Miracle-dz/UniFAR-FTUs huggingface dataset:
Bubble noise and wavelet spills recorded 1 m below the ocean surface

A remote instrument has been used to record the sound and environment of small surface spills in light winds from a depth of approximately 1 m in the open ocean. Recordings from the instrument indicate that these small breaks have no correlation with the amplitude or phase of long-period swells moving faster than prevailing winds. The sound from the spills, which is composed of a number of distinct resonant bubble oscillations, is very similar to that described by Medwin and Beaky [J. Acoust. Soc. Am. 86, 1124–1130 (1989)] for windless artificial wave breaks. Peak oscillation source pressures range up to 1.2 Pa. The average of several acoustic spectra from a single energetic spill has shown a slope of −5 dB per octave over the frequency range of the instrument, roughly 500–8000 Hz. The unique frequency for each oscillating bubble within a spill indicates that bubbles are “rung” as they are formed during entrainment, die out exponentially within milliseconds, and then no longer contribute actively to the a.
Kinematics of the Optically Visible YSOs toward the Orion B Molecular Cloud

We present results from high-resolution optical spectra toward 66 young stars in the Orion B molecular cloud to study their kinematics and other properties. Observations of the Hα and Li i 6707 Å lines are used to check membership and accretion properties. While the stellar radial velocities of NGC 2068 and L1622 are in good agreement with that of the molecular gas, many of the stars in NGC 2024 show a considerable offset. This could be a signature of either the expansion of the cluster, the high degree of the ejection of the stars from the cluster through dynamical interaction, or the acceleration of the gas due to stellar feedback.
Connecting the progenitors, pre-explosion variability and giant outbursts of luminous blue variables with Gaia16cfr

The work of AVF was conducted in part at the Aspen Center for Physics, which is supported by NSF grant PHY-1607611; the author thanks the Center for its hospitality during the neutron stars workshop in 2017 June and July. AVF is grateful for financial assistance from the TABASGO Foundation, the Christopher R. Redlich Fund, the Miller Institute for Basic Research in Science (U.C. Berkeley) and HST grants GO-13646 and AR-14295 from the Space Telescope Science Institute (STScI), which is operated by AURA under NASA contract NAS 5-26555.
Synthetic aperture radar compact polarimetry for sea ice surveillance

The focus of this thesis is to investigate the use of synthetic aperture radar (sar) compact polarimetry for studies of sea ice. Data obtained from quad-polarimetric sar systems have already been studied extensively for sea ice monitoring. This thesis focuses on finding parallels to quad-polarimetric features from the compact-polarimetric data. This is achieved through the reconstruction of a pseudo quad-polarimetric sample covariance matrix. The main contribution of this thesis is the suggestion of new reconstruction techniques for sea ice covered sar scenes. Most of the estimated polarimetric features relevant to sea ice monitoring are successfully reconstructed. Furthermore, a comparison between the different reconstruction techniques is presented for different sea ice types. It is shown that the cross-polarization intensity can be reconstructed for different sea ice types, but that the performance is strongly affected by the choice of reconstruction method. The proposed modified Souyris’ reconstruction technique turns out to be the best method for achieving high performance for different polarimetric features representing different sea ice types. Additionally, three other methods are suggested, namely a model-based, an eigenvalue-based, and a DoP-based reconstruction method. Each of these methods produce a higher accuracy than the existing reconstruction methods for most of the polarimetric features. Remote sensing instruments have been extensively used as a tool for sea ice monitoring. Information about sea ice is important for multiple industries like oil and gas, fishing, research communities, and tourism. Fulland dual polarimetric sar instruments have been used to extract useful information about the sea ice surface, but now a new polarimetric mode has been invented. In its infancy, the theoretical foundation of compact polarimetry was presented by Souyris, Nord, and later Raney with the hybridpol mode. However, compact polarimetry—especially the hybrid-pol mode—has proved valuable, and has in later years found its way into operational satellite systems such as the risat and the alos-2 satellites. The work presented in this thesis adds to the on-going discussion on the potential of compact polarimetry, and is the first comprehensive analysis of reconstruction methods for specified application to sea ice.
Assessing Populations of Painted Turtles ( Chrysemys picta ) in Ponds at Black Rock Forest, NY

