Miracle-dz/UniFAR-FTUs huggingface dataset:
Machine-learning-based photometric redshifts for galaxies of the ESO Kilo-Degree Survey data release 2

We have estimated photometric redshifts (zphot) for more than 1.1 million galaxies of the public European Southern Observatory (ESO) Kilo-Degree Survey (KiDS) data release 2. KiDS is an optical wide-field imaging survey carried out with the Very Large Telescope (VLT) Survey Telescope (VST) and the OmegaCAM camera, which aims to tackle open questions in cosmology and galaxy evolution, such as the origin of dark energy and the channel of galaxy mass growth. We present a catalogue of photometric redshifts obtained using the Multi-Layer Perceptron with Quasi-Newton Algorithm (MLPQNA) model, provided within the framework of the DAta Mining and Exploration Web Application REsource (DAMEWARE). These photometric redshifts are based on a spectroscopic knowledge base that was obtained by merging spectroscopic data sets from the Galaxy and Mass Assembly (GAMA) data release 2 and the Sloan Digital Sky Survey III (SDSS-III) data release 9. The overall 1σ uncertainty on Δz = (zspec - zphot)/(1 + zspec) is ˜0.03, with a very small average bias of ˜0.001, a normalized median absolute deviation of ˜0.02 and a fraction of catastrophic outliers (|Δz| > 0.15) of ˜0.4 per cent.
Radiation pressure confinement – II. Application to the broad-line region in active galactic nuclei

Active galactic nuclei (AGN) are characterized by similar broad emission lines properties at all luminosities ($10^{39}$-$10^{47}$ erg s$^{-1}$). What produces this similarity over a vast range of $10^8$ in luminosity? Photoionization is inevitably associated with momentum transfer to the photoionized gas. Yet, most of the photoionized gas in the Broad Line Region (BLR) follows Keplerian orbits, which suggests that the BLR originates from gas with a large enough column for gravity to dominate. The photoionized surface layer of the gas must develop a pressure gradient due to the incident radiation force. We present solutions for the structure of such a hydrostatic photoionized gas layer in the BLR. The gas is stratified, with a low-density highly-ionized surface layer, a density rise inwards, and a uniform-density cooler inner region, where the gas pressure reaches the incident radiation pressure. This radiation pressure confinement (RPC) of the photoionized layer leads to a universal ionization parameter $U\sim 0.1$ in the inner photoionized layer, independent of luminosity and distance. Thus, RPC appears to explain the universality of the BLR properties in AGN. We present predictions for the BLR emission per unit covering factor, as a function of distance from the ionizing source, for a range of ionizing continuum slopes and gas metallicity. The predicted mean strength of most lines (excluding H$\beta$), and their different average-emission radii, are consistent with the available observations.
THE PRESENT-DAY STAR FORMATION RATE OF THE MILKY WAY DETERMINED FROM SPITZER-DETECTED YOUNG STELLAR OBJECTS

We present initial results from a population synthesis model aimed at determining the star formation rate (SFR) of the Milky Way. We find that a total SFR of 0.68–1.45 M☉ yr−1 is able to reproduce the observed number of young stellar objects (YSOs) in the Spitzer/IRAC GLIMPSE survey of the Galactic plane, assuming simple prescriptions for the three-dimensional Galactic distributions of YSOs and interstellar dust, and using model spectral energy distributions to predict the brightness and color of the synthetic YSOs at different wavelengths. This is the first Galaxy-wide measurement derived from pre-main-sequence objects themselves, rather than global observables such as the total radio continuum, Hα, or FIR flux. The value obtained is slightly lower than, but generally consistent with previously determined values. We will extend this method in the future to fit the brightness, color, and angular distribution of YSOs, and simultaneously make use of multiple surveys, to place constraints on the input assumptions, and reduce uncertainties in the SFR estimate. Ultimately, this will be one of the most accurate methods for determining the Galactic SFR, as it makes use of stars of all masses (limited only by sensitivity) rather than solely massive stars or indirect tracers of massive stars.
Dielectric and X-Ray Studies of CaxBa1-xTiO3 and CaxSr1-xTiO3

