pith. sign in

arxiv: 2606.28554 · v1 · pith:EJLDWXHZnew · submitted 2026-06-26 · 🌌 astro-ph.CO · astro-ph.HE

The NANOGrav 15 yr Data Set: Impacts of Customized Chromatic Noise Models on Gravitational Wave Analyses

Nikita Agarwal , Gabriella Agazie , Alessandra Amosso , Akash Anumarlapudi , Anne M. Archibald , Zaven Arzoumanian , Anjana Ashok , Jeremy G. Baier
show 115 more authors
Paul T. Baker Bence Becsy Laura Blecha Adam Brazier Paul R. Brook Sarah Burke-Spolaor Rand Burnette Robin Case J. Andrew Casey-Clyde Yu-Ting Chang Maria Charisi Shami Chatterjee Tyler Cohen James M. Cordes Neil J. Cornish Fronefield Crawford H. Thankful Cromartie Kathryn Crowter Megan E. DeCesar Paul B. Demorest Heling Deng Lankeswar Dey Timothy Dolch Graham M. Doskoch Elizabeth C. Ferrara William Fiore Emmanuel Fonseca Gabriel E. Freedman Emiko C. Gardiner Nate Garver-Daniels Peter A. Gentile Kyle A. Gersbach Joseph Glaser Deborah C. Good Kayhan Gultekin Aiden Gundersen C. J. Harris Doa Hashemi Asl Jeffrey S. Hazboun Ross J. Jennings Aaron D. Johnson Megan L. Jones David L. Kaplan Anala K. Sreekumar Luke Zoltan Kelley Matthew Kerr Joey S. Key Nima Laal Michael T. Lam William G. Lamb Bjorn Larsen T. Joseph W. Lazio Natalia Lewandowska Tingting Liu Duncan R. Lorimer Jing Luo Ryan S. Lynch Chung-Pei Ma Dustin R. Madison Ashley Martsen Cayenne Matt Alexander McEwen James W. McKee Maura A. McLaughlin Natasha McMann Bradley W. Meyers Patrick M. Meyers Matthew T. Miles Chiara M. F. Mingarelli Andrea Mitridate Cherry Ng David J. Nice Shania Nichols Stella K. Ocker Daniel J. Oliver Ken D. Olum Timothy T. Pennucci Benetge B. P. Perera Polina Petrov Nihan S. Pol Henri A. Radovan Scott M. Ransom Paul S. Ray Joseph D. Romano Jessie C. Runnoe Alexander Saffer Shashwat C. Sardesai Ann Schmiedekamp Carl Schmiedekamp Kai Schmitz Levi Schult Brent J. Shapiro-Albert Xavier Siemens Joseph Simon Sophia V. Sosa Fiscella Ingrid H. Stairs Daniel R. Stinebring Kevin Stovall Robin Strahler Abhimanyu Susobhanan Joseph K. Swiggum Jacob Taylor Stephen R. Taylor Mercedes S. Thompson Jacob E. Turner Michele Vallisneri Rutger van Haasteren Joris P. W. Verbiest Sarah J. Vigeland Haley M. Wahl Kalista Wayt Kevin P. Wilson Caitlin A. Witt David Wright Olivia Young
This is my paper

Pith reviewed 2026-06-30 00:39 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.HE
keywords pulsar timing arraysstochastic gravitational wave backgroundHellings-Downs correlationchromatic noisenanohertz gravitational wavessupermassive black hole binariescontinuous wave searches
0
0 comments X

The pith

Customized chromatic noise models raise the Bayes factor for Hellings-Downs correlations eightfold in pulsar timing data.

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

The paper applies specialized models for frequency-dependent noise to the fifteen-year pulsar timing dataset. These models produce substantially stronger statistical evidence that the observed timing residuals contain the spatial correlations predicted for a stochastic gravitational wave background. The same models shift the inferred background to lower amplitude while permitting a steeper spectrum in a free fit. Searches for individual continuous-wave sources gain a larger effective volume, and support for nonstandard gravity modes declines. Reinterpretations under both supermassive black hole binary and cosmological source hypotheses show only small adjustments to model parameters.

Core claim

Use of the customized chromatic noise models on the fifteen-year dataset increases the Bayes factor for Hellings-Downs correlations over an uncorrelated red-noise process to 1571 using a power-law spectrum with fourteen Fourier modes, an eightfold rise over earlier results, while lowering the background amplitude to 2.1 times 10 to the minus fifteen at fixed index and raising the free spectral index to 3.5.

What carries the argument

Customized chromatic noise models that isolate frequency-dependent noise processes in pulsar timing residuals from a potential gravitational wave signal.

If this is right

  • The gravitational wave background spectrum appears quieter at fixed index and steeper when the index is allowed to vary.
  • The effective search volume for continuous gravitational wave sources increases by a factor of 3.2.
  • Evidence for a scalar-transverse gravitational wave polarization mode decreases.
  • Posterior distributions for both supermassive black hole binary and cosmological source models shift only marginally.

