Miracle-dz/UniFAR-FTUs huggingface dataset:
HST Grism Observations of a Gravitationally Lensed Redshift 9.5 Galaxy

We present deep spectroscopic observations of a Lyman break galaxy (LBG) candidate (hereafter MACS1149-JD) at z ∼ 9.5 with the Hubble Space Telescope (HST) WFC3/IR grisms. The grism observations were taken at four distinct position angles, totaling 34 orbits with the G141 grism, although only 19 of the orbits are relatively uncontaminated along the trace of MACS1149-JD. We fit a three-parameter (z, F160W mag, and Lyα equivalent width [EW]) LBG template to the three least contaminated grism position angles using a Markov chain Monte Carlo approach. The grism data alone are best fit with a redshift of (68% confidence), in good agreement with our photometric estimate of (68% confidence). Our analysis rules out Lyα emission from MACS1149-JD above a 3σ EW of 21 Å, consistent with a highly neutral IGM. We explore a scenario where the red Spitzer/IRAC [3.6]–[4.5] color of the galaxy previously pointed out in the literature is due to strong rest-frame optical emission lines from a very young stellar population rather than a 4000 Å break. We find that while this can provide an explanation for the observed IRAC color, it requires a lower redshift (z ≲ 9.1), which is less preferred by the HST imaging data. The grism data are consistent with both scenarios, indicating that the red IRAC color can still be explained by a 4000 Å break, characteristic of a relatively evolved stellar population. In this interpretation, the photometry indicates that a Myr stellar population is already present in this galaxy only ∼500 Myr after the big bang.
The role of vowel duration in the perception of /E/ and /æ/

Perceptual studies have consistently shown that the dominant acoustic correlates of vowel perception are the frequencies of the first three formants. The present studies used natural syllables to explore the role of vocalic duration in vowel perception. The first study examined the vocalic duration and frequencies of the first three formants of American‐English vowels. Out of 48 talkers, 15 were identified for whom the formant frequencies were virtually identical in the CVC words ‘‘had’’ and ‘‘head’’ at the vowel mid‐point. These tokens differed in duration and were highly intelligible. The second study used edited natural tokens from 4 of the 15 talkers to investigate the influence of vowel duration in perception. Pitch pulses from ‘‘had’’ were removed to create tokens varying in vowel duration from the natural ‘‘had’’ to a shorter duration similar to ‘‘head. ’’ Pitch pulses from ‘‘head’’ were reduplicated to create a second series for each talker. Duration was used by some listeners for some talkers, but.
Quantifying Light and Ultraviolet Radiation in Plant Biology

Abstract— Fluence rate and irradiance, two parameters used to quantify light and ultraviolet radiation, do not have a constant relation under natural light conditions. A method is described for measuring fluence rate, the preferred parameter, using meters intended for irradiance measurements. Values measured under natural light conditions are compared to a daylight model.
Shear flow in the presence of 'strong rotation'. II. Approximations for continuum-plus-rarefied flow

For pt.I see ibid., vol.16, p.1201 (1983). Plane Couette flow of a gas in a strong pseudo-centrifugal force field is studied, for conditions relevant to gas-centrifuge applications. In these conditions the gas is a continuum near boundaries, but free-molecular in much of its remaining volume. Approximate solutions are obtained for moderate and strong forces. As the force strength increases, the flow shows an increasingly large qualitative difference from the pattern predicted by hydrodynamics. For strong forces, the flow is shown to become approximately that of a free-molecular gas.
Optimising Compressed Natural Gas filling stations reservoir pressure based on thermodynamic analysis

A theoretical analysis has been developed to study the effects various parameters on the Compressed Natural Gas (CNG) filling process and the conditions. The analysis is based on first and second laws of thermodynamics, conservation of mass and the AGA8 Equation of State (EOS). Based on AGA8 EOS and thermodynamics relationships, the required properties of natural gas mixtures have been calculated. It is found that, the compositions of natural gas have big effects on the CNG filling process and final in–cylinder values. For various Iranian natural gas compositions, the optimised filling stations' reservoirs pressure has been found.
The Circumgalactic Medium