Ceramics of ${\mathrm{Ca}}_{x}{\mathrm{Ba}}_{1\ensuremath{-}x}\mathrm{Ti}{\mathrm{O}}_{3}$ and ${\mathrm{Ca}}_{x}{\mathrm{Sr}}_{1\ensuremath{-}x}\mathrm{Ti}{\mathrm{O}}_{3}$ have been prepared and their dielectric and structural properties investigated. Firing conditions were adjusted to obtain sharp x-ray back reflections. The Curie point of ${\mathrm{Ca}}_{x}{\mathrm{Ba}}_{1\ensuremath{-}x}\mathrm{Ti}{\mathrm{O}}_{3}$ increases with Ca concentration up to 136\ifmmode^\circ\else\textdegree\fi{}C for $x=0.08$, and then decreases. Both the tetragonal-orthorhombic and the orthorhombic-rhombohedral transition points of ${\mathrm{Ca}}_{x}{\mathrm{Ba}}_{1\ensuremath{-}x}\mathrm{Ti}{\mathrm{O}}_{3}$ decrease monotonically with increasing Ca concentration. ${\mathrm{Ca}}_{x}{\mathrm{Sr}}_{1\ensuremath{-}x}\mathrm{Ti}{\mathrm{O}}_{3}$ solid solutions with $0.01l~xl~0.10$ are ferroelectric at very low temperatures. SrTi${\mathrm{O}}_{3}$ assumes a tetragonal structure below about 80\ifmmode^\circ\else\textdegree\fi{}K.
Exploration of the Ps-Porb Relation for Wind-fed X-Ray Pulsars

We have investigated the relation between the orbital periods (Porb) and the spin periods (Ps) of wind-fed X-ray pulsars in high-mass X-ray binaries (HMXBs), based on population synthesis calculations of the spin evolution of neutron stars during the pre-HMXB stage. We show that most neutron stars either have steady accretion or still reside in the radio pulsar phase when the donor star starts to evolve off the main sequence. In the former case, the spin period can be decelerated to ~102-103 s, depending on the value of Porb. We briefly discuss possible origins of the Ps-Porb correlation in Be/X-ray binaries and the existence of HMXBs with main-sequence donors. We also investigate the evolution of the inclination angle between the magnetic and spin axes of neutron stars in a massive binary, suggesting secular alignment of the magnetic and spin axes during their evolution.
Dark matter response to galaxy formation

We have resimulated the six galaxy-sized haloes of the Aquarius Project including metal-dependent cooling, star formation and supernova feedback. This allows us to study not only how dark matter haloes respond to galaxy formation, but also how this response is affected by details of halo assembly history. In agreement with previous work, we find baryon condensation to lead to increased dark matter concentration. Dark matter density profiles differ substantially in shape from halo to halo when baryons are included, but in all cases the velocity dispersion decreases monotonically with radius. Some haloes show an approximately constant dark matter velocity anisotropy with β ≈ 0.1-0.2, while others retain the anisotropy structure of their baryon-free versions. Most of our haloes become approximately oblate in their inner regions, although a few retain the shape of their dissipationless counterparts. Pseudo-phase-space densities are described by a power law in radius of altered slope when baryons are included. The shape and concentration of the dark matter density profiles are not well reproduced by published adiabatic contraction models. The significant spread we find in the density and kinematic structure of our haloes appears related to differences in their formation histories. Such differences already affect the final structure in baryon-free simulations, but they are reinforced by the inclusion of baryons, and new features are produced. The details of galaxy formation need to be better understood before the inner dark matter structure of galaxies can be used to constrain cosmological models or the nature of dark matter.
A non-linear model of trading mechanism on a financial market

We introduce a prototype model in an attempt to capture some aspects of market dynamics simulating a trading mechanism. The model description starts with a discrete-space, continuous-time Markov process describing arrival and movement of orders with different prices. We then perform a re-scaling procedure leading to a deterministic dynamical system controlled by non-linear ordinary differential equations (ODEs). This allows us to introduce approximations for the equilibrium distribution of the model represented by fixed points of deterministic dynamics.
Becoming a Mathematics Teacher: Identity and Identifications

