Miracle-dz/UniFAR-FTUs huggingface dataset:
First-year Sloan Digital Sky Survey-II supernova results: consistency and constraints with other intermediate-redshift data sets

ABSTRACT We present an analysis of the luminosity distances of Type Ia Supernovae (SNe) from the Sloan Digital Sky Survey-II (SDSS-II) SN Survey in conjunction with other intermediate-redshift (z 97 per cent level from this single data set. We find good agreement between the SN and BAO distance measurements, both consistent with a Λ-dominated cold dark matter cosmology, as demonstrated through an analysis of the distance duality relationship between the luminosity (dL) and angular diameter (dA) distance measures. We then use these data to estimate w within this restricted redshift range (z < 0.4). Our most stringent result comes from the combination of all our intermediate-redshift data (SDSS-II SNe, BAO, ISW and redshift-space distortions), giving w = -0.81+0.16-0.18 (stat) +/- 0.15 (sys) and ΩM = 0.22+0.09-0.08 assuming a flat universe. This value of w and associated errors only change slightly if curvature is allowed to vary, consistent with constraints from the cosmic microwave background. We also consider more limited combinations of the geometrical (SN, BAO) and dynamical (ISW, redshift-space distortions) probes.
Testing the hadronuclear origin of PeV neutrinos observed with IceCube

We consider implications of the IceCube signal for hadronuclear (pp) scenarios of neutrino sources such as galaxy clusters/groups and star-forming galaxies. Since the observed neutrino flux is comparable to the diffuse γ-ray background flux obtained by Fermi, we place new, strong upper limits on the source spectral index, Γ≲2.1–2.2. In addition, the new IceCube data imply that these sources contribute at least 30%–40% of the diffuse γ-ray background in the 100 GeV range and even ∼100% for softer spectra. Our results, which are insensitive to details of the pp source models, are one of the first strong examples of the multimessenger approach combining the measured neutrino and γ-ray fluxes. The pp origin of the IceCube signal can further be tested by constraining Γ with sub-PeV neutrino observations, by unveiling the sub-TeV diffuse γ-ray background and by observing such pp sources with TeV γ-ray detectors. We also discuss specific pp source models with a multi-PeV neutrino break/cutoff, which are consistent with the current IceCube data.
Defining basic rules for hardening influenza A virus liquid condensates

Multiple viral infections form biomolecular condensates in the host cell to compartmentalize viral reactions. Accumulating evidence indicates that these viral condensates may be hardened, a strategy with potential for exploitation as novel antiviral therapy, given that viral reactions rely on specific material properties for function. However, there is no molecular understanding on how to specifically and efficiently modify the material properties of viral condensates, a pre-requisite for overcoming off-target effects by rational drug design. In vitro, the material properties of biological condensates are modified by different thermodynamic parameters, including free energy, concentration, and type/strength of interactions. Here, we used influenza A virus liquid cytosolic condensates, A.K. A viral inclusions, to provide a proof of concept that modulating the type/strength of transient interactions among the interactome in IAV inclusions is more efficient at hardening these structures than varying the temperature or concentration, both in in vitro and in in vivo models. This stabilization can be achieved by a known pharmacological sticker that can specifically change the material properties of viral inclusions without affecting host proteome abundance nor solubility. Our work supports the development of antivirals targeting the material properties of biomolecular condensates in viral infections. It also provides a framework for the selection of compounds with this activity for general application and thus provides an advance in disease therapy.
Double dark matter admixed neutron star

The dark matter (DM) in neutron stars can exist from the lifetime of the progenitor or when captured by this compact object. The properties of DM that enter the neutron stars through each step could be different from each other. Here, we investigate the structure of neutron stars which are influenced by the DM in two processes. Applying a generalization of two-fluid formalism to three-fluid one and the equation-of-state from the rotational curves of galaxies, we explore the structure of double DM admixed neutron stars. The behavior of the neutron and DM portions for these stars is considered. In addition, the influence of the DM equations of state on the stars with different contributions of visible and DM are studied. The gravitational redshift of these stars in different cases of DM equations of state is investigated.
Importance of relativistic effects in electronic structure and thermopower calculations for Mg 2 Si , Mg 2 Ge , and Mg 2 Sn

