Miracle-dz/UniFAR-FTUs huggingface dataset:
FastKLEE: faster symbolic execution via reducing redundant bound checking of type-safe pointers

Symbolic execution (SE) has been widely adopted for automatic program analysis and software testing. Many SE engines (e.g., KLEE or Angr) need to interpret certain Intermediate Representations (IR) of code during execution, which may be slow and costly. Although a plurality of studies proposed to accelerate SE, few of them consider optimizing the internal interpretation operations. In this paper, we propose FastKLEE, a faster SE engine that aims to speed up execution via reducing redundant bound checking of type-safe pointers during IR code interpretation. Specifically, in FastKLEE, a type inference system is first leveraged to classify pointer types (i.e., safe or unsafe) for the most frequently interpreted read/write instructions. Then, a customized memory operation is designed to perform bound checking for only the unsafe pointers and omit redundant checking on safe pointers. We implement FastKLEE on top of the well-known SE engine KLEE and combined it with the notable type inference system CCured. Evaluation results demonstrate that FastKLEE is able to reduce by up to 9.1% (5.6% on average) as the state-of-the-art approach KLEE in terms of the time to explore the same number (i.e., 10k) of execution paths. FastKLEE is opensourced at https://github.com/haoxintu/FastKLEE. A video demo of FastKLEE is available at https://youtu.be/fjV_a3kt-mo.
Warm dark haloes accretion histories and their gravitational signatures

We study clusters in Warm Dark Matter (WDM) models of a thermally produced dark matter particle 0:5 keV in mass. We show that, despite clusters in WDM cosmologies having similar density profiles as their Cold Dark Matter (CDM) counterparts, the internal properties, such as the amount of substructure, shows marked differences. This result is surprising as clusters are at mass scales that are a thousand times greater than that at which structure formation is suppressed. WDM clusters gain significantly more mass via smooth accretion and contain fewer substructures than their CDM brethren. The higher smooth mass accretion results in subhaloes which are physically more extended and less dense. These fine-scale differences can be probed by strong gravitational lensing. We find, unexpectedly, that WDM clusters have higher lensing efficiencies than those in CDM cosmologies, contrary to the naive expectation that WDM clusters should be less efficient due to the fewer substructures they contain. Despite being less dense, the larger WDM subhaloes are more likely to have larger lensing crosssections than CDM ones. Additionally, WDM subhaloes typically reside at larger distances, which radially stretches the critical lines associated with strong gravitational lensing, resulting in excess in the number of clusters with large radial cross-sections at the 2 level. Though lensing profile for an individual cluster vary significantly with the line-of-sight, the radial arc distribution based on a sample of & 100 clusters may prove to be the crucial test for the presence of WDM.
On the Origin of Fast Radio Bursts (FRBs)

We derive stringent constraints on the persistent source associated with FRB 121102: size , age year, energy erg, characteristic electron energy the radiating plasma is confined by a cold plasma of mass these properties are inconsistent with typical “magnetar wind nebulae” model predictions. The fact that suggests that the hot plasma was created by the ejection of a mildly relativistic, shell, which propagated into an extended ambient medium or collided with a pre-ejected shell. Independent of the persistent source model, we suggest a physical mechanism for the generation of fast radio bursts (FRBs): the ejection from an underlying compact object, cm, of highly relativistic shells with energy erg and Lorentz factor , into a surrounding e − p plasma with density (consistent with that inferred for the persistent source). For Es similar to observed FRB energies, plasma conditions appropriate for strong synchrotron maser emission at are formed. A significant fraction of the deposited energy is converted to an FRB with duration , accompanied by ∼10 MeV gamma-rays carrying less energy than the FRB. The inferred energy and mass associated with the source suggest some type of a “weak stellar explosion,” where a neutron star is formed with relatively low mass and energy ejection. However, the current upper limit on R does not allow one to rule out , or the ejection of a larger mass well before the ejection of the confining shell.
Exploding core collapse supernovae with jittering jets