Where Pith is reading between the lines

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

  • Improved separation of noise from signal could help future larger datasets distinguish astrophysical from cosmological origins of the background.
  • The same noise-modeling strategy may be worth testing on independent pulsar timing arrays to check consistency of the correlation signature.
  • If the models hold, earlier analyses may have underestimated the strength of the nanohertz gravitational wave signal mainly because of residual chromatic noise.

Load-bearing premise

The customized chromatic noise models correctly capture all relevant noise processes without removing or biasing any gravitational wave signal component.

What would settle it

An independent analysis of the same timing residuals that applies different noise models and recovers a Bayes factor near the earlier lower value would indicate that the reported increase depends on the specific noise modeling choice.

Figures

Figures reproduced from arXiv: 2606.28554 by Aaron D. Johnson, Abhimanyu Susobhanan, Adam Brazier, Aiden Gundersen, Akash Anumarlapudi, Alessandra Amosso, Alexander McEwen, Alexander Saffer, Anala K. Sreekumar, Andrea Mitridate, Anjana Ashok, Anne M. Archibald, Ann Schmiedekamp, Ashley Martsen, Bence Becsy, Benetge B. P. Perera, Bjorn Larsen, Bradley W. Meyers, Brent J. Shapiro-Albert, Caitlin A. Witt, Carl Schmiedekamp, Cayenne Matt, Cherry Ng, Chiara M. F. Mingarelli, Chung-Pei Ma, C. J. Harris, Daniel J. Oliver, Daniel R. Stinebring, David J. Nice, David L. Kaplan, David Wright, Deborah C. Good, Doa Hashemi Asl, Duncan R. Lorimer, Dustin R. Madison, Elizabeth C. Ferrara, Emiko C. Gardiner, Emmanuel Fonseca, Fronefield Crawford, Gabriel E. Freedman, Gabriella Agazie, Graham M. Doskoch, Haley M. Wahl, Heling Deng, Henri A. Radovan, H. Thankful Cromartie, Ingrid H. Stairs, Jacob E. Turner, Jacob Taylor, James M. Cordes, James W. McKee, J. Andrew Casey-Clyde, Jeffrey S. Hazboun, Jeremy G. Baier, Jessie C. Runnoe, Jing Luo, Joey S. Key, Joris P. W. Verbiest, Joseph D. Romano, Joseph Glaser, Joseph K. Swiggum, Joseph Simon, Kai Schmitz, Kalista Wayt, Kathryn Crowter, Kayhan Gultekin, Ken D. Olum, Kevin P. Wilson, Kevin Stovall, Kyle A. Gersbach, Lankeswar Dey, Laura Blecha, Levi Schult, Luke Zoltan Kelley, Maria Charisi, Matthew Kerr, Matthew T. Miles, Maura A. McLaughlin, Megan E. DeCesar, Megan L. Jones, Mercedes S. Thompson, Michael T. Lam, Michele Vallisneri, Natalia Lewandowska, Natasha McMann, Nate Garver-Daniels, Neil J. Cornish, Nihan S. Pol, Nikita Agarwal, Nima Laal, Olivia Young, Patrick M. Meyers, Paul B. Demorest, Paul R. Brook, Paul S. Ray, Paul T. Baker, Peter A. Gentile, Polina Petrov, Rand Burnette, Robin Case, Robin Strahler, Ross J. Jennings, Rutger van Haasteren, Ryan S. Lynch, Sarah Burke-Spolaor, Sarah J. Vigeland, Scott M. Ransom, Shami Chatterjee, Shania Nichols, Shashwat C. Sardesai, Sophia V. Sosa Fiscella, Stella K. Ocker, Stephen R. Taylor, Timothy Dolch, Timothy T. Pennucci, Tingting Liu, T. Joseph W. Lazio, Tyler Cohen, William Fiore, William G. Lamb, Xavier Siemens, Yu-Ting Chang, Zaven Arzoumanian.

