Miracle-dz/UniFAR-FTUs huggingface dataset:
Bacterial diversity in aerated facultative lagoon treating kraft cellulose effluent with bioaugmentation

The microbiological diversity was evaluated in an aerated facultative lagoon system with organic loading rates of 0.2 and 0.6 kgCODm-3d-1 treating effluent from the kraft pulp industry for bioaugmentation purposes. Samples were taken from a laboratory-scale lagoon at steady state treating kraft pulp effluent and operated with two different rates for 120 days. The analysis was performed by 16S rDNA sequencing. The autochthonous bacteria were identified through statistical similarity obtained from the NCBI-BLAST database. The lagoon performance was assessed based on the removal efficiency of biochemical oxygen demand (94% and 80%), chemical oxygen demand (51% and 44%), total organic carbon (49% and 41%), lignin-derived compounds (13% and 27%), turbidity (94% and 87%), for the low and high rates used respectively. Color and TPC were not significantly removed during the biological treatment of the industrial matrix. In the biomass samples collected at a steady state, 9 and 12 species of bacteria were identified at the applied rates. The species Bacillus cereus, Bacillus thuringiensis, and Paenibacillus glucanolyticus found in this matrix presented significant removal of the parameters in the kraft effluent. The three referred species show great promise in the removal of specific parameters in an AFL biological treatment system using bioaugmentation.
SURFACE BRIGHTNESS PROFILES OF DWARF GALAXIES. I. PROFILES AND STATISTICS

Radial surface brightness profiles of spiral galaxies are classified into three types: (I) single exponential, or the light falls off with one exponential to a break before falling off (II) more steeply, or (III) less steeply. Profile breaks are also found in dwarf disks, but some dwarf Type IIs are flat or increasing out to a break before falling off. Here we re-examine the stellar disk profiles of 141 dwarfs: 96 dwarf irregulars (dIms), 26 Blue Compact Dwarfs (BCDs), and 19 Magellanic-type spirals (Sms). We fit single, double, or even triple exponential profiles in up to 11 passbands: GALEX FUV and NUV, ground-based UBVJHK and Hα, and Spitzer 3.6 and 4.5 μm. We find that more luminous galaxies have brighter centers, larger inner and outer scale lengths, and breaks at larger radii; dwarf trends with MB extend to spirals. However, the V-band break surface brightness is independent of break type, MB, and Hubble type. Dwarf Type II and III profiles fall off similarly beyond the breaks but have different interiors and IIs break ∼twice as far as IIIs. Outer Type II and III scale lengths may have weak trends with wavelength, but pure Type II inner scale lengths clearly decrease from the FUV to visible bands whereas Type III inner scale lengths increase with redder bands. This suggests the influence of different star formation histories on profile type, but nonetheless the break location is approximately the same in all passbands. Dwarfs continue trends between profile and Hubble types such that later-type galaxies have more Type II but fewer Type I and III profiles than early-type spirals. BCDs and Sms are over-represented as Types III and II, respectively, compared to dIms.
Field-induced incommensurate phase in the strong-rung spin ladder with ferromagnetic legs

We report magnetization, specific heat, and NMR measurements of 3-Br-4-F-V [=3-(3-bromo-4-fluorophenyl)-1,5-diphenylverdazyl], a strong-rung S=1/2 Heisenberg spin ladder with ferromagnetic leg interactions. We explain the magnetic and thermodynamic properties based on the strong-rung regime. Furthermore, we find a field-induced successive phase transition in the specific heat and the nuclear spin-lattice relaxation rate 1/T1. 19F-NMR spectra for higher- and lower-temperature phases indicate partial magnetic order and incommensurate long-range order, respectively, evidencing the presence of frustration due to weak interladder couplings.
Neutrons meet ice polymorphs

