Miracle-dz/UniFAR-FTUs huggingface dataset:
The large- and small-scale properties of the intergalactic gas in the Slug Ly α nebula revealed by MUSE Heiiemission observations

With a projected size of about 450 kpc at z~2.3, the Slug Ly-alpha nebula is a rare laboratory to study, in emission, the properties of the intergalactic gas in the Cosmic Web. Since its discovery, the Slug has been the subject of several spectroscopic follow-ups to constrain the properties of the emitting gas. Here we report the results of a deep MUSE integral-field spectroscopic search for non-resonant, extended HeII1640 and metal emission. Extended HeII radiation is detected on scales of about 100 kpc, but only in some regions associated with the bright Ly-alpha emission and a continuum-detected source, implying large and abrupt variations in the line ratios across adjacent regions in projected space. The recent detection of associated H-alpha emission and similar abrupt variations in the Ly-alpha kinematics, strongly suggest that the HeII/Ly-alpha gradient is due to large variations in the physical distances between the associated quasar and these regions. This implies that the overall length of the emitting structure could extend to physical Mpc scales and be mostly oriented along our line of sight. At the same time, the relatively low HeII/Ly-alpha values suggest that the emitting gas has a broad density distribution that - if expressed in terms of a lognormal - implies dispersions as high as those expected in the interstellar medium of galaxies. These results strengthen the possibility that the density distribution of intergalactic gas at high-redshift is extremely clumpy and multiphase on scales below our current observational spatial resolution of a few physical kpc.
The Temporal and Spatial Scales of Density Structures Released in the Slow Solar Wind During Solar Activity Maximum

In a recent study, we took advantage of a highly tilted coronal neutral sheet to show that density structures, extending radially over several solar radii (Rs), are released in the forming slow solar wind approximately 4–5 Rs above the solar surface. We related the signatures of this formation process to intermittent magnetic reconnection occurring continuously above helmet streamers. We now exploit the heliospheric imagery from the Solar Terrestrial Relation Observatory (STEREO) to map the spatial and temporal distribution of the ejected structures. We demonstrate that streamers experience quasi-periodic bursts of activity with the simultaneous outpouring of small transients over a large range of latitudes in the corona. This cyclic activity leads to the emergence of well-defined and broad structures. Derivation of the trajectories and kinematic properties of the individual small transients that make up these large-scale structures confirms their association with the forming slow solar wind (SSW). We find that these transients are released, on average, every 19.5 hr, simultaneously at all latitudes with a typical radial size of 12 Rs. Their spatial distribution, release rate, and three-dimensional extent are used to estimate the contribution of this cyclic activity to the mass flux carried outward by the SSW. Our results suggest that, in interplanetary space, the global structure of the heliospheric current sheet is dominated by a succession of blobs and associated flux ropes. We demonstrate this with an example event using STEREO-A in situ measurements.
Detailed multiwavelength modelling of the dark GRB 140713A and its host galaxy

We investigate the afterglow of GRB 140713A, a gamma-ray burst (GRB) that was detected and relatively well sampled at X-ray and radio wavelengths, but was not present at optical and near-infrared wavelengths, despite searches to deep limits. We present the emission spectrum of the likely host galaxy at z = 0.935 ruling out a high-redshift explanation for the absence of the optical flux detection. Modelling the GRB multiwavelength afterglow using the radiative transfer hydrodynamics code boxfit provides constraints on physical parameters of the GRB jet and its environment, for instance a relatively wide jet opening angle and an electron energy distribution slope p below 2. Most importantly, the model predicts an optical flux about two orders of magnitude above the observed limits. We calculated that the required host extinction to explain the observed limits in the r, i, and z bands was A rm host-V gt 3.2 mag, equivalent to E(B ' V) host > 1.0 mag. From the X-ray absorption we derive that the GRB host extinction is A rm host-V = 11.6 +7.5-5.3 mag, equivalent to E(B-V) rm host = 3.7 +2.4-1.7 mag, which is consistent with the extinction required from our boxfit derived fluxes. We conclude that the origin of the optical darkness is a high level of extinction in the line of sight to the GRB, most likely within the GRB host galaxy. © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
NKp44-Derived Peptide Used in Combination Stimulates Antineoplastic Efficacy of Targeted Therapeutic Drugs