Figure 1
Figure 1. Figure 1: Changes in the GWB spectrum. We compare the inference of the HD-correlated GWB model under the different noise models of CNM (blue) and DMX (orange) for different parameterizations of the PSD. The violins compare the full posteriors of a free spectral parameterization while the blue and orange curves compare the MAP power-law spectra modeled through 14 Fourier modes. The green curve is the MAP inference of… view at source ↗
Figure 2
Figure 2. Figure 2: Changes in the power law GWB inference. Parameter posteriors for a 14 frequency power-law HD model are shown for DMX in orange and CNM in blue. CNM re￾covers a steeper spectral index, closer to the theoretical value of γ = 13/3 for GW-driven SMBHB mergers (dashed, black line). GWB posteriors under the CNM are nearly identical whether varying the chromatic parameters (dark blue, dot￾dashed) or holding them … view at source ↗
Figure 4
Figure 4. Figure 4: Changes to the fixed-γ GWB inference. Es￾timates of the GWB characteristic strain spectral amplitude A at a reference frequency of 1/yr, assuming a 14f power law spectrum with fixed γ = 13/3 from 2 to 28 nHz, with (top panel) no interpulsar correlations (CURN), and (bottom panel) Hellings-Downs (HD) correlations. We estimate a sys￾tematically lower strain amplitude of AHD = 2.1 +0.6 −0.5 ×10−15 using the C… view at source ↗
Figure 5
Figure 5. Figure 5: HD significance at different frequencies. [PITH_FULL_IMAGE:figures/full_fig_p012_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Changes in detection statistics for the GWB. [PITH_FULL_IMAGE:figures/full_fig_p013_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Alternative polarization search. Poste￾riors for the spectral parameters of a TT-polarized (HD￾correlated) GWB and an ST-polarized GWB. Baseline re￾sults using the DMX chromatic model (orange) are repro￾duced from Agazie et al. (2024). Using our CNMs (blue) substantially improves the evidence/constraints for the HD￾correlated mode, and reduces support for a large ST mode. dataset using the single-component… view at source ↗
Figure 9
Figure 9. Figure 9: Low-frequency candidate sky localization. [PITH_FULL_IMAGE:figures/full_fig_p015_9.png] view at source ↗
Figure 8
Figure 8. Figure 8: All-Sky CW significance The top panel re￾produces a portion of [PITH_FULL_IMAGE:figures/full_fig_p015_8.png] view at source ↗
Figure 11
Figure 11. Figure 11: Upper limits on the chirp mass for 3C 66B [PITH_FULL_IMAGE:figures/full_fig_p016_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Improved GW sensitivity with CNM. The top panel compares DMX (dashed, orange) and CNM (solid, blue) via their GWB sensitivity curves. A power-law GWB is plotted for the MAP values of the background with both DMX and CNM. The middle panel compares the all-sky CW sensitivity by shading a region of sensitivity at each frequency which spans the minimum and maximum sensi￾tivity across the sky at that frequency… view at source ↗
Figure 13
Figure 13. Figure 13: Significant red noise populations. The top panel reproduces [PITH_FULL_IMAGE:figures/full_fig_p018_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Astrophysical population inference. Marginalized posteriors for the astrophysical parameters fitted against the DMX (orange) and the CNM (blue) HD-only free spectra. Histograms show our raw results and we show smoothed KDEs to aid in interpretation. Priors are shown as black dashed lines and were the same for both fits. The MBH–Mbulge normalization µ and intrinsic scatter εµ, as well as the GSMF normaliza… view at source ↗
Figure 15
Figure 15. Figure 15: Astrophysical spectral fits. Free-spectral representation of the GWB spectrum with astrophysical fits to the spectra. The violins represent the KDE reconstruc￾tions of the DMX (orange) CNM (blue) HD-only free spec￾trum. The correspondingly colored shaded regions are the 68% confidence regions for the best-fit astrophysical spectra to the data for the two noise models. With the free-spectrum representation… view at source ↗
Figure 16
Figure 16. Figure 16: Inflation and Cosmological Phase Transition. [PITH_FULL_IMAGE:figures/full_fig_p021_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: Cosmic Strings. Parameter inference for a third exotic interpretations of the NG15 signal: GWs from stable cosmic strings. As in [PITH_FULL_IMAGE:figures/full_fig_p022_17.png] view at source ↗
read the original abstract

We report updated nHz gravitational wave (GW) significance, characterization, and interpretations using the customized chromatic-noise models (CNMs) developed in Larsen, Baier et al. (2026). for the NANOGrav 15-year data set. We find increased evidence for the Hellings-Downs (HD) correlation signature of the stochastic gravitational wave background (GWB), with a Bayes factor of $1571\pm14$ for HD-correlations over a common uncorrelated red-noise process using a power-law model with $14$ Fourier modes. We find this $\sim8\times$ increase in Bayes factor from Agazie et al. (2023a) is a result of improved noise mitigation. Assuming an analytic null distribution for the frequentist interpulsar correlation statistic, this corresponds to a slightly more significant measurement from $3.16\sigma$ to $3.32\sigma$ against the no-correlation scenario. Spectral inference with CNMs brings the power-law GWB amplitude down to $A_{\rm GWB} = 2.1^{+0.6}_{-0.5}\times10^{-15}$ at fixed $\gamma_{\rm GWB} = 13/3$. In a varied-$\gamma$ analysis, the spectral index increases to $\gamma_{\rm GWB}=3.5^{+0.7}_{-0.6}$. We report updates on an all-sky continuous gravitational wave (CW) search as well as select targeted searches and calculate a $3.2\times$ larger detection volume for the NANOGrav detector. With CNMs, we find reduced evidence for a non-Einsteinian, scalar-transverse mode of gravity. Finally, we reinterpret the GWB first with the assumption of an astrophysical background sourced by SMBHBs and then assuming the more exotic origins of cosmic inflation, a first-order cosmological phase transition, and stable cosmic strings. Under both the SMBHB hypothesis and the cosmological hypotheses, we see only marginal shifts in model parameter posteriors which are consistent with the slightly quieter and steeper power-law GWB spectrum.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript reports an updated analysis of the NANOGrav 15-year pulsar timing array data set using customized chromatic noise models (CNMs) from a companion paper. It claims an approximately 8-fold increase in the Bayes factor (to 1571±14) favoring the Hellings-Downs correlation over a common uncorrelated red-noise process (power-law model with 14 Fourier modes), a modest rise in frequentist significance from 3.16σ to 3.32σ, a lower GWB amplitude (A_GWB = 2.1^{+0.6}_{-0.5}×10^{-15} at γ_GWB=13/3), a steeper spectral index when γ is free (3.5^{+0.7}_{-0.6}), a 3.2× larger CW detection volume, reduced evidence for scalar-transverse modes, and only marginal shifts in SMBHB and cosmological model posteriors.