: Painted turtles ( Chrysemys picta ) are the most widespread turtles in North America and are one of the most studied species of turtles in the world. The ponds of Black Rock Forest (BRF) are the home to several species of turtles, among these is the painted turtle. However, there have been no recent studies on painted turtle populations at BRF. This study examined the population of painted turtles in three of Black Rock Forests' ponds: Upper Reservoir, Aleck Meadow Pond and Sutherland Pond. Turtles were trapped, marked and recaptured for two consecutive summers and the population size, sex ratio, and age structure were determined. Analyses showed that the population for all three ponds has not changed significantly over the years but a slight increasing trend is apparent. In addition, in all three ponds the sex ratio is close to 1:1 and there are significantly more adults than juveniles, as is expected in a painted turtle population. These findings indicate that the populations appear to be healthy. The data collected, as well as the results found will help in future studies and in the management of painted turtle populations in the ponds at BRF.
FLUORINE IN THE SOLAR NEIGHBORHOOD: NO EVIDENCE FOR THE NEUTRINO PROCESS

Asymptotic giant branch (AGB) stars are known to produce “cosmic” fluorine, but it is uncertain whether these stars are the main producers of fluorine in the solar neighborhood or if any of the other proposed formation sites, Type II supernovae (SNe II) and/or Wolf-Rayet (W-R) stars, are more important. Recent articles have proposed both AGB stars and SNe II as the dominant sources of fluorine in the solar neighborhood. In this paper we set out to determine the fluorine abundance in a sample of 49 nearby, bright K giants for which we previously have determined the stellar parameters, as well as alpha abundances homogeneously from optical high-resolution spectra. The fluorine abundance is determined from a 2.3 μm HF molecular line observed with the spectrometer Phoenix. We compare the fluorine abundances with those of alpha-elements mainly produced in SNe II and find that fluorine and the alpha-elements do not evolve in lockstep, ruling out SNe II as the dominating producers of fluorine in the solar neighborhood. Furthermore, we find a secondary behavior of fluorine with respect to oxygen, which is another evidence against the SNe II playing a large role in the production of fluorine in the solar neighborhood. This secondary behavior of fluorine will put new constraints on stellar models of the other two suggested production sites: AGB stars and W-R stars.
Effect of Hall Current on Hydromagnetic Free Convection Flow near an Accelerated Porous Plate

The effect of free convection current on the unsteady flow of MHD viscous and incompressible fluid past a uniformly accelerated vertical porous plate imbedded in a uniform applied magnetic field transverse to it is investigated, on the assumption that the induced magnetic field is negligible compared with the imposed magnetic field. The series solution for the velocity and the skin friction are obtained under the assumption that the hydromagnetic parameter Mt is small. The velocity profiles are shown graphically with the effect of the Hall parameter m, the magnetic field parameter Mt, the Grashof number Gr and the transpiration parameter a for a single value of the Prandtl number Pr=0.71 which represents air at 20°C. The numerical values of the skin friction components are given in tabular form for different values of these parameters.
Signal distortion on VHF/UHF transionospheric paths: First results from the Wideband Ionospheric Distortion Experiment

To the best of our knowledge, we report the first determination of ionospheric distortion, comprising the simultaneous characterization of both multipath and Doppler, on wideband, transionospheric VHF (158 MHz) and UHF (422 MHz) signals. The measurements took place as part of the test phase of the United Kingdom–United States Wideband Ionospheric Distortion Experiment during the evening (∼1000 UT) of 18 January 2005. This characterization has been achieved using the ALTAIR radar at the Ronald Reagan Ballistic Missile Defense Test Site on Kwajalein Atoll (9.395°N, 167.469°E (12.87°N, 237.16°E corrected geomagnetic)) in the Pacific, in conjunction with a low Earth orbiting, constant radar cross‐section, passive satellite (calibration sphere). During the period when the two‐way S4 index was above ∼0.8 on both channels, the median coherency times were 43 and 96 ms at VHF and UHF, respectively (at 1.5σ). The corresponding median coherency bandwidths were 0.8 and 2.1 MHz.
MMS Observations of Beta-dependent Constraints on Ion Temperature Anisotropy in Earth’s Magnetosheath

