Miracle-dz/UniFAR-FTUs huggingface dataset:
AN UNEXPECTEDLY LOW-REDSHIFT EXCESS OF SWIFT GAMMA-RAY BURST RATE

Gamma-ray bursts (GRBs) are the most violent explosions in the universe and can be used to explore the properties of the high-redshift universe. It is believed that long GRBs are associated with the deaths of massive stars. Therefore, it is possible to use GRBs to investigate the star formation rate (SFR). In this paper, we use Lynden-Bell’s c − ? > method to study the luminosity function and rate of Swift long GRBs without any assumptions. We find that the luminosities of GRBs evolve with redshift as L ( z ) ∝ g ( z ) = ( 1 + z ) k ? > with k = 2.43 − 0.38 + 0.41 ? > . After correcting the redshift evolution through L 0 ( z ) = L ( z ) / g ( z ) ? > , the luminosity function can be expressed as &psgr; ( L 0 ) ∝ L 0 − 0.14 ± 0.02 ? > for dim GRBs and &psgr; ( L 0 ) ∝ L 0 − 0.70 ± 0.03 ? > for bright GRBs, with the break point L 0 b = 1.43 × 10 51 erg s − 1 ? > . We also find that the formation rate of GRBs is almost constant at z < 1.0 ? > for the first time, which is remarkably different from the SFR. At z > 1.0 ? > , the formation rate of GRBs is consistent with the SFR. Our results are dramatically different from previous studies. We discuss a few possible reasons for this low-redshift excess. We also test the robustness of our results using Monte Carlo simulations. The distributions of mock data (i.e., luminosity–redshift distribution, luminosity function, cumulative distribution, and log N–log S distribution) are in good agreement with observations. Also, we find that there are remarkable differences between the mock data and the observations if long GRBs are unbiased tracers of SFR at z < 1.0 ? > .
Periodicities in sunspot activity during solar cycle 23

Aims. The data of sunspot numbers, sunspot areas and solar flare index during cycle 23 are analyzed to investigate the intermediate-term periodicities. Methods. Power spectral analysis has been performed separately for the data of the whole disk, northern and southern hemispheres of the Sun. Results. Several significant midrange periodicities (∼175, 133, 113, 104, 84, 63 days) are detected in sunspot activity. Most of the periodicities in sunspot numbers generally agree with those of sunspot areas during the solar cycle 23. The study reveals that the periodic variations in the northern and southern hemispheres of the Sun show a kind of asymmetrical behavior. Periodicities of ∼175 days and ∼133 days are highly significant in the sunspot data of northern hemisphere showing consistency with the findings of Lean (1990) during solar cycles 12-21. On the other hand, southern hemisphere shows a strong periodicity of about 85 days in terms of sunspot activity. The analysis of solar flare index data of the same time interval does not show any significant peak. The different periodic behavior of sunspot and flare activity can be understood in the light of hypothesis proposed by Ballester et al. (2002), which suggests that during cycle 23, the periodic emergence of magnetic flux partly takes place away from developed sunspot groups and hence may not necessarily increase the magnetic complexity of sunspot groups that leads to the generation of flares.
Peculiar glitch of PSR J1119−6127 and extension of the vortex creep model

Glitches are sudden changes in rotation frequency and spin-down rate, observed from pulsars of all ages. Standard glitches are characterized by a positive step in angular velocity (Delta Omega > 0) and a negative step in the spin-down rate (Delta Omega < 0) of the pulsar. There are no glitch-associated changes in the electromagnetic signature of rotation-powered pulsars in all cases so far. For the first time, in the last glitch of PSR J1119-6127, there is clear evidence for changing emission properties coincident with the glitch. This glitch is also unusual in its signature. Further, the absolute value of the spin-down rate actually decreases in the long term. This is in contrast to usual glitch behaviour. In this paper we extend the vortex creep model in order to take into account these peculiarities. We propose that a starquake with crustal plate movement towards the rotational poles of the star induces inward vortex motion which causes the unusual glitch signature. The component of the magnetic field perpendicular to the rotation axis will decrease, giving rise to a permanent change in the pulsar external torque.
Higgs Bosons at Muon Colliders