Significance. If the CNMs demonstrably preserve the common-process signal, the work would provide a concrete demonstration that refined per-pulsar noise modeling can substantially strengthen evidence for the HD signature and tighten GWB parameter constraints. The numerical updates and dual astrophysical/cosmological reinterpretations would be useful benchmarks for the PTA community. The modest frequentist significance gain and the dependence on an unvalidated separation between chromatic and achromatic terms limit the immediate strength of the conclusions.

major comments (2)
  1. [Abstract and Results] Abstract and main results: The central claim that the ~8× Bayes-factor increase results from improved noise mitigation requires explicit verification that the additional per-pulsar chromatic degrees of freedom do not absorb power from the spatially correlated common red-noise process. No injection-recovery tests, posterior comparisons of the common-process parameters with/without CNMs, or other separation diagnostics are described; the formal distinction between chromatic and achromatic spectra does not by itself guarantee that the joint posterior remains unbiased.
  2. [Results] Results on frequentist significance: The reported rise from 3.16σ to 3.32σ assumes an analytic null distribution for the interpulsar correlation statistic, but the manuscript does not state whether this null distribution has been recomputed or adjusted to account for the extra free parameters introduced by the CNMs.
minor comments (2)
  1. [Abstract] The citation 'Larsen, Baier et al. (2026)' should include a preprint identifier or note on publication status, as the CNMs are central to all quantitative claims.
  2. [Abstract] The quoted uncertainties on the Bayes factor (1571±14) and on A_GWB, γ_GWB are given to high precision; the text should briefly indicate the sampling method or convergence diagnostics used to obtain them.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thoughtful review and for identifying areas where the manuscript can be strengthened. We address each major comment below. Where appropriate, we will revise the manuscript to provide additional clarification and supporting material.

read point-by-point responses

  1. Referee: [Abstract and Results] Abstract and main results: The central claim that the ~8× Bayes-factor increase results from improved noise mitigation requires explicit verification that the additional per-pulsar chromatic degrees of freedom do not absorb power from the spatially correlated common red-noise process. No injection-recovery tests, posterior comparisons of the common-process parameters with/without CNMs, or other separation diagnostics are described; the formal distinction between chromatic and achromatic spectra does not by itself guarantee that the joint posterior remains unbiased.

    Authors: We agree that additional diagnostics would strengthen the presentation. The companion paper validates the CNMs through extensive per-pulsar tests, and the separation relies on the distinct frequency scaling of chromatic versus achromatic processes. In the revised manuscript we will add direct posterior comparisons of the common-process amplitude and spectral index with and without CNMs to demonstrate that the spatially correlated signal is preserved rather than absorbed. We will also expand the discussion of why the frequency-dependent separation provides robustness. Full injection-recovery tests specific to the GWB analysis are not included here but are referenced to ongoing work; the observed Bayes-factor increase is consistent with reduced per-pulsar noise variance allowing clearer recovery of the correlated component. revision: partial

  2. Referee: [Results] Results on frequentist significance: The reported rise from 3.16σ to 3.32σ assumes an analytic null distribution for the interpulsar correlation statistic, but the manuscript does not state whether this null distribution has been recomputed or adjusted to account for the extra free parameters introduced by the CNMs.

    Authors: The analytic null distribution is the same as that used in Agazie et al. (2023a) because the CNMs are pulsar-specific noise models that do not alter the structure of the correlation statistic or the null hypothesis of no spatial correlations. The extra degrees of freedom are absorbed into individual pulsar likelihoods and do not change the distribution of the statistic under the null. We will revise the text to explicitly state this assumption and provide the justification that recomputation is unnecessary. revision: yes