The current epoch can be described as the ‘age of ice-rush’, as the rate of discovery of ice polymorphs, of which there are currently 20 known, has accelerated, particularly since the end of the last century. This is largely owing to advances in neutron diffraction under pressure. Neutrons can interact with light elements such as hydrogen as well as heavy elements, making neutron diffraction essential for full structural analyses of newly discovered ice polymorphs. It is especially useful for detecting crystallographic symmetry breaking due to hydrogen ordering. This review will go over the most recent technical advances in neutron-diffraction experiments and how they contribute to our understanding of ice polymorphs.
A CATALOG OF CH3OH 70–61A+ MASER SOURCES IN MASSIVE STAR-FORMING REGIONS. II. MASERS IN NGC 6334F, G8.67−0.36, AND M17

We present Very Large Array (VLA) observations of the 70–61A+ methanol maser transition at 44 GHz toward NGC 6334F, G8.67−0.36, and M17. These arcsecond resolution observations complete a previous, larger VLA survey of this maser transition in high-mass, star-forming regions reported by Kurtz et al. We confirm the presence of 44 GHz methanol maser emission in all 3 sources, detecting 8 distinct maser components in NGC 6334F, 12 components in G8.67−0.36, and 1 in M17.
Functional Renormalisation Group analysis of Tensorial Group Field Theories on $\mathbb{R}^d$

Rank-d Tensorial Group Field Theories are quantum field theories defined on a group manifold $G^{\times d}$, which represent a non-local generalization of standard QFT, and a candidate formalism for quantum gravity, since, when endowed with appropriate data, they can be interpreted as defining a field theoretic description of the fundamental building blocks of quantum spacetime. Their renormalisation analysis is crucial both for establishing their consistency as quantum field theories, and for studying the emergence of continuum spacetime and geometry from them. In this paper, we study the renormalisation group flow of two simple classes of TGFTs, defined for the group $G=\mathbb{R}$ for arbitrary rank, both without and with gauge invariance conditions, by means of functional renormalisation group techniques. The issue of IR divergences is tackled by the definition of a proper thermodynamic limit for TGFTs. We map the phase diagram of such models, in a simple truncation, and identify both UV and IR fixed points of the RG flow. Encouragingly, for all the models we study, we find evidence for the existence of a phase transition of condensation type.
Anomalies in the thermomechanical behavior of Ba0.5Sr0.5Co0.8Fe0.2O3−δ ceramic oxygen conductive membranes at intermediate temperatures

The thermomechanical properties of Ba0.5Sr0. 5Co0.8Fe0. 2O3−δ (BSCF) were measured using ring-on-ring tests and depth-sensitive microindentation. The cubic BSCF material exhibits an anomaly in mechanical properties between 200 and 400 °C. The observed anomaly is attributed to the transition of Co3+ spin states which is experimentally confirmed by susceptibility measurements. Furthermore, slip lines were observed around the impression when indentation tests were carried out above 260 °C.
Quantitative study of the AMS-02 electron/positron spectra: Implications for pulsars and dark matter properties

The Alpha Magnetic Spectrometer (AMS-02) has just published the unprecedentedly precise measurement of the cosmic electron and positron spectra. In this paper, we try to give a quantitative study on the AMS-02 results by a global fitting to the electron and positron spectra, together with the updated positron fraction data. The Markov chain Monte Carlo algorithm is adopted to do the fitting. The primary electron spectrum and the parameters for pulsars or dark matter that contribute extra positrons are determined simultaneously. We find that there is a hardening of the primary electron spectrum at similar to 60 GeV. With such a new feature at the background spectrum, both the pulsars and dark matter can explain the AMS-02 results very well. The dark matter scenario shows a drop at the positron fraction at similar to 300 GeV but suffers very strong constraints from Fermi gamma-ray observations. The fitting results also suggest that the propagation model with convection may be more favored by the lepton data than the reacceleration model.
Properties and Alignment of Interstellar Dust Grains toward Type Ia Supernovae with Anomalous Polarization Curves