The gas surrounding galaxies outside their disks or interstellar medium and inside their virial radii is known as the circumgalactic medium (CGM). In recent years this component of galaxies has assumed an important role in our understanding of galaxy evolution owing to rapid advances in observational access to this diffuse, nearly invisible material. Observations and simulations of this component of galaxies suggest that it is a multiphase medium characterized by rich dynamics and complex ionization states. The CGM is a source for a galaxy's star-forming fuel, the venue for galactic feedback and recycling, and perhaps the key regulator of the galactic gas supply. We review our evolving knowledge of the CGM with emphasis on its mass, dynamical state, and coevolution with galaxies. Observations from all redshifts and from across the electromagnetic spectrum indicate that CGM gas has a key role in galaxy evolution. We summarize the state of this field and pose unanswered questions for future research.
Optical investigation of electrical spin injection into semiconductors

We investigate the electrical injection of spin-polarized electrons into a semiconductor [Al(GaAs)] heterostructure from ferromagnetic FeCo metal through an AlO x tunnel barrier. We have developed the optical oblique Hanle effect approach for the quantitative analysis of electrical spin injection into semiconductors. This technique is based on the manipulation of the electron spins within a semiconductor when spin polarized electrons have been injected. This allows us to clearly separate the effects caused by spin injection from others, that are magneto-optical, Zeeman, etc. Simultaneously, the oblique Hanle effect approach provides additional information on the spin dynamics in the semiconductor. In the FeCo/AlO x /Al(GaAs) heterostructures we observe spin injection of 21% and 16% at 80 and 300 K, respectively. The importance of electron thermalization effects and the impact of the doping level of the semiconductor for practical investigation of spin injection by optical means are demonstrated.
Analysis the Relationship between Pavement Smoothness Indices

Although the inertial profiler has been introduced for decades, most of the highway agencies in Taiwan still adopt the 3-M straightedge as the main device for pavement roughness measurements. Through the Long Term Pavement Performance database, 5280 profile data were selected in this study for analyzing the relationship between international roughness index (IRI) and standard deviator (σ). The natural logarithm transformation was applied to both variables before a linear regression model was developed with R 2 of 0.9368. However, it is found that the current smoothness acceptance specification (σ= 2.4 mm) used by Taiwan Freeway and Expressway system is equivalent to an IRI value of 2.97 m/km that is not rigorous enough while compared with that of other countries. It is recommended to modify the specification from 2.4mm to 1.1 mm that will perform an equivalent level of the IRI-based specification suggested by Federal Highway Administration.
Optical Studies of V4332 Sagittarii: Detection of Unusually Strong K I and Na I Lines in Emission

We present optical observations of the enigmatic nova-like variable V4332 Sgr. The importance of this object should not be understated since it is considered to be the possible prototype of a new class of eruptive variables. These objects have been the subject of considerable studies at present primarily because of the spectacular eruption of V838 Mon—another member of this class—recently in 2002. The cause of the outburst in such objects is not well understood. Our recent work has shown striking changes in the near-IR spectrum of V4332 Sgr since its 1994 outburst. The optical spectrum presented here confirms that V4332 Sgr is indeed an unusual and extremely interesting object. This spectrum, the first to be taken after a hiatus of nearly 10 years after the outburst, shows several lines in emission but is dominated by exceptionally strong emission in the resonance doublet of K I at 7665 and 7699 Å and to a slightly lesser strength in the unresolved Na I doublet at 5890 and 5896 Å. The K I lines are shown to be optically thick and considerably broadened. We investigate the site of origin of the K I and Na I emission. Considering the strength of the alkali metal lines—seen at similar strength only in L- and T-type dwarfs (although in absorption)—we discuss whether the outburst of V4332 Sgr was an explosion on an L- or T-type dwarf. However, BVRI photometry does not support such a scenario but rather shows the central object of V4332 Sgr to be an M-type star with a temperature of 3250 K.
A Reply to Churchland's "Perceptual Plasticity and Theoretical Neutrality"

