cometadata/datacite-rtg-text-other-reclassification-records huggingface dataset:
The first interferometric measurements of NH$_2$D/NH$_3$ ratio in hot corinos
Creators: name: Yamato, Yoshihide
name: Furuya, Kenji
name: Aikawa, Yuri
name: Persson, Magnus V.
name: Tobin, John J.
name: Jørgensen, Jes K.
name: Kama, Mihkel
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: The nitrogen chemical evolution during star and planet formation is still not fully understood. Ammonia (NH$_3$) is a key specie in the understanding of the molecular evolution in star-forming clouds and nitrogen isotope fractionation. In this paper, we present high spatial resolution observations of multiple emission lines of NH$_3$ toward the protobinary system NGC1333 IRAS4A with Karl G. Jansky Very Large Array (VLA). We spatially resolved the binary (hereafter 4A1 and 4A2) and detected compact emission of NH$_3$ transitions with high excitation energies ($\gtrsim$100 K) from the vicinity of the protostars, indicating the NH$_3$ ice has sublimated at the inner hot region. The NH$_3$ column density is estimated to be $\sim 10^{17}-10^{18}$ cm$^{-2}$. We also detected two NH$_2$D transitions, allowing us to constrain the deuterium fractionation of ammonia. The NH$_2$D/NH$_3$ ratios are as high as $\sim 0.3-1$ in both 4A1 and 4A2. From the comparisons with the astrochemical models in the literature, the high NH$_2$D/NH$_3$ ratios suggest that the formation of NH$_3$ ices mainly started in the prestellar phase after the formation of bulk water ice finished, and that the primary nitrogen reservoir in the star-forming cloud could be atomic nitrogen (or N atoms) rather than nitrogen-bearing species such as N$_2$ and NH$_3$. The implications on the physical properties of IRAS4A cores are discussed as well.
description: 20 pages, 7 figures, accepted for publication in ApJ
Conditional Hybrid Nonclassicality
Creators: name: Agudelo, E.
name: Sperling, J.
name: Costanzo, L. S.
name: Bellini, M.
name: Zavatta, A.
name: Vogel, W.
Publisher: name: arXiv
Year: 2017
Subjects: subject: Quantum Physics (quant-ph)
subject: FOS: Physical sciences

description: We derive and implement a general method to characterize the nonclassicality in compound discrete- and continuous-variable systems. For this purpose, we introduce the operational notion of conditional hybrid nonclassicality which relates to the ability to produce a nonclassical continuous-variable state by projecting onto a general superposition of discrete-variable subsystem. We discuss the importance of this form of quantumness in connection with interfaces for quantum communication. To verify the conditional hybrid nonclassicality, a matrix version of a nonclassicality quasiprobability is derived and its sampling approach is formulated. We experimentally generate an entangled, hybrid Schrödinger cat state, using a coherent photon-addition process acting on two temporal modes, and we directly sample its nonclassicality quasiprobability matrix. The introduced conditional quantum effects are certified with high statistical significance.
description: Closer to published version
N-body simulations of planet formation via pebble accretion I: First Results
Creators: name: Matsumura, Soko
name: Brasser, Ramon
name: Ida, Shigeru
Publisher: name: arXiv
Year: 2017
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: FOS: Physical sciences

description: Context. Planet formation with pebbles has been proposed to solve a couple of long-standing issues in the classical formation model. Some sophisticated simulations have been done to confirm the efficiency of pebble accretion. However, there has not been any global N-body simulations that compare the outcomes of planet formation via pebble accretion with observed extrasolar planetary systems. Aims. In this paper, we study the effects of a range of initial parameters of planet formation via pebble accretion, and present the first results of our simulations. Methods. We incorporate the pebble accretion model by Ida et al. (2016) in the N-body code SyMBA (Duncan et al. 1998), along with the effects of gas accretion, eccentricity and inclination damping and planet migration in the disc. Results. We confirm that pebble accretion leads to a variety of planetary systems, but have difficulty in reproducing observed properties of exoplanetary systems, such as planetary mass, semimajor axis, and eccentricity distributions. The main reason behind this is a too-efficient type I migration, which sensitively depends on the disc model. However, our simulations also lead to a few interesting predictions. First, we find that formation efficiencies of planets depend on the stellar metallicities, not only for giant planets, but also for Earths (Es) and Super-Earths (SEs). The dependency for Es/SEs is subtle. Although higher metallicity environments lead to faster formation of a larger number of Es/SEs, they also tend to be lost later via dynamical instability. Second, our results indicate that a wide range of bulk densities observed for Es and SEs is a natural consequence of dynamical evolution of planetary systems. Third, the ejection trend of our simulations suggest that one free-floating E/SE may be expected for two smaller-mass planets.
description: Accepted for publication in A&A, 21 pages, 15 figures
The first gradual solar energetic particle event with enhanced 3He abundance on Solar Orbiter
Creators: name: Bučík, R.
name: Mason, G. M.
name: Gómez-Herrero, R.
name: Krupar, V.
name: Lario, D.
name: Starkey, M. J.
name: Ho, G. C.
name: Rodríguez-Pacheco, J.
name: Wimmer-Schweingruber, R. F.
name: Lara, F. Espinosa
name: Tadesse, T.
name: Balmaceda, L.
name: Cohen, C. M. S.
name: Dayeh, M. A.
name: Desai, M. I.
name: Kühl, P.
name: Nitta, N. V.
name: Wiedenbeck, M. E.
name: Xu, Z. G.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: Space Physics (physics.space-ph)
subject: FOS: Physical sciences

