Miracle-dz/UniFAR-FTUs huggingface dataset:
A Search for FRB 121102-like Persistent Radio-luminous Sources—Candidates and Implications for the FRB Rate and Searches

The localization of the repeating fast radio burst (FRB), FRB 121102, suggests that it is associated with a persistent radio-luminous compact source in the FRB host galaxy. Using the FIRST radio catalog, I present a search for luminous persistent sources in nearby galaxies, with radio luminosities of the FRB 121102 persistent source luminosity. The galaxy sample contains about 30% of the total galaxy g-band luminosity within Mpc, in a footprint of 10,600 deg2. After rejecting sources likely due to active galactic nuclei activity or background sources, I am left with 11 candidates that are presumably associated with galactic disks or star-formation regions. At least some of these candidates are likely to be due to chance alignment. In addition, I find 85 sources within of galactic nuclei. Assuming that the radio persistent sources are not related to galactic nuclei and that they follow the galaxy g-band light, the 11 sources imply a 95% confidence upper limit on the space density of luminous persistent sources of Mpc−3, and that at any given time only a small fraction of galaxies host a radio-luminous persistent source ( ). Assuming a persistent source lifetime of 100 years, this implies a birth rate of yr−1 Mpc−3. Given the FRB volumetric rate, and assuming that all FRBs repeat and are associated with persistent radio sources, this sets a lower limit on the rate of FRB events per persistent source of yr−1. I argue that these 11 candidates are good targets for FRB searches and I estimate the FRB event rate from these candidates.
The Evolution Equations of Shock Deformation Problems with Plane Surfaces of Discontinuities in Elastic Inhomogeneous Mediums

For the model of the nonlinear elastic medium with inhomogeneous properties represented by a continuous change of the elastic moduli and density, the motion problems of a plane longitudinal or transverse shock waves are considered. The matched asymptotic expansions method allows to determine the evolution equations reflecting the nonlinearity of the wave processes and the inhomogeneity of the medium. The transition to the limiting inner problem of the small parameter method is dictated by the chain of inner problems, the solutions of which require a changes in all of the independent variables and their scales.
Consistent implementation of non-zero-range terms into hydrodynamics

Non-zero-range interactions are often incorporated into mean field theories through gradient terms. Here, a formalism is developed to incorporate such terms into hydrodynamics. These terms alter expressions for the entropy, chemical potential, temperature and the stress-energy tensor. The formalism respects local conservation of energy, charge and entropy. The formalism leads to static solutions where the temperature, chemical potential and hydrodynamic acceleration all vanish, even when the density profile might be non-uniform. Profiles for a phase boundary and for correlation functions are calculated to illustrate the gradient modifications for various thermodynamic quantities. Also, for hydrodynamic calculations that add thermal noise to generate density-density correlations of the desired strength, an additional noise term is derived so that, at equilibrium, correlations are generated with both the correct size and length scale.
Polarization effects, surface states, and the source of electrons in AlGaN/GaN heterostructure field effect transistors

The origin of the two-dimensional electron gas (2DEG) in AlGaN/GaN heterostructure field effect transistors is examined theoretically and experimentally. Based on an analysis of the electrostatics, surface states are identified as an important source of electrons. The role of the polarization-induced dipole is also clarified. Experimental Hall data for nominally undoped Al0.34Ga0. 66N/GaN structures indicate that ∼1.65 eV surface donors are the actual source of the electrons in the 2DEG, which forms only when the barrier thickness exceeds 35 A.
The Next Generation of Cosmological Measurements with Type Ia Supernovae

While Type Ia Supernovae (SNe Ia) are one of the most mature cosmological probes, the next era promises to be extremely exciting in the number of different ways SNe Ia are used to measure various cosmological parameters. Here we review the experiments in the 2020s that will yield orders of magnitudes more SNe Ia, and the new understandings and capabilities to constrain systematic uncertainties at a level to match these statistics. We then discuss five different cosmological probes with SNe Ia: the conventional Hubble diagram for measuring dark energy properties, the distance ladder for measuring the Hubble constant, peculiar velocities and weak lensing for measuring sigma8 and strong-lens measurements of H0 and other cosmological parameters. For each of these probes, we discuss the experiments that will provide the best measurements and also the SN Ia-related systematics that affect each one.
Spectrum and Duration of Delayed MeV-GeV Emission of Gamma-Ray Bursts in Cosmic Background Radiation Fields

