Miracle-dz/UniFAR-FTUs huggingface dataset:
The Fundamental Plane for z = 0.8-0.9 Cluster Galaxies

We present the fundamental plane (FP) for 38 early-type galaxies in the two rich galaxy clusters RX J0152.7-1357 (z = 0.83) and RX J1226.9+3332 (z = 0.89), reaching a limiting magnitude of MB = -19.8 in the rest frame of the clusters. While the zero-point offset of the FP for these high-redshift clusters relative to our low-redshift sample is consistent with passive evolution with a formation redshift of zform ≈ 3.2, the FP for the high-redshift clusters is not only shifted as expected for a mass-independent zform but rotated relative to the low-redshift sample. Expressed as a relation between the galaxy masses and the mass-to-light ratios, the FP is significantly steeper for the high-redshift clusters than for our low-redshift sample. We interpret this as a mass dependency of the star formation history, as has been suggested by other recent studies. The low-mass galaxies (1010.3 M☉) have experienced star formation as recently as z ≈ 1.35 (1.5 Gyr prior to their look-back time), while galaxies with masses larger than 1011.3 M☉ had their last major star formation episode at z > 4.5.
The Vacuum Polarization tensor in 1+1 dimensional space-time

Quantum field theory (QFT) is supposed to be gauge invariant. However it has been well established that a direct calculation of the vacuum polarization tensor produces a non-gauge invariant result. In this paper it will be shown that this problem is due to the fact that there is a lower bound to the free field energy in QFT. The vacuum polarization tensor will be calculated in 1+1 dimensional space-time and is shown not to be gauge invariant. The gauge invariance of the theory can be restored through a regularization procedure which eliminates the non-gauge invariant terms. However it will be shown that this will impact the free field energy. If the free field energy is defined so that the vacuum state has an energy of zero then the impact of regularization is to introduce states whose free field energy is less than zero.
Entanglement in relativistic quantum field theory

I present some general ideas about quantum entanglement in relativistic quantum field theory, especially entanglement in the physical vacuum. Here, entanglement is defined between different single particle states (or modes), parametrized either by energy-momentum together with internal degrees of freedom, or by spacetime coordinate together with the component index in the case of a vector or spinor field. In this approach, the notion of entanglement between different spacetime points can be established. Some entanglement properties are obtained as constraints from symmetries, e.g., under Lorentz transformation, space inversion, time reverse, and charge conjugation.
Diffuse radio sources in clusters of galaxies: models and long-wavelength radio observations

Abstract Clusters of galaxies contain several types of diffuse radio sources with very steep radio spectra which are associated with the cluster environment, including central radio bubbles, cluster radio relics, and cluster radio halos. Radio halos and relics are found only in merging clusters. Cluster radio relics may be produced by particle acceleration in merger shocks, while radio halos, may result from electron re-acceleration by turbulence produced by mergers. Secondary production of electrons and positrons by hadronic interactions also plays a role. If cluster radio halos and relics are related to mergers, then deep low frequency radio surveys could detect 1000's of clusters. Long-wavelength radio observations have a great potential to help us understand clusters and large scale structure, and can provide a diagnostic of cluster mergers, which affect the use of clusters in cosmological and dark energy studies.
Three-dimensional vortex structure of a fast rotating Bose-Einstein condensate with harmonic-plus-quartic confinement

We address the challenging proposition of using real experimental parameters in a three-dimensional (3D) numerical simulation of fast rotating Bose-Einstein condensates. We simulate recent experiments [V. Bretin, S. Stock, Y. Seurin, and J. Dalibard, Phys. Rev. Lett. 92, 050403 (2004); S. Stock, V. Bretin, S. Stock, F. Chevy, and J. Dalibard, Europhys. Lett. 65, 594 (2004)] using an anharmonic (quadratic-plus-quartic) confining potential to reach rotation frequencies $(\ensuremath{\Omega})$ above the trap frequency $({\ensuremath{\omega}}_{\ensuremath{\perp}})$. Our numerical results are obtained by propagating the 3D Gross-Pitaevskii equation in imaginary time. For $\ensuremath{\Omega}\ensuremath{\leqslant}{\ensuremath{\omega}}_{\ensuremath{\perp}}$, we obtain an equilibrium vortex lattice similar (as the size and number of vortices) to experimental observations. For $\ensuremath{\Omega}g{\ensuremath{\omega}}_{\ensuremath{\perp}}$ we observe the evolution of the vortex lattice into an array of vortices with a central hole. Since this evolution was not visible in experiments, we investigate the 3D structure of vortex configurations and 3D effects on vortex contrast. Numerical data are also compared to recent theory [D. E. Sheehy and L. Radzihovsky, Phys. Rev. A 70, 063620 (2004)] describing vortex lattice inhomogeneities and a remarkably good agreement is found.
Voids of dark energy