description: The origin of 3He abundance enhancements in coronal mass ejection (CME)-driven shock gradual solar energetic particle (SEP) events remains largely unexplained. Two mechanisms have been suggested - the re-acceleration of remnant flare material in interplanetary space and concomitant activity in the corona. We explore the first gradual SEP event with enhanced 3He abundance observed by Solar Orbiter. The event started on 2020 November 24 and was associated with a relatively fast halo CME. During the event, the spacecraft was at 0.9 au from the Sun. The event averaged 3He/4He abundance ratio is 24 times higher than the coronal or solar wind value, and the 3He intensity had timing similar to other species. We inspected available imaging, radio observations, and spacecraft magnetic connection to the CME source. It appears the most probable cause of the enhanced 3He abundance are residual 3He ions remaining from a preceding long period of 3He-rich SEPs on 2020 November 17-23.
description: 9 pages, 9 figures, accepted for publication in A&A
ODNet: A Convolutional Neural Network for Asteroid Occultation Detection
Creators: name: Cazeneuve, Dorian
name: Marchis, Franck
name: Blaclard, Guillaume
name: Dalba, Paul A.
name: Martin, Victor
name: Asencioa, Joé
Publisher: name: arXiv
Year: 2022
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: Instrumentation and Methods for Astrophysics (astro-ph.IM)
subject: Machine Learning (cs.LG)
subject: FOS: Physical sciences
subject: FOS: Computer and information sciences

description: We propose to design and build an algorithm that will use a Convolutional Neural Network (CNN) and observations from the Unistellar network to reliably detect asteroid occultations. The Unistellar Network, made of more than 10,000 digital telescopes owned by citizen scientists, and is regularly used to record asteroid occultations. In order to process the increasing amount of observational produced by this network, we need a quick and reliable way to analyze occultations. In an effort to solve this problem, we trained a CNN with artificial images of stars with twenty different types of photometric signals. Inputs to the network consists of two stacks of snippet images of stars, one around the star that is supposed to be occulted and a reference star used for comparison. We need the reference star to distinguish between a true occultation and artefacts introduced by poor atmospheric condition. Our Occultation Detection Neural Network (ODNet), can analyze three sequence of stars per second with 91\% of precision and 87\% of recall. The algorithm is sufficiently fast and robust so we can envision incorporating onboard the eVscopes to deliver real-time results. We conclude that citizen science represents an important opportunity for the future studies and discoveries in the occultations, and that application of artificial intelligence will permit us to to take better advantage of the ever-growing quantity of data to categorize asteroids.
description: 17 pages, 10 figures, 3 tables, accepted for publication in Astrophysical Journal
iPTF16fnl: a faint and fast tidal disruption event in an E+A galaxy
Creators: name: Blagorodnova, N.
name: Gezari, S.
name: Hung, T.
name: Kulkarni, S. R.
name: Cenko, S. B.
name: Pasham, D. R.
name: Yan, L.
name: Arcavi, I.
name: Ben-Ami, S.
name: Bue, B. D.
name: Cantwell, T.
name: Cao, Y.
name: Castro-Tirado, A. J.
name: Fender, R.
name: Fremling, C.
name: Gal-Yam, A.
name: Ho, A. Y. Q.
name: Horesh, A.
name: Hosseinzadeh, G.
name: Kasliwal, M. M.
name: Kong, A. K. H.
name: Laher, R. R.
name: Leloudas, G.
name: Lunnan, R.
name: Masci, F. J.
name: Mooley, K.
name: Neill, J. D.
name: Nugent, P.
name: Powell, M.
name: Valeev, A. F.
name: Vreeswijk, P. M.
name: Walters, R.
name: Wozniak, P.
Publisher: name: arXiv
Year: 2017
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: We present ground-based and \textit{Swift} observations of iPTF16fnl, a likely tidal disruption event (TDE) discovered by the intermediate Palomar Transient Factory (iPTF) survey at 66.6 Mpc. The lightcurve of the object peaked at absolute $M_g=-17.2$ mag. The maximum bolometric luminosity (from optical and UV) was $L_p~\simeq~(1.0\,\pm\,0.15) \times 10^{43}$ erg/s, an order of magnitude fainter than any other optical TDE discovered so far. The luminosity in the first 60 days is consistent with an exponential decay, with $L \propto e^{-(t-t_0)/τ}$, where $t_0$=~57631.0 (MJD) and $τ\simeq 15$ days. The X-ray shows a marginal detection at $L_X=2.4^{1.9}_{-1.1}\times 10^{39}$ erg/s (\textit{Swift} X-ray Telescope). No radio counterpart was detected down to 3$σ$, providing upper limits for monochromatic radio luminosity of $νL_ν < 2.3\times10^{36}$ erg/s and $νL_ν<1.7\times 10^{37}$ erg/s (VLA, 6.1 and 22 GHz). The blackbody temperature, obtained from combined \textit{Swift} UV and optical photometry, shows a constant value of 19,000 K. The transient spectrum at peak is characterized by broad He II and H$α$ emission lines, with an FWHM of about 14,000 km/s and 10,000 km/s respectively. He I lines are also detected at $λλ$ 5875 and 6678. The spectrum of the host is dominated by strong Balmer absorption lines, which are consistent with a post-starburst (E+A) galaxy with an age of $\sim$650 Myr and solar metallicity. The characteristics of iPTF16fnl make it an outlier on both luminosity and decay timescales, as compared to other optically selected TDEs. The discovery of such a faint optical event suggests a higher rate of tidal disruptions, as low luminosity events may have gone unnoticed in previous searches.
description: 14 pages, 11 figures, accepted for publication in ApJ
Extragalactic Peaked-Spectrum Radio Sources at Low-Frequencies are Young Radio Galaxies
Creators: name: Slob, M. M.
name: Callingham, J. R.
name: Röttgering, H. J. A.
name: Williams, W. L.
name: Duncan, K. J.
name: de Gasperin, F.
name: Hardcastle, M. J.
name: Miley, G. K.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We present a sample of 373 peaked-spectrum (PS) sources with spectral peaks around 150MHz, selected using a subset of two LOFAR all-sky surveys, the LOFAR Two Meter Sky Survey and the LOFAR LBA Sky Survey. These surveys are the most sensitive low-frequency widefield surveys to date, allowing us to select low-luminosity PS sources. Our sample increases the number of known PS sources in our survey area by a factor 50. The 5GHz luminosity distribution of our PS sample shows we sample the lowest luminosity PS sources to-date by nearly an order of magnitude. Since high-frequency PS sources and compact steep-spectrum sources are hypothesised to be the precursors to large radio galaxies, we investigate whether this is also the case for our sample of low-frequency PS sources. Using optical line emission criteria, we find that our PS sources are predominately high-excitation radio galaxies instead of low-excitation radio galaxies, corresponding to a quickly evolving population. We compute the radio source counts of our PS sample, and find they are scaled down by a factor of $\sim$40 compared to a general sample of radio-loud active galactic nuclei (AGN). This implies that the lifetimes of PS sources are 40 times shorter than large scale radio galaxies, if their luminosity functions are identical. To investigate this, we compute the first radio luminosity function for a homogeneously-selected PS sample. We find that for 144MHz luminosities $\gtrsim 10^{25}$W Hz$^{-1}$, the PS luminosity function has the same shape as an unresolved radio-loud AGN population but shifted down by a factor of $\sim$10. We interpret this as strong evidence that these high-luminosity PS sources evolve into large-scale radio-loud AGN. For local, low-luminosity PS sources, there is a surplus of PS sources, which we hypothesise to be the addition of frustrated PS sources that do not evolve into large-scale AGN.
description: 21 pages, accepted in Astronomy & Astrophysics
Strongly screening on electron capture for Nuclides $^{52, 53, 59, 60}$Fe by the Shell-Model Monte Carlo method in pre-supernova
Creators: name: Liu, Jing-Jing
name: Peng, Qiu-He
name: Liu, Dong-Mei
Publisher: name: arXiv
Year: 2017
Subjects: subject: Nuclear Theory (nucl-th)
subject: Strongly Correlated Electrons (cond-mat.str-el)
subject: FOS: Physical sciences

