Miracle-dz/UniFAR-FTUs huggingface dataset:
The nonperturbative closed string tachyon vacuum to high level

We compute the action of closed bosonic string field theory at quartic order with fields up to level ten. After level four, the value of the potential at the minimum starts oscillating around a nonzero negative value, in contrast with the proposition made in [5]. We try a different truncation scheme in which the value of the potential converges faster with the level. By extrapolating these values, we are able to give a rather precise value for the depth of the potential.
Semi-simple group unification in the supersymmetric brane world

The conventional supersymmetric grand uniﬁed theories suﬀer from two se-rious problems, the large mass splitting between doublet and triplet Higgs multiplets, and the too long lifetime of the proton. A uniﬁcation model based on a semi-simple group SU(5) GUT × U(3) H has been proposed to solve both of the problems simultaneously. Although the proposed model is perfectly consistent with observations, there are various mysteries. In this paper, we show that such mysterious features in the original model are naturally explained by embedding the model into the brane world in a higher dimensional space-time. In particular, the relatively small gauge coupling constant of the SU(5) GUT at the uniﬁcation energy scale is a consequence of relatively large volume of extra dimensions. Here, we put the SU(5) GUT gauge multiplet in a 6-dimensional bulk and assume all ﬁelds in the U(3) H sector to reside on a 3-dimensional brane located in the bulk. On the other hand, all chiral multiplets of quarks, leptons and Higgs are assumed to reside on a 3-brane at a T 2 / Z 4 orbifold ﬁxed point. The quasi- N = 2 supersymmetry in the hypercolor U(3) H sector is understood as a low-energy remnant of the N = 4 supersymmetry in a 6-dimensional space-time. We further extend the 6-dimensional model to a 10-dimensional theory. Possible frameworks of string theories are also investi-gated to accommodate the present brane-world model. We ﬁnd that the type
Gemini IFU, VLA, and HST observations of the OH Megamaser Galaxy IRAS17526 + 3253★

We present a multiwavelength study of the OH megamaser galaxy IRAS17526 + 3253, based on new Gemini multi-object spectrograph integral field unit (GMOS/IFU) observations, Hubble Space Telescope F814W, and H α + [N ii] images, and archival 2MASS and 1.49 GHz VLA data. The Hubble Space Telescope(HST) images clearly reveal a mid-to-advanced stage major merger whose northwestern and southeastern nuclei have a projected separation of ∼8.5 kpc. Our HST/H α + [N ii] image shows regions of ongoing star formation across the envelope on ∼10 kpc scales, which are aligned with radio features, supporting the interpretation that the radio emission originates from star-forming regions. The measured H α luminosities imply that the unobscured star formation rate (SFR) is ∼10–30 M⊙ yr−1. The GMOS/IFU data reveal two structures in northwestern separated by 850 pc and by a discontinuity in the velocity field of ∼ 200 km s−1. We associate the blueshifted and redshifted components with, respectively, the distorted disc of northwestern and tidal debris, possibly a tail originating in southeastern. Star formation is the main ionization source in both components, which have SFRs of ∼2.6–7.9 M⊙ yr−1 and ∼1.5–4.5 M⊙ yr−1, respectively. Fainter line emission bordering these main components is consistent with shock ionization at a velocity ∼200 km s−1 and may be the result of an interaction between the tidal tail and the northwestern galaxy’s disc. IRAS17526 + 3253 is one of only a few systems known to host both luminous OH and H2O masers. The velocities of the OH and H2O maser lines suggest that they are associated with the northwestern and southeastern galaxies, respectively (Martin et al.; Wagner).
Broadband Optical‐Fiber‐Compatible Photodetector Based on a Graphene‐MoS2‐WS2 Heterostructure with a Synergetic Photogenerating Mechanism

