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An SKAO pulsar timing array of 174 millisecond pulsars can dominate international nanohertz gravitational-wave sensitivity within four years and resolve multiple continuous sources.

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2026-07-12 05:09 UTC pith:5YO7N4XE

load-bearing objection Solid, transparent SKAO PTA science-case update that turns MeerTime numbers into concrete 2030s forecasts; useful planning document, not a new result. the 2 major comments →

arxiv 2607.03059 v1 pith:5YO7N4XE submitted 2026-07-03 astro-ph.IM astro-ph.COastro-ph.HEgr-qc

The SKAO Pulsar Timing Array

Ryan M. Shannon , N. D. Ramesh Bhat , Aur\'elien Chalumeau , Siyuan Chen , H. Thankful Cromartie , A. Gopakumar , Kathrin Grunthal , Jeffrey S. Hazboun
show 17 more authors
Francesco Iraci Bhal Chandra Joshi Ryo Kato Michael J. Keith Kejia Lee Kuo Liu Hannah Middleton Matthew T. Miles Chiara M. F. Mingarelli Aditya Parthasarathy Daniel J. Reardon Golam M. Shaifullah Keitaro Takahashi Caterina Tiburzi Riccardo J. Truant Xiao Xue Andrew Zic
This is my paper
classification astro-ph.IM astro-ph.COastro-ph.HEgr-qc
keywords pulsar timing arraynanohertz gravitational wavesSKAOsupermassive black hole binariesgravitational-wave backgroundmillisecond pulsarsinterstellar mediumcontinuous gravitational waves
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This chapter argues that the Square Kilometre Array Observatory can host a practical pulsar timing array that turns recent hints of a nanohertz gravitational-wave background into confident detection and source characterization. Using MeerKAT-based timing data, the authors design a realistic campaign that times 174 southern millisecond pulsars to roughly one-microsecond precision every two weeks, taking advantage of sub-arrays and multi-band coverage. Forecasts show this array would outpace existing and planned experiments for a background of amplitude 2 imes10^{-15} within about four years and could resolve multiple continuous-wave signals after a decade or two. The same sensitivity enables maps of sky anisotropy, probes of early-universe processes, and multi-messenger follow-up once host galaxies are identified. The paper therefore frames the SKAO PTA as the southern pillar of 2030s nanohertz gravitational-wave astronomy.

Core claim

A carefully designed SKAO PTA using the AA4 (or AA*) configuration can time 174 known millisecond pulsars at two-week cadence with white-noise floors near 1 µs, delivering a signal-to-noise ratio for a gravitational-wave background of A_yr = 2 imes10^{-15} that dominates the International Pulsar Timing Array within four years and can resolve multiple continuous-wave supermassive black-hole binaries after 10–20 years of observation.

What carries the argument

Sensitivity scaling relations for stochastic backgrounds and continuous waves (Siemens et al. 2013 and extensions) applied to a concrete 174-pulsar array whose integration times and precisions are extrapolated from the MeerTime MSP census under the assumption that SKA-Mid is three-to-four times more sensitive than MeerKAT.

Load-bearing premise

The forecasts assume that SKA-Mid will deliver exactly the advertised three-to-four times sensitivity gain over MeerKAT and that the chosen 174 pulsars will reach the quoted white-noise floors without being limited by unmodeled red noise or scattering.

What would settle it

After four years of SKAO PTA operations, measure the array’s actual signal-to-noise ratio on a common red process of amplitude ~2 imes10^{-15}; if it remains well below the IPTA combined sensitivity, the claimed dominance fails.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • An SKAO PTA becomes the dominant southern contribution to any global nanohertz gravitational-wave data set by the early 2030s.
  • Multiple continuous-wave supermassive black-hole binaries become individually resolvable, enabling host-galaxy identification and multi-messenger follow-up.
  • Anisotropy maps of the nanohertz sky can reach multipoles high enough to cross-correlate with large-scale structure.
  • Wide-band SKA-Low plus SKA-Mid observations can separate chromatic interstellar and solar-wind delays from achromatic gravitational-wave signals at higher fidelity than present arrays.
  • Joint VLBI distances for a few key pulsars tighten continuous-wave localization by more than an order of magnitude near those pulsars.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the sensitivity forecasts hold, the SKAO PTA will set the practical timetable for the first confident multi-messenger nanohertz detections rather than merely adding data to northern arrays.
  • The same sub-array flexibility that optimizes white-noise floors also provides a natural path for real-time solar-wind and coronal-mass-ejection monitoring that benefits space-weather models.
  • Failure of the white-noise-floor assumption for even a modest fraction of the 174 pulsars would shift the optimal strategy toward fewer, better-timed sources, changing the claimed four-year dominance timeline.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 6 minor