We generally analyze prompt high-energy emission above a few hundred GeV due to synchrotron self-Compton scattering in internal shocks. However, such photons cannot be detected because they may collide with cosmic infrared background photons, leading to electron/positron pair production. Inverse Compton scattering of the resulting electron/positron pairs off cosmic microwave background photons will produce delayed MeV-GeV emission, which may be much stronger than a typical high-energy afterglow in the external shock model. We expand on the model of Cheng & Cheng by deriving the emission spectrum and duration in the standard fireball shock model. A typical duration of the emission is ~103 s, and the time-integrated scattered photon spectrum is ν-(p+6)/4, where p is the index of the electron energy distribution behind internal shocks. This is slightly harder than the synchrotron photon spectrum, ν-(p+2)/2. The lower energy property of the scattered photon spectrum is dependent on the spectral energy distribution of the cosmic infrared background radiation. Therefore, future observations on such delayed MeV-GeV emission and the higher energy spectral cutoff by the Gamma-Ray Large Area Space Telescope (GLAST) would provide a probe of the cosmic infrared background radiation.
A new method for performing an absolute measurement of the geomagnetic field

The paper describes a method for measuring the geomagnetic field vector using a scalar magnetometer and a three-axis flux-gate magnetometer rotating about two defined axes. The proposed method is an alternative to DI-flux measurement (D: declination; I: inclination), which is based on a theodolite-borne one-component flux-gate magnetometer. The basic idea is that the calibration of the magnetometer and the determination of the field in the direction of the rotation axis can be carried out using the same procedure. Requirements concerning the three-component magnetometer and the mechanics will be discussed. The method presented will be compared with the DI-flux procedure.
Intensity Fluctuations of Partially Polarized Light

The ensemble distribution is derived for the number of photons n counted in a short time interval by a photodetector which is illuminated by a partially polarized beam of thermal light. It is shown to be of the form expected for n bosons distributed between 2/(1 + P) cells of phase space, where P is the degree of polarization. This number also has a simple classical analogue as the statistical degrees of freedom of light waves with a Gaussian amplitude distribution, and it is completely determined by the ratio of the eigenvalues of the usual 2 × 2 coherence matrix. It is suggested that no comparable simple conclusions will normally hold for non-thermal light, as, for example, from an optical maser.
Photoluminescence of a single InAs quantum dot molecule under applied electric field

We study the electronic coupling between two vertically stacked InAs quantum dots, which are embedded in the center of a n-i-n structure. We use a microphotoluminescence setup to optically isolate a single quantum dot pair and measure the time-averaged photoluminescence under an applied vertical electric field. We find that field tunable coupling between excited states of the two quantum dots leads to charge transfer from one dot to the other. We model the spectra including simultaneously the field-dependent charge transfer and exciton capture rates, and the many-body spectra of the quantum dot molecule for different carrier configurations.
A Detection of Sgr A* in the Far Infrared

We report the first detection of the Galactic Center massive black hole, Sgr A*, at 100 μm and 160 μm. Our measurements were obtained with PACS on board the Herschel satellite. While the warm dust in the Galactic Center is too bright to allow for a direct detection of Sgr A*, we measure a significant and simultaneous variation of its flux of and during one observation. The significance level of the variability in the 160 μm band is 4. 5σ, and the corresponding variability in the 100 μm band is significant at 1. 6σ. We find no example of an equally significant false positive detection. Conservatively assuming a variability of 25% in the FIR, we can provide upper limits to the flux. Comparing the latter with theoretical models, we find that 1D radiatively inefficient accretion flow models have difficulties explaining the observed faintness. However, the upper limits are consistent with modern observations by ALMA and the Very Large Array. Our upper limits provide further evidence for a spectral peak at ∼1012 Hz and constrain the number density of γ ∼ 100 electrons in the accretion disk and/or outflow.
Correction algorithms in a laser scanning dimension measurement system