description: The death of the massive stars due to supernova explosion is a key ingredient in stellar evolution, stellar population synthesis. The electron capture (EC) plays a vital role in supernovae explosions. According to the Shell-Model Monte Carlo (SMMC) method, basing onthe Random Phase Approximation (RPA) and Linear Response Theory Model (LRTM), we study the strongly screening EC rates of nuclides $^{52, 53, 59, 60}$Fe in presupernova. The results show that the screening rates can decrease about 18.66\%. We compare our results with those of Fuller et al. (FFN), Aufderheide et al. (AUFD), and Nabi et al. (NKK)in the case with and without strong electron screening(SES). For the case without SES, our calculations are in very good agreement with those of AUFD in relatively high density surroundings and the maximum error is within 0.35\% at $ρ_7=100$ (e. g., even-even nuclei $^{60}$Fe). However, for odd-A nuclei$^{59}$Fe, our rates are close to one, one, two order magnitude smaller than those of FFN, AUFD, and NKK. For the case with SES, our screening results are about three, two orders magnitude, and 7.27\% lower than those of FFN, AUFD, NKK for $^{60}$Fe, respectively, and it is lower about two, two orders magnitude, and 12.42\% than those of FFN, AUFD, NKK for odd-A nuclide $^{59}$Fe.
description: 12 pages, 9 figures. arXiv:1312.7502,accepted for publication in chinese physics C
Electron density variations in the interstellar medium and the average frequency profile of a scintle from pulsar scintillation spectra
Creators: name: Bartel, N.
name: Burgin, M. S.
name: Fadeev, E. N.
name: Popov, M. V.
name: Ronaghikhameneh, N.
name: Smirnova, T. V.
name: Soglasnov, V. A.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We observed the scintillation pattern of nine bright pulsars at 324 MHz and three at 1.68 GHz and analyzed the wavenumber spectrum which is related to electron density variations of the plasma turbulence of the interstellar medium. For all pulsars the frequency section of the autocorrelation function of the dynamic spectra to at least 45\% of the maximum corresponds to predictions of scattering theories with a range of power-law exponents of the wavenumber spectrum of $3.56 \leq α\leq 3.97$ with errors $\leq 0.05$ and a mean with standard deviation of $3.76\pm0.13$. The range includes $α=3.67$ for the Kolmogorov spectrum. Similar results although with larger errors were found from the Fourier transform of the autocorrelation functions down to $\sim 10^{-3}$ of the maximum. No clear case of a distinction between thin-screen and extended-medium scattering models was found. The average frequency profile of the scintles can be characterized for steep wavenumber spectra with $α\lesssim4$ by a cusp with a somewhat rounded peak. For flatter spectra, down to at least $α\sim 3.56$ the cusp with its peak becomes more pronounced and its decay steepens. We discuss our findings in the context of scattering characteristics of the interstellar medium.
description: 16 pages, 8 figures, accepted by The Astrophysical Journal. Changes in this revision: change of the paper title on the HTML page, correction of misprints
Pulsar revival in neutron star mergers: multi-messenger prospects for the discovery of pre-merger coherent radio emission
Creators: name: Cooper, A. J.
name: Gupta, O.
name: Wadiasingh, Z.
name: Wijers, R. A. M. J.
name: Boersma, O. M.
name: Andreoni, I.
name: Rowlinson, A.
name: Gourdji, K.
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: We investigate pre-merger coherent radio emission from neutron star mergers arising due to the magnetospheric interaction between compact objects. We consider two plausible radiation mechanisms, and show that if one neutron star has a surface magnetic field $B_{\rm s} \ge 10^{12}$G, coherent millisecond radio bursts with characteristic temporal morphology and inclination angle dependence are observable to Gpc distances with next-generation radio facilities. We explore multi-messenger and multi-wavelength methods of identification of a NS merger origin of radio bursts, such as in fast radio burst surveys, triggered observations of gamma-ray bursts and gravitational wave events, and optical/radio follow-up of fast radio bursts in search of kilonova and radio afterglow emission. We present our findings for current and future observing facilities, and make recommendations for verifying or constraining the model.
description: Re-upload to match journal accepted version. Clarifying corrections included to subsection 3.2
Configurational entropy measurements in extremely supercooled liquids that break the glass ceiling
Creators: name: Berthier, Ludovic
name: Charbonneau, Patrick
name: Coslovich, Daniele
name: Ninarello, Andrea
name: Ozawa, Misaki
name: Yaida, Sho
Publisher: name: arXiv
Year: 2017
Subjects: subject: Statistical Mechanics (cond-mat.stat-mech)
subject: Soft Condensed Matter (cond-mat.soft)
subject: FOS: Physical sciences

