bluuebunny/crossref_metadata_2025_split huggingface dataset:
Development of a DDP-Based Trajectory Generation Method Considering the Manipulability Measure for 6-DOF Collaborative Robots
Authors: Lee Jaesoon , Cho Baek-Kyu 
Published: December 2024

Abstract
This paper presents a trajectory generation method for 6-DOF collaborative robots using the Differential Dynamic Programming algorithm, integrating the Manipulability Measure to effectively avoid singularities. Traditional trajectory generation methods often neglect the robot’s dynamics, leading to non-optimized trajectories and potential singularity issues. Our approach integrates Manipulability Measure into the Differential Dynamic Programming algorithm, ensuring consideration of the robot’s dynamics while effectively avoiding singularities. The proposed algorithm is applied to the 6-Degrees of freedom collaborative robot RB1-500e and validated on the actual robot. The results demonstrate that the proposed method significantly improves trajectory generation and singularity avoidance compared to traditional methods. This study offers a robust solution that enhances both efficiency and safety in dynamic trajectory planning for collaborative robots.
Early progressive disease within 2 years in isocitrate dehydrogenase (IDH)–mutant astrocytoma may indicate radiation necrosis
Authors: Ozeki Yukie , Honda-Kitahara Mai , Yanagisawa Shunsuke , Takahashi Masamichi , Ohno Makoto , Miyakita Yasuji , Kikuchi Miu , Nakano Tomoyuki , Hosoya Tomohiro , Sugino Hirokazu , Satomi Kaishi , Yoshida Akihiko , Igaki Hiroshi , Kubo Yuko , Ichimura Koichi , Suzuki Hiromichi , Masutomi Kenkichi , Kondo Akihide , Narita Yoshitaka 
Published: December 2024

Abstract

Background
Isocitrate dehydrogenase–mutant astrocytoma without cyclin-dependent kinase inhibitor 2A/B (CDKN2A/B) homozygous deletion typically follows a slow clinical course. However, some cases show early progression on magnetic resonance imaging, and these characteristics remain under-reported. This study aimed to elucidate the characteristics of isocitrate dehydrogenase–mutant astrocytoma showing early progression on magnetic resonance imaging.

Methods
This retrospective study included 52 cases of primary astrocytoma, isocitrate dehydrogenase–mutant, Central Nervous System (CNS) 5 World Health Organization grade 2–3 according to the World Health Organization 2021 classification. Patients underwent surgery followed by radiation therapy and/or chemotherapy at our institution from 2006 to 2019. Progression-free survival and overall survival were analyzed.

Results
There were 24 and 28 grade 2 and grade 3 astrocytomas, respectively. The median patient age was 38 years. Forty-three patients underwent radiotherapy. Progression was diagnosed by magnetic resonance imaging in 22 patients with initial radiotherapy. Thirteen of the 22 patients underwent surgery, and seven of the 13 patients received surgery within 24 months of the initial radiotherapy. Histopathologically, radiation necrosis was confirmed in four of these seven patients (57.1%). The true progression-free survival rate, excluding radiation necrosis, at 2 years after surgery was 91.3% for grade 2 astrocytoma and 88.5% for grade 3 astrocytoma. The 5-year overall survival rate was 85.7% for grade 2 tumours and 76.4% for grade 3 tumours.

Conclusions
Radiation necrosis should be considered in cases showing early progression of isocitrate dehydrogenase–mutant astrocytoma, and a second surgery should be performed to confirm true recurrence or radiation necrosis. Astrocytomas with telomerase reverse-transcriptase promoter mutations may relapse relatively early and should be followed up with caution.
Influence of a nearby hemisphere on the immersed on-wall collision dynamics of a sphere
Authors: Wu H , Yang F-L 
Published: December 2024

ABSTRACT
Systematic experiments were conducted to elucidate how the dynamics of a fully immersed spherical pendulum in a normal approach to a wall may change with the presence of a third object–a hemisphere added to the wall at different vertical distances from the collision point. The studied collision regime ranges from non-bouncing to bouncing by changing the pendulum’s size, density, release angle, and liquid viscosity. In the non-bouncing regime, we analyzed the approach motion and found that the hemisphere decelerates the pendulum approach when it enters the area within one diameter of the pendulum sphere. The deceleration is stronger with decreasing particle Reynolds number. In the cases with rebounds, we measured the wet coefficient of restitution and correlated it to the impact Stokes number. A critical Stokes number was identified to signal the rebound transition, whose value is slightly augmented by the adjacent hemisphere when this third boundary is within one diameter. Most importantly, the previously reported relation between the wet coefficient of restitution and Stokes number remains feasible as long as the decelerated impact velocity of the pendulum is taken into account.
Capsaicin: pharmacological applications and prospects for drug designing
Authors: Gupta Anshita , Joshi Renjil , Dewangan Lokkanya , Shah Kamal , Soni Deependra , Patil Umesh K , Chauhan Nagendra Singh 
Published: December 2024

