Miracle-dz/UniFAR-FTUs huggingface dataset:
Constraints on the Minor Merging and Star Formation History of the Wolf-Rayet Galaxy NGC 5430 Through Observations

We used multi-wavelength analysis of the newly observed molecular gas (12CO and 13CO (1-0)) with interferometer CARMA and archival star formation tracers to constrain the interaction, merging, and star formation history of an off-center minor merger, a three-spiral barred galaxy NGC 5430 and its satellite embedded in the bar. Morphology of the molecular gas in the bar of NGC 5430 shows minimal signs of recent interactions in our resolution. The apparent morphological remnant of the past galaxy interaction is an asymmetric spiral arm, containing more molecular gas and exhibiting higher star formation rate (SFR) surface density than the two primary arms. Rotation curve analysis suggests that NGC 5430 and its satellite collided several Gyr ago. History of star formation was constrained by using SFRs that trace different timescales (infrared, radio continuum, and H-alpha). The collision occurred 5 - 10 Myr ago, triggering a transient off-center starburst of Wolf-Rayet stars at the eastern bar end. In the past, the global SFR during the Wolf-Rayet starburst peaked at 35 Msun/yr. At present, the merger-driven starburst is rapidly decaying and the current global SFR has decreased to the Galactic value. The SFR will continue to decay as suggested by the present amount of dense gas (traced by HCN (1-0)). Nonetheless, the global SFR is still dominated by the Wolf-Rayet region rather than the circumnuclear region. Compared with other barred galaxies, the circumnuclear region exhibits particularly low dense gas fraction, low star formation activity and high concentration of gas. Physical properties of the molecular gas are inferred by using the large velocity gradient (LVG) calculations. The initial mass ratio of the NGC 5430 and its satellite are suggested to be in the intermediate ratio range of 7:1-20:1.
Spectral-Correlation Based Spectrum Sensing Under Large Delay Spread Channels

Correlation based detectors are very popular for spectrum sensing. In these detectors, temporal correlation is often employed to discriminate the signals of primary users from noises. However, large channel delay spread can significantly decrease the correlation of neighbouring samples of received signals, inducing severe performance degradation of temporal correlation based detectors. In this work, we show that the power spectral densities of different delayed versions of a primary signal have high correlation, despite unknown delays. Then, by exploiting the correlation of power spectral densities of received signals, we propose a spectral-correlation detector. To facilitate the practical application of the proposed detector, we also derive a theoretical expression for its decision threshold to achieve a given false alarm probability. Furthermore, in order to handle the case of channels with unknown delay profile, we employ the OR rule to combine the temporal- and spectral-correlation detectors, leading to a temporal-spectral-correlation detector. An expression for its decision threshold is also derived. Extensive numerical simulations are provided to verify the theoretical analysis and demonstrate the superior performance of the two proposed detectors compared to state-of-the-art temporal correlation based detectors.
A SEARCH FOR STARS OF VERY LOW METAL ABUNDANCE. VI. DETAILED ABUNDANCES OF 313 METAL-POOR STARS

We present radial velocities, equivalent widths, model atmosphere parameters, and abundances or upper limits for 53 species of 48 elements derived from high resolution optical spectroscopy of 313 metal-poor stars. A majority of these stars were selected from the metal-poor candidates of the HK Survey of Beers, Preston, and Shectman. We derive detailed abundances for 61% of these stars for the first time. Spectra were obtained during a 10 yr observing campaign using the Magellan Inamori Kyocera Echelle spectrograph on the Magellan Telescopes at Las Campanas Observatory, the Robert G. Tull Coudé Spectrograph on the Harlan J. Smith Telescope at McDonald Observatory, and the High Resolution Spectrograph on the Hobby–Eberly Telescope at McDonald Observatory. We perform a standard LTE abundance analysis using MARCS model atmospheres, and we apply line-by-line statistical corrections to minimize systematic abundance differences arising when different sets of lines are available for analysis. We identify several abundance correlations with effective temperature. A comparison with previous abundance analyses reveals significant differences in stellar parameters, which we investigate in detail. Our metallicities are, on average, lower by ≈0.25 dex for red giants and ≈0.04 dex for subgiants. Our sample contains 19 stars with [Fe/H] ⩽−3.5, 84 stars with [Fe/H] ⩽−3.0, and 210 stars with [Fe/H] ⩽−2.5. Detailed abundances are presented here or elsewhere for 91% of the 209 stars with [Fe/H] ⩽−2.5 as estimated from medium resolution spectroscopy by Beers, Preston, and Shectman. We will discuss the interpretation of these abundances in subsequent papers.
Running coupling effects in the evolution of jet quenching

