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LISA is a planned space-based gravitational-wave observatory, while LIGO, Virgo and KAGRA are ground-based interferometers. Their most important difference is the frequency range they can study. LISA is designed for much lower frequencies, opening a view of compact binaries and massive black-hole systems that terrestrial detectors cannot observe well.
LISA is not a larger LIGO placed in orbit. Three spacecraft will fly in a triangular formation, exchange laser beams across millions of kilometres and track changes between free-floating test masses. The result will complement, rather than replace, ground observatories and pulsar-timing experiments.
The short answer: different locations, scales and gravitational-wave frequencies
Gravitational waves are extremely small changes in spacetime produced by accelerating massive objects. No single observatory can detect every wave because different sources radiate at different frequencies. Detector size, location and environmental noise determine which part of that spectrum is practical to measure.
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LIGO, Virgo and KAGRA use laser interferometers on Earth. Their arms are several kilometres long, and their observing programs focus on higher-frequency signals such as mergers involving stellar-mass black holes and neutron stars. LISA will operate in space with three spacecraft separated by 2.5 million kilometres per side. Its planned science band is approximately 0.1 millihertz to 0.1 hertz, well below the frequencies targeted by terrestrial facilities.
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That lower-frequency window changes the astronomy. LISA is intended to study compact binaries, including white-dwarf systems, and mergers of massive black holes. In some cases it could observe an inspiral before a later merger becomes visible to a ground detector, allowing the same cosmic event to be followed at different stages.
What LISA is and how its constellation is arranged
Three spacecraft form one giant triangular detector
ESA describes LISA as three spacecraft trailing Earth in its orbit around the Sun. The spacecraft form a triangle, with a planned 2.5-million-kilometre separation along each side. The formation is not an incidental arrangement: the long, changing laser links between spacecraft are the detector.
Each spacecraft carries free-floating test masses. Laser interferometry monitors the relative motion of those masses across the spacecraft-to-spacecraft links. A passing gravitational wave changes the measured separations by an extraordinarily small amount. Scientists look for the characteristic, correlated pattern in the laser measurements rather than treating any single distance change as a detection.
Why this is not an orbital version of LIGO
A terrestrial interferometer has two arms extending from a central facility. LISA has three independent spacecraft and no central, rigid tunnel connecting them. The spacecraft must maintain the constellation while the test masses provide the near-inertial references used for the measurement.
The millions-of-kilometres scale also changes the measurement problem. LISA needs precision laser links over vast distances and a data-analysis system suited to a moving constellation. Simply enlarging a ground detector would not reproduce those conditions, and putting a conventional terrestrial instrument in orbit would not provide LISA’s three-spacecraft geometry.
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Frequency range: the key reason LISA complements LIGO
What 0.1 millihertz to 0.1 hertz means
ESA’s LISA Science Team gives an approximate design band of 0.1 millihertz to 0.1 hertz. In ordinary units, that is 0.0001 to 0.1 cycles per second. A 0.1-millihertz wave changes on a timescale of roughly 10,000 seconds, while a 0.1-hertz wave has a period of about 10 seconds. The figures describe the intended science range, not a measured on-orbit sensitivity curve; the mission has not yet launched.
Ground interferometers are constrained to higher-frequency signals by the terrestrial environment and by the practical length of their arms. LISA’s location and much longer baselines make lower-frequency measurements feasible. The two approaches therefore observe different portions of the gravitational-wave spectrum.
Why frequency identifies different sources
A gravitational-wave frequency is related to the orbital motion of the emitting system. Widely separated or very massive objects can radiate at lower frequencies than compact objects completing their final orbits. As a result, moving to lower frequencies does not merely make the same catalog of events easier to see; it adds source classes and earlier evolutionary stages.
- Compact binaries: LISA is designed to observe systems such as binaries containing white dwarfs. Some of these systems emit persistently in the low-frequency band.
- Massive black-hole systems: Their inspiral and merger signals are among LISA’s central science targets and occur at frequencies below the range where terrestrial instruments are most effective.
- Earlier inspiral stages: For some systems that later produce a ground-detectable merger, LISA may provide information about the preceding low-frequency phase. This is a conditional complement, not a promise that every LISA source will later be seen by LIGO, Virgo or KAGRA.
LISA compared with LIGO, Virgo and KAGRA
The following comparison uses ESA’s descriptions. Exact sensitivity, observing schedules and operating configurations for the ground facilities can change between observing runs, so the table does not assign them a single permanent frequency cutoff.
| Feature | LISA | LIGO, Virgo and KAGRA |
|---|---|---|
| Location | Three spacecraft in a heliocentric orbit, trailing Earth around the Sun | Ground-based interferometers on Earth |
| Detector geometry | Three spacecraft arranged as a triangle | Interferometer arms extending from terrestrial facilities |
| Baseline | 2.5 million km planned for each side of the triangle | Arms measured in several kilometres, according to ESA’s detector overview |
| Main frequency distinction | Approximately 0.1 mHz–0.1 Hz; lower frequencies than terrestrial observatories | Higher-frequency signals accessible from Earth; facility-specific limits vary and are not fixed here |
| Representative science | Compact binaries, white-dwarf systems and massive black-hole systems | Stellar-mass black-hole and neutron-star mergers, among other ground-accessible sources |
| Status | Under construction; launch currently planned for 2035 | Operating observatories whose sensitivity and schedules depend on the observing run |
The practical distinction is coverage, not a contest to identify one “best” detector. A source may be invisible to a ground instrument because its signal is too slow, while a different source may change too rapidly for LISA’s primary band. Using both types of observatory produces a more complete record of how a system evolves.
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How LISA will measure a gravitational wave
- Maintain the constellation: The three spacecraft fly in a controlled heliocentric formation with million-kilometre separations.
