Miracle-dz/UniFAR-FTUs huggingface dataset:
Laser-driven ion acceleration from relativistically transparent nanotargets

Here we present experimental results on laser-driven ion acceleration from relativistically transparent, overdense plasmas in the break-out afterburner (BOA) regime. Experiments were preformed at the Trident ultra-high contrast laser facility at Los Alamos National Laboratory, and at the Texas Petawatt laser facility, located in the University of Texas at Austin. It is shown that when the target becomes relativistically transparent to the laser, an epoch of dramatic acceleration of ions occurs that lasts until the electron density in the expanding target reduces to the critical density in the non-relativistic limit. For given laser parameters, the optimal target thickness yielding the highest maximum ion energy is one in which this time window for ion acceleration overlaps with the intensity peak of the laser pulse. A simple analytic model of relativistically induced transparency is presented for plasma expansion at the time-evolving sound speed, from which these times may be estimated. The maximum ion energy attainable is controlled by the finite acceleration volume and time over which the BOA acts.
DAMA/LIBRA-phase2 in WIMP effective models

The DAMA/LIBRA collaboration has recently released updated results from their search for the annual modulation signal expected from Dark Matter (DM) scattering in their NaI detectors. We have fitted the updated DAMA result for the modulation amplitudes in terms of a Weakly Interacting Massive Particle (WIMP) signal, parameterizing the interaction with nuclei in terms of the most general effective Lagrangian for a WIMP particle spin up to 1/2, systematically assuming dominance of one of the 14 possible interaction terms, and assuming for the WIMP velocity distribution a standard Maxwellian. We find that most of the couplings of the non-relativistic effective Hamiltonian can provide a better fit compared to the standard Spin Independent interaction case, and with a reduced fine-tuning of the three parameters (WIMP mass, WIMP-nucleon effective cross-section and ratio between the WIMP-neutron and the WIMP-proton couplings). Moreover, effective models for which the cross section depends explicitly on the WIMP incoming velocity can provide a better fit of the DAMA data at large values of mχ compared to the standard velocity-independent cross-section due to a different phase of the modulation amplitudes. All the best fit solutions are in tension with exclusion plots of both XENON1T and PICO60.
Superfilling and the curvature enhanced accelerator coverage mechanism

The Electrochemical Society Interface • Winter 2004 tate-of-the-art manufacturing of semiconductor devices involves the electrodeposition of copper for on-chip wiring of integrated circuits. In the Damascene process, interconnects are fabricated by first patterning trenches and vias in a dielectric medium and then filling by metal electrodeposition over the entire wafer surface. This is followed by a planarization step that leaves an array of wires and interlevel vias embedded in the dielectric matrix. The metallization process, pioneered by IBM, depends on the use of electrolyte additives that affect the local metal deposition rate, thereby resulting in superfilling, or bottom-up void-free filling of trenches and vias.1,2 An example of this remarkable deposition behavior is given in Fig. 1 where growth as a function of electrodeposition time and feature aspect ratio reveals preferential metal deposition at the bottom of the trenches followed by bump formation above the filled trench.3 In the early years of copper Damascene technology an understanding of the superfilling process lagged behind its implementation due to a combination of factors. The first generation of electrolytes contained numerous components and general knowledge of both the chemistry and processing conditions was significantly constrained by proprietary concerns. As a result, early modeling studies focused on traditional leveling theory where the location-dependent growth rate derived from diffusion-limited accumulation and consumption of an inhibiting species on the metal surface.2,4,5 In these studies it was necessary to empirically modify the area-blockage leveling theory to describe feature filling.2,4 Despite these modifications, detailed studies of shape evolution and the observation of bump formation above the filled trenches made it clear that superfilling could not be rationalized by traditional transport-limited leveling Superfilling and the Curvature Enhanced Accelerator Coverage Mechanism
Magnetic anisotropy and valence states in L a 2 C o 1 − x M n 1 + x O 6 ( x ≈ 0.23 ) thin films studied by x-ray absorption spectroscopy techniques