This book is about people preparing to teach mathematics to children in the first half of their schooling. It is also about what mathematics becomes in a school context responding to insistent demands to raise standards. The book asks how aspirant teachers begin to think of themselves as teachers, and about mathematics in particular, when they have many years of experience as pupils in school behind them, which did not always leave a positive image of mathematics. How do they change how they are, or even who they are, as they proceed through a teacher education programme into their first teaching post, where mathematics is just one of many subjects to be taught? They will encounter diverse and complex social demands that cannot necessarily be reconciled, since the work of schools is targeted at enabling pupils to participate in a rapidly changing world where consensus on educational objectives seems difficult to achieve. Conflicting priorities can result in teachers being pulled in many directions, where their personal aspirations confront an official story that portrays the journey into teaching as a sequence of criteria to be fulfilled. Centred on over 200 hours of interview data from government-funded studies directed by the authors the book documents teachers over a five-year period, from the outset of their training to the end of their first year of teaching in a school. These interviews coincided with a major national curriculum initiative that through prescriptive and detailed regulation set the characteristics of a good teacher and the content of mathematics to be taught. Aimed primarily at teacher educators the book will also appeal to researchers across the field of education for its unique theoretical perspective drawing on contemporary psychoanalytical theory in portraying the identities that teachers come to occupy, and the forms of mathematics with which they identify. It also presents a vivid account of what educational policy implementation looks like through the voices of teachers building their practices.
A search for correlation of ultra-high energy cosmic rays with IRAS-PSCz and 2MASS-6dF galaxies

We study the arrival directions of 69 ultra-high energy cosmic rays (UHECRs) observed at the Pierre Auger Observatory (PAO) with energies exceeding 55 EeV. We investigate whether the UHECRs exhibit the anisotropy signal expected if the primary particles are protons that originate in galaxies in the local universe, or in sources correlated with these galaxies. We cross-correlate the UHECR arrival directions with the positions of IRAS-PSCz and 2MASS-6dF galaxies taking into account particle energy losses during propagation. This is the first time that the 6dF survey is used in a search for the sources of UHECRs and the first time that the PSCz survey is used with the full 69 PAO events. The observed cross-correlation signal is larger for the PAO UHECRs than for 94% (98%) of realisations from an isotropic distribution when cross-correlated with the PSCz (6dF). On the other hand the observed cross-correlation signal is lower than that expected from 85% of realisations, had the UHECRs originated in galaxies in either survey. The observed cross-correlation signal does exceed that expected by 50% of the realisations if the UHECRs are randomly deflected by intervening magnetic fields by 5° or more. We propose a new method of analysing the expected anisotropy signal, by dividing the predicted UHECR source distribution into equal predicted flux radial shells, which can help localise and constrain the properties of UHECR sources. We find that the 69 PAO events are consistent with isotropy in the nearest of three shells we define, whereas there is weak evidence for correlation with the predicted source distribution in the two more distant shells in which the galaxy distribution is less anisotropic.
Characterization of magnetic properties of Sr2CuWO6 and Sr2CuMoO6

Sami Vasala,1 Hassan Saadaoui,2 Elvezio Morenzoni,2 Omar Chmaissem,3,4 Ting-Shan Chan,5 Jin-Ming Chen,5 Ying-Ya Hsu,6 Hisao Yamauchi,1 and Maarit Karppinen1,* 1Department of Chemistry, Aalto University, FI-00076 AALTO, Finland 2Laboratory for Muon Spin Spectroscopy, Paul Scherrer Institute, CH-5232 Villigen PSI, Switzerland 3Department of Physics, Northern Illinois University, DeKalb, Illinois 60115, USA 4Materials Science Division, Argonne National Laboratory, Argonne, Illinois 60439, USA 5National Synchrotron Radiation Research Center, Hsinchu 30076, Taiwan 6Program for Science and Technology of Accelerator Light Source, National Chiao Tung University, Hsinchu 30076, Taiwan (Received 9 February 2014; revised manuscript received 4 April 2014; published 21 April 2014)
Three-Dimensional Distribution of the ISM in the Milky Way Galaxy: III. The Total Neutral Gas Disk

