Miracle-dz/UniFAR-FTUs huggingface dataset:
Measurement of the Higgs boson mass and e + e − → Z H cross section using Z → μ + μ − and Z → e + e − at the ILC

This paper presents a full simulation study of the measurement of the production cross section (${\ensuremath{\sigma}}_{ZH}$) of the Higgsstrahlung process ${e}^{+}{e}^{\ensuremath{-}}\ensuremath{\rightarrow}ZH$ and the Higgs boson mass (${M}_{\mathrm{H}}$) at the International Linear Collider (ILC), using events in which a Higgs boson recoils against a $Z$ boson decaying into a pair of muons or electrons. The analysis is carried out for three center-of-mass energies $\sqrt{s}=250$, 350, and 500 GeV, and two beam polarizations ${e}_{\mathrm{L}}^{\ensuremath{-}}{e}_{\mathrm{R}}^{+}$ and ${e}_{\mathrm{R}}^{\ensuremath{-}}{e}_{\mathrm{L}}^{+}$, for which the polarizations of ${e}^{\ensuremath{-}}$ and ${e}^{+}$ are $(P{e}^{\ensuremath{-}},P{e}^{+})=\phantom{\rule{0ex}{0ex}}(\ensuremath{-}80%,+30%)$ and ($+80%$, $\ensuremath{-}30%$), respectively. Assuming an integrated luminosity of $250\text{ }\text{ }{\mathrm{fb}}^{\ensuremath{-}1}$ for each beam polarization at $\sqrt{s}=250\text{ }\text{ }\mathrm{GeV}$, where the best lepton momentum resolution is obtainable, ${\ensuremath{\sigma}}_{ZH}$ and ${M}_{\mathrm{H}}$ can be determined with a precision of 2.5% and 37 MeV for ${e}_{\mathrm{L}}^{\ensuremath{-}}{e}_{\mathrm{R}}^{+}$ and 2.9% and 41 MeV for ${e}_{\mathrm{R}}^{\ensuremath{-}}{e}_{\mathrm{L}}^{+}$, respectively. Regarding a 20 year ILC physics program, the expected precisions for the HZZ coupling and ${M}_{\mathrm{H}}$ are estimated to be 0.4% and 14 MeV, respectively. The event selection is designed to optimize the precisions of ${\ensuremath{\sigma}}_{ZH}$ and ${M}_{\mathrm{H}}$ while minimizing the bias on the measured ${\ensuremath{\sigma}}_{ZH}$ due to discrepancy in signal efficiencies among Higgs decay modes. For the first time, model independence has been demonstrated to a sub-percent level for the ${\ensuremath{\sigma}}_{ZH}$ measurement at each of the three center-of-mass energies. The results presented show the impact of center-of-mass energy and beam polarization on the evaluated precisions and serve as a benchmark for the planning of the ILC run scenario.
Effects of Process Parameters on the Quality of Suantang Beef

Suantang beef is a traditional delicious Chinese food cooked in Suantang (ST, a sour soup fermented by microorganisms). However, the impact of ST on beef quality is unclear, and the process of ST beef lacks unified technical standards. In the presented study, we found that the additional amount of salt, cooking time, meat thickness, and beef–ST ratio significantly affect the quality of ST beef. After optimization, it was found that when salt addition was 1%, cooking time was 3 min, meat thickness was 2 cm, and beef–ST ratio was 40%, the color determined by colorimeter, texture determined by texture analyzer, and sensory scores of beef cooked by ST were improved compared with boiled beef. ST decreased the pH value and cathepsin L activity of beef, increased the content of organic acid, and changed the protein composition of beef. ST made the beef have higher hardness, and have better chewiness and cohesion. At the same time, ST reduced the disagreeable odors of beef and improved beef flavor. In addition, 88 volatile compounds were detected in ST beef by HS-SPME/GC-MS. According to odor, threshold, and odor activity value (OAV), 24 critical aroma-active compounds were confirmed in ST beef. This study provides a basis for the potential industrialized production of ST beef.
Biases in, and corrections to, KSB shear measurements