description: Liquids relax extremely slowly upon approaching the glass state. One explanation is that an entropy crisis, due to the rarefaction of available states, makes it increasingly arduous to reach equilibrium in that regime. Validating this scenario is challenging, because experiments offer limited resolution, while numerical studies lag more than eight orders of magnitude behind experimentally-relevant timescales. In this work we not only close the colossal gap between experiments and simulations but manage to create in-silico configurations that have no experimental analog yet. Deploying a range of computational tools, we obtain four estimates of their configurational entropy. These measurements consistently confirm that the steep entropy decrease observed in experiments is also found in simulations, even beyond the experimental glass transition. Our numerical results thus extend the new observational window into the physics of glasses and reinforce the relevance of an entropy crisis for understanding their formation.
description: 4+23 pages, 3+12 figures; v2: final version, with various changes made. Data relevant to this work can be accessed at http://dx.doi.org/10.7924/G8ZG6Q9T
Radio observations of four active galactic nuclei hosting intermediate-mass black hole candidates: studying the outflow activity and evolution
Creators: name: Yang, Xiaolong
name: Mohan, Prashanth
name: Yang, Jun
name: Ho, Luis C.
name: Aditya, J. N. H. S.
name: Zhang, Shaohua
name: Jaiswal, Sumit
name: Yang, Xiaofeng
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: Observational searches for intermediate-mass black holes (IMBHs; $10^2 - 10^6$ $M_\odot$) include relatively isolated dwarf galaxies. For those that host active galactic nuclei (AGNs), the IMBH nature may be discerned through the accretion - jet activity. We present radio observations of four AGN-hosting dwarf galaxies (which potentially harbor IMBHs). Very large array (VLA) observations indicate steep spectra (indices of $-$0.63 to $-$1.05) between 1.4 and 9 GHz. A comparison with the 9 GHz in-band spectral index however shows a steepening for GH047 and GH158 (implying older/relic emission) and flattening for GH106 and GH163 (implying recent activity). Overlapping emission regions in the VLA 1.4 GHz and our very long baseline array (VLBA) 1.5 GHz observations, and possibly symmetric pc-scale extensions are consistent with recent activity in the latter two. Using the compact VLBA radio luminosity, X-ray luminosity (probing the accretion activity) and the black hole masses, all AGNs are found to lie on the empirical fundamental plane relation. The four AGN are radio quiet with relatively higher Eddington ratios ($0.04 - 0.32$) and resemble the X-ray binaries during spectral state transitions that entail an outflow ejection. Furthermore, the radio to X-ray luminosity ratio $\log{R_\mathrm{X}}$ of $-3.9$ to $-5.6$ in these four sources support the scenarios including corona mass ejection from accretion disk and wind activity. The growth to kpc-scales likely proceeds along a trajectory similar to young AGNs and peaked spectrum sources. The above complex clues can thus aid in the detection and monitoring of IMBHs in the nearby Universe.
description: 21 pages, 3 figures, 5 tabels, accepted for publication in ApJ
Körperliche Erkrankungen bei psychischen Störungen: Aktuelle Befunde und Bedarfe
Creators: name: Jacobi, Frank
name: Volkmann, Hannah
Publisher: name: figshare
Year: 2022
Subjects: subject: 170106 Health, Clinical and Counselling Psychology
subject: FOS: Psychology