We present newly obtained three-dimensional gaseous maps of the Milky Way Galaxy; HI, H$_2$ and total-gas (HI plus H$_2$) maps, which were derived from the HI and $^{12}$CO($J=1$--0) survey data and rotation curves based on the kinematic distance. The HI and H$_2$ face-on maps show that the HI disk is extended to the radius of 15--20 kpc and its outskirt is asymmetric to the Galactic center, while most of the H$_2$ gas is distributed inside the solar circle. The total gas mass within radius 30 kpc amounts to $8.0\times 10^9$ M$_\odot$, 89\% and 11\% of which are HI and H$_2$, {respectively}. The vertical slices show that the outer HI disk is strongly warped and the inner HI and H$_2$ disks are corrugated. The total gas map is advantageous to trace spiral structure from the inner to outer disk. Spiral structures such as the Norma-Cygnus, the Perseus, the Sagittarius-Carina, the Scutum-Crux, and the Orion arms are more clearly traced in the total gas map than ever. All the spiral arms are well explained with logarithmic spiral arms with pitch angle of $11\degree$ -- $15\degree$. The molecular fraction to the total gas is high near the Galactic center and decreases with the Galactocentric distance. The molecular fraction also locally enhanced at the spiral arms compared with the inter-arm regions.
Planetary influence on the young Sun's evolution: the solar neutrino probe

Recent observations of solar twin stars with planetary syst ems like the Sun, have uncovered that these present a peculiar surface chemical composition . This is believed to be related to the formation of earth-like planets. This suggests that twi n stars have a radiative interior that is richer in heavy elements than their envelopes. Moreover, the current standard solar model does not fully agree with the helioseismology data and solar neutrino flux measurements. In this work, we find that this agreement can improve if the Sun has mass loss during the pre-main sequence, as was previously shown by other groups. Despite this better agreement, the internal composition of the Sun is still uncertain, espe cially for elements heavier than helium. With the goal of inferring the chemical abundance of the solar interior, we tested several chemical compositions. We found that heavy element abundances influence the sound speed and solar neutrinos equally. Nevertheless, the carbo n-nitrogen-oxygen (CNO; 13 N, 15 O and 17 F) neutrino fluxes are the most affected; this is due to the fac t that contrarily to protonproton (pp, pep, 8 B and 7 Be) neutrino fluxes, the CNO neutrino fluxes are less dependen t on the total luminosity of the star. Furthermore, if the centra l solar metallicity increases by 30%, as hinted by the solar twin stars observations, this new sola r model predicts that 13 N, 15 O and 17 F neutrino fluxes increase by 25%-80% relative to the standar d solar model. Finally, we highlight that the next generation of solar neutrino experi ments will not only put constraints on the abundances of carbon, oxygen and nitrogen, but will also give some information about their radial distribution.
Reflector antenna distortion determination: An iterative‐field‐matrix solution

The idealized shapes of satellite reflector antennas are often distorted once they are placed in orbit. The performance of such antennas can be improved by identifying the locations and amount of their surface distortions and then by correcting them using active surface distortion or array feeding. This work presents a method to determine the required discrete surface distortions to correct errors. The algorithm starts by discretizing the entire reflector surface into triangular patches, then by determining the linear relationship between the local distortion and the difference between distorted and undistorted far‐fields patterns. A linear system of equations with discrete distortions as unknowns results when this scattered field is sampled at specific observation points. Singular Value Decomposition combined with Tikhonov regularization, is used to solve for the set of distortions, which are translated into a physically realizable continuous surface by projecting onto a Polynomial‐Fourier‐Series basis. The later scheme is iteratively repeated in order to minimize the residual error. The method has been applied successfully to determine thermal/gravitational distortions on a reflector antenna, with up to 97% accuracy in tenth iteration.
Remarks about a transitive version of perfectly meager sets

We show that if X has the property that every continuous image into Baire space is bounded and 2 ω is not a continuous image of X , then X is always of ﬁrst category in some additive sense. This gives an answer to an oral question of L. Bukovsk´y, whether every wQN set has the latter property.
Selection of the Heat Transfer Coefficient Using Swarming Algorithms

