Miracle-dz/UniFAR-FTUs huggingface dataset:
UvA-DARE (Digital Academic Does employee perceived person-organization fit promote performance? The moderating role of supervisor perceived person-organization fit

Prior research has shown inconsistent and mostly nonsignificant relationships between employee person-organization (P-O) fit and in-role performance. In this study, we examine whether the strength of the relationship between employee perceived P-O fit and supervisor-rated performance depends on the perceived P-O fit of the supervisor. We propose that (a) in-role task-related processes are facilitated when both supervisor and employee share a common frame of understanding about what is important for the organization and (b) that high P-O fit supervisors attach value to the work behaviours of high P-O fit employees, both of which should translate into more positive performance evaluations. The results of a field study among 155 employees and their supervisors provided support for this proposition: employees ’ perceived P-O fit was positively associated with their performance evaluation when supervisor perceived P-O fit was high, whereas this association was absent when supervisor perceived P-O fit was low. Our study contributes to the P-O fit literature by unpacking whether and when employee perceived P-O fit is important for functioning and performance evaluations.
What’s Interrupting Your Search? A Diary Study of Everyday Mobile Search Interruptions

Introduction. Web search is a common activity in a mobile context. However, the nature of performing tasks in a mobile environment means there is the risk interruption. While the effects of interruptions on mobile search have been studied in recent years, the nature of such interruptions occurring in real-world mobile settings have not. Methods. Using a diary study approach, we collected data from 20 participants on the everyday interruptions they faced conducting mobile web searches over a 10-day period. Analysis. We used inductive open coding to categorise the nature of the interruptions assigning each interruption to a category/sub-category combination. We then used a deductive coding approach to classify each interruption as being either internally or externally-induced; and mobile or non mobile-specific. Results. We found a broad range of interruptions, which we have organised into an extensive taxonomy. Further, a substantial proportion of the interruptions are externally-induced and more than half are unique to mobile contexts. Conclusion. The empirical evidence of the nature of mobile search interruptions in our findings provide insight into the complex environment of mobile search, information upon which to base future mobile search studies (e.g., surveys, controlled laboratory studies), and motivation for the study of search interface designs that can help mitigate the effects of such interruptions.
A CONDITIONAL LUMINOSITY FUNCTION MODEL OF THE COSMIC FAR-INFRARED BACKGROUND ANISOTROPY POWER SPECTRUM

The cosmic far-infrared background (CFIRB) is expected to be generated by faint, dusty star-forming galaxies during the peak epoch of galaxy formation. The anisotropy power spectrum of the CFIRB captures the spatial distribution of these galaxies in dark matter halos and the spatial distribution of dark matter halos in the large-scale structure. Existing halo models of CFIRB anisotropy power spectrum either are incomplete or lead to halo model parameters that are inconsistent with the galaxy distribution selected at other wavelengths. Here, we present a conditional luminosity function approach to describe the far-IR bright galaxies. We model the 250 μm luminosity function and its evolution with redshift and model-fit the CFIRB power spectrum at 250 μm measured by the Herschel Space Observatory. We introduce a redshift-dependent duty cycle parameter so that we are able to estimate the typical duration of the dusty star formation process in the dark matter halos as a function of redshifts. We find that the duty cycle of galaxies contributing to the far-IR background is 0.3–0.5 with a dusty star formation phase lasting for ∼0.3–1.6 Gyr. This result confirms the general expectation that the far-IR background is dominated by star-forming galaxies in an extended phase, not bright starbursts that are driven by galaxy mergers and last ∼10–100 Myr. The halo occupation number for satellite galaxies has a power-law slope that is close to unity over 0 < z < 4. We find that the minimum halo mass for dusty, star-forming galaxies with L250 > 1010 L☉ is 2 × 1011 M☉ and 3 × 1010 M☉ at z = 1 and 2, respectively. Integrating over the galaxy population with L250 > 109 L☉, we find that the cosmic density of dust residing in the dusty, star-forming galaxies is responsible for the background anisotropies Ωdust ∼ 3 × 10−6 to 2 × 10−5, relative to the critical density of the universe.
How does offering remote work affect the diversity of the labor pool? Evidence from technology startups

