LWA Antenna — Engineered for Radio Astronomy

Burns Industries has played a pivotal role in the development and ongoing production of the LWA (Long Wavelength Array) Antenna. Our involvement began with the design and prototyping of this innovative antenna, and today, we are the sole manufacturer, delivering these high-performance systems to the global scientific community.

The LWA Antenna plays a crucial role in advancing our understanding of the universe. Its applications include:

• Solar and Ionospheric Studies: Monitoring solar emissions and ionospheric conditions to better understand space weather phenomena.

• Cosmic Evolution Research: Investigating the formation and evolution of galaxies, stars, and other celestial bodies.

• Astrophysical Plasma Observations: Studying the properties and behaviors of plasma in various astrophysical contexts.

• Decametric Radio Emissions: Detecting and analyzing low-frequency radio emissions from Jupiter-like extrasolar planets.

• Magnetar Flares: Observing intense radio flares from magnetars to gain insights into these enigmatic objects.

Our involvement with the LWA Antenna began with the design and prototyping phases, where we collaborated closely with leading research institutions to refine the antenna's specifications. Drawing from our extensive experience in manufacturing and engineering, we helped address the unique challenges posed by low-frequency radio astronomy.

Today, as the manufacturer of the LWA Antenna, we continue to uphold the highest standards of quality and reliability. Our MOQ is 32 antennas, for smaller quantities visit www.reeve.com Contact us for more information.

Key Features and Capabilities

• Wide Frequency Range: Operates across the 10–88 MHz spectrum, capturing a broad range of radio frequencies for astronomical observations.

• Active Crossed-Dipole Design: Uses a dual-polarized dipole configuration to enhance signal reception and minimize noise.

• Compact and Rugged Construction: Designed for durability and ease of deployment in diverse field conditions.

• Low Noise Performance: Engineered to achieve a noise figure at least 6 dB better than the Galactic background emission over the operational band for high sensitivity in observations.

• Scalability: Suitable for both standalone installations and integration into larger arrays, providing flexibility for various research needs.