Miracle-dz/UniFAR-FTUs huggingface dataset:
Testing gravity with galaxy-galaxy lensing and redshift-space distortions using CFHT-Stripe 82, CFHTLenS, and BOSS CMASS datasets

The combination of galaxy-galaxy lensing (GGL) and redshift space distortion of galaxy clustering (RSD) is a privileged technique to test general relativity predictions and break degeneracies between the growth rate of structure parameter f and the amplitude of the linear power spectrum σ8. We performed a joint GGL and RSD analysis on 250 sq. deg using shape catalogues from CFHTLenS and CFHT-Stripe 82 and spectroscopic redshifts from the BOSS CMASS sample. We adjusted a model that includes non-linear biasing, RSD, and Alcock–Paczynski effects. We used an N-body simulation supplemented by an abundance matching prescription for CMASS galaxies to build a set of overlapping lensing and clustering mocks. Together with additional spectroscopic data, this helps us to quantify and correct several systematic errors, such as photometric redshifts. We find f(z = 0.57) = 0.95 ± 0.23, σ8(z = 0.57) = 0.55 ± 0.07 and Ωm = 0.31 ± 0.08, in agreement with Planck cosmological results 2018. We also estimate the probe of gravity EG = 0.43 ± 0.10, in agreement with ΛCDM−GR predictions of EG = 0.40. This analysis reveals that RSD efficiently decreases the GGL uncertainty on Ωm by a factor of 4 and by 30% on σ8. We make our mock catalogues available on the Skies and Universe database.
A parallel implementation of an O ∗ ( n 4 ) volume algorithm. (English)

Res. 23, No. (2015). Summary: Recently an O ∗ ( n 4 ) volume algorithm has been presented for convex bodies by L. Lovász and S. Vempala [J. Comput. Syst. Sci. 72, No. 2, 392–417 (2006; Zbl 1090.68112)], where n is the number of dimensions of the convex body. Essentially the algorithm consists of several, interlocked simulational steps of slightly diﬀerent natures. A computer implementation was later developed to gather some information about the numerical aspects of the algorithm, the number of dimensions in the examples was at most 10, and the errors of the results were somewhat dissatisfying. Now we present a parallel version of the improved algorithm, where variance reducing was added to make the algorithm faster, and the use of a GPU with 480 processors made experimentation easier. Computational results for convex bodies in dimensions ranging from 2 to 20 are presented as well.
A fresh approach to forecasting in astroparticle physics and dark matter searches

We present a toolbox of new techniques and concepts for the efficient forecasting of experimental sensitivities. These are applicable to a large range of scenarios in (astro-)particle physics, and based on the Fisher information formalism. Fisher information provides an answer to the question 'what is the maximum extractable information from a given observation? '. It is a common tool for the forecasting of experimental sensitivities in many branches of science, but rarely used in astroparticle physics or searches for particle dark matter. After briefly reviewing the Fisher information matrix of general Poisson likelihoods, we propose very compact expressions for estimating expected exclusion and discovery limits ('equivalent counts method'). We demonstrate by comparison with Monte Carlo results that they remain surprisingly accurate even deep in the Poisson regime. We show how correlated background systematics can be efficiently accounted for by a treatment based on Gaussian random fields. Finally, we introduce the novel concept of Fisher information flux. It can be thought of as a generalization of the commonly used signal-to-noise ratio, while accounting for the non-local properties and saturation effects of background and instrumental uncertainties. It is a powerful and flexible tool ready to be used as core concept for informed strategy development in astroparticle physics and searches for particle dark matter.
Strong field tests of gravity with PSR J1141–6545

Abstract The initial results from timing observations of PSR J1141–6545, a relativistic pulsar-white dwarf binary system, are presented. Predictions from the timing baseline hint at the most stringent test of gravity by an asymmetric binary yet. The timing precision has been hindered by the dramatic variations of the pulse profile due to geodetic precession, a pulsar glitch and red timing noise. Methods to overcome such timing irregularities are briefly presented along with preliminary results from the test of the General Theory of Relativity (GR) from this pulsar.
Levitation of quantum Hall critical states in a lattice model with spatially correlated disorder