We analyse the Kaiser–Squires–Broadhurst (KSB) method to estimate gravitational shear from surface-brightness moments of small and noisy galaxy images. We identify three potentially problematic assumptions. These are as follows. (1) While gravitational shear must be estimated from averaged galaxy images, KSB derives a shear estimate from each individual image and then takes the average. Since the two operations do not commute, KSB gives biased results. (2) KSB implicitly assumes that galaxy ellipticities are small, while weak gravitational lensing only assures that the change in ellipticity due to the shear is small. (3) KSB does not invert the convolution with the point spread function (PSF), but gives an approximate PSF correction which – even for a circular PSF – holds only in the limit of circular sources. The effects of assumptions (2) and (3) partially counteract in a way dependent on the width of the weight function and of the PSF. We quantitatively demonstrate the biases due to all assumptions, extend the KSB approach consistently to third order in the shear and ellipticity and show that this extension lowers the biases substantially. The issue of proper PSF deconvolution will be addressed in Melchior et al.
SUBMILLIMETER AND MOLECULAR VIEWS OF THREE GALACTIC RING-LIKE H ii REGIONS

We use SCUBA 850 μm and CO observations to analyze the surroundings of three Galactic ring-like H ii regions, KR 7, KR 81, and KR 120 (Sh 2-124, Sh 2-165, and Sh 2-187), with the aim of finding sites of triggered star formation. We find one prominent submillimeter (sub-mm) source for each region, located at the interface between the H ii region and its neutral surroundings. Using Two Micron All Sky Survey photometry, we find that the prominent sub-mm source for KR 120 probably contains an embedded cluster of young stellar objects (YSOs), making it a likely site for triggered star formation. The KR 7 sub-mm source could possibly contain embedded YSOs, while the KR 81 sub-mm source likely does not. The mass column densities for these dominant sub-mm sources fall in the ∼0.1–0.6 g cm−2 range. The mass of the cold, dense material (clumps) seen as the three dominant sub-mm sources falls around ∼100 M☉. We use the SCUBA Legacy catalog to characterize the populations of sub-mm sources around the H ii regions, and compare them to the sources found around a previously studied similar ring-like H ii region (KR 140) and near a massive star-forming region (W3). Finally, we estimate the IR luminosities of the prominent newly detected sub-mm sources and find that they are correlated with the clump mass, consistent with a previously known luminosity–mass relationship which this study shows to be valid over four orders of magnitude in mass.
Single-cell transcriptomic atlas of mouse cochlear aging

Abstract Progressive functional deterioration in the cochlea is associated with age-related hearing loss (ARHL). However, the cellular and molecular basis underlying cochlear aging remains largely unknown. Here, we established a dynamic single-cell transcriptomic landscape of mouse cochlear aging, in which we characterized aging-associated transcriptomic changes in 27 different cochlear cell types across five different time points. Overall, our analysis pinpoints loss of proteostasis and elevated apoptosis as the hallmark features of cochlear aging, highlights unexpected age-related transcriptional fluctuations in intermediate cells localized in the stria vascularis (SV) and demonstrates that upregulation of endoplasmic reticulum (ER) chaperon protein HSP90AA1 mitigates ER stress-induced damages associated with aging. Our work suggests that targeting unfolded protein response pathways may help alleviate aging-related SV atrophy and hence delay the progression of ARHL.
Graphene nanoribbons subjected to axial stress

Atomistic simulations are used to study the bending of rectangular graphene nano ribbons subjected to axial stress both for free boundary and supported boundary conditions. The shape of the deformations of the buckled graphene nano ribbons, for small values of the stress, are sine waves where the number of nodal lines depend on the longitudinal size of the system and the applied boundary condition. The buckling strain for the supported boundary condition is found to be independent of the longitudinal size and estimated to be 0.86%. From a calculation of the free energy at finite temperature we find that the equilibrium projected two-dimensional area of the graphene nano ribbon is less than the area of a flat sheet. At the optimum length the boundary strain for the supported boundary condition is 0.48%.
Performance optimization of radio over fiber system using particle swarm optimization algorithm against cross-phase modulation crosstalk