We present a theoretical study of the influence of relativistic effects on the electronic band structure and thermopower of Mg${}_{2}X$ ($X=$ Si, Ge, Sn) semiconductors. The full potential Korringa-Kohn-Rostoker (KKR) method is used, and a detailed comparison between the fully relativistic and semirelativistic electronic structure features is done. We show that the spin-orbit (S-O) interaction splits the valence band at $\ensuremath{\Gamma}$ point in good agreement with the experimental data, and this effect strongly depends on $X$ atom. The S-O modifications of the topology of the $\ensuremath{\Gamma}$-centered holelike Fermi surface pockets lead to a change in electron transport properties, which are investigated using the Boltzmann approach. In addition, a simple and efficient method is presented for the calculation of density of states effective mass ${m}^{*}$, and then used to examine the impact of relativistic effects on ${m}^{*}$. It is found that the S-O coupling of the valence bands reduces the effective mass and therefore significantly lowers the thermopower, primarily in ${\mathrm{Mg}}_{2}\mathrm{Sn}$, but also in ${\mathrm{Mg}}_{2}\mathrm{Ge}$. A detrimental influence of the S-O interaction on the thermoelectric performance of $p$-type Mg${}_{2}X$ is analyzed as a function of temperature ($10\text{--}900$ K) and carrier concentration (${10}^{18}\text{--}{10}^{22}$ cm${}^{\ensuremath{-}3}$). Interestingly, similar calculations in $n$-type Mg${}_{2}$X, show a negligible effect of the S-O interaction on the lowest conduction bands and, consequently, also on the Seebeck coefficient.
The 200-pc molecular cylinder in the Galactic Centre

Analyzing the 3D structure of the molecular gas distribution in the central 200 pc region of the Galaxy, we show that the expanding molecular ring (EMR, also known as the parallelogram) and the central molecular zone (CMZ) exhibit quite different distributions and kinematics. The EMR composes a bipolar vertical cylinder with the total length as long as $\sim 170$ pc and shows large non-circular velocities. On the contrary, the CMZ is distributed in a nearly rigid-body rotating ring and arms tightly concentrated near the galactic plane with full thickness less than $\sim 30$ pc. Furthermore, the mass and density ratios of the EMR to CMZ are as small as $\sim 0.13$ and $0.04$, respectively. We discuss the origins of the EMR and CMZ based on the bar and explosion models. We suggest that the EMR's large vertical extent can be explained by a cylindrical shock wave model driven by an explosive activity in the Galactic Centre.
Tomographic Magnification of Lyman Break Galaxies in The Deep Lens Survey

Using about 450 000 galaxies in the Deep Lens Survey, we present a detection of the gravitational magnification of z > 4 Lyman-break galaxies by massive foreground galaxies with 0.4 7. 5σ with a fixed σ8 and is found to be consistent with the expected redshift dependence of the Wilkinson Microwave Anisotropy Probe 7 Λ cold dark matter cosmology.
The impact of baryonic physics on the shape and radial alignment of substructures in cosmological dark matter haloes

We use two simulations performed within the Constrained Local UniversE Simulation (CLUES) project to study both the shape and radial alignment of (the dark matter component of) subhaloes; one of the simulations is a dark matter only model while the other run includes all the relevant gas physics and star formation recipes. We find that the involvement of gas physics does not have a statistically significant effect on either property – at least not for the most massive subhaloes considered in this study. However, we observe in both simulations including and excluding gas dynamics a (pronounced) evolution of the dark matter shapes of subhaloes as well as of the radial alignment signal since infall time. Further, this evolution is different when positioned in the central and outer regions of the host halo today; while subhaloes tend to become more aspherical in the central 50 per cent of their host’s virial radius, the radial alignment weakens in the central regime while strengthening in the outer parts. We confirm that this is due to tidal torquing and the fact that subhaloes at pericentre move too fast for the alignment signal to respond.
Electoral Cycles in Tax Reforms

: We examine electoral cycles in tax reforms using monthly data over the period of 1990-2018 for 22 advanced economies and emerging markets. We show that governments tend to avoid announcing tax reforms during the months running up to elections. In addition, they become more likely to announce those reforms in the first few months following elections, indicating that “political capital” plays a role in the timing of reforms. These patterns are broad-based regarding the changes in tax base and rate, and for various types of taxes. We also find that the pre-election decrease in the likelihood of tax reform announcements is stronger in emerging markets, and weaker in the countries with relatively better institutional quality. Finally, our results indicate that neither fiscal rules nor IMF programs appear to have differential effects on electoral cycles in tax reforms.
Earthshine observations at high spectral resolution: exploring and detecting metal lines in the Earth's upper atmosphere