The fate of the current carrying states of a quantum Hall system is considered in the situation when the disorder strength is increased and the transition from the quantum Hall liquid to the Hall insulator takes place. We investigate a two-dimensional lattice model with spatially correlated disorder potentials and calculate the density of states and the localization length either by using a recursive Green-function method or by direct diagonalization in connection with the procedure of level statistics. From the knowledge of the energy and disorder dependence of the localization length and the density of states (DOS) of the corresponding Landau bands, the movement of the current carrying states in the disorder-energy and disorder-filling-factor planes can be traced by tuning the disorder strength. We show results for all subbands, particularly the traces of the Chern and anti-Chern states as well as the peak positions of the DOS. For small disorder strength W we recover the well-known weak levitation of the critical states, but we also reveal, for larger W, the strong levitation of these states across the Landau gaps without merging. We find the behavior to be similar for exponentially, Gaussian, and Lorentzian correlated disorder potentials. Our study resolves the discrepancies of previously published work in demonstrating the conflicting results to be only special cases of a general lattice model with spatially correlated disorder potentials. To test whether the mixing between consecutive Landau bands is the origin of the observed floating, we truncate the Hilbert space of our model Hamiltonian and calculate the behavior of the current carrying states under these restricted conditions.
Pulsar Emission Physics: The First Fifty Years

Abstract Over the last fifty years since the discovery of pulsars, our understanding of where and how pulsars emit the radiation we observe has undergone significant revision. The location and mechanisms of high-energy radiation are intimately tied to the sites of particle acceleration. The evolution of emission models has paralleled the development of increasingly more sensitive telescopes, especially at high energies. I will review the history of pulsar emission modeling, from the early days of gaps at the polar caps, to outer gaps and slot gaps in the outer magnetosphere, to the present era of global magnetosphere simulations that locate most acceleration and high-energy emission in the current sheets.
Observational Constraints on Correlated Star Formation and Active Galactic Nuclei in Late-stage Galaxy Mergers

Galaxy mergers are capable of triggering both star formation and active galactic nuclei (AGNs) and therefore may represent an important pathway in the co-evolution of galaxies and supermassive black holes (SMBHs). However, correlated enhancements of merger-induced star formation and AGN triggering may be hidden by the variable conditions and timescales during which they occur. In Paper I, we presented evidence of merger-triggered AGN in a sample of six late-stage galaxy mergers ( 2 – 8 kpc nuclear separations). In this follow-up work, we use multi-wavelength Hubble Space Telescope imaging and additional archival data to examine their star-forming properties to test for merger-triggered star formation and if it is correlated with SMBH growth. We find that the morphological asymmetries are correlated with enhanced specific star formation rates, indicating the presence of merger-triggered star formation. Additionally, the stellar populations become younger with increasing radius from the nucleus, indicating that the merger-induced star formation primarily occurs on global scales. However, we also find that the star formation rate enhancements are consistent with or lower than those of larger separation galaxy pair samples. This result is consistent with simulations predicting a decline of the global star formation rates in late-stage galaxy mergers with < 10 kpc nuclear separations. Finally, we find that enhancements in specific star formation rate and AGN luminosity are positively correlated, but that an average temporal delay of ≳ 10 8 years likely exists between the peak of global star formation and the onset of AGN triggering in 80% of the systems.
Hydrodynamical evolution near the QCD critical end point