X-ray absorption spectroscopy was used to determine the valence state in La$_2$Co$_{1-x}$Mn$_{1+x}$O$_6$ ($x\approx 0.23$) thin films. We found that in spite of the non-stoichiometry, Co is in a divalent state while Mn ions show a mixed valence state. The relation of this finding with the magnetic properties of the films is discussed. X-ray magnetic circular dichroism measurements prove that magnetic anisotropy originates from Co spin-orbit coupling and it is strain-dependent: a strong increase of the angular contribution to the magnetic moment is found when in-plane (out-of-plane) and cell parameters get expanded (compressed). This behavior is reproduced by first order perturbation theory calculations.
Family and Caregiver Characteristics Contribute to Caregiver Change in Use of Strategies and Growth in Child Spoken Language in a Parent-Implemented Language Intervention in Fragile X Syndrome

Purpose: This study examined relationships among family characteristics, caregiver change in use of strategies, and child growth in spoken language over the course of a parent-implemented language intervention (PILI) that was developed to address some of the challenges associated with the fragile X syndrome (FXS) phenotype. Method: Participants were 43 parent–child dyads from two different PILI studies, both of which taught parents various language facilitation strategies to support child language. Before starting the intervention, parents reported on their mental health, parenting stress, and parenting competence. This study focused on potential barriers to treatment gains by examining correlations between the measures of parent well-being and (a) parent change in use of intervention strategies taught in the PILI and (b) changes in child language outcomes from preto post-intervention. Results: Parents in this study had elevated mental health symptoms across several domains and increased rates of parenting stress. Furthermore, although PILI resulted in treatment gains for both parents and children, a variety of parent mental health symptoms were found to be significantly and negatively associated with change in use of strategies and growth in child language over the course of the intervention. Some inconsistent findings also emerged regarding the relationships between parenting stress and competence and change in parent strategy use and growth in child language. Conclusions: This study provides preliminary evidence that parents who are experiencing significant mental health challenges may have a more difficult time participating fully in PILIs and that there may be subsequent effects on child outcomes. Future PILIs could benefit from addressing parent well-being as a substantial part of the intervention program.
Gaia unveils the kinematics of multiple stellar populations in 47 Tucanae

The series of events, which occurred at high redshift and originated multiple stellar populations in Globular Clusters (GCs) are still poorly understood. Theoretical work suggests that the present-day dynamics of stars in nearby GCs, including the rotation and velocity dispersion, may retain important clues on the formation of multiple populations. So far, the dynamics of multiple populations have been investigated either from radial velocities of a relatively-small sample of stars, or from relative proper motions of stars in the small field of view provided by the Hubble Space Telescope. In this context, Gaia provides the unique opportunity to investigate the dynamics of thousands GC stars over a wide field of view. For the first time, we combine Gaia DR2 proper motions and multi-band photometry to study the internal motions of the two main stellar populations of 47 Tucanae in a wide field of view. We confirm that this cluster exhibits high rotation on the plane of the sky and find that both stellar generations share similar rotation patters. Second-generation stars show stronger anisotropies and smaller tangential-velocity dispersion than the first generation, while there is no significant difference between their radial-velocity dispersion profiles. We discuss the impact of these results in the context of the formation scenarios for multiple stellar populations in GCs.
Self-Supervised Encoders Are Better Transfer Learners in Remote Sensing Applications

Transfer learning has been shown to be an effective method for achieving high-performance models when applying deep learning to remote sensing data. Recent research has demonstrated that representations learned through self-supervision transfer better than representations learned on supervised classification tasks. However, little research has focused explicitly on applying self-supervised encoders to remote sensing tasks. Using three diverse remote sensing datasets, we compared the performance of encoders pre-trained through both supervision and self-supervision on ImageNet, then fine-tuned on a final remote sensing task. Furthermore, we explored whether performance benefited from further pre-training on remote sensing data. Our experiments used SwAV due to its comparably lower computational requirements, as this method would prove most easily replicable by practitioners. We show that an encoder pre-trained on ImageNet using self-supervision transfers better than one pre-trained using supervision on three diverse remote sensing applications. Moreover, self-supervision on the target data alone as a pre-training step seldom boosts performance beyond this transferred encoder. We attribute this inefficacy to the lower diversity and size of remote sensing datasets, compared to ImageNet. In conclusion, we recommend that researchers use self-supervised representations for transfer learning on remote sensing data and that future research should focus on ways to increase performance further using self-supervision.
Superhumps in Cataclysmic Binaries. XXIII. V442 Ophiuchi and RX J1643.7+3402