Lung cancer cells in the tumor microenvironment facilitate immune evasion that leads to failure of conventional chemotherapies, despite provisionally decided on the genetic diagnosis of patients in a clinical setup. The current study follows three lung cancer patients who underwent “personalized” chemotherapeutic intervention. Patient-derived xenografts (PDXs) were subjected to tumor microarray and treatment screening with chemotherapies, either individually or in combination with the peptide R11-NLS-pep8; this peptide targets both membrane-associated and nuclear PCNA. Ex vivo, employing PDX-derived explants, it was found that combination with R11-NLS-pep8 stimulated antineoplastic effect of chemotherapies that were, although predicted based on the patient’s genetic mutation, inactive on their own. Furthermore, treatment in vivo of PDX-bearing mice showed an exactly similar trend in the result, corroborating the finding to be translated into clinical setup.
Photon superbunching from a generic tunnel junction

Photon pairs are generated in an electrically driven tunnel junction. Generating time-correlated photon pairs at the nanoscale is a prerequisite to creating highly integrated optoelectronic circuits that perform quantum computing tasks based on heralded single photons. Here, we demonstrate fulfilling this requirement with a generic tip-surface metal junction. When the junction is luminescing under DC bias, inelastic tunneling events of single electrons produce a stream of visible photons of plasmonic origin whose superbunching index is 17 (improved to a record of 70 by the authors during publication) when measured with a 53-ps instrumental resolution limit. The effect is driven electrically, rather than optically. This discovery has immediate and profound implications for quantum optics and cryptography, notwithstanding its fundamental importance to basic science and its ushering in of heralded photon experiments on the nanometer scale.
Unifying B2 radio galaxies with BL Lacertae objects

In an earlier paper we presented nuclear X-ray flux densities , measured with ROSAT, for the B2 bright sample of nearby low-luminosity radio galaxies. In this paper we construct a nuclear X-ray luminosity function for the B2 radio galaxies, and discuss the consequences of our results for models in which such radio galaxies are the parent population of BL Lac objects. Based on our observations of the B2 sample, we use Monte Carlo techniques to simulate samples of beamed radio galaxies, and use the selection criteri a of existing samples of BL Lac objects to compare our simulated results to what is observed. We find that previous analytical results are not applicable since the BL Lac samples are selected on beamed flux density. A simple model in which BL Lacs are the moderately beamed (γ � 3) counterparts of radio galaxies, with some random dispersion (� 0.4 decades) in the intrinsic radio-X-ray relationship, can reproduce many of the features of the radio-selected and X-ray-selected BL Lac samples, including their radio and X-ray luminosity functions and the distributions of their radio-to-X-ray spectral indices. In contrast, models in wh ich the X-ray and radio emission have systematically different beaming parameters cannot reproduce important features of the radio-galaxy and BL Lac populations, and recently proposed models in which the radio-toX-ray spectral index is a function of source luminosity cannot in themselves account for the differences in the slopes of the radio and X-ray-selected BL Lac luminosity functions. The redshift distribution and number counts of the X-ray-selected EMSS sample are well reproduced by our best models, supporting a picture in which these objects are beamed FRI radio galaxies with intrinsic luminosities similar to those of th e B2 sample. However, we cannot match the redshift distribution of the radio-selected 1-Jy sample, and it is likely that a population of FRII radio galaxies is responsible for the high-r edshift objects in this sample, in agreement with previously reported results on the sample’s radio and optical-emission-line properties.
Spontaneous breaking of the Fermi-surface symmetry in the t-J model : A numerical study