Churchland's paper "Perceptual Plasticity and Theoretical Neutrality" offers empirical, semantical and epistemological arguments intended to show that the cognitive impenetrability of perception "does not establish a theory-neutral foundation for knowledge" and that the psychological account of perceptual encapsulation that I set forth in The Modularity of Mind "[is] almost certainly false". The present paper considers these arguments in detail and dismisses them.
An XMM-Newton Study of the Coronae of σ2 Coronae Borealis

We present results of XMM-Newton Guaranteed Time observations of the RS CVn binary σ2 Coronae Borealis. The spectra obtained with the Reflection Grating Spectrometers and the European Photon Imaging Camera MOS2 were simultaneously fitted with collisional ionization equilibrium plasma models to determine coronal abundances of various elements. Contrary to the solar first ionization potential (FIP) effect, in which elements with a low FIP are overabundant in the corona compared to the solar photosphere, and contrary to the "inverse" FIP effect observed in several active RS CVn binaries, coronal abundance ratios in σ2 CrB show a complex pattern, as supported by similar findings in the Chandra HETGS analysis of σ2 CrB with a different methodology by Osten and coworkers in 2003. Low-FIP elements (<10 eV) have abundance ratios relative to Fe that are consistent with the solar photospheric ratios, whereas high-FIP elements have abundance ratios that increase with increasing FIP. We find that the coronal Fe abundance is consistent with the stellar photospheric value, indicating that there is no metal depletion in σ2 CrB. However, we obtain a higher Fe absolute abundance than Osten and coworkers did. Except for Ar and S, our absolute abundances are about 1.5 times larger than those reported by Osten and coworkers. However, a comparison of their model with our XMM-Newton data (and vice versa) shows that both models work adequately in general. We find, therefore, no preference for one methodology over the other for deriving coronal abundances. Despite the systematic discrepancy in absolute abundances, our abundance ratios are very close to those obtained by Osten and coworkers. Finally, we confirm the measurement of a low density in O VII (<4 × 1010 cm-3) but could not confirm the higher densities measured in spectral lines formed at higher temperatures that were derived by other studies of σ2 CrB due to the lower spectral resolution of the XMM-Newton grating spectrometers.
Thermal effects in partially saturated soils: a constitutive model

The present paper is centred on the assessment of an elastic–plastic model for partially saturated soils, earlier proposed by the authors, for its predictive capability with respect to temperature changes, on the light of available experimental results. The model is cast within a constitutive framework that uses Bishop's stress and suction as main variables governing the volumetric response of the material. Some enhancement to the original temperature‐independent formulation is proposed. In particular, functions describing the yield surface and the compressibility modulus are modified to account for the shrinking of the elastic domain and for the increase of irreversible volumetric strain with heating. Some examples illustrate the main features of the present proposal. Comparison with some experimental results is also included. Copyright © 2005 John Wiley & Sons, Ltd.
Heating of an Erupting Prominence Associated with a Solar Coronal Mass Ejection on 2012 January 27

We investigate the heating of an erupting prominence and loops associated with a coronal mass ejection and X-class flare. The prominence is seen as absorption in EUV at the beginning of its eruption. Later, the prominence changes to emission, which indicates heating of the erupting plasma. We find the densities of the erupting prominence using the absorption properties of hydrogen and helium in different passbands. We estimate the temperatures and densities of the erupting prominence and loops seen as emission features using the differential emission measure method, which uses both EUV and X-ray observations from the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory and the X-ray Telescope on board Hinode. We consider synthetic spectra using both photospheric and coronal abundances in these calculations. We verify the methods for the estimation of temperatures and densities for the erupting plasmas. Then, we estimate the thermal, kinetic, radiative loss, thermal conduction, and heating energies of the erupting prominence and loops. We find that the heating of the erupting prominence and loop occurs strongly at early times in the eruption. This event shows a writhing motion of the erupting prominence, which may indicate a hot flux rope heated by thermal energy release during magnetic reconnection.
Quasiparticle density of states ofBi2Sr2CaCu2O8+δsingle crystals probed using tunneling spectroscopy in the30–50mKtemperature range in high magnetic fields