We review the role of a muon collider in the study of Higgs bosons via production in the s-channel. Very precise measurements of a Standard Model-like Higgs boson mass and total width can be performed, and may lead to a discrimination between a Standard Model Higgs boson and the light Higgs boson of the minimal supersymmetric theory. The heavier Higgs bosons from a supersymmetric theory or an exotic Higgs sector can be studied in the s-channel. A muon collider may play a crucial role in separating the overlapping signals for two heavy nearly degenerate Higgs bosons, and may play an important role in precision tests of radiative corrections in the Higgs sector. The measurements at a muon collider will be complementary to the Higgs studies at the Large Hadron Collider and at an electron-positron Linear Collider.
Effect of elevated ozone and carbon dioxide on growth and yield of rice (Oryza sativa)

An experiment was conducted by growing Pusa 44 rice (Oryza sativa L.) variety under different treatments: Ambient, Elevated O3 (EO3: 60 ± 10 ppb), Elevated CO2 (ECO2: 550 ± 10 ppm) and Elevated CO2 and O3 (550 ± 10 ppm CO2 and 60 ± 10 ppb EO3) in free air carbon dioxide and ozone enrichment facility (FACE-O3) with the objective to assess the impact of elevated tropospheric ozone (O3) and carbon dioxide (CO2) interaction on growth and yield of rice. The crop was exposed to elevated levels of gases from transplanting to maturity. EO3 was found to be having a negative impact on all the growth parameters at vegetative, anthesis and maturity stages. ECO2 was found to be having a compensatory effect over EO3 for the different growth parameters. On an average the compensatory effect of ECO2 over EO3 on yield was about 40% and negative impact of elevated O3 over control was around 26% in both the years.
SPECTRAL ENERGY DISTRIBUTION MAPPING OF TWO ELLIPTICAL GALAXIES ON SUB-kpc SCALES

We use high-resolution Herschel-PACS data of two nearby elliptical galaxies, IC 1459 and NGC 2768, to characterize their dust and stellar content. IC 1459 and NGC 2768 have an unusually large amount of dust for elliptical galaxies ((1–3) × 105 ); this dust is also not distributed along the stellar content. Using data from GALEX (ultra-violet) to PACS (far-infrared, FIR), we analyze the spectral energy distribution (SED) of these galaxies with CIGALEMC as a function of the projected position, binning images in 7. ″2 pixels. From this analysis, we derive maps of SED parameters, such as the metallicity, the stellar mass, the fraction of young stars, and the dust mass. The larger amount of dust in FIR maps seems related in our model to a larger fraction of young stars which can reach up to 4% in the dustier area. The young stellar population is fitted as a recent (∼0.5 Gyr) short burst of star formation for both galaxies. The metallicities, which are fairly large at the center of both galaxies, decrease with the radial distance with a fairly steep gradient for elliptical galaxies.
K-mouflage effects on clusters of galaxies

We investigate the effects of a K-mouflage modification of gravity on the dynamics of clusters of galaxies. We extend the description of K-mouflage to situations where the scalar field responsible for the modification of gravity is coupled to a perfect fluid with pressure. We describe the coupled system at both the background cosmology and cosmological perturbations levels, focusing on cases where the pressure emanates from small-scale nonlinear physics. We derive these properties in both the Einstein and Jordan frames, as these two frames already differ by a few percents at the background level for K-mouflage scenarios, and next compute cluster properties in the Jordan frame that is better suited to these observations. Galaxy clusters are not screened by the K-mouflage mechanism and therefore feel the modification of gravity in a maximal way. This implies that the halo mass function deviates from $\Lambda$-CDM by a factor of order one for masses $M\gtrsim 10^{14} \ h^{-1} M_\odot$. We then consider the hydrostatic equilibrium of gases embedded in galaxy clusters and the consequences of K-mouflage on the X-ray cluster luminosity, the gas temperature, and the Sunyaev-Zel'dovich effect. We find that the cluster temperature function, and more generally number counts, are largely affected by K-mouflage, mainly due to the increased cluster abundance in these models. Other scaling relations such as the mass-temperature and the temperature-luminosity relations are only modified at the percent level due to the constraints on K-mouflage from local Solar System tests.
Cosmic-ray propagation with DRAGON2: I. numerical solver and astrophysical ingredients

