Miracle-dz/UniFAR-FTUs huggingface dataset:
Ultraluminous X-ray sources with flat-topped noise and QPO

We analysed the X-ray power density spectra of five ultraluminous X-ray sources (ULXs) NGC 5408 X-1, NGC 6946 X-1, M 82 X-1, NGC 1313 X-1, and IC 342 X-1 that are the only ULXs that display both flat-topped noise (FTN) and quasi-periodic oscillations (QPOs). We studied the QPO frequencies, fractional root-mean-square (rms) variability, X-ray luminosity, and spectral hardness. We found that the level of FTN is anticorrelated with the QPO frequency. As the frequency of the QPO and brightness of the sources increase, their fractional variability decreases. We propose a simple interpretation using the spherization radius, viscosity time, and α-parameter as basic properties of these systems. The main physical driver of the observed variability is the mass accretion rate that varies ≳3 between different observations of the same source. As the accretion rate decreases the spherization radius reduces and the FTN plus the QPO move towards higher frequencies, resulting in a decrease of the fractional rms variability. We also propose that in all ULXs when the accretion rate is low enough (but still super-Eddington) the QPO and FTN disappear. Assuming that the maximum X-ray luminosity depends only on the black hole (BH) mass and not on the accretion rate (not considering the effects of either the inclination of the super-Eddington disc or geometrical beaming of radiation), we estimate that all the ULXs have about similar BH masses, with the exception of M 82 X-1, which might be 10 times more massive.
Overshoot Inwards from the Bottom of the Intershell Convective Zone in (S)AGB stars

We estimate the extent of overshooting inwards from the bottom of the intershell convective zone in thermal pulses in (S)AGB stars. We find that the buoyancy is so strong that any overshooting should be negligible. The temperature inversion at the bottom of the convective zone adds to the stability of the region. Any mixing that occurs in this region is highly unlikely to be due to convective overshooting, and so must be due to another process.
Probing the Intergalactic Medium with Lyα and 21 cm Fluctuations

We study 21 cm and Lyα fluctuations, as well as Hα, while distinguishing between Lyα emission of galactic, diffuse, and scattered intergalactic medium (IGM) origin. Cross-correlation information about the state of the IGM is obtained, testing neutral versus ionized medium cases with different tracers in a seminumerical simulation setup. In order to pave the way toward constraints on reionization history and modeling beyond power spectrum information, we explore parameter dependencies of the cross-power signal between 21 cm and Lyα, which displays a characteristic morphology and a turnover from negative to positive correlation at scales of a couple Mpc−1. In a proof of concept for the extraction of further information on the state of the IGM using different tracers, we demonstrate the use of the 21 cm and Hα cross-correlation signal to determine the relative strength of galactic and IGM emission in Lyα. We conclude by showing the detectability of the 21 cm and Lyα cross-correlation signal over more than one decade in scale at high signal-to-noise ratio for upcoming probes like SKA and the proposed all-sky intensity mapping satellites SPHEREx and CDIM, while also including the Lyα damping tail and 21 cm foreground avoidance in the modeling.
Acetylene measurement using quantum cascade lasers at 14μm

The monitoring of acetylene (C2H2) concentrations is important for many chemical processes. Industrial trace gas measurements are usually performed using gas chromatographs (GC) which have time constants of several minutes. Optical analyzers are expected to yield faster response times with lower maintenance costs. We investigated the use of quantum cascade laser (QCL) spectroscopy in the 14μm range for the sensitive and fast detection of C2H2. This spectral range is favorable, as it avoids spectral interferences by other components which could be present in typical process gases. We developed new custom DFB QCLs and characterized their spectral properties. We determined the performance of our QCL gas analyzer setup and demonstrate a noise equivalent concentration of 10 ppb in 20 s average time.
HERschel Observations of Edge-on Spirals (HEROES)