Observations of the Earth as a planet using the earthshine technique (i.e. looking at the light reflected from the darkside of the Moon), have been used for cl imate and astrobiology studies. They provide information about the planetary albedo, a fundamental parameter of the Earth’s energy balance. Here we present for the first time, observati ons of the earthshine taken at high spectral resolution. The high spectral resolution was chos en in order to investigate the possibility of detecting metallic layers in the Earth’s atmosphe re of geological or meteoritic origin. The SARG echelle spectrograph at the Telescopio Nazionale Galileo in La Palma was used to acquire the earthshine data. Observations were carried out on several nights in February 2011, with the spectral resolution set at 29,000, covering a spect ral range from the near-ultraviolet (360 nm) to near-infrared (1011.9 nm). While we find evidence for the detection of a Na layer in the earthshine, other atomic species are not detected, pe rhaps due to the low signal-to-noise ratio of the observations and the difficult telluric correct ions. The Na layer is found to vary between observation dates, which we speculate is due to physical variations in mesospheric Na concentrations.
DISCOVERY OF 1–5 Hz FLARING AT HIGH LUMINOSITY IN SAX J1808.4–3658

We report the discovery of a 1–5 Hz X-ray flaring phenomenon observed at >30 mCrab near peak luminosity in the 2008 and 2011 outbursts of the accreting millisecond X-ray pulsar SAX J1808.4–3658 in observations with the Rossi X-ray Timing Explorer. In each of the two outbursts this high luminosity flaring is seen for ∼3 continuous days and switches on and off on a timescale of 1–2 hr. The flaring can be seen directly in the light curve, where it shows sharp spikes of emission at quasi-regular separation. In the power spectrum it produces a broad noise component, which peaks at 1–5 Hz. The total 0.05–10 Hz variability has a fractional rms amplitude of 20%–45%, well in excess of the 8%–12% rms broadband noise usually seen in power spectra of SAX J1808.4–3658. We perform a detailed timing analysis of the flaring and study its relation to the 401 Hz pulsations. We find that the pulse amplitude varies proportionally with source flux through all phases of the flaring, indicating that the flaring is likely due to mass density variations created at or outside the magnetospheric boundary. We suggest that this 1–5 Hz flaring is a high mass accretion rate version of the 0.5–2 Hz flaring which is known to occur at low luminosity (<13 mCrab), late in the tail of outbursts of SAX J1808.4–3658. We propose the dead-disk instability, previously suggested as the mechanism for the 0.5–2 Hz flaring, as a likely mechanism for the high luminosity flaring reported here.
FORMATION OF HIGH-REDSHIFT (z>6) QUASARS DRIVEN BY NUCLEAR STARBURSTS

Based on the physical model of a supermassive black hole (SMBH) growth via gas accretion in a circumnuclear disk (CND) proposed by Kawakatu & Wada, we describe the formation of high-z (z>6) quasars (QSOs) whose BH masses are MBH>109 M☉. We derive the necessary conditions to form QSOs at z>6 by only gas accretion: (1) a large mass supply with Msup>1010 M☉from host galaxies to CNDs, because the final BH mass is only 1%–10% of the total supplied mass from QSO hosts. (2) High star formation efficiency for a rapid BH growth which is comparable to high-z starburst galaxies such as submillimeter galaxies. We also find that if the BH growth is limited by the Eddington accretion, the final BH mass is greatly suppressed when the period of mass supply from hosts, tsup, is shorter than the Eddington timescale. Thus, the super-Eddington growth is required for the QSO formation while tsup, which is determined by the efficiency of angular momentum transfer, is shorter than ∼108 yr. The evolution of the QSO luminosity depends on the redshift zi at which accretion onto a seed BH is initiated. In other words, the brighter QSOs at z>6 favor the late growth of SMBHs (i.e., zi ≈ 10) rather than early growth (i.e., zi ≈ 30). For zi ≈ 10, tsup ≃ 108 yr is shorter than that of the star formation in the CND. Thus, the gas in the CND can accrete onto a BH more efficiently, compared with the case for zi ≈ 30 (or tsup ≈ 109 yr). Moreover, we predict the observable properties and the evolution of QSOs at z>6. In a QSO phase, there should exist a stellar rich massive CND, whose gas mass is about 10% of the dynamical mass inside ∼0.1–1 kpc. On the other hand, in a phase where the BH grows (i.e., a proto-QSO phase), the proto-QSO has a gas-rich massive CND whose gas mass is comparable to the dynamical mass. Compared with the observed properties of the distant QSO SDSS J1148+5251 observed at z = 6.42, we predict that SDSS J1148+5251 corresponds to the scenario of the late growth of SMBH with zi ∼ 10, which is accompanied by a massive CNDs with Mg ≈ 5 × 1010 M☉ and the luminous nuclear starburst LSBat infrared band with LSB ≈ 1047 erg s−1. Moreover, we predict that the progenitor of SDSS J1148+5251 can be the super-Eddington object. These predictions can be verified by ALMA, SPICA, and JWST.
Improved 2D Intelligent Driver Model simulating synchronized flow and evolution concavity in traffic flow

