Miracle-dz/UniFAR-FTUs huggingface dataset:
An X-Ray Study of the Supernova Remnant G290.1–0.8

G290.1-0.8 (MSH 11-61A) is a supernova remnant (SNR) whose X-ray morphology is centrally bright. However, unlike the class of X-ray composite SNRs whose centers are dominated by nonthermal emission presumably driven by a central pulsar, we show that the X-ray emission from G290.1-0.8 is thermal in nature, placing the remnant in an emerging class which includes such remnants as W44, W28, 3C391, and others. The evolutionary sequence which leads to such X-ray properties is not well understood. Here we investigate two scenarios for such emission: evolution in a cloudy interstellar medium, and early-stage evolution of a remnant into the radiative phase, including the effects of thermal conduction. We construct models for these scenarios in an attempt to reproduce the observed center-filled X-ray properties of G290.1-0.8, and we derive the associated age, energy, and ambient density conditions implied by the models. We find that for reasonable values of the explosion energy, the remnant age is of order (1-2) × 104 yr. This places a fairly strong constraint on any association between G290.1-0.8 and PSR J1105-610, which would require an anomalously large velocity for the pulsar.
Mg II Absorber Number Density at z ≃ 0.05: Implications for ΩDLA Evolution

An unbiased sample of 147 quasar/active galactic nuclei spectra, obtained with the Faint Object Spectrograph on board the Hubble Space Telescope, has been searched for intervening Mg II λλ2796, 2803 absorbers over the redshift range 0 < z ≤ 0.15. The total redshift path searched is 18.8, with the survey being 80% complete to a 5 σ rest-frame equivalent width Wr(λ2796) of 0.6 Å and 20% complete to Wr(λ2796) = 0.3 Å. Main results of this work are the following: (1) Four systems were found, with a mean redshift of ⟨z⟩ = 0.06, yielding a redshift number density dN/dz = 0.22 for absorbers with Wr(λ2796) ≥ 0.6 Å. This is consistent with the value expected if these systems do not evolve from higher redshifts (z = 2.2). (2) No systems with Wr(λ2796) < 0.6 Å were found. Based on no evolution expectations and accounting for the survey completeness, it is a 2 σ result to have a null detection of smaller Wr(λ2796) systems. If this implies a turnover in the low Wr(λ2796) region of the equivalent width distribution at z ~ 0, then there is at least a 25% reduction in the average galaxy gas cross section from z ≤ 0.2 galaxies. (3) These systems have strong Fe II absorption and, based on the results of Rao & Turnshek, are good candidates for damped Lyα absorbers (DLAs). This translates to a redshift number density of dN/dz = 0.08 for DLAs at z ~ 0. In tandem with the data analyzed by Rao & Turnshek, these results indicate that the redshift number density of DLAs does not evolve from z ≃ 4 to z ≃ 0. If the H I mass function does not evolve from z ≃ 0.5 to z ≃ 0, then the cosmological H I mass density ΩDLA is also deduced so as to not evolve from z ≃ 4 to z ≃ 0. These z ≃ 0 results for Mg II absorption-selected DLAs are at odds with those based on 21 cm emission from H I galaxies by a factor of 5-6.
Discovery of a Radio Supernova Remnant and Nonthermal X-Rays Coincident with the TeV Source HESS J1813–178

We present the discovery of nonthermal radio and X-ray emission positionally coincident with the TeV gamma-ray source HESS J1813-178. We demonstrate that the nonthermal radio emission is due to a young shell-type supernova remnant (SNR), G12.8-0.0, and constrain its distance to be greater than 4 kpc. The X-ray emission is primarily nonthermal and is consistent with either an SNR shell or unidentified pulsar or pulsar wind nebula origin; pulsed emission is not detected in archival ASCA data. A simple synchrotron plus inverse Compton model for the broadband emission assuming that all of the emission arises from the SNR shell implies maximum energies of (30-450)[B/(10 μG)]-0.5 TeV. Further observations are needed in order to confirm that the broadband emission has a common origin and to better constrain the X-ray spectrum.
Interstellar dust in the solar system: model versus in situ spacecraft data