Phenomenologically, hydrodynamical calculations have been successful in describing global observables in ultrarelativistic heavy-ion collisions, which aim to observe the production of the quark-gluon plasma. On the other hand, theoretically, a lot of evidence that there exists a critical end point (CEP) in the phase diagram of the quantum chromodynamics has been accumulating recently. Nevertheless, so far, no equation of state with the CEP has been employed in hydrodynamical calculations. In this article, we construct the equation of state with the CEP on the basis of the universality hypothesis and show that the CEP acts as an attractor of isentropic trajectories. We also consider the time evolution in the case with the CEP and discuss how the CEP affects the final state observables, such as the correlation length, fluctuation, chemical freeze-out, kinetic freeze-out, and so on. Finally, we argue that the anomalously low kinetic freeze-out temperature at the Relativistic Heavy-Ion Collider at the Brookhaven National Laboratory suggests the possibility of the existence of the CEP.
SOME RECENT OBJECTIONS TO THE BAYESIAN THEORY OF SUPPORT

BLACKMORE, J. T. [1972]: Ernst Mach—His Life, Work 8c Influence. University of California Press. CLARK, P. [1976]: 'Atomism versus Thermodynamics', in Method and Appraisal in the Physical Science, ed. C. Howson, pp. 41-105. Cambridge University Press. CLARK, P. [1982]: 'Matter, Motion & Irreversibility' (Review of S. G. Brush The Kind of Motion We Call Heat) British Journal for the Philosophy of Science, 33, pp. 165-86. FEYERABEND, P. [1980]: 'Zahar on Mach, Einstein and Modern Science', British Journal for the Philosophy of Science, 31, pp. 273—82. GARDNER, M. [1979]: 'Realism and Instrumentalism in 19th Century Atomism', Philosophy of Science, 46, pp. 1—34. LAUDAN, L. [1976]: 'The Methodological Foundation of Mach's Anti-Atomism and Their Historical Roots', in Motion and Time Space and Matter, ed. P. K. Machamer and R. G. Tumbull, pp. 390-417. Ohio State Universtiy Press. MACH, E. [1896]: Die Prindpien der Warmelehre—historisch-kritisch entxcickclt. 4. Auflage 1923. Verlag von Johann Ambrosius Barth. MACH, E. [1910]: 'Die Leitgedanken meiner naturwissenschaftlichen Erkenntnislehre und ihre Aufnahme durch die Zwitgenossen' Physikalische Zeitschrift, n , pp. 599-606. MACH, E. [1919]: Die Leitgedanken meiner naturwissenschaftlichen Erkenntnislehre und ihre Aufnahme durch die Zeitgenossen. Simtliche Elemente und naturzcissenschaftliche Begriffe. Verlag von Johann Ambrosius Barth. MEYER, S. [1950]: 'Die VorgeschichtederGrundungunddasersteJahrzehntdes Institutes fur Radiumforschung' Sitxungsberichte der Osterreichischen Akademie der Wissenschaft, 159, pp. 5-00. NYHOF, J. [1981]: Instrumentalism and Beyond, Doctoral Dissertation, University of Otago, Dunedin, New Zealand. OSTWALD, W. [1901]: Vorlesungen uber Naturphilosophie. 2. Auflage, 1902, p. 4. Verlag von Johann Ambrosius Barth. POPPER, K. R. [1974]: 'Autobiography of Karl Popper', in The Philosophy of Karl Popper, ed. P. A. Schilpp, pp. 156-67. Later published as Unended Quest [1976]. Fifth Impression [1980]. Fontana/Collins. TRAVERS, M. [1951]: Sir William Ramsay, pp. 251—2. London. TREVOR, J. E. [1897]: Journal of Physical Chemistry, 1, p. 431.
Lectures from the CERN Winter School on Supergravity, Strings, and Gauge Theory, CERN, 25–29 January, 2010