Protons (ionized hydrogen) in the solar wind frequently exhibit distinct temperatures (T⊥p and T∥p) perpendicular and parallel to the plasma’s background magnetic field. Numerous prior studies of the interplanetary solar wind have shown that, as proton beta (β∥p) increases, a narrower range of proton temperature anisotropy (Rp ≡ T⊥p/T∥p) values is observed. Conventionally, this effect has been ascribed to the actions of kinetic microinstabilities. This study is the first to use data from the Magnetospheric Multiscale Mission to explore such β∥p-dependent limits on Rp in Earth’s magnetosheath. The distribution of these data across the (β∥p, Rp)-plane reveals limits on both Rp > 1 and Rp < 1. Linear Vlasov theory is used to compute contours of constant growth rate for the ion–cyclotron, mirror, parallel-firehose, and oblique-firehose instabilities. These instability thresholds closely align with the contours of the data distribution, which is consistent with these instabilities acting to limit extremes of proton temperature anisotropy in the magnetosheath.
Evolution of the Gas Mass Fraction of Progenitors to Today’s Massive Galaxies: ALMA Observations in the CANDELS GOODS-S Field

We present an Atacama Large Millimeter/submillimeter Array (ALMA) survey of dust continuum emission in a sample of 70 galaxies in the redshift range z = 2–5 selected from the CANDELS GOODS-S field. Multi-epoch abundance matching (MEAM) is used to define potential progenitors of a z = 0 galaxy of stellar mass 1.5 × 1011 M⊙. Gas masses are derived from the 850 μm luminosity. Ancillary data from the CANDELS GOODS-S survey are used to derive the gas mass fractions. The results at z ≲ 3 are mostly in accord with expectations: The detection rates are 75% for the z = 2 redshift bin, 50% for the z = 3 bin, and 0% for z ≳ 4. The average gas mass fraction for the detected z = 2 galaxies is fgas = 0.55 ± 0.12 and fgas = 0.62 ± 0.15 for the z = 3 sample. This agrees with expectations for galaxies on the star-forming main sequence, and shows that gas fractions have decreased at a roughly constant rate from z = 3 to z = 0. Stacked images of the galaxies not detected with ALMA give upper limits to fgas of <0.08 and <0.15, for the z = 2 and z = 3 redshift bins. None of our galaxies in the z = 4 and z = 5 sample are detected, and the upper limit from stacked images, corrected for low metallicity, is fgas < 0.66. We do not think that lower gas-phase metallicities can entirely explain the lower dust luminosities. We briefly consider the possibility of accretion of very low-metallicity gas to explain the absence of detectable dust emission in our galaxies at z ≳ 4.
Gamma-ray line measurements from supernova explosions

Abstract Gamma ray lines are expected to be emitted as part of the afterglow of supernova explosions, because radioactive decay of freshly synthesised nuclei occurs. Significant radioactive gamma ray line emission is expected from 56Ni and 44Ti decay on time scales of the initial explosion (56Ni, τ ~days) and the young supernova remnant (44Ti,τ ~90 years). Less specific, and rather informative for the supernova population as a whole, are lessons from longer lived isotopes such as 26Al and 60Fe. From isotopes of elements heavier than iron group elements, any interesting gamma-ray line emission is too faint to be observable. Measurements with space-based gamma-ray telescopes have obtained interesting gamma ray line emissions from two core collapse events, Cas A and SN1987A, and one thermonuclear event, SN2014J. We discuss INTEGRAL data from all above isotopes, including all line and continuum signatures from these two objects, and the surveys for more supernovae, that have been performed by gamma ray spectrometry. Our objective here is to illustrate what can be learned from gamma-ray line emission properties about the explosions and their astrophysics.
Rational Use of CT-Scan for the Diagnosis of Pneumonia: Comparative Accuracy of Different Strategies