We study the consequences of including the running of the QCD coupling in the equation describing the evolution of the jet quenching parameter $\stackrel{^}{q}$ in the double logarithmic approximation. To start with, we revisit the case of a fixed coupling, for which we obtain exact solutions valid for generic values of the transverse momentum (above the medium saturation scale) and corresponding to various initial conditions. In the case of a running coupling, we construct approximate solutions in the form of truncated series obtained via successive iterations, whose convergence is well under control. We thus deduce the dominant asymptotic behavior of the renormalized $\stackrel{^}{q}$ in the limit of a large ``evolution time'' $Y\ensuremath{\equiv}\mathrm{ln}(L/\ensuremath{\lambda})$, with $L$ the size of the medium and $\ensuremath{\lambda}$ the typical wavelength of a medium constituent. We show that the asymptotic expansion is universal with respect to the choice of the initial condition at $Y=0$ and, moreover, it is remarkably similar to the corresponding expansion for the saturation momentum of a ``shockwave'' (a large nucleus). As expected, the running of the coupling significantly slows down the increase of $\stackrel{^}{q}$ with $Y$ in the asymptotic regime at $Y\ensuremath{\gg}1$. For the phenomenologically interesting value $Y\ensuremath{\simeq}3$, we find an enhancement factor close to 3, independently of the initial condition and for both fixed and running coupling.
P-satI-D Shape Regulation of Soft Robots

Soft robots are intrinsically underactuated mechanical systems that operate under uncertainties and disturbances. In these conditions, this letter proposes two versions of PID-like control laws with a saturated integral action for the particularly challenging shape regulation task. The closed-loop system is asymptotically stabilized and matched constant disturbances are rejected using a very reduced amount of system information for control implementation. Stability is assessed on the underactuated dynamic model through the Invariant Set Theorem for two relevant classes of soft robots, i.e., elastically decoupled and elastically dominated soft robots. Extensive simulation results validate the proposed controllers.
Toward Synthetic Vascular Graft Monitoring Using a Flip-Chip-on-Flex Impedance Spectroscopy Sensor

Synthetic vascular grafts are used in a wide range of clinical applications. However, they can become prone to occlusion over time, due to the growth of vascular smooth muscle cells (VSMCs). This phenomenon is associated with graft failure. Here, we describe novel techniques for packaging and integration of a miniature sensor of VSMC growth. The sensor was based on a microfabricated array of interdigitated platinum electrodes on a silicon substrate. It was assembled using flip-chip-on-flex (FCOF) technology to create a low-profile package that can be manufactured using industry-standard tools and is suitable for integration with a synthetic vascular graft. The packaged sensor responded to changes in solution impedance and accurately detected the growth of VSMC in vitro. We also demonstrated successful proof-of-concept integration of the sensor with a custom synthetic graft. Together these technologies have the potential to allow early detection of VSMC growth prior to graft occlusion, enabling more timely and effective clinical interventions to be made.
Multi-black rings on Eguchi–Hanson space

We construct new supersymmetric multi-black ring solutions on the Eguchi–Hanson base space as solutions of the five-dimensional minimal supergravity. The spacetime has an asymptotically locally Euclidean time slice, i.e., it has the spatial infinity with the topology of the lens space . The configurations of black rings are restricted by the requirement of the absence of a Dirac–Misner string everywhere outside horizons. Especially, in the case of two black rings, the solutions have the limit to a pair of rotating black holes with the horizon topology of S3.
Modeling and Analysis of Cu-Carbon Nanotube Composites for Sub-Threshold Interconnects