We argue that jittering jets, i.e. jets that have their launching direction rapidly change, launched by the newly formed neutron star in a core-collapse supernova can explode the star. We show that under a wide range of parameters the fast narrow jets deposit their energy inside the star via shock waves, and form two hot bubbles, that eventually merge, accelerate the rest of the star and lead to the explosion. To prevent the jets from penetrating through the collapsing stellar core and escape with their energy, instead of forming the hot bubbles, the jets should be prevented from drilling a hole through the star. This condition can be met if the jets’ axis rapidly changes its direction. This process of depositing jets’ energy into the ambient medium is termed the penetrating jet feedback mechanism. The feedback exists in that the neutron star (or a black hole) at the centre of the core-collapse supernova shuts off its own growth by exploding the star. The jets deposit their energy at a distance of ∼1000 km from the centre and expel the mass above that radius. In our model, the material near the stalled shock at several hundreds kilometers from the centre is not expelled, but it is rather accreted and feed the accretion disc that blows the jets. The neutrinos might influence the accretion flow, but in the proposed model their role in exploding the star is small.
Simple expressions for second order density perturbations in standard cosmology

In this paper we present four simple expressions for the relativistic first and second order fractional density perturbations for ΛCDM cosmologies in different gauges: the Poisson, uniform curvature, total matter and synchronous gauges. A distinctive feature of our approach is the use of a canonical set of quadratic differential expressions involving an arbitrary spatial function, the so-called comoving curvature perturbation, to describe the spatial dependence, which enables us to unify, simplify and extend previous seemingly disparate results. The simple structure of the expressions makes the evolution of the density perturbations completely transparent and clearly displays the effect of the cosmological constant on the dynamics, namely that it stabilizes the perturbations. We expect that the results will be useful in applications, for example, studying the effects of primordial non-Gaussianity on the large scale structure of the universe.
The further implementation of robots in welfare: A co-created application for robot-assisted medication counselling

Here we present the development of a new robot application. Using a user-centered approach, the aim is to enable human-robot interaction and promote patient safety in medication counselling relevant to emergency contraceptive pill. Emergency contraceptive pills seemed like a suitable choice because the primary pharmacy customers, being young, are comfortable with technology, no prescription is needed to buy the pills in Finland, and the robot can provide non-judgmental interaction to the costumers. We suggest the use of field study methods in future research in which both qualitative and quantitative data analyses are combined to expose the challenges and/or opportunities inherent to the design of robot applications for use in human-robot interaction.
GALAXY CANDIDATES AT z ∼ 10 IN ARCHIVAL DATA FROM THE BRIGHTEST OF REIONIZING GALAXIES (BORG[z8]) SURVEY

The Wide Field Camera 3 (WFC3) on the Hubble Space Telescope (HST) enabled the search for the first galaxies observed at z ∼ 8–11 (500–700 Myr after the Big Bang). To continue quantifying the number density of the most luminous galaxies (MAB ∼ −22.0) at the earliest epoch observable with HST, we search for z ∼ 10 galaxies (F125W-dropouts) in archival data from the Brightest of Reionizing Galaxies (BoRG[z8]) survey, originally designed for detection of z ∼ 8 galaxies (F098M-dropouts). By focusing on the deepest 293 arcmin2 of the data along 62 independent lines of sight, we identify six z ∼ 10 candidates satisfying the color selection criteria, detected at S/N > 8 in F160W with MAB = −22.8 to −21.1 if at z = 10. Three of the six sources, including the two brightest, are in a single WFC3 pointing (∼4 arcmin2), suggestive of significant clustering, which is expected from bright galaxies at z ∼ 10. However, the two brightest galaxies are too extended to be likely at z ∼ 10, and one additional source is unresolved and possibly a brown dwarf. The remaining three candidates have mAB ∼ 26, and given the area and completeness of our search, our best estimate is a number density of sources that is marginally higher but consistent at 2σ with searches in legacy fields. Our study highlights that z ∼ 10 searches can yield a small number of candidates, making tailored follow-ups of HST pure-parallel observations viable and effective.
Inspirals into a charged black hole

