Miracle-dz/UniFAR-FTUs huggingface dataset:
GRB spectral parameter modeling

Abstract Fireball model of the gamma-ray bursts (GRBs) predicts generation of numerous internal shocks, which efficiently accelerate charged particles and generate relatively small-scale stochastic magnetic and electric fields. The accelerated particles diffuse in space due to interaction with the random waves and so emit so called Diffusive Synchrotron Radiation (DSR) in contrast to standard synchrotron radiation they would produce in a large-scale regular magnetic fields. In this contribution we present key results of detailed modeling of the GRB spectral parameters, which demonstrate that the non-perturbative DSR emission mechanism in a strong random magnetic field is consistent with observed distributions of the Band parameters and also with cross-correlations between them.
Stability of rotating self-gravitating filaments: effects of magnetic field

We have performed systemmatic local linear stability analysis on a radially stratified infinite self-gravitating cylinder of rotating plasma under the influence of magnetic field. In order to render the system analytically tractable, we have focussed solely on the axisymmetric modes of perturbations. Using cylindrical coordinate system, we have derived the critical linear mass density of a non-rotating filament required for gravitational collapse to ensue in the presence of azimuthal magnetic field. Moreover, for such filaments threaded by axial magnetic field, we show that the growth rates of the modes having non-zero radial wavenumber are reduced more strongly by the magnetic field than that of the modes having zero radial wavenumber. More importantly, our study contributes to the understanding of the stability property of rotating astrophysical filaments that are more often than not influenced by magnetic fields. In addition to complementing many relevant numerical studies reported the literature, our results on filaments under the influence of magnetic field generalize some of the very recent analytical works (e.g.,~\citet{jog2014}, etc.). For example, here we prove that even a weak magnetic field can play a dominant role in determining stability of the filament when the rotation timescale is larger than the free fall timescale. A filamentary structure with faster rotation is, however, comparatively more stable for the same magnetic field. The results reported herein, due to strong locality assumption, are strictly valid for the modes for which one can ignore the radial variations in the density and the magnetic field profiles.
SERENDIPITOUS DISCOVERY OF A MASSIVE cD GALAXY AT z = 1.096: IMPLICATIONS FOR THE EARLY FORMATION AND LATE EVOLUTION OF cD GALAXIES

We have made a serendipitous discovery of a massive (∼5 × 1011 M☉) cD galaxy at z = 1.096 in a candidate-rich cluster in the Hubble Ultra Deep Field (HUDF) area of GOODS-South. This brightest cluster galaxy (BCG) is the most distant cD galaxy confirmed to date. Ultra-deep HST/WFC3 images reveal an extended envelope starting from ∼10 kpc and reaching ∼70 kpc in radius along the semimajor axis. The spectral energy distributions indicate that both its inner component and outer envelope are composed of an old, passively evolving (specific star formation rate <10−4 Gyr−1) stellar population. The cD galaxy lies on the same mass–size relation as the bulk of quiescent galaxies at similar redshifts. The cD galaxy has a higher stellar mass surface density () but a similar velocity dispersion () to those of more massive, nearby cDs. If the cD galaxy is one of the progenitors of today's more massive cDs, its size (R50) and stellar mass have had to increase on average by factors of 3.4 ± 1.1 and 3.3 ± 1.3 over the past ∼8 Gyr, respectively. Such increases in size and stellar mass without being accompanied by significant increases in velocity dispersion are consistent with evolutionary scenarios driven by both major and minor dissipationless (dry) mergers. If such cD envelopes originate from dry mergers, our discovery of even one example proves that some BCGs entered the dry merger phase at epochs earlier than z = 1. Our data match theoretical models which predict that the continuance of dry mergers at z < 1 can result in structures similar to those of massive cD galaxies seen today. Moreover, our discovery is a surprise given that the extreme depth of the HUDF is essential to reveal such an extended cD envelope at z > 1 and, yet, the HUDF covers only a minuscule region of sky (∼3.1 × 10−8). Adding that cDs are rare, our serendipitous discovery hints that such cDs may be more common than expected, perhaps even ubiquitous. Images reaching HUDF depths of more area (especially with cluster BCGs at z > 1) are needed to confirm this conjecture.
Skyrmion confinement in ultrathin film nanostructures in the presence of Dzyaloshinskii-Moriya interaction