Summary. This chapter motivates and designs a realistic SKAO Pulsar Timing Array for the 2030s. It reviews nanohertz GW signals (stochastic backgrounds, continuous waves, bursts, anisotropy maps, and ultra-low-frequency parameter drifts), their astrophysical and cosmological sources (SMBHBs and early-Universe processes), and the principal noise sources that must be mitigated. The core quantitative contribution is a concrete observing strategy based on the MeerTime MSP census: an AA4 array of 174 MSPs timed to ~1 µs at fortnightly cadence, using sub-arrays, is forecast to dominate IPTA GWB sensitivity within ~4 years for A_yr = 2e-15 and to resolve multiple continuous-wave sources after 10–20 years (Sections 6.1–6.2, Figures 3–5). Complementary roles for SKA-Low, VLBI pulsar distances, and high-energy timing are outlined, together with technical requirements and multi-facility synergies.

Significance. If the forecasts hold under realistic red-noise and scattering floors, the SKAO PTA becomes the dominant southern-hemisphere contributor to the IPTA and enables post-detection science (anisotropy maps, individual SMBHB characterization, multi-messenger follow-up) that current arrays cannot reach. The work is a transparent science-case chapter rather than a new detection claim: sensitivity curves reuse published formalisms (Siemens et al. 2013; Hazboun et al. 2019; Rosado et al. 2015) and an independent MeerTime census, with assumptions (SEFD factor 3–4, white-noise floors) stated explicitly. Strengths include the concrete 174-pulsar strategy, sub-array efficiency calculation, CGW population forecasts, and the local angular-resolution analysis (Grunthal et al. framework). These make the chapter a useful planning document for SKAO operations and IPTA coordination.

major comments (2)
  1. Section 6 (paragraph beginning “We assume that AA* is a factor of three…”): the SEFD improvement factors (3× for AA*, 4× for AA4 relative to MeerKAT) are taken from SKAO documentation without independent verification or a sensitivity study. Because the entire S/N forecast (Eqs. 13–14, Figures 3–5) scales with these factors, a short table or appendix showing how GWB S/N and CGW counts degrade if the realized gain is only 2–2.5× would make the central claim more robust for planning purposes.
  2. Section 6.1–6.2 and Figures 3–5: the forecasts adopt white-noise floors extrapolated from MeerTime and assume that multi-band mitigation (Sections 5.2, 7) fully removes chromatic red noise and scattering for the fainter, more distant MSPs that dominate the 174-pulsar sample. The text acknowledges that the campaign is “not fully optimized,” but does not quantify residual red-noise floors. A brief Monte-Carlo or scaling estimate of how residual spin/scattering noise at the level seen in current PTA MSPs would slow the S/N growth would strengthen the claim that SKAO dominates the IPTA within ~4 years.
minor comments (6)
  1. Figure 1 caption and surrounding text: the correlation coefficients are shown without error bars or a clear statement of which data release each curve uses; a one-sentence clarification would help non-PTA readers.
  2. Section 2.4: “Thsee approach” is a typographical error for “This approach.”
  3. Section 5.4: “erroswof” should be “errors of”; “non-orthogonaligies” should be “non-orthogonalities.”
  4. Section 6: the integration-time strategy (256 s MeerKAT-sized sub-array, up to 1300 s full array) is clear, but a short table listing the number of pulsars in each tier would make the 8.9 h / 12.4 h totals easier to verify.
  5. Section 8 / Figure 9: the VLBI distance precisions (0.37 pc, 1.7 pc) are taken from Kato & Takahashi (2026); a brief note on whether these are already demonstrated or projected would help the reader assess readiness.
  6. References: a few arXiv-only entries (e.g., 2025–2026 papers) will need updating to journal citations before final publication; this is expected for a 2026 chapter.

Circularity Check

0 steps flagged

No significant circularity: science-case forecasts use external formalisms, stated SEFD scalings, and an independent MeerTime census; self-citations are ordinary PTA literature, not load-bearing uniqueness claims.

full rationale

The paper is a strategic SKAO science-case chapter, not a first-principles derivation or a fit-then-predict exercise. Its central quantitative claims (Section 6, Figures 3–5) are transparent forecasts: an AA4 array of 174 MSPs timed to ~1 µs at fortnightly cadence reaches GWB S/N that dominates the IPTA within ~4 years for A_yr = 2e-15 and can resolve multiple CGWs after 10–20 years. The SEFD factors of 3–4 over MeerKAT, the 174-pulsar sample drawn from the MeerTime census (Spiewak et al. 2022), the Siemens/Hazboun sensitivity formalisms, and the input GWB amplitude taken from published multi-PTA results are all stated as external inputs or planning assumptions; the text explicitly notes the campaign is “not fully optimized.” No equation reduces a claimed prediction to a fitted parameter by construction, no uniqueness theorem is imported from the authors’ prior work to forbid alternatives, and no ansatz is smuggled in via self-citation. Ordinary self-citations of co-author PTA data releases and methods appear but do not force the forecasts. Circularity burden is therefore negligible.

