Geotechnical characterization of Vertisols from Bahia State, Brazil.

Despite the existence of vertic soils with predominance of kaolinite is reported around the world, there are few studies shown the influence of this clay mineral in their geotechnical characteristics. The work aimed to perform a geotechnical characterization of Vertisols from Bahia, Brazil, besides understanding the influence of physical, chemical and mineralogical properties on the geotechnical behavior. Three Vertisols were collected in Juazeiro city, in a semi-arid region, one kaolinitic Vertisol and two smectite Vertisols. Other three Vertsols were collected in Recôncavo region, all presented clay mineralogy with codominance of smectite and kaolinite (Sm-K). A geotechnical characterization was carried out in their diagnostic horizons, determining properties such as granulometric curve, clay activity, linear expansion coefficient, compaction capacity, cohesion (c?), and internal friction angle (ϕ) of saturated soils. We observed that the clay content was the attribute that most influenced the geotechnical characteristics. All soils showed expansion potential above 0.01, considered as very high. The kaolinitic Vertisol showed the lowest clay activity. However, the clay content of 68% contributed to this soil to present an expansion potential similar to the smectite Vertisol with clay content of 35%. The major values of soil compaction were observed for the kaolinitic Vertisol, which presented greater reduction of void ratio and higher density as a function of moisture increase. For this soil, the optimal moisture content (OMC) and maximum dry density (MDD) were 22% and 1.65 g cm-3, respectively. The other soils presented OMC between 18-41% and MDD between 1.75-1.24 g cm-3. These smectite-soils, MDD decreased with increasing of OMC. All soils had low c? values, which is expected for high clay content soils. The c? values increased with increasing of kaolinite and decreased with increasing of clay content. The kaolinite Vertisol showed c? of 0.19 kgf cm-2. The c? values to Sm-K Vertisols ranged between 0.05-0.11 kgf cm-2. As for smectite-soil, c? values ranged between 0.02-0.03 kgf cm-2. Low ϕ values were observed for all soils, which indicates low shear resistance. In its turn, ϕ was more influenced by granulometry, in which higher levels of sand and gravel provided higher ϕ, independently of the type of clay. Vertisols with different mineralogy present different geotechnical characteristics. Keywords: Smectite; kaolinite; expansive soil

Gamma/hadron discrimination using a small-WCD with four PMTs

The Southern Wide-field Gamma-ray Observatory (SWGO) is the next-generation gamma-ray observatory, currently in an R&D phase. The experiment is expected to have a large array of water Cherenkov detectors (WCD) placed at a high elevation (> 4.4 km a.s.l.) in South America. Here we present a WCD concept with reduced surface area and height of stations comprising four PMTs at the bottom. We show that it is possible to reach an excellent gamma/hadron discrimination by analysing the data gathered by this station with machine learning techniques. Such performance can be achieved by analysing the shower patterns at the ground or through the PMTs signal time structure to tag muons. Moreover, it is shown that the station's performance does not depend on the array configuration (dense or sparse) nor on the shower inclination (θ< 40◦). Such a concept reduces the cost associated with the transport of massive amounts of water to high elevation sites while keeping a high physics performance. Therefore, it could be a good candidate station for SWGO, enabling to reach good sensitivities from low energies (∼ 100 GeV) up to the PeV region, covering large ground surface areas (few square km)

The Southern Wide-field Gamma-ray Observatory reach for Primordial Black Hole evaporation

The Southern Wide-field Gamma-ray Observatory (SWGO) is a proposed ground-based gamma-ray detector that will be located in the Southern Hemisphere and is currently in its design phase. In this contribution, we will outline the prospects for Galactic science with this Observatory. Particular focus will be given to the detectability of extended sources, such as gamma-ray halos around pulsars; optimisation of the angular resolution to mitigate source confusion between known TeV sources; and studies of the energy resolution and sensitivity required to study the spectral features of PeVatrons at the highest energies. Such a facility will ideally complement contemporaneous observatories in studies of high energy astrophysical processes in our Galaxy