Miracle-dz/UniFAR-FTUs huggingface dataset:
Objects in Relation for Scene Understanding

The goal of visual image understanding is to have machines which can perceive the world similar to a human. Achieving this goal will provide numerous opportunities for machines to seamlessly interact with users, improving the quality of life of individuals. As the need for understanding a large number of scene classes with thousands of objects grows, there is a gradual shift towards a more fine-grained understanding of scenes. Thus, image understanding algorithms are now faced with the need to be able to scale to an increasing number of scenes and objects, and to better discriminate between fine-grained scenes. Furthermore, we would like to achieve these goals in a robust and generalizable manner, in such a way that the developed algorithms are effective in understanding scene images taken with smartphones, digital cameras, security cameras, or any other means without any further modification or adjustment. Traditional methods rely on visual appearance information to understand scenes. In contrast, to achieve the desired detailed, yet generalizable, level of scene understanding, we need to explore high-level semantic information of scenes. Such information will enable machines to perceive relationships, co-occurrences, and informativeness of the different components of a scene image in a similar manner to a person. Among the different components of scenes, objects provide the richest semantic entity of a scene image; they provide hints about the type of the scene, its location, and how closely it relates to other scenes. Furthermore, objects enable algorithms to reason about the semantic relationships among the different components of a real world scene. In this thesis, we propose techniques for a fine-grained level of scene understanding through exploiting highlevel contextual scene knowledge. We show how to jointly exploit the visual appearance and context of objects in scenes; how to explore the underlying semantic space of related fine-grained scenes; and how to recognize a wide range of objects in scenes and exploit
Prediction of Aerobic Performance in Distance from 1200 to 2800 M for Laboratory Testing with Military Runners

Redkva PE, Zagatto AM, Gomes EB, Kalva-Filho CA, Loures JP, Kaminagakura EI, Papoti M. Prediction of Aerobic Performance in Distance from 1200 to 2800 M for Laboratory Testing with Military Runners. JEPonline 2012;15(5):107-114. An analysis of different techniques for the prediction of running performance has been widely investigated to improve athletes. The purpose of this study was to evaluate the use of laboratory tests to predict running performance. The relationship between maximal oxygen consumption (VO2 max), velocity associated with VO2 max (vVO2 max), and critical velocity (CV) with 1200, 2400, and 2800 m performances. Thirteen Brazilian Army runners performed an incremental treadmill test starting at 12 km·h with increments of 1 km·h every 3 min until exhaustion to determine VO2 max and vVO2 max. Later, the runners ran at 100, 110, and 120% of vVO2 max to determine CV on treadmill. In addition to the laboratory test, the subjects performed three maximal runs at 1200 (P1200), 2400 (P2400), and 2800 (P2800) m on the track. Data normality was verified using the Shapiro Wilk’s and Pearson correlations (P=0.05) were used to determine the relationship between the laboratory variables and the performances field test. The results showed significant correlations for P1200, P2400, and P2800 with CV (r = -0.70) and vVO2 max (r = -0.85). Based on the results of this investigation, we conclude that CV and vVO2 max determined in the laboratory can be used to predict performance in the distances studied in military runners.
THE NEW EXPERIMENTAL DESIGN OF ARTERIALIZED VENOUS FLAP ON THE RABBIT EAR MODEL

The aim of this study was to test a new experimental design of venous system arterialization on the rabbit ear arterialized venous flap (AVF) model. Total number of 10 "Big Chinchila" rabbits were divided in two experimental groups. On both ears of the five rabbits (Group 1) we have performed our original method of venous system arterialization with microsurgical arterialization of the central artery and vein with the preservation of central and peripheral vascular perfusion; at both ears of five rabbits (Group 2) we have performed AVF according to Byan et al., (1995). Vital AVF surface and necrosis percentage were determined in both experimental groups at day 1 and day 14 and results were compared using Student t-test. The results of our experiment indicate that our new experimental design of the AVF on rabbit ear model has better hemodynamic conditions, improves AVF survival and gives significantly bigger vital flap surface at 14 days after venous system arterialization.
THE EXTENDED CHANDRA DEEP FIELD-SOUTH SURVEY: OPTICAL SPECTROSCOPY OF FAINT X-RAY SOURCES WITH THE VLT AND KECK

