Miracle-dz/UniFAR-FTUs huggingface dataset:
Stellar inventory of the solar neighbourhood using Gaia DR1

The absolute number and the density profiles of different types of stars in the solar neighborhood are a fundamental anchor for studies of the initial mass function, stellar evolution, and galactic structure. Using data from the Gaia DR1 Tycho-Gaia Astrometric Solution, we reconstruct Gaia's selection function and we determine Gaia's volume completeness, the local number density, and the vertical profiles of different spectral types along the main sequence from early A stars to late K stars as well as along the giant branch. We clearly detect the expected flattening of the stellar density profile near the mid-plane for all stellar types: All vertical profiles are well represented by sech^2 profiles, with scale heights ranging from ~50 pc for A stars to ~150 pc for G and K dwarfs and giants. We determine the luminosity function along the main sequence for M_V ~ $0.72 M_\odot$) and along the giant branch for M_J >~ -2.5. Converting this to a mass function, we find that the high-mass (M > $1\,M_\odot$) present-day mass function along the main sequence is d n / d M = 0.016 $(M/M_\odot)^{-4.7}$ stars/pc^3/$M_\odot$. Extrapolating below M = $0.72\,M_\odot$, we find a total mid-plane stellar density of 0.040+/-0.002 $M_\odot$/pc^3. Giants contribute 0.00039+/-0.00001 stars/pc^3 or about 0.00046+/-0.00005 $M_\odot$/pc^3. The star-formation rate surface density is \Sigma(t) = 7+/-1 exp(-t/[7+/-1 Gyr]) $M_\odot$/pc^2/Gyr. Surprisingly, we find that the Sun is exactly at the mid-plane defined by A and F stars (zsun = -0.9+/-0.9 pc), but appears to be offset from the mid-plane defined by older stars (zsun = 29+/-4 pc with respect to giants). Overall, we find that Gaia DR1's selection biases are manageable and allow a detailed new inventory of the solar neighborhood to be made that agrees with and extends previous studies. This bodes well for mapping the Milky Way with the full Gaia data set.
Contributions to the cross shock electric field at a quasiperpendicular collisionless shock

The normal electric field structure of a supercritical (Mms = 5.2), quasiperpendicular (θBn = 70°) collisionless shock is examined using Cluster four‐spacecraft observations of the terrestrial bow shock. Comparing the observed electric field with magnetic field and plasma observations, two different techniques find that the J × B/ne term in the generalized Ohm's law accounts for a majority of the large‐scale normal electric field and potential drop encountered by the ions ‐ the solar wind ion deceleration is in good empirical agreement with the observed potential drop, confirming earlier work. Large amplitude electric field fluctuations on shorter timescales, corresponding to fine scale structure, are not observed to contribute to the ion energization.
Variable Linear Polarization from Sagittarius A*: Evidence of a Hot Turbulent Accretion Flow

We report the discovery of variability in the linear polarization from the Galactic center black hole source Sagittarius A*. New polarimetry obtained with the Berkeley-Illinois-Maryland Association array at a wavelength of 1.3 mm shows a position angle that differs by 28° ± 5° from observations 6 months prior and then remains stable for 15 months. This difference may be due to a change in the source emission region on a scale of 10 Schwarzschild radii or due to a change of 3 × 105 rad m-2 in the rotation measure. We consider a change in the source physics unlikely, however, since we see no corresponding change in the total intensity or polarized intensity fraction. On the other hand, turbulence in the accretion region at a radius ~10RS-1000RS could readily account for the magnitude and timescale of the position angle change.
The Aquarius Superclusters. II. Spectroscopic and Photometric Data

We present spectroscopic and photometric data for 920 galaxies selected in 68 fields of the Aquarius Cluster Catalog. Typically, the 15 brightest candidate members with magnitudes in the range 16 < bJ < 21 were selected for observations, and ∼71% turn out to be cluster members. Using the new redshift determinations, we assign galaxies to groups and clusters, and by including data from the literature we calculate systemic velocities and velocity dispersions for 74 clusters, each with redshifts measured for at least six individual galaxies.
Multiplicity of Nearby Free-floating Ultracool Dwarfs: A Hubble Space Telescope WFPC2 Search for Companions