description: Das Wechselspiel psychischer und körperlicher Faktoren im menschlichen Krankheitsgeschehen betrifft viele Facetten und Perspektiven. Zum einen können psychische Störungen körperliche Ursachen, Begleiterscheinungen und Folgen haben. Die »andere Seite der Medaille« betrifft körperliche Erkrankungen, bei denen bei Entstehung und Verlauf sowie bei der Krankheitsbewältigung psychologische Faktoren eine wichtige Rolle spielen. Der vorliegende Beitrag berichtet nach einer Übersicht zu psychischen und körperlichen Faktoren im menschlichen Krankheitsgeschehen aktuelle Befunde zu komorbiden somatischen Erkrankungen und erhöhter Mortalität bei Menschen mit psychischen Störungen.
A Cartesian Encoding Graph Neural Network for Crystal Structures Property Prediction: Application to Thermal Ellipsoid Estimation
Creators: name: Solé, Àlex
name: Mosella-Montoro, Albert
name: Cardona, Joan
name: Gómez-Coca, Silvia
name: Aravena, Daniel
name: Ruiz, Eliseo
name: Ruiz-Hidalgo, Javier
Publisher: name: arXiv
Year: 2025
Subjects: subject: Machine Learning (cs.LG)
subject: FOS: Computer and information sciences

description: In diffraction-based crystal structure analysis, thermal ellipsoids, quantified via Anisotropic Displacement Parameters (ADPs), are critical yet challenging to determine. ADPs capture atomic vibrations, reflecting thermal and structural properties, but traditional computation is often expensive. This paper introduces CartNet, a novel graph neural network (GNN) for efficiently predicting crystal properties by encoding atomic geometry into Cartesian coordinates alongside the crystal temperature. CartNet integrates a neighbour equalization technique to emphasize covalent and contact interactions, and a Cholesky-based head to ensure valid ADP predictions. We also propose a rotational SO(3) data augmentation strategy during training to handle unseen orientations. An ADP dataset with over 200,000 experimental crystal structures from the Cambridge Structural Database (CSD) was curated to validate the approach. CartNet significantly reduces computational costs and outperforms existing methods in ADP prediction by 10.87%, while delivering a 34.77% improvement over theoretical approaches. We further evaluated CartNet on other datasets covering formation energy, band gap, total energy, energy above the convex hull, bulk moduli, and shear moduli, achieving 7.71% better results on the Jarvis Dataset and 13.16% on the Materials Project Dataset. These gains establish CartNet as a state-of-the-art solution for diverse crystal property predictions. Project website and online demo: https://www.ee.ub.edu/cartnet
The gradient flow running coupling in SU(2) gauge theory with $N_f=8$ fundamental flavors
Creators: name: Leino, Viljami
name: Rantaharju, Jarno
name: Rantalaiho, Teemu
name: Rummukainen, Kari
name: Suorsa, Joni M.
name: Tuominen, Kimmo
Publisher: name: arXiv
Year: 2017
Subjects: subject: High Energy Physics - Lattice (hep-lat)
subject: High Energy Physics - Phenomenology (hep-ph)
subject: FOS: Physical sciences

description: We study the evolution of the coupling in SU(2) gauge field theory with $N_f=8$ fundamental fermion flavors on the lattice. This model is expected to have an infrared fixed point at high coupling. We use HEX-smeared Wilson-clover action, and measure the gradient flow running coupling with Dirichlet boundary conditions. Extrapolating our results to continuum, we find an infrared fixed point at $g^2=8.24(59)^{+0.97}_{-1.64}$, with statistical and systematic error estimates. We also measure the anomalous dimension of the quark mass operator, and find its value at the fixed point $γ\approx 0.15 \pm 0.02$.
description: 24 pages, 11 figures, updated to match the published version
title: Improving Small-Volume Antibiotic Administration for Surgical Prophylaxis
Creators: name: Thomas, Benjamin
Publisher: name: Digital Commons@Becker, Barnes Jewish College Goldfarb School of Nursing
Year: 2023
Subjects: classificationCode: 3.3
subject: FOS: Health sciences