We present version 2 of the DRAGON code designed for computing realistic predictions of the CR densities in the Galaxy. The code numerically solves the interstellar CR transport equation (including inhomogeneous and anisotropic diffusion, either in space and momentum, advective transport and energy losses), under realistic conditions. The new version includes an updated numerical solver and several models for the astrophysical ingredients involved in the transport equation. Improvements in the accuracy of the numerical solution are proved against analytical solutions and in reference diffusion scenarios. The novel features implemented in the code allow to simulate the diverse scenarios proposed to reproduce the most recent measurements of local and diffuse CR fluxes, going beyond the limitations of the homogeneous galactic transport paradigm. To this end, several applications using DRAGON2 are presented as well. This new version facilitates the users to include their own physical models by means of a modular C++ structure.
V473 Lyrae, a unique second-overtone Cepheid with two modulation cycles

V473 Lyrae is the only Galactic Cepheid with confirmed periodic amplitude and phase variations similar to the Blazhko effect observed in RR Lyrae stars. We collected all available photometric data and some radial velocity measurements to investigate the nature of the modulation. The comparison of the photometric and radial velocity amplitudes confirmed that the star pulsates in the second overtone. The extensive data set, spanning more than 40 years, allowed us to detect a secondary modulation cycle with a period of approximately 5300 days or 14.5 years. The secondary variations can be detected in the period of the primary modulation, as well. Phenomenologically, the light variations are analogous to the Blazhko effect. To find a physical link, we calculated linear hydrodynamic models to search for potential mode resonances that could drive the modulation and found two viable half-integer (n:2) and three n:4 resonances between the second overtone and other modes. If any of these resonances will be confirmed by non-linear models, it may confirm the mode resonance model, a common mechanism that can drive modulations both in RR Lyrae and Cepheid stars.
Lectures on instantons

This is a self-contained set of lecture notes on instantons in (super) Yang-Mills theory in four dimensions and in quantum mechanics. First the basics are derived from scratch: the regular and singular one-instanton solutions for Yang-Mills theories with gauge groups SU(2) and SU(N), their bosonic and fermionic zero modes, the path integral instanton measure, and supersymmetric Yang-Mills theories in Euclidean space. Then we discuss applications: the \theta-angle of QCD, the solution of the U(1) problem, the way Higgs fields solve the large-instanton problem, and tunneling and phase transitions in quantum mechanics and in nonabelian gauge theories. These lecture notes are an extension of a review on Yang-Mills and D-instantons written in 2000 by both authors and A.Belitsky
Effects on Autophagy of Moxibustion at Governor Vessel Acupoints in APP/PS1double-Transgenic Alzheimer's Disease Mice through the lncRNA Six3os1/miR-511-3p/AKT3 Molecular Axis

