Milestones in the Pulsar Literature

Maximum mass of a white dwarf.

Chadwick established the neutron as a fundamental particle. This made neutron stars physically plausible and provided the constituent particle implied by their name.

Jansky identified extraterrestrial radio emission from the direction of the Galactic centre. This opened the observing domain in which pulsars would later be discovered.

Baade and Zwicky explicitly proposed that supernovae produce neutron stars. This was the first direct astrophysical prediction of the objects later identified observationally as pulsars.

Oppenheimer and Volkoff derived hydrostatic equilibrium for a relativistic star made of neutron matter. The resulting Tolman-Oppenheimer-Volkoff framework remains the standard basis of neutron-star mass-radius calculations.

Alfvén introduced waves carried by magnetic tension in conducting plasma. Magnetohydrodynamics and Alfvénic disturbances are fundamental to pulsar magnetospheres, winds, current systems and nebulae.

Dicke developed switched microwave radiometry and quantified receiver-noise sensitivity. The radiometer equation remains basic to pulsar detectability, telescope sensitivity and observing-time estimates.

Ryle and Vonberg demonstrated astronomical radio interferometry. Its descendants provide pulsar positions, proper motions, parallaxes, scattering images and associations with nebulae or binaries.

Radio detection of the neutral-hydrogen line enabled mapping of Galactic gas and kinematics. H I absorption and emission remain useful for constraining pulsar distances and line-of-sight environments.

A signal acquires an additional propagation delay while traversing a companion's gravitational potential. In binary-pulsar timing, its range and shape constrain the companion mass and orbital inclination, enabling strong-field tests of gravity.

Hewish, Scott and Wills established interplanetary scintillation as a probe of compact radio sources. The Cambridge scintillation survey and its chart records directly created the observational route to pulsar discovery.

Reconstructs polarized emission as a function of Faraday depth from complex polarization across wavelength squared. It resolves multiple magneto-ionic components and avoids the ambiguities that limit straight position-angle fits.

Pacini proposed that a rapidly rotating, strongly magnetized neutron star could power the Crab Nebula. This was the key theoretical precursor immediately before pulsars were recognized.

Jocelyn Bell Burnell identified the first regularly pulsing celestial radio source in Cambridge interplanetary-scintillation records in August 1967. The discovery paper was published in 1968 and established the observational existence of pulsars. In 1974, Antony Hewish received half of the Nobel Prize in Physics for his decisive role in the discovery of pulsars.

Simplest model to explain observed scattering and scintillation in pulsars

Gold and Pacini independently argued that pulsars are rotating neutron stars, establishing the physical interpretation of pulsars soon after their discovery.

Fast Folding Algorithm

Rotating Vector Model

A rotating magnetized neutron star establishes a charge-filled, approximately corotating magnetosphere with a characteristic Goldreich-Julian charge density. Open field lines support currents, particle acceleration, a relativistic wind and electromagnetic spin-down.

The Vela pulsar underwent an abrupt fractional decrease in its rotation period of approximately two parts per million between 24 February and 3 March 1969, revealing the first observed pulsar glitch. An independent detection by Reichley and Downs was published in the same issue of Nature, making the observational priority effectively simultaneous.

The Crab Pulsar, PSR B0531+21, was discovered and strongly linked pulsars to supernova remnants.

Spin and orbital period change due to the pulsar transverse velocity

Pulse width and the separation of profile components systematically increase at lower observing frequencies. Komesaroff proposed this as a consequence of higher-frequency emission being produced closer to the neutron-star surface than lower-frequency emission; this became known as radius-to-frequency mapping.

A search of the galactic plane for high dispersion pulsars (31 new pulsars)

Cen X-3 was discovered as an X-ray pulsar, showing that pulsars can emit strongly at X-ray wavelengths.

Minimum spin period reachable through Eddington-limited accretion onto a neutron star.

The galactic distribution of pulsars (39 new pulsars)

Broadband measurements showed that steep pulsar radio spectra can flatten or turn over toward low frequencies instead of following one power law. Such departures constrain intrinsic emission and propagation or absorption while informing low-frequency survey design.

