be naturally explained by a model that considers a disk evolving with photoevaporation.
Ubiquitous signs of interactions in early-type galaxies with prolate rotation
Authors: Ebrová Ivana , Bílek Michal , Vudragović Ana , Yıldız Mustafa K. , Duc Pierre-Alain 
Published: March 2021

Context. A small fraction of early-type galaxies (ETGs) show prolate rotation; that is, they rotate around their long photometric axis. In simulations, certain configurations of galaxy mergers are known to produce this type of rotation.
Aims. We investigate the association of prolate rotation and signs of galaxy interactions among the observed galaxies.
Methods. We collected a sample of 19 nearby ETGs with distinct prolate rotation from the literature and inspected their ground-based deep optical images for interaction signs – 18 in archival images and 1 in a new image obtained with the Milanković telescope.
Results. Tidal tails, shells, disturbed asymmetric stellar halos, or ongoing interactions are present in all the 19 prolate rotators. Comparing this with the frequency of tidal disturbance among the general sample of ETGs of a roughly similar mass range and surface-brightness limit, we estimate that the chance probability of such an observation is only 0.00087. We also find a significant overabundance of prolate rotators that are hosting multiple stellar shells. The visible tidal features imply a relatively recent galaxy interaction. That agrees with the Illustris large-scale cosmological hydrodynamical simulation, where prolate rotators are predominantly formed in major mergers during the last 6 Gyr. In the appendix, we present the properties of an additional galaxy, NGC 7052, a prolate rotator for which no deep images are available, but for which an HST image revealed the presence of a prominent shell, which had not been reported before.
Tumornachsorge sinunasaler Papillome – Risikofaktoren für Rezidiv-Entwicklung und maligne Entartung
Authors: Pähler Anja , Welkoborsky Hans-Jürgen 
Published: March 2021

ZusammenfassungHintergrund Sinunasale Papillome sind Tumoren der Nasenhaupt- und Nasennebenhöhlen. Therapie der Wahl ist die vollständige Resektion unter tumorchirurgischen Kautelen. Zwei Eigenschaften machen die Tumornachsorge zu einer Herausforderung: Erstens die häufige Rezidiv-Entwicklung (auch viele Jahre nach Erstdiagnose) und zweitens die Möglichkeit der malignen Entartung. Diese Übersichtsarbeit beleuchtet diesbezügliche Risikofaktoren, um „Hochrisikopatienten“ zu identifizieren, die in der Tumornachsorge besondere Aufmerksamkeit verdienen.Materialen und Methoden Es erfolgte eine ausführliche Literaturrecherche in PubMed (NCBI).Ergebnisse Hauptrisikofaktor für Rezidive ist die unvollständige Tumorresektion. Daraus ergeben sich weitere Faktoren wie unzureichend radikale Operationstechnik, ausgedehnte Tumoren, erschwerte intraoperative Verhältnisse aufgrund der Tumorlokalisation oder bei der Rezidiv-Chirurgie. Zudem neigen junge Patienten und Raucher vermehrt zu Rezidiven. Risikofaktoren für eine maligne Entartung sind große Tumoren, Rauchen, höheres Alter bei Erstdiagnose, weibliches Geschlecht, Knocheninvasion und fehlende inflammatorische Polypen. Histopathologische Risikofaktoren für Rezidive sowie für maligne Entartung sind Dysplasien, Hyperkeratose, plattenepitheliale Hyperplasie und – sofern bestimmt – eine erhöhte Proliferationsrate, Aneuploidie sowie eine Infektion mit humanen Papillomaviren.Schlussfolgerungen Eine vollständige Resektion der sinunasalen Papillome unter tumorchirurgischen Kautelen ist der Goldstandard. Postoperativ ist eine engmaschige Tumornachsorge (analog zu malignen Tumoren) zwingend erforderlich. Die meisten Autoren empfehlen einen Nachsorgezeitraum von mindestens 5 Jahren, manche sogar eine lebenslange Nachsorge. Patienten mit einem oder mehreren Risikofaktoren sollten engmaschiger nachbetreut werden.
Corona-Prämien: Witz oder Wertschätzung?
Authors: Roßius Sabrina 
Published: March 2021

ZusammenfassungCorona-Prämien – wo beginnt Anerkennung und wann mündet sie in Wertschätzung? Die vergangenen Monate mit den unzähligen Herausforderungen der Corona-Pandemie in den Kliniken haben unter anderem zu einem enormen medialen Interesse am Gesundheitssystem geführt.
Gene Therapy for Inherited Retinal Disorders: Update on Clinical Trials
Authors: Michalakis Stylianos , Gerhardt Maximilian , Rudolph Günter , Priglinger Siegfried , Priglinger Claudia 
Published: March 2021

AbstractWithin the last decade, continuous advances in molecular biological techniques have made it possible to develop causative therapies for inherited retinal disorders (IRDs). Some of the most promising options are gene-specific approaches using adeno-associated virus-based vectors to express a healthy copy of the disease-causing gene in affected cells of a patient. This concept of gene supplementation therapy is already advocated for the treatment of retinal dystrophy in RPE65-linked Leberʼs congenital amaurosis (LCA) patients. While the concept of gene supplementation therapy can be applied to treat autosomal recessive and X-linked forms of IRD, it is not sufficient for autosomal dominant IRDs, where the pathogenic gene product needs to be removed. Therefore, for autosomal dominant IRDs, alternative approaches that utilize CRISPR/Cas9 or antisense oligonucleotides to edit or deplete the mutant allele or gene product are needed. In recent years, research retinal gene
therapy has intensified and promising approaches for various forms of IRD are currently in preclinical and clinical development. This review article provides an overview of current clinical trials for the treatment of IRDs.