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We have observed a significant enhancement in the energy deposition by 25– 100 GeV photons in a 1 cm thick tungsten crystal oriented along its ⟨ 111 ⟩ lattice axes. At 100 GeV , this enhancement, with respect to the value observed without axial alignment, is more than twofold. This effect, together with the measured huge increase in secondary particle generation is ascribed to the acceleration of the electromagnetic shower development by the strong axial electric field. The experimental results have been critically compared with a newly developed Monte Carlo adapted for use with crystals of multi- X 0 thickness. The results presented in this paper may prove to be of significant interest for the development of high-performance photon absorbers and highly compact electromagnetic calorimeters and beam dumps for use at the energy and intensity frontiers.

Thickening of the gallbladder wall is often associated with acute or chronic cholecystitis, adenomyomatosis and gallbladder carcinoma or seen in the context of liver and systemic diseases (acute hepatitis, cirrhosis, sepsis). Here we present a case of a 61 y.o. man with focal thickening of the gallbladder wall, in whom all imaging techniques were inconclusive. Pathological examination of the resected gallbladder revealed acute-on-chronic cholecystitis. We describe focal acute cholecystitis in absence of the classic clinical and imaging findings (Murphy’s sign, fever, gallstones, hydrops, pericholecystic fluid) and mimicking a gallbladder carcinoma.

In the parameter estimation the sensitivity analysis of the temperature to the unknown parameter (such as thermal conductivity, heat capacity) plays a fundamental role. In the experimental setup for thermal properties measurements of solid materials, the heater in contact with the specimen can be modelled through an high conductivity thin layer. In such a case the one dimensional finite rectangular body, representing the sample, is subject to a boundary condition of the 4th kind at the heated boundary. Also, a constant heat flux applied for a finite period of time is considered in the analysis and the sample backside is assumed insulated. The temperature field within the finite body is obtained by using the superposition principle. Then, the scaled sensitivity coefficients are computed analytically for two different locations: at the interface between the heater and the sample, and at the sample backside. The results show that the sensitivity coefficients with respect to the thermal conductivity and to the volumetric heat capacity of the sample are uncorrelated.

The MIllimetric Sardinia radio Telescope Receiver based on Array of Lumped elements KIDs, MISTRAL, is a cryogenic W-band (77–103 GH) LEKID camera which will be integrated at the Gregorian focus of the 64 m aperture Sardinia Radio Telescope, in Italy, in Autumn 2022. This instrument, thanks to its high angular resolution ( ∼ 13 arcsec ) and the wide instantaneous field of view ( ∼ 4 arcmin ), will allow continuum surveys of the mm-wave sky with a variety of scientific targets, spanning from extragalactic astrophysics to solar system science. In this contribution, we will describe the design of the MISTRAL camera, with a particular focus on the optimisation and test of a prototype of the focal plane.

We describe the setup for the broadband millimeter/submillimeter characterization of the quasi-optical elements and the dielectric materials commonly used in microwave receivers operated in microwave astronomy. The setup is made of a large aperture (100 mm) Fourier transform spectrometer coupled to a transition edge superconducting detector. The system has been assembled and characterized in different configurations and operation modes for the acquisition of interferograms from various kinds of samples. After the initial test runs, the configuration is now being updated to ensure a broader range of measurements, including reflectance and scattering. We plan to first use this testbed for the characterization of the dielectric materials used in the LSPE/SWIPE experiment, devoted to the study the polarization of the Cosmic Microwave Background.

Purpose Self-induced soft-tissue injuries (SSI) are reported as local anesthesia complications, particularly in children. The purpose of the study was to evaluate the frequency of SSI following dental anesthesia in children with and without intellectual disability. Methods 241 children receiving dental treatments with local anesthesia were divided into 2 groups: A, children without intellectual disability (159 individuals, 299 injections); B, children with intellectual disability (82 individuals, 165 injections). Each group was divided into subgroups according to age, injection technique and dental treatment. Two days after the dental procedure, a phone survey was conducted to determine the presence of SSI. Results The frequency of SSI in group B was 19%, with no differences in relation to gender and age. In group A the frequency of SSI was significantly lower (9%; p  = 0.002; Chi-square test); the children in the ≤ 6 years-old subgroup experienced a higher frequency of SSI ( p  = 0.002). The lower arch was at major risk of SSI in both groups ( p  = 0.002). According to a multilevel approach group ( p  = 0.001) and injection technique ( p  = 0.0001) significantly influenced SSI; no influence of dental treatment is evidenced. Conclusions SSI are common complications of local anesthesia in young children and individuals with intellectual disability.