Improved 2D Intelligent Driver Model simulating synchronized flow and evolution concavity in traffic flow Junfang Tian*, Rui Jiang, Geng Li*Martin TreiberChenqiang Zhu, Bin Jia Institute of Systems Engineering, College of Management and Economics, Tianjin University, Tianjin 300072, China MOE Key Laboratory for Urban Transportation Complex Systems Theory and Technology, Beijing Jiaotong University, Beijing 100044, China
Advective balance in pipe-formed vortex rings

Vorticity distributions in axisymmetric vortex rings produced by a piston–pipe apparatus are numerically studied over a range of Reynolds numbers, $Re$ , and stroke-to-diameter ratios, $L/D$ . It is found that a state of advective balance, such that $\unicode[STIX]{x1D701}\equiv \unicode[STIX]{x1D714}_{\unicode[STIX]{x1D719}}/r\approx F(\unicode[STIX]{x1D713},t)$ , is achieved within the region (called the vortex ring bubble) enclosed by the dividing streamline. Here $\unicode[STIX]{x1D701}\equiv \unicode[STIX]{x1D714}_{\unicode[STIX]{x1D719}}/r$ is the ratio of azimuthal vorticity to cylindrical radius, and $\unicode[STIX]{x1D713}$ is the Stokes streamfunction in the frame of the ring. Some, but not all, of the $Re$ dependence in the time evolution of $F(\unicode[STIX]{x1D713},t)$ can be captured by introducing a scaled time $\unicode[STIX]{x1D70F}=\unicode[STIX]{x1D708}t$ , where $\unicode[STIX]{x1D708}$ is the kinematic viscosity. When $\unicode[STIX]{x1D708}t/D^{2}\gtrsim 0.02$ , the shape of $F(\unicode[STIX]{x1D713})$ is dominated by the linear-in- $\unicode[STIX]{x1D713}$ component, the coefficient of the quadratic term being an order of magnitude smaller. An important feature is that, as the dividing streamline ( $\unicode[STIX]{x1D713}=0$ ) is approached, $F(\unicode[STIX]{x1D713})$ tends to a non-zero intercept which exhibits an extra $Re$ dependence. This and other features are explained by a simple toy model consisting of the one-dimensional cylindrical diffusion equation. The key ingredient in the model responsible for the extra $Re$ dependence is a Robin-type boundary condition, similar to Newton’s law of cooling, that accounts for the edge layer at the dividing streamline.
Observing nonstandard $W'$ and $Z'$ through the third generation and Higgs lens

We reinterpret $W'$, $Z'$ and Higgs searches at the LHC in terms of a model with nonuniversal $V'$ couplings to fermions in order to gauge how well these searches can be applied outside the (simplified) scenarios for which they were optimized. In particular, we consider bounds from $V'$ searches in final states $\tau \tau$, $e\nu$, $ll$ and $t b$, and discuss the impact of width effects. We then show that decays of the type $V' \rightarrow V h$ yield additional bounds on the heavy vector masses and, in the case of a discovery, provide an important probe of the heavy sector. Finally, we match the low energy limit of the model to an effective theory and compare the bounds on the resulting dimension-6 operators with the direct searches discussed in this paper.
Stable clustering and the resolution of dissipationless cosmological N-body simulations