We model the quasi-circular inspiral of a compact object into a more massive charged black hole. Extreme and intermediate mass-ratio inspirals are considered through a small mass-ratio approximation. Reissner-Nordstr$\ddot{\text{o}}$m spacetime is used to describe the charged black hole. The effect of radiation reaction on the smaller body is quantified through calculation of electromagnetic and gravitational energy fluxes via solution of Einstein's and Maxwell's equations. Inspiral trajectories are determined by matching the orbital energy decay rate to the rate of radiative energy dissipation. We observe that inspirals into a charged black hole evolve more rapidly than comparable inspirals into a neutral black hole. Through analysis of a variety of inspiral configurations, we conclude that electric charge is an important effect concerning gravitational wave observations when the charge exceeds the threshold $|Q|/M \gtrsim 0.071 \sqrt{\epsilon}$, where $\epsilon$ is the mass-ratio.
Planetary Candidates from K2 Campaign 16

Given that Campaign 16 of the K2 mission is one of just two K2 campaigns observed so far in “forward-facing” mode, which enables immediate follow-up observations from the ground, we present a catalog of interesting targets identified through photometry alone. Our catalog includes 30 high-quality planet candidates (showing no signs of being non-planetary in nature), 48 more ambiguous events that may be either planets or false positives, 164 eclipsing binaries, and 231 other regularly periodic variable sources. We have released light curves for all targets in C16 and have also released system parameters and transit vetting plots for all interesting candidates identified in this paper. Of particular interest is a candidate planet orbiting the bright F dwarf HD 73344 (V = 6.9, K = 5.6) with an orbital period of 15 days. If confirmed, this object would correspond to a 2.56 ± 0.18 R⊕ planet and would likely be a favorable target for radial velocity characterization. This paper is intended as a rapid release of planet candidates, eclipsing binaries, and other interesting periodic variables to maximize the scientific yield of this campaign, and as a test run for the upcoming TESS mission, whose frequent data releases call for similarly rapid candidate identification and efficient follow up.
ISS control for continuous‐time systems with filtered time‐varying parameter and saturating actuators

This paper presents new convex conditions to design robust and linear parameter varying (LPV) gains for continuous time‐varying systems subject to saturating actuator and energy bounded disturbances. The input‐to‐state stability conditions are used to design controllers ensuring the minimization of the L2 ‐gain between the disturbance input and the controlled output. Furthermore, optimization procedures to maximize the estimate of the region of attraction, and the bound to the control signal as well, are formulated. The efficacy of the proposed methods is illustrated with numerical examples, including a reference tracking problem, where realistic simulations are performed.
GLOBAL H i KINEMATICS IN DWARF GALAXIES

H i line widths are typically interpreted as a measure of interstellar medium turbulence, which is potentially driven by star formation (SF). In an effort to better understand the possible connections between line widths and SF, we have characterized H i kinematics in a sample of nearby dwarf galaxies by co-adding line-of-sight spectra after removing the rotational velocity to produce average global H i line profiles. These “superprofiles” are composed of a central narrow peak (∼6–10 km s−1) with higher-velocity wings to either side that contain ∼10%–15% of the total flux. The superprofiles are all very similar, indicating a universal global H i profile for dwarf galaxies. We compare characteristics of the superprofiles to various galaxy properties, such as mass and measures of SF, with the assumption that the superprofile represents a turbulent peak with energetic wings to either side. We use these quantities to derive average scale heights for the sample galaxies. When comparing to physical properties, we find that the velocity dispersion of the central peak is correlated with 〈ΣH i〉. The fraction of mass and characteristic velocity of the high-velocity wings are correlated with measures of SF, consistent with the picture that SF drives surrounding H i to higher velocities. While gravitational instabilities provide too little energy, the SF in the sample galaxies does provide enough energy through supernovae, with realistic estimates of the coupling efficiency, to produce the observed superprofiles.
THE SIZE–VIRIAL RADIUS RELATION OF GALAXIES