- Use free-floating references: Each spacecraft carries test masses intended to provide the inertial references for the measurement. The spacecraft and the test masses are not treated as one rigid object.
- Exchange laser signals: Lasers travel between spacecraft along the three sides of the triangle. Interferometry compares the returning and outgoing light to determine minute changes in separation.
- Record time-dependent changes: A gravitational wave alters the relative distances in a specific pattern. The instruments continuously monitor those changes rather than taking occasional snapshots.
- Combine the links in analysis: Researchers combine measurements from the constellation to distinguish a gravitational-wave signal from instrument noise and other disturbances, then infer properties of the source.
This arrangement makes the constellation itself part of the observatory. The long arms provide the response needed for low-frequency waves, while the triangular network supplies multiple laser links for reconstructing the signal.
Why LISA has to be in space
Earth is a noisy environment for low-frequency measurements
Seismic motion, human activity, weather and changes in local gravity all disturb instruments on the ground. Terrestrial interferometers use extensive isolation and control systems, but those measures cannot remove every disturbance at very low frequencies. Earth-based facilities also cannot make their arms millions of kilometres long.
In space, LISA can place its test masses and laser links far from most of those local disturbances. The trade-off is substantial engineering complexity: the spacecraft must fly in formation, keep the optical links aligned over enormous distances and control the spacecraft without contaminating the free-falling references.
Longer does not mean automatically more sensitive
It is tempting to describe LISA as a scaled-up interferometer, but baseline length alone does not determine performance. Laser stability, test-mass control, spacecraft motion, instrument noise and data analysis all matter. The 2.5-million-kilometre design is valuable because it shifts the detector’s response toward lower frequencies; it is not a guarantee that every tiny disturbance will be measurable.
What LISA may observe that ground detectors cannot
Long-lived compact binaries
Many compact binaries orbit slowly enough to remain in LISA’s frequency range. White-dwarf binaries are an important example. Their signals can provide information about binary populations and the behavior of compact stellar remnants that are not accessible through the brief, high-frequency merger signals emphasized by ground detectors.
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Massive black-hole mergers
Systems containing massive black holes radiate at frequencies suited to LISA’s design. Observing their inspiral and merger would probe the assembly of black holes and galaxies across cosmic history. ESA’s mission description emphasizes that LISA could investigate events at a different scale from those seen by terrestrial observatories.
Signals before a possible ground-based merger
Some binaries can pass through LISA’s low-frequency band before their final, faster evolution reaches a ground detector’s range. If both observations are possible, the earlier LISA measurement and the later terrestrial measurement would be complementary views of one system. Whether a particular source follows this path depends on its masses, orbit and distance.
Independent reader supportYour contribution helps us test, update, and keep practical guides available for everyone.“From its vantage point in space, LISA will capture gravitational waves of lower frequencies than is possible from Earth, uncovering events of a different scale – all the way back to the dawn of time.”
— Carole Mundell, ESA Director of Science, in ESA’s June 2025 construction announcement
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Where other gravitational-wave methods fit
LISA and ground interferometers are only two parts of a broader network. ESA also identifies pulsar timing arrays as complementary gravitational-wave experiments. Instead of exchanging laser beams between spacecraft or along terrestrial arms, pulsar-timing projects monitor highly regular radio pulses from many neutron stars and search for correlated shifts in their arrival times.
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The three approaches cover different frequency regimes and source populations. Pulsar timing arrays extend the search toward still slower variations, ground interferometers cover higher-frequency events, and LISA is designed for the low-frequency space between those approaches. The combined network is more informative than any one facility operating alone.
LISA’s current status and mission plan
Construction and launch target
In June 2025, ESA announced that it had signed an agreement with OHB System AG to build the LISA spacecraft. Industrial development and construction were scheduled to begin under that agreement. ESA currently plans to launch LISA in 2035 on Ariane 6.
“Planned for 2035” is a schedule, not a completed launch or a guarantee. Space missions can change dates as design, testing, launch-vehicle availability and funding decisions evolve. LISA’s frequency band and science goals should therefore be understood as mission design objectives until the observatory is operating.
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ESA’s factsheet gives LISA a nominal four-year mission lifetime, with the possibility of a six-year extension. The extension is contingent on the spacecraft’s condition, available resources and mission decisions; it should not be treated as a guaranteed ten-year operating period.
Common misconceptions about LISA and LIGO
- “LISA replaces LIGO.” No. LISA targets lower frequencies, while LIGO and other ground facilities observe higher-frequency signals. Their science is complementary.
- “LISA is one enormous laser tube.” No. It is a constellation of three spacecraft linked by laser measurements across space.
- “The 0.1 mHz–0.1 Hz figures are guaranteed performance.” No. They are ESA’s approximate planned science band, not an on-orbit sensitivity measurement.
- “Every LISA source will later be seen from Earth.” No. Only some systems may evolve into a later ground-observable phase; many low-frequency sources are not expected to produce a corresponding terrestrial detection.
- “A 2035 launch means LISA is already collecting data.” No. The mission is under construction and has a current launch plan, but it is not yet an operating observatory.
What the difference means for gravitational-wave astronomy
LISA expands the observable spectrum rather than competing for the same events. Its space-based triangle and million-kilometre baselines are designed to reveal slow, low-frequency waves from compact binaries and massive black-hole systems. Ground observatories retain their role in detecting faster signals from sources such as stellar-mass black-hole and neutron-star mergers.
When observations overlap, the payoff is evolutionary context: one facility can measure an earlier inspiral while another measures a later, faster phase. When they do not overlap, each observatory contributes source populations the others cannot reach. That division of labor is why ESA presents LISA, terrestrial interferometers and pulsar timing arrays as a coordinated gravitational-wave observatory network.
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