description: Background: Small-volume IV antibiotics are commonly administered for surgical prophylaxis, but no clear policy on administration method exists, leading to wide variation in anesthesia provider practice at a large academic medical center. Administration via a secondary tubing set is the recommended practice to minimize significant medication losses which could lead to poor patient outcomes. This large academic medical center performed below the national benchmark for one of these outcomes–surgical site infections.
Goals and Objectives: Objectives of this project included eliminating a potential systematic shortcoming in the administration of prophylactic antibiotics. The goal was to increase the use of secondary tubing techniques for small-volume antibiotics in order to reduce medication losses and waste in administration sets. The expected outcome of this project was 100% provider adoption of the use of secondary tubing for all small-volume antibiotic administration.
Design and Methods: The pre-intervention phase involved observation of provider practices and measurements of medication waste and was followed by an educational intervention for nurse anesthetists on the new policy and best practices for administration of small-volume antibiotics. Following the education, three PDSA cycles were run to evaluate changes in practice and reductions in medication waste over a six-week period. Mean volumes were evaluated using two sample t-tests.
Results: The most common pre-intervention tubing method used was primary tubing (52%), and the most common post-intervention tubing method was secondary tubing (93%). Mean dead volume for these methods were13.45mL and 0.79mL (p<0.01) respectively. Statisitcally significant (p < 0.01) decreases in dead volumes and percentage of medication lost were observed from all pre-intervention methods to post-intervention.
Conclusions: System and person changes were made to foster consistent practice and to potentially prevent poor patient outcomes in the operating rooms at the project site. Providers benefited from the educational intervention by strengthening their clinical practices, and the proposed project intervention required minimal upfront cost with tremendous upside both for cost-reduction and patient well-being.
GraviDy, a GPU modular, parallel direct-summation $N-$body integrator: Dynamics with softening
Creators: name: Maureira-Fredes, Cristián
name: Amaro-Seoane, Pau
Publisher: name: arXiv
Year: 2017
Subjects: subject: Instrumentation and Methods for Astrophysics (astro-ph.IM)
subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: A wide variety of outstanding problems in astrophysics involve the motion of a large number of particles ($N\gtrsim 10^{6}$) under the force of gravity. These include the global evolution of globular clusters, tidal disruptions of stars by a massive black hole, the formation of protoplanets and the detection of sources of gravitational radiation. The direct-summation of $N$ gravitational forces is a complex problem with no analytical solution and can only be tackled with approximations and numerical methods. To this end, the Hermite scheme is a widely used integration method. With different numerical techniques and special-purpose hardware, it can be used to speed up the calculations. But these methods tend to be computationally slow and cumbersome to work with. Here we present a new GPU, direct-summation $N-$body integrator written from scratch and based on this scheme. This code has high modularity, allowing users to readily introduce new physics, it exploits available high-performance computing resources and will be maintained by public, regular updates. The code can be used in parallel on multiple CPUs and GPUs, with a considerable speed-up benefit. The single GPU version runs about 200 times faster compared to the single CPU version. A test run using 4 GPUs in parallel shows a speed up factor of about 3 as compared to the single GPU version. The conception and design of this first release is aimed at users with access to traditional parallel CPU clusters or computational nodes with one or a few GPU cards.
description: minor modifications, version of the code includes now post-Newtonian corrections
Neutral Atmospheric Density Measurement Using Insight-HXMT Data by Earth Occultation Technique
Creators: name: Xue, Wang-Chen
name: Li, Xiao-Bo
name: Xiong, Shao-Lin
name: Chen, Yong
name: Zhang, Shuang-Nan
name: Song, Li-Ming
name: Zhang, Shu
name: Ge, Ming-Yu
name: Tuo, You-Li
name: Li, Hai-Tao
name: Yu, Dao-Chun
name: Guo, Dong-Ya
name: Liu, Jia-Cong
name: Zhang, Yan-Qiu
name: Zheng, Chao
Publisher: name: arXiv
Year: 2022
Subjects: subject: Instrumentation and Methods for Astrophysics (astro-ph.IM)
subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: The Earth occultation technique has broad applications in both astronomy and atmospheric density measurements. We construct the background model during the occultation of the Crab Nebula observed by the Insight-Hard X-ray Modulation Telescope (Insight-HXMT) at energies between 6 keV and 100 keV. We propose a Bayesian atmospheric density retrieval method based on the Earth occultation technique, combining Poisson and Gaussian statistics. By modeling the atmospheric attenuation of X-ray photons during the occultation, we simultaneously retrieved the neutral densities of the atmosphere at different altitude ranges. Our method considers the correlation of densities between neighboring atmospheric layers and reduces the potential systematic bias to which previous work may be subject. Previous analyses based on light curve fitting or spectral fitting also lost some spectral or temporal information of the data. In contrast to previous work, the occultation data observed by the three telescopes onboard Insight-HXMT is fully used in our analysis, further reducing the statistical error in density retrieval. We apply our method to cross-check the (semi-)empirical atmospheric models, using 115 sets of occultation data of the Crab Nebula observed by Insight-HXMT. We find that the retrieved neutral density is ~10%, ~20%, and ~25% less than the values of the widely used atmospheric model NRLMSISE-00, in the altitude range of 55--80 km, 80--90 km, and 90--100 km, respectively. We also show that the newly released atmospheric model NRLMSIS 2.0 is generally consistent with our density measurements.
description: 20 pages, 12 figures, accepted for publication in ApJS
Enhanced power factor and reduced Lorenz number in the Wiedemann--Franz law due to pudding mold type band structures
Creators: name: Usui, Hidetomo
name: Kuroki, Kazuhiko
Publisher: name: arXiv
Year: 2016
Subjects: subject: Materials Science (cond-mat.mtrl-sci)
subject: FOS: Physical sciences

description: We study the relationship between the shape of the electronic band structure and the thermoelectric properties. In order to study the band shape dependence of the thermoelectric properties generally, we first adopt models with band structures having the dispersion $E({\bf k}) \sim |{\bf k}|^n$ with $n = 2, 4$ and 6. We consider one, two- and three dimensional systems, and calculate the thermoelectric properties using the Boltzmann equation approach within the constant quasi-particle lifetime approximation. $n = 2$ corresponds to the usual parabolic band structure, while the band shape for $n = 4, 6$ has a flat portion at the band edge, so that the density of states diverges at the bottom of the band. We call this kind of band structure the "pudding mold type band". $n \ge 4$ belong to the pudding mold type band, but since the density of states diverges even for $n= 2$ in one dimensional system, this is also categorized as the pudding mold type. Due to the large density of states and the rapid change of the group velocity around the band edge, the spectral conductivity of the pudding mold type band structures becomes larger than that of the usual parabolic band structures. It is found that the pudding mold type band has a coexistence of large Seebeck coefficient and large electric conductivity, and small Lorenz number in the Wiedemann--Franz law due to the specific band shape. We also find that the low dimensionality of the band structure can contribute to large electronic conductivity and hence a small Lorenz number. We conclude that the pudding mold type band, especially in low dimensional systems, can enhance not only the power factor but also the dimensionless figure of merit due to stronger violation of the Wiedemann--Franz law.
description: 13 pages, 9 figures
Fundamental Vortices, Wall-Crossing, and Particle-Vortex Duality
Creators: name: Hwang, Chiung
name: Yi, Piljin
name: Yoshida, Yutaka
Publisher: name: arXiv
Year: 2017
Subjects: subject: High Energy Physics - Theory (hep-th)
subject: FOS: Physical sciences