The sub-threshold regime is suited for applications requiring ultra-low power consumption with low to medium frequency (tens to hundreds of MHz) of operation. Therefore, this paper presents electrical modeling and comprehensive analysis of copper-carbon nanotube (Cu-CNT) composite interconnects for sub-threshold circuit design. At lower operating frequencies, the effective complex conductivity of Cu-CNT composites in the nanoscale is formulated by developing an analytical model. Based on the proposed equivalent single conductor model, the frequency-dependent resistance and inductance of composite interconnects are computed. Finally, the sub-threshold crosstalk effect, transfer gain, and Nyquist stability of coupled Cu-CNT composite interconnect are analyzed using ABCD matrix approach.
DISCOVERY OF A GIANT, HIGHLY COLLIMATED JET FROM SANDULEAK'S STAR IN THE LARGE MAGELLANIC CLOUD

Highly collimated gas ejections are among the most dramatic structures in the universe, observed to emerge from very different astrophysical systems—from active galactic nuclei down to young brown dwarf stars. Even with the huge span in spatial scales, there is convincing evidence that the physics at the origin of the phenomenon, namely, the acceleration and collimation mechanisms, is the same in all classes of jets. Here we report on the discovery of a giant, highly collimated jet from Sanduleak's star in the Large Magellanic Cloud (LMC). With a physical extent of 14 pc at the distance of the LMC, it represents the largest stellar jet ever discovered, and the first resolved stellar jet beyond the Milky Way. The kinematics and extreme chemical composition of the ejecta from Sanduleak's star bear strong resemblance with the low-velocity remnants of SN1987A and with the outer filaments of the most famous supernova progenitor candidate, η Carinae. Moreover, the precise knowledge of the jets distance implies that it will be possible to derive accurate estimates of most of its physical properties. Sanduleak's bipolar outflow will thus become a crucial test bed for future theoretical modeling of astrophysical jets.
Testing chemical composition of highest energy comic rays

We study basic characteristics of distributions of the dept hs of shower maximum in air showers caused by cosmic rays with the highest energies. The consistency between their average values and widths, and their energy dependences are discussed within a simple phenomenological model of shower development independently of assumptions about detailed features of high-energy interactions. It is shown that reliable information on primary species can be derived within a partition method. We present examples demonstrating implications for the changes in mass composition of primary cosmic rays.
Scaling Properties of light (anti)nuclei and (anti)hypertriton production in Au+Au collisions at $\sqrt{s_{\rm{NN}}} = 200$ GeV

We present the scaling properties of mass number of light (anti)nuclei production in midrapidity Au + Au collisions at $\sqrt {s_{NN}}=200$ GeV based on the PACIAE + DCPC model. It is found that the integrated yield of light (anti)nuclei decreased exponentially with the increase of mass numbers which depends on the centrality, this properties of the system can be described quantitatively by temperature $T$ at hadronic freeze-out, and the model results are consistent with STAR data. Furthermore, we found that the integrated yield of heavier (anti)nuclei per participant nucleon increases from peripheral to central collisions more rapidly than that of $d(\bar{d})$, indicating that the mass scale of light (anti)nuclei production was presented in relativistic heavy ion collisions.
Extended Lyman-alpha emission from a high-z DLA at z=3.115

We searched for star formation activity associated with high-z Damped Lyman-alpha systems (DLAs) with Subaru telescope. We used a set of narrow-band (NB) filters whose central wavelengths correspond to the redshifted Lyman-alpha emission lines of targeted DLA absorbers at 3<z<4.5. We detected one apparent NB-excess object located 3.80 arcsec (~28kpc) away from the quasar SDSS J031036.84+005521.7. Follow-up spectroscopy revealed an asymmetric Lyman-alpha emission at z_em=3.115+/-0.003, which perfectly matches the sub-DLA trough at z_abs=3.1150 with logN(HI)/cm^-2=20.05. The Lyman-alpha luminosity is estimated to be L(LyA)=1.07x10^42 erg s^-1, which corresponds to a star formation rate of 0.97 M_\odot yr^-1. Interestingly, the detected Lyman-alpha emission is spatially extended with a sharp peak. The large extent of the Lyman-alpha emission is remarkably one-sided toward the quasar line-of-sight, and is redshifted. The observed spatially asymmetric surface brightness profile can be qualitatively explained by a model of a DLA host galaxy, assuming a galactic outflow and a clumpy distribution of HI clouds in the circumgalactic medium. This large Lyman-alpha extension, which is similar to those found in Rauch et al. (2008), could be the result of complicated anisotropic radiative transfer through the surrounding neutral gas embedded in the DLA.
Probing the properties of Be star discs with spectroastrometry and NLTE radiative transfer modelling: β CMi

