We present a method to test the impact of ad hoc modifications of some of the generic parameters of hadronic interactions-cross section, elasticity, and multiplicity-on any observable quantity using full three-dimensional simulations of extensive air showers induced by ultrahigh-energy cosmic rays. Our approach not only extends the existing one-dimensional tools to three dimensions, but also introduces more flexible features to better respond to the needs of both theory and experiment. We first thoroughly validate the Conex 3D framework for the simulation of both longitudinal and lateral features of air showers, in particular, for a nonstandard configuration of the framework in which different energy thresholds for modifications are applied. Moreover, we show that the implementations of the ad hoc modifications in this configuration are consistent with the previous one-dimensional simulations. Finally, we discuss the importance of studying the interaction modifications in three dimensions and the effects of parallel modifications of multiple parameters.

The family Kogiidae, comprising the pygmy sperm whale (Kogia breviceps) and the dwarf sperm whale (K. sima), represents some of the least-known cetaceans worldwide. Their small size, deep-diving behaviour, and elusive surface activity result in very few live sightings, particularly in the North Atlantic Ocean. Here, we report two significant observations from the Azores in July 2025: a group of six K. breviceps, the largest reported group size of this species, and a confirmed sighting of K. sima off Pico Island - representing only the sixth record for the archipelago. Photographic evidence and expert validation confirmed the identification of K. sima based on body proportions. We also review records of both species, including other live encounters and strandings, across the Macaronesian archipelagos (Azores, Madeira, Canary Islands, and Cape Verde). Together, our observations and synthesis document an exceptional group size for K. breviceps, emphasise the rarity of K. sima in the region, and highlight the value of whale-watching platforms and citizen science for monitoring elusive cetaceans.

The Auger Engineering Radio Array (AERA) measures radio emission from high-energy extensive air showers. Consisting of 153 autonomous radio-detector stations spread over 17 km^2, it detects radio waves in the frequency range of 30 to 80 MHz. Accurate characterization of the detector response is crucial for proper interpretation of the collected data. Previously, this was achieved through laboratory measurements of the analog chain and simulations and measurements of the antenna's directional response. In this paper, we perform an absolute calibration using the continuously monitored sidereal modulation of the diffuse Galactic radio emission. Calibration is done by comparing the average frequency spectra recorded by the stations with predictions from seven different models of the full radio sky, accounting for the system response, which includes the antenna, filters, and amplifiers. The analysis of the calibration constants over a period of seven years shows no relevant and no significant ageing effect in the AERA antennas. This result confirms the long-term stability of the detector stations and demonstrates the possibility for a radio detector to effectively monitor ageing effects of other detectors operating over extended periods.

The visibility of stars is often used for cloud detection using all-sky cameras, which have however only a limited reach and resolution near the horizon due to the lack of detectable stars. At the Pierre Auger Observatory, it is also used by the current generation of FRAM robotic telescopes, but – due to their limited field of view – only for a small number of selected showers. Thanks to the recent development in astronomical CMOS cameras, we are able to propose a new type of device, specifically tailored to the field of view of the fluorescence detectors (FD) of the Pierre Auger Observatory. The sub-second readout times available with CMOS cameras allows the efficient use of short exposures, and so the field of view of one FD can be covered within half a minute with a resolution and limiting magnitude sufficient to detect small clouds with a setup that is significantly smaller, simpler and cheaper than the current FRAMs. The FRAM Next Generation (framNG) device will be able not only to detect clouds, but also to assess their optical thickness, provide information on aerosol extinction, sky brightness and possibly even record atmospheric phenomena and astrophysical transients. The main challenge lies in the large data volume produced which necessitates reliable real-time data processing.