Miracle-dz/UniFAR-FTUs huggingface dataset:
Universal fault-tolerant quantum computation with Bacon-Shor codes

We present a fault-tolerant universal gate set consisting of Hadamard and controlled-controlled-Z (CCZ) on Bacon-Shor subsystem codes. Transversal non-Clifford gates on these codes are intriguing in that higher levels of the Clifford hierarchy become accessible as the code becomes more asymmetric. For instance, in an appropriate gauge, Bacon-Shor codes on an $m\times m^k$ lattice have transversal $k$-qubit-controlled $Z$. Through a variety of tricks, including intermediate error-correction and non-Pauli recovery, we reduce the overhead required for fault-tolerant CCZ. We calculate pseudothresholds for our universal gate set on the smallest $3\times3$ Bacon-Shor code and also compare our gates with magic-states within the framework of a proposed ion trap architecture.
Neutrino-nucleus reactions on 
O16
 based on new shell-model Hamiltonians

Neutrino-induced reactions on O are investigated by shell-model calculaions with new shellmodel Hamiltonians, which can describe well the structure of p-shell and p-sd shell nuclei. Distribution of the spin-dipole strengths in O, which give major contributions to the ν-O reaction cross sections, is studied with the new Hamiltonians. Muon-capture reaction rates on O are also studied to discuss the quenching of the axial-vector coupling in nuclear medium. Charged-current and neutral-current reaction cross sections are evaluated in various particle and γ emission channels as well as the total ones at neutrino energies up to Eν ≈ 100 MeV. Branching ratios for the various channels are obtained by the Hauser-Feshbach statistical model calculations, and partial cross sections for singleand multi-particle emission channels are evaluated. The cross sections updated are compared with previous continuum random phase approximation (CRPA) calculations. Effects of multi-particle emission channels on nucleosynthesis in core-collapse supernova (SN) explosions are investigated. Inclusion of αp emission channels is found to lead to an enhancement of production yields of B and C through O (ν, ν’ αp) B and O (ν, e αp) C reactions, respectively. PACS numbers: 25.30. -c, 21.60. Cs, 25.40. Kv, 26.30. -k, 26.30. Jk, 27.20. +n
A Petrov type I cylindrically symmetric solution for perfect fluid in steady rigid body rotation

A stationary cylindrically symmetric solution of Einstein's equations is given for a perfect fluid in rigid body rotation about a regular axis. The fluid has the equation of state with pressure p and density finite and steadily decreasing to zero as the radial coordinate . The spacetime is free of singularities and of Petrov type I.
Ultraviolet Detection of the Binary Companion to the Type IIb SN 2001ig

We present HST/WFC3 ultraviolet imaging in the F275W and F336W bands of the Type IIb SN 2001ig at an age of more than 14 years. A clear point source is detected at the site of the explosion, with mF275W = 25.39 ± 0.10 and mF336W = 25.88 ± 0.13 mag. Despite weak constraints on both the distance to the host galaxy NGC 7424 and the line-of-sight reddening to the supernova, this source matches the characteristics of an early B-type main-sequence star with 19,000 < Teff < 22,000 K and . A BPASS v2.1 binary evolution model, with primary and secondary masses of 13 M⊙ and 9 M⊙, respectively, is found to simultaneously resemble, in the Hertzsprung–Russell diagram, both the observed location of this surviving companion, and the primary star evolutionary endpoints for other Type IIb supernovae. This same model exhibits highly variable late-stage mass loss, as expected from the behavior of the radio light curves. A Gemini/GMOS optical spectrum at an age of 6 years reveals a narrow He ii λ4686 emission line, indicative of continuing interaction with a dense circumstellar medium at large radii from the progenitor. We review our findings on SN 2001ig in the context of binary evolution channels for stripped-envelope supernovae. Owing to the uncrowded nature of its environment in the ultraviolet, this study of SN 2001ig represents one of the cleanest detections to date of a surviving binary companion to a Type IIb supernova.
A search for signatures of Europa’s atmosphere and plumes in Galileo charged particle data