We present Hubble Space Telescope (HST) Wide Field Planetary Camera 2 (WFPC2) observations of a sample of 134 ultracool objects (spectral types later than M7) coming from the Deep Near Infrared Survey (DENIS), Two Micron All Sky Survey (2MASS), and Sloan Digital Sky Survey (SDSS), with distances estimated to range from 7 to 105 pc. Fifteen new ultracool binary candidates are reported here. Eleven known binaries are confirmed, and orbital motion is detected in some of them. We estimate that the closest binary systems in this sample have periods between 5 and 20 yr, and thus dynamical masses will be derived in the near future. For the calculation of binary frequency, we restrict ourselves to systems with distances less than 20 pc. After correction of the binaries bias, we find a ratio of visual binaries (at the HST limit of detection) of around 10%, and that ∼15% of the 26 objects within 20 pc are binary systems with separations between 1 and 8 AU. The observed frequency of ultracool binaries is similar to that of binaries with G-type primaries in the separation range from 2.1 to 140 AU. There is also a clear deficit of ultracool binaries with separations greater than 15 AU, and a possible tendency for the binaries to have mass ratios near unity. Most systems have indeed visual and near-infrared brightness ratios between 1 and 0.3. We discuss our results in the framework of current scenarios for the formation and evolution of free-floating brown dwarfs.
An Empirical Calibration of the Completeness of the SDSS Quasar Survey

Spectra of nearly 20,000 pointlike objects to a Galactic reddening–corrected magnitude of i = 19.1 have been obtained to test the completeness of the Sloan Digital Sky Survey (SDSS) quasar survey. We focus on spatially unresolved quasars, which comprise 94% of all SDSS quasars to the main survey magnitude limit. The objects were selected from all regions of color space, sparsely sampled from within a 278 deg2 area (effective area 233 deg2) of sky covered by this study. Only 10 quasars were identified that were not targeted as candidates by the SDSS quasar survey (including both color and radio source selection). The inferred density of unresolved quasars on the sky that are missed by the SDSS algorithm is 0.44 deg-2, compared with 8.28 deg-2 for the selected quasar density, giving a completeness of 94.9% to the limiting magnitude. Omitting radio selection reduces the color-only selection completeness by about 1%. Of the 10 newly identified quasars, three have detected broad absorption line systems, six are significantly redder than other quasars at the same redshift, and four have redshifts between 2.7 and 3.0 (the redshift range where the SDSS colors of quasars intersect the stellar locus). The fraction of quasars (and other unresolved sources) missed because of image defects and blends, independent of the selection algorithm, is ≈4%, but this number varies by a few percent with magnitude. Quasars with extended images comprise about 6% of the SDSS sample, and the completeness of the selection algorithm for extended quasars is approximately 81%, based on the SDSS galaxy survey. The combined end-to-end completeness for the SDSS quasar survey is ≈89%. The total corrected density of quasars on the sky to i = 19.1 is estimated to be 10.2 deg-2. The SDSS completeness restricted to z ≳ 3 quasars is expected to be considerably lower and is a strong function of redshift. The determination of the global completeness is required for the statistical properties of quasars to i = 19.1 derived from the SDSS data set, such as the luminosity function and correlation function, to be accurately determined.
A Quasi-linear Kinetic Theory for Charged-Particle Transport in Two-dimensional Turbulence

There is growing evidence for the presence of a strong two-dimensional MHD turbulence component in the solar wind. The theory for energetic charged-particle transport and energization in such two-dimensional turbulence, however, is not well developed. In particular, the role of turbulent electric fields, generated by the turbulent convective motions of the two-dimensional magnetic field fluctuations, needs to be clarified. We present a new quasi-linear kinetic theory of super-Alfvénic charged-particle transport and energization in quasi-static homogeneous incompressible two-dimensional MHD turbulence, including the associated turbulent electric fields. We find for a nearly gyrotropic particle distribution that field-aligned turbulent electric fields are mainly responsible for causing particle pitch angle scattering and momentum diffusion. The new theory allows for efficient scattering through a 90° pitch angle whereby a long-standing problem in standard magnetostatic quasi-linear theory is addressed anew.
Transport Phenomena in Stochastic Magnetic Mirrors