Diagnosing pneumonia in emergency departments is challenging because the accuracy of symptoms, signs and laboratory tests is limited. As a confirmation test, chest X-ray has significant limitations and is outperformed by CT-scan. However, obtaining a CT-scan in all cases of suspected pneumonia has significant drawbacks. We used a cohort of 200 consecutive elderly patients admitted to the hospital for suspected pneumonia to build a simple prediction score, which was used to determine indication for performing a CT-scan. The reference diagnosis was adjudicated by experts considering all available data, including evolution until discharge and CT scan in all patients. Results were externally validated in a second cohort of 319 patients. Pneumonia was confirmed in 133 patients (67%). Area under the receiver operator curve (AUROC) of physician evaluation was 0.55 (0.46–0.64). The score incorporated four variables independently predicting confirmed pneumonia: male gender, acute cough, C-reactive protein >70 mg/L, and urea <7 mmol/L. AUROC of the score was 0.68 (95% confidence interval (CI) 0.60–0.76). When a CT-scan was obtained for patients at low or intermediate predicted risk (108 patients, 54% of the cohort), AUROC was 0.71 (0.63–0.80) and 0.69 (0.64–0.74) in the derivation and validation cohort, respectively. A simple prediction score for pneumonia had moderate accuracy and could guide the performance of a CT-scan.
The central spheroids of Milky Way mass-sized galaxies

We study the properties of the central spheroids located within 10 kpc of the centre of mass of Milky Way mass-sized galaxies simulated in a cosmological context. The simulated central regions are dominated by stars older than 10 Gyr, mostly formed in situ, with a contribution of ~30 per cent from accreted stars. These stars formed in well-defined starbursts, although accreted stars exhibit sharper and earlier ones. The fraction of accreted stars increases with galactocentric distance, so that at a radius of ~8-10 kpc a fraction of ~40 per cent, on average, are detected. Accreted stars are slightly younger, lower metallicity, and more $\alpha$-enhanced than in situ stars. A significant fraction of old stars in the central regions come from a few ($2-3$) massive satellites ($\sim 10^{10}{\rm M}_\odot$). The bulge components receive larger contributions of accreted stars formed in dwarfs smaller than $\sim 10^{9.5}{\rm M}_\odot$. The difference between the distributions of ages and metallicities of old stars is thus linked to the accretion histories -- those central regions with a larger fraction of accreted stars are those with contributions from more massive satellites. The kinematical properties of in situ and accreted stars are consistent with the latter being supported by their velocity dispersions, while the former exhibit clear signatures of rotational support. Our simulations demonstrate a range of characteristics, with some systems exhibiting a co-existing bar and spheroid in their central regions, resembling in some respect the central region of the Milky Way.
Structure and decays of nuclear three-body systems: The Gamow coupled-channel method in Jacobi coordinates

${\bf Background:}$ Weakly bound and unbound nuclear states appearing around particle thresholds are prototypical open quantum systems. Theories of such states must take into account configuration mixing effects in the presence of strong coupling to the particle continuum space. ${\bf Purpose:}$ To describe structure and decays of three-body systems, we developed a Gamow coupled-channel (GCC) approach in Jacobi coordinates by employing the complex-momentum formalism. We benchmarked the new framework against the complex-energy Gamow Shell Model (GSM). ${\bf Methods:}$ The GCC formalism is expressed in Jacobi coordinates, so that the center-of-mass motion is automatically eliminated. To solve the coupled-channel equations, we use hyperspherical harmonics to describe the angular wave functions while the radial wave functions are expanded in the Berggren ensemble, which includes bound, scattering and Gamow states. ${\bf Results:}$ We show that the GCC method is both accurate and robust. Its results for energies, decay widths, and nucleon-nucleon angular correlations are in good agreement with the GSM results. ${\bf Conclusions:}$ We have demonstrated that a three-body GSM formalism explicitly constructed in cluster-orbital shell model coordinates provides similar results to a GCC framework expressed in Jacobi coordinates, provided that a large configuration space is employed. Our calculations for $A=6$ systems and $^{26}$O show that nucleon-nucleon angular correlations are sensitive to the valence-neutron interaction. The new GCC technique has many attractive features when applied to bound and unbound states of three-body systems: it is precise, efficient, and can be extended by introducing a microscopic model of the core.
PSR J0636+5128: A Heated Companion in a Tight Orbit