We investigate the clustering properties of a dynamical dark energy component. In a cosmic mix of a pressureless fluid and a light scalar field, we follow the linear evolution of spherical matter perturbations. We find that the scalar field tends to form underdensities in response to the gravitationally collapsing matter. We thoroughly investigate these voids for a variety of initial conditions, explain the physics behind their formation, and consider possible observational implications. Detection of dark energy voids will clearly rule out the cosmological constant as the main source of the present acceleration.
Charged Higgs pair production in association with the 
Z0
 boson at electron-positron colliders

In this paper, the production of the charged Higgs pair associated with the ${Z}^{0}$ boson is analyzed in the minimal extension of the standard model, the so-called two-Higgs-doublet model. The process ${e}^{+}{e}^{\ensuremath{-}}\ensuremath{\rightarrow}{H}^{+}{H}^{\ensuremath{-}}{Z}^{0}$ is calculated at the tree level including all the possible diagrams in the two-Higgs-doublet model. The numerical analysis is performed in consideration of the current experimental constraints and various scenarios for the free parameters of the model. The results are presented as a function of the center-of-mass energy, the charged Higgs mass (${m}_{{H}^{\ifmmode\pm\else\textpm\fi{}}}$), and the ratio of the vacuum expectation values (${t}_{\ensuremath{\beta}}$). The unpolarized cross section, taking into account the results in the flavor physics, gets up to 0.278 fb for ${m}_{{H}^{\ifmmode\pm\else\textpm\fi{}}}=175\text{ }\text{ }\mathrm{GeV}$, and it declines with decreasing ${m}_{{H}^{\ifmmode\pm\else\textpm\fi{}}}$ in type I. However, it gets down to 0.073 fb for ${m}_{{H}^{\ifmmode\pm\else\textpm\fi{}}}=500\text{ }\text{ }\mathrm{GeV}$ in type II. Further, the calculation is also carried out in the nonalignment scenario and low-${m}_{{h}^{0}}$ scenario. The effect of the polarized incoming ${e}^{+}$ and ${e}^{\ensuremath{-}}$ beams shows that the cross section is enhanced by a factor up to 2.5 at $\mathrm{P}(+0.60,\ensuremath{-}0.80)$ polarization configuration. Decay channels of the charged Higgs, possible final states of the process, and some differential distributions belonging to the charged Higgs and ${Z}^{0}$ boson are examined for each scenario. The analysis shows that some channels have a higher branching ratio such as ${H}^{+}\ensuremath{\rightarrow}t\overline{b}$, ${H}^{+}\ensuremath{\rightarrow}{W}^{+}{h}^{0}$, and ${H}^{+}\ensuremath{\rightarrow}{W}^{+}{H}^{0}$. These decay channels are essential in the charged Higgs searches at the lepton colliders for the scenarios interested. The detection of the charged Higgs is a powerful sign for the extended scalar sectors, and the results show the potential of a future lepton collider.
Planetary Engulfment in the Hertzsprung–Russell Diagram

Planets accompany most Sun-like stars. The orbits of many are sufficiently close that they will be engulfed when their host stars ascend the giant branch. This Letter compares the power generated by orbital decay of an engulfed planet to the intrinsic stellar luminosity. Orbital decay power is generated by drag on the engulfed companion by the surrounding envelope. As stars ascend the giant branch their envelope density drops and so does the power injected through orbital decay, scaling approximately as . Their luminosity, however, increases along the giant branch. These opposed scalings indicate a crossing, where . We consider the engulfment of planets along isochrones in the Hertzsprung–Russell (H–R) diagram. We find that the conditions for such a crossing occur around (or au) for Jovian planetary companions. The consumption of closer-in giant planets, such as hot Jupiters, leads to , while more distant planets such as warm Jupiters, , lead to minor perturbations of their host stars with . Our results map out the parameter space along the giant branch in the H–R Diagram where interaction with planetary companions leads to significant energetic disturbance of host stars.
A high precision semi-analytic mass function