Orthogonal Polarization Modes

Assuming general relativity, microscopic stability and causality, and an equation of state known below a fiducial matching density, Rhoades and Ruffini proved that the largest mass is obtained by adopting the maximally stiff causal equation of state at higher densities. They derived an absolute upper limit of approximately 3.2 M_☉, establishing a robust mass ceiling for distinguishing neutron stars from black holes.

Joseph Taylor and Russell Hulse discovered PSR B1913+16, the first binary pulsar. Its orbital decay provided indirect evidence for gravitational waves, and the discovery led to the 1993 Nobel Prize in Physics.

Anderson and Itoh proposed that pulsar glitches and rotational irregularities arise from the irregular motion of quantized vortices through the neutron superfluid in the stellar crust. Their work established superfluid vortex dynamics as the foundation of modern glitch theory, including models involving vortex pinning, collective unpinning, and angular-momentum transfer to the crust.

A deep sample of new pulsars and their spatial extent in the Galaxy (40 new pulsars)

The Ruderman-Sutherland model introduced an inner polar gap above the neutron-star magnetic pole, where intense electric fields accelerate particles to ultra-relativistic speeds; it became a foundational framework for coherent radio emission and drifting subpulses.

Technique for completely removing intra-channel dispersive smearing.

Early binary-pulsar timing model for Keplerian orbits and relativistic timing effects.

Manchester and Lyne proposed that interpulses can represent emission from the extreme edges of a single wide beam.

The second Molonglo pulsar survey.

The SCLF polar-cap model assumes charges freely escape the stellar surface; acceleration occurs because the relativistic plasma flow cannot adjust its charge density quickly enough to match the changing geometry of curved magnetic field lines.

Using modern nuclear equations of state regarded as reliable to 2ρ_sat and a maximally stiff causal continuation at higher densities, Kalogera and Baym derived a secure upper bound of 2.9 M_☉. They showed that reducing this ceiling to 2.2 M_☉ would require reliable knowledge of neutron matter to approximately 4ρ_sat.

How millisecond pulsars form

PSR B1937+21, the first millisecond pulsar, has a rotation period of about 1.6 ms.

Prediction of the expected cross-correlation of the residuals of pulsars in various sky positions

Pair-production thresholds define boundaries in the period-period-derivative plane beyond which polar-cap discharges cannot sustain ordinary radio emission. Model and geometry dependence broaden these boundaries into a death valley rather than a universal sharp line.

The original slot gap model recognized that near the edge of the open field-line region the accelerating potential drops to zero, delaying pair production to higher altitudes and leaving a narrow unscreened acceleration slot.

PSR B0529-66 was discovered in the Large Magellanic Cloud, extending pulsar studies beyond the Milky Way.

Equation that describes telescope sensitivity for pulsar searches and observations.

Theory-independent binary model (good for testing theories of gravity)

The Damour-Deruelle framework separates Keplerian elements from measurable post-Keplerian effects such as periastron advance, Einstein delay, Shapiro delay and orbital decay. Intersecting their mass constraints provides theory-independent strong-field tests.

I - Morphological taxonomy
II - On the Spectral Behavior of Component Width
III - Mode changing, drifting subpulses, and pulse nulling
IV - Geometry of the core emission region
V - On the circular polarization in pulsar radiation
VI - The geometry of the conal emission region
VII - On the Spectral Behavior of Conal Beam Radii and Emission Heights
VIII - Subbeam Circulation and the Polarization-Modal Structure of Conal Beams
IX - On the Peculiar Properties and Geometric Regularity of Lyne and Manchester's "Partial Cone" Pulsars
X - On the Precursor and Postcursor Emission
XI - Understanding the Orientations of Pulsar Radiation and Supernova "Kicks"

The classic outer gap model places a vacuum gap near the null charge surface, sustained by gamma-ray photon collisions rather than strong magnetic fields.

On the detectability of pulsars in close binary systems

Fourier-domain profile cross-correlation for time-of-arrival extraction

Duncan and Thompson proposed that a newborn neutron-star dynamo could generate magnetic fields of 10¹⁴-10¹⁵ gauss, coining the magnetar class. The work established magnetic energy as a reservoir for high-energy transients; it was a theoretical prediction rather than an observational discovery.

