SPIDER 300A Mark II radio telescope with H142 receiver. Located at the University of Alcalá Space Weather Station. Continuously monitors solar radio burst occurrence from sunrise to sunset at 1.42 GHz, capturing both left and right circular polarization.

Lunt 130 mm telescope with H-alpha filter and ASI 533 MM camera for observations of the solar chromosphere.

Low power flux-gate magnetometer LEMI-031 is intended for the monitoring of three components of the magnetic field vector in land conditions. The instrument is specially designed for battery powered applications and has differential outputs for easy coupling with analogue to digital converter. Several know-hows are used to keep the power consumption of LEMI-031 magnetometer at world lowest level.

GNSS station with a Septentrio PolaRx5S receiver and PolaNt Choke Ring B3/E6 antenna, located at the University of Alcalá Space Weather Station. It monitors satellite signal integrity and ionospheric indices. The station currently tracks GPS, Galileo, GLONASS, BeiDou, SBAS, and NavIC constellations across all available frequencies.

Local pertubation meter. The main objective of this equipement is to address the need for a network of magnetic stations in the Spain and Portugal region, with an inter-station distance not exceeding 1000 km, thereby contributing to the SSA SWE Services Network. To this end, a "Space Weather" prototype has been developed to record data for the detection of solar storms and other types of events, enabling improved anticipation of risks to satellites, power grids, and navigation systems.

Very Low Frequency (VLF) communications refer to radio waves in the 3 to 30 kHz range, which can penetrate seawater and travel long distances by reflecting between the Earth’s surface and the ionosphere. This makes them ideal for communication with submarines. Additionally, VLF signals are highly sensitive to changes in the ionosphere, which is influenced by solar activity such as solar flares and geomagnetic storms. By monitoring variations in VLF signal strength and propagation, we can indirectly study solar activity and its effects on Earth's upper atmosphere. This is a made in-house instrument.