description: We explore 1d vortex dynamics of 3d supersymmetric Yang-Mills theories, as inferred from factorization of exact partition functions. Under Seiberg-like dualities, the 3d partition function must remain invariant, yet it is not a priori clear what should happen to the vortex dynamics. We observe that the 1d quivers for the vortices remain the same, and the net effect of the 3d duality map manifests as 1d Wall-Crossing phenomenon; Although the vortex number can shift along such duality maps, the ranks of the 1d quiver theory are unaffected, leading to a notion of fundamental vortices as basic building blocks for topological sectors. For Aharony-type duality, in particular, where one must supply extra chiral fields to couple with monopole operators on the dual side, 1d wall-crossings of an infinite number of vortex quiver theories are neatly and collectively encoded by 3d determinant of such extra chiral fields. As such, 1d wall-crossing of the vortex theory encodes the particle-vortex duality embedded in the 3d Seiberg-like duality. For $\mathcal N = 4$, the D-brane picture is used to motivate this 3d/1d connection, while, for $\mathcal N = 2$, this 3d/1d connection is used to fine-tune otherwise ambiguous vortex dynamics. We also prove some identities of 3d supersymmetric partition functions for the Aharony duality using this vortex wall-crossing interpretation.
description: 75 pages, 24 figures; v2: a reference added, published version
Fast Multipole Method for Gravitational Lensing. Application to High Magnification Quasar Microlensing
Creators: name: Vicente, J. Jiménez
name: Mediavilla, E.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences

description: We introduce the use of the Fast Multipole Method (FMM) to speed up gravitational lensing ray tracing calculations. The method allows very fast calculation of ray deflections when a large number of deflectors, $N_*$, is involved, while keeping rigorous control on the errors. In particular, we apply this method, in combination with the Inverse Polygon Mapping technique (IPM), to quasar microlensing to generate microlensing magnification maps with very high workloads (high magnification, large size and/or high resolution) that require a very large number of deflectors. Using, FMM-IPM, the computation time can be reduced by a factor $\sim 10^5$ with respect to standard Inverse Ray Shooting, making the use of this algorithm on a personal computer comparable to the use of standard IRS on GPUs. We also provide a flexible web interface for easy calculation of microlensing magnification maps using FMM-IPM\footnote{http://gloton.ugr.es/microlensing/}. We exemplify the power of this new method by applying it to some challenging interesting astrophysical scenarios, including clustered primordial black holes, or extremely magnified stars close to the giant arcs of galaxy clusters. We also show the performance/use of FMM to calculate ray deflection for a halo resulting from cosmological simulations composed by a large number ($N\gtrsim 10^7$) of elements.
description: 17 pages, 10 figures. Accepted for publication in The Astrophysical Journal. Accompanying web for microlensing map calculation at https://gloton.ugr.es/microlensing/
title: Tetravalent lead in nature
Creators: name: Folkers, Laura Christina
name: Pöttgen, Rainer
Publisher: name: Deutsche Geologische Gesellschaft - Geologische Vereinigung e.V. (DGGV)
Year: 2022

description:
Of the three industrially important lead oxides PbO, Pb3O4 and PbO2 [1-4] the first two are readily accessible through chemical synthesis, whereas PbO2 can only be reached through high pressure, electrochemical or strongly oxidizing synthesis routes [5-7].

In nature lead dioxide forms oxidatively during hydrothermal mineralization [8]. The respective β modification, named plattnerite is a rare mineral and has hitherto only been characterized by powder X-ray or neutron diffraction.

The samples studied originate from Mine du Pradet in Cap Garonne, France and from Mount Trevasco in Bergamo, Italy. Single crystal X-ray diffraction measurements show that β-PbO2 crystallizes in the rutile-type structure with space group P42/mnm without additional reflections or a sign for a structural transformation between room temperature and 90 K [9].

[1] G. Hantke, Gmelins Handbuch der anorganischen Chemie, 8. Auflage, Verlag Chemie, Weinheim, 1969.

[2] K. Rumpf, Gmelins Handbuch der anorganischen Chemie, 8. Auflage, Verlag Chemie, Weinheim, 1973.

[3] H. E. Brown, Lead oxide – Properties and Applications, International Lead Zinc Organization, New York, 1985.

[4] D. L. Perry, Lead Oxides: Synthesis and Applications, in Transparent Electronics, (Eds.: A. Facchetti, T. J. Marks) John Wiley & Sons, West Sussex, 2010.

[5] G. L. Clark, et al., J. Am. Chem. Soc., 1937, 59, 2305.

[6] W. B. White, R. Roy, J. Am. Ceram. Soc., 1964, 47, 242.

[7] E. Torikai, Y. Kawami, US Patent 3,959,453, 1976.

[8] J. E. Taggart Jr., et al., Can. Mineral., 1988, 26, 905.