Abstract The article presents the use of swarming algorithms in selecting the heat transfer coefficient, taking into account the boundary condition of the IV types. Numerical calculations were made using the proprietary TalyFEM program and classic form of swarming algorithms. A function was also used for the calculations, which, during the calculation, determined the error of the approximate solution and was minimalised using a pair of individually employed algorithms, namely artificial bee colony (ABC) and ant colony optimisation (ACO). The tests were carried out to select the heat transfer coefficient from one range. Describing the geometry for a mesh of 408 fine elements with 214 nodes, the research carried out presents two squares (one on top of the other) separated by a heat transfer layer with a κ coefficient. A type III boundary condition was established on the right and left of both edges. The upper and lower edges were isolated, and a type IV boundary condition with imperfect contact was established between the squares. Calculations were made for ABC and ACO, respectively, for populations equal to 20, 40 and 60 individuals and 2, 6 and 12 iterations. In addition, in each case, 0%, 1%, 2% and 5% noise of the reference values were also considered. The obtained results are satisfactory and very close to the reference values of the κ parameter. The obtained results demonstrate the possibility of using artificial intelligence (AI) algorithms to reconstruct the IV type boundary condition value during heat conduction modelling.
A proposed spectral form for fully developed wind seas based on the similarity theory of S

This invention relates to the recovery of precious metals. More particularly, the invention relates to a process for the recovery of a catalytic metal from a carbonaceous residue or support comprising subjecting an aqueous slurry of material containing catalytic metal to be recovered to a temperature of not less than 200 DEG C and a pressure not less than 75 atmospheres in an atmosphere comprising a quantity of oxygen at least sufficient to oxidize substantially all the carbon present, the oxidation being carried out in the presence of a liquid aqueous phase. The process also relates to the recovery of silver from photographic film.
High signal‐to‐noise ratio observations and the ultimate limits of precision pulsar timing

We demonstrate that the sensitivity of high-precision pulsar timing experiments will be ultimately limited by the broad-band intensity modulation that is intrinsic to the pulsar’s stochastic radio signal. That is, as the peak flux of the pulsar approaches that of the system equivalent flux density, neither greater antenna gain nor increased instrumental bandwidth will improve timing precision. These conclusions proceed from an analysis of the covariance matrix used to characterize residual pulse profile fluctuations following the template-matching procedure for arrival time estimation. We perform such an analysis on 25 h of high-precision timing observations of the closest and brightest millisecond pulsar, PSR J0437−4715. In these data, the standard deviation of the post-fit arrival time residuals is approximately four times greater than that predicted by considering the system equivalent flux density, mean pulsar flux and the effective width of the pulsed emission. We develop a technique based on principal component analysis to mitigate the effects of shape variations on arrival time estimation and demonstrate its validity using a number of illustrative simulations. When applied to our observations, the method reduces arrival time residual noise by approximately 20 per cent. We conclude that, owing primarily to the intrinsic variability of the radio emission from PSR J0437−4715 at 20 cm, timing precision in this observing band better than 30–40 ns in 1 h is highly unlikely, regardless of future improvements in antenna gain or instrumental bandwidth. We describe the intrinsic variability of the pulsar signal as stochastic wide-band impulse modulated self-noise (SWIMS) and argue that SWIMS will likely limit the timing precision of every millisecond pulsar currently observed by pulsar timing array projects as larger and more sensitive antennas are built in the coming decades.
Luminous red galaxies in simulations: cosmic chronometers?

There have been a number of attempts to measure the expansion rate of the Universe at high redshift using luminous red galaxies (LRGs) as ‘chronometers’. The method generally assumes that stars in LRGs are all formed at the same time. In this paper, we quantify the uncertainties on the measurement of H(z) which arise when one considers more realistic, extended star formation histories. In selecting galaxies from the Millennium simulation for this study, we show that using rest-frame criteria significantly improves the homogeneity of the sample and that H(z) can be recovered to within 3 per cent at z ∼ 0.42 even when extended star formation histories are considered. We demonstrate explicitly that using single stellar populations (SSPs) to age-date galaxies from the semi-analytical simulations provides insufficient accuracy for this experiment but accurate ages are obtainable if the complex star formation histories extracted from the simulation are used. We note, however, that problems with SSP fitting might be overestimated since the semi-analytical models tend to overpredict the late-time star formation in LRGs. Finally, we optimize an observational programme to carry out this experiment.