We present results of the detailed dust energy balance study for the seven large edge-on galaxies in the HEROES sample using three-dimensional (3D) radiative transfer (RT) modelling. Based on available optical and near-infrared (NIR) observations of the HEROES galaxies, we derive the 3D distribution of stars and dust in these galaxies. For the sake of uniformity, we apply the same technique to retrieve galaxy properties for the entire sample: we use a stellar model consisting of a Sérsic bulge and three double-exponential discs (a superthin disc for a young stellar population and thin and thick discs for old populations). For the dust component, we adopt a double-exponential disc with the new THEMIS dust-grain model. We fit oligochromatic RT models to the optical and NIR images with the fitting algorithm FITSKIRT and run panchromatic simulations with the SKIRT code at wavelengths ranging from ultraviolet to submillimeter. We confirm the previously stated dust energy balance problem in galaxies: for the HEROES galaxies, the dust emission derived from our RT calculations underestimates the real observations by a factor 1.5–4 for all galaxies except NGC 973 and NGC 5907 (apparently, the latter galaxy has a more complex geometry than we used). The comparison between our RT simulations and the observations at mid-infrared–submillimetre wavelengths shows that most of our galaxies exhibit complex dust morphologies (possible spiral arms, star-forming regions, more extended dust structure in the radial and vertical directions). We suggest that, in agreement with results from the literature, the large- and small-scale structure is the most probable explanation for the dust energy balance problem.
Localization of compressional Alfven eigenmodes in spherical tori

Edge-localized compressional Alfven eigenmodes (CAE) may be responsible for the observed emission in the ion cyclotron frequency range in the National Spherical Torus experiments (NSTX) [M. Ono et al., Nucl. Fusion 40, 557 (2000)]. These modes can be driven unstable by resonant interaction with a small population of energetic ions, having an anisotropic distribution in velocity space. In the present paper, the radial and poloidal structure of these eigenmodes is analyzed, by solving the eigenmode equation using a variational approach. The analysis shows that CAE are radially and poloidally localized near the plasma edge and have eigenfrequencies in the range corresponding to experimentally measured frequencies in NSTX.
De Sitter and scaling solutions in a higher-order modified teleparallel theory

The existence and the stability conditions for some exact relativistic solutions of special interest are studied in a higher-order modified teleparallel gravitational theory. The theory with the use of a Lagrange multiplier is equivalent with that of General Relativity with a minimally coupled noncanonical field. The conditions for the existence of de Sitter solutions and ideal gas solutions in the case of vacuum are studied as also the stability criteria. Furthermore, in the presence of matter the behaviour of scaling solutions is given. Finally, we discuss the degrees of freedom of the field equations and we reduce the field equations in an algebraic equation, where in order to demonstrate our result we show how this noncanonical scalar field can reproduce the Hubble function of Λ-cosmology.
Magnetoelectrically tunable Andreev bound state spectra and spin polarization in 
p
-wave Josephson junctions

We demonstrate how the boundary-driven reconstruction of the superconducting order parameter can be employed to manipulate the zero-energy Majorana bound states (MBSs) occurring in a topological Josephson junction. We focus on an interface of two p-wave superconductors, which are described by a spin-vector order parameter $\bf{d}$. Apart from the sensitivity of $\bf{d}$ to external Zeeman/exchange fields, here, we show that the orientation of $\bf{d}$ throughout the junction can be controlled by electrically gating the weak link. The remarkable local character of this knob is a manifestation of the edge reconstruction of the order parameter, which takes place whenever different $\bf{d}$-vector configurations in each superconductor compete and are close in energy. As a consequence, the spin-dependent superconducting-phase difference across the junction is switchable from $0$ to $\pi$. Moreover, in the regime where multiple edge MBSs occur for each superconductor, the Andreev-bound-state (ABS) spectra can be twisted by the application of either a charge- or spin-phase difference across the interface, and give rise to a rich diversity of nonstandard ABS dispersions. Interestingly, some of these dispersions show band crossings protected by fermion parity, despite their $2\pi$-periodic character. These crossings additionally unlock the possibility of nontrivial topology in synthetic spaces, when considering networks of such 1D junctions. Lastly, the interface MBSs induce a distinct elecronic spin polarization near the junction, which possesses a characteristic spatial pattern that allows the detection of MBSs using spin-polarized scanning tunneling microscopy. These findings unveil novel paths to mechanisms for ABS engineering and single-out signatures relevant for the experimental detection and manipulation of MBSs.
Closed string amplitudes from gauge fixed string field theory