I use the abundance matching ansatz, which has proven to be successful in reproducing galaxy clustering and other statistics, to derive estimates of the virial radius, R200, for galaxies of different morphological types and a wide range of stellar masses. I show that over eight orders of magnitude in stellar mass galaxies of all morphological types follow an approximately linear relation between half-mass radius of their stellar distribution, r1/2, and virial radius, r1/2 ≈ 0.015 R200, with scatter of ≈0.2 dex. Such scaling is in remarkable agreement with the expectation of models that assume that galaxy sizes are controlled by halo angular momentum, r1/2∝λR200, where λ is the spin of galaxy parent halo. The scatter about the relation is comparable with the scatter expected from the distribution of λ. Moreover, I show that when the stellar and gas surface density profiles of galaxies of different morphological types are rescaled by the radius rn = 0.015 R200, the rescaled profiles follow approximately universal exponential (for late types) and de Vaucouleurs (for early types) form with scatter of only ≈30%–50% at R ≈ 1–3rn. Remarkably, both late- and early-type galaxies have similar mean stellar surface density profiles at R ≳ 1rn. The main difference between their stellar distributions is thus at R < rn. The results of this study imply that galaxy sizes and radial distribution of baryons are shaped primarily by properties of their parent halos and that the sizes of both late-type disks and early-type spheroids are controlled by halo angular momentum.
Latent disease similarities and therapeutic repurposing possibilities uncovered by multi-modal generative topic modeling of human diseases

Human diseases are characterized by multiple features such as their pathophysiological, molecular, and genetic changes. The rapid expansion of such multi-modal disease-omics space provides an opportunity to re-classify diverse human diseases and uncover their latent molecular similarities, which could be exploited to repurpose a therapeutic-target for one disease to another. Herein, we probe this underexplored space by soft-clustering 6,955 human diseases by multi-modal generative topic-modeling. Focusing on chronic kidney disease and myocardial infarction, two most life-threatening diseases, unveiled are their previously underrecognized molecular similarities to neoplasia and mental/neurological-disorders, and 69 repurposable therapeutic-targets for these diseases. Using an edit-distance based pathway-classifier, we also find molecular pathways by which these targets could elicit their clinical effects. Importantly, for the 17 targets, the evidence for their therapeutic usefulness is retrospectively found in the pre-clinical and clinical space, illustrating the effectiveness of the method, and suggesting its broader applications across diverse human diseases.
SOURCE REGIONS OF THE TYPE II RADIO BURST OBSERVED DURING A CME–CME INTERACTION ON 2013 MAY 22

We report on our study of radio source regions during the type II radio burst on 2013 May 22 based on direction-finding analysis of the Wind/WAVES and STEREO/WAVES (SWAVES) radio observations at decameter–hectometric wavelengths. The type II emission showed an enhancement that coincided with the interaction of two coronal mass ejections (CMEs) launched in sequence along closely spaced trajectories. The triangulation of the SWAVES source directions posited the ecliptic projections of the radio sources near the line connecting the Sun and the STEREO-A spacecraft. The WAVES and SWAVES source directions revealed shifts in the latitude of the radio source, indicating that the spatial location of the dominant source of the type II emission varies during the CME–CME interaction. The WAVES source directions close to 1 MHz frequencies matched the location of the leading edge of the primary CME seen in the images of the LASCO/C3 coronagraph. This correspondence of spatial locations at both wavelengths confirms that the CME–CME interaction region is the source of the type II enhancement. Comparison of radio and white-light observations also showed that at lower frequencies scattering significantly affects radio wave propagation.
The dynamical properties of dense filaments in the infrared dark cloud G035.39−00.33⋆