Context. In the early 1990s, contemporary interstellar dust penetrating deep into the heliosphere was identified with the in situ dust detector on board the Ulysses spacecraft. Later on, interstellar dust was also identified in the data sets measured with dust instruments on board Galileo, Cassini, and Helios. Ulysses monitored the interstellar dust stream at high ecliptic latitudes for about 16 yr. The three other spacecraft data sets were obtained in the ecliptic plane and cover much shorter time intervals. Aims. To test the reliability of the model predictions, we compare previously published in situ interstellar dust measurements, obtained with these four spacecraft, with predictions of an advanced model for the dynamics of interstellar dust in the inner solar system (Interplanetary Meteoroid environment for EXploration; IMEX). Methods. Micrometer and sub-micrometer-sized dust particles are subject to solar gravity, radiation pressure and the Lorentz force on a charged dust particle moving through the interplanetary magnetic field. These forces lead to a complex size-dependent flow pattern of interstellar dust in the planetary system. The IMEX model was calibrated with the Ulysses interstellar dust measurements and includes these relevant forces. We study the time-resolved flux and mass distribution of interstellar dust in the solar system. Results. The IMEX model agrees with the spacecraft measurements within a factor of 2–3, including time intervals and spatial regions not covered by the original model calibration with the Ulysses data set. The model usually underestimates the dust fluxes measured by the space missions which were not used for the model calibration, i.e. Galileo, Cassini, and Helios. Conclusions. A unique time-dependent model, IMEX is designed to predict the interstellar dust fluxes and mass distributions for the inner and outer solar system. The model is suited to study dust detection conditions for past and future space missions.
Star Formation in the ISO Atlas of Spiral Galaxies

We investigate star formation along the Hubble sequence using the ISO Atlas of Spiral Galaxies. Using mid-infrared and far-infrared flux densities normalized by K-band flux densities as indicators of recent star formation, we find several trends. First, star formation activity is stronger in late-type (Sc - Scd) spirals than in early-type (Sa - Sab) spirals. This trend is seen both in nuclear and disk activity. These results confirm several previous optical studies of star formation along the Hubble sequence but conflict with the conclusions of most of the previous studies using IRAS data, and we discuss why this might be so. Second, star formation is significantly more extended in later-type spirals than in early-type spirals. We suggest that these trends in star formation are a result of differences in the gas content and its distribution along the Hubble sequence, and it is these differences that promote star formation in late-type spiral galaxies. We also search for trends in nuclear star formation related to the presence of a bar or nuclear activity. The nuclear star formation activity is not significantly different between barred and unbarred galaxies. We do find that star formation activity appears to be inhibited in LINERs and transition objects compared to HII galaxies. The mean star formation rate in the sample is 1.4 Msun/yr based on global far-infrared fluxes. Combining these data with CO data gives a mean gas consumption time of 6.4 x 10^8 yr, which is ~5 times lower than the values found in other studies. Finally, we find excellent support for the Schmidt Law in the correlation between molecular gas masses and recent star formation in this sample of spiral galaxies.
Giant gigahertz optical activity in multiferroic ferroborate

In contrast to well studied multiferroic manganites with a spiral structure, the electric polarization in multiferroic borates is induced within collinear antiferromagnetic structure and can easily be switched by small static fields. Because of specific symmetry conditions, static and dynamic properties in borates are directly connected, which leads to giant magnetoelectric and magnetodielectric effects. Here we prove experimentally that the giant magnetodielectric effect in samarium ferroborate SmFe3(BO3)4 is of intrinsic origin and is caused by an unusually large electromagnon situated in the microwave range. This electromagnon reveals strong optical activity exceeding 120 degrees of polarization rotation in a millimeter thick sample.
Massive Molecular Outflows at High Spatial Resolution