Abstract. In this paper, the particle swarm optimization (PSO) algorithm is used to optimize the performance of a radio over fiber system against cross-phase modulation (XPM) crosstalk by finding the optimum value of crosstalk by independently considering the range of various fiber parameters in the V band (40 to 75 GHz) and W band (75 to 110 GHz). Results show that, without using any optimization technique, the crosstalk is found to be minimum at the small frequency in both frequency bands. Without optimization, XPM crosstalk is found to be −62.2, −56.2, and −52.7 dB at 40 GH, 75 and 110 GHz, respectively, at the fiber length of 20 km, whereas after PSO, XPM crosstalk is −65.4 and −71.9 dB at 75 and 110 GHz, respectively, at the high fiber length of 50 km. After applying the PSO optimization technique, XPM crosstalk is optimized with the minimum at high frequencies in both frequency bands at large fiber lengths. It is found that XPM is optimized at different values of the dispersion parameter without the use of a dispersion-shifted fiber. Joint optimization is also done for the complete range of frequencies from 40 to 110 GHz, and optimized crosstalk is obtained independently at high frequencies and large fiber lengths in both frequency bands. From the results, it can be seen that a radio-over-fiber system can be designed by choosing a single-mode fiber with the optimized parameter value. The XPM crosstalk keeps increasing with the increase in the length of the fiber and frequency, and PSO was used to counter the crosstalk by optimizing the various fiber parameter values.
A sensor fusion method of radar and camera

In autonomous vehicles, vehicle perception is very important for vehicle behavior planning and execution. In order to solve the problem that it is difficult to use a single sensor in autonomous driving to cope with the complex driving environment, and in the traditional method of lidar and camera fusion, lidar is affected by the weather environment, resulting in serious signal attenuation, short laser detection distance, high price and large amount of data calculation. In this paper, a method for fusion of radar and camera is proposed. In this method, two radars are selected to detect the object and obtain the speed, distance, angle and other information of the object. In terms of vision, the object category is obtained through yolov3 algorithm, and the object information detected by the radar is mapped to the image after semantic segmentation through spatial coordinate transformation, finally, the sensor joint detection model is established by k-nearest neighbor method, and the fused target detection results are obtained. Compared with the fusion method of lidar and camera, this method has the advantages of low cost, small amount of data calculation, strong anti-jamming ability, and can meet the requirements of real-time and accuracy in performance.
THE XMM-NEWTON X-RAY SPECTRA OF THE MOST X-RAY LUMINOUS RADIO-QUIET ROSAT BRIGHT SURVEY-QSOs: A REFERENCE SAMPLE FOR THE INTERPRETATION OF HIGH-REDSHIFT QSO SPECTRA

We present the broadband X-ray properties of four of the most X-ray luminous (LX ⩾ 1045 erg s−1 in the 0.5–2 keV band) radio-quiet QSOs found in the ROSAT Bright Survey. This uniform sample class, which explores the extreme end of the QSO luminosity function, exhibits surprisingly homogenous X-ray spectral properties: a soft excess with an extremely smooth shape containing no obvious discrete features, a hard power law above 2 keV, and a weak narrow/barely resolved Fe Kα fluorescence line for the three high signal-to-noise ratio (S/N) spectra. The soft excess can be well fitted with only a soft power law. No signatures of warm or cold intrinsic absorbers are found. The Fe Kα centroids and the line widths indicate emission from neutral Fe (E = 6.4 keV) originating from cold material from distances of only a few light days or further out. The well-constrained equivalent widths (EW) of the neutral Fe lines are higher than expected from the X-ray Baldwin effect which has been only poorly constrained at very high luminosities. Taking into account our individual EW measurements, we show that the X-ray Baldwin effect flattens above LX ∼ 1044 erg s−1 (2–10 keV band) where an almost constant 〈EW〉 of ∼100 eV is found. We confirm the assumption of having very similar X-ray active galactic nucleus properties when interpreting stacked X-ray spectra. Our stacked spectrum serves as a superb reference for the interpretation of low S/N spectra of radio-quiet QSOs with similar luminosities at higher redshifts routinely detected by XMM-Newton and Chandra surveys.
THE LONG-TERM EVOLUTION OF DOUBLE WHITE DWARF MERGERS