Three experiments were conducted on Martina Franca jennies. Experiment 1 tested Wood’s model for evaluating the lactation curve. Data from the entire lactation period of 12 jennies were used. The results showed that Wood’s model was able to recognize the shape of the lactation curve from pooled data (r2 = 0.11; P < 0.01), with the lactation peak occurring at 48 d. Individual curves showed wide variability. Experiment 2 aimed to evaluate the effects of the daily number of milkings (1, 3, or 6) and the interval between the separation of foals from dams and milking (2 or 3 h) on milk yield and udder health. Four groups of jennies (n = 5) were considered: 1 x 3H, milked once per day (1x) with a 3-h interval from the time of foal removal (3H) from the dams to mechanical milking (3-h interval); 3 x 3H, milked 3 times per day with 3-h intervals; 3 x 2H, milked 3 times per day with 2-h intervals; and 6 x 2H, milked 6 times per day with 2-h intervals. The milk somatic cell count (SCC) was monitored. Better efficiency was observed for 3 vs. 1 milking per day and for 3-h vs. 2-h intervals. The regimen of 6 daily milkings at 2-h intervals did not increase milk yield and was related to an increase in the SCC compared with 3 daily milkings. In Exp. 3, the effects of the interval from foal removal to milking (3, 5, or 8 h) on yield, gross chemical composition, organoleptic characteristics of the milk, and udder health of the jennies were evaluated. The effects of milking time were also evaluated. Twenty jennies milked twice daily (2x) were subdivided into 4 groups (n = 5): 2 x 3H, with milkings at 1200 h and 1900 h and an interval of 3 h; 2 x 5H, milked at 1200 h and 1900 h with a 5-h interval; 2 x 8H1, milked at 1200 h and 2200 h with an 8-h interval; and 2 x 8H2, milked at 0700 h and 1900 h with an 8-h interval. Milk yield was greater by 28.4% when an 8-h interval was used compared with a 3-h interval and at the morning vs. the evening milking. The milk yield per milking was greatest at 0700 h, indicating the existence of a circadian rhythm in milk secretion processes. Intervals of 5 and 8 h caused significant decreases in the fat and lactose content and organoleptic characteristics of the milk, whereas an 8-h interval led to an increase in the SCC. In conclusion, a milking regimen of twice-daily milking at 0700 h and 1900 h with an 8-h interval provided the maximum yield per day. In terms of milk quality, a 3-h interval yielded the best results.

COSMO is a ground-based instrument to measure the spectral distortions (SD) of the Cosmic Microwave Background (CMB). In this paper, we present preliminary results of electromagnetic simulations of its reference blackbody calibrator. HFSS simulations provide a calibrator reflection coefficient of R ∼ 10 - 6 , corresponding to an emissivity ϵ = 1 - R = 0.999999 . We also provide a forecast for the instrument performance by using an ILC-based simulation. We show that COSMO can extract the isotropic Comptonization parameter (modeled as | y | = 1.77 · 10 - 6 ) as | y | = ( 1.79 ± 0.19 ) · 10 - 6 , in the presence of the main Galactic foreground (thermal dust) and of CMB anisotropies, and assuming perfect atmospheric emission removal.

Kinetic Inductance Detectors (KIDs) are superconductive low-temperature detectors useful for astrophysics and particle physics. We have developed arrays of lumped elements KIDs (LEKIDs) sensitive to microwave photons, optimized for the four horn-coupled focal planes of the OLIMPO balloon-borne telescope, working in the spectral bands centered at 150 GHz, 250 GHz, 350 GHz, and 460 GHz. This is aimed at measuring the spectrum of the Sunyaev-Zel'dovich effect for a number of galaxy clusters, and will validate LEKIDs technology in a space-like environment. Our detectors are optimized for an intermediate background level, due to the presence of residual atmosphere and room-temperature optical system and they operate at a temperature of 0.3 K. The LEKID planar superconducting circuits are designed to resonate between 100 and 600 MHz, and to match the impedance of the feeding waveguides; the measured quality factors of the resonators are in the 104 - 105 range, and they have been tuned to obtain the needed dynamic range. The readout electronics is composed of a cold part, which includes a low noise amplifier, a dc-block, coaxial cables, and power attenuators; and a room-temperature part, FPGA-based, including up and down-conversion microwave components (IQ modulator, IQ demodulator, amplifiers, bias tees, attenuators). In this contribution, we describe the optimization, fabrication, characterization and validation of the OLIMPO detector system.

In the quest for the faint primordial B-mode polarization of the Cosmic Microwave Background, three are the key requirements for any present or future experiment: an utmost sensitivity, excellent control over instrumental systematic effects and over Galactic foreground contamination. Bolometric Interferometry (BI) is a novel technique that matches them all by combining the sensitivity of bolometric detectors, the control of instrumental systematics from interferometry and a software-based, tunable, in-band spectral resolution due to its ability to perform band-splitting during data analysis (spectral imaging). In this paper, we investigate how the spectral imaging capability of BI can help in detecting residual contamination in case an over-simplified model of foreground emission is assumed in the analysis. To mimic this situation, we focus on the next generation of ground-based CMB experiment, CMB-S4, and compare its anticipated sensitivities, frequency and sky coverage with a hypothetical version of the same experiment based on BI, CMB-S4/BI, assuming that lineof-sight (LOS) frequency decorrelation is present in dust emission but is not accounted for during component separation. We show results from a Monte-Carlo analysis based on a parametric component separation method (FGBuster), highlighting how BI has the potential to diagnose the presence of foreground residuals in estimates of the tensor-to-scalar ratio r in the case of unaccounted Galactic dust LOS frequency decorrelation.