Abstract

Objectives
A primary objective of this review is to summarize the evidence-based pharmacological applications of capsaicin, particularly its use to manage pain and treat various health conditions. A second goal of the review is to research how recent technological advances are improving the bioavailability and therapeutic index of capsaicin, as well as the development of novel capsaicin-mimetics that are able to enhance therapeutic responses in various human diseases.

Methods
In the review, numerous human clinical trials and preclinical studies are examined to determine how effective, safe, and optimal dosages of capsaicin can be used in pain management and therapeutic applications. Furthermore, it discusses capsaicin’s mechanisms of action, specifically its interactions with the transient receptor potential vanilloid 1 (TRPV1) channel. As a result of this review, the potential of nanotechnology systems for bypassing the limits of capsaicin’s pungency is discussed. The review takes into account individual factors such as pain tolerance and skin sensitivity.

Key findings
For topical applications, capsaicin is typically used in concentrations ranging from 0.025% to 0.1%, with higher concentrations being used under medical supervision for neuropathic pain. The formulation can come in the form of creams, gels, or patches, which provide sustained release over the course of time. A condition such as arthritis or neuropathy can be relieved with capsaicin as it depletes substance P from nerves. Neuropathy and osteoarthritis as well as musculoskeletal disorders have been treated successfully with this herbal medicine. A major mechanism through which capsaicin relieves pain is through activating TRPV1 channels, which induce calcium influx and neurotransmitter release. Additionally, it affects the transcription of genes related to pain modulation and inflammation, particularly when disease conditions or stress are present. There have been recent developments in technology to reduce capsaicin’s pungency and improve its bioavailability, including nanotechnology.

Conclusions
It is proven that capsaicin is effective in pain management as well as a variety of therapeutic conditions because of its ability to deplete substance P and desensitize nerve endings. Although capsaicin is highly pungent and associated with discomfort, advancements in delivery technologies and the development of capsaicin-mimetics promise improved therapeutic outcomes. There is a great deal of complexity in the pharmacological action of capsaicin due to its interaction with TRPV1 channels and its ability to affect gene transcription. There is a need for further research and development in order to optimize capsaicin’s clinical applications and to enhance its therapeutic index in a variety of human diseases.
Perineal hernia repair with a combined abdominoperineal approach with biologic mesh placement and peritoneal flap reconstruction
Authors: Massé Gabrielle , Al Khaldi M , Schwenter F , Coeugniet E , Sebajang H 
Published: December 2024

Abstract
Perineal hernias occur rarely following abdominoperineal resections. No standardized surgical approach exists for treating PH. We herein present the case of a large, symptomatic PH that was repaired with a combined abdominal and perineal approach, with peritoneal flap reconstruction of the pelvic floor and placement of a biological mesh. The patient has not recurred after 3 years of follow-up. In conclusion, despite the lack of a standardized approach for tackling perineal hernias, a combined one with peritoneal flap reconstruction can be successfully used.
Collisional excitation of c-MgC2 by Helium
Authors: M’hamdi M , Bop C T , Lique F , Ben Houria A , Hammami K 
Published: December 2024