Remote sensing observations indicate that Europa is surrounded by a tenuous atmosphere. Furthermore, recent observations and historic data from Galileo hint at the occurrence of water vapour eruptions originating from the interior that create 200 km high plumes. Due to the lack of adequate measurements large uncertainties exist in the properties of Europa’s atmosphere (e.g. loss rate and structure) and plumes (e.g. structure, source location, duration), of the latter one the existence is not even confirmed. Unexploited opportunities to constrain properties of the atmosphere or plumes remain in the in-situ data collected by the Galileo mission, the only mission that has surveyed Europa from close by. In this thesis, I investigate how to constrain the properties (density, scale height) of Europa’s tenuous atmosphere and plumes, using data from the Galileo in-situ particle detector instruments (PLS, EPD). First, I analyse and compare the flybys, with a focus on the E12 flyby as it demonstrates the strongest signs of interaction of the atmosphere and the magnetospheric environment. Next, I simulate the depletion of energetic protons and oxygen ions measured during the E12 flyby. A Monte Carlo particle tracing method is used to simulate the particle trajectories and determine where they are depleted: at the surface or in the atmosphere. The simulations show that the depletions of energetic ions observed in the range 80 to 540 keV can be explained by charge exchange with neutral atmospheric particles, but not by impact on the surface alone. This suggests that an atmosphere must have been present during the E12 flyby. The simulations best represent the sublimated component of the atmosphere and favour higher surface densities than the literature, but are not sensitive to the scale height. Furthermore, an additional depletion is visible very briefly in the energetic protons with energies from 540 to 1040 keV. This feature could be consistent with localized losses from a Europa plume, although such a solution is not unique.
Dynamical fermion mass generation at a tricritical point in strongly coupled U(1) lattice gauge theory

Fermion mass generation in the strongly coupled U(1) lattice gauge theory with fermion and scalar fields of equal charge is investigated by means of numerical simulation with dynamical fermions. The chiral symmetry of this model is broken by the gauge interaction and restored by the light scalar. We present evidence for the existence of a particular, tricritical point of the corresponding phase boundary where the continuum limit might possibly be constructed. It is of interest as a model for dynamical symmetry breaking and mass generation due to a strong gauge interaction. In addition to the massive and unconfined fermion $F$ and Goldstone boson $\ensuremath{\pi},$ a gauge ball of mass ${m}_{S}\ensuremath{\simeq}{1/2m}_{F},$ and some other states are found. The tricritical exponents appear to be nonclassical.
New Approach to Evolving Gravitational Waves in Loop Quantum Cosmology.

With the observational advance in recent years, primordial gravitational waves (GWs), known as the tensor-mode cosmic perturbations, in the Loop Quantum Cosmology (LQC) are becoming testable and thus require better framework through which to bridge between the observations and the theories. In this work we present a new formalism that employs the transfer functions to bring the GWs from any epoch, even before the quantum bounce, to a later time, including the present. The evolutionary epochs considered here include the possible deflation, quantum bounce, and inflation. This formalism enables us to predict more accurately the GW power spectrum today. With the ADM formalism for the LQC background dynamics, our approach is equivalent to the commonly used Bogoliubov transformations for evolving the primordial GWs, but more transparent for discussions and easier to calculate due to its nature of being linear algebra dealing with linear perturbations. We utilize this advantage to have resolved the IR suppression problem. We also propose the field-free approximation for the effective mass in the quantum bounce epoch to largely improve the accuracy in the predicted GW power spectrum. Our transfer-function formalism is general in dealing with any linear problems, and thus expected to be equally useful under other context with linearity.
Carbon Stars Identified from LAMOST DR4 Using Machine Learning

In this work, we present a catalog of 2651 carbon stars from the fourth Data Release (DR4) of the Large Sky Area Multi-Object Fiber Spectroscopy Telescope (LAMOST). Using an efficient machine-learning algorithm, we find these stars from more than 7 million spectra. As a by-product, 17 carbon-enhanced metal-poor turnoff star candidates are also reported in this paper, and they are preliminarily identified by their atmospheric parameters. Except for 176 stars that could not be given spectral types, we classify the other 2475 carbon stars into five subtypes: 864 C-H, 226 C-R, 400 C-J, 266 C-N, and 719 barium stars based on a series of spectral features. Furthermore, we divide the C-J stars into three subtypes, C-J(H), C-J(R), and C-J(N), and about 90% of them are cool N-type stars as expected from previous literature. Besides spectroscopic classification, we also match these carbon stars to multiple broadband photometries. Using ultraviolet photometry data, we find that 25 carbon stars have FUV detections and that they are likely to be in binary systems with compact white dwarf companions.
Modeling ionized gas in low-metallicity environments: the Local Group dwarf galaxy IC 10