The B1257+12 planetary system, discovered by Aleksander Wolszczan and Dale Frail at Arecibo from observations made in 1990, contains two Earth-mass planets and one lunar-mass planet. It was the first extrasolar planetary system to be discovered.

Frequency-resolved template portraits model intrinsic profile evolution across wide observing bands and jointly estimate pulse phase and dispersion measure. This reduces frequency-dependent timing bias and improves precision over conventional one-dimensional templates.

Population patterns in profile widths were used to reconstruct the radio beam across magnetic colatitude. Preferred angular scales supported a core-and-nested-cone geometry and linked observed pulse morphology to viewing angle and spin period.

B1620-26 is a pulsar, white dwarf, and Jupiter-mass planet system identified by Stephen Thorsett and collaborators in the globular cluster M4, highlighting the rich variety of evolutionary scenarios possible in globular clusters.

Parallactic changes in viewing geometry modulate the apparent projected semimajor axis and longitude of periastron through Earth's annual motion and the pulsar's binary orbit. Measuring these terms can determine distance, orbital orientation and companion mass.

Extends the Damour-Deruelle binary model with Kopeikin's annual-orbital-parallax and proper-motion terms. Fitting these geometric signatures constrains the longitude of ascending node, orbital inclination and distance, giving a three-dimensional orbital solution.

A binary's transverse motion changes the line of sight and produces apparent secular variations in projected semimajor axis and longitude of periastron. These kinematic terms constrain orbital orientation and prevent geometric effects from being mistaken for intrinsic evolution.

IAU/IEEE definitions of the Stokes parameters.

The Princeton-Arecibo Declination-Strip Survey

The Parkes Southern Pulsar Survey

The extended outer gap model added special-relativistic geometry and radiation-reaction limits to reproduce wide, double-peaked gamma-ray pulse profiles.

The Green Bank Northern Sky Survey for fast pulsars.

I - High frequency data.

Coherent 401-hertz X-ray pulsations from SAX J1808.4-3658 demonstrated that an accreting neutron star can rotate at millisecond periods. The discovery supplied the direct evolutionary link between low-mass X-ray binaries and recycled millisecond radio pulsars.

A compilation of 281 pulsars found that most spectra above 100 megahertz follow a single steep power law with mean spectral index about -1.8. Broken, flat and gigahertz-turnover spectra are uncommon but provide important constraints on emission and survey selection.

I - Spectra, Pulse Shapes, and the Beaming Fraction
II - Polarimetry
III - From Low to High Frequencies

Detailed non-conservative low-mass X-ray binary calculations established the relation between final orbital period and helium-white-dwarf mass. The relation is a key diagnostic of stable mass transfer and the recycling history of wide binary millisecond pulsars.

Treating the Stokes parameters as a four-vector yields an invariant-interval pulse profile that is unchanged by non-depolarizing instrumental transformations. Timing this profile suppresses systematic errors from imperfect polarimetric calibration, though often with reduced signal-to-noise ratio.

Intermediate-mass X-ray binary evolution produces recycled pulsars with carbon-oxygen or oxygen-neon-magnesium white-dwarf companions. Short, highly super-Eddington mass-transfer phases limit neutron-star accretion, explaining why these pulsars are generally less strongly recycled than helium-white-dwarf systems.

Simple Keplerian model suitable for very low eccentricities

The Parkes Multibeam Pulsar Survey

Pulsars discovered in the Small and Large Magellanic Clouds

Sideband searching and the ten-percent rule in the constant-acceleration approximation.

Electron Density model of the Milky Way

Comparing the observational predictions of rival beam geometries, the authors found pulse-width, component-location and frequency-evolution evidence broadly consistent with nested emission cones and generally inconsistent with randomly distributed patches.

Arecibo 430 MHz Intermediate Galactic Latitude Survey

Models for how massive-star core collapse forms neutron stars.

This slot gap model includes general-relativistic frame dragging, which strengthens the accelerating electric fields at high altitudes.