We study the modification of micromagnetic configurations in nanostructures, due to the Dzyaloshinskii-Moriya interaction (DMI), that appear at the interface of an ultrathin film. We show that this interaction leads to micromagnetic boundary conditions that bend the magnetization at the edges. We explore several cases of ultrathin film nanostructures that allow analytical calculations (one-dimensional systems, domain walls, cycloids, and skyrmions), compare with fully numerical calculations, and show that a good physical understanding of this type of micromagnetics can be reached. We particularly focus on skyrmions confined in circular nanodots and show that edges allow for the isolation of single skyrmions for a large range of the DMI parameter.
Hard and soft walls

In a continuing effort to understand divergences which occur when quantum fields are confined by bounding surfaces, we investigate local energy densities (and the local energy-momentum tensor) in the vicinity of a wall. In this paper, attention is largely confined to a scalar field. If the wall is an infinite Dirichlet plane, well known volume and surface divergences are found, which are regulated by a temporal point-splitting parameter. If the wall is represented by a linear potential in one coordinate z, the divergences are softened. The case of a general wall, described by a potential of
Factors affecting green building consumer behaviour: evidence from Brazil

ABSTRACT This article identifies the key factors that influenced the consumer purchase behaviour of green-certified buildings in Brazil. To do this, a theoretical model was developed from three systematic literature reviews (SLR) on three literature streams (green buildings, traditional buildings, and green products) – alongside classical consumer behaviour model. The resulting model was then used to set up the hypotheses that were evaluated through a mixed-method approach based on in-depth interviews and a survey with Brazilian customers who had bought a green building certified apartment or house. Our findings showed that there were nine key factors that positively influenced their purchasing behaviour: motivation, knowledge, environmental attitude, values and personality, physical attributes, external environment, trust, lifestyle, and situation. They were motivated by the desire to live in a sustainable property, live in a more secure environment, own a home and leave a legacy for future generations; and having background information and knowledge about green buildings and a high degree of environmental attitude and sustainability related values and lifestyle. Our contribution is threefold. To the best of our knowledge, this is the first study that investigates the key factors that influenced the actual behaviour of green building consumers in the Brazilian market, and one of the few that studies the actual buying behaviour rather than intention. It extends the extant literature by studying a more comprehensive set of factors and it contributes to the investigation of consumer behaviour of traditional and sustainable products in emerging markets.
Bow-shock pulsar-wind nebulae passing through density discontinuities

Bow-shock pulsar wind nebulae are a subset of pulsar wind nebulae that form when the pulsar has high velocity due to the natal kick during the supernova explosion. The interaction between the relativistic wind from the fast-moving pulsar and the interstellar medium produces a bow-shock and a trail, which are detectable in H$_{\alpha}$ emission. Among such bow-shock pulsar wind nebulae, the Guitar Nebula stands out for its peculiar morphology, which consists of a prominent bow-shock head and a series of bubbles further behind. We present a scenario in which multiple bubbles can be produced when the pulsar encounters a series of density discontinuities in the ISM. We tested the scenario using 2-D and 3-D hydrodynamic simulations. The shape of the guitar nebula can be reproduced if the pulsar traversed a region of declining low density. We also show that if a pulsar encounters an inclined density discontinuity, it produces an asymmetric bow-shock head, consistent with observations of the bow-shock of the millisecond pulsar J2124-3358.
FCNC B s and Λ b transitions: Standard model versus a single universal extra dimension scenario