Circularity Check

0 steps flagged

Standard Bayesian GW analyses with companion-supplied noise models show no algebraic reduction to inputs

full rationale

The paper performs standard likelihood comparisons (Bayes factors for HD correlations vs. common uncorrelated red noise, spectral inference on power-law GWB parameters) after substituting the CNMs developed in the cited companion paper. These outputs are computed quantities from the data and the fixed noise-model parameterization; they are not equivalent by construction to the CNM parameters themselves, nor do any equations define the target GWB evidence in terms of the noise-model fit. The self-citation supplies the per-pulsar chromatic terms but does not carry the load of proving the HD signature; the correlation statistic and model comparison remain independent of that construction. No self-definitional steps, fitted inputs relabeled as predictions, or imported uniqueness theorems appear in the reported chain.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The analysis depends on the accuracy of the CNMs from the companion paper and on standard PTA assumptions; only the abstract is available so the full parameter count cannot be audited.

free parameters (2)
  • A_GWB = 2.1 x 10^{-15}
    Amplitude of the power-law GWB spectrum fitted at fixed gamma=13/3
  • gamma_GWB = 3.5
    Spectral index of the GWB when allowed to vary
axioms (1)
  • domain assumption Hellings-Downs correlations are the expected signature for an isotropic stochastic gravitational wave background in general relativity
    Used as the target model for the Bayes factor comparison

pith-pipeline@v0.9.1-grok · 6564 in / 1437 out tokens · 63749 ms · 2026-06-30T00:39:08.199670+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

294 extracted references · 251 canonical work pages · 69 internal anchors

  1. [1]

    , year = 1990, month = sep, volume =

    The generation of timing noise by superfluid rotation in pulsars. , year = 1990, month = sep, volume =

    1990

  2. [2]

    Handbook of Pulsar Astronomy

  3. [3]

    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 =

    work page doi:10.1088/1361-6382/adbbab

  4. [4]

    , keywords =

    Separating deterministic and stochastic gravitational wave signals in realistic pulsar timing array datasets. , keywords =. doi:10.1051/0004-6361/202451809 , archivePrefix =. 2407.21105 , primaryClass =

    work page doi:10.1051/0004-6361/202451809

  5. [5]

    The weighted likelihood ratio, linear hypotheses on normal location parameters , year =

    Dickey, James M , journal =. The weighted likelihood ratio, linear hypotheses on normal location parameters , year =

  6. [7]

    , keywords =

    Exploring the time variability of the solar wind using LOFAR pulsar data. , keywords =. doi:10.1051/0004-6361/202450680 , archivePrefix =. 2409.09838 , primaryClass =

    work page doi:10.1051/0004-6361/202450680

  7. [8]

    New advances in the Gaussian-process approach to pulsar-timing data analysis

    doi:10.1103/PhysRevD.90.104012 , eid =. arXiv , author =:1407.1838 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.90.104012

  8. [9]

    The NANOGrav Nine-Year Data Set: Measurement and Interpretation of Variations in Dispersion Measures

    doi:10.3847/1538-4357/aa73df , eid =. arXiv , author =:1612.03187 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa73df

  9. [10]

    Cordes and Stella Koch Ocker and Shami Chatterjee and Timothy Dolch and Ross J

    James M. Cordes and Stella Koch Ocker and Shami Chatterjee and Timothy Dolch and Ross J. Jennings and Michael T. Lam and Jacob E. Turner , title =. , year =

  10. [11]

    Pulsar timing noise from superfluid turbulence

    Pulsar timing noise from superfluid turbulence. , keywords =. doi:10.1093/mnras/stt1828 , archivePrefix =. 1310.3108 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt1828

  11. [12]

    Understanding and analysing time-correlated stochastic signals in pulsar timing

    Understanding and analysing time-correlated stochastic signals in pulsar timing. , keywords =. doi:10.1093/mnras/sts097 , archivePrefix =. 1202.5932 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sts097

  12. [13]

    , keywords =

    On measuring the gravitational-wave background using Pulsar Timing Arrays. , keywords =. doi:10.1111/j.1365-2966.2009.14590.x , archivePrefix =. 0809.0791 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.14590.x 2009

  13. [14]

    An Asteroid Belt Interpretation for the Timing Variations of the Millisecond Pulsar B1937+21

    An Asteroid Belt Interpretation for the Timing Variations of the Millisecond Pulsar B1937+21. , keywords =. doi:10.1088/0004-637X/766/1/5 , archivePrefix =. 1301.6429 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/766/1/5

  14. [15]

    , keywords =

    Precision Orbital Dynamics from Interstellar Scintillation Arcs for PSR J0437-4715. , keywords =. doi:10.3847/1538-4357/abbd40 , archivePrefix =. 2009.12757 , primaryClass =

    work page doi:10.3847/1538-4357/abbd40 2009

  15. [16]

    The NANOGrav 15-Year Data Set: A Case Study for Simplified Dispersion Measure Modeling for PSR J1455-3330 and the Impact on Gravitational Wave Sensitivity

    The NANOGrav 15-Year Data Set: A Case Study for Simplified Dispersion Measure Modeling for PSR J1455-3330 and the Impact on Gravitational Wave Sensitivity. arXiv e-prints , keywords =. doi:10.48550/arXiv.2506.03597 , archivePrefix =. 2506.03597 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2506.03597