Context. Star formation activity is an important driver of galaxy evolution and is influenced by the physical properties of the interstellar medium. Dwarf galaxies allow us to understand how the propagation of radiation and the physical conditions of the different ISM phases are affected by the low-metallicity environment. Aims. Our objective is to investigate the physical properties of the ionized gas of the low-metallicity dwarf galaxy, IC 10, at various spatial scales: from individual H II regions to the entire galaxy scale and examine whether diagnostics for integrated measurements introduce bias in the results. Methods. We modeled the ionized gas combining the mid- and far-infrared fine-structure cooling lines observed with Spitzer/IRS and Herschel/PACS, with the photoionization code CLOUDY. The free parameters of the models are the age of the stellar cluster, the density, and the ionization parameter of the ionized gas as well as the depth of the cloud. The latter is used to investigate the leakage of the ionizing photons from the analyzed regions of IC 10. We investigated H II regions in the main star-forming body, on scales of ~25 pc, three in the main star-forming region in the center of the galaxy and two on the first arc. We then considered larger sizes on the scale of ~200 pc. Results. Most clumps have almost-identical properties, density ~102–102.6 cm−3, ionization parameter between 10−2.2 and 10−1.6, and age of the stellar cluster ~5.5 Myr. All of them are matter-bounded regions, allowing ionizing photons to leak. The relatively uniform physical properties of the clumps suggest a common origin for their star formation activity, which could be related to the feedback from stellar winds or supernovae of a previous generation of stars. The properties derived for ~200 pc size “zones” have similar properties as the H II regions they encompass, but with the larger regions tending to be more radiation bounded. Finally, we investigated the fraction of [CII] 157.7 μm, [SiII] 34.8 μm and [FeII] 25.9 μm emission arising from the ionized gas phase and we find that most of the emission originates from the neutral gas, not from the ionized gas.
Color Dispersion as an Indicator of Stellar Population Complexity: Insights from the Pixel Color–Magnitude Diagrams of 32 Bright Galaxies in Abell 1139 and Abell 2589

We investigate the properties of bright galaxies of various morphological types in Abell 1139 and Abell 2589, using pixel color–magnitude diagram (pCMD) analysis. The sample contains 32 galaxies brighter than Mr = −21.3 mag with spectroscopic redshifts, which are deeply imaged in the g and r bands using the MegaCam mounted on the Canada–France–Hawaii Telescope. After masking contaminants with two-step procedures, we examine how the detailed properties in the pCMDs depend on galaxy morphology and infrared color. The mean g − r color as a function of surface brightness (μr) in the pCMD of a galaxy shows good performance in distinguishing between early- and late-type galaxies, but it is not perfect because of the similarity between elliptical galaxies and bulge-dominated spiral galaxies. On the other hand, the g − r color dispersion as a function of μr works better. We find that the best set of parameters for galaxy classification is a combination of the minimum color dispersion at μr ≤ 21.2 mag arcsec−2 and the maximum color dispersion at 20.0 ≤ μr ≤ 21.0 mag arcsec−2; the latter reflects the complexity of stellar populations at the disk component in a typical spiral galaxy. Finally, the color dispersion measurements of an elliptical galaxy appear to be correlated with the Wide-field Infrared Survey Explorer infrared color ([4.6]–[12]). This indicates that the complexity of stellar populations in an elliptical galaxy is related to its recent star formation activities. From this observational evidence, we infer that gas-rich minor mergers or gas interactions may have usually occurred during the recent growth of massive elliptical galaxies.
Designing defect-based qubit candidates in wide-gap binary semiconductors