The principal system error in a laser scanning dimension measurement system (LSDMS) is the variation of the scanning speed of the laser beam at different locations of the measuring region, which is caused mainly by the conventionally corrected lens. When a small spin gauge is positioned and measured within the measuring region of the LSDMS, the deviation of the scanning speed from a constant speed can be obtained. This deviation is the criterion on which two correction algorithms are based. The correction algorithms are proposed and discussed, and both show satisfactory improvement in the performance of the LSDMS.
Nonspherical perturbations of relativistic gravitational collapse

It is known that there can be no gravitational, electromagnetic, or scalar field perturbations (except angular momentum) of a Schwarzschild black hole. A gravitationally collapsing star with nonspherical perturbations must therefore radiate away its perturbations or halt its collapse. The results of computations in comoving coordinates are presented to show that the scalar field in a collapsing star neither disappears nor halts the collapse, as the star passes inside its gravitational radius. On the star's surface, near the event horizon, the scalar field varies as a_1 + a_2 exp (-t/2M) due to time dilation. The dynamics of the field outside the star can be analyzed with a simple wave equation containing a spacetime-curvature induced potential. This potential is impenetrable to zero-frequency waves and thus a_1, the final value of the field on the stellar surface, is not manifested in the exterior; the field vanishes. The monopole perturbation falls off as t^(-2); higher l-poles fall off as ln t/t^(2l+3). The analysis of scalar-field perturbations works as well for electromagnetic and gravitational perturbations and also for zero-restmass perturbation fields of arbitrary integer spin. All these perturbation fields obey wave equations with curvature potentials that differ little from one field to another. For all fields, radiatable multipoles (l ≥ spin of the field) fall off as lnt/t^(2l+3).
The Diverse Science Return from a Wide-Area Survey of the Galactic Plane

The overwhelming majority of objects visible to LSST lie within the Galactic Plane. Though many previous surveys have avoided this region for fear of stellar crowding, LSST's spatial resolution combined with its state-of-the-art Difference Image Analysis mean that it can conduct a high cadence survey of most of the Galaxy for the first time. Here we outline the many areas of science that would greatly benefit from an LSST survey that included the Galactic Plane, Magellanic Clouds and Bulge at a cadence of 2-3 d. Particular highlights include measuring the mass spectrum of black holes, and mapping the population of exoplanets in the Galaxy in relation to variations in star forming environments. But the same survey data will provide a goldmine for a wide range of science, and we explore possible survey strategies which maximize the scientific return for a number of fields including young stellar objects, cataclysmic variables and Neptune Trojans.
Real-World Effectiveness, Tolerability, and Safety of Dolutegravir/Lamivudine in Korea

Most studies on the real-world effectiveness and safety of dolutegravir/lamivudine (DTG/3TC) have been conducted in Western countries, and Asian reports are lacking. We evaluated the effectiveness and safety of DTG/3TC in Korean adult people living with HIV (PLWH). This retrospective study was conducted from July 2020 to July 2022 at a tertiary hospital in Korea. Those who were followed up for more than 12 months were included. We analyzed the baseline characteristics, effectiveness, resistant profiles, body weights, metabolic parameters, and safety of DTG/3TC treatment in 151 PLWH, dividing them into the treatment-naïve group and the switching group. The median DTG/3TC treatment durations in the treatment-naïve and switching groups were 507.5 and 525.0 days. In the treatment-naïve group, the viral RNA titer was undetectable at 6 and 12 months in 95% of patients. In the switching group, virologic suppression was well-maintained. Meanwhile, the creatinine levels were slightly elevated in both groups compared to baseline. Five participants complained of mild side effects, such as indigestion, constipation, diarrhea, and fatigue. However, no patient stopped treatment during the follow-up period. Since there was no virological failure or serious complications observed in this study, DTG/3TC may be a good treatment option for PLWH in Korea.
Differential rotation and meridional flow in the solar convection zone and beneath