Objective To explore the effect and mechanism of moxibustion at acupoints of the governor vessel on lncRNA Six3os1 in amyloid precursor protein/presenilin1 (APP/PS1) double-transgenic Alzheimer's disease (AD) mice. Methods Twenty-four specific pathogen-free and APP/PS1 double-transgenic male mice were randomly allocated into the AD model and moxibustion groups, with 12 cases in each group. Twelve syngeneic C57BL/6J mice were selected as the control group. Mice in the moxibustion group received aconite cake-separated moxibustion at the Baihui acupoint. Suspension moxibustion was applied at Fengfu and Dazhui for 15 minutes each day. All treatments were conducted over two weeks. Control and AD model mice were routinely fed without any intervention. Behavioral observation tests were conducted before and after the intervention. The autophagosome in the hippocampus was observed using transmission electron microscopy. Immunohistochemistry was performed to detect Aβ1-42 expression. LC3B and P62 expressions were evaluated by immunofluorescence. The expression levels of the lncRNAs Six3os1, miR-511-3p, and AKT3 were detected by qRT-PCR. The differential expression of PI-3K, AKT3, mTOR, LC3B-II/I, and P62 proteins in the hippocampus was detected by western blot. The dual-luciferase assay was undertaken to examine the targeting relationships of the lncRNAs Six3os1, miR-511-3p, and AKT3. Results Compared with the control group, the AD model showed higher escape latency in the Morris Water Maze and reduced autophagic vacuoles in the cytoplasm of hippocampal neurons (both p < 0.01). Compared with the control group, the AD model showed higher expression of Aβ1-42, the lncRNAs Six3os1, PI-3K, mTOR, P62, and AKT3 protein (all p < 0.01); but lower mir-511-3p and LC3B (both p < 0.01). Compared with the AD model group, the moxibustion group had a shorter escape latency, more autophagic bubbles in the hippocampus, and lower expression of positive Aβ1-42, the lncRNAs Six3os1, PI-3K, mTOR, P62, and AKT3 protein (all p < 0.01). In contrast, the levels of miR-511-3p and LC3B proteins were considerably increased in the moxibustion group compared to the AD model group (both p < 0.01). Based on the dual-luciferase assay, there was a targeting link among the lncRNAs Six3os1, miR-511-3p, and AKT3. Conclusion Moxibustion at acupoints of the governor vessel can suppress the lncRNA Six3os1 expression, promote cell autophagy, accelerate Aβ1-42 clearance and alleviate cognitive dysfunction of AD mediated by the PI3K/AKT/mTOR signaling pathway through the lncRNA Six3os1/miR-511-3p/AKT3 axis.
Analytical formulation of lunar cratering asymmetries

Context. The cratering asymmetry of a bombarded satellite is related to both its orbit and impactors. The inner solar system impactor populations, that is, the main-belt asteroids (MBAs) and the near-Earth objects (NEOs), have dominated during the late heavy bombardment (LHB) and ever since, respectively. Aims. We formulate the lunar cratering distribution and verify the cratering asymmetries generated by the MBAs as well as the NEOs. Methods. Based on a planar model that excludes the terrestrial and lunar gravitations on the impactors and assuming the impactor encounter speed with Earth v enc is higher than the lunar orbital speed v M , we rigorously integrated the lunar cratering distribution, and derived its approximation to the first order of v M / v enc . Numerical simulations of lunar bombardment by the MBAs during the LHB were performed with an Earth–Moon distance a M = 20−60 Earth radii in five cases. Results. The analytical model directly proves the existence of a leading/trailing asymmetry and the absence of near/far asymmetry. The approximate form of the leading/trailing asymmetry is (1 + A 1 cos β ), which decreases as the apex distance β increases. The numerical simulations show evidence of a pole/equator asymmetry as well as the leading/trailing asymmetry, and the former is empirically described as (1 + A 2 cos2 ϕ ), which decreases as the latitude modulus | ϕ | increases. The amplitudes A 1,2 are reliable measurements of asymmetries. Our analysis explicitly indicates the quantitative relations between cratering distribution and bombardment conditions (impactor properties and the lunar orbital status) like A 1 ∝ v M / v enc , resulting in a method for reproducing the bombardment conditions through measuring the asymmetry. Mutual confirmation between analytical model and numerical simulations is found in terms of the cratering distribution and its variation with a M . Estimates of A 1 for crater density distributions generated by the MBAs and the NEOs are 0.101−0.159 and 0.117, respectively.
Excitation entanglement entropy in two dimensional conformal field theories

We analyze how excitations affect the entanglement entropy for an arbitrary entangling interval in a 2d conformal field theory (CFT) using the holographic entanglement entropy techniques as well as direct CFT computations. We introduce the excitation entanglement entropy.hS, the difference between the entanglement entropy generic excitations and their arbitrary conformal descendants denoted through h. The excitation entanglement entropy, unlike the entanglement entropy, is a finite quantity (independent of the cutoff), and hence a good physical observable. We show that the excitation entanglement entropy for any given interval is uniquely specified by a local second order differential equation sourced by the one point function of the energy momentum tensor computed in the excited background state, and two boundary and smoothness conditions. We analyze low and high temperature behavior of the excitation entanglement entropy and show that Delta S-h grows as a function of temperature. We prove an "integrated positivity" for the excitation entanglement entropy, that although Delta S-h can be positive or negative, its average value is always positive. We also discuss the mutual and multipartite information and (strong) subadditivity inequality in the presence of generic excitations and their conformal descendants.
Sarcopenia is associated with mortality in patients with COVID-19 independent of other demographic risk factors