We report the results of long observing campaigns on two novalike variables: V442 Ophiuchi and RX J1643.7+3402. These stars have high‐excitation spectra, complex line profiles signifying mass loss at particular orbital phases, and similar orbital periods (respectively, 0.12433 and 0.12056 days). They are well‐credentialed members of the SW Sex class of cataclysmic variables. Their light curves are also quite complex. V442 Oph shows periodic signals with periods of 0.12090(8) and 4.37(15) days, and RX J1643.7+3402 shows similar signals at 0.11696(8) and 4.05(12) days. We interpret these short and long periods, respectively, as a “negative superhump” and the wobble period of the accretion disk. The superhump could then possibly arise from the heating of the secondary (and structures fixed in the orbital frame) by inner‐disk radiation, which reaches the secondary relatively unimpeded since the disk is not coplanar. At higher frequencies, both stars show another type of variability: quasi‐periodic oscillations with a period near 1000 s. Underlying these strong signals of low stability may be weak signals of higher stability. Similar quasi‐periodic oscillations, and negative superhumps, are quite common features in SW Sex stars. Both can in principle be explained by ascribing strong magnetism to the white dwarf member of the binary; and we suggest that SW Sex stars are borderline AM Herculis binaries, usually drowned by a high accretion rate. This would provide an ancestor channel for AM Hers, whose origin is still mysterious.
Increased Surgical Experience in Microendoscopic Spinal Surgery Can Reduce Development of Postoperative Spinal Epidural Hematoma and Improve the Clinical Outcomes

No reports have previously evaluated the association between surgical technique and the incidence of postoperative spinal epidural hematoma (PSEH) following microendoscopic decompression surgery (MED). This study aimed to evaluate the association between the development of radiographic PSEH (rPSEH) following MED and microendoscopic surgical experience and postoperative clinical outcomes related to the quality of life (QoL). This retrospective cohort study included 3922 patients who had undergone MED performed by a single surgeon. rPSEH was defined as a hematoma that was identified via routine magnetic resonance images performed 3–4 days postoperatively. Patients were divided into rPSEH and control groups to identify the risk factor of rPSEH and assess clinical outcomes. In the multivariate analysis, age (p = 0.002), surgical experience (p = 0.003), surgical time (p = 0.038), multilevel decompression (p < 0.001), and diagnosis (p = 0.004) were identified as independent variables associated with rPSEH. Moreover, in mixed-effect models, the rPSEH group showed less improvement in Oswestry Disability Index (p = 0.014) than the control group. In conclusion, the surgical experience was identified as a risk factor for rPSEH that could lead to poor QoL. The sharing of microendoscopic surgical techniques among surgeons may reduce rPSEH incidence and improve patients’ QoL.
The clearing of discs around late-type T Tauri stars: constraints from the infrared two-colour plane

We have undertaken spectral energy distribution (SED) modelling of discs around low-mass T Tauri stars in order to delineate regions of the infrared two-colour plane (K - [8] versus K - [24]) that correspond to discs in different evolutionary stages. This provides a tool for classifying the nature of star-disc systems based on infrared photometry. In particular, we demonstrate the distinct loci followed by discs that undergo 'uniform draining' (reduction in surface density by a spatially uniform factor) from those that clear from the inside-out. We draw attention to the absence of objects on this 'draining locus' in those star-forming regions where the 24-μm sensitivity would permit their detection, as compared with the ~20 objects in these regions with colours suggestive of inner holes. We thus conclude that discs predominantly clear from the inside-out. We also apply our classification of the infrared two-colour plane to stars of spectral types M3-M5 in the IC 348 cluster and show that some of its members (dubbed 'weak excess' sources by Muzerolle et al.) that had previously been assumed to be in a state of clearing are instead likely to be optically thick discs in which the dust is well settled towards the mid-plane. Nevertheless, there are many discs in a state of partial clearing in IC 348, with their abundance (relative to the total population of disc bearing stars) being around four times higher than for comparable stars in Taurus. However, the number of partially cleared discs relative to the total number of late-type stars is similarly low in both regions (10 and 20 per cent, respectively). We therefore conclude that IC 348 represents a more evolved version of the Taurus population (with more of its discs being highly settled or partially cleared) but that the time-scale for clearing is similarly short (a few times 10 5 yr) in both cases.
Planar superconductor-normal-superconductor Josephson junctions in MgB2