In this paper, extending past works of Del Popolo, we show how a high precision mass function (MF) can be obtained using the excursion set approach and an improved barrier taking implicitly into account a non-zero cosmological constant, the angular momentum acquired by tidal interaction of proto-structures and dynamical friction. In the case of the ΛCDM paradigm, we find that our MF is in agreement at the 3% level to Klypin's Bolshoi simulation, in the mass range Mvir = 5 × 109 h−1M⊙–−5 × 1014 h−1M⊙ and redshift range 0 ≲ z ≲ 10. For z = 0 we also compared our MF to several fitting formulae, and found in particular agreement with Bhattacharya's within 3% in the mass range 1012–1016 h−1M⊙. Moreover, we discuss our MF validity for different cosmologies.
Fast relaxation in a fragile liquid under pressure

The incoherent dynamic structure factor of ortho-terphenyl has been measured by neutron time-of-flight and backscattering technique in the pressure range from 0.1 MPa to 240 MPa for temperatures between 301 K and 335 K. Tagged-particle correlations in the compressed liquid decay in two steps. The alpha-relaxation lineshape is independent of pressure, and the relaxation time proportional to viscosity. A kink in the amplitude f_Q(P) reveals the onset of beta relaxation. The beta-relaxation regime can be described by the mode-coupling scaling function; amplitudes and time scales allow a consistent determination of the critical pressure P_c(T). alpha and beta relaxation depend in the same way on the thermodynamic state; close to the mode-coupling cross-over, this dependence can be parametrised by an effective coupling Gamma ~ n*T**{-1/4}.
Invariance properties of boundary sets of open embeddings of manifolds and their application to the abstract boundary

The {\em abstract boundary\/} (or {\em {\em a\/}-boundary\/}) of Scott and Szekeres \cite{Scott94} constitutes a ``boundary'' to any $n$-dimensional, paracompact, connected, Hausdorff, $C^\infty$-manifold (without a boundary in the usual sense). In general relativity one deals with a {\em space-% time\/} $(\cM,g)$ (a 4-dimensional manifold $\cM$ with a Lorentzian metric $g$), together with a chosen preferred class of curves in $\cM$. In this case the {\em a\/}-boundary points may represent ``singularities'' or ``points at infinity''. Since the {\em a\/}-boundary itself, however, does not depend on the existence of further structure on the manifold such as a Lorentzian metric or connection, it is possible for it to be used in many contexts. In this paper we develop some purely topological properties of abstract boundary sets and abstract boundary points ({\em a\/}-boundary points). We prove, amongst other things, that compactness is invariant under boundary set equivalence, and introduce another invariant concept ({\em isolation\/}), which encapsulates the notion that a boundary set is ``separated'' from other boundary points of the same embedding. [The abstract continues in paper proper - truncated to fit here. ]
The Internal‐Viscosity Dumbbell in the High‐IV Limit: Implications for Rheological Modeling

The internal viscosity (IV) polymer chain model, which features an interbead connector functioning as a Hookean spring and a dashpot in parallel, is examined for the case of dumbbells (N=2) in the limit of very high IV. When the IV parameter Φ becomes very large, the moments of the configurational diffusion equation become identical to those of the rigid rod, thus establishing equivalence of rheological predictions for these two models. Next, an approximate linearization (preaveraging) technique for computing bead deformational and rotational velocities—previously found to give useful results in the limit Φ→0—is examined also in the limit Φ→∞. Predictions for non‐Newtonian viscosity and first normal stress coefficient are made using both the exact and approximate methods. Major differences are found, with the approximate method leading to an unrealistic (Newtonian) viscosity and vanishing normal stress, thus casting doubt on earlier results obtained with this method for high‐N chains with large Φ. For the.
A generalized Weyl relation approach to the time operator and its connection to the survival probability

The time operator, an operator which satisfies the canonical commutation relation with the Hamiltonian, is investigated, on the basis of a certain algebraic relation for a pair of operators T and H, where T is symmetric and H self-adjoint. This relation is equivalent to the Weyl relation, in the case of self-adjoint T, and is satisfied by the Aharonov–Bohm time operator T0 and the free Hamiltonian H0 for the one-dimensional free-particle system. In order to see the qualitative properties of T0, the operators T and H satisfying this algebraic relation are examined. In particular, it is shown that the standard deviation of T is directly connected to the survival probability, and H is absolutely continuous. Hence, it is concluded that the existence of the operator T implies the existence of scattering states. It is also shown that the minimum uncertainty states do not exist. Other examples of these operators T and H, than the one-dimensional free-particle system, are demonstrated.
Testing supersymmetry with lepton flavor violating τ and μ decays