We present the results of a program to acquire high-quality optical spectra of X-ray sources detected in the Extended-Chandra Deep Field-South (E-CDF-S) and its central 2 Ms area. New spectroscopic redshifts, up to z = 4, are measured for 283 counterparts to Chandra sources with deep exposures (t ∼ 2–9 hr per pointing) using multi-slit facilities on both VLT (VIMOS) and Keck (DEIMOS), thus bringing the total number of spectroscopically identified X-ray sources to over 500 in this survey field. Since our new spectroscopic identifications are mainly associated with X-ray sources in the shallower 250 ks coverage, we provide a comprehensive catalog of X-ray sources detected in the E-CDF-S including the optical and near-infrared counterparts, determined by a likelihood routine, and redshifts (both spectroscopic and photometric), that incorporate published spectroscopic catalogs, thus resulting in a final sample with a high fraction (80%) of X-ray sources having secure identifications. We demonstrate the remarkable coverage of the luminosity–redshift plane now accessible from our data while emphasizing the detection of active galactic nuclei (AGNs) that contribute to the faint end of the luminosity function (L0.5–8 keV ∼ 1043–1044 erg s−1) at 1.5 ≲ z ≲ 3 including those with and without broad emission lines. Our redshift catalog includes 17 type-2 QSOs at 1 ≲ z ≲ 3.5 that significantly increases such samples (2×). Based on our deepest (9 hr) VLT/VIMOS observation, we identify “elusive” optically faint galaxies (Rmag ∼ 25) at z ∼ 2–3 based upon the detection of interstellar absorption lines (e.g., O ii+Si iv, C ii], C iv); we highlight one such case, an absorption-line galaxy at z = 3.208 having no obvious signs of an AGN in its optical spectrum. In addition, we determine accurate distances to eight galaxy groups with extended X-ray emission detected both by Chandra and XMM-Newton. Finally, we measure the physical extent of known large-scale structures (z ∼ 0.7) evident in the CDF-S. While a thick sheet (a radial size of 67.7 Mpc) at z ∼ 0.67 extends over the full field, the z ∼ 0.73 structure is thin (18.8 Mpc) and filamentary as traced by both AGNs and galaxy groups. In the Appendix, we provide spectroscopic redshifts for 49 counterparts to fainter X-ray sources detected only in the 1 and 2 Ms catalogs, and 48 Very Large Array radio sources not detected in X-rays.
CARMA CO(J = 2 − 1) OBSERVATIONS OF THE CIRCUMSTELLAR ENVELOPE OF BETELGEUSE

We report radio interferometric observations of the 12C16O 1.3 mm J = 2 − 1 emission line in the circumstellar envelope of the M supergiant α Ori and have detected and separated both the S1 and S2 flow components for the first time. Observations were made with the Combined Array for Research in Millimeter-wave Astronomy (CARMA) interferometer in the C, D, and E antenna configurations. We obtain good u − v coverage (5–280 kλ) by combining data from all three configurations allowing us to trace spatial scales as small as 0. ″9 over a 32″ field of view. The high spectral and spatial resolution C configuration line profile shows that the inner S1 flow has slightly asymmetric outflow velocities ranging from −9.0 km s−1 to +10.6 km s−1 with respect to the stellar rest frame. We find little evidence for the outer S2 flow in this configuration because the majority of this emission has been spatially filtered (resolved out) by the array. We also report a SOFIA–GREAT CO(J = 12 − 11) emission line profile, which we associate with this inner higher excitation S1 flow. The outer S2 flow appears in the D and E configuration maps and its outflow velocity is found to be in good agreement with high-resolution optical spectroscopy of K i obtained at the McDonald Observatory. We image both S1 and S2 in the multi-configuration maps and see a gradual change in the angular size of the emission in the high absolute velocity maps. We assign an outer radius of 4″ to S1 and propose that S2 extends beyond CARMA's field of view (32″ at 1.3 mm) out to a radius of 17″, which is larger than recent single-dish observations have indicated. When azimuthally averaged, the intensity falloff for both flows is found to be proportional to R−1, where R is the projected radius, indicating optically thin winds with ρ∝R−2.
Web‐based lectures, peer instruction and ultrasound‐integrated medical education

with the statement: ‘I would utilise a PBL case in the future to facilitate a group process. ’ Half of the respondents reported that using the PBL case advanced the group process and half indicated that the PBL case helped in some ways and hindered in others. Generally, there was satisfaction with this approach related to its contribution towards facilitating group process and generating discussion. Members commented about having a clearer understanding of the mission statement. Conversely, the structured nature of PBL was seen by some as impeding brainstorming. The use of a PBL case was successful in providing structure to group members for a complex problemsolving and creative task. This approach provided an opportunity for all group members to participate in discussion, create a common understanding of the elements of the problem, and identify and seek clarification of learning issues as needed. It also helped the group to share a conceptual mental model as they progressed through the case. Although the task for this group was related to curriculum redesign, this is a process-based approach that can be adapted to multiple situations and medical school contexts in which problem solving is the goal.
System Support for Improving the Reliability of MPI Applications and Libraries