A significant element of managerial post-COVID job design regards remote work. In an era of renewed recognition of diversity, equity and inclusion, employers may wonder how diverse (gender and race) and experienced job applicants respond to remote job listings, especially for high-skilled technical and managerial positions. Prior work has shown that while remote work allows employee flexibility, it may limit career promotion prospects, so the net effect of designating a job as remote-eligible is not clear from an applicant interest standpoint, particularly when recruiting females and underrepresented minorities (URM). We analyze job applicant data from a leading startup job platform, AngelList Talent, that spans long windows before and after the COVID-19 pandemic-induced shutdowns of March 2020. To overcome the empirical challenge that remote job designation may be co-determined with unobserved job and employer characteristics, we leverage a matching approach (and an alternative method which leverages the sudden shutdowns) to estimate how applicant characteristics differ for otherwise similar remote and onsite job postings. We find that offering remote work attracts more experienced and diverse job applicants, with larger effects in less diverse geographic areas. When onsite and remote jobs receive similar numbers of applications, remote jobs attract about 1.25 more applications from URM candidates and from women, and applicants have about 1 year more of experience. The average estimated compensated wage differential for remote work is about 7% (for females 17% and for URM candidates 3%) of posted salaries.
The evolution of the stellar mass function in star clusters

Context. The dynamical escape of stars from star clusters affects the shape of the stellar mass function (MF) in these clusters, because the escape probability of a star depends on its mass. This is found in N-body simulations and has been approximated in analytical cluster models by fitting the evolution of the MF. Both approaches are naturally restricted to the set of boundary conditions for which the simulations were performed. Aims. The objective of this paper is to provide and to apply a simple physical model for the evolution of the MF in star clusters for a large range of the parameter space. It should also offer a new perspective on the results from N-body simulations. Methods. A simple, physically self-contained model for the evolution of the stellar MF in star clusters is derived from the basic principles of two-body encounters and energy considerations. It is independent of the adopted mass loss rate or initial mass function (IMF), and contains stellar evolution, stellar remnant retention, dynamical dissolution in a tidal field, and mass segregation. Results. The MF evolution in star clusters depends on the disruption time, remnant retention fraction, initial-final stellar mass relation, and IMF. Low-mass stars are preferentially ejected after t ∼ 400 Myr. Before that time, masses around 15–20% of the maximum stellar mass are lost due to their rapid two-body relaxation with the massive stars that still exist at young ages. The degree of low-mass star depletion grows for increasing disruption times, but can be quenched when the retained fraction of massive remnants is large. The highly depleted MFs of certain Galactic globular clusters are explained by the enhanced low-mass star depletion that occurs for low remnant retention fractions. Unless the retention fraction is exceptionally large, dynamical evolution always decreases the mass-tolight ratio. The retention of black holes reduces the fraction of the cluster mass in remnants because white dwarfs and neutron stars have masses that are efficiently ejected by black holes. Conclusions. The modeled evolution of the MF is consistent with N-body simulations when adopting identical boundary conditions. However, it is found that the results from N-body simulations only hold for their specific boundary conditions and should not be generalised to all clusters. It is concluded that the model provides an efficient method to understand the evolution of the stellar MF in star clusters under widely varying conditions.
ON LITHIUM-RICH RED GIANTS. I. ENGULFMENT OF SUBSTELLAR COMPANIONS

