The sensitivity of a radio astronomy receiver determines what science is possible. Every fraction of a kelvin gained in system noise temperature translates directly into scientific capability — from detecting faint emissions of distant galaxies to tracking spacecraft at the edge of the solar system.
Celestia TTI engineers and manufactures the complete RF receive chain for radio telescopes and deep space ground stations: individual feed components (feeders, polarisers, OMTs, diplexers), cryostats with volumes up to 1 m³ and cooling temperatures down to 4 K, cryogenic and warm LNAs, and high-power GaN SSPAs in S, X, and Ka bands for deep space uplink chains. For observatories requiring a single engineering partner from design through commissioning, Celestia TTI also delivers complete turnkey receivers for both cryogenic and uncooled applications.
| Band | Frequency | Noise Temperature | Technology |
|---|---|---|---|
| W band | 72–116 GHz | 31 K (avg) | InP/GaAs |
| Q band | 31–50 GHz | 14 K (avg) | InP/GaAs |
| K-Ka band | 18–32.4 GHz | 8 K (avg) | InP/GaAs |
| X band | 8.4–8.5 GHz | <3 K | InP/GaAs |
| X band | 8–9 GHz | <4 K | InP/GaAs |
| C-X band | 4–12 GHz | 5 K (avg) | InP/GaAs |
| C band | 5.7–6.3 GHz | <2.5 K | InP/GaAs |
| C band | 4–8 GHz | <3.5 K | InP/GaAs |
| S band | 2–4.5 GHz | <3 K | InP/GaAs |
| S band | 2.3–4.8 GHz | <3.5 K | InP/GaAs |
| UHF–S | 0.1–1.1 GHz | 4.5 K (avg) | InP/GaAs |
Every cryo-LNA is fully tested at cryogenic operating temperatures and delivered with a complete factory acceptance test report. Contact Celestia TTI for wideband configurations and custom frequency ranges.
InP and GaAs HEMT technology achieves noise temperatures from under 2.5 K at C band to 31 K at W band, tested and verified at cryogenic operating temperatures with full factory acceptance documentation.
Celestia TTI designs and manufactures the full passive feed chain — corrugated feed horns, OMTs, polarisers, diplexers, and waveguide transitions — minimising loss and noise contribution before the first amplification stage.
Custom cryogenic vessels with volumes up to 1 m³ and base temperatures down to 4 K accommodate complex multi-feed receiver systems, designed for integration with Gifford-McMahon and pulse-tube cryo-coolers.
From preliminary design through manufacturing, site integration, and commissioning, Celestia TTI manages the complete project lifecycle for cryogenic and uncooled receiver systems.
Modular S, X, and Ka band power amplifiers with graceful degradation, hot-swappable modules, and significant OPEX savings over legacy tube technology — for stations requiring both receive and transmit capability.
Frequency bands, polarisation modes, cryostat volumes, and M&C interfaces vary between telescope projects. Celestia TTI's engineering team develops custom configurations tailored to each observatory's specific requirements.
Radio astronomy and deep space station projects involve long development timelines, demanding specifications, and institutional customers who require demonstrated engineering capability. With nearly 30 years of specialist experience, Celestia TTI brings the technical depth and programme track record that observatory and space agency procurement processes demand.
Cryogenic LNA development for SKA band receiver requirements demonstrates the ability to meet specifications set by the most demanding radio telescope projects in construction today.
Cryo-LNA expertise spanning UHF through W band, with every device characterised at cryogenic operating temperatures before delivery.
Custom cryostat design up to 1 m³ and 4 K, with in-house expertise covering RF design, vacuum technology, thermal analysis, and precision mechanical integration.
ISO 9001:2015 and ISO 9100:2018 certified manufacturing. Every cryo-LNA delivered with a complete factory acceptance test report.
Major steerable radio telescopes and VLBI network stations require custom cryogenic receiver systems across multiple frequency bands. Celestia TTI delivers complete receivers for these installations, from individual cryo-LNA modules to fully integrated multi-band cryostats with all passive RF components.
Celestia TTI has developed cryogenic LNA technology for SKA frequency band requirements — including dual-band amplifiers covering the 4.6–8.5 GHz and 8.3–15.4 GHz sub-bands — demonstrating the engineering capability required by the most demanding radio telescope projects currently in development.
Very Long Baseline Interferometry stations require ultra-low-noise cryogenic receivers to maximise the coherent signal available for correlation across intercontinental baselines. Celestia TTI's cryo-LNAs and feed components are suited for new VLBI station builds and receiver upgrades at existing network stations.
Ground stations supporting planetary science missions and interplanetary spacecraft navigation require both high-sensitivity cryogenic receivers and high-power uplink amplifiers. Celestia TTI provides both chains — making it a single engineering partner for the complete RF system at deep space stations.
A cryogenic radio astronomy receiver cools its low noise amplifier and associated passive RF components to cryogenic temperatures — typically between 4 K and 20 K — using a mechanical cryo-cooler. At these temperatures, thermal noise from the receiver electronics drops dramatically, enabling detection of extremely faint radio signals. The cryostat provides the vacuum enclosure and thermal insulation that maintains these operating temperatures around the sensitive components.
An OMT separates the two orthogonal polarisation states of the incoming signal from the feed horn into two independent signal paths, each feeding its own cryogenic LNA. This enables simultaneous dual-polarisation reception, which doubles the available signal bandwidth for continuum observations and allows polarimetric measurements of source properties — essential for studies of magnetic fields and polarised emission from astronomical objects.
The cryo-LNA portfolio spans from UHF–S band (0.1 GHz) through W band (116 GHz), covering the principal frequency allocations used by radio telescope receivers worldwide. Noise temperatures range from under 2.5 K at C band to 31 K average at W band, with all units characterised at cryogenic operating temperatures before delivery.
Celestia TTI’s turnkey receiver scope covers the complete system: feed horn and passive RF component design, cryostat mechanical design and fabrication, LNA selection and integration, warm electronics and IF chain, monitoring and control interfaces, and on-site installation and commissioning. The customer receives a tested, operational receiver rather than individual components requiring separate integration.
Celestia TTI offers GaN-based SSPAs in S, X, and Ka bands for deep space station transmit chains. These modular systems feature graceful degradation, hot-swappable modules for minimal downtime, and significant CAPEX and OPEX savings versus legacy tube amplifiers — the reliability profile that long-duration scientific programmes require.
Yes. Beyond the standard portfolio, the engineering team develops custom amplifiers and receivers for non-standard frequency ranges, specific sub-band coverage, custom form factors, or integration with legacy receiver infrastructure.