The TPC model treats high-energy emission as originating from thin ribbons along the last open magnetic field lines, extending from the neutron-star surface to the light cylinder at both magnetic poles.

PSR J0737-3039A/B, discovered in 2003, consists of a 22.7 ms pulsar in orbit around a 2.77 s pulsar. It is the first double neutron-star binary in which both components have been observed as radio pulsars, and it provides a unique laboratory for testing general relativity.

Calibration method based on multiple observations of a reference pulsar taken at many HA's

Empirical relation between dispersion measure and scattering timescale as a function of frequency.

The annular gap and inner annular gap models place acceleration in an annular region between the open field lines and the null charge surface, allowing geometries that can explain complex multi-peaked gamma-ray light curves.

The PSPC model applies to older or lower-energy pulsars where particles can be accelerated, but the magnetic field is too weak to trigger a screening cascade of electron-positron pairs, leaving the open volume starved and accelerating.

Technique that uses the full polarimetric information to extract times of arrival. Can also be used to calibrate data.

The High Time Resolution Survey - North

Arecibo Pulsar Survey Using ALFA

The Parkes High Latitude Pulsar Survey

XTE J1810-197 was detected as a transient, highly polarized radio pulsar with a flat spectrum and rapidly varying profile. It showed that magnetars can generate coherent radio emission and connected them observationally with the wider pulsar population.

Eleven sources were found through isolated dispersed bursts only 2-30 milliseconds long, with periodicities of 0.4-7 seconds in ten cases. Their extreme intermittency revealed a potentially large, previously missed Galactic neutron-star population.

Pioneering survey and research on single-pulse phenomenology, including drifting, nulling and modulation behaviour in radio pulsars.

PSR J1748-2446ad spins at 716 hertz, corresponding to a period of approximately 1.396 milliseconds. Its extreme rotation sets an observational lower bound on the neutron-star centrifugal break-up limit and constrains allowed mass-radius relations.

Archival Parkes data revealed a 30-jansky dispersed burst lasting less than 5 milliseconds whose properties argued against a Galactic or Small Magellanic Cloud origin. The Lorimer Burst became the first reported fast radio burst and opened a new population of extragalactic millisecond transients as cosmological probes.

A changing free-electron column introduces chromatic timing delays much larger than signals sought by pulsar timing arrays. Multifrequency monitoring probes interstellar turbulence, astronomical-unit-scale gradients and the solar wind, while careful correction preserves achromatic gravitational-wave signatures.

Gigahertz-peaked-spectrum pulsars reach maximum flux near or above one gigahertz and have positive or flat low-frequency indices. Their association with dense environments, plus orbital spectral evolution, supports external free-free absorption as an important cause.

Blind periodicity searches with the Fermi Large Area Telescope discovered 16 gamma-ray pulsars without prior radio timing solutions. This demonstrated direct discovery through gamma-ray pulsations and revealed a population hidden from conventional radio-selected searches.

The Fermi Large Area Telescope detected strong gamma-ray pulsations from eight known millisecond pulsars, establishing recycled pulsars as a substantial high-energy source population. Their pulse profiles and spectra linked their emission physics to that of young gamma-ray pulsars and favoured emission far from the stellar surface.

Sixteen millisecond-duration swept-frequency pulses resembled the Lorimer Burst but were detected through a Parkes sidelobe and shown to be terrestrial. They established a critical radio-frequency-interference class that fast-transient searches must distinguish from genuinely dispersed extragalactic bursts.

Orbital Doppler modulation spreads a pulsar's Fourier power and can substantially reduce search sensitivity, especially for compact systems with massive companions. Calculations for arbitrary eccentricity show that acceleration and acceleration-jerk searches can recover much of this loss.

Defines the electromagnetic-wave, Stokes-parameter and receptor-basis conventions implemented by PSRCHIVE and PSRFITS, and contrasts them with International Astronomical Union and engineering definitions. Explicit convention tracking prevents handedness and Stokes-sign errors between instruments and software.

The separatrix layer model uses force-free magnetospheres from simulations and restricts caustic emission to the layer near the current sheet along the boundary between closed and open field lines.

The striped wind current sheet model places caustic emission beyond the light cylinder, in the thin undulating current sheet embedded in the relativistic wind outside the magnetosphere.