Break-junction tunneling spectroscopy at temperatures 30-50 mK in high magnetic field is used to directly probe the quasiparticle density of states within the energy gap in a single crystal Bi2212 high-$T_c$ superconductor. The measured tunneling conductances $dI/dV(V)$ in the subgap region have a zero flat region with no evidence for a linear increase of the density of states with voltage. A number of tunnel break-junctions exhibited $dI/dV(V)$ curves with a second energy gap structure at the average magnitude 2$\Delta _{p-p}/e=13$ mV. Our data cannot be explained by either a pure $s$ pairing or a pure $d_{x^2-y^2}$ pairing.
Lossless Tapers, Gaussian Beams, Free-Space Modes: Standing Waves Versus Through-Flowing Waves

It was noticed in the past that, to avoid physical inconsistencies, in Marcatili’s lossless tapers through-ﬂowing waves must be drastically diﬀerent from standing waves. First, we reconﬁrm this by means of numerical results based on an extended BPM algorithm. Next, we show that this apparently surprising behavior is a straightforward fallout of Maxwell’s equations. Very similar remarks apply to Gaussian beams in a homogeneous medium. As a consequence, Gaussian beams are shown to carry reactive powers, and their active power distributions depart slightly from their standard pictures. Similar conclusions hold for free-space modes expressed in terms of Bessel functions.
Weighing neutrinos in the scenario of vacuum energy interacting with cold dark matter: application of the parameterized post-Friedmann approach

We constrain the neutrino mass in the scenario of vacuum energy interacting with cold dark matter by using current cosmological observations. To avoid the large-scale instability problem in interacting dark energy models, we employ the parameterized post-Friedmann (PPF) approach to do the calculation of perturbation evolution, for the Q = βHρc and Q = βHρΛ models. The current observational data sets used in this work include Planck (cosmic microwave background), BSH (baryon acoustic oscillations, type Ia supernovae, and Hubble constant), and LSS (redshift space distortions and weak lensing). According to the constraint results, we find that β > 0 at more than 1σ level for the Q = βHρc model, which indicates that cold dark matter decays into vacuum energy; while β = 0 is consistent with the current data at 1σ level for the Q = βHρΛ model. Taking the ΛCDM model as a baseline model, we find that a smaller upper limit, ∑mν < 0.11 eV (2σ), is induced by the latest BAO BOSS DR12 data and the Hubble constant measurement H0 = 73.00 ± 1.75 km s−1 Mpc−1. For the Q = βHρc model, we obtain ∑mν<0.20 eV (2σ) from Planck+BSH. For the Q = βHρΛ model, ∑mν<0.10 eV (2σ) and ∑mν<0.14 eV (2σ) are derived from Planck+BSH and Planck+BSH+LSS, respectively. We show that these smaller upper limits on ∑mν are affected more or less by the tension between H0 and other observational data.
Low‐frequency ac conduction in lightly doped polypyrrole films

The total measured ac conductivity σ(ω)m of lightly doped polypyrrole films has been measured in the frequency range 100 Hz–10 MHz and in the temperature range 77–350 K. In the low‐temperature region the measured ac conductivity is almost independent of temperature but shows a strong dependence on frequency and can be described by a relation σ(ω) = Aωs where the exponent s has been observed to be less than unity. In the high‐temperature region the frequency dependence becomes weak at low frequencies but remains strongly frequency dependent at high frequencies. The weak frequency dependence is due to the contribution of dc conductivity to the measured ac conductivity. A clear Debye‐type loss peak is observed by substracting the contribution of dc conductivity. The frequency dependence of conductivity remains less than quadratic at low frequencies indicating thereby some distribution of relaxation times. This is confirmed by the measurement of dielectric constant as a function of frequency and temperature.
Observations of the 6 cm Lines of OH in Evolved (OH/IR) Stars

Recent observational and theoretical advances have called into question traditional OH maser pumping models in evolved (OH/IR) stars. The detection of excited-state OH lines would provide additional constraints to discriminate among these theoretical models. In this Letter, we report on VLA observations of the 4750 and 4765 MHz lines of OH toward 45 sources, mostly evolved stars. We detect 4765 MHz emission in the star-forming regions Mon R2 and LDN 1084, but we do not detect excited-state emission in any evolved stars. The flux density and velocity of the 4765 MHz detection in Mon R2 suggest that a new flaring event has begun.
The Discus Comet: C/2014 B1 (Schwartz)