Although the Message Passing Interface (MPI) is widely used to develop parallel programs on computing systems such as clusters, MPI applications and libraries suffer from bugs. A recent survey of MPI users indicated that programmers had problems with different types of MPI errors such as non-deterministic errors and distributed operation ordering errors. Furthermore, the underlying MPI library implementations also suffer from software bugs. For example, more than 500 bug tickets are created for various versions of Open MPI each year. Similarly, about 350 bug tickets are reported for MPICH2 each year. These MPI bugs can severely affect the availability and productivity of MPI programs. This dissertation proposes runtime support to improve the reliability of MPI applications and libraries. Our approach is to build software tools using system methods including instrumentation-based profiling and runtime analysis to help detect software bugs in MPI applications and libraries. First, this dissertation proposes a method called FlowChecker to detect communication errors in MPI libraries. The main idea of FlowChecker is to extract program intentions of message passing and to check whether these intentions are fulfilled by the underlying MPI libraries, i.e., whether messages are delivered from the specified sources to the specified destinations. Second, this dissertation proposes another approach called SyncChecker to detect synchronization errors between MPI applications and libraries. SyncChecker tracks relevant memory
THE COMPLEX PHYSICS OF DUSTY STAR-FORMING GALAXIES AT HIGH REDSHIFTS AS REVEALED BY HERSCHEL AND SPITZER

We combine far-infrared photometry from Herschel (PEP/HerMES) with deep mid-infrared spectroscopy from Spitzer to investigate the nature and the mass assembly history of a sample of 31 luminous and ultraluminous infrared galaxies ((U)LIRGs) at z ∼ 1 and 2 selected in GOODS-S with 24 μm fluxes between 0.2 and 0.5 mJy. We model the data with a self-consistent physical model (GRASIL) which includes a state-of-the-art treatment of dust extinction and reprocessing. We find that all of our galaxies appear to require massive populations of old (>1 Gyr) stars and, at the same time, to host a moderate ongoing activity of star formation (SFR ⩽ 100 M☉ yr−1). The bulk of the stars appear to have been formed a few Gyr before the observation in essentially all cases. Only five galaxies of the sample require a recent starburst superimposed on a quiescent star formation history. We also find discrepancies between our results and those based on optical-only spectral energy distribution (SED) fitting for the same objects; by fitting their observed SEDs with our physical model we find higher extinctions (by ΔAV ∼ 0.81 and 1.14) and higher stellar masses (by Δlog(M⋆) ∼ 0.16 and 0.36 dex) for z ∼ 1 and z ∼ 2 (U)LIRGs, respectively. The stellar mass difference is larger for the most dust-obscured objects. We also find lower SFRs than those computed from LIR using the Kennicutt relation due to the significant contribution to the dust heating by intermediate-age stellar populations through “cirrus” emission (∼73% and ∼66% of the total LIR for z ∼ 1 and z ∼ 2 (U)LIRGs, respectively).
Young People, the Internet, and Civic Participation: An Overview of Key Findings from the CivicWeb Project

Amid growing concern about young people's apparent lack of interest and involvement in politics and civil society, many have looked to the Internet for the solution to the problem of “civic disconnection. ” But does the Internet really help to overcome young people's feelings of exclusion, apathy, and lack of motivation, thus improving prospects for democratic citizenship? This article provides an overview of key findings from a pan-European project that set out to address this issue. The CivicWeb project involved three main forms of investigation.First, it looked at the range of websites that seek to promote civic and political participation among young people, particularly focusing on the technological affordances, pedagogies, and ideologies in play on such sites. Second, it explored whether and how young people are involved in civic action on- and offline, their general and specific motivations, and the constraints on their participation. Finally, it addressed issues from the perspective of producers: h.
The Dual Pathway to Information Avoidance in Information Systems Use