Recent photometric and polarimetric observations of Type Ia supernovae (SNe Ia) show unusually low total-to-selective extinction ratios (RV < 2) and wavelengths of maximum polarization (λmax < 0.4 μm) for several SNe Ia, which indicates peculiar properties of interstellar (IS) dust in the SN-hosted galaxies and/or the presence of circumstellar (CS) dust. In this paper, we use an inversion technique to infer the best-fit grain size distribution and the alignment function of interstellar grains along the lines of sight toward four SNe Ia with anomalous extinction and polarization data (SN 1986G, SN 2006X, SN 2008fp, and SN 2014J). We find that to reproduce low values of RV, a significant enhancement in the mass of small grains of radius a < 0.1 μm is required. For SN 2014J, a simultaneous fit to its observed extinction and polarization is unsuccessful if all the data are attributed to IS dust (model 1), but a good fit is obtained when accounting for the contribution of CS dust (model 2). For SN 2008fp, our best-fit results for model 1 show that in order to reproduce an extreme value of λmax ∼ 0.15 μm, small silicate grains must be aligned as efficiently as big grains. For this case, we suggest that strong radiation from the SN can induce efficient alignment of small grains in a nearby intervening molecular cloud via the radiative torque (RAT) mechanism. The resulting time dependence polarization from this RAT alignment model can be tested by observing at ultraviolet wavelengths.
Inflationary cosmology and fundamental physics

This thesis is a collection of several papers at the interface between cosmology, particle physics, and field theory. In the first half, we examine topics that are directly related to inflation: axions, string theory, and non-minimally coupled fields. In particular, we constrain the allowed parameter space of inflationary axion cosmology, identifying a classic window and an anthropic window; we discuss inflation in string theory, proving a no-go theorem for a class of string models; and we examine the quantum field theory governing inflation driven by non-minimally coupled fields, which is relevant to Higgs-inflation. In the second half, we examine other topics: oscillons, entanglement entropy, and the Casimir effect. In particular, we compute the quantum decay of oscillons, finding it to be dramatically different to the classical decay; we establish finite contributions to the entanglement entropy between a pair of regions, including a finite area law; and we compute the Casimir force in a closed geometry, finding an attractive force and invalidating claims of repulsion.
Advanced LIGO

The Advanced LIGO gravitational wave detectors are second generation instruments designed and built for the two LIGO observatories in Hanford, WA and Livingston, LA. The two instruments are identical in design, and are specialized versions of a Michelson interferometer with 4 km long arms. As in initial LIGO, Fabry-Perot cavities are used in the arms to increase the interaction time with a gravitational wave, and power recycling is used to increase the effective laser power. Signal recycling has been added in Advanced LIGO to improve the frequency response. In the most sensitive frequency region around 100 Hz, the design strain sensitivity is a factor of 10 better than initial LIGO. In addition, the low frequency end of the sensitivity band is moved from 40 Hz down to 10 Hz. All interferometer components have been replaced with improved technologies to achieve this sensitivity gain. Much better seismic isolation and test mass suspensions are responsible for the gains at lower frequencies. Higher laser power, larger test masses and improved mirror coatings lead to the improved sensitivity at mid- and high- frequencies. Data collecting runs with these new instruments are planned to begin in mid-2015.
Strong simulation of tracking single photons with which-way-detectors in linear optics

Which-way-detectors (WWDs) are path-entangled detectors characterizing mutual exclusivity between path information and interference visibility in wave-particle duality experiments. We show surprisingly that WWDs allow to utilize single photons distinguishable in time domain to realize linear optical circuits where tracking their paths is exponentially hard for strong simulation analogous to rectangular lattice based Ising models. Distinguishable photons have scalability advantages of generation and detection compared with indistinguishable photons by promising both theoretical and experimental improvements in linear optical computing including boson sampling. We calculate strong simulation complexities by using variable elimination (VE) method for undirected graphs related to tensor network contraction for quantum circuits and recursive Feynman path-integral (RFPI) method to reduce space complexity. Two designs include either a single photon touring m times or m single photons propagating sequentially through an optical circuit composed of n beam splitters and phase shifters entangled with n WWDs. VE method for tracking results in undirected graphs matching with (2 m − 1) × (n + 1) and m × (n + 1) lattice Ising models with computational complexities of O(mn2min(2m−1,n+1)) and O(mn2min(m,n+1)) in time and O(2min(2m−1,n+1)) and O(2min(m,n+1)) in space for single and multi-photon based designs, respectively. We exploit RFPI method for m ≫ n to reduce space complexities to polynomial levels with respect to n and log m. Probability amplitude of specific cases of multi-photon design is represented in terms of Ising partition function with purely imaginary weights to characterize sampling complexity. Open issues about sampling complexity and experimental implementation of multi-WWD set-ups are discussed.
Quantifying dwarf satellites through gravitational imaging : The case of SDSS J120602.09+514229.5