In this work the following lepton flavor violating {tau} and {mu} decays are studied: {tau}{sup -}{yields}{mu}{sup -}{mu}{sup -}{mu}{sup +}, {tau}{sup -}{yields}e{sup -}e{sup -}e{sup +}, {mu}{sup -}{yields}e{sup -}e{sup -}e{sup +}, {tau}{sup -}{yields}{mu}{sup -}{gamma}, {tau}{sup -}{yields}e{sup -}{gamma}, and {mu}{sup -}{yields}e{sup -}{gamma}. We work in a supersymmetric scenario consisting of the minimal supersymmetric standard model particle content, extended by the addition of three heavy right-handed Majorana neutrinos and their supersymmetric partners, and where the generation of neutrino masses is done via the seesaw mechanism. Within this context, a significant lepton flavor mixing is generated in the slepton sector due to the Yukawa neutrino couplings, which is transmitted from the high to the low energies via the renormalization group equations. This slepton mixing then generates via loops of supersymmetric particles significant contributions to the rates of l{sub j}{yields}3l{sub i} and the correlated l{sub j}{yields}l{sub i}{gamma} decays. We analyze here in full detail these rates in terms of the relevant input parameters, which are the usual minimal supergravity parameters and the seesaw parameters. For the l{sub j}{yields}3l{sub i} decays, a full one-loop analytical computation of all the contributing supersymmetric loops is presented. This completes and corrects previous computations in the literature. In the numerical analysismore » compatibility with the most recent experimental upper bounds on all these {tau} and {mu} decays, with the neutrino data, and with the present lower bounds on the supersymmetric particle masses are required. Two typical scenarios with degenerate and hierarchical heavy neutrinos are considered. We will show here that the minimal supergravity and seesaw parameters do get important restrictions from these {tau} and {mu} decays in the hierarchical neutrino case. « less
Floquet-Mode Solutions of Space-Time Modulated Huygens' Metasurfaces

A rigorous Floquet mode analysis is proposed for a zero thickness space-time modulated Huygens' metasurface to model and determine the strengths of the new harmonic components of the scattered fields. The proposed method is based on Generalized Sheet Transition Conditions (GSTCs) treating a metasurface as a spatial discontinuity. The metasurface is described in terms of Lorentzian electric and magnetic surface susceptibilities, $\chi_\text{ee}$ and $\chi_\text{mm}$, respectively, and its resonant frequencies are periodically modulated in both space and time. The unknown scattered fields are then expressed in terms of Floquet modes, which when used with the GSTCs, lead to a system of field matrix equations. The resulting set of linear equations are then solved numerically to determine the total scattered fields. Using a finite-difference time domain (FDTD) solver, the proposed method is validated and confirmed for several examples of modulation depths ($\Delta_p$) and frequencies ($\omega_p$). Finally, the computed steady-state scattered fields are Fourier propagated analytically, for visualization of refracted harmonics. The proposed method is simple and versatile and able to determine the steady-state response of a space-time modulated Huygen's metasurface, for arbitrary modulation frequencies and depths.
EXACT POTENTIAL AND SCATTERING AMPLITUDES FROM THE TACHYON NONLINEAR BETA FUNCTION

We compute, on the disk, the non-linear tachyon β-function, βT, of the open bosonic string theory. βT is determined both in an expansion to the third power of the field and to all orders in derivatives and in an expansion to any power of the tachyon field in the leading order in derivatives. We construct the Witten-Shatashvili (WS) space-time effective action S and prove that it has a very simple universal form in terms of the renormalized tachyon field and βT. The expression for S is well suited to studying both processes that are far off-shell, such as tachyon condensation, and close to the mass-shell, such as perturbative on-shell amplitudes. We evaluate S in a small derivative expansion, providing the exact tachyon potential. The normalization of S is fixed by requiring that the field redefinition that maps S into the tachyon effective action derived from the cubic string field theory is regular on-shell. The normalization factor is in precise agreement with the one required for verifying all the conjectures on tachyon condensation. The coordinates in the space of couplings in which the tachyon β-function is non linear are the most appropriate to study RG fixed points that can be interpreted as solitons of S, i.e. D-branes.
Specification of Monthly Precipitation over the United States from the Surrounding 700 mb Height Field