While the presence of discs around classical Be stars is well established, their origin is still uncertain. To understand what processes result in the creation of these discs and how angular momentum is transported within them, their physical properties must be constrained. This requires comparing high spatial and spectral resolution data with detailed radiative transfer modelling. We present a high spectral resolution, R ∼ 80 000, sub-milliarcsecond precision, spectroastrometric study of the circumstellar disc around the Be star β CMi. The data are confronted with 3D, non-local thermodynamic equilibrium radiative transfer calculations to directly constrain the properties of the disc. Furthermore, we compare the data to disc models featuring two velocity laws: Keplerian, the prediction of the viscous disc model, and angular momentum conserving rotation. It is shown that the observations of β CMi can only be reproduced using Keplerian rotation. The agreement between the model and the observed spectral energy distribution, polarization and spectroastrometric signature of β CMi confirms that the discs around Be stars are well modelled as viscous decretion discs.
An X-shooter composite of bright 1 < z < 2 quasars from UV to infrared

Quasi-stellar object (QSO) spectral templates are important both to QSO physics and for investigations that use QSOs as probes of intervening gas and dust. However, combinations of various QSO samples obtained at different times and with different instruments so as to expand a composite and to cover a wider rest frame wavelength region may create systematic effects, and the contribution from QSO hosts may contaminate the composite. We have constructed a composite spectrum from luminous blue QSOs at 1 < z < 2.1 selected from the Sloan Digital Sky Survey (SDSS). The observations with X-shooter simultaneously cover ultraviolet (UV) to near- infrared (NIR) light, which ensures that the composite spectrum covers the full rest-frame range from Ly$\beta$ to 11350 $\AA$ without any significant host contamination. Assuming a power-law continuum for the composite we find a spectral slope of $\alpha_\lambda$ = 1.70+/-0.01, which is steeper than previously found in the literature. We attribute the differences to our broader spectral wavelength coverage, which allows us to effectively avoid fitting any regions that are affected either by strong QSO emissions lines (e.g., Balmer lines and complex [Fe II] blends) or by intrinsic host galaxy emission. Finally, we demonstrate the application of the QSO composite spectrum for evaluating the reddening in other QSOs.
Transcriptomic and Proteomic Profiles for Elucidating Cisplatin Resistance in Head-and-Neck Squamous Cell Carcinoma

Simple Summary Most treatment failures in head and neck squamous cell carcinoma (HNSCC) patients are due to the presence of resistant cells. Despite the chemotherapeutic advances that have taken place in recent decades, there are hardly new alternatives for HNSCC patients, with cisplatin being the most widely used chemotherapy drug. Therefore, it is urgent to propose new potential biomarkers and alternative therapeutic modalities capable of preventing the acquisition of resistance to treatment. We have conducted a RNA sequencing and proteomics study in cisplatin resistant and sensitive HNSCC cells with the aim of unravelling the molecular mechanisms involved in chemoresistance. Then, by an extensive literature search, in silico studies in cBioportal and in vitro experiments in biopsies from resistant and sensitive patients, we have listed potentially involved genes and proteins. Overall, the overexpression of MAGEB2 was identified in resistant tumours, revealing it as a novel protein targeting sensitised HNSCC resistant patients. Abstract To identify the novel genes involved in chemoresistance in head and neck squamous cell carcinoma (HNSCC), we explored the expression profiles of the following cisplatin (CDDP) resistant (R) versus parental (sensitive) cell lines by RNA-sequencing (RNA-seq): JHU029, HTB-43 and CCL-138. Using the parental condition as a control, 30 upregulated and 85 downregulated genes were identified for JHU029-R cells; 263 upregulated and 392 downregulated genes for HTB-43-R cells, and 154 upregulated and 68 downregulated genes for CCL-138-R cells. Moreover, we crossed-checked the RNA-seq results with the proteomic profiles of HTB-43-R (versus HTB-43) and CCL-138-R (versus CCL-138) cell lines. For the HTB-43-R cells, 21 upregulated and 72 downregulated targets overlapped between the proteomic and transcriptomic data; whereas in CCL-138-R cells, four upregulated and three downregulated targets matched. Following an extensive literature search, six genes from the RNA-seq (CLDN1, MAGEB2, CD24, CEACAM6, IL1B and ISG15) and six genes from the RNA-seq and proteomics crossover (AKR1C3, TNFAIP2, RAB7A, LGALS3BP, PSCA and SSRP1) were selected to be studied by qRT-PCR in 11 HNSCC patients: six resistant and five sensitive to conventional therapy. Interestingly, the high MAGEB2 expression was associated with resistant tumours and is revealed as a novel target to sensitise resistant cells to therapy in HNSCC patients.
DYNAMICS OF CORONAL RAIN AND DESCENDING PLASMA BLOBS IN SOLAR PROMINENCES. I. FULLY IONIZED CASE