We report the successful creation of planar MgB2 junctions by localized ion damage in thin (100 nm) films of MgB2 on sapphire by milling a 50 nm trench with a focused-ion beam across tracks of widths between 1 and 5 μm. When the depth of the trench is between 70% and 80% of the film thickness, devices show critical currents (IC) for temperatures below 25 K. The IC of these devices is strongly modulated by applied microwave radiation and magnetic field. The product of the critical current and normal state resistance (ICRN) is remarkably high, implying a potential for very-high-frequency applications.
Evolution of spatially resolved star formation main sequence and surface density profiles in massive disc galaxies at 0 ≲ z ≲ 1: inside–out stellar mass buildup and quenching

We investigate a relation between surface densities (at a $\sim 1$kpc scale) of star formation rate (SFR) and stellar mass ($M_{*}$) namely spatially resolved star formation main sequence (SFMS) at $z\sim 0$ and $z\sim 1$ of massive ($\log(M_{*}/M_{\odot})>10.5$) face-on disc galaxies and examine the evolution of the relation with cosmic time. The spatially resolved SFMS of $z\sim 0$ galaxies is discussed in a companion paper. For $z\sim 1$ sample, we use 8 bands imaging dataset from CANDELS and 3D-HST which provides a rest-frame FUV-NIR SED for galaxies at $0.8\lesssim z \lesssim 1.8$. We perform a pixel-to-pixel SED fitting to derive the spatially resolved SFR and $M_{*}$ distributions in a galaxy. We find a linear spatially resolved SFMS in the $z\sim 1$ galaxies that lie within $\pm 0.3$ dex from the global SFMS, while a "flattening" at high $\Sigma_{*}$ end is found in the spatially resolved SFMS of the galaxies that lie below $-0.3$ dex from the global SFMS. The "flattening" trend is consistent with a decline of the sSFR radial profile (sSFR$(r)$) in the central region of the corresponding galaxies. Comparison with the spatially resolved SFMS in the $z\sim 0$ galaxies shows smaller difference in the sSFR at low $\Sigma_{*}$ ($\sim 0.4$ dex at $\log(\Sigma_{*}[M_{\odot} \text{kpc}^{-2}])=7.0$) than that at high $\Sigma_{*}$ ($\sim 1.5$ dex at $\log(\Sigma_{*}[M_{\odot} \text{kpc}^{-2}])=8.5$). This trend is consistent with the evolution of the sSFR$(r)$ radial profile, which shows a faster decrease in the central region than in the outskirt, agrees with the inside-out quenching scenario. We then derive an empirical model for the evolution of the $\Sigma_{*}(r)$, $\Sigma_{\rm SFR}(r)$ and sSFR$(r)$ radial profiles. Based on the empirical model, we estimate the radial profile of the quenching timescale and reproduce the observed spatially resolved SFMS at $z\sim 1$ and $z\sim 0$.
Determinants and impacts of intangible investment: Evidence from Chinese private manufacturing firms

Determinants of investment in intangibles by firms and the effects of intangible investment on firm productivity have been documented for developed economies. Evidence on these issues in emerging economies, however, is scarce. Using data from China Enterprise Survey 2012 conducted by the World Bank, this study examines the determinants and impacts of intangible investment by private manufacturing firms in China, thus shedding light on recent development of intangibles in one of the largest emerging economies in the world. It is found that more human capital, larger firm size and better institutional quality generally increase the propensity and the amount of intangible investment, and yet fiercer market competition decreases both the propensity and the amount to invest in intangibles. We also provide evidence that the three components of intangibles including research and development (R&D) investment, software investment and organization investment as well as ICT investment are positively correlated with firm productivity. Furthermore there is complementarity between software investment and organization investment. Implications for policies to enhance investment in intangibles are identified from the empirical results.
Looking into the heart of a beast: The black hole binary LS 5039