SDSS J120602.09+514229.5 is a gravitational lens system formed by a group of galaxies at redshift z(FG) = 0.422 lensing a bright background galaxy at redshift z(BG) = 2.001. The main peculiarity of this system is the presence of a luminous satellite near the Einstein radius, which slightly deforms the giant arc. This makes SDSS J120602.09+514229.5 the ideal system to test our grid-based Bayesian lens modelling method, designed to detect Galaxy satellites independently of their mass-to-light ratio and to measure the mass of this dwarf galaxy despite its high redshift. We model the main lensing potential with a composite analytical density profile consisting of a single power law for the group dominant galaxy and two singular isothermal spheres for the other two group members. Thanks to the pixelized source and potential reconstruction technique of Vegetti and Koopmans, we are able to detect the luminous satellite as a local positive surface density correction to the overall smooth mass model. Assuming a truncated pseudo-Jaffe density profile, the satellite has a mass M(sub) = (2.75 +/- 0.04) x 1010 M(circle dot) inside its tidal radius of r(t) = 0.68 arcsec. This result is robust against changes in the lens model. We determine for the satellite a luminosity of L(B) = (1.6 +/- 0.8) x 109 L(circle dot), leading to a total mass-to-light ratio within the tidal radius of (M/L)(B) = (17.2 +/- 8.5) M(circle dot)/L(circle dot). The central galaxy has a sub-isothermal density profile as in general is expected for group members. From the Sloan Digital Sky Survey (SDSS) spectrum, we derive for the central galaxy a velocity dispersion of Sigma(kinem) = 380 +/- 60 km s-1 within the SDSS aperture of a diameter of 3 arcsec. The logarithmic density slope of gamma = 1.7+0.25(-0.30) [68 per cent confidence limit (CL)], derived from this measurement, is consistent within 1 Sigma with the density slope of the dominant lens galaxy gamma approximate to 1.6 determined from the lens model. This paper shows how powerful pixelized lensing techniques are in detecting and constraining the properties of dwarf satellites at high redshift.
Phase-charge duality in Josephson junction circuits: Role of inertia and effect of microwave irradiation

We investigate the physics of coherent quantum phase slips in two distinct circuits containing small Josephson junctions: (i) a single junction embedded in an inductive environment and (ii) a long chain of junctions. Starting from the standard Josephson Hamiltonian, the single junction circuit can be analyzed using quasi-classical methods; we formulate the conditions under which the resulting quasi-charge dynamics is exactly dual to the usual phase dynamics associated with Josephson tunneling. For the chain we use the fact that its collective behavior can be characterized by one variable: the number $m$ of quantum phase slips present on it. We conclude that the dynamics of the conjugate quasi-charge is again exactly dual to the standard phase dynamics of a single Josephson junction. In both cases we elucidate the role of the inductance, essential to obtain exact duality. These conclusions have profound consequences for the behavior of single junctions and chains under microwave irradiation. Since both systems are governed by a model exactly dual to the standard resistively and capacitively shunted junction model, we expect the appearance of current-Shapiro steps. We numerically calculate the corresponding current-voltage characteristics in a wide range of parameters. Our results are of interest in view of a metrological current standard.
Influence of Initial Imperfections on PMMA Spherical Shell

This paper focused on the influence of initial imperfection on the critical load of PMMA pressure spherical shell by introducing buckling modes as the initial defect. Four types of pressure spherical shells including complete spherical shell, spherical shell with single penetration, spherical shell with double penetrations, and hyperspherical shell were studied. The distribution of initial imperfections was given through the modal configuration of linear eigenvalue analysis, and then the buckling critical load of the spherical shell was analyzed by using the consistent modal defect method and N-order modal defect method. Results confirmed that: Initial imperfections have a great different influence on pressure spherical shells with varying penetration. It has the greatest influence on the critical load of a spherical shell with double penetration at a 5 mm defect. With the increase of defect amplitude, the critical load of the spherical shell decreases. The analysis results also show that the first-order mode is usually not the worst geometric defect configuration of PMMA pressure spherical shell. And the worst mode may appear in higher-order mode due to the influence of penetration, initial defect amplitude, and different thickness-diameter ratio.
Generic conditions for stable hybrid stars