Axiom & Free-Parameter Ledger

4 free parameters · 4 axioms · 0 invented entities

The central forecasts rest on a small set of domain assumptions about telescope performance and pulsar properties taken from SKAO documentation and the MeerTime census, plus standard PTA scaling relations. No new free parameters are fitted to data inside this paper; the GWB amplitude is an external input. No invented entities appear.

free parameters (4)
  • SEFD improvement factor (AA*/AA4 vs MeerKAT) = 3 (AA*), 4 (AA4)
    Taken as exactly 3× (AA*) and 4× (AA4) from SKAO performance documents; directly scales all timing-precision and S/N forecasts.
  • Number of MSPs in array = 174
    Fixed at 174 from the MeerTime census after applying a 2000 s integration-time cut; controls the N_psr scaling of S/N.
  • Target white-noise timing precision = 1 µs
    Set by hand to 1 µs as the inclusion threshold; determines which pulsars are observed and for how long.
  • GWB amplitude A_yr = 2e-15
    External input taken from recent PTA analyses; used as the signal strength for all S/N forecasts.
axioms (4)
  • domain assumption Siemens et al. (2013) weak- and strong-signal S/N scalings remain valid for the SKAO array configuration.
    Invoked throughout Section 6 to convert N_psr, cadence, and sigma into detection forecasts.
  • domain assumption MeerTime L-band timing precisions and spectral indices can be linearly extrapolated to SKA-Mid Band 2 and to AA4 sensitivity.
    Stated in Section 6; underpins the entire integration-time and sensitivity-curve calculation.
  • domain assumption Hellings-Downs correlations and the power-law GWB spectrum with alpha = -2/3 are the correct signal model for the dominant background.
    Used as the target signal in all sensitivity forecasts (Sections 2 and 6).
  • ad hoc to paper Sub-arraying with MeerKAT-sized sub-arrays incurs no additional calibration or beam-forming loss beyond the stated SEFD.
    Assumed when calculating the 2.8 h per-epoch saving; not independently verified in the text.

pith-pipeline@v1.1.0-grok45 · 49564 in / 2785 out tokens · 28259 ms · 2026-07-12T05:09:28.536588+00:00 · methodology

0 comments
read the original abstract

Pulsar timing arrays (PTAs) are ensembles of millisecond pulsars observed for years to decades. The primary goal of PTAs is to study gravitational-wave astronomy at nanohertz frequencies, with secondary goals of undertaking other fundamental tests of physics and astronomy. Recently, compelling evidence has emerged in established PTA experiments for the presence of a gravitational-wave background. To accelerate a confident detection of such a signal and then study gravitational-wave emitting sources, it is necessary to observe a larger number of millisecond pulsars to greater timing precision. The SKAO telescopes, which will be a factor of three to four greater in sensitivity compared to any other southern hemisphere facility, are poised to make such an impact. In this chapter, we motivate an SKAO pulsar timing array (SKAO PTA) experiment. We discuss the classes of gravitational waves present in PTA observations and how an SKAO PTA can detect and study them. We then describe the sources that can produce these signals. We discuss the astrophysical noise sources that must be mitigated to undertake the most sensitive searches. We then describe a realistic PTA experiment implemented with the SKA and place it in context alongside other PTA experiments likely ongoing in the 2030s. We describe the techniques necessary to search for gravitational waves in the SKAO PTA and motivate how very long baseline interferometry can improve the sensitivity of an SKAO PTA. The SKAO PTA will provide a view of the Universe complementary to those of the other large facilities of the 2030s.

Figures

Figures reproduced from arXiv: 2607.03059 by Aditya Parthasarathy, A. Gopakumar, Andrew Zic, Aur\'elien Chalumeau, Bhal Chandra Joshi, Caterina Tiburzi, Chiara M. F. Mingarelli, Daniel J. Reardon, Francesco Iraci, Golam M. Shaifullah, Hannah Middleton, H. Thankful Cromartie, Jeffrey S. Hazboun, Kathrin Grunthal, Keitaro Takahashi, Kejia Lee, Kuo Liu, Matthew T. Miles, Michael J. Keith, N. D. Ramesh Bhat, Riccardo J. Truant, Ryan M. Shannon, Ryo Kato, Siyuan Chen, Xiao Xue.