A small fraction of red giants are known to be lithium (Li) rich, in contradiction with expectations from stellar evolutionary theory. A possible explanation for these atypical giants is the engulfment of an Li-rich planet or brown dwarf by the star. In this work, we model the evolution of Li abundance in canonical red giants including the accretion of a substellar mass companion. We consider a wide range of stellar and companion masses, Li abundances, stellar metallicities, and planetary orbital periods. Based on our calculations, companions with masses lower than dissolve in the convective envelope and can induce Li enrichment in regimes where extra mixing does not operate. Our models indicate that the accretion of a substellar companion can explain abundances up to A(Li) ≈ 2.2, setting an upper limit for Li-rich giants formed by this mechanism. Giants with higher abundances need another mechanism to be explained. For reasonable planetary distributions, we predict the Li abundance distribution of low-mass giants undergoing planet engulfment, finding that between 1% and 3% of them should have . We show that depending on the stellar mass range, this traditional definition of Li-rich giants is misleading, as isolated massive stars would be considered anomalous while giants engulfing a companion would be set aside, flagged as normal. We explore the detectability of companion engulfment, finding that planets with masses higher than produce a distinct signature, and that descendants of stars originating in the Li dip and low-luminosity red giants are ideal tests of this channel.
Long-term variability of high-mass X-ray binaries. I.Photometry

We present photometric observations of the field around the optical counterparts of high-mass X-ray binaries. Our aim is to study the long-term photometric variability in correlation with their X-ray activity and derive a set of secondary standard stars that can be used for time series analysis. We find that the donors in Be/X-ray binaries exhibit larger amplitude changes in the magnitudes and colours than those hosting a supergiant companion. The amplitude of variability increases with wavelength in Be/X-ray binaries and remains fairly constant in supergiant systems. When time scales of years are considered, a good correlation between the X-ray and optical variability is observed. The X-rays cease when optical brightness decreases. These results reflect the fact that the circumstellar disk in Be/X-ray binaries is the main source of both optical and X-ray variability. We also derive the colour excess, E(B-V), selecting data at times when the contribution of the circumstellar disk was supposed to be at minimum, and we revisit the distance estimates.
ON THE ORIGIN OF THE HIGH COLUMN DENSITY TURNOVER IN THE H i COLUMN DENSITY DISTRIBUTION

We study the high column density regime of the H i column density distribution function and argue that there are two distinct features: a turnover at NH i ≈ 1021 cm−2, which is present at both z = 0 and z ≈ 3, and a lack of systems above NH i ≈ 1022 cm−2 at z = 0. Using observations of the column density distribution, we argue that the H i–H2 transition does not cause the turnover at NH i ≈ 1021 cm−2 but can plausibly explain the turnover at NH i ≳ 1022 cm−2. We compute the H i column density distribution of individual galaxies in the THINGS sample and show that the turnover column density depends only weakly on metallicity. Furthermore, we show that the column density distribution of galaxies, corrected for inclination, is insensitive to the resolution of the H i map or to averaging in radial shells. Our results indicate that the similarity of H i column density distributions at z = 3 and 0 is due to the similarity of the maximum H i surface densities of high-z and low-z disks, set presumably by universal processes that shape properties of the gaseous disks of galaxies. Using fully cosmological simulations, we explore other candidate physical mechanisms that could produce a turnover in the column density distribution. We show that while turbulence within giant molecular clouds cannot affect the damped Lyα column density distribution, stellar feedback can affect it significantly if the feedback is sufficiently effective in removing gas from the central 2–3 kpc of high-redshift galaxies. Finally, we argue that it is meaningful to compare column densities averaged over ∼ kpc scales with those estimated from quasar spectra that probe sub-pc scales due to the steep power spectrum of H i column density fluctuations observed in nearby galaxies.
Coir from coconut processing waste as a raw material for applications beyond traditional uses