Closed string diagrams are derived from cubic open string field theory using a gauge fixed kinetic operator. The basic idea is to use a string propagator that does not generate a boundary to the world sheet. Using this propagator and the closed string vertex, the moduli space of closed string surfaces is covered, so closed string scattering amplitudes should be reproduced. This kinetic operator could be a gauge fixed form of the string field theory action around the closed string vacuum.
Near-IR integral-field spectroscopy of the companion to GQ Lup

The first substellar companion of possibly planetary mass around a normal star, GQ Lup, has been directly imaged (Neuhaeuser et al., 2005). Besides the unknown formation history, the mass of such an object is a criterion to decide about its true nature. We aim to determine the physical properties of the GQ Lup companion - effective temperate and surface gravity, and thus its mass independently from evolutionary models. We use the adaptive optics integral-field spectrograph SINFONI at the VLT for near-infrared spectroscopy from 1.1 to 2.5 um with a resolution of R = 2500--4000. We compare these spectra with synthetic atmospheric models (GAIA v2.0 cond). From the complete set of spectra we find a consistent effective temperature of Teff = 2600 +/- 100 K and surface gravity of log{g} = 3.7 +/- 0.5. Combined with a slightly revised luminosity of log(L/L_(\sun)) = -2.25 +/- 0.24 for the companion, we determine a radius of R = 3.50 (+1.50/-1.03) Jupiterradii and thus a mass of ~ 25 Jupitermasses. Due to the large uncertainty of the surface gravity, the mass could range from 4 to 155 Jupitermasses. By comparing the paramaters of the companion of GQ Lup to the ones of 2MASS J05352184-0546085, published by Stassun et al. (2006), we conclude that the companion to GQ Lup A has a mass lower than 36 Jupitermasses.
Color Degradation of Textiles with Natural Yellow Dyes under Exhibition Lighting and Evaluation of CIE Standard of Museum Lighting

In 2004, CIE issued a technical report (CIE 157: 2004) entitled "Control of Damage to Museum Objects by Optical Radiation," in which it recommended that materials classified as highly responsive to light (ex. blue wool standard 1 to 3) be exposed for a maximum of 15000 lx·hr/yr. The aim of this report is to validate the new CIE recommendation for natural yellow dyes categorized below the blue scale grade 4. Twenty types of natural yellow dyes on silk were exposed to both white and non-UV fluorescent museum lamps. Color differences were measured at 15000 lx·hr (500 lx at fabric surface x 300 hr) intervals for 10 times, for an accumulated exposure totaling 150000 lx·hr. The results show that non-UV fluorescent museumlamp was 24% more effective in reducing the fading rate compared with white fluorescent lamp. Complying with the new CIE recommended maximum exposure of 15000 lx·hr/yr, the fading rate for most yellow dyes, will be below the noticeable fading degree (ΔE1.6) thus, the CIE recommendation is valid. However, additional dyes should also be classified as "extremely highly responsive. " The limiting exposure for Ukon (Turmeric, Cucuma longa L., colorant: curcumin) should be 3500 lx·hr/yr, and Kihada (Amur cork tree, Phellodendron amurencse Rupr., colorant: berberine) and Onion skin (Allium cepa L., colorant: quercetin) should be 8000∼12000 lx·hr/yr. This study demonstrated a need for revised classification of "extremely highly responsive" materials under museum lighting conditions.
Impact of Increasing Urban Density on Local Climate: Spatial and Temporal Variations in the Surface Energy Balance in Melbourne, Australia