[9] C. Paulsen, et al., Z. Naturforsch., 2019, 74, 427.
Continuous variable steering and incompatibility via state-channel duality
Creators: name: Kiukas, Jukka
name: Budroni, Costantino
name: Uola, Roope
name: Pellonpää, Juha-Pekka
Publisher: name: arXiv
Year: 2017
Subjects: subject: Quantum Physics (quant-ph)
subject: FOS: Physical sciences

description: The term Einstein-Podolsky-Rosen steering refers to a quantum correlation intermediate between entanglement and Bell nonlocality, which has been connected to another fundamental quantum property: measurement incompatibility. In the finite-dimensional case, efficient computational methods to quantify steerability have been developed. In the infinite-dimensional case, however, less theoretical tools are available. Here, we approach the problem of steerability in the continuous variable case via a notion of state-channel correspondence, which generalizes the well-known Choi-Jamiołkowski correspondence. Via our approach we are able to generalize the connection between steering and incompatibility to the continuous variable case and to connect the steerability of a state with the incompatibility breaking property of a quantum channel, e.g., noisy NOON states and amplitude damping channels. Moreover, we apply our methods to the Gaussian steering setting, proving, among other things, that canonical quadratures are sufficient for steering Gaussian states.
description: 13 pages, 2 figures
ALMA Observations for CO Emission from Luminous Lyman-break Galaxies at $z=6.0293$-$6.2037$
Creators: name: Ono, Yoshiaki
name: Fujimoto, Seiji
name: Harikane, Yuichi
name: Ouchi, Masami
name: Vallini, Livia
name: Ferrara, Andrea
name: Shibuya, Takatoshi
name: Pallottini, Andrea
name: Inoue, Akio K.
name: Imanishi, Masatoshi
name: Shimasaku, Kazuhiro
name: Hashimoto, Takuya
name: Lee, Chien-Hsiu
name: Sugahara, Yuma
name: Tamura, Yoichi
name: Kohno, Kotaro
name: Schramm, Malte
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We present our new Atacama Large Millimeter/submillimeter Array (ALMA) observations targeting CO(6-5) emission from three luminous Lyman break galaxies (LBGs) at $z_{\rm spec} = 6.0293$-$6.2037$ found in the Subaru/Hyper Suprime-Cam survey, whose [OIII]$88μ$m and [CII]$158μ$m emission have been detected with ALMA. We find a marginal detection of the CO(6-5) line from one of our LBGs, J0235-0532, at the $\simeq 4 σ$ significance level and obtain upper limits for the other two LBGs, J1211-0118 and J0217-0208. Our $z=6$ luminous LBGs are consistent with the previously found correlation between the CO luminosity and the infrared luminosity. The unique ensemble of the multiple far-infrared emission lines and underlying continuum fed to a photodissociation region model reveal that J0235-0532 has a relatively high hydrogen nucleus density that is comparable to those of low-$z$ (U)LIRGs, quasars, and Galactic star-forming regions with high $n_{\rm H}$ values, while the other two LBGs have lower $n_{\rm H}$ consistent with local star-forming galaxies. By carefully taking account of various uncertainties, we obtain total gas mass and gas surface density constraints from their CO luminosity measurements. We find that J0235-0532 locates below the Kennicutt-Schmidt (KS) relation, comparable to the previously CO(2-1) detected $z=5.7$ LBG, HZ10. Combined with previous results for dusty starbursts at similar redshifts, the KS relation at $z=5$-$6$ is on average consistent with the local one.
description: 33 pages, 12 figures, accepted for publication in ApJ
R-axion at colliders
Creators: name: Bellazzini, Brando
name: Mariotti, Alberto
name: Redigolo, Diego
name: Sala, Filippo
name: Serra, Javi
Publisher: name: arXiv
Year: 2017
Subjects: subject: High Energy Physics - Phenomenology (hep-ph)
subject: High Energy Physics - Experiment (hep-ex)
subject: High Energy Physics - Theory (hep-th)
subject: FOS: Physical sciences

description: We study the effective theory of a generic class of hidden sectors where supersymmetry is broken together with an approximate R-symmetry at low energy. The light spectrum contains the gravitino and the pseudo-Nambu-Goldstone boson of the R-symmetry, the R-axion. We derive new model-independent constraints on the R-axion decay constant for R-axion masses ranging from GeV to TeV, which are of relevance for hadron colliders, lepton colliders and B-factories. The current bounds allow for the exciting possibility that the first sign of SUSY will be the R-axion. We point out its most distinctive signals, providing a new experimental handle on the properties of the hidden sector and a solid motivation for searches of axion-like particles.
description: 7 pages, 2 figures. v2: typos fixed, appendix added. v3: R-axion as motivation for ALP phenomenological studies made explicit, minor clarifications. Accepted for publication on PRL
Three-dimensional Simulations of Magnetospheric Accretion in a T Tauri Star: Accretion and Wind Structures Just Around Star
Creators: name: Takasao, Shinsuke
name: Tomida, Kengo
name: Iwasaki, Kazunari
name: Suzuki, Takeru K.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: We perform three-dimensional magnetohydrodynamic simulations of magnetospheric accretion in a T Tauri star to study the accretion and wind structures in the close vicinity of the star. The gas accreting onto the star consists of the gas from the magnetospheric boundary and the failed disk winds. The accreting gas is commonly found as a multi-column accretion, which is consistent with observations. A significant fraction of the angular momentum of the accreting flows is removed by the magnetic fields of conical disk winds and turbulent failed winds inside and near the magnetosphere. As a result, the accretion torque is significantly reduced compared to the simple estimation based on the mass accretion rate. The stellar spin affects the time variability of the conical disk wind by changing the stability condition of the magnetospheric boundary. However, the time-averaged magnetospheric radius only weakly depends on the stellar spin, which is unlike the prediction of classical theories that the stellar spin controls the magnetospheric radius through the magnetic torque. The ratio of the toroidal to the poloidal field strengths at the magnetospheric boundary, which is a key parameter for the magnetic torque, is also insensitive to the spin; it is rather determined by the disk dynamics. Considering newly found three-dimensional effects, we obtain a scaling relation of the magnetospheric radius very similar to the Ghosh & Lamb relation from the steady angular momentum transport equation.
description: 38 pages, 21 figures. Accepted for publication in ApJ