Pulsar PSR J1823-3021A in NGC 6624

The High Time Resolution Survey - South

A snapshot survey detected 12 previously X-ray-undetected pulsars and placed deep limits on 11 more. The results exposed an intrinsic spread of over five orders of magnitude in non-thermal X-ray efficiency and evidence for a change in luminosity scaling with spin-down power.

Scoring, neural-network, image-recognition and streaming classifiers rank pulsar-like candidates amid overwhelming interference and noise. They retain high pulsar recall while reducing millions of candidates to a tractable set, making large modern surveys operationally feasible.

Calibration method based on a single observation of a reference pulsar

Arecibo All-sky 327 MHz Drift Pulsar Survey

The Green Bank Telescope 350 MHz Drift-scan survey

The Perseus Arm Pulsar Survey

The European Pulsar Timing Array and the Large European Array for Pulsars

The International Pulsar Timing Array

The North American Nanohertz Observatory for Gravitational Waves

The Parkes Pulsar Timing Array

Mass transfer to a compact companion can strip a helium star to a near-Chandrasekhar metal core before collapse, leaving only about 0.05-0.20 solar masses of ejecta. The resulting fast, faint explosion and potentially small natal kick provide a key route to compact double-neutron-star systems.

The Green Bank Northern Celestial Cap Pulsar Survey

The LOFAR pilot surveys for pulsars and fast radio transients

Pulsar plus stellar-mass black-hole binaries are a classic target for testing relativistic gravity. As of 2026, no secure Galactic radio pulsar plus stellar-mass black-hole binary has been established.

Via rotationally-delayed accretion-induced collapse (RDAIC)
Via the interaction of the binary with a circumstellar disk

More than 100 maser parallaxes and proper motions mapped spiral-arm segments and a nearly flat Galactic rotation curve. The resulting Galactic-centre distance and rotation speed improve pulsar distances, kinematic corrections and precision tests using binary orbital decay.

Frequency-Dependent Profile Evolution

Implements the Damour-Deruelle model with the Freire-Wex orthometric parametrization of Shapiro delay. Fitting the less-covariant orthometric amplitude and ratio improves companion-mass and inclination measurements, particularly when the traditional range and shape parameters are strongly correlated.

The GMRT High Resolution Southern Sky Survey for Pulsars and Transients

Multiwavelength Single Pulse Polarimetric Survey with GMRT.

The Large European Array for Pulsars

New Electron Density model of the Milky Way, refinement of NE2001

The SUrvey for Pulsars and Extragalactic Radio Bursts

An observation-constrained mass model combines stellar and gas discs, bulge and dark halo into a computable Galactic potential. It provides forces and orbit integrations needed to correct measured pulsar spin and binary-period derivatives for Galactic acceleration.

Evolution through a high-mass X-ray binary, common-envelope phase and Case BB mass transfer mildly recycles the first-born neutron star before an ultra-stripped second supernova forms the binary. The framework links component masses, spin, eccentricity and natal kicks to merger outcomes.

The LOFAR Tied-Array All-Sky Survey

The result shows that fast radio burst emission can survive propagation down to approximately 150 MHz. Strong universal low-frequency suppression by absorption or scattering is therefore disfavoured.

Timing a pulsar close to the Galactic centre black hole could measure relativistic precession, potentially black hole spin, and test the Kerr metric. There is a reported millisecond pulsar candidate near the Galactic centre in 2026, but not yet the clean, tightly orbiting pulsar.

No neutron star with spin less than 1 ms has been securely detected. Such a discovery would strongly constrain the neutron star EOS, maximum rotation rate, mass shedding and recycling physics.

Radio emission theory; pair plasma and pulsar magnetosphere model.

Classic synthesis of radio-wave propagation through the turbulent ionized interstellar medium.

ISM turbulence; electron-density fluctuation spectrum.

Pair cascades above polar caps; important for magnetospheric plasma production.

ISM plasma lensing; refractive caustics.

Major review of scintillation, scattering, angular broadening and pulse broadening.

Early Galactic free-electron model used for pulsar distances.