Observations of active regions and limb prominences often show cold, dense blobs descending with an acceleration smaller than that of free fall. The dynamics of these condensations falling in the solar corona is investigated in this paper using a simple fully ionized plasma model. We find that the presence of a heavy condensation gives rise to a dynamical rearrangement of the coronal pressure that results in the formation of a large pressure gradient that opposes gravity. Eventually this pressure gradient becomes so large that the blob acceleration vanishes or even points upward. Then, the blob descent is characterized by an initial acceleration phase followed by an essentially constant velocity phase. These two stages can be identified in published time–distance diagrams of coronal rain events. Both the duration of the first stage and the velocity attained by the blob increase for larger values of the ratio of blob to coronal density, for larger blob mass, and for smaller coronal temperature. Dense blobs are characterized by a detectable density growth (up to 60% in our calculations) and by a steepening of the density in their lower part, that could lead to the formation of a shock. They also emit sound waves that could be detected as small intensity changes with periods of the order of 100 s and lasting between a few and about 10 periods. Finally, the curvature of falling paths with large radii is only relevant when a very dense blob falls along inclined magnetic field lines.
Uniqueness of photon spheres in electro-vacuum spacetimes

In a recent paper (Cederbaum C and Galloway G J 2015 Commun. Analysis Geom. at press), the authors established the uniqueness of photon spheres in static vacuum asymptotically flat spacetimes by adapting Bunting and Masood-ul-Alam’s proof of static vacuum black hole uniqueness. Here, we establish uniqueness of suitably defined sub-extremal photon spheres in static electro-vacuum asymptotically flat spacetimes by adapting the argument of Masood-ul-Alam (1992 Class. Quantum Grav. 9 L53-5). As a consequence of our result, we can rule out the existence of electrostatic configurations involving multiple ‘very compact’ electrically charged bodies and sub-extremal black holes.
Real-time digital holographic microscopy observable in multi-view and multi-resolution

We propose a real-time digital holographic microscopy that enables simultaneous multiple reconstructed images with arbitrary resolution, depth and positions, using shifted-Fresnel diffraction instead of Fresnel diffraction. In this system, we used four graphics processing units (GPUs) for multiple reconstructions in real-time. We demonstrate four reconstruction images from a hologram with arbitrary depths, positions and resolutions.
The Universal Faber-Jackson Relation

In the context of modified Newtonian dynamics, the Fundamental Plane, as the observational signature of the Newtonian virial theorem, is defined by high-surface-brightness objects that deviate from being purely isothermal: the line-of-sight velocity dispersion should slowly decline with radius as observed in luminous elliptical galaxies. All high-surface-brightness objects (e.g. globular clusters, ultra-compact dwarfs) will lie, more or less, on the Fundamental Plane defined by elliptical galaxies, but low-surface-brightness objects (dwarf spheroidals) would be expected to deviate from this relation. This is borne out by observations. With Milgrom's modified Newtonian dynamics (MOND), the Faber-Jackson relation (L proportional to Sigma 4), ranging from globular clusters to clusters of galaxies and including both high- and low-surface-brightness objects, is the more fundamental and universal scaling relation in spite of its larger scatter. The Faber-Jackson relation reflects the presence of an additional dimensional constant (the MOND acceleration a(0)) in the structure equation.