Integrating 2D crystals into optical fibers can grant them optoelectronic properties and extend their range of applications. However, the ability to produce complicated structures is limited by the challenges of chemical vapor deposition manufacturing. Here, a 2D‐material heterostructure created on a fiber end‐face is successfully demonstrated by integrating a microscale multilayer graphene‐MoS2‐WS2 heterostructure film on it, using a simple layer‐by‐layer transferring method. The all‐in‐fiber photodetector (FPD) exhibits an ultrahigh photoresponsivity of ≈6.6 × 107 A·W−1 and a relatively fast time response of ≈7 ms at 400 nm light wavelength, due to the strong light absorption and the built‐in electric field of the heterostructure. Moreover, owing to the type‐II staggered band alignments in the MoS2‐WS2 heterostructure, the interlayer optical transition between the MoS2 and WS2 layers enables the FPD to sense the infrared light, displaying a photoresponsivity of ≈17.1 A·W−1 at 1550 nm. In addition, an inverse photoresponse is observed under high illuminating powers, indicating a competing photocurrent generation mechanism, comprising the photoconductive and photobolometric effects. It is believed that the findings will offer a new strategy for the development of novel all‐fiber optoelectronic devices based on 2D crystals.
Electronic coherence in metals: comparing weak localization and time-dependent conductance fluctuations

Quantum corrections to the conductivity allow experimental assessment of electronic coherence in metals. We consider whether independent measurements of different corrections are quantitatively consistent, particularly in systems with spin-orbit or magnetic impurity scattering. We report weak localization and time-dependent universal conductance fluctuation data in quasi-one- and two-dimensional AuPd wires between 2 and $20\phantom{\rule{0.3em}{0ex}}\mathrm{K}$. The data inferred from both methods are in excellent quantitative agreement, implying that precisely the same coherence length is relevant to both corrections.
Far Ultraviolet Spectroscopic Explorer Observations of O VI Overlying the Scutum Supershell

We present Far Ultraviolet Spectroscopic Explorer observations of the B0 III star HD 177989 (l = 17.°8, b = -11.°9, d = 4.9 kpc). This line of sight passes through the high-latitude outflow from the Scutum supershell (GS 018-04+44), a structure that lies at a kinematic distance of ~3.5 kpc and spans ~5° in diameter. The O VI λ1031. 93 line is compared with Space Telescope Imaging Spectrograph (STIS) observations of Si IV, C IV, and N V to examine the ionizing mechanisms responsible for producing the high ion absorption, as well as to study the processes by which gas is expelled into the halo. The O VI profile spans a similar velocity range as the other highly ionized atoms, from -70 to +80 km s-1. Component fits reveal very broad absorption at the kinematic velocity of the Scutum shell, which differs from the narrow Si IV, C IV, and N V components, suggesting that these other species occupy a more confined region. It is possible that the O VI is present in hot gas from the shell interior that is diffusing into the high-latitude region above it. The column densities in the Scutum supershell component are N(Si ) = (3.59 ± 0.09) × 1013, N(C ) = (1.78 ± 0.04) × 1014, N(N ) = (8.89 ± 0.79) × 1012, and N(O ) = (7.76 ± 0.75) × 1013 cm-2. The corresponding column density ratios of N(C )/N(Si ) = 4.96 ± 0.17, N(C )/N(N ) = 20.0 ± 1.8, and N(C )/N(O ) = 2.29 ± 0.23 show that while the C IV and Si IV columns are amplified in this region, the enhancement is not reflected in N V or O VI. We suggest that such ionic ratios and column densities could be produced by ~150-200 turbulent mixing layers lying in a fragmented medium above the polar cap of the superbubble. We note through a sight-line comparison that although these absorption characteristics are similar to those near the center of Radio Loops I and IV, they differ considerably from those near the edges of the loops. It is apparent that the traits of high ion absorption in a supershell, as well as the ionizing mechanisms responsible, can vary among sight lines through the shell.
Subclustering in rich clusters of galaxies and their environs

Substructure and small-scale clustering in and around rich clusters of galaxies formed in different cosmogonic scenarios are studied using N-body simulations and the results are compared with available observations. Several new statistical tests for subclustering are developed and applied to both the simulated and observed clusters. Results indicate the presence of some substructure in both the simulated and observed clusters. However, in most cases the actual amount of subclustering detected within the inner few megaparsecs is rather small. The results suggest that most rich clusters are in a relaxed state at present. A more promising means for distinguishing between the different cosmogonic scenarios is found from statistical measurements of small-scale clustering in the regions immediately surrounding rich clusters in the simulations, which show significant dependence on the amount of small-scale power present in the initial fluctuation spectrum. 65 references.
On the Mathematical Modeling of Pollen Dispersal and Deposition