Parallel thermal conduction along stochastic magnetic field lines may be reduced because the heat-conducting electrons become trapped and detrapped between regions of strong magnetic field (magnetic mirrors). The problem reduces to a simple but realistic model for diffusion of monoenergetic electrons based on the fact that when there is a reduction of diffusion, it is controlled by a subset of the mirrors, the principal mirrors. The diffusion reduction can be considered as equivalent to an enhancement of the pitch angle scattering rate. Therefore, in deriving the collision integral, we modify the pitch angle scattering term. We take into account the full perturbed electron-electron collision integral, as well as the electron-proton collision term. Finally, we obtain the four plasma transport coefficients and the effective thermal conductivity. We express them as reductions from the classical values. We present these reductions as functions of the ratio of the magnetic field decorrelation length to the electron mean free path at the thermal speed VT = 1/2. We briefly discuss an application of our results to clusters of galaxies.
Semimodular functions and combinatorial geometries

A point-lattice £ being given, to any normalized, nondecreasing, integer-valued, semimodular function / defined on £, we can associate a class of combinatorial geometries called expansions of /. The family of expansions of / is shown to have a largest element for the weak map order, E(f), the free expansion of /. Expansions generalize and clarify the relationship between two known constructions, one defined by R
Discovery of the X-Ray Counterpart to the Rotating Radio Transient J1819–1458

We present the discovery of the first X-ray counterpart to a Rotating RAdio Transient (RRAT) source. RRAT J1819-1458 is a relatively highly magnetized (B ~ 5 × 1013 G) member of a new class of unusual pulsar-like objects discovered by their bursting activity at radio wavelengths. A Chandra observation of that position revealed a pointlike source, CXOU J181934.1-145804, with a soft spectrum well fit by an absorbed blackbody with NH = 7 × 1021 cm-2, temperature kT = 0.12 ± 0.04 keV, and an unabsorbed flux of ~2 × 10-12 ergs cm-2 s-1 between 0.5 and 8 keV. No optical or infrared (IR) counterparts are visible within 1'' of our X-ray position. The positional coincidence, spectral properties, and lack of an optical/IR counterpart make it highly likely that CXOU J181934.1-145804 is a neutron star and is the same object as RRAT J1819-1458. The source showed no variability on any timescale from the pulse period of 4.26 s up to the 5 day window covered by the observations, although our limits (especially for pulsations) are not particularly constraining. The X-ray properties of CXOU J181934.1-145804, while not yet measured to high precision, are similar to those of comparably aged radio pulsars and are consistent with thermal emission from a cooling neutron star.
Power counting with one-pion exchange

Techniques developed for handing inverse-power-law potentials in atomic physics are applied to the tensor one-pion exchange potential to determine the regions in which it can be treated perturbatively. In $S,P$, and $D$ waves, the critical values of the relative momentum are less than or of the order of 400 MeV. The Wilsonian renormalization group (RG) is then used to determine the power counting for short-range interaction in the presence of this potential. In the $P$ and $D$ waves, where there are no low-energy bound or virtual states, these interactions have half-integer RG eigenvalues and are substantially promoted relative to naive expectations. These results are independent of whether the tensor force is attractive or repulsive. In the ${}^{3}{S}_{1}$ channel, the leading term is relevant, but it is demoted by half an order compared to the counting for the effective-range expansion with only a short-range potential. The tensor force can be treated perturbatively in those $F$ waves and above that do not couple to $P$ or $D$ waves. The corresponding power counting is the usual one given by naive dimensional analysis.
Least Favorable Probability of Failure for 5- and 10-story RC Frame Structures with Vertical Irregularities