The global production of coconut, mainly for food and oil production, exceeds 62 million tonnes per annum. Large quantities of coconut husk remain unutilized after industrial processing, giving rise to environmental problems. This fails to exploit the potential presented by the extraction of coir, which could have numerous applications. Traditional products such as textiles, mats, and brushes made from coir are increasingly being joined by new, high-value, non-traditional uses. This review article summarizes new fields of application for coir as reinforcing fibers in binderless fiberboards, natural fiber composites, construction materials, solid biofuels, and an absorbent for heavy metals and toxic materials. The use of coir in these new fields will reduce waste and increase sustainability.
Linear Boltzmann Transport for Jet Propagation in the Quark-Gluon Plasma: Elastic Processes and Medium Recoil

A Linear Boltzmann Transport model within perturbative QCD is developed for the study of parton propagation inside the quark-gluon plasma. Both leading partons and thermal recoil partons are tracked so that one can also study jet-induced medium excitations. In this study, we implement the complete set of elastic parton scattering processes and investigate elastic parton energy loss, transverse momentum broadening and their nontrivial energy and length dependence. We further investigate medium modifications of the jet shape and fragmentation functions of reconstructed jets. Contributions from thermal recoil partons are found to have significant influences on jet shape, fragmentation functions and angular distribution of reconstructed jets.
DETECTION OF FLUX EMERGENCE, SPLITTING, MERGING, AND CANCELLATION OF NETWORK FIELDS. II. APPARENT UNIPOLAR FLUX CHANGE AND CANCELLATION

In this second paper in the series, we investigate occurrence frequencies of apparent unipolar processes, cancellation, and emergence of patch structures in quiet regions. Apparent unipolar events are considerably more frequent than cancellation and emergence, per our definition, which is consistent with Lamb et al. Furthermore, we investigate the frequency distributions of changes in flux during apparent unipolar processes and find that they concentrate around the detection limit of the analysis. Combining these findings with the results of our previous paper, Iida et al., which found that merging and splitting are more dominant than emergence and cancellation, these results support the understanding that apparent unipolar processes are actually interactions with and among patches below the detection limit and that there still are numerous flux interactions between the flux range in this analysis and below the detection limit. We also investigate occurrence frequency distributions of flux decrease during cancellation. We found a relatively strong dependence, 2.48 ± 0.26 as a power-law index. This strong dependence on flux is consistent with the model, which was suggested in the previous paper.
A PUBLIC Ks-SELECTED CATALOG IN THE COSMOS/UltraVISTA FIELD: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR POPULATION PARAMETERS,

We present a catalog covering 1.62 deg2 of the COSMOS/UltraVISTA field with point-spread function (PSF) matched photometry in 30 photometric bands. The catalog covers the wavelength range 0.15–24 μm including the available GALEX, Subaru, Canada–France–Hawaii Telescope, VISTA, and Spitzer data. Catalog sources have been selected from the DR1 UltraVISTA Ks band imaging that reaches a depth of Ks, tot = 23.4 AB (90% completeness). The PSF-matched catalog is generated using position-dependent PSFs ensuring accurate colors across the entire field. Also included is a catalog of photometric redshifts (zphot) for all galaxies computed with the EAZY code. Comparison with spectroscopy from the zCOSMOS 10k bright sample shows that up to z ∼ 1.5 the zphot are accurate to Δz/(1 + z) = 0.013, with a catastrophic outlier fraction of only 1.6%. The zphot also show good agreement with the zphot from the NEWFIRM Medium Band Survey out to z ∼ 3. A catalog of stellar masses and stellar population parameters for galaxies determined using the FAST spectral energy distribution fitting code is provided for all galaxies. Also included are rest-frame U − V and V − J colors, L2800 and LIR. The UVJ color–color diagram confirms that the galaxy bi-modality is well-established out to z ∼ 2. Star-forming galaxies also obey a star-forming “main sequence” out to z ∼ 2.5, and this sequence evolves in a manner consistent with previous measurements. The COSMOS/UltraVISTA Ks-selected catalog covers a unique parameter space in both depth, area, and multi-wavelength coverage and promises to be a useful tool for studying the growth of the galaxy population out to z ∼ 3–4.
NEARBY GALAXIES IN MORE DISTANT CONTEXTS