ABSTRACT
The cyclic form of magnesium dicarbide molecule (c-MgC$_2$) has been detected in the carbon-rich circumstellar envelope of IRC+10216 and is considered as a valuable tracer for characterizing the physical conditions of the surrounding gas. In order to make the most of c-MgC$_2$ observations and accurately derive the physical conditions of the media where c-MgC$_2$ is detected, radiative transfer modelling, including collisional and radiative (de-)excitations, have to be performed. Here, we study the excitation of c-MgC$_{2}$ induced by collisions with He (as a proxy for H$_2$). A new 3D potential energy surface (PES) is constructed using highly correlated ab initio methods. This PES reveals a minimum with a well depth of 20.66 cm$^{-1}$ below the c-MgC$_2$-He dissociation limit. Using this PES, we compute excitation cross sections for transitions between the low-lying rotational energy levels of c-MgC$_2$ using the time-independent quantum mechanical close-coupling formalism. These cross sections are then thermally averaged over a Boltzmann energy distribution in order to derive excitation rate coefficients at low temperatures ($T \le 30$ K). To evaluate the impact of these new rate coefficients on the interpretation of c-MgC$_2$ observational spectra, we perform radiative transfer calculations. We find that a very high gas density ($n \gt 10^6$ cm$^{-3}$) is needed in order for the collisional excitation to compete with the radiative de-excitation. We also find that the excitation temperatures of the observed lines predicted by our model differ by a factor two from the value derived from the observations in IRC+10216 circumstellar envelope, indicating that the excitation of c-MgC$_{2}$ may also be driven by a strong radiative pumping in such media. Therefore, a more sophisticated non-LTE modelling, that takes into account the collisional and radiative excitations as well as the radiative pumping, is required to accurately interpret the observational spectra of c-MgC$_2$.
Precision of meteor trajectory and orbital measurements by the MIOS
Authors: Li Yi , Li Guozhu , Hu Lianhuan , Zhao Xiukuan , Sun Wenjie , Xie Haiyong , Dai Guofeng , Liu Jianfei , Ning Baiqi 
Published: December 2024

ABSTRACT
Measurement errors of meteors can substantially affect the accuracy of meteoroid trajectory and orbit determinations, potentially leading to spurious meteoroid orbits. Here, we evaluate the measurement errors associated with the meteor and ionospheric irregularity observation system (MIOS) developed at low-latitude Ledong and Sanya, China, aimed at observing various meteors and their associated plasma density irregularity phenomena, and investigate how these errors affect the determination of meteor trajectories and orbits. The measurement error of meteor position is estimated to be $\sim$2 pixels, corresponding to 0.04$^\circ$, which is sufficient to detect true radiant dispersion and structural characteristics in younger meteor showers. By simulating meteoroids from the Draconid, Geminid, and Perseid meteor showers with the $\sim$2 pixels measurement error and the Monte Carlo trajectory method, the precision of corresponding meteoroid trajectories is derived. The radiant accuracy is 1.09$^\circ$, with right ascension and declination accuracies of 0.78$^\circ$ and 0.77$^\circ$, respectively. The velocity accuracy is 0.64 km/s. The comparison of estimated and true radiant uncertainties shows that the estimated errors of the MIOS are generally consistent with the true meteor trajectory errors. Finally, we estimate the orbital measurement errors, which include an eccentricity of 0.05, a perihelion distance of 0.0086 au, an inclination of 1.4$^\circ$, and an argument of the perihelion of 1.86$^\circ$. Based on observations of eight representative meteor showers during 2019–2023, the accuracy of the MIOS in detecting meteor trajectories and orbits is further validated.
DUVET: sub-kiloparsec resolved star formation driven outflows in a sample of local starbursting disc galaxies
Authors: Reichardt Chu Bronwyn , Fisher Deanne B , Chisholm John , Berg Danielle , Bolatto Alberto , Cameron Alex J , Fielding Drummond B , Herrera-Camus Rodrigo , Kacprzak Glenn G , Li Miao , McLeod Anna F , McPherson Daniel K , Nielsen Nikole M , Rickards Vaught Ryan J , Ridolfo Sophia G , Sandstrom Karin 
Published: December 2024

ABSTRACT
We measure resolved (kiloparsec-scale) outflow properties in a sample of 10 starburst galaxies from the Deep near-UV observations of Entrained gas in Turbulent (DUVET) galaxies sample, using Keck/KCWI observations of H $\beta$ and [O iii] $\lambda$5007. We measure $\sim 460$ lines of sight that contain outflows, and use these to study scaling relationships of outflow velocity ($v_{\rm out}$), mass-loading factor ($\eta$; mass outflow rate per star formation rate) and mass flux ($\dot{\Sigma }_{\rm out}$; mass outflow rate per area) with co-located star formation rate surface density ($\Sigma _{\rm SFR}$) and stellar mass surface density ($\Sigma _{\ast }$). We find strong, positive correlations of $\dot{\Sigma }_{\rm out} \propto \Sigma _{\rm SFR}^{1.2}$ and $\dot{\Sigma }_{\rm out} \propto \Sigma _{\ast }^{1.5}$. We also find shallow correlations between $v_{\rm out}$ and both $\Sigma _{\rm SFR}$ and $\Sigma _{\ast }$. Our resolved observations do not suggest a threshold in outflows with $\Sigma _{\rm SFR}$, but rather we find that the local specific star formation rate ($\Sigma _{\rm SFR}/\Sigma _\ast$) is a better predictor of where outflows are detected. We find that outflows are very common above $\Sigma _{\rm SFR}/\Sigma _\ast \gtrsim 0.1$ Gyr$^{-1}$ and rare below this value. We argue that our results are consistent with a picture in which outflows are driven by supernovae, and require more significant injected energy in higher mass surface density environments to overcome local gravity. The correlations we present here provide a statistically robust, direct comparison for simulations and higher redshift results from JWST.
Deep imaging of three accelerating stars using SHARK-NIR and LMIRCam at LBT
Authors: Mesa D , Gratton R , D’Orazi V , Carolo E , Vassallo D , Farinato J , Marafatto L , Wagner K , Hom J , Ertel S , Henning Th , Desgrange C , Barbato D , Bergomi M , Cerpelloni P , Desidera S , Filippo S Di , Doelman D , Machado T S Gomes , Greggio D , Grenz P , Kenworthy M , Laudisio F , Lazzoni C , Leisenring J , Lorenzetto A , Santhakumari K K R , Ricci D , Snik F , Umbriaco G , Pallauta M C Vega , Viotto V 
Published: December 2024