Figure 1
Figure 1. Figure 1: Inter-pulsar correlations from recent pulsar timing array gravitational-wave searches. We show the correlations derived from the the European Pulsar Timing Array and Indian Pulsar Timing Array (EPTA+InPTA Collaboration et al., 2023), the North American Nanohertz Observatory for Gravitational Waves (Agazie et al., 2023b), the MeerKAT Pulsar Timing Array (Miles et al., 2025b), the Parkes Pulsar Timing Array … view at source ↗
Figure 2
Figure 2. Figure 2: Effective integration time for a SKAO-PTA. Pulsars for which the effective integration time is 64 𝑚𝑢s are observed in a MeerKAT-size sub-array for 256 s. The points are shaded by the timing precision achieved by the SKA observations. not expect to see any appreciable difference in timing precision from the telescope backends as both are designed using similar principles (including coherent dedispersion). W… view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of PTA sensitivities. For the EPTA, MPTA, NANOGrav, and EPTA the curves are calculated assuming the observing strategies of the early 2020s. The number next to the name of the PTA in the legend indicates the number of pulsars observed by the PTA at that time. The IPTA curve is calculated by including all pulsars timed as part of PTA experiments. The solid black curve shows the projected sensitiv… view at source ↗
Figure 4
Figure 4. Figure 4: Strain sensitivity curves for the MeerKAT Pulsar Timing Array and a conceptual SKAO Pulsar Timing Array after observing for 5, 10, and 15 years. The left panel shows the sensitivity to a GWB. The black dashed lines shows the spectrum of a SMBHB driven GWB at an amplitude of 𝐴yr = 2×10−15 for a power law (top) and broken power law (lower) as specified in Equation 7. The black dash dotted line shows the spec… view at source ↗
Figure 5
Figure 5. Figure 5: Predicted number of detectable single sources with SKAO-PTA. The open dots represent the median number of resolved continuous gravitational waves resolved from the 200 SMBHB populations, while error bars represent the 64 and 32 percentiles of the distribution. 10h 8h 6h 4h 2h 0h 22h 20h 18h 16h 14h -75° -60° -45° -30° -15° 0° 15° 30° 45° 60° 75° Tobs = 20yr SKA CGW [PITH_FULL_IMAGE:figures/full_fig_p025_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Sky distribution of the SKAO PTA pulsars (light-blue) and the SMBHBs detected as continuous gravitational waves (dark violet) in a single realization SMBHB population. The size of the dark violet points is weighted by the CGW S/N 25 [PITH_FULL_IMAGE:figures/full_fig_p025_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Maximum spherical harmonics degree locally constrainable by the MPTA and proposed SKAO PTA data sets, derived from the angular separations between the pulsars in the respective data sets. Left: Comparison between the minimum angular scale corresponding to the spherical harmonics degree ℓ (black curve) and the mean next-neighbour distance in the MPTA (purple line) and the SKAO PTA simulated from the MeerTim… view at source ↗
Figure 8
Figure 8. Figure 8: Spread of a point-source (point-spread-area) function of the sky position. Left: A simulated 4.5-year MeerKAT PTA data set. Right: A simulated 4.5-year SKAO PTA data set, with timing precisions based on the MeerTime MSP census. Both simulations assume white noise is the only noise source present in the observations. maps were calculated with ℓmax = 8 and a singular value cutoff of 𝑛SV = 32, these values we… view at source ↗
Figure 9
Figure 9. Figure 9: Expected localization precision (8 𝜎) of a single GW source around two pulsars, J0437-4715 and J0030+0451 (Kato and Takahashi, 2026). Source localizations are shown at different assumed positions. The outer contours (green dashed line) correspond to the case without distance information, while the inner contour (blue solid line) correspond to the case with distance errors expected in the SKA era. The analy… view at source ↗

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Reference graph

Works this paper leans on

299 extracted references · 7 canonical work pages · 4 internal anchors

  1. [1]

    arXiv e-prints , keywords =

    Bias from small-scale leakage in Pulsar Timing Array maps. arXiv e-prints , keywords =. doi:10.48550/arXiv.2510.24857 , archivePrefix =. 2510.24857 , primaryClass =

    doi:10.48550/arxiv.2510.24857

  2. [2]

    , keywords =

    The NANOGrav 15 yr Data Set: Chromatic Gaussian Process Noise Models for Six Pulsars. , keywords =. doi:10.3847/1538-4357/ad5291 , archivePrefix =. 2405.14941 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/ad5291

  3. [3]

    Nature Astronomy , keywords =

    Insights into supermassive black hole mergers from the gravitational wave background. Nature Astronomy , keywords =. doi:10.1038/s41550-025-02482-1 , archivePrefix =. 2501.08956 , primaryClass =

    Pith/arXiv arXiv doi:10.1038/s41550-025-02482-1

  4. [4]

    , keywords =

    Quasars Can Signpost Supermassive Black Hole Binaries. , keywords =. doi:10.3847/1538-4357/adce05 , archivePrefix =. 2405.19406 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/adce05