We study the flavor changing neutral current B{sub s}{yields}{phi}{gamma}, {phi}{nu}{nu} and {lambda}{sub b}{yields}{lambda}{gamma}, {lambda}{nu}{nu} transitions in the standard model and in a scenario with a single universal extra dimension. In particular, we focus on the present knowledge of the hadronic uncertainties and on possible improvements. We discuss how the measurements of these modes can be used to constrain the new parameter involved in the extra-dimensional scenario, the radius R of the extra dimension, completing the information available from B-factories. The rates of these b{yields}s induced decays are within the reach of new experiments, such as LHCb.
Magnetic Resonance Imaging in Trigeminal Neuralgia

Background: Trigeminal neuralgia (TN) is still a serious neurologic condition that causes significant facial pain that is unilateral and is distributed across the trigeminal nerve. Magnetic resonance imaging (MRI) is an excellent imaging technique for determining the aetiology of TN, despite the fact that there are no particular clinical tests for its diagnosis. 3D FIESTA MRI helps to improve diagnostic precision and identify neurovascular compression when used in conjunction with conventional MRI. MRI is used to rule out alternative causes of TN, such as cerebellopontine angle lesions, demyelinating diseases, and inflammatory conditions, in addition to neurovascular compression. Aim of the Work: The objective of this study was to assess the utility of MRI in the diagnosis of TN and its various causes. Patients and Methods: In this prospective study, 30 patients (14 men and 16 women), with an average age of 49.6 years, were referred to Tanta University Hospital's Radiodiagnosis and Medical Imaging Department from outpatient neurosurgery and/or dental clinics. Results: The commonest affected side was the left side (46.7%) followed by the right one (40%), while bilateral affection was seen in (13.3%) of cases. According to aetiological factor, TN was secondary to underlying pathology in 24 cases (80%), while idiopathic TN with no underlying pathology was found in 6 cases (20%). Neurovascular compression and neoplastic lesions had the higher incidence. The most affected segment of the trigeminal nerve was the cisternal segment that was involved in 15 cases out of 24 cases with abnormal MRI findings. Conclusion: Many CPA lesions may cause TN such as schwannomas and meningiomas. Demyelinating disease as multiple sclerosis were reported in our study to cause also TN. MRI showed that it has significant diagnostic role denoting brain lesions in patients with TN as it has a diagnostic accuracy 62.5%, sensitivity 60% and specificity 100% (P < 0.001).
A Theory-Informed Systematic Review of Barriers and Enablers to Implementing Multi-Drug Pharmacogenomic Testing

PGx testing requires a complex set of activities undertaken by practitioners and patients, resulting in varying implementation success. This systematic review aimed (PROSPERO: CRD42019150940) to identify barriers and enablers to practitioners and patients implementing pharmacogenomic testing. We followed PRISMA guidelines to conduct and report this review. Medline, EMBASE, CINAHL, PsycINFO, and PubMed Central were systematically searched from inception to June 2022. The theoretical domain framework (TDF) guided the organisation and reporting of barriers or enablers relating to pharmacogenomic testing activities. From the twenty-five eligible reports, eleven activities were described relating to four implementation stages: ordering, facilitating, interpreting, and applying pharmacogenomic testing. Four themes were identified across the implementation stages: IT infrastructure, effort, rewards, and unknown territory. Barriers were most consistently mapped to TDF domains: memory, attention and decision-making processes, environmental context and resources, and belief about consequences.
Intervention, war expansion, and the international sources of civil war

Why do some civil wars turn into interstate wars? I analyze an asymmetric information model of civil war onset, rebel-sided intervention, and interstate retaliation with endogenous stakes. Interstate war occurs when rebels believe that the threat of intervention will compel the government to acquiesce, the third party believes that the government will tolerate an intervention, but they both underestimate the government's resolve. The model also has implications for civil wars. Retaliation can deter intervention and rebellion, but intervention can compel the government to give up power, so predicting civil war requires accounting for this triadic interaction.
Probing holographic semilocal quantum liquids with D-branes