This article evaluates the seismic control effect of vertical irregularity factors for RC frame structures using the Monte Carlo simulation method. Typical 5- and 10-story frame structures with different irregularities of strength or stiffness are assessed. The upper- and lower-bound probabilities of failure exceeding the limit state are studied. The results indicate that the exceeding probability increases as the vertical irregularity factor decreases. The upper-bound probability of failure, which is sensitive to the vertical irregularities and is an effective indicator for evaluating the performance control parameter, is significantly larger compared with the lower-bound probability of failure. A minimum strength and stiffness irregularity factor of 0.7 can serve as the seismic control limit.
Effects of mode mixing and avoided crossings on the transverse spin in a metal-dielectic-metal sphere

We study transverse spin in a sub-wavelength metal-dielectric-metal (MDM) sphere when the MDM sphere exhibits the avoided crossing due to hybridization of the surface plasmon with the Mie localized plasmon. We show that the change in the absorptive and dispersive character near the crossing can have a significant effect on the transverse spin. An enhancement in the transverse spin is shown to be possible associated with the transparency (suppression of extinction) of the MDM sphere. The effect is attributed to the highly structured field emerging as a consequence of the competition of the electric and magnetic modes.
Rapid Progression of COVID-19-Associated Fatal Capillary Leak Syndrome

Several cases of capillary leak syndrome (CLS) related to COVID-19 or vaccination against SARS-CoV-2 have been described in the literature. We present a case of a 42-year-old, previously healthy male, presenting with a mild form of COVID-19, who suddenly developed severe shock with hypotension and severe hemoconcentration within hours of admission to the hospital. Volume resuscitation was not effective, increasing hemoglobin (198 g/L on admission, 222 g/L 9 h later) suggested fluid leak into peripheral tissues. After cardiac arrest, the patient was resuscitated and connected to extracorporeal membrane oxygenation, but died shortly afterwards due to refractory heart failure. Retrospective investigation of blood samples confirmed diagnosis of CLS by progressive hypoalbuminemia (40 g/L on admission, 14 g/L 19 h later) and monoclonal gammopathy kappa (4.7 g/L). Patient’s CLS was triggered by COVID-19, either a first attack of idiopathic CLS called Clarkson’s disease or a COVID-19-induced secondary CLS.
Bulges and Disklike Components in the Host Galaxies of Low-Redshift 3CR Sources: A Near-Infrared View of Their Radial Brightness Profiles

We analyze the near-infrared luminosity profiles and photometric parameters of the host galaxies of 3CR radio sources with z < 0.3, to investigate their physical nature. Our sample includes 82 galaxies, of which 22 (27%) are FR Is and 60 (73%) are FR IIs. Using near-infrared data taken both with NICMOS on board the Hubble Space Telescope and from the ground with the Telescopio Nazionale Galileo, we find that luminosity profiles are very well described by a single Sérsic law in 52% of the cases and that for the remaining objects (48%) it is necessary to include an exponential profile, which indicates the presence of a second disklike component. The average bulge-to-disklike components luminosity ratio for the galaxies is (b/e) ~ 1.1. The analysis of the photometric parameters of the subsamples indicates that FR Is and FR IIs show rather similar bulges in terms of effective surface magnitude, effective radius, and Sérsic index. On the other hand, the disklike components in FR I and FR II hosts show, on average, different properties. Central surface magnitudes are dimmer and scale lengths are greater by a factor of 2 in FR Is when compared to FR IIs. We also estimate the black hole mass associated with each galaxy using two different methods that claim tight correlations of the black hole mass (MBH) with the infrared bulge luminosity (Lbulge) and with the Sérsic index (n). Our data indicate that masses obtained through these two methods show a high dispersion and that MBH obtained through Lbulge are systematically higher (by a factor of ~3) than those obtained using n. This result may reflect the fact that for our sample galaxies we do not find any correlation between Lbulge and n.
Fresh look at the scalar-tensor theory of gravity in Jordan and Einstein frames from undiscussed standpoints

We study the scalar-tensor theory of gravity profoundly in the action level as well as in the thermodynamic level. Contrary to the usual description in the literature about the equivalence in the two conformally connected frames, this paper addresses several incomplete inferences regarding it and mentions some inequivalences which were not pointed out earlier. In the thermodynamic level, our analysis shows the two frames are equivalent. In that process, we identify the entropy, the energy and the temperature for the thermodynamic description, and we find these quantities are conformally invariant even without any prior assumption. The same conclusion is reached from the gravitational action as well as from the Gibbons-Hawking-York boundary term, establishing the result in a more convincing manner.
Dephasing mechanisms of diamond-based nuclear-spin memories for quantum networks