Abstract The relations between monthly precipitation in each of 60 climate divisions in the contiguous United States and the simultaneous field of monthly mean 700 mb height over North America and vicinity were investigated for both frequency and amount by applying a stepwise forward regression procedure to 30 years of data from January 1951 to December 1980. For winter, a good grid for specifying precipitation from 700 mb heights was found to consist of 79 points located every 5° of latitude from 20°–60°N and every 10° of longitude from 45°–150°W. Best results were obtained by expressing all data as ordinary anomalies and by pooling all cases for December, January and February. Fitting monthly totals by a gamma distribution and classifying into 21 percentiles gave as good results as those obtained by any other transformation of precipitation amount, with almost 42 percent of the precipitation variance, nationwide, explained by less than 3 heights. However, this was not as good as the 45 percent explained.
A New Constraint on Reionization from the Evolution of the Lyα Luminosity Function at z ∼ 6–7 Probed by a Deep Census of z = 7.0 Lyα Emitter Candidates to 0.3L*

We detect 20 z = 7.0 Lyα emitter (LAE) candidates to L(Lyα) ∼ 2 × 1042 erg s−1 or 0.3 L z = 7 * and in a volume of 6.1 × 105 Mpc3 in the Subaru Deep Field and the Subaru/XMM-Newton Deep Survey field by 82 hr and 37 hr of Subaru Suprime-Cam narrowband NB973 and reddest optical y-band imaging. We compare their Lyα and UV luminosity functions (LFs) and densities and Lyα equivalent widths (EWs) to those of z = 5.7, 6.6, and 7.3 LAEs from previous Suprime-Cam surveys. The Lyα LF (density) rapidly declines by a factor of ×1.5 (1.9) in L(Lyα) at z = 5.7–6.6 (160 Myr), ×1.5 (1.6) at z = 6.6–7.0 (60 Myr) at the faint end, and ×2.0 (3.8) at z = 7.0–7.3 (40 Myr). Also, in addition to the systematic decrease in EW at z = 5.7–6.6 previously found, two-thirds of the z = 7.0 LAEs detected in the UV continuum exhibit lower EWs than the z = 6.6 ones. Moreover, while the UV LF and density do not evolve at z = 5.7–6.6, they modestly decline at z = 6.6–7.0, implying galaxy evolution contributing to the decline of the Lyα LF. Comparison of the z = 7.0 Lyα LF to the one predicted by an LAE evolution model further reveals that galaxy evolution alone cannot explain all of the decline of the Lyα LF. If we attribute the discrepancy to Lyα attenuation by neutral hydrogen, the intergalactic medium transmission of Lyα photons at z = 7.0 would be T Ly α IGM ≤ 0.6 – 0.7 . It is lower (higher) than the T Ly α IGM at z = 6.6 (7.3) derived by previous studies, suggesting rapid increase in neutral fraction at z > 6.
Magnetic anisotropy in prismatic nickel nanowires

Nickel nanowire arrays with a diamond-shaped cross section and the same orientation have been fabricated in nanoporous single mica crystal membranes by electrodeposition. All wires are 5 μm long with an effective diameter of 120 nm. The sample can be considered as a collection of laterally and vertically aligned identical micromagnetic prisms. We report on the magnetic anisotropy due to the quasi-one-dimensional wire shape and diamond cross section.
Estimating the power spectrum of the cosmic microwave background

We develop two methods for estimating the power spectrum, C_l, of the cosmic microwave background (CMB) from data and apply them to the COBE/DMR and Saskatoon datasets. One method involves a direct evaluation of the likelihood function, and the other is an estimator that is a minimum-variance weighted quadratic function of the data. Applied iteratively, the quadratic estimator is not distinct from likelihood analysis, but is rather a rapid means of finding the power spectrum that maximizes the likelihood function. Our results bear this out: direct evaluation and quadratic estimation converge to the same C_ls. The quadratic estimator can also be used to directly determine cosmological parameters and their uncertainties. While the two methods both require O(N^3) operations, the quadratic is much faster, and both are applicable to datasets with arbitrary chopping patterns and noise correlations. We also discuss approximations that may reduce it to O(N^2) thus making it practical for forthcoming megapixel datasets.