Miracle-dz/UniFAR-FTUs huggingface dataset:
Characterizing motion types of G-band bright points in the quiet Sun

We study the motion of G-band bright points (GBPs) in the quiet Sun to obtain the characteristics of different motion types. A high resolution image sequence taken with the Hinode/Solar Optical Telescope (SOT) is used, and GBPs are automatically tracked by segmenting 3D evolutional structures in a space-time cube. After putting the GBPs that do not move during their lifetimes aside, the non-stationary GBPs are categorized into three types based on an index of their motion type. Most GBPs that move in straight or nearly straight lines are categorized as a straight motion type, a few moving in rotary paths into rotary motion, and the others fall into a motion type we called erratic. The mean horizontal velocities are 2.18±0.08 km s−1, 1.63±0.09 km s−1 and 1.33±0.07 km s−1 for straight, erratic and rotary motion types, respectively. We find that a GBP drifts at a higher and constant velocity during its whole life if it moves in a straight line. However, it has a lower and variational velocity if it moves on a rotary path. The diffusive process is ballistic-, super- and sub-diffusion for straight, erratic and rotary motion types, respectively. The corresponding diffusion index (γ) and coefficients (K) are 2.13±0.09 and 850±37 km2 s−1, 1.82±0.07 and 331±24 km2 s−1, and 0.73±0.19 and 13±9 km2 s−1. In terms of direction of motion, it is homogeneous and isotropic, and usually persists between neighboring frames, no matter what motion type a GBP is classified as.
Detection of Ly\beta auto-correlations and Ly\alpha-Ly\beta cross-correlations in BOSS Data Release 9

The Lyman-$\beta$ forest refers to a region in the spectra of distant quasars that lies between the rest-frame Lyman-$\beta$ and Lyman-$\gamma$ emissions. The forest in this region is dominated by a combination of absorption due to resonant Ly$\alpha$ and Ly$\beta$ scattering. When considering the 1D Ly$\beta$ forest in addition to the 1D Ly$\alpha$ forest, the full statistical description of the data requires four 1D power spectra: Ly$\alpha$ and Ly$\beta$ auto-power spectra and the Ly$\alpha$-Ly$\beta$ real and imaginary cross-power spectra. We describe how these can be measured using an optimal quadratic estimator that naturally disentangles Ly$\alpha$ and Ly$\beta$ contributions. Using a sample of approximately 60,000 quasar sight-lines from the BOSS Data Release 9, we make the measurement of the one-dimensional power spectrum of fluctuations due to the Ly$\beta$ resonant scattering. While we have not corrected our measurements for resolution damping of the power and other systematic effects carefully enough to use them for cosmological constraints, we can robustly conclude the following: i) Ly$\beta$ power spectrum and Ly$\alpha$-Ly$\beta$ cross spectra are detected with high statistical significance; ii) the cross-correlation coefficient is $\approx 1$ on large scales; iii) the Ly$\beta$ measurements are contaminated by the associated OVI absorption, which is analogous to the SiIII contamination of the Ly$\alpha$ forest. Measurements of the Ly$\beta$ forest will allow extension of the usable path-length for the Ly$\alpha$ measurements while allowing a better understanding of the physics of intergalactic medium and thus more robust cosmological constraints.
THE ACS SURVEY OF GALACTIC GLOBULAR CLUSTERS. X. NEW DETERMINATIONS OF CENTERS FOR 65 CLUSTERS

We present new measurements of the centers for 65 Milky Way globular clusters. Centers were determined by fitting ellipses to the density distribution within the inner 2′ of the cluster center, and averaging the centers of these ellipses. The symmetry of clusters was also analyzed by comparing cumulative radial distributions on opposite sides of the cluster across a grid of trial centers. All of the determinations were done with stellar positions derived from a combination of two single-orbit Advanced Camera for Surveys images of the core of the cluster in F606W and F814W. We find that the ellipse-fitting method provides remarkable accuracy over a wide range of core sizes and density distributions, while the symmetry method is difficult to use on clusters with very large cores or low density. The symmetry method requires a larger field or a very sharply peaked density distribution.
Wire recycling for quantum circuit optimization