The influence of the basic rotation on anisotropic and inhomogeneous turbulence is discussed in the context of differential rotation theory. An improved representation for the original turbulence leads to a Λ-effect which complies with the results of 3D numerical simulations. The resulting rotation law and meridional flow agree well with both the surface observations (∂Ω/∂r < 0 and meridional flow towards the poles) and with the findings of helioseismology. The computed equatorward flow at the bottom of convection zone has an amplitude of about 10 m/s and may be significant for the solar dynamo. The depth of the meridional flow penetration into the radiative zone is proportional to ν0. 5core, where νcore is the viscosity beneath the convection zone. The penetration is very small if the tachocline is laminar. (© 2005 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)
ALMA reveals the aftermath of a white dwarf–brown dwarf merger in CK Vulpeculae

We present Atacama Large Millimeter–Submillimeter Array (ALMA) observations of CK Vulpeculae which is identified with “Nova Vulpeculae 1670”. They trace obscuring dust in the inner regions of the associated nebulosity. The dust forms two cocoons, each extending ∼5″ north and south of the presumed location of the central star. Brighter emission is in a more compact east–west structure (2″ × 1″) where the cocoons intersect. We detect line emission in NH2CHO, CN, four organic molecules and C17O. CN lines trace bubbles within the dusty cocoons; CH3OH a north–south S–shaped jet; and other molecules a central cloud with a structure aligned with the innermost dust structure. The major axis of the overall dust and gas bubble structure has a projected inclination of ∼24° with respect to a 71″ extended “hourglass” nebulosity, previously seen in Hα. Three cocoon limbs align with dark lanes in the inner regions of the same Hα images. The central 2″ × 1″ dust is resolved into a structure consistent with a warped dusty disc. The velocity structure of the jets indicates an origin at the centre of this disc and precession with an unknown period. Deceleration regions at both the northern and southern tips of the jets are roughly coincident with additional diffuse dust emission over regions approximately 2″ across. These structures are consistent with a bipolar outflow expanding into surrounding high density material. We suggest that a white dwarf and brown dwarf merged between 1670 and 1672, with the observed structures and extraordinary isotopic abundances generated as a result.
ROSAT and ASCA Observations of the Crab-like Supernova Remnant N157B in the Large Magellanic Cloud

We report the results of ROSAT and ASCA X-ray observations of the supernova remnant N157B (or 30 Dor B, SNR 0539-69.1) in the Large Magellanic Cloud. For comparison, we also briefly describe the results on SNR 0540-69.3, the only confirmed Crab-like remnant in the Cloud. The X-ray emission from N157B can be decomposed into a bright comet-shaped feature, superposed on a diffuse emission region with a dimension of ~20 pc. The flat and nearly featureless spectrum of the remnant is distinctly different from those of young shell-like remnants, suggesting a predominantly Crab-like nature of N157B. Characterized by a power law with an energy slope of ~1.5, the spectrum of N157B above ~2 keV is, however, considerably steeper than that of SNR 0540-69.3, which has a slope of ~1.0. At lower energies, the spectrum of N157B presents marginal evidence for emission lines, which if real most likely arise in hot gas of the diffuse emission region. The hot gas has a characteristic thermal temperature of 0.4-0.7 keV. No significant periodic signal is detected from N157B in the period range of 3×10-3-2000 s. The pulsed fraction is ≲9% (99% confidence) in the 2-7 keV range. We discuss the nature of the individual X-ray components. In particular, we suggest that the synchrotron radiation of relativistic particles from a fast-moving (~103 km s-1) pulsar explains the size, morphology, spectrum, and energetics of the comet-shaped X-ray feature. We infer the age of the remnant as ~5 × 103 yr. The lack of radio polarization of the remnant may be due to Faraday dispersion by foreground H II gas.
Probing the structure of the cold dark matter halo using ancient mica