This special section is devoted to the proceedings of the CERN Winter School on Supergravity, Strings and Gauge Theory 2010, which took place at CERN in Geneva, Switzerland, from 25–29 January 2010. This event was organized in the tradition of the yearly training schools of the former EC–RTN string network `Constituents, Fundamental Forces and Symmetries of the Universe'. Previous schools in this series were organized in 2005 at SISSA in Trieste and from 2006–2009 at CERN. Other similar schools have been organized in the past by the former related RTN `The Quantum Structure of Spacetime and the Geometric Nature of Fundamental Interactions'. Since 2009, the school has been funded by CERN and the Arnold Sommerfeld Center at Ludwig–Maximilians University of Munich. The event is organized by the Theoretical Physics Division, CERN Physics Department. The 2011 school will take place from 24–28 January 2011. As with its predecessors, this school was meant primarily for training doctoral students and young postdoctoral researchers in recent developments in theoretical high-energy physics and string theory. The programme consisted of five series of pedagogical lectures of four hours each, complemented by tutorial discussion sessions in the afternoons. The school was attended by approximately 140 participants from around the world. The topics of the lecture series were chosen to represent a broad section of current research, from cosmology and string phenomenology to mathematical physics, and gauge theory to properties of quantum black holes. Lecturers were invited based on their expertise and ability to communicate with students.
Communication: Two-structure thermodynamics unifying all scenarios for water anomalies

Anomalous behavior of water in superooled region (namely decrease of density and sharp increase of response functions at atmospheric pressure) are manly associated with either existence of liquid-liquid criticality or re-entering vapor-liquid spinodal into positive pressure. Despite different origin both scenarios introduce divergence of the response functions. We articulate in the communication that the criticality is behind water anomalies, water has normal vapor-liquid spinodal and that the re-entering feature was predicted because of curved density surface as a consequence of existence of critical point. We can proof this by new two structure equation of state with criticality resulting from non-ideal mixing of two states and a background state being modeled by exactly the same equation of state which was deployed for predicting of vapor-liquid spinodal while formulating the re-entering scenario.
The Flowing System Gasdynamics Part 1: On static head in the pipe flowing element

The solution of problem on distribution of static head along the pipe flowing element is submitted. The solution is reached on the basis of consideration of contact interaction of gas and liquid stream with the wall of the pipe flowing element. The expression for distribution of static head along the pipe flowing element is obtained on the basis of usage of three fundamental laws in fluid dynamics: Torricelli formula, Weissbach-Darcy formula and Bernoulli equation. The general solution is obtained for a gas stream. The special case of the obtained solution is retrieved for liquid stream.
$L^{p}$-estimates for solutions to the instationary Navier-Stokes equations in dimension two.

O* Introduction* The regularity of the weak solutions* to the Navier-Stokes-equations is an outstanding problem in the mathematical theory of fluid dynamics. In the three-dimensional case the answer to this question is still unknown in general, though definite answers have been given in the case of small data for arbitrary large times, and in the case of large data and small time intervals, cf. the remarks in [4, Chap. 6]. In the two-dimensional case the problem is much easier to settle: it is well-known that the (unique) weak solution to the Navier-Stokes-equations is regular provided the data are smooth enough. However, the answer is not quite satisfactory since the results of the Z^-theory of the nonstationary hydrodynamic potentials have not been carried over to the Navier-Stokes-equations, e.g., to prove that the solution has square integrable second derivatives one has not only to assume that the external force is square integrable but also that it has a square integrable time derivative. Recently, v. Wahl filled this gap in proving that in dimension two the solution of the Navier-Stokes-equations has r-summable second derivatives if the right-hand side of the system is r-summable for 2 <̂ r < oo. Actually, he gave a detailed proof in the case r = 2, and indicated the steps necessary to prove the general result. The aim of this paper is to give a simple proof of v. WahΓs result. To prove the . [/-estimates for arbitrary r ^ 2 we apply the results of Solonnikov [7, § 17] valid for the linear Stokesequations. In the interesting case r = 2 we shall give an elementary proof relying only on GronwalΓs inequality and a well-known interpolation theorem of Nirenberg. In this case we shall obtain an a priori estimate which does not depend on time explicitly. From this result we deduce a number of interesting conclusions concerning the solu-
Fundamentals of the KRAKEN code. [Eulerian hydrodynamics code for compressible nonviscous flow of several fluids in two-dimensional (axially symmetric) region]

