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Background Minor Recurrent Aphthous Stomatitis (RAS) represents a disease which is very difficult to prevent. This case-control study focused on possible associations between minor Recurrent Aphthous Stomatitis in children, their oral health, and underlying behavioral indexes of children’s attitudes and habits pertaining to (home) oral hygiene, with the further goal of enabling the dentist to prevent these specific kind of lesions, both from a clinical and a broader psychosocial perspective. Methods Four hundred one school-children (5–10 years old) in Milan (Italy) were submitted to an intra-oral examination, and interviewed with the aid of a brief psychosocial questionnaire. Results At the clinical level, statistically significant associations were observed between the presence of decayed teeth and minor Recurrent Aphthous Stomatitis ( Odds Ratio : 3.15; 95% CI : lower limit 1.06; upper limit: 9.36; Z-test : 2.07, p  = 0.039; Chi-square  = 4.71, p  = 0.030), and between the Decayed Missing or Filled Teeth (DMFT) index and minor aphthous stomatitis ( Odds Ratio : 3.30; 95% CI : lower limit 1.13; upper limit: 9.67; Z-test  = 2.18, p  = 0.029; Chi-square  = 5.27; p  = 0.022), both results pointing to a significant increase—by circa 3 times—in the risk of developing minor Recurrent Aphthous Stomatitis in children exposed to the two above-identified factors (i.e., the presence of decayed teeth and a clearly compromised oral condition, as signaled by the DMFT index), if compared with the risk run by their non-exposed counterparts. At the psychosocial level of analysis, statistically significant associations were observed (1) between children’s practice of spontaneously brushing teeth when not at home and a comparatively lower (i.e. better) Decayed Missing or Filled Teeth index ( Chi-square : 8.95; p  = 0.011), and (2) between receiving parental aid (e.g., proper brushing instructions) while practicing home oral hygiene and a significantly reduced presence of decayed teeth ( Chi-square  = 5.40; p  = .067; Spearman’s Rho , p  = .038). Further, significant associations were also observed between children’s reported severity of dental pain and both (a) the presence of decayed teeth ( Chi-square  = 10.80; p  = 0.011), and (b) children’s (poor) oral health condition as expressed by the Decayed Missing or Filled Teeth index ( Chi-square  = 6.29; p  = 0.043). Interestingly, specific lifestyles and social status, showed no systematic association to other clinical or psychological/psychosocial indices. Conclusions These systematic relations suggest that, in the presence of Recurrent Aphthous Stomatitis in pediatric patients, the dentist should carefully monitor children for potential carious lesions, implement protocols of prevention to control Recurrent Aphthous Stomatitis disease in children affected by caries, and also be particularly aware of the right or wrong habits children may acquire in the course of continued social exchange with their caregivers and peers.

The water at the proposed site of the CHIPS water Cherenkov detector has been studied to measure its attenuation length as a function of filtering time. A 3.2 m vertical column was filled with the water from the Wentworth Pit, proposed site of the CHIPS deployment. Results consistent with attenuation lengths of up to 100m have been observed at this wavelength with filtration and UV sterilization alone.

The observations of the exceptionally bright gamma-ray burst (GRB) 130427A by the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope provide constraints on the nature of these unique astrophysical sources. GRB 130427A had the largest fluence, highest-energy photon (95 GeV), longest γ-ray duration (20 hours), and one of the largest isotropie energy releases ever observed from a GRB. Temporal and spectral analyses of GRB 130427A challenge the widely accepted model that the nonthermal high-energy emission in the afterglow phase of GRBs is synchrotron emission radiated by electrons accelerated at an external shock.

The light emitted by stars and accreting compact objects through the history of the universe is encoded in the intensity of the extragalactic background light (EBL). Knowledge of the EBL is important to understand the nature of star formation and galaxy evolution, but direct measurements of the EBL are limited by galactic and other foreground emissions. Here, we report an absorption feature seen in the combined spectra of a sample of gamma-ray blazars out to a redshift of z ~1.6. This feature is caused by attenuation of gamma rays by the EBL at optical to ultraviolet frequencies and allowed us to measure the EBL flux density in this frequency band.

The origin of Galactic cosmic rays is a century-long puzzle. Indirect evidence points to their acceleration by supernova Shockwaves, but we know little of their escape from the shock and their evolution through the turbulent medium surrounding massive stars. Gamma rays can probe their spreading through the ambient gas and radiation fields. The Fermi Large Area Telescope (LAT) has observed the star-forming region of Cygnus X. The 1-to 100-gigaelectronvolt images reveal a 50-parsec-wide cocoon of freshly accelerated cosmic rays that flood the cavities carved by the stellar winds and ionization fronts from young stellar clusters. It provides an example to study the youth of cosmic rays in a superbubble environment before they merge into the older Galactic population.

The two-detector design of the NOvA neutrino oscillation experiment, in which two functionally identical detectors are exposed to an intense neutrino beam, aids in canceling leading order effects of cross-section uncertainties. However, limited knowledge of neutrino interaction cross sections still gives rise to some of the largest systematic uncertainties in current oscillation measurements. We show contemporary models of neutrino interactions to be discrepant with data from NOvA, consistent with discrepancies seen in other experiments. Adjustments to neutrino interaction models in GENIE are presented, creating an effective model that improves agreement with our data. We also describe systematic uncertainties on these models, including uncertainties on multi-nucleon interactions from a newly developed procedure using NOvA near detector data.