  16. [17]

    , keywords =

    Pulsar scintillation through thick and thin: bow shocks, bubbles, and the broader interstellar medium. , keywords =. doi:10.1093/mnras/stad3683 , archivePrefix =. 2309.13809 , primaryClass =

    work page doi:10.1093/mnras/stad3683

  17. [19]

    A Second Chromatic Timing Event of Interstellar Origin toward PSR J1713+0747

    doi:10.3847/1538-4357/aac770 , eid =. arXiv , author =:1712.03651 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aac770

  18. [20]

    Frequency-Dependent Dispersion Measures and Implications for Pulsar Timing

    doi:10.3847/0004-637X/817/1/16 , eid =. arXiv , author =:1503.08491 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/817/1/16

  19. [21]

    arXiv , author =:2202.08293 , journal =

    doi:10.1103/PhysRevD.105.084049 , eid =. arXiv , author =:2202.08293 , journal =

    work page doi:10.1103/physrevd.105.084049

  20. [22]

    arXiv , author =:2012.11726 , journal =

    doi:10.1051/0004-6361/202039846 , eid =. arXiv , author =:2012.11726 , journal =

    work page doi:10.1051/0004-6361/202039846 2012

  21. [23]

    doi:10.1093/mnras/stv2143 , eprint =

    , keywords =. doi:10.1093/mnras/stv2143 , eprint =

    work page doi:10.1093/mnras/stv2143

  22. [24]

    arXiv , author =:1912.08807 , journal =

    doi:10.1088/1361-6382/ab8bbd , eid =. arXiv , author =:1912.08807 , journal =

    work page doi:10.1088/1361-6382/ab8bbd 1912

  23. [25]

    doi:10.1038/s41550-017-0299-6 , eprint =

    Nature Astronomy , keywords =. doi:10.1038/s41550-017-0299-6 , eprint =

    work page doi:10.1038/s41550-017-0299-6

  24. [26]

    Are we there yet? Time to detection of nanohertz gravitational waves based on pulsar-timing array limits

    doi:10.3847/2041-8205/819/1/L6 , eid =. arXiv , author =:1511.05564 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8205/819/1/l6 2041

  25. [27]

    arXiv , author =:2010.11950 , journal =

    doi:10.3847/2041-8213/abf2c9 , eid =. arXiv , author =:2010.11950 , journal =

    work page doi:10.3847/2041-8213/abf2c9 2041

  26. [28]

    Optimal Frequency Ranges for Sub-Microsecond Precision Pulsar Timing

    doi:10.3847/1538-4357/aac48d , eid =. arXiv , author =:1710.02272 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aac48d

  27. [29]

    doi:10.1088/0264-9381/30/22/224009 , eid =

    Classical and Quantum Gravity , month = nov, number =. doi:10.1088/0264-9381/30/22/224009 , eid =

    work page doi:10.1088/0264-9381/30/22/224009

  28. [30]

    The Parkes Pulsar Timing Array Project

    doi:10.1017/pasa.2012.017 , eid =. arXiv , author =:1210.6130 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1017/pasa.2012.017 2012

  29. [31]

    Cingoranelli and J

    Luke Zoltan Kelley and Emiko C Gardiner and David Wright and Magdalena Siwek and Cayenne Matt and Jeff Hazboun and A. Cingoranelli and J. Andrew Casey-Clyde and Tingting Liu and Kayhan G. holodeck , url =. 2023 , bdsk-url-1 =. doi:10.5281/zenodo.10966412 , eid =

    work page doi:10.5281/zenodo.10966412 2023

  30. [32]

    arXiv , author =:2305.01116 , journal =

    doi:10.1103/PhysRevD.108.104050 , eid =. arXiv , author =:2305.01116 , journal =

    work page doi:10.1103/physrevd.108.104050

  31. [33]

    Practical Methods for Continuous Gravitational Wave Detection using Pulsar Timing Data

    doi:10.1088/0004-637X/753/2/96 , eid =. arXiv , author =:1202.0808 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/753/2/96

  32. [34]

    Accelerated Bayesian model-selection and parameter-estimation in continuous gravitational-wave searches with pulsar-timing arrays

    doi:10.1103/PhysRevD.90.104028 , eid =. arXiv , author =:1406.5224 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.90.104028

  33. [35]

    Targeted search for continuous gravitational waves: Bayesian versus maximum-likelihood statistics

    doi:10.1088/0264-9381/26/20/204013 , eid =. arXiv , author =:0907.2569 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0264-9381/26/20/204013

  34. [36]

    The generalized F-statistic: multiple detectors and multiple GW pulsars

    doi:10.1103/PhysRevD.72.063006 , eid =. arXiv , author =:gr-qc/0504011 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.72.063006

  35. [37]

    Data analysis of gravitational-wave signals from spinning neutron stars. I. The signal and its detection

    doi:10.1103/PhysRevD.58.063001 , eid =. arXiv , author =:gr-qc/9804014 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.58.063001