Abstract A common method of predicting pollen concentration in a turbulent atmosphere involves solving a partial differential equation that governs the simultaneous convection and diffusion of airborne particles. This equation is subject to boundary conditions that include a mathematical description of the settling out process. This paper concentrates on the form of the lower boundary condition. We discuss (with reference to the structure of well known Gaussian solutions) the limitations of using a constant deposition velocity and show that errors induced when studying dispersal in an open environment are significantly reduced when applied to problems of transport through forests or plant canopies.
Thermodynamic performance evaluation of an air-air heat pipe heat exchanger

In this paper, heat transfer analysis for an air-air heat exchanger was experimentally carried out to find its thermal performance and effectiveness. Air-air heat exchanger equipped with finned heat pipes was considered for the experimentation. Mass flow rate of air was considered in between 0.24 to 0.53 [kg/sec]. The temperature at the condenser side of the heat pipe heat exchanger was kept constant at around 23 [°C] and at the evaporator part it was varied from 88 to 147 [°C]. The performance of heat pipe heat exchanger was evaluated at different mass flow rate of air, in terms of effectiveness and compared with its corresponding value found by theoretical analysis.
Limitations of ray tracing techniques in optical modeling of silicon solar cells and photodiodes

The physical optical effects which take place when the size of the surface textures of a solar cell or a photodiode is in the micron range are studied. Both the antireflective and the light trapping properties of linear periodic grooves of triangular cross sections are treated in the framework of an exact, coupled-wave, electromagnetic analysis. The most important physical optics effects are the diffraction of light at the groove edges, the interference of light reflected by the different surfaces of the grooves, and the tunneling across the grooved surface of light incident from the silicon side at an angle greater than the critical angle. There is also the effect of the interference of the light reflected by the front and back surfaces of the silicon layer which is important only for very thin layers. As the groove period increases above the wavelength, the exact results approach the geometrical optics predictions rather slowly in an oscillatory way. Simple physical optics arguments are presented for ob.
EGRET Upper Limits and Stacking Searches of Gamma-Ray Observations of Luminous and Ultraluminous Infrared Galaxies

We present a stacking analysis of EGRET γ-ray observations at the positions of luminous and ultraluminous infrared galaxies. The latter were selected from the recently presented HCN survey, which is thought to contain the most active star-forming regions of the universe. Different sorting criteria are used, and since there is no positive collective detection of γ-ray emission from these objects, we determined both collective and individual upper limits. The uppermost excess we find appears in the case of ULIRGs ordered by redshift, at a value of 1.8 σ.
3D Morphable Models and Beyond

3D Morphable Models are models separating shape from appearance variation. Typically, they are used as a statistical prior in computer graphics and vision. Recent success with neural representations have caused a resurgence of interest in visual computing problems, leading to more accurate, higher fidelity, more expressive, and memory-efficient solutions. This report documents the program and the outcomes of Dagstuhl Seminar 22121, “3D Morphable Models and Beyond”. This meeting of 39 researchers covered various topics, including 3D morphable models, implicit neural representations, physics-inspired approaches, and more. We summarise the discussions, presentations and results of this workshop.
Syntactic identity and locality restrictions on verbal ellipsis

This dissertation investigates the topic of verbal ellipsis in English. Two main issues are addressed in this work: (i) the identity condition that restricts the application of ellipsis and (ii) the different locality restrictions that apply to elliptical constructions. The identity condition is examined from the point of view of competence, while the locality condition is given a natural answer from the processing domain. Furthermore, a parsing algorithm based on minimalist grammars is defined. Chapter 1 introduces the topic. Chapter 2 and Chapter 3 deal with the syntactic identity condition. Chapter 2 reviews some proposals in the literature, namely, Lasnik (1995b), Kitagawa (1991) and Fiengo and May (1994). All these analyses examine controversial examples where, apparently, partial syntactic identity between antecedent and gap is found. Chapter 3 presents a new analysis which assumes late lexical insertion, in the spirit of derivational morphology (Marantz 1993), and offers a unified account of all the cases of partial identity introduced in the previous chapter. It is argued that syntactic identity must be respected, and that the crucial notion for ellipsis is identity of syntactic categories—a condition that is met before lexical items are inserted. Also, the different readings that obtain under ellipsis (i.e., sloppy and strict readings) are explained as emerging at different points in the derivation: before and after lexical insertion, respectively. Chapter 4 reviews one proposal in the parsing literature (Lappin and McCord 1990) as well as the problems it faces. Chapter 5 offers a processing account of the locality restrictions on gapping (as opposed to VPE and Pseudogapping), those are analyzed as a result of (i) tense absence/presence (Fodor 1985), (ii) low initial attachment of coordinates, and (iii) Spell-out operations which render syntactic structure unavailable (Uriagereka 1999). A two-fold ellipsis resolution process is presented here—where some work is done on-line, but some at the LF level. Chapter 6 defines an algorithm based on minimalist grammar operations, precisely on the preference of Merge-over-Move-over-Spell-out (as defined by Weinberg 1999); thus, showing that minimalist grammar models can be translated into computational models. Chapter 7 presents the conclusions.
A genetic algorithm for the biconnectivity augmentation problem