We present high spatial resolution Plateau de Bure Interferometer CO (2-1) and SiO (2-1) observations of one intermediate-mass and one high-mass star-forming region. The intermediate-mass region IRAS 20293+3952 exhibits four molecular outflows, one being as collimated as the highly collimated jetlike outflows observed in low-mass star formation sources. Furthermore, comparing the data with additional infrared H2 and centimeter observations, we see indications that the nearby ultracompact H II region triggers a shock wave interacting with the outflow. The high-mass region IRAS 19217+1651 exhibits a bipolar outflow as well, and the region is dominated by the central driving source. Adding two more sources from the literature, we compare position-velocity diagrams of the intermediate-to-high-mass sources with previous studies in the low-mass regime. We find similar kinematic signatures; some sources can be explained by jet-driven outflows, whereas others are better constrained by wind-driven models. The data also allow us to estimate accretion rates varying from a few times 10-5 M☉ yr-1 for the intermediate-mass sources to a few times 10-4 M☉ yr-1 for the high-mass source, consistent with models explaining star formation of all masses via accretion processes.
Planetary nebulae in the circumnuclear region of M31: a spectroscopic sample

Planetary nebulae (PNe) are an important tool for studying the dynamics and chemical evolution of galaxies in the Local Universe, given their characteristic bright emission line spectra. The Andromeda Galaxy (M31) provides a unique laboratory for studying PNe in the circumnuclear region, thanks to its proximity and almost uniformly low line-of-sight extinction that ensures observations with high resolution and sensitivity. Using the WIYN/Hydra multi-fiber spectrograph, we have obtained optical (4119–6882 Å) spectra of 77 PN candidates selected from Hubble Space Telescope narrow-band imaging, which are located within the central ∼500 pc region of M31. Among these candidates, 49 (64%) are spectroscopically observed for the first time. The spectra of 300 previously known PNe and H ii regions, which primarily reside in the disk, are also taken for comparison. All 77 circumnuclear PN candidates exhibit prominent emission lines, including [O iii] λ5007, [N ii] λ6583, Hα and Hβ, strongly suggesting that they are genuine PNe. We measured the line fluxes, radial velocities and line widths for all objects, and found that the radial velocities of the circumnuclear PNe generally trace rotation of the inner bulge. We also estimated a dynamical mass of ∼6.4 ± 0.5 × 109 M ⊙ enclosed within an effective galactocentric radius of 340 pc, which is compatible with the previously estimated total stellar mass in this region.
Generalized Dirichlet to Neumann map for moving initial-boundary value problems

We present an algorithm for characterizing the generalized Dirichlet to Neumann map for moving initial-boundary value problems. This algorithm is derived by combining the so-called global relation, which couples the initial and boundary values of the problem, with a new method for inverting certain one-dimensional integrals. This new method is based on the spectral analysis of an associated ordinary differantial equation and on the use of the d-bar formalism. As an illustration, the Neumann boundary value for the linearized Schrodinger equation is determined in terms of the Dirichlet boundary value and of the initial condition.
Interaction-driven topological switch in a 
P
-band honeycomb lattice

The non-interacting band structure of spinless fermions in a two-dimensional ($d=2$) $p$-band honeycomb lattice exhibits two quadratic band touching points (QBTPs), which lie at the Fermi levels of filling $\nu=1/4$ and its particle-hole conjugated filling $\nu=3/4$. A weak Hubbard interaction $U$ spontaneously breaks the time-reversal symmetry and removes the QBTP, rendering the system into a quantum anomalous Hall insulator (QAHI). The first-order topological nature of QAHI is characterized by a nontrivial Chern number and supports ($d-1$)-dimensional chiral edge modes. With increasing the interaction $U$, the system is driven into a Dirac semimetal by breaking the crystal symmetry through a discontinuous quantum phase transition. The emergent Dirac points each with Berry flux $\pi$ are generated in pairs, originating from the $2\pi$ Berry flux of QBTP. A sufficiently large $U$ ultimately drives the system into a dimerized insulator (DI) by simultaneously annihilating the Dirac points at the Brillouin zone boundary. The second-order topological nature of DI is characterized by the quantized polarizations and supports ($d-2$)-dimensional corner states. Our study provides a unique setting for exploring the topological switch between the first-order and second-order topological insulators.
Integral Representations for Bessel Matrix Functions

Jodar et. al. [Util. Math. 46 (1994) 129-141] introduced the concept of Bessel matrix functions of the first kind. In this paper, we derive integral representations for these functions. 2010 Mathematics Subject Classification. Primary 33C45, 33C10; Secondary 15A60. Key words: Bessel matrix function, Jordan block, Gamma matrix function, Beta matrix function, integral representations.
Adherence to international perioperative antimicrobial prophylaxis guidelines in three general hospitals: A cross-sectional study