In this paper, we present a model for the long-term evolution of the merger of two unequal mass C/O white dwarfs (WDs). After the dynamical phase of the merger, magnetic stresses rapidly redistribute angular momentum, leading to nearly solid-body rotation on a viscous timescale of 10−4–1 yr, long before significant cooling can occur. Due to heating during the dynamical and viscous phases, the less massive WD is transformed into a hot, slowly rotating, and radially extended envelope supported by thermal pressure. Following the viscous phase of evolution, the maximum temperature near the envelope base may already be high enough to begin off-center convective carbon burning. If not, Kelvin–Helmholtz contraction of the inner region of the envelope on a thermal timescale of 103–104 yr compresses the base of the envelope, again yielding off-center burning. As a result, the long-term evolution of the merger remnant is similar to that seen in previous calculations: the burning shell diffuses inward over ∼104 yr, eventually yielding a high-mass O/Ne WD or a collapse to a neutron star, rather than a Type Ia supernova. During the cooling and shell-burning phases, the merger remnant radiates near the Eddington limit. Given the double WD merger rate of a few per 1000 yr, a few dozen of these ∼1038 erg s−1 sources should exist in a Milky Way type galaxy. While the end result is similar to that of previous studies, the physical picture and the dynamical state of the matter in our model differ from previous work. Furthermore, substantial remaining uncertainties related to the convective structure near the photosphere and mass loss during the thermal evolution may significantly affect our conclusions. Thus, future work within the context of the physical model presented here is required to better address the eventual fate of double WD mergers, including those for which one or both of the components is a He WD.
New constraints on the polarization of anomalous microwave emission in nearby molecular clouds

Anomalous microwave emission (AME) has been previously studied in two well-known molecular clouds and is thought to be due to electric dipole radiation from small spinning dust grains. It is important to measure the polarization properties of this radiation both for component separation in future cosmic microwave background (CMB) experiments and also to constrain dust models. We have searched for linearly polarized radio emission associated with the ? � Ophiuchi and Perseus molecular clouds using WMAP 7-year data. We found no significant polarization within an aperture of 2�? diameter. The upper limits on the fractional polarization of spinning dust in the ? � Ophiuchi cloud are 1.7, 1.6 and 2.6 per cent (at 95 per cent confidence level) at K, Ka and Q bands, respectively. In the Perseus cloud we derived upper limits of 1.4, 1.9 and 4.7 per cent, at K, Ka and Q bands, respectively; these are similar to those found by L? pez-Caraballo et al. If AME at high Galactic latitudes has a similarly low level of polarization, this will simplify component separation for CMB polarization measurements. We can also rule out single domain magnetic dipole radiation as the dominant emission mechanism for the 20-40 GHz. The polarization levels are consistent with spinning dust models.
Dynamics of spontaneous emission in a single-end photonic waveguide

We investigate the spontaneous emission of a two-level system, e.g. an atom or atomlike object, coupled to a single-end, i.e., semi-infinite, one-dimensional photonic waveguide such that one end behaves as a perfect mirror while light can pass through the opposite end with no back-reflection. Through a quantum microscopic model we show that such geometry can cause non-exponential and long-lived atomic decay. Under suitable conditions, a bound atom-photon stationary state appears in the atom-mirror interspace so as to trap a considerable amount of initial atomic excitation. Yet, this can be released by applying an atomic frequency shift causing a revival of photon emission. The resilience of such effects to typical detrimental factors is analyzed.
Dust size distributions in coagulation/fragmentation equilibrium: numerical solutions and analytical fits

Context. Grains in circumstellar disks are believed to grow by mutual collisions and subsequent sticking due to surface forces. Results of many fields of research involving circumstellar disks, such as radiative transfer calculations, disk chemistry, magneto-hydrodynamic simulations largely depend on the unknown grain size distribution. Aims. As detailed calculations of grain growth and fragmentation are both numerically challenging and computationally expensive, we aim to find simple recipes and analytical solutions for the grain size distribution in circumstellar disks for a scenario in which grain growth is limited by fragmentation and radial drift can be neglected. Methods. We generalize previous analytical work on self-similar steady-state grain distributions. Numerical simulations are carried out to identify under which conditions the grain size distributions can be understood in terms of a combination of power-law distributions. A physically motivated fitting formula for grain size distributions is derived using our analytical predictions and numerical simulations. Results. We find good agreement between analytical results and numerical solutions of the Smoluchowski equation for simple shapes of the kernel function. The results for more complicated and realistic cases can be fitted with a physically motivated "black box" recipe presented in this paper. Our results show that the shape of the dust distribution is mostly dominated by the gas surface density (not the dust-to-gas ratio), the turbulence strength and the temperature and does not obey an MRN type distribution.
Impact of baryonic streaming velocities on the formation of supermassive black holes via direct collapse