Quantum information processing is expressed using quantum bits (qubits) and quantum gates which are arranged in the terms of quantum circuits. Here, each qubit is associated to a quantum circuit wire which is used to conduct the desired operations. Most of the existing quantum circuits allocate a single quantum circuit wire for each qubit and, hence, introduce a significant overhead. In fact, qubits are usually not needed during the entire computation but only between their initialization and measurement. Before and after that, corresponding wires may be used by other qubits. In this work, we propose a solution which exploits this fact in order to optimize the design of quantum circuits with respect to the required wires. To this end, we introduce a representation of the lifetimes of all qubits which is used to analyze the respective need for wires. Based on this analysis, a method is proposed which "recycles" the available wires and, by this, reduces the size of the resulting circuit. Experimental evaluations based on established reversible and fault-tolerant quantum circuits confirm that the proposed solution reduces the amount of wires by more than 90% compared to unoptimized quantum circuits.
The mass distribution and gravitational potential of the Milky Way

We present mass models of the Milky Way created to fit observational constraints and to be consistent with expectations from theoretical modelling. The method used to create these models is that demonstrated in our previous study, and we improve on those models by adding gas discs to the potential, considering the effects of allowing the inner slope of the halo density profile to vary, and including new observations of maser sources in the Milky Way amongst the new constraints. We provide a best-fitting model, as well as estimates of the properties of the Milky Way. Under the assumptions in our main model, we find that the Sun is R0 = 8.20 ± 0.09 kpc from the Galactic Centre, with the circular speed at the Sun being v0 = 232.8 ± 3.0 kms-1; and that the Galaxy has a total stellar mass of (54.3 ± 5.7) × 109 M⊙, a total virial mass of (1.30 ± 0.30) × 1012M⊙ and a local dark-matter density of 0.40 ± 0.04 GeV cm-3, where the quoted uncertainties are statistical. These values are sensitive to our choice of priors and constraints. We investigate systematic uncertainties, which in some cases may be larger. For example, if we weaken our prior on R0, we find it to be 7.97 ± 0.15 kpc and that v0 = 226.8 ± 4.2 kms-1.We find that most of these properties, including the local dark-matter density, are remarkably insensitive to the assumed power-law density slope at the centre of the dark-matter halo. We find that it is unlikely that the local standard of rest differs significantly from that found under assumptions of axisymmetry. We have made code to compute the force from our potential, and to integrate orbits within it, publicly available. (Less)
Constrained Liquidity Provision in Currency Markets*

We study dealers’ liquidity provision in the currency market. We show that at times when dealers’ intermediation capacity is constrained their cost of liquidity provision increases disproportionately relative to dealer-provided volume. As a result, the elasticity of dealers’ liquidity provision weakens by at least 80% relative to periods when they are unconstrained. We identify constrained periods based on leverage ratios, Value-at-Risk measures, credit default spreads, and debt funding costs. We interpret our novel empirical findings within a parsimonious model that sheds light on the key mechanisms of how liquidity provision by dealers tends to weaken when intermediary constraints are tightening. J.E. L. classification: F31, G12, G15
The local value of H0 in an inhomogeneous universe

The effects of local inhomogeneities on low redshift H0 determinations are studied by estimating the redshift-distance relation of mock sources in N-body simulations. The results are compared to those obtained using the standard approach based on Hubble's law. The comparison shows a clear tendency for the standard approach to yield lower values of H0 than the approach based on the scheme using light rays. The difference is, however, small. More precisely, it is found that the overall effect of inhomogeneities on the determination of H0 is a small increase in the local estimates of about 0.3% compared to the results obtained with Hubble's law, when based on a typical distribution of supernovae in the redshift range 0.01 < z < 0.1. The overall conclusion of the study is a verification of the results that have earlier been obtained by using Hubble's law: the effects of inhomogeneities on local H0 estimates are not significant enough to make it plausible that differences in high- and low-redshift estimates of H0 are due to small inhomogeneities within the setting of standard cosmology.
CQMC: an improved code for low-dimensional Compressed Quasi-MonteCarlo cubature *