Infrared Dark Clouds (IRDCs) are unique laboratories to study the initial conditions of high-mass star and star cluster formation. We present high-sensitivity and high-angular resolution IRAM PdBI observations of N2H+ (1-0) towards IRDC G035.39-00.33. It is found that G035.39-00.33 is a highly complex environment, consisting of several mildly supersonic filaments (sigma_NT/c_s ~1.5), separated in velocity by <1 km s^-1 . Where multiple spectral components are evident, moment analysis overestimates the non-thermal contribution to the line-width by a factor ~2. Large-scale velocity gradients evident in previous single-dish maps may be explained by the presence of substructure now evident in the interferometric maps. Whilst global velocity gradients are small (<0.7 km s^-1 pc^-1), there is evidence for dynamic processes on local scales (~1.5-2.5 km s^-1 pc^-1 ). Systematic trends in velocity gradient are observed towards several continuum peaks. This suggests that the kinematics are influenced by dense (and in some cases, starless) cores. These trends are interpreted as either infalling material, with accretion rates ~(7 \pm 4)x10^-5 M_sun yr^-1 , or expanding shells with momentum ~24 \pm 12 M_sun km s^-1 . These observations highlight the importance of high-sensitivity and high-spectral resolution data in disentangling the complex kinematic and physical structure of massive star forming regions.
Using Unlabeled Information of Embryo Siblings from the Same Cohort Cycle to Enhance In Vitro Fertilization Implantation Prediction

High content time-lapse embryo imaging assessed by machine learning is revolutionizing the field of in vitro fertilization (IVF). However, the vast majority of IVF embryos are not transferred to the uterus, and these masses of embryos with unknown implantation outcomes are ignored in current efforts that aim to predict implantation. Here, we explore whether, and to what extent the information encoded within “sibling” embryos from the same IVF cohort contribute to the performance of machine learning-based implantation prediction. First, we show that the implantation outcome is correlated with attributes derived from the cohort siblings. Second, we demonstrate that this unlabeled data boosts implantation prediction performance. Third, we characterize the cohort properties driving embryo prediction, especially those that rescued erroneous predictions. Our results suggest that predictive models for embryo implantation can benefit from the overlooked, widely available unlabeled data of sibling embryos by reducing inherent noise of the individual transferred embryo. Significance statement We use in vitro fertilization (IVF) as a model to study the effect of genotypic and environmental variation on phenotype and demonstrate a potential translational application. This is achieved by associating the implantation potential of transferred embryos and the visual information encoded within their non-transferred “sibling” embryos from the same IVF cohort, and establishing that these cohort features contribute to consistent improvement in machine learning implantation prediction regardless of the embryo-focused model. Our results suggest a general concept where the uncertainty in the implantation potential for the transferred embryo can be reduced by information encapsulated in the correlated cohort embryos. Since the siblings’ data are routinely collected, incorporating cohort features in AI-driven embryo implantation prediction can have direct translational implications.
THE MYSTERY OF SPECTRAL BREAKS: LYMAN CONTINUUM ABSORPTION BY PHOTON–PHOTON PAIR PRODUCTION IN THE FERMI GeV SPECTRA OF BRIGHT BLAZARS

We re-analyze Fermi/LAT γ-ray spectra of bright blazars using the new Pass 7 version of the detector response files and detect breaks at ∼5 GeV in the rest-frame spectra of 3C 454.3 and possibly also 4C +21.35, associated with the photon–photon pair production absorption by the He ii Lyman continuum (LyC). We also detect significant breaks at ∼20 GeV associated with hydrogen LyC in both the individual spectra and the stacked redshift-corrected spectrum of several bright blazars. The detected breaks in the stacked spectra univocally prove that they are associated with atomic ultraviolet emission features of the quasar broad-line region (BLR). The dominance of the absorption by the hydrogen Ly complex over He ii, a small detected optical depth, and break energy consistent with head-on collisions with LyC photons imply that the γ-ray emission site is located within the BLR, but most of the BLR emission comes from a flat disk-like structure producing little opacity. Alternatively, the LyC emission region size might be larger than the BLR size measured from reverberation mapping, and/or the γ-ray emitting region is extended. These solutions would resolve the long-standing issue of how the multi-hundred GeV photons can escape from the emission zone without being absorbed by softer photons.
Sneutrino Inflation with α-attractors

Sneutrino inflation employs the fermionic partners of the inflaton and stabilizer field as right-handed neutrinos to realize the seesaw mechanism for light neutrino masses. We show that one can improve the latest version of this scenario and its consistency with the Planck data by embedding it in the theory of cosmological α-attractors.