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ESA’s LISA mission entered industrial development on June 17, 2025, when ESA and OHB System AG signed the agreement to finalize the spacecraft design and begin construction of the three-spacecraft observatory. LISA has not launched or begun taking data: as of 2026, it remains under development, with launch currently planned for 2035.
The mission is often described as the first to “surf” gravitational waves. More precisely, LISA will be the first space-based observatory dedicated to gravitational-wave astronomy. It will use laser beams spanning 2.5 million kilometres between spacecraft to measure tiny changes in distance caused by ripples in spacetime.
What began in June 2025?
The June 17, 2025 announcement marked the start of LISA’s industrial development, not the completion of the observatory. ESA and OHB System AG signed an implementation agreement under which OHB will lead the spacecraft development, finalize the design and begin construction of the three spacecraft. ESA described the milestone as the beginning of construction.
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That step followed a separate milestone: ESA formally adopted LISA on January 25, 2024, after determining that its concept and enabling technologies were mature enough to proceed toward development. Prototype hardware and subsystem work continued through 2025 and 2026.
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For example, NASA reported in January 2026 that engineers had tested a second early version of a laser-frequency-reference system for LISA. In May 2026, Thales Alenia Space announced a €26.1 million ESA contract for Phase 1 development of the mission’s six telescopes. These are important hardware-development steps, but they do not mean the flight observatory is already assembled.
LISA is currently planned to launch from Europe’s Spaceport in French Guiana aboard an Ariane 6 rocket in 2035. That is a target, not an immovable launch appointment.
LISA in one sentence
LISA will be a giant laser interferometer in space, formed by three spacecraft flying in a triangular formation around the Sun and measuring changes in their separation caused by low-frequency gravitational waves.
The spacecraft will trail Earth in a heliocentric orbit. Their near-equilateral triangle will have arms approximately 2.5 million kilometres long—about 1.6 million miles. The spacecraft will not be connected by cables or rigid beams. Their formation will be maintained through coordinated orbits, laser links and precision spacecraft control.
Why put a gravitational-wave detector in space?
Gravitational waves are oscillations in spacetime produced by accelerating massive objects, such as merging black holes. They stretch and compress distances as they pass, but the effect is extraordinarily small.
Earth-based observatories such as LIGO and Virgo are highly sensitive, but their terrestrial location and physical size limit the frequencies they can study. Seismic motion, local gravity gradients, traffic, weather and other disturbances also create challenges. Building an Earth-based interferometer with million-kilometre arms is not practical.
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LISA will target a different part of the gravitational-wave spectrum: approximately 0.1 millihertz to 100 millihertz, according to Thales Alenia Space. This low-frequency range is largely inaccessible to current ground-based detectors.
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How the three-spacecraft detector works
Each LISA spacecraft will contain two free-floating gold-platinum cubes called test masses or proof masses. They are designed to behave as extremely quiet inertial reference bodies, shielded as much as possible from forces other than gravity.
Laser beams will be exchanged between the spacecraft. By comparing the phase of the laser light across the three enormous arms, LISA will reconstruct changes in the distances between the proof masses. A passing gravitational wave will produce a time-dependent pattern of stretching and compression across the triangular constellation.
The required sensitivity is extraordinary. ESA describes the measurement as detecting shifts of only a few billionths of a millimetre over a 2.5-million-kilometre baseline. NASA uses comparisons involving changes smaller than the diameter of a hydrogen or helium atom.
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Why gold-platinum proof masses?
The proof masses must provide reference points that are affected almost entirely by gravity. Any contact, mechanical suspension or unwanted electrical force could overwhelm the tiny signal LISA is trying to measure.
The gold-platinum alloy helps provide dense, electrically conductive test masses with suitable magnetic and material properties. The spacecraft will need to shield and monitor them, manage their electrostatic charge and prevent the spacecraft itself from disturbing their motion.
This technology builds on ESA’s LISA Pathfinder mission, which demonstrated the ability to maintain test masses in highly precise free fall.
What could LISA discover?
Merging massive black holes
When galaxies merge, the massive black holes at their centres may eventually spiral together. These systems can produce gravitational waves at frequencies suited to LISA. Observing them could help scientists investigate how black holes formed, grew and evolved across cosmic history.
Extreme-mass-ratio inspirals
LISA may detect extreme-mass-ratio inspirals, in which a compact object such as a stellar remnant orbits a much more massive black hole. The gradual inspiral can encode information about the black hole’s mass, spin and surrounding spacetime, offering tests of gravity under extreme conditions.