An improved version of Compressed Quasi-MonteCarlo cubature (CQMC) on large low-discrepancy samples is implemented, on 2D and 3D regions with complex shape. The algorithms rests on the concept of Tchakaloff set and on NNLS solution of a sequence of “small” moment-matching systems. Examples of area and volume integration are provided.
GEOMETRIC TRIANGULATION OF IMAGING OBSERVATIONS TO TRACK CORONAL MASS EJECTIONS CONTINUOUSLY OUT TO 1 AU

We describe a geometric triangulation technique, based on time–elongation maps constructed from imaging observations, to track coronal mass ejections (CMEs) continuously in the heliosphere and predict their impact on the Earth. Taking advantage of stereoscopic imaging observations from the Solar Terrestrial Relations Observatory, this technique can determine the propagation direction and radial distance of CMEs from their birth in the corona all the way to 1 AU. The efficacy of the method is demonstrated by its application to the 2008 December 12 CME, which manifests as a magnetic cloud (MC) from in situ measurements at the Earth. The predicted arrival time and radial velocity at the Earth are well confirmed by the in situ observations around the MC. Our method reveals non-radial motions and velocity changes of the CME over large distances in the heliosphere. It also associates the flux-rope structure measured in situ with the dark cavity of the CME in imaging observations. Implementation of the technique, which is expected to be a routine possibility in the future, may indicate a substantial advance in CME studies as well as space weather forecasting.
Early flattening of dark matter cusps in dwarf spheroidal galaxies

Simulations of the clustering of cold dark matter yield dark-matter halos that have central density cusps, but observations of totally dark-matter dominated dwarf spheroidal galaxies imply that they do not have cuspy central density profiles. We use analytic calculations and numerical modelling to argue that whenever stars form, central density cusps are likely to be erased. Gas that accumulates in the potential well of an initially cuspy dark-matter halo settles into a disc. Eventually the surface density of the gas exceeds the threshold for fragmentation into self-gravitating clouds. The clouds are massive enough to transfer energy to the dark-matter particles via dynamical friction on a short time-scale. The halo's central cusp is heated to form a core with central logarithmic density slope gamma=0 before stellar feedback makes its impact. Since star formation is an inefficient process, the clouds are disrupted by feedback when only a small fraction of their mass has been converted to stars, and the dark matter dominates the final mass distribution.
Conclusive exclusion of quantum states

In the task of quantum state exclusion, we consider a quantum system prepared in a state chosen from a known set. The aim is to perform a measurement on the system which can conclusively rule that a subset of the possible preparation procedures cannot have taken place. We ask what conditions the set of states must obey in order for this to be possible and how well we can complete the task when it is not. The task of quantum state discrimination forms a subclass of this set of problems. Within this paper, we formulate the general problem as a semidefinite program (SDP), enabling us to derive sufficient and necessary conditions for a measurement to be optimal. Furthermore, we obtain a necessary condition on the set of states for exclusion to be achievable with certainty, and we give a construction for a lower bound on the probability of error. This task of conclusively excluding states has gained importance in the context of the foundations of quantum mechanics due to a result from Pusey, Barrett, and Rudolph (PBR). Motivated by this, we use our SDP to derive a bound on how well a class of hidden variable models can perform at a particular task, proving an analog of Tsirelson's bound for the PBR experiment and the optimality of a measurement given by PBR in the process. We also introduce variations of conclusive exclusion, including unambiguous state exclusion, and state exclusion with worst-case error.
Testing the low-mass end of X-ray scaling relations with a sample of Chandra galaxy groups