This article develops an explanatory model of information avoidance behavior from extant theory and examines its hypotheses using psychophysiological methods. It integrates existing but partially conflicting explanations into a coherent positivist model based on Coping Theory. The existence of two distinct but interlinked causal pathways to information avoidance will be outlined. Both pathways are cause by defects in the information quality. The first pathway is grounded on being threatened by the information’s inconsistency. The second pathway is based on being distressed by the information’s complexity. Due to the involvement of cognition as well as affect, the usefulness of traditional measurement methods alone is deemed to be limited. Thus, we will draw upon recent advances from NeuroIS research in order to integrate psychophysiological measures into an extended, triangulated measurement protocol. This article intends to contribute to this special issue in three ways. First, it shapes a theoretical model for studying information avoidance which has received little attention in IS research. Second, it exemplifies the derivation and instantiation of a NeuroIS measurement model and the selection of appropriate NeuroIS methods for scrutinizing the theoretical information avoidance model. Third, based on the evidence of an experiment, it provides guidelines for how to conduct eye-tracking, pupillometry, and facial electromyography measurements as well as how to subsequently derive meaning from the initial data collected.
DYNAMICS OF LARGE FRAGMENTS IN THE TAIL OF ACTIVE ASTEROID P/2010 A2

We examine the motions of large fragments at the head of the dust tail of the active asteroid P/2010 A2. In previous work, we showed that these fragments were ejected from the primary nucleus in early 2009, either following a hypervelocity impact or by rotationally induced breakup. Here, we follow their positions through a series of Hubble Space Telescope images taken during the first half of 2010. The orbital evolution of each fragment allows us to constrain its velocity relative to the main nucleus after leaving its sphere of gravitational influence. We find that the fragments constituting a prominent X-shaped tail feature were emitted in a direction opposite to the motion of the asteroid and toward the south of its orbital plane. Derived emission velocities of these primary fragments range between 0.02 and 0.3 m s−1, comparable to the ∼0.08 m s−1 gravitational escape speed from the nucleus. Their sizes are on the order of decimeters or larger. We obtain the best fits to our data with ejection velocity vectors lying in a plane that includes the nucleus. This may suggest that the cause of the disruption of P/2010 A2 is rotational breakup.
Sugar-and-acid profile of Penjar tomatoes and its evolution during storage

The alcobaca mutation in the Penjar tomato (Solanum lycopersicum L.) variety alters the ripening process and confers a long shelf life (more than four months). Storage of Penjar tomatoes leads to a distinctive sensory profile valued by local consumers, who prefer aged tomatoes to fresh ones. To study chemical changes occurring during storage, we characterized the complete sugar-and-acid profile of 25 accessions at harvest and at 2 and 4 months after harvest. We found considerable variability in the sugar-and-acid profile within the Penjar variety, especially for fructose and glucose. Some accessions presented exceptionally high values for sugars, making them especially interesting for breeding programs. During postharvest, the concentration of glucose, fructose, and citric acid decreased, whereas the concentration of malic and glutamic acids increased. Data from this study offer novel insights into postharvest changes in tomato quality parameters and help elucidate the reasons for the appreciation of this variety by consumers.
A WEAK LENSING STUDY OF X-RAY GROUPS IN THE COSMOS SURVEY: FORM AND EVOLUTION OF THE MASS–LUMINOSITY RELATION

Measurements of X-ray scaling laws are critical for improving cosmological constraints derived with the halo mass function and for understanding the physical processes that govern the heating and cooling of the intracluster medium. In this paper, we use a sample of 206 X-ray-selected galaxy groups to investigate the scaling relation between X-ray luminosity (LX) and halo mass (M200) where M200 is derived via stacked weak gravitational lensing. This work draws upon a broad array of multi-wavelength COSMOS observations including 1.64 degrees2 of contiguous imaging with the Advanced Camera for Surveys to a limiting magnitude of IF814W = 26.5 and deep XMM-Newton/Chandra imaging to a limiting flux of 1.0 × 10−15 erg cm−2 s−1 in the 0.5–2 keV band. The combined depth of these two data sets allows us to probe the lensing signals of X-ray-detected structures at both higher redshifts and lower masses than previously explored. Weak lensing profiles and halo masses are derived for nine sub-samples, narrowly binned in luminosity and redshift. The COSMOS data alone are well fit by a power law, M200 ∝ (LX)α, with a slope of α = 0.66 ± 0.14. These results significantly extend the dynamic range for which the halo masses of X-ray-selected structures have been measured with weak gravitational lensing. As a result, tight constraints are obtained for the slope of the M–LX relation. The combination of our group data with previously published cluster data demonstrates that the M–LX relation is well described by a single power law, α = 0.64 ± 0.03, over two decades in mass, M200 ∼ 1013.5–1015.5 h−172 M☉. These results are inconsistent at the 3. 7σ level with the self-similar prediction of α = 0.75. We examine the redshift dependence of the M–LX relation and find little evidence for evolution beyond the rate predicted by self-similarity from z ∼ 0.25 to z ∼ 0.8.
Time as Quantum Observable, Canonical Conjugated to Energy