The development of novel quantum bits is key to extend the scope of solid-state quantum information science and technology. Using first-principles calculations, we propose that large metal ion - vacancy complexes are promising qubit candidates in two binary crystals: 4H-SiC and w-AlN. In particular, we found that the formation of neutral Hf- and Zr-vacancy complexes is energetically favorable in both solids; these defects have spin-triplet ground states, with electronic structures similar to those of the diamond NV center and the SiC di-vacancy. Interestingly, they exhibit different spin-strain coupling characteristics, and the nature of heavy metal ions may allow for easy defect implantation in desired lattice locations and ensure stability against defect diffusion. In order to support future experimental identification of the proposed defects, we report predictions of their optical zero-phonon line, zero-field splitting and hyperfine parameters. The defect design concept identified here may be generalized to other binary semiconductors to facilitate the exploration of new solid-state qubits.
Particle protection capability of SEMI-compliant EUV-pod carriers

With the projected rollout of pre-production extreme ultraviolet lithography (EUVL) scanners in 2010, EUVL pilot line production will become a reality in wafer fabrication companies. Among EUVL infrastructure items that must be ready, EUV mask carriers remain critical. To keep non-pellicle EUV masks free from particle contamination, an EUV pod concept has been extensively studied. Early prototypes demonstrated nearly particle-free results at a 53 nm PSL equivalent inspection sensitivity during EUVL mask robotic handling, shipment, vacuum pump-purge, and storage. After the passage of SEMI E152, which specifies the EUV pod mechanical interfaces, standards-compliant EUV pod prototypes, including a production version inner pod and prototype outer pod, were built and tested. Their particle protection capability results are reported in this paper. A state-of-the-art blank defect inspection tool was used to quantify their defect protection capability during mask robotic handling, shipment, and storage tests. To ensure the availability of an EUV pod for 2010 pilot production, the progress and preliminary test results of pre-production EUV outer pods are reported as well.
OUTFLOW AND METALLICITY IN THE BROAD-LINE REGION OF LOW-REDSHIFT ACTIVE GALACTIC NUCLEI

Outflows in active galactic nuclei (AGNs) are crucial to understand in investigating the co-evolution of supermassive black holes (SMBHs) and their host galaxies since outflows may play an important role as an AGN feedback mechanism. Based on archival UV spectra obtained with the Hubble Space Telescope and IUE, we investigate outflows in the broad-line region (BLR) in low-redshift AGNs (z < 0.4) through detailed analysis of the velocity profile of the C iv emission line. We find a dependence of the outflow strength on the Eddington ratio and the BLR metallicity in our low-redshift AGN sample, which is consistent with earlier results obtained for high-redshift quasars. These results suggest that BLR outflows, gas accretion onto SMBHs, and past star formation activity in host galaxies are physically related in low-redshift AGNs as in powerful high-redshift quasars.
Quantum critical environment assisted quantum magnetometer

A central qubit coupled to an Ising ring of N qubits, operating close to a critical point is investigated as a potential precision quantum magnetometer for estimating an applied transverse magnetic field. We compute the quantum Fisher information for the central, probe qubit with the Ising chain initialized in its ground state or in a thermal state. The non-unitary evolution of the central qubit due to its interaction with the surrounding Ising ring enhances the accuracy of the magnetic field measurement. Near the critical point of the ring, Heisenberg-like scaling of the precision in estimating the magnetic field is obtained when the ring is initialized in its ground state. However, for finite temperatures, the Heisenberg scaling is limited to lower ranges of N values.
Descent Relations in Type 0A/0B

The type 0 theories have twice as many stable D-branes as the type II theories. In light of this added complication, we ﬁnd the descent relations for D-branes in the type 0A and 0B theories. In addition, we work out how the two types of D-branes diﬀer in their couplings to NS-NS ﬁelds.
Nonadiabatic Electron Dynamics Effects on High-Harmonic Generation Spectrum of