Compact binaries in the Milky Way
White-dwarf binaries and other compact stellar-remnant systems are expected to form a major population of LISA sources. Their signals may allow astronomers to study large numbers of otherwise difficult-to-observe systems across the Milky Way.
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A possible gravitational-wave background
LISA may also search for a stochastic background made from overlapping astrophysical signals or relic signals from the early universe. These are scientific possibilities, not guaranteed discoveries. The mission will not directly photograph the Big Bang or produce ordinary images of merging black holes.
ESA’s mission overview presents a headline expectation of more than 10,000 gravitational-wave events, but that figure is an anticipated mission yield rather than a guaranteed number of confirmed discoveries. Finding a signal and identifying its source are separate challenges, particularly when many compact-binary signals overlap.
LISA versus LIGO and Virgo
| Feature | LISA | LIGO/Virgo-type detectors |
|---|---|---|
| Location | Space, in a heliocentric orbit | On Earth |
| Architecture | Three spacecraft forming a triangular constellation | Ground-based laser interferometers |
| Arm scale | Approximately 2.5 million km | Much shorter terrestrial arms |
| Main frequency range | Low frequencies, roughly the millihertz band | Higher-frequency gravitational waves |
| Important targets | Massive black-hole mergers, compact binaries and extreme-mass-ratio inspirals | Many stellar-mass black-hole and neutron-star mergers |
| Primary advantage | Long baselines and freedom from terrestrial seismic noise | Already operating and sensitive to rapid, high-frequency events |
LISA will not replace LIGO or Virgo. The observatories will cover different frequency ranges and source populations. Together, space- and ground-based detectors can provide a much broader view of the gravitational-wave Universe.
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The mission’s science depends on an engineering chain in which every component must remain extraordinarily stable:
- Near-perfect free fall: the proof masses must be protected from non-gravitational disturbances.
- Drag-free control: spacecraft must follow the test masses without disturbing them.
- Laser stability: laser frequency and phase must be controlled precisely across millions of kilometres.
- Long-distance optical links: the spacecraft must exchange and measure laser signals across the constellation.
- Pointing and alignment: telescopes must remain accurately aimed despite formation motion and thermal changes.
- Charge management: ultraviolet systems and other controls must prevent electrostatic charge from affecting the proof masses.
- Data analysis: measurements from all three spacecraft must be combined to distinguish gravitational waves from instrument noise and overlapping sources.
NASA says its laser systems are being developed for picometer-level control of the laser frequency reference, and that each spacecraft is expected to carry six laser heads. Thales Alenia Space says the six telescopes will use Zerodur and require picometer-level stability.
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Who is building LISA?
ESA leads the mission and is responsible for the spacecraft programme, launch, mission operations and data handling. OHB System AG leads the industrial spacecraft implementation and assembly.
Thales Alenia Space is part of the industrial core team and is responsible for major spacecraft and telescope-related elements. NASA contributes laser systems, telescopes, charge-management devices, data-analysis systems and engineering expertise. ESA member states and the international LISA Consortium provide additional hardware, scientific planning and research participation.
NASA is therefore a major partner, but describing NASA as the organisation building or leading LISA would be inaccurate. The mission is ESA-led and internationally developed.
LISA’s development timeline
- 2017: LISA was selected as ESA’s third large-class Cosmic Vision mission.
- January 25, 2024: ESA formally adopted the mission.
- June 17, 2025: ESA and OHB signed the agreement that began industrial development and spacecraft construction.
- January 2026: NASA reported testing of a second early laser-frequency-reference prototype.
- May 5, 2026: Thales Alenia Space announced ESA’s Phase 1 contract for development of LISA’s six telescopes.
- 2035: Current planned launch target on Ariane 6 from French Guiana.
What “surfing gravitational waves” really means
The phrase is useful as a metaphor, but LISA will not ride a wave like a spacecraft riding ocean surf. It will measure how gravitational waves alter the geometry between freely falling reference masses.
Nor is LISA the first gravitational-wave detector. LIGO and other ground-based observatories have already detected gravitational waves. LISA’s distinction is that it is intended to be the first dedicated gravitational-wave observatory in space, opening the low-frequency millihertz window.
If development, testing and launch proceed as planned, LISA will add a new observational channel to astronomy. Its three spacecraft will listen for signals from massive black holes, compact binaries and possibly the early universe—sources that ground-based detectors cannot adequately study from Earth.
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