Time, as well as 3-position, sometimes is a parameter, but sometimes is an observable that in quantum theory would be expected to be associated with an operator. However, almost from the birth of quantum mechanics (cf., e.g., Ref.(Pauli, 1926; 1980)), it is known that time cannot be represented by a selfadjoint operator, except in the case of special systems (such as an electrically charged particle in an infinite uniform electric field)1. The list of papers devoted to the problem of time in quantum mechanics is extremely large (see, for instance, Refs. (Aharonov et al., 1998; Atmanspacher & Amann, 1998; Blanchard P & Jadczyk, 1996; Busch et al., 1994; Delgado, 1999; Egusquiza & Muga, 1999; Giannitrapani, 1997; Goźdź A & Dȩbicki, 2007; Grot et al., 1996; Holevo, 1978; 1982; Kijowski, 1997; Kobe et al., 1994; Kocha’nski & Wo’dkievicz, 1999; Leo’n, 1997; Muga et al., 1999; Olkhovsky & Recami, 1968; 1969; 1970; Olkhovsky, 1973; Olkhovsky et al., 1974; Olkhovsky, 1984; 1990; 1992; Olkhovsky & Recami, 1992; Olkhovsky et al., 1995; Olkhovsky & Agresti, 1997; Olkhovsky, 1998; Olkhovsky et al., 2004; Olkhovsky & Recami, 2007; Olkhovsky, 2009; 2011; Recami, 1976; 1977; Srinivas & Vijayalakshmi, 1981; Toller, 1999; Wang & Xiong, 2007), and references therein). The same situation had to be faced also in quantum electrodynamics and, more in general, in relativistic quantum field theory (see, for instance, Refs.(Olkhovsky & Recami, 1968; 1969; Olkhovsky et al., 2004; Olkhovsky & Recami, 2007)). As to quantum mechanics, the very first relevant articles are probably Refs. (Holevo, 1978; 1982; Olkhovsky & Recami, 1968; 1969; 1970; Olkhovsky, 1973; Olkhovsky et al., 1974; Olkhovsky, 1984; 1990; 1992; 1998; Recami, 1976; 1977), and refs. therein. A second set of papers on time in quantum physics (Aharonov et al., 1998; Atmanspacher & Amann, 1998; Blanchard P & Jadczyk, 1996; Busch et al., 1994; Delgado, 1999; Egusquiza & Muga, 1999; Giannitrapani, 1997; Goźdź A & Dȩbicki, 2007; Grot et al., 1996; Kijowski, 1997; Kobe et al.,
ON A SYSTEM OF AXIOMS FOR GEOMETRY ' BY

In these Transactions, vol. 3 (1902), p. 142, E. H. Moore has given a set of projective axioms for geometry. In further development of the standpoint of Moore a system of axioms for three dimensional Euclidian geometry has been constructed by Veblen f by means of the " betweenness " relation. J A feature of Veblen's system is that a planar axiom (axiom VIII, 1. c.) is necessary to establish the existence of an infinitude of points and to prove the theorem, "To any four distinct points of a line the notation A, B, C, D may always be assigned so that they are in the order AB CD. " In this note I give a set of independent axioms in terms of sameness of sense of dyads, abstractly expressed by aßKy8§, which implies Veblen's axioms I-VIII, but which does not require a planar axiom for the proof of the preceding properties. Of the two relations, sameness of sense and betweenness, one is definable in terms of the other; but the two definitions are not equally simple, as will appear below. §2. The axioms and definitions in terms of the relation K are as follows : ||