We present a variational Monte Carlo (VMC) study of spontaneous Fermi surface symmetry breaking in the t-J model. We find that the variational energy of a Gutzwiller projected Fermi sea is lowered by allowing for a finite asymmetry between the x- and the y-directions. However, the best variational state remains a pure superconducting state with d-wave symmetry, as long as the underlying lattice is isotropic. Our VMC results are in good overall agreement with slave boson mean field theory (SBMFT) and renormalized mean field theory (RMFT), although apparent discrepancies do show up in the half-filled limit, revealing some limitations of mean field theories. VMC and complementary RMFT calculations also confirm the SBMFT predictions that many-body interactions can enhance any anisotropy in the underlying crystal lattice. Thus, our results may be of consequence for the description of strongly correlated superconductors with an anisotropic lattice structure.
A multi‐model approach to intravenous filter optimization

We present a multi‐model approach to the study of side‐effects of endovascular implants. A 2D model of elastic walls and a local 3D model of blood flow are combined with a 1D network blood circulation model. The three numerical models form an endovascular computational stand. Copyright © 2010 John Wiley & Sons, Ltd.
Two-tone optomechanical instability in backaction-evading measurements

While quantum mechanics imposes a fundamental limit on the precision of interferometric measurements of mechanical motion due to measurement backaction, the nonlinear nature of the coupling also leads to parametric instabilities that place practical limits on the sensitivity by limiting the power in the interferometer. Such instabilities have been extensively studied in the context of gravitational wave detectors, and their presence has recently been reported in Advanced LIGO. Here we observe experimentally and describe theoretically a new type of optomechanical instability that arises in two-tone backaction-evading (BAE) measurements, designed to overcome the standard quantum limit (SQL), and demonstrate the effect in the optical domain with a photonic crystal nanobeam, and in the microwave domain with a micromechanical oscillator coupled to a microwave resonator. In contrast to the well-known oscillatory parametric instability that occurs in single-tone, blue-detuned pumping, which is characterized by a vanishing effective mechanical damping, the parametric instability in balanced two-tone optomechanics is exponential, and is a result of small detuning errors in the two pump frequencies. Its origin can be understood in a rotating frame as the vanishing of the effective mechanical frequency due to an optical spring effect. Counterintuitively, the instability occurs even in the presence of perfectly balanced intracavity fields, and can occur for both signs of detuning. We find excellent quantitative agreement with our theoretical predictions. Since the constraints on tuning accuracy become stricter with increasing probe power, it imposes a fundamental limitation on BAE measurements, as well as other two-tone schemes. In addition to introducing a new limitation in two-tone BAE measurements, the results also introduce a new type of nonlinear dynamics in cavity optomechanics.
Model-based linear manifold clustering

A new paradigm of clustering called “Linear Manifold Clustering” which is based on linear manifolds is designed, analyzed, and evaluated throughout this thesis. A Linear manifold is a translated subspace. Linear manifold clustering seeks to identify groups of points that are embedded in lower dimensional linear manifolds. The “birth” of this paradigm of clustering is a consequence of what we believe is a need for an important yet overlooked cluster model, and as a result of what we identify as an acute need to sufficiently address certain clustering requirements that current state of art methods are unable to address. In many problem domains it assumed that linear models are sufficient enough to describe and capture the data's inherent structure. Yet very few remote attempts have been made to devise clustering methods able to identify or learn mixtures of linear manifolds. None of these attempts posed the problem in a model-based statistical setting intended to model and understand the underlying “process” responsible for generating sets of points that lie on lower dimensional linear manifolds. In this thesis we introduce a formal stochastic linear manifold cluster model. Based on this model we present a series of results and techniques demonstrating the applicability of the linear manifold clustering paradigm to a wide range of applications. We show that this model is a generalization of other more common and somewhat limited cluster models. This generalization allows for less assumptions to be imposed on the data, which typically yield biased results, and more freedom for the data to “speak for itself”. An emphasis is put on the paradigms of pattern and correlation clustering and on the application of DNA microarray analysis, where we show that pattern clusters or correlations manifest themselves as linear manifolds in the data space. Based on the linear manifold cluster model we present two clustering algorithms: one for clustering or learning mixtures of linear manifolds, and the other tailored to the application of correlation clustering and DNA micro array analysis. The efficacy of these techniques is demonstrated by a series of experiments on synthetic and real data sets. Most clustering methods focus only on the grouping aspects of clustering and lack the ability to provide any scientific content. In this thesis, we also present two linear manifold based modeling techniques that deliver scientific content and with which data can be described. One based on a probabilistic density estimation model with which statistical inference such as predictions can be based upon. The other, a model which describes the linear dependencies in the data in the form of a set of linear equations.
The CERES Astronomical Database

