Apulsar timing array (PTA) is a set ofgalacticpulsars that is monitored and analyzed to search for correlated signatures in the pulse arrival times on Earth. As such, they are galactic-sized detectors. Although there are many applications for pulsar timing arrays, the best known is the use of an array ofmillisecond pulsars to detect and analyse long-wavelength (i.e., low-frequency)gravitational wave background. Such a detection would entail a detailed measurement of agravitational wave (GW) signature, like the GW-inducedquadrupolar correlation^[1] between arrival times of pulses emitted by different millisecond pulsar pairings that depends only on the pairings' angular separations in the sky. Larger arrays may be better for GW detection because the quadrupolar spatial correlations induced by GWs can be better sampled by many more pulsar pairings. With such a GW detection, millisecond pulsar timing arrays would open a new low-frequency window ingravitational-wave astronomy to peer into potential ancientastrophysical sources andearly Universe processes, inaccessible by any other means.^[2][3]

The proposal to usepulsars asgravitational wave (GW) detectors was originally made byMikhail Sazhin^[4] andSteven Detweiler^[5] in the late 1970s. The idea is to treat theSolar Systembarycenter and a galactic pulsar as opposite ends of an imaginary arm in space. The pulsar acts as the reference clock at one end of the arm sending out regular signals which are monitored by an observer on Earth. The effect of a passing long-wavelength GW would be to perturb the galacticspacetime and cause a small change in the observed time of arrival of the pulses.^{[6]: 207–209}

In 1983, Hellings and Downs^[7] extended this idea to an array of pulsars and found that astochastic background of GWs would produce a distinctive GW signature: a quadrupolar and higher multipolar spatial correlation between arrival times of pulses emitted by differentmillisecond pulsar pairings that depends only on the pairing'sangular separation in the sky as viewed from Earth (more precisely the solar system barycenter).^[8] The key property of a pulsar timing array is that the signal from a stochastic GW background will be correlated across the sightlines of pulsar pairs, while that from the other noise processes will not.^[9] In the literature, this spatial correlation curve is called theHellings-Downs curve or the overlap reduction function.^[10]

The Hellings and Downs work was limited in sensitivity by the precision and stability of the pulsar clocks in the array. Following the discovery of the more stable millisecond pulsar in 1982, Foster andBacker^[11] improved the sensitivity to GWs by applying in 1990 the Hellings-Downs analysis to an array of highly stable millisecond pulsars and initiated a 'pulsar timing array program' to observe three pulsars using theNational Radio Astronomy Observatory 43 m telescope.

Millisecond pulsars are used because they are not prone to thestarquakes andglitches,^[12] accretion events or stochastic timing noise^[13] which can affect the period of slower classical pulsars. Millisecond pulsars have a stability comparable toatomic-clock-based time standards when averaged over decades.^[14]

One influence on these propagation properties are low-frequency GWs, with a frequency of 10⁻⁹ to 10⁻⁶hertz; the most likely astrophysical sources of such GWs are supermassiveblack hole binaries in the centres ofmerging galaxies, where tens of millions ofsolar masses are in orbit with a period between months and a few years.

GWs cause the time of arrival of the pulses to vary by a few tens of nanoseconds over their wavelength (so, for a frequency of 3 x 10⁻⁸ Hz, one cycle per year, one would find that pulses arrive 20 ns early in July and 20 ns late in January). This is a delicate experiment, although millisecond pulsars are stable enough clocks that the time of arrival of the pulses can be predicted to the required accuracy; the experiments use collections of 20 to 50 pulsars to account fordispersion effects in the atmosphere and in the space between the observer and the pulsar. It is necessary to monitor each pulsar roughly once a week; a higher cadence of observation would allow the detection of higher-frequency GWs, but it is unclear whether there would be loud enough astrophysical sources at such frequencies.

It is not possible to get accurate sky locations for the sources by this method, as analysing timings for twenty pulsars would produce a region of uncertainty of 100 square degrees – a patch of sky about the size of the constellationScutum which would contain at least thousands of merging galaxies.

The main goal of PTAs is measuring the amplitude of background GWs, possibly caused by a history of supermassiveblack hole mergers. The amplitudes can describe the history of how galaxies were formed. The bound on the amplitude of the background waves is called an upper limit. The amplitude of the GW background is less than the upper limit.