ABSTRACT
The combination of detection techniques enhances our ability to identify companions orbiting nearby stars. We employed high-contrast imaging to constrain mass and separation of possible companions responsible for the significant proper motion anomalies of the nearby stars HIP 11696, HIP 47110, and HIP 36277. These targets were observed using the LBT’s high-contrast camera, SHARK-NIR, in H band using a Gaussian coronagraph, and with the LMIRCam instrument in the L’ band and using a vAPP coronagraph. Both observations were conducted simultaneously. Additionally, constraints at short separations from the host star are derived analysing the renormalized unit weight error values from the Gaia catalogue. We find that the companion responsible for the anomaly signal of HIP 11696 is likely positioned at a distance from 2.5 to 28 astronomical units from its host. Its mass is estimated to be between 4 and 16 Jupiter masses, with the greater mass possible only at the upper end of the separation range. Similar limits were obtained for HIP 47110 where the companion should reside between 3 and 30 au with a mass between 3 and 10 MJup. For HIP 36277, we identified a faint stellar companion at large separation, though it might be substellar depending on the assumed age for the star. Considering the older age, this object accounts for the absolute value of the PMa vector but not for its direction. Additionally, we found a substellar candidate companion at a closer separation that could explain the PMa signal, considering a younger age for the system.
Reconciling S8: insights from interacting dark sectors
Authors: Shah Rahul , Mukherjee Purba , Pal Supratik 
Published: December 2024

ABSTRACT
We do a careful investigation of the prospects of dark energy (DE) interacting with cold dark matter in alleviating the $S_8$ clustering tension. To this end, we consider various well-known parametrizations of the DE equation of state (EoS) and consider perturbations in both the dark sectors, along with an interaction term. Moreover, we perform a separate study for the phantom and non-phantom regimes. Using cosmic microwave background (CMB), baryon acoustic oscillations, and Type Ia supernovae data sets, constraints on the model parameters for each case have been obtained and a generic reduction in the $H_0 \!\!-\!\! \sigma _{8,0}$ correlation has been observed, both for constant and dynamical DE EoS. This reduction, coupled with a significant negative correlation between the interaction term and $\sigma _{8,0}$, contributes to easing the clustering tension by lowering $\sigma _{8,0}$ to somewhere in between the early CMB and late-time clustering measurements for the phantom regime, for almost all the models under consideration. Additionally, this is achieved without exacerbating the Hubble tension. In this regard, the interacting Chevallier–Polarski–Linder and Jassal–Bagla–Padmanabhan models perform the best in relaxing the $S_8$ tension to $&lt;\!\! 1\sigma$. However, for the non-phantom regime the $\sigma _{8,0}$ tension tends to have worsened, which reassures the merits of phantom DE from latest data. We further investigate the role of redshift space distortion data sets and find an overall reduction in tension, with a $\sigma _{8,0}$ value relatively closer to the CMB value. We finally check whether further extensions of this scenario, such as the inclusion of the sound speed of DE and warm dark matter interacting with DE, can have some effects.
Neutrino-driven core-collapse supernova yields in Galactic chemical evolution
Authors: Jost Finia P , Molero Marta , Navó Gerard , Arcones Almudena , Obergaulinger Martin , Matteucci Francesca 
Published: December 2024