  5. [5]

    arXiv e-prints , keywords =

    The NANOGrav 15 yr Data Set: Targeted Searches for Supermassive Black Hole Binaries. arXiv e-prints , keywords =. doi:10.48550/arXiv.2508.16534 , archivePrefix =. 2508.16534 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2508.16534

  6. [6]

    , keywords =

    The NANOGrav 15 yr Data Set: Looking for Signs of Discreteness in the Gravitational-wave Background. , keywords =. doi:10.3847/1538-4357/ad93d5 , archivePrefix =. 2404.07020 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/ad93d5

  7. [7]

    , keywords =

    Constraining the solution to the last parsec problem with pulsar timing. , keywords =. doi:10.1103/PhysRevD.91.084055 , archivePrefix =. 1503.02662 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevd.91.084055

  8. [8]

    , keywords =

    Insights into searches for anisotropies in the nanohertz gravitational-wave background. , keywords =. doi:10.1103/PhysRevD.103.042009 , archivePrefix =. 2010.13958 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevd.103.042009 2010

  9. [9]

    , keywords =

    Fisher formalism for anisotropic gravitational-wave background searches with pulsar timing arrays. , keywords =. doi:10.1103/PhysRevD.102.122005 , archivePrefix =. 2006.14570 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevd.102.122005 2006

  10. [10]

    , keywords =

    Characterizing gravitational wave stochastic background anisotropy with pulsar timing arrays. , keywords =. doi:10.1103/PhysRevD.88.062005 , archivePrefix =. 1306.5394 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevd.88.062005

  11. [11]

    2026 ,publisher =

    Caterina Tiburzi and author2 and author3 and author4 and author5 ,title =. 2026 ,publisher =

    2026

  12. [12]

    , keywords =

    Pulsars with NenuFAR: Backend and pipelines. , keywords =. doi:10.1051/0004-6361/202039339 , archivePrefix =. 2009.02076 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202039339 2009

  13. [13]

    , keywords =

    The stochastic gravitational-wave background from massive black hole binary systems: implications for observations with Pulsar Timing Arrays. , keywords =. doi:10.1111/j.1365-2966.2008.13682.x , archivePrefix =. 0804.4476 , primaryClass =

    doi:10.1111/j.1365-2966.2008.13682.x 2008

  14. [14]

    , keywords =

    Gas-driven massive black hole binaries: signatures in the nHz gravitational wave background. , keywords =. doi:10.1111/j.1365-2966.2010.17782.x , archivePrefix =. 1002.0584 , primaryClass =

    doi:10.1111/j.1365-2966.2010.17782.x 2010

  15. [15]

    Classical and Quantum Gravity , keywords =

    Insights into the astrophysics of supermassive black hole binaries from pulsar timing observations. Classical and Quantum Gravity , keywords =. doi:10.1088/0264-9381/30/22/224014 , archivePrefix =. 1307.2600 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0264-9381/30/22/224014

  16. [16]

    , keywords =

    Forecasting Pulsar Timing Array Sensitivity to Anisotropy in the Stochastic Gravitational Wave Background. , keywords =

  17. [17]

    , keywords =

    Search for Gravitational-wave Memory in PPTA and EPTA Data: A Complete Signal Model. , keywords =. doi:10.1051/0004-6361/202557896 , archivePrefix =. 2601.13957 , primaryClass =

    doi:10.1051/0004-6361/202557896

  18. [18]

    , keywords =

    Search for Gravitational-wave Memory in PPTA and EPTA Data: A Complete Signal Model. , keywords =. doi:10.3847/2041-8213/ae2912 , archivePrefix =. 2512.14650 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/2041-8213/ae2912 2041

  19. [19]

    , year = 2012, month = dec, volume =

    Pulsar timing arrays as imaging gravitational wave telescopes: Angular resolution and source (de)confusion. , year = 2012, month = dec, volume =

    2012

  20. [20]

    , year = 2019, month = jun, volume =

    The astrophysics of nanohertz gravitational waves. , year = 2019, month = jun, volume =. doi:10.1007/s00159-019-0115-7 , adsurl =

    doi:10.1007/s00159-019-0115-7 2019

  21. [21]

    arXiv e-prints , keywords =

    The Science of the Einstein Telescope. arXiv e-prints , keywords =. doi:10.48550/arXiv.2503.12263 , archivePrefix =. 2503.12263 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2503.12263

  22. [22]

    , keywords =

    GW250114: Testing Hawking's Area Law and the Kerr Nature of Black Holes. , keywords =. doi:10.1103/kw5g-d732 , archivePrefix =. 2509.08054 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/kw5g-d732

  23. [23]

    Physical Review X , year = 2016, month = jan, volume =

    Gravitational-Wave Cosmology across 29 Decades in Frequency. Physical Review X , year = 2016, month = jan, volume =

    2016

  24. [24]