KRAKEN is an Eulerian hydrodynamics code capable of treating compressible nonviscous flow of several fluids in a two-dimensional (axially symmetric) region. In many respects it is reminiscent of the FLIC/PIC methods, although it is considerably different in detail. Both Lagrangian and advection (transport) phases of the problem are considered. The code has a straight-forward approach to differencing. The presently used version of the code is discussed; it is hoped that a more efficient version will soon be completed. (RWR)
Cosmological constant vis-à-vis dynamical vacuum: Bold challenging the ΛCDM

Next year we will celebrate 100 years of the cosmological term, Λ, in Einstein’s gravitational field equations, also 50 years since the cosmological constant problem was first formulated by Zeldovich, and almost about two decades of the observational evidence that a nonvanishing, positive, Λ-term could be the simplest phenomenological explanation for the observed acceleration of the Universe. This mixed state of affairs already shows that we do no currently understand the theoretical nature of Λ. In particular, we are still facing the crucial question whether Λ is truly a fundamental constant or a mildly evolving dynamical variable. At this point the matter should be settled once more empirically and, amazingly enough, the wealth of observational data at our disposal can presently shed true light on it. In this short review, I summarize the situation of some of these studies. It turns out that the Λ = const. hypothesis, despite being the simplest, may well not be the most favored one when we put it in hard-fought competition with specific dynamical models of the vacuum energy. Recently, it has been shown that the overall fit to the cosmological observables SNIa+BAO+H(z)+LSS+BBN+CMB do favor the class of “running” vacuum models (RVM’s) — in which Λ = Λ(H) is a function of the Hubble rate — against the “concordance” ΛCDM model. The support is at an unprecedented level of ∼ 4σ and is backed up with Akaike and Bayesian criteria leading to compelling evidence in favor of the RVM option and other related dynamical vacuum models. I also address the implications of this framework on the possible time evolution of the fundamental constants of Nature.
Robust subpixel image registration of different-exposed images

Proposed is a new robust image registration method that can perform subpixel image registration for different-exposed images with highly photometric distortion. In this method, phase congruency is used to eliminate the effects of illumination change and photometric distortion for image registration using the phase correlation technique. Considering the presence of non-overlapped regions owing to photometric distortion, evolutionary programming is applied to search for the accurate translation parameters. Experimental results show that the proposed method is efficient and robust against illumination change and photometric distortion.
Synchrotron X-ray Powder Diffraction Studies in Pulsed Magnetic Fields

X‐ray powder diffraction experiments under pulsed magnetic fields were carried out at the DUBBLE beamline (BM26B) at the ESRF. A mobile generator delivered 110kJ to the magnet coil, which was sufficient to generate peak fields of 30T. A liquid He flow cryostat allowed us to vary the sample temperature accurately between 8K and 300K.
Rotation and accretion of very low mass objects in the sigma Ori cluster

We report on two photometric monitoring campaigns of Very Low Mass (VLM) objects in the young open cluster around σ Orionis. Our targets were pre-selected with multi-filter photometry in a field of 0.36 sqdeg. For 23 of these objects, spanning a mass range from 0.03 to 0.7 M� , we detect periodic variability. Of these, 16 exhibit low-level variability, with amplitudes of less than 0.2 mag in the I-band, which is mostly well-approximated by a sine wave. These periodicities are probably caused by photospheric spots co-rotating with the objects. In contrast, the remaining variable targets show high- level variability with amplitudes ranging from 0.25 to 1.1 mag, consisting of a periodic light variation onto which short-term fluctuations are superimposed. This variability pattern is very similar to the photometric behaviour of solar-mass, classical T Tauri stars. Low-resolution spectra of a few of these objects reveal strong Hα and Ca-triplet emission, indicative of ongoing accretion processes. This suggests that 5−7% of our targets still possess a circumstellar disk. In combination with previous results for younger objects, this translates into a disk lifetime of 3−4 Myr, significantly shorter than for solar mass stars. The highly variable objects rotate on average slower than the low-amplitude variables, which is expected in terms of a disk-locking scenario. There is a trend towards faster rotation with decreasing mass, which might be caused by shortening of the disk lifetimes or attenuation of magnetic fields.