LS 5039 is a relatively close microquasar consisting of a late O-type star and a compact object (very possibly a black hole) on a highly eccentric orbit with a period of 3.9 days. The high X-ray, gamma-ray and radio luminosity indicate light-matter interaction, which arise from the stellar wind of the primary star accreting toward the black hole. Former examinations suggest that LS 5039 could be a prototype of wind-fed high mass X-ray binaries (WXBs) with diskless main sequence O primaries. Now there is a great chance to better understand the configuration and the physical processes in the exotic system. In July 2009 LS 5039 was followed by the Canadian MOST space telescope to get ultraprecise photometric data in a month-long semi-continuous time series. Parallel to this, we have taken simultaneous high-resolution optical spectra using the 2.3m ANU telescope of the Siding Spring Observatory, supplemented with further data obtained in early August 2009 with the same instrument. Here we present the first results from the new echelle spectra, which represent the best optical spectroscopy ever obtained for this intriguing system. We determined fundamental orbital and physical parameters of LS 5039 and examined the configuration and the circumstellar environment of the system via radial velocity measurements and detailed line-profile analysis of H-Balmer, He I and He II lines.
Suzaku observations of low surface brightness cluster Abell 1631

We present analysis results for a nearby galaxy cluster Abell 1631 at $z~=~0.046$ using the X-ray observatory Suzaku. This cluster is categorized as a low X-ray surface brightness cluster. To study the dynamical state of the cluster, we conduct four-pointed Suzaku observations and investigate physical properties of the Mpc-scale hot gas associated with the A1631 cluster for the first time. Unlike relaxed clusters, the X-ray image shows no strong peak at the center and an irregular morphology. We perform spectral analysis and investigate the radial profiles of the gas temperature, density, and entropy out to approximately 1.5~Mpc in the east, north, west, and south directions by combining with the XMM-Newton data archive. The measured gas density in the central region is relatively low (${\rm a~few} \times~10^{-4}~{\rm cm^{-3}}$) at the given temperature ($\sim2.9~{\rm keV}$) compared with X-ray-selected clusters. The entropy profile and value within the central region ($r<0.1~r_{200}$) are found to be flatter and higher ($\gtrsim400~ {\rm keV~cm}^2$). The observed bolometric luminosity is approximately three times lower than that expected from the luminosity-temperature relation in previous studies for relaxed clusters. These features are also observed in another low surface brightness cluster, Abell 76. The spatial distributions of galaxies and the hot gas appear to be different. The X-ray luminosity is relatively lower than that expected from the velocity dispersion. A post-merger scenario may explain the observed results.
Ultra-High Energy Neutrinos

Ultra-high energy neutrinos hold promise as cosmic messengers to advance the understanding of extreme astrophysical objects and environments as well as possible probes for discovering new physics. This proceeding describes the motivation for measuring high energy neutrinos. A short summary of the mechanisms for producing high energy neutrinos is provided along with an overview of current and proposed modes of detection. The science reach of the field is also briefly surveyed. As an example of the potential of neutrinos as cosmic messengers, the recent results from an IceCube Collaboration real-time high energy neutrino alert and subsequent search of archival data are described.
Direct evidence of acceleration from a distance modulus–redshift graph

The energy conditions give upper bounds on the luminosity distance. We apply these upper bounds to the 192 ESSENCE supernova Ia data to show that the Universe has experienced accelerated expansion. This conclusion is drawn directly from the distance modulus–redshift graph. In addition to being a very simple method, this method is also totally independent of any cosmological model. From the degeneracy of the distance modulus at low redshift, we argue that the choice of w0 for probing the property of dark energy is misleading. One explicit example is used to support this argument.