We numerically solved the full-dimensional electronic time-dependent Schr\"{o}dinger equation for H$_2^+$ with Born-Oppenheimer approximation under different sin$^2$-shaped and trapezoidal laser pulses at some different wavelengths, with $I=$1 $\times 10^{13}$ Wcm$^{-2}$, 3 $\times 10^{13}$ Wcm$^{-2}$, and 6 $\times 10^{13}$ Wcm$^{-2}$ intensity at 4.73 a.u. and 7.0 a.u. internuclear distances. Some structures such as complexity, minima, and oscillatory patterns appeared in the high-order harmonic generation (HHG) spectra are investigated in this work by considering the electron localization, electron nonadiabatic dynamics, spatially asymmetric of the HHG, and the Rabi frequency of the population of the ground and excited electronic states to better understand the origins of these structures in the HHG spectrum. We will clear that the origin of complicated patterns of the HHG spectra in sin$^2$-shaped laser pulse is due to that the most portion of the HHG emission occurs at the falling part of the laser pulse. We explore that the oscillatory pattern in the HHG spectra originate from an oscillatory pattern in the $S_g$ and $S_u$ spectra and these oscillatory patterns in turn are due to the nonadiabatic electronic behavior appeared as the slow oscillation pattern in the ground and first excited electronic states populations. Also, our result shows that the minima of the HHG are related to the oscillatory patterns in $S_g$ and $S_u$ spectra.
Rotation and magnetism in intermediate-mass stars

Rotation and magnetism are increasingly recognized as important phenomena in stellar evolution. Surface magnetic fields from a few to $20{,}000\,$G have been observed and models have suggested that magnetohydrodynamic transport of angular momentum and chemical composition could explain the peculiar composition of some stars. Stellar remnants such as white dwarfs have been observed with fields from a few to more than $10^{9}\,$G. We investigate the origin of and the evolution, on thermal and nuclear rather than dynamical time-scales, of an averaged large-scale magnetic field throughout a star's life and its coupling to stellar rotation. Large-scale magnetic fields sustained until late stages of stellar evolution with conservation of magnetic flux could explain the very high fields observed in white dwarfs. We include these effects in the Cambridge stellar evolution code using three time-dependant advection-diffusion equations coupled to the structural and composition equations of stars to model the evolution of angular momentum and the two components of the magnetic field. We present the evolution in various cases for a $3\rm\,M_{\odot}$ star from the beginning to the late stages of its life. Our particular model assumes that turbulent motions, including convection, favour small-scale field at the expense of large-scale field. As a result the large-scale field concentrates in radiative zones of the star and so is exchanged between the core and the envelope of the star as it evolves. The field is sustained until the end of the asymptotic giant branch, when it concentrates in the degenerate core.
BRST-invariant boundary conditions for gauge theories

A systematic way of generating sets of local boundary conditions on the gauge fields in a path integral is presented. These boundary conditions are suitable for one-loop effective action calculations on manifolds with a boundary and for quantum cosmology. For linearized gravity, the general procedure described here leads to new sets of boundary conditions. {copyright} {ital 1997} {ital The American Physical Society}
Investigating light-curve modulation via kernel smoothing – II. New additional modes in single-mode OGLE classical Cepheids

Detailed knowledge of the variability of classical Cepheids, in particular their modulations and mode composition, provides crucial insight into stellar structure and pulsation. However, tiny modulations of the dominant radial-mode pulsation were recently found to be very frequent, possibly ubiquitous in Cepheids, which makes secondary modes difficult to detect and analyse, since these modulations can easily mask the potentially weak secondary modes. The aim of this study is to re-investigate the secondary mode content in the sample of OGLE-III and -IV single-mode classical Cepheids using kernel regression with adaptive kernel width for pre-whitening, instead of using a constant-parameter model. This leads to a more precise removal of the modulated dominant pulsation, and enables a more complete survey of secondary modes with frequencies outside a narrow range around the primary. Our analysis reveals that significant secondary modes occur more frequently among first overtone Cepheids than previously thought. The mode composition appears significantly different in the Large and Small Magellanic Clouds, suggesting a possible dependence on chemical composition. In addition to the formerly identified non-radial mode at $P_2 \approx 0.6\ldots 0.65 P_1$ (0.62-mode), and a cluster of modes with near-primary frequency, we find two more candidate non-radial modes. One is a numerous group of secondary modes with $P_2 \approx 1.25 P_1$, which may represent the fundamental of the 0.62-mode, supposed to be the first harmonic of an $l \in \{7,8, 9\}$ non-radial mode. The other new mode is at $P_2 \approx 1.46 P_1$, possibly analogous to a similar, rare mode recently discovered among first overtone RR Lyrae stars.