Abstract: The CERES Astronomical Archive was created initially in order to make the large amount of data that were collected from the two surveys, the Jodrell-VLA Astrometric Survey (JVAS) and the Cosmic Lens All-Sky Survey (CLASS), easily accessible to the partner members of the Consortium for European Research on Extragalactic Surveys (CERES) through the web. Here we describe the web based archive of the 15,000 flat spectrum radio sources. There is a wealth of information that one can access including downloading the raw and processed data for each of the sources. We also describe the search engines that were developed so that a) one can search through the archive for an object or a sample of objects by setting specific criteria and b) select new samples. Since new data are continually gathered on the same sources from follow up programs, an automatic update engine was created so that the new information and data can be added easily in the archive.
Cluster Merger Variance and the Luminosity Gap Statistic

The presence of multiple luminous galaxies in clusters can be explained by the finite time over which a galaxy sinks to the center of the cluster and merges with the central galaxy. The simplest measurable statistic to quantify the dynamical age of a system of galaxies is the luminosity (magnitude) gap, which is the difference in photometric magnitude between the two most luminous galaxies. We present a simple analytical estimate of the luminosity gap distribution in groups and clusters as a function of dark matter halo mass. The luminosity gap is used to define "fossil" groups; we expect the fraction of fossil systems to exhibit a strong and model-independent trend with mass: ~1%-3% of massive clusters and ~5%-40% of groups should be fossil systems. We compare our predictions to the luminosity gap distribution in a sample of 730 clusters in the Sloan Digital Sky Survey C4 Catalog and find good agreement. This suggests that theoretical excursion-set merger probabilities and the standard theory of dynamical segregation are valid on cluster scales.
DMStag: Staggered, Structured Grids for PETSc

“Staggered grid” codes arise in many applications, where a physical problem is discretized and solved in terms of unknowns located at different locations on a structured grid. For example, the Navier-Stokes and Stokes equations can be solved on a staggered grid with the classical Marker and Cell (MAC) method (Harlow & Welch, 1965), storing pressure unknowns in element centers and velocities on element boundaries. This gives a simple and compact method which exhibits superior numerical properties to colocated grid methods which consider all unknowns to be located on the same grid of points.
Relationship between Key Environmental Factors and the Architecture of Fruit Shape and Size in Near-Isogenic Lines of Cucumber (Cucumis sativus L.)