Variations in urban surface characteristics are known to alter the local climate through modification of land surface processes that influence the surface energy balance and boundary layer and lead to distinct urban climates. In Melbourne, Australia, urban densities are planned to increase under a new strategic urban plan. Using the eddy covariance technique, this study aimed to determine the impact of increasing housing density on the surface energy balance and to investigate the relationship to Melbourne’s local climate. Across four sites of increasing housing density and varying land surface characteristics (three urban and one rural), it was found that the partitioning of available energy was similar at all three urban sites. Bowen ratios were consistently greater than 1 throughout the year at the urban sites (often as high as 5) and were higher than the rural site (less than 1) because of reduced evapotranspiration. The greatest difference among sites was seen in urban heat storage, which was influenced by urban canopy complexity, albedo, and thermal admittance. Resulting daily surface temperatures were therefore different among the urban sites, yet differences in above-canopy daytime air temperatures were small because of similar energy partitioning and efficient mixing. However, greater nocturnal temperatures were observed with increasing density as a result of variations in heat storage release that are in part due to urban canyon morphology. Knowledge of the surface energy balance is imperative for urban planning schemes because there is a possibility for manipulation of land surface characteristics for improved urban climates.
Infalling Faint [O II] Emitters in Abell 851. II. Environment, Kinematics, and Star Formation History

We report on the local environment, kinematics, and star formation history of [O II]-selected objects in the z ≈ 0.4 galaxy cluster Abell 851, using Keck optical spectra. A large fraction (≈55%) of cluster [O II] emitters show strong Balmer absorptions (≳4 Å in Hδ equivalent width). These e(a)-type spectra have been attributed to dusty starburst galaxies by Poggianti & Wu, an interpretation supported by our reddening measurements, which show a high frequency of very reddened [E(B - V) ≳ 0.5] galaxies. Our spectral modeling requires starburst ages of ≲1 Gyr, which is shorter than the cluster crossing timescale. We argue that this starburst phase occurs during cluster infall on the basis of the radial velocity distribution of the [O II] emitters, which present a deficit of systems near the cluster systemic velocity when compared to a virialized population (or a backsplash population). The spatial segregation of some redshifted and blueshifted groups strongly indicates that the accretion was recent. Throughout the cluster, the presence of [O II] emitters is strongly suppressed in dense environments. Our analysis supports previous suggestions that dusty starburst galaxies arise at the expense of gas-rich spiral galaxies [i.e., the e(c) type; Dressler and coworkers]. In addition, we describe a fainter population comprised largely of dwarf galaxies (Martin and coworkers) and find an even stronger suppression of [O II] emitters in high-density environments, indicative of more effective destruction by harassment and/or gas stripping. Comparison to previous morphological studies, limited to the cluster core, suggests that galaxy-galaxy interactions may trigger the starbursts. The high e(a) galaxy fraction in Abell 851 as compared to that in the field, however, suggests that some cluster-specific mechanism, likely related to the dynamical assembly of the cluster, also contributes to the high number of starbursts.
A Polylogarithmic Bound for an Iterative Substructuring Method for Spectral Elements in Three Dimensions

Iterative substructuring methods form an important family of domain decomposition algorithms for elliptic finite element problems. A $p$-version finite element method based on continuous, piecewise $Q_p$ functions is considered for second-order elliptic problems in three dimensions; this special method can also be viewed as a conforming spectral element method. An iterative method is designed for which the condition number of the relevant operator grows only in proportion to $(1+\log p)^2 . $ This bound is independent of jumps in the coefficient of the elliptic problem across the interfaces between the subregions. Numerical results are also reported which support the theory.
Evolution of Molecular Clouds in the Superwind Galaxy NGC 1808 Probed by ALMA Observations

ALMA imaging of the cold molecular medium in the nearby starburst galaxy NGC 1808 is presented. The observations reveal the distribution of molecular gas, traced by 12CO (1–0) and 12CO (3–2), and continuum (93 and 350 GHz) across the central 1 kpc starburst region at a high resolution of . A molecular gas torus (radius ∼ 30 pc) is discovered in the circumnuclear disk (CND; central 100 pc), with a high CO (3–2)/CO (1–0) ratio of ∼1, surrounded by massive (106– ) clouds with high star formation efficiency ( yr−1), molecular spiral arms, and a 500 pc pseudo-ring. The CND harbors a continuum core and molecular gas exhibiting peculiar motion. The new data confirm the line splitting along the minor galactic axis, interpreted as a nuclear gas outflow with average velocity ∼180 km s−1, and show evidence of a velocity gradient of km s−1 pc−1 along the axis. In addition, supershells expanding from the 500 pc ring with maximum velocities of ∼75 km s−1 are revealed. The distribution and CO luminosities of molecular clouds in the central 1 kpc starburst region indicate an evolutionary sequence, from gas accretion onto the 500 pc ring from the large-scale bar to enhanced star formation in the ring, and outflow as feedback.
Quantum-memory-assisted multi-photon generation for efficient quantum information processing