A young and energetic pulsar powers the well-known Crab Nebula. Here, we describe two separate gamma-ray (photon energy greater than 100 mega-electron volts) flares from this source detected by the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. The first flare occurred in February 2009 and lasted approximately 16 days. The second flare was detected in September 2010 and lasted approximately 4 days. During these outbursts, the gamma-ray flux from the nebula increased by factors of four and six, respectively. The brevity of the flares implies that the gamma rays were emitted via synchrotron radiation from peta-electron-volt (10¹⁵ electron volts) electrons in a region smaller than 1.4 x 10⁻² parsecs. These are the highest-energy particles that can be associated with a discrete astronomical source, and they pose challenges to particle acceleration theory.

GRB 090510: a test for special relativity Observations of the distant and short γ-ray burst GRB 090510 with the Fermi Gamma-ray Space Telescope have provided an opportunity to test a central prediction of Einstein's special theory of relativity — the Lorentz invariance. This holds that all observers measure exactly the same speed of light in a vacuum, independent of photon energy. A key test of the violation of Lorentz invariance is a possible variation of photon speed with energy. Accumulated over cosmological light-travel times, even a tiny variation in photon speed should become observable — as for instance sharp features in the light curve of a γ-ray burst. No evidence for the violation of Lorentz invariance was found in the GRB 090510 spectrum, at least down to a limit of the Planck length divided by 1.2. This argues against quantum-gravity theories where the quantum nature of space–time linearly alters the speed of light with photon energy. Lorentz invariance — the postulate that all observers measure exactly the same speed of light in vacuum, independent of photon energy — is a cornerstone of Einstein's special relativity, but it has been suggested that it might break near the Planck scale. A possible variation of photon speed with energy is a key test for this proposed violation; here, by studying sharp features in γ-ray burst light-curves to look for even tiny variations in photon speed, no evidence for the violation of Lorentz invariance is found. A cornerstone of Einstein’s special relativity is Lorentz invariance—the postulate that all observers measure exactly the same speed of light in vacuum, independent of photon-energy. While special relativity assumes that there is no fundamental length-scale associated with such invariance, there is a fundamental scale (the Planck scale, l Planck  ≈ 1.62 × 10 -33  cm or E Planck = M Planck c 2  ≈ 1.22 × 10 19  GeV), at which quantum effects are expected to strongly affect the nature of space–time. There is great interest in the (not yet validated) idea that Lorentz invariance might break near the Planck scale. A key test of such violation of Lorentz invariance is a possible variation of photon speed with energy 1 , 2 , 3 , 4 , 5 , 6 , 7 . Even a tiny variation in photon speed, when accumulated over cosmological light-travel times, may be revealed by observing sharp features in γ-ray burst (GRB) light-curves 2 . Here we report the detection of emission up to ∼31 GeV from the distant and short GRB 090510. We find no evidence for the violation of Lorentz invariance, and place a lower limit of 1.2 E Planck on the scale of a linear energy dependence (or an inverse wavelength dependence), subject to reasonable assumptions about the emission (equivalently we have an upper limit of l Planck /1.2 on the length scale of the effect). Our results disfavour quantum-gravity theories 3 , 6 , 7 in which the quantum nature of space–time on a very small scale linearly alters the speed of light.

A classical nova results from runaway thermonuclear explosions on the surface of a white dwarf that accretes matter from a low-mass main-sequence stellar companion. In 2012 and 2013, three novae were detected in γ rays and stood in contrast to the first γ-ray–detected nova V407 Cygni 2010, which belongs to a rare class of symbiotic binary systems. Despite likely differences in the compositions and masses of their white dwarf progenitors, the three classical novae are similarly characterized as soft-spectrum transient γ-ray sources detected over 2- to 3-week durations. The γ-ray detections point to unexpected high-energy particle acceleration processes linked to the mass ejection from thermonuclear explosions in an unanticipated class of Galactic γ-ray sources.

Astrophysical jet power A small fraction of active galaxies are extreme phenomena, powered by the release of gravitational energy near the supermassive black hole at the galaxy's centre. Just what goes on in the emitting zone, where inflowing gases interact with the outflowing jets, is not clear. One such extreme object is the blazar 3C 279. Multi-band observations of 3C 279 using the Fermi space telescope have revealed a spectacular γ-ray flare coincident with a dramatic change of optical polarization angle. This points to co-spatiality of the optical and γ-ray emission regions and indicates a highly ordered jet magnetic field. Future observation of cosmic accelerators of this type should throw light on how the immense power required to accelerate matter to close to the speed of light is generated. It is widely accepted that strong and variable radiation detected over all accessible energy bands in a number of active galaxies arises from a relativistic, Doppler-boosted jet pointing close to our line of sight. However, the size of the emitting zone and the location of this region relative to the central supermassive black hole are poorly understood. Here, the coincidence of a γ-ray flare with a dramatic change of optical polarization angle is reported, providing evidence for co-spatiality of optical and γ-ray emission regions and indicating a highly ordered jet magnetic field. It is widely accepted that strong and variable radiation detected over all accessible energy bands in a number of active galaxies arises from a relativistic, Doppler-boosted jet pointing close to our line of sight 1 . The size of the emitting zone and the location of this region relative to the central supermassive black hole are, however, poorly known, with estimates ranging from light-hours to a light-year or more. Here we report the coincidence of a gamma (γ)-ray flare with a dramatic change of optical polarization angle. This provides evidence for co-spatiality of optical and γ-ray emission regions and indicates a highly ordered jet magnetic field. The results also require a non-axisymmetric structure of the emission zone, implying a curved trajectory for the emitting material within the jet, with the dissipation region located at a considerable distance from the black hole, at about 10 5 gravitational radii.