Some supermassive black hole binaries may form a stable binary and only merge after many times the current age of the universe. This is called thefinal parsec problem. It is unclear how supermassive black holes approach each other at this distance.

While supermassive black hole binaries are the most likely source of very low frequency GWs, other sources could generate the waves, such ascosmic strings, which may have formed early in the history of the universe. When cosmic strings interact, they can form loops that decay by radiating GWs.^[15][16]

Globally there are five active pulsar timing array projects. The first three projects (PPTA, EPTA, and NANOGrav) have begun collaborating under the title of theInternational Pulsar Timing Array project, InPTA became a member in 2021. Recently China has also become active although not a full member of IPTA yet.

1. TheParkes Pulsar Timing Array (PPTA) at theParkes radio-telescope has been collecting data since 2005.
2. TheEuropean Pulsar Timing Array (EPTA) has been collecting data since 2009; it uses the five largest radio telescopes in Europe:
   • Lovell Telescope
   • Westerbork Synthesis Radio Telescope
   • Effelsberg Telescope
   • Nancay Radio Telescope
   • Sardinia Radio Telescope.
3. TheNorth American Nanohertz Observatory for Gravitational Waves (NANOGrav) uses data, collected since 2005, from theArecibo andGreen Bank radio telescopes.
4. TheIndian Pulsar Timing Array (InPTA) uses the upgradedGiant Metrewave Radio Telescope.^[17][18]
5. The Chinese Pulsar Timing Array (CPTA) uses theFive-hundred-meter Aperture Spherical radio Telescope (FAST).^[19]
6. The MeerKAT Pulsar Timing Array (MPTA), part of MeerTime, aMeerKAT Large Survey Project. The MPTA aims to precisely measure pulse arrival times from an ensemble of 88 pulsars visible from the Southern hemisphere, with the goal of contributing to the search, detection, and study of nanohertz-frequency gravitational waves as part of theInternational Pulsar Timing Array.

In 2020, the NANOGrav collaboration presented the 12.5-year data release, which included strong evidence for a power-law stochastic process with common strain amplitude and spectral index across all pulsars, but statistically inconclusive data for the critical Hellings-Downs quadrupolar spatial correlation.^[22][23]

In June 2023,NANOGrav,EPTA, PPTA, and InPTA announced that they found evidence for agravitational wave background. NANOGrav's 15-year data on 68 pulsars provided a measurement of the distinctive Hellings-Downs curve, a tell-tale quadrupolar signature of gravitational waves.^[24]Simultaneously, similar results were published by European Pulsar Timing Array, who claimed a${\displaystyle 3\sigma }$-significance, the standard for evidence. They expect that a${\displaystyle 5\sigma }$-significance, the standard for detection, would be achieved around 2025 by combining the measurements of several collaborations.^[25][26]Also in June 2023, the Chinese Pulsar Timing Array (CPTA) reported similar findings with a${\displaystyle 4.6\sigma }$-significance; they monitored 57 millisecond pulsars over just 41 months, taking advantage of the high sensitivity ofFAST, the world's largest radio telescope.^[27][28] Four independent collaborations reporting similar results provided cross validation of the evidence for GWB using different telescopes, different arrays of pulsars, and different analysis methods.^[29] The sources of the gravitational-wave background can not be identified without further observations and analyses, although binaries ofsupermassive black holes are leading candidates.^[3]

• Gravitational-wave observatory

• G. Hobbs; et al. (2010). "The International Pulsar Timing Array project: using pulsars as a gravitational wave detector".Classical and Quantum Gravity.27 (8): 8.arXiv:0911.5206.Bibcode:2010CQGra..27h4013H.doi:10.1088/0264-9381/27/8/084013.S2CID 56073764.
• G. Hobbs (2011). "Pulsars as gravitational wave detectors".High-Energy Emission from Pulsars and their Systems. Astrophysics and Space Science Proceedings. Vol. 21. pp. 229–245.arXiv:1006.3969.Bibcode:2011ASSP...21..229H.doi:10.1007/978-3-642-17251-9_20.ISBN 978-3-642-17250-2.S2CID 119277779.

• Pulsar timing array simulatorSimPTA
• European Pulsar Timing Array
• North American Nanohertz Gravitational Wave Observatory (NANOGrav)

• Gravitational-wave astronomy

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