We study dynamics of probe D-branes in $(d+2)$-dimensional background with general semi-locality. The background is characterized by a parameter $\eta$ and is conformal to $AdS_{2}\times\mathbb{R}^{d}$. We discuss thermodynamics of the probe D-branes and find that the entropy density is vanishing in the extremal limit, which indicates that the background may correspond to the true ground state of the system. We also clarify the conditions under which the specific heat matches to the behavior of a Fermi liquid or a Bose liquid. We calculate the current-current and density-density retarded Green's functions, from which we can obtain the AC conductivity and the zero sound mode. The AC conductivity scales as $\omega^{-1}$ when $d/\eta 2$, while it contains a logarithmic term in $\omega$ when $d/\eta=2$. We also observe that there is no quasi-particle excitation when $d/\eta\geq2$ and classify the conditions under which the quasi-particle description is valid when $d/\eta<2$.
Instance, Scale, and Teacher Adaptive Knowledge Distillation for Visual Detection in Autonomous Driving

Efficient visual detection is a crucial component in self-driving perception and lays the foundation for later planning and control stages. Deep-networks-based visual systems achieve state-of-the-art performance, but they are usually cumbersome and computationally infeasible for embedded devices (e.g., dash cams). Knowledge distillation is an effective way to derive more efficient models. However, most existing works target classification tasks and treat all instances equally. In this paper, we first present our Adaptive Instance Distillation (AID) method for self-driving visual detection. It can selectively impart the teacher's knowledge to the student by re-weighing each instance and each scale for distillation based on the teacher's loss. In addition, to enable the student to effectively digest knowledge from multiple sources, we also propose a Multi-Teacher Adaptive Instance Distillation (M-AID) method. Our M-AID helps the student to learn the best knowledge from each teacher w.r. t. certain instances and scales. Unlike previous KD methods, our M-AID adjusts the distillation weights in an instance, scale, and teacher adaptive manner. Experiments on the KITTI, COCO-Traffic, and SODA10 M datasets show that our methods improve the performance of a wide variety of state-of-the-art KD methods on different detectors in self-driving scenarios. Compared to the baseline, our AID leads to an average of 2.28% and 2.98% mAP increases for single-stage and two-stage detectors, respectively. By strategically integrating knowledge from multiple teachers, our M-AID method achieves an average of 2.92% mAP improvement.
CoGeNT: A Search for Low-Mass Dark Matter using p-type Point Contact Germanium Detectors

CoGeNT employs $p$-type point-contact (PPC) germanium detectors to search for weakly interacting massive particles (WIMPs). By virtue of its low-energy threshold and ability to reject surface backgrounds, this type of device allows an emphasis on low-mass dark matter candidates (${m}_{\ensuremath{\chi}}\ensuremath{\sim}10\text{ }\text{ }\mathrm{GeV}/{c}^{2}$). We report on the characteristics of the PPC detector presently taking data at the Soudan Underground Laboratory, elaborating on aspects of shielding, data acquisition, instrumental stability, data analysis, and background estimation. A detailed background model is used to investigate the low-energy excess of events previously reported and to assess the possibility of temporal modulations in the low-energy event rate. Extensive simulations of all presently known backgrounds do not provide a viable background explanation for the excess of low-energy events in the CoGeNT data or the previously observed temporal variation in the event rate. Also reported for the first time is a determination of the surface (slow pulse rise time) event contamination in the data as a function of energy. We conclude that the CoGeNT detector technology is well suited to search for the annual modulation signature expected from dark matter particle interactions in the region of WIMP mass and coupling favored by the DAMA/LIBRA results.
The XMM–Newton Bright Survey sample of absorbed quasars: X-ray and accretion properties