Fruit shape and size are complex traits influenced by numerous factors, especially genetics and environment factors. To explore the mechanism of fruit shape and size development in cucumber, a pair of near-isogenic lines (NIL) Ln35 and Ln37 were used. The fruit length and diameter, cell length and diameter, and related gene expression were measured. Both the fruit length, diameter, and cell length and diameter showed sigmate curves in the two lines. The cell length and diameter were significantly positively correlated with fruit length and diameter both in two lines. The expression of CsACS2 and CsLNG showed significant positive correlations with fruit length and diameter increment in Ln35, and there was no correlation in Ln37. Furthermore, there were significant positive correlations between fruit size and thermal effectiveness (TE), as well as between fruit size and photosynthetic active radiation (PAR), both in two lines. Two models using logistic regression were formulated to assess the relationships among fruit length and diameter in Ln35 and Ln37, respectively, based on thermal effectiveness and photosynthetic active radiation (TEP). The coefficient R2 values of the models were 0.977 and 0.976 in Ln35, and 0.987 and 0.981 in Ln37, respectively. The root mean square error (RMSE) was 12.012 mm and 4.338 mm in Ln35, and 5.17 mm and 7.082 mm in Ln37, respectively, which illustrated the accurate and efficient of these models. These biologically interpreted parameters will provide precision management for monitoring fruit growth and forecasting the time of harvesting under different temperatures and light conditions.
Inferring a difference in the star-forming properties of lower versus higher X-ray luminosity AGNs

We explore the distribution of RMS ≡ SFR/SFRMS (where SFRMS is the star formation rate of ‘main-sequence’ star-forming galaxies) for AGN hosts at z = 1. We split our sample into two bins of X-ray luminosity divided at LX = 2 × 1043 erg s−1 to investigate whether the RMS distribution changes as a function of AGN power. Our main results suggest that, when the RMS distribution of AGN hosts is modelled as a log-normal distribution (i.e. the same shape as that of MS galaxies), galaxies hosting more powerful X-ray AGNs (i.e. LX > 2 × 1043 erg s−1) display a narrower RMS distribution that is shifted to higher values compared to their lower LX counterparts. In addition, we find that more powerful X-ray AGNs have SFRs that are more consistent with that of MS galaxies compared to lower LX AGNs. Despite this, the mean SFRs (as opposed to RMS) measured from these distributions are consistent with the previously observed flat relationship between SFR and LX. Our results suggest that the typical star-forming properties of AGN hosts change with LX, and that more powerful AGNs typically reside in more MS-like star-forming galaxies compared to lower LX AGNs.
Tracing the Dynamics of Disk Galaxies with Optical and Infrared Surface Photometry: Color Gradients in M99

We present optical and IR surface photometry of M99 (NGC 4254) at g, r_S i, J and K'. We also present a K' image of M51 (NGC 5194) for comparison. Fourier decomposition of the disk light reveals that the radial distribution of power depends on wavelength, which in turn implies that the spiral structure traced in the visual (i.e. young population I and dust) is different from the one detected at 2 microns (i.e. old stellar disk). We observe radial modulation of the power and a dependency of power with wavelength that are consistent with modal theory of spiral structure. A central motivation for our research is the fundamental idea of density wave theory that the passage of a spiral density wave triggers star formation. We have found a stellar population age gradient consistent with this scenario in a reddening-free, red supergiant-sensitive, Q-like photometric parameter at 6 kpc galactocentric distance across one of the arms of M99. We rule out that the change in this parameter, Q(r_SJgi), across the arm is mainly due to dust. The difference in Q(r_SJgi) going from the interarm regions to the arms also indicates that arms cannot be due exclusively to crowding of stellar orbits. We present the first measurement of Omega_p, the angular speed of the spiral pattern, and of the location of the corotation radius, derived from the drift velocity of the young stars away from their birth site. The measured Q(r_SJgi) implies a star formation rate for M99 within the range of 10-20 M_odot/yr; a disk stellar mass surface density of ~80 M_odot/pc^2; and a maximum contribution of ~20 percent from red supergiants to the K' light in a small region, and much smaller on average. We measure a K' arm--interarm contrast of 2-3, too high for M99 to be a truly isolated galaxy.
Full counting statistics of chaotic cavities with many open channels

Explicit formulas are obtained for all moments and for all cumulants of the electric current through a quantum chaotic cavity attached to two ideal leads, thus providing the full counting statistics for this type of system. The approach is based on random matrix theory, and is valid in the limit when both leads have many open channels. For an arbitrary number of open channels we present the third cumulant and an example of nonlinear statistics.