Context. Well-determined scaling relations between X-ray observables and cluster mass are essential for using large cluster samples to constrain fundamental cosmological parameters. Scaling relations between cluster masses and observables, such as the luminositytemperature, mass-temperature, luminosity-mass relations, have been investigated extensively, however the question of whether these relations hold true also for poor clusters and groups remains unsettled. Some evidence supports a “break” at the low end of the group/cluster mass range, possibly caused by the stronger influence of non-gravitational physics on low-mass systems. Aims. The main goal of this work is to test local scaling relations for the low-mass range in order to check whether or not there is a systematic difference between clusters and groups, and to thereby extend this method of reliable and convenient cluster mass determination for future large samples down to the group regime. Methods. We compiled a statistically complete sample of 112 X-ray galaxy groups, 26 of which have usable Chandra data. Temperature, metallicity, and surface brightness profiles were created for these 26 groups, and used to determine the main physical quantities and scaling relations. We then compared the group properties to those of the HIFLUGCS clusters, as well as several other group and cluster samples. Results. We present radial profiles for the individual objects and scaling relations of the whole sample (Lx − T , M − T , Lx − M, Mg − M, M − Yx, Lx − Yx, fg − T ). Temperature and metallicity profiles behave universally, except for the core regions. The Lx − T , M − T , Lx − M, Mg − M, M − Yx, and Lx − Yx relations of the group sample are generally in good agreement with clusters. The Lx − T relation steepens for T < 3 keV, which could point to a larger impact of heating mechanisms on cooler systems. We found a significant drop in the gas mass fraction below <∼1 keV, as well as a correlation with radius, which indicates the ICM is less dominant in groups compared to clusters and the galaxies have a stronger influence on the global properties of the system. In all relations the intrinsic scatter for groups is larger than for clusters, which appears not to be correlated with merger activity but could be due to scatter caused by baryonic physics in the group cores. We also demonstrate the importance of selection effects. Conclusions. We have found some evidence for a similarity break between groups and clusters. However this does not have a strong effect on the scaling relations.
DETECTING INDUSTRIAL POLLUTION IN THE ATMOSPHERES OF EARTH-LIKE EXOPLANETS

Detecting biosignatures, such as molecular oxygen in combination with a reducing gas, in the atmospheres of transiting exoplanets has been a major focus in the search for alien life. We point out that in addition to these generic indicators, anthropogenic pollution could be used as a novel biosignature for intelligent life. To this end, we identify pollutants in the Earth's atmosphere that have significant absorption features in the spectral range covered by the James Webb Space Telescope. We focus on tetrafluoromethane (CF4) and trichlorofluoromethane (CCl3F), which are the easiest to detect chlorofluorocarbons (CFCs) produced by anthropogenic activity. We estimate that ∼1.2 days (∼1.7 days) of total integration time will be sufficient to detect or constrain the concentration of CCl3F (CF4) to ∼10 times the current terrestrial level.
UvA-DARE (Digital Academic Beyond Experience: On the Radicalization of the Social Approach to Emotions and the Emancipation of Verbal Emotional Expressions

Emotions have traditionally been viewed as intrapersonal phenomena. Over the past decades, theory and research have shifted toward a more social perspective that emphasizes the role of emotional expressions in coordinating social interaction. I provide a brief history of this ongoing paradigm shift, which reveals two critical developments. The first concerns a continuing shift in emphasis on the social-communicative rather than individual-level functions and effects of emotions—the radicalization of the social approach to emotion. The second concerns a growing awareness that emotions can be expressed through multiple modalities, including words—the emancipation of verbal emotional expressions. I discuss theoretical challenges and opportunities presented by these developments and consider their implications for understanding emotions as a source of social influence. Abstract The present contribution provides a constructive criticism of Brian Parkinson’s “Heart to Heart: A Relation-Alignment Approach to Emotion’s Social Effects. ” I outline a number of points in Parkinson’s approach that I find particularly useful from a sociological perspective on emotions and provide suggestions for further extending his account. In doing so, I concentrate on issues regarding the social ontology of emotion, the proposition of emotional adjacency pairs in verbal and facial communication, the importance of social appraisals in intergroup contexts, and the relevance of social institutions for understanding how some emotions come to dominate certain social relations.
On the nature of the progenitors of three Type II-P supernovae: 2004et, 2006my and 2006ov