Objectives: To investigate whether sarcopenia had an effect on in-hospital mortality independent from other demographic characteristics in patients with Coronavirus disease 2019 (COVID-19), and to determine a reliable cut-off value for sarcopenia if there is such a relationship. Methods: A total of 302 patients with COVID-19 were included in the study. Sarcopenia was assessed by indexed skeletal muscle mass at T12 vertebrae level (T12-SMI) on initial chest computed tomography (CT). A receiver operating characteristic (ROC) curve analysis was performed to detect a cut-off value of T12-SMI for mortality prediction. Then, sarcopenia was diagnosed by this value. Multivariable logistic regression analysis was used to detect independent variables for mortality. Results: Patients were separated into groups; 26 (8.6%) patients in the mortality group and 276 (91.4%) patients in the no-mortality group. In ROC analysis, cut-off values of 34.06 cm²/m² (sensitivity: 70%, specificity: 77%) in males and 29.36 cm²/m² (sensitivity: 67%, specificity: 69%) in females for T12-SMI were computed for mortality prediction. There were 110 (36.4%) patients with sarcopenia. Sarcopenia was more frequent in the mortality group than the no-mortality group (73.1% vs 33%, p < 0.001). In multivariate analysis age, previous cardiovascular and respiratory disease, and sarcopenia were independently associated with mortality in COVID-19 patients. Conclusions: A cut-off value of 34.06 cm²/m² in males and 29.36 cm²/m² in females for T12-SMI can be used to diagnose sarcopenia in patients with COVID-19. Sarcopenia is clearly associated with mortality in these patients.
Worldwide site comparison for submillimetre astronomy

Aims. The most important limitation for ground-based submillimetre (submm) astronomy is the broad-band absorption of the total water vapour in the atmosphere above an observation site, often expressed as the precipitable water vapour (PWV). A long-term statistic on the PWV is thus mandatory to characterize the quality of an existing or potential site for observational submm-astronomy. In this study we present a three-year statistic (2008–2010) of the PWV for ground-based telescope sites all around the world and for stratospheric altitudes relevant for SOFIA (Stratospheric Observatory for Far-Infrared Astronomy). The submm-transmission is calculated for typical PWVs using an atmospheric model. Methods. We used data from IASI (Infrared Atmospheric Sounding Interferometer) on the Metop-A satellite to retrieve water vapour profiles for each site (11 in total, comprising Antarctica, Chile, Mauna Kea, Greenland, Tibet). The use of a single instrument to make the comparison provides unbiased data with a common calibration method. The profiles are integrated above the mountain/stratospheric altitude to get an estimation of the PWV. We then applied the atmospheric model MOLIERE (Microwave Observation and LIne Estimation and REtrieval) to compute the corresponding atmospheric absorption for wavelengths between 150 μm and 3 mm. Results. We present the absolute PWV values for each site sorted by year and time percentage. The PWV corresponding to the first decile (10%) and the quartiles (25%, 50%, 75%) are calculated and transmission curves between 150 μm and 3 mm for these values are shown. The Antarctic and South-American sites present very good conditions for submillimetre astronomy. The 350 μm and 450 μm atmospheric windows are open all year long, whereas the 200 μm atmospheric window opens reasonably for 25% of the time in Antarctica and the extremely high-altitude sites in Chile. Potential interesting new facilities are Macon in Argentina and Summit in Greenland, which show similar conditions to for example, Mauna Kea (Hawaii). For SOFIA, we present transmission curves for different altitudes (11 to 14 km), PWV values, and higher frequencies (up to 5 THz) in more detail. Though the atmosphere at these altitude is generally very transparent, the absorption at very high frequencies becomes more important, partly caused by minor species. The method presented in this paper could identify sites on Earth, with great potential for submillimetre astronomy, and guide future site testing campaigns in situ.