Taylor-Cordes electron-density model; standard before NE2001.

Evidence for a broad, approximately Kolmogorov spectrum of electron-density fluctuations.

Coherent curvature radiation by solitons in pulsar plasma.

Secondary-spectrum arcs as probes of scattering geometry and AU-scale interstellar structure.

Non-Gaussian scattering statistics for ISM propagation.

Coherent curvature radiation in pair plasma.

Scintillation arcs and AU-scale ISM structure.

Magnetospheric propagation effects on observed pulsar polarization.

Constraints on Galactic plasma lenses from an extreme scattering event.

Candidate explanation for coherent radio emission in pulsars.

Critical review of coherent curvature, plasma and anomalous Doppler emission models.

Soliton formation in hot streaming pair pulsar plasmas.

Tests plasma-lens morphology using pulsar scintillation parabolic arcs.

Galactic scattering distribution and the pulse-broadening versus dispersion-measure relation.

Physical model of scintillation arcs.

H II regions and anomalous pulsar DMs/scattering.

First optical pulsations from a pulsar; pulsars are multiwavelength emitters.

Evidence linking anomalous X-ray pulsars with soft gamma repeaters.

Observational link between a radio millisecond pulsar and an X-ray binary state.

A high-magnetic-field radio pulsar produced magnetar-like bursts and an outburst, including rotation-powered pulsar X-ray bursts.

PSR J0337+1715 is a millisecond pulsar orbited by two white-dwarf companions.

AR Scorpii has a white-dwarf spin period of about 117 seconds and a dominant beat period of about 118 seconds.

PSR J2007+2722 was discovered through Einstein@Home volunteer distributed computing.

PSR J1311-3430 is a black-widow binary found through a blind gamma-ray pulsation search.

Follow-up detections showed that a Galactic magnetar can emit radio bursts ranging from weak events to FRB-like energies, strongly supporting the magnetar-FRB connection.

PSR J0901-4046 has a spin period of 75.88 seconds, establishing that coherent radio emission can persist in the ultra-long-period regime. Its location beyond conventional death-line expectations challenges standard models of pulsar emission and neutron-star evolution.

H.E.S.S. detected a new pulsed gamma-ray component extending to at least 20 TeV, demonstrating extreme particle acceleration and challenging standard high-energy pulsar emission models.

First-principles plasma simulations produced self-consistent electric gaps, electron-positron discharges and escaping electromagnetic modes with properties relevant to pulsar radio emission.

Timing of PSR J0514-4002E revealed a compact companion with a mass between 2.09 and 2.71 solar masses at 95 percent confidence. Its location in the neutron-star-black-hole mass gap makes it either an unusually massive neutron star or a low-mass black hole, constraining compact-object formation and dense-matter limits.

LST-1 characterized the pulse peaks, bridge emission and phase-resolved spectrum from roughly 20 GeV to several hundred GeV, refining constraints on pulsar high-energy emission models.

Alpar and collaborators developed a quantitative theory in which thermally activated motion of pinned superfluid vortices governs interglitch evolution and post-glitch relaxation. Its application reproduced the complex recovery of the Vela pulsar and established vortex creep as a principal framework for interpreting pulsar timing after glitches.

Andersson and collaborators showed that crustal entrainment reduces the mobility, and hence the effective angular-momentum reservoir, of the inner-crust superfluid. Chamel subsequently demonstrated that this reservoir cannot readily account for Vela-sized glitches, implying the involvement of additional superfluid, plausibly extending into the neutron-star core.

The magnetar 1E 2259+586 exhibited the first clearly identified anti-glitch: an abrupt decrease in spin frequency accompanied by X-ray radiative changes and a substantial change in its spin-down rate. The event demonstrated that neutron-star rotational irregularities are not restricted to conventional spin-up glitches and challenged standard models of glitch dynamics.

Continuous single-pulse observations captured the 2016 Vela glitch as it occurred, revealing transient changes in pulse shape, polarisation, and arrival time. Subsequent analysis constrained the spin-up time to less than 12.6 seconds, detected a rapid rotational-frequency overshoot and relaxation, and found evidence of a brief pre-glitch slowdown, providing the first direct view of angular-momentum exchange on seconds-long timescales inside a neutron star.