In the last two decades, many quantum optics experiments have demonstrated small-scale quantum information processing applications with several photons. Beyond such proof-of-principle demonstrations, efficient preparation of large, but definite, numbers of photons is of great importance for further scaling up and speeding up photonic quantum information processing. Typical single-photon generation techniques based on nonlinear parametric processes face challenges of probabilistic generation. Here we demonstrate efficient synchronization of photons from multiple nonlinear parametric heralded single-photon sources (HSPSs), using quantum memories (QMs). Our low-loss optical memories greatly enhance (~30x) the generation rate of coincidence photons from two independent HSPSs, while maintaining high indistinguishability (95.7%) of the synchronized photons. As an application, we perform the first demonstration of HSPS-based measurement-device-independent quantum key distribution (MDI-QKD). The synchronized HSPSs demonstrated here will pave the way toward efficient quantum communication and larger scale optical quantum computing.
Conditional bootstrap methods in the mean-shift model

SUMMARY Bootstrap methods are not inherently conditional, but they can be made so by appropri- ate stratification of the simulated samples which bootstrap produces. We show how stratification can work in a bootstrap analysis of mean-shift in Nile river flow data. The results are compared with both parametric and semiparametric likelihood analyses. The paper ends with some general remarks on conditional bootstraps. Bootstrap methods (Efron, 1982) are simulation methods for assessing frequency properties of statistical analyses, the simulation model being that which is fitted to the actual data. Often the simulation involves Monte Carlo, rather than theoretical, evaluation. Unfortunately the bootstrap as usually described is inherently unconditional; Rubin's (1981) discussion bears on this point. However, if the bootstrap simulation results can be properly stratified, then it is possible to estimate relevant conditional probabilities. Stratification can sometimes be effected in the model itself, as when fixing the values of sample sizes or explanatory variables. Otherwise one must run the unconditional bootstrap and stratify its output. In the present paper we illustrate the latter situation in the analysis of a mean-shift model. Section 2 describes the application and its analysis by parametric methods. Sections 3 and 4 produce alternative bootstrap analyses, the first of which uses the stratification of an unconditional Monte Carlo simulation; the second bootstrap analysis involves estimation of a likelihood function. The final section contains some brief general remarks about conditional bootstraps.
A Survey of Local Group Galaxies Currently Forming Stars. II. UBVRI Photometry of Stars in Seven Dwarfs and a Comparison of the Entire Sample

We have obtained UBVRI images with the Kitt Peak National Observatory and Cerro Tololo Inter-American Observatory 4 m telescopes and Mosaic cameras of seven dwarfs in (or near) the Local Group, all of which have known evidence of recent star formation: IC 10, NGC 6822, WLM, Sextans B, Sextans A, Pegasus, and Phoenix. We construct color-magnitude diagrams (CMDs) of these systems, as well as neighboring regions that can be used to evaluate the degree of foreground contamination by stars in the Milky Way. Intercomparison of these CMDs with those of M31, M33, the LMC, and the SMC permits us to determine improved reddening values for a typical OB star found within these galaxies. All of the CMDs reveal a strong or modest number of blue supergiants. All but Pegasus and Phoenix also show the clear presence of red supergiants in the CMD, although IC 10 appears to be deficient in these objects given its large Wolf-Rayet star population. The bright stars of intermediate color in the CMD are badly contaminated by foreground stars (30%-100%), and considerable spectroscopy is needed before statistics on the yellow supergiants in these systems will be known. This study is intended to serve as both the impetus and "finding charts" for further space-based imaging and for many spectroscopic programs at large aperture.
Size, angular momentum and mass for objects

We obtain a geometrical inequality involving the ADM mass, the angular momentum and the size of an ordinary, axially symmetric object. We use the monotonicity of the Geroch quasi-local energy on 2-surfaces along the inverse mean curvature flow. We also compute numerical examples to test the robustness of our hypotheses and results