    Annalen der Physik , keywords =

    The basic physics of the binary black hole merger GW150914. Annalen der Physik , keywords =. doi:10.1002/andp.201600209 , archivePrefix =. 1608.01940 , primaryClass =

    Pith/arXiv arXiv doi:10.1002/andp.201600209

  25. [25]

    , keywords =

    Observation of Gravitational Waves from a Binary Black Hole Merger. , keywords =. doi:10.1103/PhysRevLett.116.061102 , archivePrefix =. 1602.03837 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevlett.116.061102

  26. [26]

    , keywords =

    GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral. , keywords =. doi:10.1103/PhysRevLett.119.161101 , archivePrefix =. 1710.05832 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevlett.119.161101

  27. [27]

    , keywords =

    Multi-messenger Observations of a Binary Neutron Star Merger. , keywords =. doi:10.3847/2041-8213/aa91c9 , archivePrefix =. 1710.05833 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/2041-8213/aa91c9 2041

  28. [29]

    , keywords =

    The NANOGrav 15 yr Data Set: Observations and Timing of 68 Millisecond Pulsars. , keywords =. doi:10.3847/2041-8213/acda9a , archivePrefix =. 2306.16217 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/2041-8213/acda9a 2041

  29. [30]

    , keywords =

    The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background. , keywords =. doi:10.3847/2041-8213/acdac6 , archivePrefix =. 2306.16213 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/2041-8213/acdac6 2041

  30. [31]

    , keywords =

    Comparing Recent Pulsar Timing Array Results on the Nanohertz Stochastic Gravitational-wave Background. , keywords =. doi:10.3847/1538-4357/ad36be , archivePrefix =. 2309.00693 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/ad36be

  31. [32]

    , keywords =

    The NANOGrav 15 yr Data Set: Bayesian Limits on Gravitational Waves from Individual Supermassive Black Hole Binaries. , keywords =. doi:10.3847/2041-8213/ace18a , archivePrefix =. 2306.16222 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/2041-8213/ace18a 2041

  32. [33]

    arXiv e-prints , keywords =

    CHIME-o-Grav: Wideband Timing of Four Millisecond Pulsars from the NANOGrav 15-yr dataset. arXiv e-prints , keywords =. doi:10.48550/arXiv.2510.16668 , archivePrefix =. 2510.16668 , primaryClass =

    doi:10.48550/arxiv.2510.16668

  33. [34]

    arXiv e-prints , keywords =

    The International Pulsar Timing Array checklist for the detection of nanohertz gravitational waves. arXiv e-prints , keywords =. doi:10.48550/arXiv.2304.04767 , archivePrefix =. 2304.04767 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2304.04767

  34. [35]

    , keywords =

    A new class of radio pulsars. , keywords =. doi:10.1038/300728a0 , adsurl =

    doi:10.1038/300728a0

  35. [36]

    , keywords =

    Electron Density Power Spectrum in the Local Interstellar Medium. , keywords =. doi:10.1086/175515 , adsurl =

    doi:10.1086/175515

  36. [37]

    , keywords =

    The NANOGrav Nine-year Data Set: Observations, Arrival Time Measurements, and Analysis of 37 Millisecond Pulsars. , keywords =. doi:10.1088/0004-637X/813/1/65 , archivePrefix =. 1505.07540 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/813/1/65

  37. [38]

    , keywords =

    The NANOGrav 12.5 yr Data Set: Search for an Isotropic Stochastic Gravitational-wave Background. , keywords =. doi:10.3847/2041-8213/abd401 , archivePrefix =. 2009.04496 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/2041-8213/abd401 2041

  38. [39]

    The second data release from the European Pulsar Timing Array. V. Search for continuous gravitational wave signals. , keywords =. doi:10.1051/0004-6361/202348568 , archivePrefix =. 2306.16226 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202348568

  39. [40]

    , keywords =

    A millisecond pulsar. , keywords =. doi:10.1038/300615a0 , adsurl =

    doi:10.1038/300615a0

  40. [41]

    , year = 1970, month = dec, volume =

    Peculiar Pulse Burst in PSR 1237 + 25. , year = 1970, month = dec, volume =. doi:10.1038/2281297a0 , adsurl =

    doi:10.1038/2281297a0 1970

  41. [42]

    Classical and Quantum Gravity , keywords =

    A sensitivity curve approach to tuning a pulsar timing array in the detection era. Classical and Quantum Gravity , keywords =. doi:10.1088/1361-6382/adbbab , archivePrefix =. 2409.00336 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/1361-6382/adbbab

  42. [43]

    , keywords =

    The MeerKAT telescope as a pulsar facility: System verification and early science results from MeerTime. , keywords =. doi:10.1017/pasa.2020.19 , archivePrefix =. 2005.14366 , primaryClass =

    Pith/arXiv arXiv doi:10.1017/pasa.2020.19 2020

  43. [44]