A hidden Markov model tracks pulse frequency and its derivative while accounting explicitly for stochastic timing noise. Bayesian comparison of glitch and no-glitch models enables automated detection, objective false-alarm calibration, and systematic searches without relying on manual inspection of timing residuals.

The Ooty Radio Telescope pipeline processes incoming pulsar observations using data-quality checks, timing analysis, and statistical detection algorithms to issue real-time glitch alerts. Its deployment demonstrated how rapid detection can trigger higher-cadence observations of the otherwise poorly sampled early post-glitch recovery.

Flexible Image Transport System for Pulsar Observations

Planetary and lunar ephemerides used for barycentric corrections in precision pulsar timing.

Standardised integrated pulse profiles, downloadable in PSRFITS, text, and original formats.

Positions, spin parameters, binary parameters, distances, and bibliographic references for published pulsars.

A long-term catalogue of published pulsar glitches and events detected through Jodrell Bank monitoring. It records glitch epochs, fractional spin-frequency changes, and associated changes in spin-down rate, providing a major observational resource for population studies and tests of neutron-star interior models.

Published rotating radio transients and measured source properties.

Fermi LAT instrument, source catalogues, gamma-ray pulsars, timing solutions, and spectral properties.

The first Parkes Pulsar Timing Array release provides calibrated observations and timing products for 20 millisecond pulsars monitored in three radio bands. Its long, multifrequency baselines support dispersion correction, clock and ephemeris studies, and nanohertz gravitational-wave searches.

Public TOAs and timing models in TEMPO and TEMPO2 formats.

X-ray and gamma-ray pulsar catalogues, survey tables, and mission products.

Calibrated low-frequency profiles, dispersion measures, flux densities, and spectra for non-recycled pulsars.

High-precision timing for 42 millisecond pulsars combines European observations extending to mid-2014, with individual baselines of 7-18 years. The release supplies timing solutions, noise characterizations and measurements for pulsar astrophysics and gravitational-wave analyses.

The first International Pulsar Timing Array release combines European, North American and Parkes data for 49 millisecond pulsars, with some baselines approaching three decades. Its broader sky coverage and complementary observing systems establish the value and challenges of globally combined timing data.

Flux-calibrated profiles and measurements for millisecond pulsars at 110-188 MHz.

FRB detections, observed properties, and discovery metadata; relevant to pulsar and single-pulse pipelines.

Timing data and noise models for 65 millisecond pulsars.

Profiles, flux densities, and dispersion measures at approximately 25-80 MHz.

MeerKAT integrated profiles, polarimetry, rotation measures, and population measurements.

uGMRT timing data, TOAs, and timing models for InPTA millisecond pulsars.

uGMRT timing data, TOAs, and timing models for InPTA millisecond pulsars.

PSRFITS integrated profiles for MeerKAT-observed millisecond pulsars.

FAST timing data for the Chinese Pulsar Timing Array.

Up to 24.7 years of European PTA timing data, including combinations with InPTA DR1.

First 2.5 years of timing data for the MeerKAT Pulsar Timing Array.

Narrowband and wideband TOAs, timing models, noise files, and reproducibility software for 68 MSPs.

Database of the Multiwavelength Single Pulse Polarimetric Survey.

Search-mode single-pulse observations of 1,192 pulsars, typically containing roughly 1,000 consecutive pulses per source.

Observations, arrival-time measurements and analysis of 37 millisecond pulsars.

High-precision timing of 45 millisecond pulsars.

Narrowband timing data for 47 millisecond pulsars.

Wideband timing data for 47 millisecond pulsars.

Timing analysis for the Parkes Pulsar Timing Array second data release.

Timing data and noise models for the Parkes Pulsar Timing Array third data release.

Timing model and precision estimates; pulsar timing package.

Pulsar timing package.

Pulsar searching package; described in Scott Ransom's PhD thesis.

Time-domain pulsar searching package.

Pulsar archive data reduction and analysis package.

Suite of algorithms for statistical analysis, polarimetry, single pulses, and fluctuation spectra.