We thank the referee for her/his constructive comments that improved the paper. The research leading to these results has received funding from the European Commission Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 267251 ‘Astronomy Fellowships in Italy’ (AstroFIt). The authors acknowledge financial support from the Italian Ministry of Education, Universities and Research (PRIN2010-2011, grant no. 2010NHBSBE) and from ASI (grant no. I/088/06/0). SM and FJC acknowledge financial support by the Spanish Ministry of Economy and Competitiveness through grant AYA2012-31447. SM acknowledges support from the ARCHES project (Seventh Framework of the European Union, no. 313146). We thank F. Pozzi, A. Feltre and E. Lusso for the useful discussions; T. Maccacaro and L. Maraschi for their helpful suggestions; and R. Paladini for her assistance with the WISE data and catalogue. Based on observations obtained with XMM – Newton (an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA, NASA). Based on observations made under the proposals GTC18-10B and GTC44-11A with the Gran Telescopio Canarias (GTC), installed at the Spanish ‘Observatorio del Roque de los Muchachos’ of the Instituto de Astrofisica de Canarias, in the island of La Palma. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS web site is http://www.sdss. org/ . The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. This publication makes use of data products from the WISE , which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has made use of NASA's Astrophysics Data System.
Characterizing Intracluster Light in the Hubble Frontier Fields

We investigate the intracluster light (ICL) in the six Hubble Frontier Field clusters at 0.3 < z < 0.6 . We employ a new method, which is free from any functional form of the ICL profile, and exploit the unprecedented depth of this Hubble Space Telescope imaging to map the ICL’s diffuse light out to clustrocentric radii R ∼ 300 kpc ( μ ICL ∼ 27 mag arcsec−2). From these maps, we construct radial color and stellar mass profiles via SED fitting and find clear negative color gradients in all systems with increasing distance from the Brightest Cluster Galaxy (BCG). While this implies older/more metal-rich stellar components in the inner part of the ICL, we find that the ICL mostly consists of a ≲ 2 Gyr population, and plausibly originated with log M * / M ⊙ ≲ 10 cluster galaxies. Furthermore, we find that 10%–15% of the ICL’s mass at large radii ( ≳ 150 kpc) lies in a younger/bluer stellar population (∼1 Gyr), a phenomenon not seen in local samples. We attribute this light to the higher fraction of star-forming/(post-)starburst galaxies in clusters at z ∼ 0.5 . Ultimately, we find the ICL’s total mass to be log M * ICL / M ⊙ ∼ 11 –12, constituting 5%–20% of the clusters’ total stellar mass, or about half of the value at z ∼ 0 . The above implies distinct formation histories for the ICL and BCGs/other massive cluster galaxies; i.e., the ICL at this epoch is still being constructed rapidly ( ∼ 40 M ⊙ yr−1), while the BCGs have mostly completed their evolution. To be consistent with the ICL measurements of local massive clusters, such as Virgo, our data suggest mass acquisition mainly from quiescent cluster galaxies is the principal source of ICL material in the subsequent ∼5 Gyr of cosmic time.
Star-forming galaxies in low-redshift clusters: Effects of environment on the concentration of star formation

Aims. We attempt to determine the dominant processes acting on star-forming disk galaxies as a result of the cluster environment by studying the normalised rates and radial distributions of star formation in galaxies within low-redshift clusters. Methods. We develop indicators of different processes based on the radial concentrations of R-band and Hα light within each of the galaxies studied. The tests are applied to galaxies in each of 3 environments – cluster, supercluster (outside the cluster virial radius) and field. We develop new diagnostic diagrams combining star-formation rate and spatial distribution information to differentiate between stripping of outer disk gas, general gas depletion, nuclear starbursts and galaxy-wide enhancement of star formation. Results. Hubble type classifications of cluster galaxies are found to correlate only weakly with their concentration indices, whereas this correlation is strong for non-cluster populations of disk galaxies. We identify a population of early-type disk galaxies in the cluster population with both enhanced and centrally-concentrated star formation compared to their field counterparts. The enhanced cluster galaxies frequently show evidence of disturbance. A small but non-negligible population of cluster galaxies with truncation of star formation in their outer disks is also found.