Evidence-based guidelines for perioperative antimicrobial prophylaxis (PAP) are well established. It is unknown whether PAP practice in Gaza Strip hospitals follows those guidelines. This study aimed to assess the adherence of PAP practice at surgical wards in Gaza Strip hospitals to the American Society of Health-System Pharmacists (ASHP) guidelines for antimicrobial surgical prophylaxis. Data were collected over a 6-month period by direct observation and chart review methods. Aspects of PAP (indication, selection, duration, dosing, and first dose timing) were assessed against ASHP guidelines. The study enrolled 444 surgical patients, of whom 94.8% received PAP. The overall adherence rate was 7.4%. Adherence rates for indication, selection, dosing, timing of first dose, and duration were 70.7%, 56.3%, 17.7%, 59%, and 58%, respectively. Patients who underwent clean surgeries were less likely to be given the recommended antibiotic than those who underwent clean-contaminated surgeries (OR 0.480, 95% CI 0.375–0.615, p -value 0.021). Nurses were less likely to adhere to the right first dose timing than anesthesiologists (OR 0.132, 95% CI 0.051–0.374, p -value 0.011). This study showed poor adherence to guidelines in all aspects of PAP use, particularly dosing. Strategies to improve PAP practice should be adopted and implemented.
Numerical analysis of aerodynamic characteristics of multi-pod hyperloop system

The Hyperloop system is a new and innovative mode of transportation in which high-speed pods move through near-vacuum tubes. The multi-pod Hyperloop Systems are essential for increased transportation capacity. In this study, a multi-pod Hyperloop System was analyzed using numerical simulations at different values of the distance between the pods (i.e., 2 L–3.5 L). The pressure and velocity flow fields and the aerodynamic characteristics of the pods were analyzed for four different flow speeds, that is, 100, 200, 300, and 400 m/s, using unsteady compressible flow conditions. The simulation results indicated that the pressure waves generated across the pods play a significant role in the determination of the aerodynamic characteristics of the pods. Increasing the distance between the pods results in the delay of the pressure wave interaction. The aerodynamic drag increases on the first pod with the increase in the distance between the pods due to an increase in the pressure gradient. In contrast, the aerodynamic drag decreases across the second pod with the increase in the distance between them. So, the distance between the pods is a critical factor that should be considered when designing the Hyperloop System with more than one pod.
Finite‐time stability of switched positive linear systems

This brief paper addresses the finite‐time stability problem of switched positive linear systems. First, the concept of finite‐time stability is extended to positive linear systems and switched positive linear systems. Then, by using the state transition matrix of the system and copositive Lyapunov function, we present a necessary and sufficient condition and a sufficient condition for finite‐time stability of positive linear systems. Furthermore, two sufficient conditions for finite‐time stability of switched positive linear systems are given by using the common copositive Lyapunov function and multiple copositive Lyapunov functions, a class of switching signals with average dwell time is designed to stabilize the system, and a computational method for vector functions used to construct the Lyapunov function of systems is proposed. Finally, a concrete application is provided to demonstrate the effectiveness of the proposed method. Copyright © 2012 John Wiley & Sons, Ltd.
NGC 3576 and NGC 3603: Two Luminous Southern H II Regions Observed at High Resolution with the Australia Telescope Compact Array