Bayesian pulsar timing and stochastic-noise analysis using TEMPO2 and MultiNest.

Folding and dedispersion package for pulsar data.

Python interface to the TEMPO2 timing engine.

Code for modelling the ionospheric contribution to the Rotation Measure

Automated ranking of pulsar-search candidates using heuristic candidate features.

Bayesian pulsar-timing-array analysis and gravitational-wave inference.

Bayesian PTA timing and gravitational-wave analysis.

Open-source Python package for pulsar population synthesis.

Image-based machine-learning classification of pulsar candidates.

Frequency-dependent pulse-profile modelling and wideband TOA and DM estimation.

Bayesian coherent multi-epoch pulsar searching package.

Python bindings for the SLALIB positional-astronomy library, used by pulsar tools.

Pulsar-search candidate management, inspection, and pipeline database system.

Fast Folding Algorithm pulsar searching package

GPU-accelerated dedispersion and single-pulse/transient search pipeline.

Pure-Python PSRFITS reading, pulsar profile analysis, scintillation, and timing tools.

GPU-accelerated Fourier Domain Acceleration Search

Bayesian pulsar timing, noise analysis, and nanohertz gravitational-wave inference.

Higher-level PTA models, frequentist statistics, and wrappers around ENTERPRISE.

Fast Folding Algorithm pulsar searching package

Python interface for downloading, querying, and manipulating the ATNF Pulsar Catalogue.

MPI-enabled parallel-tempering Markov-chain Monte Carlo sampler widely used by ENTERPRISE.

Versatile RFI mitigation tool by V. Morello.

PTA sensitivity-curve calculation and forecasting.

Trans-dimensional Bayesian searches for continuous gravitational waves in PTA data.

Bayesian search for gravitational-wave bursts and burst-with-memory signals in PTA data.

Rapid refitting and combination of PTA free-spectrum likelihoods.

Neural-network classification of dispersed fast-radio-burst and single-pulse candidates.

Fast Folding Algorithm pulsar searching package

uGMRT RFI filtering, bandshape correction, and data-quality analysis.

Modern pure-Python pulsar timing package; PINT is not TEMPO3.

InPTA/uGMRT data-reduction pipeline for RFI excision, dedispersion, and folding into PSRFITS.

Fourier-domain periodic RFI detection and excision, used by PINTA.

Candidate post-processing and machine-learning utilities used in modern surveys.

High-performance GPU pulsar searching, acceleration searching, and folding.

Bayesian pulsar timing and noise modelling written in Julia.

ENTERPRISE-based framework for new-physics searches using PTA likelihoods.

A program for planning observations of specific orbital phases of binary pulsars

Pulsar archive data reduction package

Automatic timing solution finder

C++/CUDA GPU pulsar searching library

Pulsar searching package - GPU accelerated

Pulsar archive data reduction package

Folding, dedispersion, subbanding, merging of PSRFITS files

Pulsar population synthesis

A program for computing rise/set times of pulsars

Orbital motion remover

Python-based pulsar search data manipulation package

Orbital phase search

Raw and processed Parkes, ASKAP, and ATCA observations after applicable proprietary periods.

Folded profiles for 1,271 pulsars, MSP census products, and public MeerTime releases.

Authors: D. R. Lorimer and Michael Kramer

Authors: Andrew Lyne and Francis Graham-Smith

Authors: James J. Condon and Scott M. Ransom

Authors: Geoff McNamara

Authors: Thomas L. Wilson, Kristen Rohlfs, and Susanne Hüttemeister

Authors: A. V. Gurevich, V. S. Beskin, and Ya. N. Istomin

Authors: George B. Rybicki and Alan P. Lightman

Authors: Stuart L. Shapiro and Saul A. Teukolsky

Authors: Norman K. Glendenning

Authors: P. Haensel, A. Y. Potekhin, and D. G. Yakovlev

Authors: Luciano Rezzolla, Pierre Pizzochero, David Ian Jones, Nanda Rea, and Isaac Vidaña

Converts uGMRT raw data files to SIGPROC filterbank format.

Python script that estimates the dispersion measure of wide-band pulsar data in PSRFITS format.