    , keywords =

    Gravitational wave spectrum induced by primordial scalar perturbations. , keywords =. doi:10.1103/PhysRevD.76.084019 , archivePrefix =. hep-th/0703290 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevd.76.084019

  44. [45]

    , keywords =

    Massive black hole binaries in active galactic nuclei. , keywords =. doi:10.1038/287307a0 , adsurl =

    doi:10.1038/287307a0

  45. [46]

    , keywords =

    Studying the Solar system with the International Pulsar Timing Array. , keywords =. doi:10.1093/mnras/sty2632 , archivePrefix =. 1809.10744 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/sty2632

  46. [47]

    Characteristic Forms and Geometric Invariants , urldate =

    Shiing-Shen Chern and James Simons , journal =. Characteristic Forms and Geometric Invariants , urldate =

  47. [48]

    , keywords =

    Efficient computation of the gravitational wave spectrum emitted by eccentric massive black hole binaries in stellar environments. , keywords =. doi:10.1093/mnras/stx1093 , archivePrefix =. 1612.00455 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stx1093

  48. [49]

    , keywords =

    Common-red-signal analysis with 24-yr high-precision timing of the European Pulsar Timing Array: inferences in the stochastic gravitational-wave background search. , keywords =. doi:10.1093/mnras/stab2833 , archivePrefix =. 2110.13184 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stab2833

  49. [50]

    , keywords =

    The Chinese Pulsar Timing Array Data Release I: Single pulsar noise analysis. , keywords =. doi:10.1051/0004-6361/202452550 , archivePrefix =. 2506.04850 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202452550

  50. [51]

    , keywords =

    The TRAPUM L-band survey for pulsars in Fermi-LAT gamma-ray sources. , keywords =. doi:10.1093/mnras/stac3742 , archivePrefix =. 2212.08528 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stac3742

  51. [52]

    2024 , eprint=

    LISA Definition Study Report , author=. 2024 , eprint=

    2024

  52. [53]

    , keywords =

    Pulsars as tools for fundamental physics & astrophysics. , keywords =. doi:10.1016/j.newar.2004.09.040 , archivePrefix =. astro-ph/0505555 , primaryClass =

    Pith/arXiv arXiv doi:10.1016/j.newar.2004.09.040 2004

  53. [54]

    arXiv e-prints , keywords =

    A Measurement Model for Precision Pulsar Timing. arXiv e-prints , keywords =. doi:10.48550/arXiv.1010.3785 , archivePrefix =. 1010.3785 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.1010.3785

  54. [55]

    , keywords =

    Detecting Gravitational Wave Memory with Pulsar Timing. , keywords =. doi:10.1088/0004-637X/752/1/54 , adsurl =

    doi:10.1088/0004-637x/752/1/54

  55. [56]

    , keywords =

    Frequency-dependent Dispersion Measures and Implications for Pulsar Timing. , keywords =. doi:10.3847/0004-637X/817/1/16 , archivePrefix =. 1503.08491 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/0004-637x/817/1/16

  56. [57]

    , keywords =

    Wide-band Timing of the Parkes Pulsar Timing Array UWL Data. , keywords =. doi:10.3847/1538-4357/aca535 , archivePrefix =. 2211.12924 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/aca535

  57. [58]

    , keywords =

    Frequency- and phase-resolved polarimetry of millisecond pulsars and its application to timing. , keywords =. doi:10.1093/mnras/stag835 , archivePrefix =. 2512.09220 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stag835

  58. [59]

    , keywords =

    Limits on the Stochastic Gravitational Wave Background from the North American Nanohertz Observatory for Gravitational Waves. , keywords =. doi:10.1088/0004-637X/762/2/94 , archivePrefix =. 1201.6641 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/762/2/94

  59. [60]

    , keywords =

    Cyclic spectral analysis of radio pulsars. , keywords =. doi:10.1111/j.1365-2966.2011.19230.x , archivePrefix =. 1106.3345 , primaryClass =

    doi:10.1111/j.1365-2966.2011.19230.x 2011

  60. [61]

    , keywords =

    Pulsar timing measurements and the search for gravitational waves. , keywords =. doi:10.1086/157593 , adsurl =

    doi:10.1086/157593

  61. [62]

    , keywords =

    Gravitational waves from black-hole encounters: Prospects for ground and galaxy-based observatories. , keywords =. doi:10.1103/PhysRevD.108.024013 , archivePrefix =. 2305.19318 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevd.108.024013

  62. [63]

    doi:10.5281/zenodo.4059815 , version =

    ENTERPRISE: Enhanced Numerical Toolbox Enabling a Robust PulsaR Inference SuitE. doi:10.5281/zenodo.4059815 , version =

    doi:10.5281/zenodo.4059815

  63. [64]