NGC 3576 (G291.28-0.71) and NGC 3603 (G291.58-0.43) are optically visible, luminous H II regions located at distances of 3.0 kpc and 6.1 kpc, respectively. We present 3.4 cm Australia Telescope Compact Array (ATCA) observations of these two sources in the continuum and the H90α, He90α, C90α, and H113β recombination lines with an angular resolution of 7″ and a velocity resolution of 2.6 km s-1. All four recombination lines are detected in the integrated profiles of the two sources. Broad radio recombination lines are detected in both NGC 3576 (ΔVFWHM ≥ 50 km s-1) and NGC 3603 (ΔVFWHM ≥ 70 km s-1). In NGC 3576 a prominent north-south velocity gradient (∼30 km s-1 pc-1) is observed, and a clear temperature gradient (6000–8000 K) is found from east to west, consistent with a known infrared color gradient in the source. In NGC 3603, the H90α, He90α, and the H113β lines are detected from 13 individual sources. The Y+ (He/H) ratios in the two sources range from 0.08 ± 0.04 to 0.26 ± 0.10. The H113β/H90α ratio in NGC 3576 is close to the theoretical value, suggesting that local thermodynamic equilibrium exists. This ratio is enhanced for most regions in NGC 3603; enhanced β/α ratios in other sources have been attributed to high optical depth or stimulated emission. We compare the morphology and kinematics of the ionized gas at 3.4 cm with the distribution of stars, 10 μm emission, and H2O, OH, and CH3OH maser emission. These comparisons suggest that both NGC 3576 and NGC 3603 have undergone sequential star formation.
The Radio/Optical Catalog of the SSA 13 Field

We present a 1.4 GHz catalog of 810 radio sources (560 sources in the complete sample) found in the SSA 13 field (R.A. = 13h12m, decl. = 42°38'). The 1.4 GHz radio image was obtained from a 91 hr VLA integration with an rms noise level of 4.82 μJy beam-1 at the field center. Optical images in the R band (6300 Å) and z band (9200 Å) with 3 σ detection magnitudes of 26.1 and 24.9, respectively, were obtained from three observing nights on the 8 m Subaru Telescope. We find that 88% ± 2% of the radio sources are identified with an optical counterpart. There is significantly more reddening for the optical counterparts that are fainter than 24 mag, probably caused by the somewhat larger redshifts of these faint galaxies. The radio and optical parameters are tabulated, and source morphologies are displayed by radio contours overlaid on optical false-color images. The brightness distributions show a wealth of complexity and are classified into a small number of categories. About one-third of the radio sources are larger than 1. ″2, and their orientation is often similar to that of the associated galaxy or binary galaxy system. Radio emission is sometimes located outside of the nuclear regions of the galaxy. The density of sources in the SSA 13 field above 75 μJy is 0.40 arcmin-2, with a slope of -2.43 in the differential counts. This source density is somewhat higher than that in the Hubble Deep Field North. The radio spectral index may steepen for sources below 75 μJy and is consistent with the difference in the slope of the source counts observed between 1.4 and 8.4 GHz. We estimate that at most 40% of the microjansky radio sources are dominated by AGN processes, while the remainder are mostly the consequence of star formation and associated supernova activity.
Spectral Energy Distributions of Seyfert Nuclei

We present nuclear spectral energy distributions (SEDs) in the range 0.4–16 μm for an expanded CfA sample of Seyfert galaxies. The spectral indexes (fν ∝ ν) from 1 to 16 μm range from αIR ∼ 0.9 to 3.8. The shapes of the spectra are correlated with Seyfert type in the sense that steeper nuclear SEDs (νfν increasing with increasing wavelength) tend to be found in Seyfert 2's, and flatter SEDs (νfν is constant) in Seyfert 1–1.5's. The galaxies optically classified as Seyferts 1.8's and 1.9's display values of αIR as in type 1 objects, or values intermediate between those of Seyfert 1's and Seyfert 2's. The intermediate SEDs of many Seyfert 1.8–1.9's may be consistent with the presence of a pure Seyfert 1 viewed through a moderate amount (AV ≲ 5 mag) of foreground galaxy extinction. We find, however, that between 10% and 20% of galaxies with broad optical line components have steep infrared SEDs. Torus models usually adopt high equatorial opacities to reproduce the infrared properties of Seyfert 1's and 2's, resulting in a dichotomy of infrared SEDs (flat for type 1's, and steep for type 2's). Such a dichotomy, however, is not observed in our sample. The wide range of spectral indexes observed in the type 2 objects, the lack of extremely steep SEDs, and the large numbers of objects with intermediate spectral indexes cannot be reconciled with predictions from existing optically thick torus models. We discuss possible modifications to improve torus models, including low optical depth tori, clumpy dusty tori, and high optical depth tori with an extended optically thin component.