  36. [38]

    Optimization of NANOGrav's Time Allocation for Maximum Sensitivity to Single Sources

    doi:10.1088/0004-637X/794/2/163 , eid =. arXiv , author =:1409.7722 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/794/2/163

  37. [39]

    The stochastic background: scaling laws and time to detection for pulsar timing arrays

    doi:10.1088/0264-9381/30/22/224015 , eid =. arXiv , author =:1305.3196 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0264-9381/30/22/224015

  38. [40]

    arXiv , author =:2309.07227 , journal =

    doi:10.3847/1538-4357/ad2be8 , eid =. arXiv , author =:2309.07227 , journal =

    work page doi:10.3847/1538-4357/ad2be8

  39. [41]

    doi:10.1093/mnras/stv1098 , eprint =

    , keywords =. doi:10.1093/mnras/stv1098 , eprint =

    work page doi:10.1093/mnras/stv1098

  40. [42]

    Searching For Anisotropic Gravitational-wave Backgrounds Using Pulsar Timing Arrays

    doi:10.1103/PhysRevD.88.084001 , eid =. arXiv , author =:1306.5395 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.88.084001

  41. [43]

    Characterising gravitational wave stochastic background anisotropy with Pulsar Timing Arrays

    doi:10.1103/PhysRevD.88.062005 , eid =. arXiv , author =:1306.5394 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.88.062005

  42. [44]

    doi:10.1093/mnras/stac3237 , eprint =

    , keywords =. doi:10.1093/mnras/stac3237 , eprint =

    work page doi:10.1093/mnras/stac3237

  43. [45]

    arXiv , author =:2404.02864 , journal =

    doi:10.48550/arXiv.2404.02864 , eid =. arXiv , author =:2404.02864 , journal =

    work page doi:10.48550/arxiv.2404.02864

  44. [46]

    Time-domain Implementation of the Optimal Cross-Correlation Statistic for Stochastic Gravitational-Wave Background Searches in Pulsar Timing Data

    doi:10.1103/PhysRevD.91.044048 , eid =. arXiv , author =:1410.8256 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.91.044048

  45. [47]

    Optimal strategies for gravitational wave stochastic background searches in pulsar timing data

    doi:10.1103/PhysRevD.79.084030 , eid =. arXiv , author =:0809.0701 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.79.084030

  46. [48]

    doi:10.1088/0004-637X/718/2/1400 , eprint =

    , keywords =. doi:10.1088/0004-637X/718/2/1400 , eprint =

    work page doi:10.1088/0004-637x/718/2/1400

  47. [49]

    Assessing Pulsar Timing Array Sensitivity to Gravitational Wave Bursts with Memory

    doi:10.1088/0004-637X/788/2/141 , eid =. arXiv , author =:1404.5682 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/788/2/141

  48. [50]

    Sensitivity curves for searches for gravitational-wave backgrounds

    doi:10.1103/PhysRevD.88.124032 , eid =. arXiv , author =:1310.5300 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.88.124032

  49. [51]

    arXiv , author =:2309.00693 , journal =

    doi:10.48550/arXiv.2309.00693 , eid =. arXiv , author =:2309.00693 , journal =

    work page doi:10.48550/arxiv.2309.00693

  50. [52]

    arXiv , author =:2301.07135 , journal =

    doi:10.3847/1538-4357/acb492 , eid =. arXiv , author =:2301.07135 , journal =

    work page doi:10.3847/1538-4357/acb492

  51. [53]

    arXiv , author =:2303.12105 , journal =

    doi:10.1103/PhysRevD.108.023008 , eid =. arXiv , author =:2303.12105 , journal =

    work page doi:10.1103/physrevd.108.023008

  52. [54]

    doi:10.1086/191076 , journal =

    work page doi:10.1086/191076

  53. [55]

    arXiv , author =:1010.3785 , journal =

    Pith/arXiv arXiv

  54. [56]

    Effects of the ISM on Detection of Low-frequency Gravitational Waves

    doi:10.1088/0264-9381/30/22/224006 , eid =. arXiv , author =:1310.8316 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0264-9381/30/22/224006

  55. [57]

    in preparation , title =

  56. [58]

    doi:10.1119/1.1374248 , journal =

    work page doi:10.1119/1.1374248

  57. [59]

    Paradigms in Physics 2.0

    doi:10.48550/arXiv.1706.09975 , eid =. arXiv , author =:1706.09975 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1706.09975

  58. [60]

    arXiv , author =:2306.16223 , journal =

    doi:10.48550/arXiv.2306.16223 , eid =. arXiv , author =:2306.16223 , journal =

    work page doi:10.48550/arxiv.2306.16223

  59. [61]

    arXiv , author =:2303.15442 , journal =

    doi:10.48550/arXiv.2303.15442 , eid =. arXiv , author =:2303.15442 , journal =

    work page doi:10.48550/arxiv.2303.15442

  60. [62]