Mica can store (for {gt}1thinspGyr) etchable tracks caused by atoms recoiling from WIMPs. Ancient mica is a directional detector despite the complex motions it makes with respect to the WIMP {open_quotes}wind. {close_quotes} We can exploit the properties of directionality and long integration time to probe for structure in the dark matter halo of our galaxy. We compute a sample of possible signals in mica for a plausible model of halo structure. {copyright} {ital 1998} {ital The American Physical Society}
A Conceptual Model for Entrainment in Cumulus Clouds

Abstract Cumulus clouds are generally modeled as a plume, and the model works well up until the cloud base is encountered, beyond which the continuously entraining model does not appear appropriate. Although it has been known for a long time that cumulus clouds have very little lateral entrainment, the reason for it is not evident. An expression for the mean streamwise velocity profile as a Gaussian multiplied by a fourth-order polynomial factor is hereby proposed such that the mass and momentum fluxes are decoupled. This model suggests that cumulus clouds differ from other shear flows in that the former need not interact with the ambient for some downstream distance. The proposed model replicates a number of characteristics of cumulus clouds like a conserved mass flux with varying momentum flux, and may therefore be employed to describe them, in a time-averaged sense, beyond the cloud base.
Fully analytical solutions for Bondi accretion in galaxies with a central Black Hole

Abstract The fully analytical solution for isothermal Bondi accretion on a black hole (MBH) at the center of JJ two-component Jaffe (1983) galaxy models is presented. In JJ models the stellar and total mass density distributions are described by the Jaffe profile, with different scale-lengths and masses, and to which a central MBH is added; all the relevant stellar dynamical properties can also be derived analytically. In these new accretion solutions the hydrodynamical and stellar dynamical properties are linked by imposing that the gas temperature is proportional to the virial temperature of the stellar component. The formulae that are provided allow to evaluate all flow properties, and are then useful for estimates of the accretion radius and the mass flow rate when modeling accretion on MBHs at the center of galaxies.
Tracking down quirks at the Large Hadron Collider

Non-helical tracks are the smoking gun signature of charged and/or colored quirks, which are pairs of particles bound by a new, long-range confining force. We propose a method to efficiently search for these non-helical tracks at the LHC, without the need to fit their trajectories. We show that the hits corresponding to quirky trajectories can be selected efficiently by searching for co-planar hits in the inner layers of the ATLAS and CMS trackers, even in the presence of on average 50 pile-up vertices. We further argue that backgrounds from photon conversions and unassociated pile-up hits can be removed almost entirely, while maintaining a signal reconstruction efficiency as high as 70%. With the 300 fb$^{-1}$ dataset, this implies a discovery potential for string tension between 100 eV and 30 keV, and colored (electroweak charged) quirks as heavy as 1600 (650) GeV may be discovered.
Time variability of TeV cosmic ray sky map

The variation in the intensity of cosmic rays at small angular scales is attributed to the interstellar turbulence in the vicinity of the Solar system. We show that {a turbulent origin of the small-scale structures implies that} the morphology of the observed cosmic-ray intensity skymap varies with our location in the interstellar turbulence. The gyroradius of cosmic rays is shown to be the length scale associated with an observable change in the skymap over a radian angular scale. The extent to which the intensity \mpo{at a certain} angular scale varies is proportional to the change in our location with a maximum change of about the amplitude of intensity variation at that scale in the existing skymap. } We suggest that for TeV cosmic rays a measurable variation could occur over a time scale of a decade due to the Earth's motion through the interstellar medium, if interstellar turbulence persists down to the gyroradius, \mpo{about $00\ \mu\mathrm{pc}$ for TeV-ish cosmic rays}. Observational evidence of the variability, or an absence of it, could provide a useful insight into the physical origin of the small-scale anisotropy.
Empirical likelihood inference for parameters in a partially linear errors-in-variables model

In this paper, we consider the application of the empirical likelihood method to a partially linear model with measurement errors in the non-parametric part. It is shown that the empirical log-likelihood ratio at the true parameters converges to the standard chi-square distribution. Furthermore, we obtain the maximum empirical likelihood estimate of the unknown parameter by using the empirical log-likelihood ratio function, and the resulting estimator is shown to be asymptotically normal. Some simulations and an application are conducted to illustrate the proposed method.