Baryonic streaming motions produced prior to the epoch of recombination became supersonic during the cosmic dark ages. Various studies suggest that such streaming velocities change the halo statistics and also influence the formation of Population III stars. In this study, we aim to explore the impact of streaming velocities on the formation of supermassive black holes at z > 10 via the direct collapse scenario. To accomplish this goal, we perform cosmological large eddy simulations for two halos of a few times 10 7 M⊙ with initial streaming velocities of 3, 6 and 9 km/s. These massive primordial halos illuminated by the strong Lyman Werner flux are the potential cradles for the formation of direct collapse seed black holes. To study the evolution for longer times, we employ sink particles and track the accretion for 10,000 years. Our findings show that higher streaming velocities increase the circular velocities from about 14 km/s to 16 km/s. They also delay the collapse of halos for a few million years, but do not have any significant impact on the halo properties such as turbulent energy, radial velocity, density and accretion rates. Sink particles of about ∼ 10 5 M⊙ are formed at the end of our simulations and no clear distribution of sink masses is observed in the presence of streaming motions. It is further found that the impact of streaming velocities is less severe in massive halos compared to the minihalos as reported in the previous studies.
Pressure-induced reversible phase transition and amorphization of CH$_3$NH$_3$PbI$_3$

Recent advances of highly efficient solar cells based on organic-inorganic halide perovskites have triggered intense research efforts to establish the fundamental properties of these materials. In this work, we utilized diamond anvil cell to investigate the pressure-induced structural and electronic transformations in methylammonium lead iodide (CH$_3$NH$_3$PbI$_3$) up to 7 GPa at room temperature. The synchrotron X-ray diffraction experiment show that the sample transformed from tetragonal to orthorhombic phase at 0.3 GPa and amorphized above 4 GPa. Further high pressure IR spectroscopy experiments illustrated the high pressure behavior of organic (CH$_3$NH$_3$)$^+$ cations. We also analyzed the pressure dependence of the band gap energy based on the optical absorption and photoluminescence (PL) results. Moreover, all the observed changes were fully reversible when the pressure was completely released. Our in situ high pressure studies provide essential information for the intrinsic properties and stability of organic-inorganic halide perovskites, which significantly affect the performance of perovskite solar cells.
Restricted three-body problem in effective-field-theory models of gravity

One of the outstanding problems of classical celestial mechanics was the restricted 3-body prob- lem, in which a planetoid of small mass is subject to the Newtonian attraction of two celestial bodies of large mass, as it occurs, for example, in the sun-earth-moon system. On the other hand, over the last decades, a systematic investigation of quantum corrections to the Newtonian potential has been carried out in the literature on quantum gravity. The present paper studies the effect of these tiny quantum corrections on the evaluation of equilibrium points. It is shown that, despite the extreme smallness of the corrections, there exists no choice of sign of these corrections for which all qualitative features of the restricted 3-body problem in Newtonian theory remain unaffected. Moreover, first-order stability of equilibrium points is characterized by solving a pair of algebraic equations of fifth degree, where some coefficients depend on the Planck length. The coordinates of stable equilibrium points are slightly changed with respect to Newtonian theory, because the planetoid is no longer at equal distance from the two bodies of large mass. The effect is conceptually interesting but too small to be observed, at least for the restricted 3-body problems available in the solar system.
The Wild, Elusive Singularities of the T-fractal Surface

We give a rigorous definition of the T-fractal translation surface, and describe some its basic geometric and dynamical properties. In particular, we study the singularities attached to the surface by its metric completion and show there exists a Cantor set of "elusive singularities. " We show these elusive singularities can be thought of as a generalization of the wild singularities introduced by Bowman and Valdez. In particular, we show that every elusive singularities has an infinite discrete set of rotational components.