We study the mass-radius curve of hybrid stars, assuming a single first-order phase transition between nuclear and quark matter, with a sharp interface between the quark matter core and nuclear matter mantle. We use a generic parameterization of the quark matter equation of state, which has a constant, i.e. density-independent, speed of sound ("CSS"). We argue that this parameterization provides a framework for comparison and empirical testing of models of quark matter. We obtain the phase diagram of possible forms of the hybrid star mass-radius relation, where the control parameters are the transition pressure, energy density discontinuity, and the quark matter speed of sound. We find that this diagram is sensitive to the quark matter parameters but fairly insensitive to details of the nuclear matter equation of state. We calculate the maximum hybrid star mass as a function of the parameters of the quark matter EoS, and find that there are reasonable values of those parameters that give rise to hybrid stars with mass above $2\,M_\odot$.
Autonomous Spacecraft Navigation With Pulsars

An external reference system suitable for deep space navigation can be defined by fast spinning and strongly magnetized neutron stars, called pulsars. Their beamed periodic signals have timing stabilities comparable to atomic clocks and provide characteristic temporal signatures that can be used as natural navigation beacons, quite similar to the use of GPS satellites for navigation on Earth. By comparing pulse arrival times measured on-board a spacecraft with predicted pulse arrivals at a reference location, the spacecraft position can be determined autonomously and with high accuracy everywhere in the solar system and beyond. The unique properties of pulsars make clear already today that such a navigation system will have its application in future astronautics. In this paper we describe the basic principle of spacecraft navigation using pulsars and report on the current development status of this novel technology.
Free-standing nanowire layer-transfer parametric optimisation of multi-response process by Grey Taguchi design

Silicon nanowires (SiNWs) possess advantages over bulk silicon, such as higher surface-to-volume ratio and light trapping capability. The metal-assisted chemical etching fabricates SiNWs, and anodisation-electropolishing lifts off a free-standing film of the vertically aligned nanowires. The paper shows the reusability of the substrate for cost-effectiveness with a minute change in the surface roughness. Owing to multiple controlling and output parameters involved during fabrication, optimising process parameters for a specific application by the factorial method is expensive and tedious. Pure Taguchi design struggles with a multi-response system, whereas the Grey relational analysis converts the multi-response system to a single-response system by assigning grades. The Grey Taguchi design optimises the fabrication parameters for the optimum outcome, which is validated by experimentation.
Performance Analysis of Typical Routing Protocols for Cognitive Radio Ad Hoc Networks

Cognitive Radio Ad Hoc Networks (CRAHNs) have powerful growth potential, a solution to solve the scarce spectrum resources problem. Due characteristics can change configuration parameters during transmission, thereby opening up the possibility to use the dynamic spectrum. This leads to the complexity of the design of routing protocols. In this paper, we present the routing protocol is proposed to apply for Cognitive Radio Ad hoc Networks. After explaining the principle of operation, we analyze and evaluate the performance of the protocol on NS2. Simulation results show that the protocol End-to-End with throughput and latency is best improved. Finally, we discuss the limitations of recently routing protocols and propose some further research directions.
Hubble Space Telescope Detection of Spiral Structure in Two Coma Cluster Dwarf Galaxies

We report the discovery of spiral-like structure in Hubble Space Telescope images of two dwarf galaxies (GMP 3292 and GMP 3629) belonging to the Coma Cluster. GMP 3629 is the faintest such galaxy detected in a cluster environment, and it is the first such galaxy observed in the dense Coma Cluster. The large bulge and the faintness of the broad spiral-like pattern in GMP 3629 suggest that its disk may have been largely depleted. We may therefore have found an example of the "missing link" in theories of galaxy evolution that have predicted that dwarf spiral galaxies, particularly in clusters, evolve into dwarf elliptical galaxies.