    , keywords =

    First detection of frequency-dependent, time-variable dispersion measures. , keywords =. doi:10.1051/0004-6361/201834059 , archivePrefix =. 1902.03814 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201834059 1902

  64. [65]

    Dispersion measure variability for 36 millisecond pulsars at 150MHz with LOFAR

    Dispersion measure variability for 36 millisecond pulsars at 150 MHz with LOFAR. , keywords =. doi:10.1051/0004-6361/202039517 , archivePrefix =. 2011.13742 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202039517 2011

  65. [66]

    The second data release from the European Pulsar Timing Array. III. Search for gravitational wave signals. , keywords =. doi:10.1051/0004-6361/202346844 , archivePrefix =. 2306.16214 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202346844

  66. [67]

    Classical and Quantum Gravity , keywords =

    The gravitational-wave memory effect. Classical and Quantum Gravity , keywords =. doi:10.1088/0264-9381/27/8/084036 , archivePrefix =. 1003.3486 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0264-9381/27/8/084036

  67. [68]

    , keywords =

    Cosmological Background Interpretation of Pulsar Timing Array Data. , keywords =. doi:10.1103/PhysRevLett.132.171002 , archivePrefix =. 2307.02399 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevlett.132.171002

  68. [69]

    , keywords =

    Measuring the crust-superfluid coupling time-scale for 105 UTMOST pulsars with a Kalman filter. , keywords =. doi:10.1093/mnras/staf2053 , archivePrefix =. 2511.15134 , primaryClass =

    doi:10.1093/mnras/staf2053

  69. [70]

    A Gamma-ray Pulsar Timing Array Constrains the Nanohertz Gravitational Wave Background

    A gamma-ray pulsar timing array constrains the nanohertz gravitational wave background. Science , keywords =. doi:10.1126/science.abm3231 , archivePrefix =. 2204.05226 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.abm3231

  70. [71]

    , keywords =

    Constructing a Pulsar Timing Array. , keywords =. doi:10.1086/169195 , adsurl =

    doi:10.1086/169195

  71. [72]

    , keywords =

    Flux density monitoring of 89 millisecond pulsars with MeerKAT. , keywords =. doi:10.1093/mnras/stad2841 , archivePrefix =. 2309.07564 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stad2841

  72. [73]

    , keywords =

    Optimising the MeerKAT pulsar timing array and towards precision pulsar timing with SKA-mid. , keywords =. doi:10.1017/pasa.2025.10107 , archivePrefix =. 2510.03139 , primaryClass =

    doi:10.1017/pasa.2025.10107 2025

  73. [74]

    , keywords =

    Identifying and mitigating noise sources in precision pulsar timing data sets. , keywords =. doi:10.1093/mnras/staa3411 , archivePrefix =. 2010.06109 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/staa3411 2010

  74. [75]

    , keywords =

    On the Evidence for a Common-spectrum Process in the Search for the Nanohertz Gravitational-wave Background with the Parkes Pulsar Timing Array. , keywords =. doi:10.3847/2041-8213/ac17f4 , archivePrefix =. 2107.12112 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/2041-8213/ac17f4 2041

  75. [76]

    , keywords =

    Consistency of the Parkes Pulsar Timing Array Signal with a Nanohertz Gravitational-wave Background. , keywords =. doi:10.3847/2041-8213/ac76bb , archivePrefix =. 2206.03766 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/2041-8213/ac76bb 2041

  76. [77]

    Zhurnal Eksperimentalnoi i Teoreticheskoi Fiziki , year = 1974, month = jan, volume =

    Amplification of gravitational waves in an isotropic universe. Zhurnal Eksperimentalnoi i Teoreticheskoi Fiziki , year = 1974, month = jan, volume =

    1974

  77. [78]

    , keywords =

    The MeerKAT Pulsar Timing Array: Maps of the gravitational wave sky with the 4.5-yr data release. , keywords =. doi:10.1093/mnras/stae2573 , archivePrefix =. 2412.01214 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stae2573

  78. [79]

    , year = 1981, month = jan, volume =

    Inflationary universe: A possible solution to the horizon and flatness problems. , year = 1981, month = jan, volume =. doi:10.1103/PhysRevD.23.347 , adsurl =

    doi:10.1103/physrevd.23.347 1981

  79. [80]

    , keywords =

    Binary pulsars as detectors of ultralow-frequency gravitational waves. , keywords =. doi:10.1103/PhysRevD.56.4455 , adsurl =

    work page doi:10.1103/physrevd.56.4455

  80. [81]

    Bayesian Solar Wind Modeling with Pulsar Timing Arrays

    Bayesian Solar Wind Modeling with Pulsar Timing Arrays. , keywords =. doi:10.3847/1538-4357/ac5829 , archivePrefix =. 2111.09361 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ac5829

Showing first 80 references.