Long-period comet C/2014 B1 (Schwartz) exhibits a remarkable optical appearance, like that of a discus or bi-convex lens viewed edgewise. Our measurements in the four years since discovery reveal a unique elongated dust coma whose orientation is stable with respect to the projected antisolar and orbital directions. With no tail and no trail, the limited influence of radiation pressure on the dust coma sets a lower limit to the effective particle size ≳100 μm, while the photometry reveals a peak coma scattering cross-section 2.7 × 104 km2 (geometric albedo 0.1 assumed). From the rate of brightening of the comet we infer a dust production rate ≳10 kg s−1 at 10 au heliocentric distance, presumably due to the sublimation of supervolatile ices, and perhaps triggered by the crystallization of amorphous water ice. We consider several models for the origin of the peculiar morphology. The disk-like shape is best explained by equatorial ejection of particles from a nucleus whose spin vector lies near the plane of the sky. In this interpretation, the unique appearance of C/2014 B1 is a result of a near equality between the rotation-assisted nucleus escape speed (∼1–10 m s−1 for a 2–20 km scale nucleus) and the particle ejection velocity, combined with a near-equatorial viewing perspective. To date, most other comets have been studied at heliocentric distances less than half that of C/2014 B1, where their nucleus temperatures, gas fluxes, and dust ejection speeds are much higher. The throttling role of nucleus gravity is correspondingly diminished, so that the disk morphology has not before been observed.
Measurement of the solar neutrino capture rate with gallium metal

The solar neutrino capture rate measured by the Russian-American Gallium Experiment (SAGE) on metallic gallium during the period January 1990 through December 1997 is 67 . 2 +7 . 2+3 . 5 − 7 . 0 − 3 . 0 SNU, where the uncertainties are statistical and systematic, respectively. This represents only about half of the predicted standard solar model rate of 129 SNU. All the experimental procedures, including extraction of germanium from gallium, counting of 71 Ge, and data analysis, are discussed in detail.
Impact of young stellar components on quiescent galaxies: deconstructing cosmic chronometers

Context. Cosmic chronometers may be used to measure the age difference between passively evolving galaxy populations to calculate the Hubble parameter H(z) as a function of redshift z. The age estimator emerges from the relationship between the amplitude of the rest frame Balmer break at 4000 Å and the age of a galaxy, assuming that there is one single stellar population within each galaxy. Aims. First, we analyze the effect on the age estimates from the possible contamination (< 2.4% of the stellar mass in our high-redshift sample) of a young component of ≲ 100 Myr embedded within the predominantly old population of the quiescent galaxy. Recent literature has shown this combination to be present in very massive passively evolving galaxies. Second, we evaluate how the available data compare with the predictions of nine different cosmological models. Methods. For the first task, we calculated the average flux contamination due to a young component in the Balmer break from the data of 20 galaxies at z > 2 that included photometry from the far-ultraviolet to near-infrared at rest. For the second task, we compared the data with the predictions of each model, using a new approach of distinguishing between systematic and statistical errors. In previous work with cosmic chronometers, these have simply been added in quadrature. We also evaluated the effects of contamination by a young stellar component. Results. The ages inferred using cosmic chronometers represent a galaxy-wide average rather than a characteristic of the oldest population alone. The average contribution from the young component to the rest luminosity at 4000 Å may constitute a third of the luminosity in some samples, which means that this is far from negligible. This ratio is significantly dependent on stellar mass, proportional to M−07. Consequently, the measurements of the absolute value of the age or the differential age between different redshifts are at least partially incorrect and make the calculation of H(z) very inaccurate. Some cosmological models, such as the Einstein-de Sitter model or quasi-steady state cosmology, which are rejected under the assumption of a purely old population, can be made compatible with the predicted ages of the Universe as a function of redshift if we take this contamination into account. However, the static Universe models are rejected by these H(z) measurements, even when this contamination is taken into account.