In this paper we present a genetic algorithm (GA) for the NP-hard biconnectivity problem for graphs. Suppose a 2-connected, undirected weighted graph G(V,E) and a spanning subset of edges E/sub 0//spl sub/E are given. The goal is to augment set E/sub 0/ with a set AUG/spl sub/E-E/sub 0/ of minimal weight, such that graph G(V,E/sub 0//spl cup/AUG) is biconnected. To our knowledge, this is the first time a GA is applied to this problem. First, a straight-forward "pure" GA improved with caching is introduced, which is then hybridized with a greedy, problem dependent heuristic. The proposed approaches are problem instances with up to 1160 feasible edges. While the pure GA performs well, significantly better solutions can be obtained by the hybrid strategy.
The Proposal Auto-Categorizer and Manager for Time Allocation Review at the Space Telescope Science Institute

The Proposal Auto-Categorizer and Manager (PACMan) tool was written to respond to concerns about subjective flaws and potential biases in some aspects of the proposal review process for time allocation for the Hubble Space Telescope (HST), and to partially alleviate some of the anticipated additional workload from the James Webb Space Telescope (JWST) proposal review. PACMan is essentially a mixed-method Naive Bayesian spam filtering routine, with multiple pools representing scientific categories, that utilizes the Robinson method for combining token (or word) probabilities. PACMan was trained to make similar programmatic decisions in science category sorting, panelist selection, and proposal-to-panelists assignments to those made by individuals and committees in the Science Policies Group (SPG) at the Space Telescope Science Institute. Based on training from the previous cycle’s proposals, at an average of 87%, PACMan made the same science category assignments for proposals in Cycle 24 as the SPG. Tests for similar science categorizations, based on training using proposals from additional cycles, show that this accuracy can be further improved, to the level. This tool will be used to augment or replace key functions in the Time Allocation Committee review processes in future HST and JWST cycles.
Low Energy Branes, Effective Theory and Cosmology

The low energy regime of cosmological BPS-brane configurations with a bulk scalar field is studied. We construct a systematic method to obtain five-dimensional solutions to the full system of equations governing the geometry and dynamics of the bulk. This is done for an arbitrary bulk scalar field potential and taking into account the presence of matter on the branes. The method, valid in the low energy regime, is a linear expansion of the system about the static vacuum solution. Additionally, we develop a four-dimensional effective theory describing the evolution of the system. At the lowest order in the expansion, the effective theory is a biscalar tensor theory of gravity. One of the main features of this theory is that the scalar fields can be stabilized naturally without the introduction of additional mechanisms, allowing satisfactory agreement between the model and current observational constraints. The special case of the Randall-Sundrum model is discussed.
On the Convective Coupling and Moisture Organization of East Pacific Easterly Waves

AbstractProcesses associated with the local amplification of easterly waves (EWs) in the east Pacific warm pool are explored. Developing EWs favor convection in the southwest and northeast quadrants of the disturbance. In nascent EWs, convection favors the southwest quadrant. As the EW life cycle progresses, convection in the northeast quadrant becomes increasingly prominent and southwest quadrant convection wanes. The EW moisture budget reveals that anomalous meridional winds acting on the mean meridional moisture gradient of the ITCZ produce moisture anomalies supportive of convection in the southwest quadrant early in the EW life cycle. As EWs mature, moisture anomalies on the poleward side of the EW begin to grow and are supported by the advection of anomalous moisture by the mean zonal wind.In the southwest and northeast portions of the wave, where convection anomalies are favored, lower-tropospheric vorticity is generated locally through vertical stretching that supports a horizontal tilt of the wav.
Launching of hot gas outflow by disc-wide supernova explosions