The determination of the resolution of cosmological N-body simulations, i.e., the range of scales in which quantities measured in them represent accurately the continuum limit, is an important open question. We address it here using scale-free models, for which self-similarity provides a powerful tool to control resolution. Such models also provide a robust testing ground for the so-called stable clustering approximation, which gives simple predictions for them. Studying large N-body simulations of such models with different force smoothing, we find that these two issues are in fact very closely related: our conclusion is that the accuracy of two point statistics in the non-linear regime starts to degrade strongly around the scale at which their behaviour deviates from that predicted by the stable clustering hypothesis. Physically the association of the two scales is in fact simple to understand: stable clustering fails to be a good approximation when there are strong interactions of structures (in particular merging) and it is precisely such non-linear processes which are sensitive to fluctuations at the smaller scales affected by discretisation. Resolution may be further degraded if the short distance gravitational smoothing scale is larger than the scale to which stable clustering can propagate. We examine in detail the very different conclusions of studies by Smith et al. (2003) and Widrow et al. (2009} and find that the strong deviations from stable clustering reported by these works are the results of over-optimistic assumptions about scales resolved accurately by the measured power spectra, and the reliance on Fourier space analysis. We emphasise the much poorer resolution obtained with the power spectrum compared to the two point correlation function.
Wilson Line Response of Holographic Superconductors in Gauss-Bonnet Gravity

We study the Wilson line response in the holographic superconducting phase transitions in the Gauss-Bonnet gravity. In the black brane background case, the Little-Parks periodicity is independent of the Gauss-Bonnet parameter, while in the anti-de Sitter soliton case, there is no evidence for the Little-Parks periodicity. We further study the impact of the Gauss-Bonnet term on the holographic phase transitions quantitatively. For a given Wilson line, a bigger Gauss-Bonnet coefficient makes the phase transition easier for the black brane background while harder for the soliton background. For a given chemical potential, the response to the Wilson line is less sensitive for a bigger Gauss-Bonnet coefficient in the black brane case while the response is more sensitive in the soliton case. And more, a bigger Gauss-Bonnet coefficient makes the superconducting state more stable for both the black brane and the soliton backgrounds. DOI: 10.1103/PhysRevD.87. 026002
Augmented security for healthcare data using obfuscation and elliptic curve cryptography algorithm in health cloud environment

In the past few years, the growing demands of cloud computing became high in the healthcare sector. The electronic health record (EHR) has turned out to be the chosen system to uphold patient's healthcare data. Due to the advancement of cloud computing, the users in the cloud are empowered to access their data with elasticity and offering huge storage capability at minimum costs. This motivates EHR maintainers to transfer their personal storage to the remote cloud servers as it significantly reduces the burden of storage and computation. Nevertheless, securing healthcare data file poses a gigantic challenge as data outsourced in the cloud are too sensitive. Several security features such as data confidentiality, data privacy, access control, data integrity, and data security necessities to be satisfied. This article proposed a secure sharing of healthcare data file by incorporating obfuscation technique and elliptic curve cryptography (ECC) algorithm to enforce better data confidentiality and integrity. Data obfuscation is a beneficial technique in preserving the data confidentiality on the cloud by minimizing the risk of data theft and data leakage. Moreover, ECC methodology aims to provide a high level of security, low communication and computation cost with smaller key size. Experimental analysis reveals better performance than other existing schemes in terms of computation time, communication time, key generation time, throughput rate, turnaround time, and uploading speed. Besides, it exposes that the proposed framework is highly secure and efficient in the field of healthcare system.
The dynamics of azurite Cu3(CO3)2(OH)2 in a magnetic field as determined by neutron scattering

Azurite, a natural mineral made up of CuO chains, is also an intriguing spin-1/2 quantum magnet. There has been much debate as to the one-dimensional (1D) nature of this material by theorists and experimentalists alike. The focus of this debate lies in the interactions between Cu ions within the antiferromagnetically ordered state below 1.9 K. We present high-resolution inelastic neutron-scattering data that highlight the complexity of the magnetic ground state of azurite. The application of magnetic fields and temperatures were used to probe the excitations revealing important information about the dynamics in this system. From this we are able to conclude that the 1D Heisenberg antiferromagnetic spin chain model is not sufficient to describe the dynamics in azurite. Instead additional coupling including interchain interactions and an anisotropic staggered field are necessary to fully model the observed excitations.