We probe dephasing mechanisms within a quantum network node consisting of a single nitrogen-vacancy center electron spin that is hyperfine coupled to surrounding C13 nuclear-spin quantum memories. Previous studies have analyzed memory dephasing caused by the stochastic electron-spin reset process, which is a component of optical internode entangling protocols. Here, we find, by using dynamical decoupling techniques and exploiting phase matching conditions in the electron-nuclear dynamics, that control infidelities and quasistatic noise are the major contributors to memory dephasing induced by the entangling sequence. These insights enable us to demonstrate a 19-fold improved memory performance which is still not limited by the electron reinitialization process. We further perform pump-probe studies to investigate the spin-flip channels during the optical electron spin reset. We find that spin flips occur via decay from the metastable singlet states with a branching ratio of 8(1):1:1, in contrast with previous work. These results allow us to formulate straightforward improvements to diamond-based quantum networks and similar architectures.
Spatially Resolved STIS Spectra of WR + OB Binaries with Colliding Winds

We present spatially resolved spectra of the visual WR + OB massive binaries WR 86, WR 146, and WR 147, obtained with the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope. The systems are classified as follows: WR 86 = WC 7 + B0 III, WR 146 = WC 6 + O8 I–IIf, WR 147 = WN 8 + O5–7 I–II(f). Both WR 146 and WR 147 are known to have strong nonthermal radio emission arising in a wind-wind collision shock zone between the WR and OB components. We find that the spectra of their O companions show Hα profiles in emission, indicative of large mass-loss rates and consistent with the colliding-wind model. Our spectra indicate that the B component in WR 86 has a low mass-loss rate, which possibly explains the fact that WR 86, despite being a long-period WR + OB binary, was not found to be a strong nonthermal radio emitter. Because of the small mass-loss rate of the B-star component in WR 86, the wind collision region must be closer to the B star and smaller in effective area, hence generating smaller amounts of nonthermal radio emission. Absolute magnitudes for all the stars are estimated based on the spectral types of the components (based on the tables by Schmidt-Kaler for OB stars and van der Hucht for WR stars) and compared with actual, observed magnitude differences. While the derived luminosities for the WC 7 and B0 III stars in WR 86 are consistent with the observed magnitude difference, we find a discrepancy of at least 1.5 mag between the observed luminosities of the components in each of WR 146 and WR 147 and the absolute magnitudes expected from their spectral types. In both cases, it looks as though either the WR components are about 2 mag too bright for their spectral types or that the O components are about 2 mag too faint. We discuss possible explanations for this apparent discrepancy.
A practical computational method for the anisotropic redshift-space three-point correlation function

Author(s): Slepian, Z; Eisenstein, DJ | Abstract: © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. We present an algorithm enabling computation of the anisotropic redshift-space galaxy threepoint correlation function (3PCF) scaling as N2, with N the number of galaxies. Our previous work showed how to compute the isotropic 3PCF with this scaling by expanding the radially binned density field around each galaxy in the survey into spherical harmonics and combining these coefficients to form multipole moments. The N2 scaling occurred because this approach never explicitly required the relative angle between a galaxy pair about the primary galaxy. Here, we generalize this work, demonstrating that in the presence of azimuthally symmetric anisotropy produced by redshift-space distortions (RSD), the 3PCF can be described by two triangle side lengths, two independent total angular momenta, and a spin. This basis for the anisotropic 3PCF allows its computation with negligible additional work over the isotropic 3PCF. We also present the covariance matrix of the anisotropic 3PCF measured in this basis. Our algorithm tracks the full 5D redshift-space 3PCF, uses an accurate line of sight to each triplet, is exact in angle, and easily handles edge correction. It will enable use of the anisotropic large-scale 3PCF as a probe of RSD in current and upcoming large-scale redshift surveys.