ABSTRACT
We provide yields from 189 neutrino-driven core-collapse supernova (CCSN) simulations covering zero-age main sequence masses between 11 and $75\ \mathrm{M}_\odot$ and three different metallicities. Our CCSN simulations have two main advantages compared to previous methods used for applications in Galactic chemical evolution (GCE). First, the mass cut between remnant and ejecta evolves naturally. Secondly, the neutrino luminosities and thus the electron fraction are not modified. Both are key to obtain an accurate nucleosynthesis. We follow the composition with an in situ nuclear reaction network including the 16 most abundant isotopes and use the yields as input in a GCE model of the Milky Way. We adopt a GCE that takes into account infall of gas as well as nucleosynthesis from a large variety of stellar sources. The GCE model is calibrated to reproduce the main features of the solar vicinity. For the CCSN models, we use different calibrations and propagate the uncertainty. We find a big impact of the CCSN yields on our GCE predictions. We compare the abundance ratios of C, O, Ne, Mg, Si, S, Ar, Ca, Ti, and Cr with respect to Fe to an observational data set as homogeneous as possible. From this, we conclude that at least half of the massive stars have to explode to match the observed abundance ratios. If the explosions are too energetic, the high amount of iron will suppress the abundance ratios. With this, we demonstrate how GCE models can be used to constrain the evolution and death of massive stars.
The reliability of gas-phase metallicities immediately adjacent to non-star-forming spaxels in MaNGA
Authors: Scudder Jillian M , Khelil Aidan , Ordower Jonah Z 
Published: December 2024

ABSTRACT
In this work, we use gas phase metallicities calculated from the Sloan Digital Sky Survey (SDSS) Mapping Nearby Galaxies at Apache Point (MaNGA) Data Release 17 (DR17) to assess the extent of potential biases in spaxels which are spatially adjacent to spaxels identified as non-star forming (non-SF) on a BPT diagram. We identify a sample of $\sim 21\,000$ such spaxels with calculable metallicities from the full metallicity catalogue ($\sim$1.57 million), representing a small fraction ($\sim 1.3$ per cent) of the full metallicity sample. $\sim$23 per cent of all galaxies with at least one spaxel with a calculable metallicity also contain at least one spaxel with a calculated metallicity adjacent to a non-SF spaxel, with a typical galaxy hosting 9 non-SF-adjacent spaxels. From our suite of 6 different metallicity calibrations, we find that only the metallicity calibrations based entirely on the [N ii]$_{6584}$/H $\alpha$ ratio are affected, showing systematic offsets to higher metallicities by up to $\sim$0.04 dex if they are located adjacent to a non-SF flagged spaxel, relative to a radially matched control sample. The inclusion of additional diagnostic diagrams (based on [O i]$_{6300}$ and/or [S ii]$_{6717+6731}$) is insufficient to remove the observed offset in the [N ii]$_{6584}$/H $\alpha$ based calibrations. Using a stricter diagnostic line on the BPT diagram removes $\sim$94 per cent of identified bordering spaxels with metallicities for all metallicity calibrations, and removes the residual offset to higher metallicity values seen in [N ii]$_{6584}$/H $\alpha$ calibrations. If science cases demand an exceptionally clean metallicity sample, we recommend either a stricter BPT cut, and/or a non-[N ii]$_{6584}$/H $\alpha$ based metallicity calibration.
Properties of the lower segment of M31’s North West stream
Authors: Preston Janet , Erkal Denis , Collins Michelle L M , Ibata Rodrigo , Rich R Michael 
Published: December 2024

ABSTRACT
We present a kinematic and spectroscopic analysis of 40 red giant branch stars, in 9 fields, exquisitely delineating the lower segment of the North West stream (NW-K2), which extends for $\sim$80 kpc from the centre of the Andromeda galaxy. We measure the stream’s systemic velocity as −439.3$^{+4.1}_{-3.8}$ km s$^{-1}$ with a velocity dispersion =16.4$^{+5.6}_{-3.8}$ km s$^{-1}$ that is in keeping with its progenitor being a dwarf galaxy. We find no detectable velocity gradient along the stream. We determine $-1.3\pm0.1$$\le$$\langle[\mathrm{ Fe/H}]_{\rm spec}\rangle$$\le$$-1.2\pm0.8$ but find no metallicity gradient along the stream. We are able to plausibly associate NW-K2 with the globular clusters PAndAS-04, PAndAS-09, PAndAS-10, PAndAS-11, and PAndAS-12 but not with PAndAS-13 or PAndAS-15, which we find to be superimposed on the stream but not kinematically associated with it.