We present an analysis of archival Gemini g′, r′, K and Keck H, Ks imaging of this nearby short-period binary (PB = 95.8 minutes) 2.87 ms pulsar. The heated companion is clearly detected. Direct pulsar heating provides an acceptable model at the revised >700 pc parallax distance. The relatively shallow light curve modulation prefers an inclination i < 40°; this high-latitude view provides a likely explanation for the lack of radio signatures of wind dispersion or eclipse. It also explains the low minimum companion mass and, possibly, the faintness of the source in X-rays and γ-rays.
A dearth of short-period massive binaries in the young massive star forming region M 17 - Evidence for a large orbital separation at birth?

Aims. The formation of massive stars remains poorly understood and little is known about their birth multiplicity properties. Here, we aim to quantitatively investigate the strikingly low radial-velocity dispersion measured for a sample of 11 massive pre- and near-main-sequence stars (σ1D= 5.6 ± 0.2 km s-1) in the very young massive star forming region M 17, in order to obtain first constraints on the multiplicity properties of young massive stellar objects. Methods. We compute the radial-velocity dispersion of synthetic populations of massive stars for various multiplicity properties and we compare the obtained σ1D distributions to the observed value. We specifically investigate two scenarios: a low binary fraction and a dearth of short-period binary systems. Results. Simulated populations with low binary fractions (fbin = 0.12-0.09+0.16) or with truncated period distributions (Pcutoff > 9 months) are able to reproduce the low σ1D observed within their 68%-confidence intervals. Furthermore, parent populations with fbin > 0.42 or Pcutoff < 47 d can be rejected at the 5%-significance level. Both constraints are in stark contrast with the high binary fraction and plethora of short-period systems in few Myr-old, well characterized OB-type populations. To explain the difference in the context of the first scenario would require a variation of the outcome of the massive star formation process. In the context of the second scenario, compact binaries must form later on, and the cut-off period may be related to physical length-scales representative of the bloated pre-main-sequence stellar radii or of their accretion disks. Conclusions. If the obtained constraints for the M 17’s massive-star population are representative of the multiplicity properties of massive young stellar objects, our results may provide support to a massive star formation process in which binaries are initially formed at larger separations, then harden or migrate to produce the typical (untruncated) power-law period distribution observed in few Myr-old OB binaries.
KINEMATICS OF EXTREMELY METAL-POOR GALAXIES: EVIDENCE FOR STELLAR FEEDBACK

The extremely metal-poor (XMP) galaxies analyzed in a previous paper have large star-forming regions with a metallicity lower than the rest of the galaxy. Such a chemical inhomogeneity reveals the external origin of the metal-poor gas fueling star formation, possibly indicating accretion from the cosmic web. This paper studies the kinematic properties of the ionized gas in these galaxies. Most XMPs have a rotation velocity around a few tens of km s−1. The star-forming regions appear to move coherently. The velocity is constant within each region, and the velocity dispersion sometimes increases within the star-forming clump toward the galaxy midpoint, suggesting inspiral motion toward the galaxy center. Other regions present a local maximum in velocity dispersion at their center, suggesting a moderate global expansion. The Hα line wings show a number of faint emission features with amplitudes around a few per cent of the main Hα component, and wavelength shifts between 100 and 400 km s−1. The components are often paired, so that red and blue emission features with similar amplitudes and shifts appear simultaneously. Assuming the faint emission to be produced by expanding shell-like structures, the inferred mass loading factor (mass loss rate divided by star formation rate) exceeds 10. Since the expansion velocity far exceeds the rotational and turbulent velocities, the gas may eventually escape from the galaxy disk. The observed motions involve energies consistent with the kinetic energy released by individual core-collapse supernovae. Alternative explanations for the faint emission have been considered and discarded.