We use published reconstructions of the star formation history (SFH) of the Large Magellanic Cloud (LMC), Small Magellanic Cloud, and NGC 300 from the analysis of resolved stellar populations to investigate where such galaxies might land on well-known extragalactic diagnostic plots over the galaxies' lifetime (assuming that nothing other than their stellar populations change). For example, we find that the evolution of these galaxies implies a complex evolution in the Tully–Fisher relation with look-back time and that the observed scatter is consistent with excursions these galaxies take as their stellar populations evolve. We find that the growth of stellar mass is weighted to early times, despite the strongly star-forming current nature of the three systems. Lastly, we find that these galaxies can take circuitous paths across the color–magnitude diagram. For example, it is possible, within the constraints provided by the current determination of its SFH, that the LMC reached the red sequence at intermediate age prior to ending back up on the blue cloud at the current time. Unfortunately, this behavior happens at sufficiently early times that our resolved SFH is crude and insufficiently constraining to convincingly demonstrate that this was the actual evolutionary path. The limited sample size precludes any general conclusions, but we present these as examples how we can bridge the study of resolved populations and the more distant universe.
Heating the intra-cluster medium by jet-inflated bubbles

We examine the heating of the intra-cluster medium (ICM) of cooling flow clusters of galaxies by jet-inflated bubbles and conclude that mixing of hot bubble gas with the ICM is more important than turbulent heating and shock heating. We use the PLUTO hydrodynamical code in full 3D to properly account for the inflation of the bubbles and to the multiple vortices induced by the jets and bubbles. The vortices mix some hot shocked jet gas with the ICM. For the parameters used by us the mixing process accounts for about four times as much heating as that by the kinetic energy in the ICM, namely, turbulence and sound waves. We conclude that turbulent heating plays a smaller role than mixing. Heating by shocks is even less efficient.
LEVERAGING LABEL HIERARCHIES FOR FEW-SHOT EVERYDAY SOUND RECOGNITION

Everyday sounds cover a considerable range of sound categories in our daily life, yet for certain sound categories it is hard to collect sufficient data. Although existing works have applied few-shot learning paradigms to sound recognition successfully, most of them have not exploited the relationship between labels in audio tax-onomies. This work adopts a hierarchical prototypical network to leverage the knowledge rooted in audio taxonomies. Specifically, a VGG-like convolutional neural network is used to extract acoustic features. Prototypical nodes are then calculated in each level of the tree structure. A multi-level loss is obtained by multiplying a weight decay with multiple losses. Experimental results demonstrate our hierarchical prototypical networks not only outperform prototypical networks with no hierarchy information but yield a better result than other state-of-the-art algorithms. Our code is available in: https://github.com/
Eccentric disc instability in stellar discs formed from inspiralling gas clouds in the Galactic Centre

The inspiral of a turbulent molecular cloud in the Galactic centre may result in the formation of a small, dense and moderately eccentric gas disc around the supermassive black hole (SMBH). Such a disc is unstable to fragmentation and may lead to the formation of young massive stars in the central parsec of the Galaxy. Here we perform high-accuracy direct summation N-body simulations of a ring of massive stars (with initial semi-major axes 0.1 6 a/pc 6 0.4 and eccentricities 0.2 6 e 6 0.4), subject to the potential of the SMBH, a stellar cusp, and the parent gas disc, to study how the orbital elements of the ring evolve in time. The initial conditions for the stellar ring are drawn from the results of previous simulations of molecular cloud infall and disruption in the SMBH potential. While semi-major axes do not evolve significantly, the distribution of eccentricities spreads out very fast (� 1Myr) as a consequence of cusp precession. In particular, stellar orbits with initial eccentricity e > 0.3 (e < 0.3) tend to become even more (less) eccentric, resulting in a bimodal eccentricity distribution. The distribution is qualitatively consistent with that of the massive stars observed in the Galactic centre’s clockwise disc.