    Searching for the nano-Hertz stochastic gravitational wave background with the Chinese Pulsar Timing Array Data Release I

    doi:10.1088/1674-4527/acdfa5 , eid =. arXiv , author =:2306.16216 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1674-4527/acdfa5

  61. [63]

    arXiv , author =:2306.16228 , journal =

    doi:10.48550/arXiv.2306.16228 , eid =. arXiv , author =:2306.16228 , journal =

    work page doi:10.48550/arxiv.2306.16228

  62. [64]

    arXiv , author =:2306.16227 , journal =

    doi:10.48550/arXiv.2306.16227 , eid =. arXiv , author =:2306.16227 , journal =

    work page doi:10.48550/arxiv.2306.16227

  63. [65]

    arXiv , author =:2306.16226 , journal =

    doi:10.48550/arXiv.2306.16226 , eid =. arXiv , author =:2306.16226 , journal =

    work page doi:10.48550/arxiv.2306.16226

  64. [66]

    The second data release from the European Pulsar Timing Array III. Search for gravitational wave signals

    doi:10.48550/arXiv.2306.16214 , eid =. arXiv , author =:2306.16214 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2306.16214

  65. [67]

    arXiv , author =:2306.16225 , journal =

    doi:10.48550/arXiv.2306.16225 , eid =. arXiv , author =:2306.16225 , journal =

    work page doi:10.48550/arxiv.2306.16225

  66. [68]

    arXiv , author =:2306.16224 , journal =

    doi:10.48550/arXiv.2306.16224 , eid =. arXiv , author =:2306.16224 , journal =

    work page doi:10.48550/arxiv.2306.16224

  67. [69]

    arXiv , author =:2306.16229 , journal =

    doi:10.3847/2041-8213/acdd03 , eid =. arXiv , author =:2306.16229 , journal =

    work page doi:10.3847/2041-8213/acdd03 2041

  68. [70]

    arXiv , author =:2306.16230 , journal =

    doi:10.48550/arXiv.2306.16230 , eid =. arXiv , author =:2306.16230 , journal =

    work page doi:10.48550/arxiv.2306.16230

  69. [71]

    Search for an isotropic gravitational-wave background with the Parkes Pulsar Timing Array

    doi:10.3847/2041-8213/acdd02 , eid =. arXiv , author =:2306.16215 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/acdd02 2041

  70. [72]

    The NANOGrav 15-year Data Set: Search for Signals from New Physics

    doi:10.3847/2041-8213/acdc91 , eid =. arXiv , author =:2306.16219 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/acdc91 2041

  71. [73]

    arXiv , author =:2306.16221 , journal =

    doi:10.48550/arXiv.2306.16221 , eid =. arXiv , author =:2306.16221 , journal =

    work page doi:10.48550/arxiv.2306.16221

  72. [74]

    , keywords =

    doi:10.3847/2041-8213/acda9a , eid =. arXiv , author =:2306.16217 , journal =

    work page doi:10.3847/2041-8213/acda9a 2041

  73. [75]

    arXiv , author =:2306.16218 , journal =

    doi:10.3847/2041-8213/acda88 , eid =. arXiv , author =:2306.16218 , journal =

    work page doi:10.3847/2041-8213/acda88 2041

  74. [76]

    The NANOGrav 15-year Data Set: Evidence for a Gravitational-Wave Background

    doi:10.3847/2041-8213/acdac6 , eid =. arXiv , author =:2306.16213 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/acdac6 2041

  75. [77]

    The NANOGrav 15 yr Data Set: Targeted Searches for Supermassive Black Hole Binaries

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2508.16534

  76. [78]

    arXiv , author =:2306.16222 , journal =

    doi:10.48550/arXiv.2306.16222 , eid =. arXiv , author =:2306.16222 , journal =

    work page doi:10.48550/arxiv.2306.16222

  77. [79]

    , keywords =

    Fast Bayesian analysis of individual binaries in pulsar timing array data. , keywords =. doi:10.1103/PhysRevD.105.122003 , archivePrefix =. 2204.07160 , primaryClass =

    work page doi:10.1103/physrevd.105.122003

  78. [80]

    , keywords =

    The NANOGrav 15 yr Data Set: Constraints on Supermassive Black Hole Binaries from the Gravitational-wave Background. , keywords =. doi:10.3847/2041-8213/ace18b , archivePrefix =. 2306.16220 , primaryClass =

    work page doi:10.3847/2041-8213/ace18b 2041

  79. [81]

    doi:10.1088/1538-3873/aaecbe , eprint =

    , keywords =. doi:10.1088/1538-3873/aaecbe , eprint =

    work page doi:10.1088/1538-3873/aaecbe

  80. [82]

    The Pan-STARRS1 Surveys

    doi:10.48550/arXiv.1612.05560 , eid =. arXiv , author =:1612.05560 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1612.05560

Showing first 80 references.