Galactic gas outflows are driven by stellar feedback with dominant contribution from supernovae (SN) explosions. The question of whether the energy deposited by SNe initiates a large scale outflow or gas circulation on smaller scales -- between discs and intermediate haloes, depends on SN rate and their distribution in space and time. We consider here gas circulation by disc-wide unclustered SNe with galactic star formation rate in the range from {$\simeq 6\times 10^{-4}$ to $\simeq 6\times 10^{-2}~M_\odot$~yr$^{-1}$~kpc$^{-2}$, corresponding to mid-to-high star formation observed in galaxies. We show that such disc-wide SN explosion regime can form circulation of warm ($T\sim 10^4$ K) and cold ($T 10^5$ K)} gas at higher ($z>1$ kpc) heights. We found that the threshold energy input rate for hot gas outflows with disc-wide supernovae explosions is estimated to be of the order $\sim 4\times 10^{-4}$~erg~s$^{-1}$~cm$^{-2}$. We discuss the observational manifestations of such phenomena in optical and X-ray bands. In particular, we found that for face-on galaxies with SF ($\Sigma_{_{\rm SF}}>0.02~M_\odot$~yr$^{-1}$~kpc$^{-2}$), the line profiles of ions typical for warm gas show a double-peak shape, corresponding to out-of-plane outflows. In the X-ray bands, galaxies with high SF rates ($\Sigma_{_{\rm SF}}>0.006~M_\odot$~yr$^{-1}$~kpc$^{-2}$) can be bright, with a smooth surface brightness in low-energy bands ($0.1\hbox{--}0.3$~keV) and patchy at higher energies ($1.6\hbox{--}8.3$~keV). }
The omega dependence in the equations of motion

We show that the equations of motion governing the evolution of a collisionless gravitating system of particles in an expanding universe can be cast in a form which is almost independent of the cosmological density parameter, $\Omega$, and the cosmological constant, $\Lambda$. The new equations are expressed in terms of a time variable $\tau\equiv \ln D$, where $D$ is the linear rate of growth of density fluctuations. The weak dependence on the density parameter is proportional to $\epsilon=\Omega^{-0.2}-1$ times the difference between the peculiar velocity (with respect to $\tau$) of particles and the gravity field. In the general case, the effect of this weak $\Omega$ dependence is to enhance the rate of evolution of density perturbations in dense regions. In a flat universe with $\Lambda\ne 0$, this enhancement is less pronounced than in an open universe with $\Lambda=0$ and the same $\Omega$. Using the spherical collapse model, we find that the increase of the $rms$ density fluctuations in a low $\Omega$ universe relative to that in a flat universe with the same linear normalization is $\sim 0.01 \epsilon(\Omega) $, where $\delta$ is the density field in the flat universe. The equations predict that the smooth average velocity field scales like $\Omega^{0.6}$ while the local velocity dispersion (rms value) scales, approximately, like $\Omega^{0.5}$. High resolution N-body simulations confirm these results and show that density fields, when smoothed on scales slightly larger than clusters, are insensitive to the cosmological model. Halos in an open model simulation are more concentrated than halos of the same $M/\Omega$ in a flat model simulation.
Non-LTE Line Formation for Hydrogen Revisited

We discuss aspects of non-LTE line formation for hydrogen in early-type stars. We evaluate the effect of variations in the electron-impact excitation cross sections in model atoms of differing complexity by comparison with observation. While the Balmer lines are basically unaffected by the choice of atomic data, the Paschen, Brackett, and Pfund series members allow us to discriminate between the different models. Non-LTE calculations based on the widely used approximation formulae of Mihalas, Heasley, & Auer and of Johnson fail to simultaneously reproduce the optical and IR spectra over the entire parameter range. The use of data from ab initio calculations up to principal quantum number n ≤ 7 largely solves the problem. We recommend a reference model using the available data. This model is of general interest because of the ubiquity of the hydrogen spectrum.