The pre-explosion observations of the Type II-P supernovae 2006my, 2006ov and 2004et are re-analysed. In the cases of supernovae 2006my and 2006ov we argue that the published candidate progenitors are not coincident with their respective supernova sites in pre-explosion Hubble Space Telescope observations. We therefore derive upper luminosity and mass limits for the unseen progenitors of both these supernovae, assuming they are red supergiants: 2006my (log L/L ⊙ = 4.51; m < 13 M ⊙ ) and 2006ov (logL/L ⊙ = 4.29; m < 10 M ⊙ ). In the case of supernova 2004et we show that the yellow supergiant progenitor candidate, originally identified in Canada-France-Hawaii Telescope images, is still visible ~3 yr post-explosion in observations from the William Herschel Telescope. High-resolution Hubble Space Telescope and Gemini (North) adaptive optics late-time imagery reveal that this source is not a single yellow supergiant star, but rather is resolved into at least three distinct sources. We report the discovery of the unresolved progenitor as an excess of flux in pre-explosion Isaac Newton Telescope i'-band imaging. Accounting for the late-time contribution of the supernova using published optical spectra, we calculate the progenitor photometry as the difference between the pre- and post-explosion, ground-based observations. We find the progenitor was most likely a late K to late M-type supergiant of 8 +5 -1 M ⊙ . In all cases we conclude that future, high-resolution observations of the supernova sites will be required to confirm these results.
The Gaia-ESO Survey: Tracing interstellar extinction

Context. Large spectroscopic surveys have in recent years enabled computing three-dimensional interstellar extinction maps thanks to the accurate stellar atmospheric parameters and line-of-sight distances these surveys provide. Interstellar extinction maps are complementary to 3D maps extracted from photometry and allow a more thorough studying of the dust properties. Aims. Our goal is to use the high-resolution spectroscopic survey Gaia-ESO to obtain with a good distance resolution the interstellar extinction and its dependency as a function of the environment and the Galactocentric position. Methods. We used the stellar atmospheric parameters of more than 5000 stars, obtained from the Gaia-ESO survey second internal data release, and combined them with optical (SDSS) and near-infrared (VISTA) photometry as well as different sets of theoretical stellar isochrones to calculate line-of-sight extinction and distances. The extinction coefficients were then compared with the literature to discuss their dependency on the stellar parameters and position in the Galaxy. Results. Within the errors of our method, our work does not show any dependence of the interstellar extinction coefficient on the stellar atmospheric parameters. We find no evidence of a variation of E(J - H) = E(J - K) with the angle from the Galactic centre or with Galactocentric distance. This suggests that we are dealing with a uniform extinction law in the SDSS ugriz bands and the near-IR JHKs bands. Therefore, extinction maps built from mean colour-excesses that assume a constant extinction coefficient can be used without introducing any systematic errors. (Less)
First T dwarfs in the VISTA Hemisphere Survey

School of Physics & Astronomy, Queen Mary University of London, Mile End Road, London E1 4NS, United KingdomOctober 19, 2012; October 19, 2012ABSTRACTAims.The aim of the project is to improve our current knowledge of the density of T dwarfs and the shape of the substellar initialmass function by identifying a magnitude-limited sample ofT dwarfs in the full southern sky.Methods. We present the results of a photometric search aimed at discovering cool brown dwarfs in the Southern sky imaged atinfrared wavelengths by the Visible and Infrared Survey Telescope for Astronomy (VISTA) and the Wide Infrared Survey Explorer(WISE) satellite mission. We combined the ﬁrst data release (DR1) of the VISTA Hemisphere Survey (VHS) and the WISE prelimi-nary data release to extract candidates with red mid-infrared colours and near- to mid-infrared colours characteristics of cool browndwarfs.Results. The VHS DR1 vs. WISE search returned tens of T dwarf candidates, 13 of which are presented here, including two previ-ously published in the literature and ﬁve new ones conﬁrmed s pectroscopically with spectral types between T4.5 and T8. We estimatethat the two T6 dwarfs lie within 16 pc and the T4.5 within 25 pc. The remaining three are 30–50 pc distant. The only T7 dwarf inour sample is the faintest of its spectral class with J =19.28 mag. The other six T dwarf candidates remain without spectroscopicfollow-up. We also improve our knowledge on the proper motion accuracy for three bright T dwarfs by combining multi-epoch datafrom public databases (DENIS, 2MASS, VHS, WISE, Spitzer). Key words. Stars: low-mass stars and brown dwarfs — techniques: photom etric — techniques: spectroscopic — Infrared: Stars —surveys