Combining the second data release of the European Pulsar Timing Array with low-frequency pulsar data

Context. Low radio frequency data are highly valuable for enhancing the sensitivity of pulsar timing arrays (PTAs) to propagation effects, such as dispersion measure (DM) variations. These low-frequency observations are particularly sensitive to DM fluctuations and can therefore significantly improve noise characterization in PTA datasets, which is essential for detecting the stochastic gravitational wave background (GWB). Aims. For this work we incorporated for the first time low-frequency observations from LOFAR (100 − 200 MHz) and NenuFAR (30 − 90 MHz) into a PTA context by combining them with the most recent data release from the European and Indian PTAs (in particular, with the subsample labeled DR2new+ , which includes only data from the new backends). This new combined dataset, labeled DR2low , consists of 12 pulsars observed over a time span of ∼11 years, with radio frequencies spanning the range 30 − 2500 MHz. The expanded frequency coverage of DR2low enables us to update and refine the noise models of DR2new+ , and this is crucial in order to increase the PTA sensitivity when searching for the stochastic gravitational wave background, which is the primary goal of PTA observations. This work is a milestone in the integration of low-frequency data into the upcoming third data release of the International PTA, which is posed to achieve the 5 σ detection of the GWB. Methods. We used the pulsar timing software packages L IBSTEMPO and E NTERPRISE to perform a noise analysis of DR2low . At first, we applied a standard noise model including red noise (RN) and time-variable dispersion measure (DMv) as power laws, with Fourier components up to 30 and 100 frequencies, respectively. Next, we performed a fully Bayesian model selection to identify the favored noise model for each pulsar and compute the Bayes factors across all combinations of RN, DMv, and a noise term with a chromatic index of 4 (CN 4 ). Finally, we carried out a detailed analysis on the choice of the chromatic index for CN 4 and the contribution of the solar wind. Results. The comparison between DR2low and DR2new+ using the standard noise model highlights the benefits of including low-frequency data. In particular, the additional frequency coverage improves the constraints on the DM variations and helps disentangle the DM and RN noise components in most pulsars. Through a Bayesian model selection, we found that the RN is required in the final model for 10 out of 12 pulsars, compared to only 5 in the DR2new+ dataset. The improved sensitivity to plasma effects provided by DR2low also favors the identification of significant CN 4 in eight pulsars, while none showed such evidence in DR2new+ . The chromatic index of this process is consistent with four of the five pulsars, while two (PSRs J0030+0451 and J1022+1001) show significant deviations from such a value. We attribute this discrepancy to unmodeled contributions from the solar wind, especially because of the high DM sensitivity of LOFAR and NenuFAR and the high observing cadence provided by these datasets near solar conjunction. A dedicated analysis confirms that the current solar wind model fails to fully capture the observed delay, and residual power is absorbed into the DM component of the model.

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Journal
Astronomy and Astrophysics
Published
2025-10-08
DOI
https://doi.org/10.1051/0004-6361/202555516
Citations
1
Primary Topic
Geophysics and Gravity Measurements
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article
Field-Weighted Citation Impact
1.79
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article

Combining the second data release of the European Pulsar Timing Array with low-frequency pulsar data

Jaikhomba Singha, M. Krämer, Ismaël Cognard, A. Chalumeau et al.
1 citations
Astronomy and Astrophysics
Geophysics and Gravity Measurements
1.79
article

Combining the second data release of the European Pulsar Timing Array with low-frequency pulsar data

Jaikhomba Singha, M. Krämer, Ismaël Cognard, A. Chalumeau, R. N. Caballero, A. Parthasarathy, C. Bassa, Y. Liu, C. Tiburzi, C. Vocks, Andrea Possenti, B. Ciardi, Keitaro Takahashi, Suvankar Roy Chowdhury, S. Desai, Baptiste Cecconi, В. В. Захаренко, Siyuan Chen, Aaron Golden, G. Shaifullah, D. Schwarz, J. P. W. Verbiest, Pooja Rana, І. P. Kravtsov, E. F. Keane, Manjari Bagchi, А. А. Коноваленко, Aman Srivastava, Pratik Tarafdar, Shubham Kala, M. Hoeft, B. C. Joshi, John Antoniadis, H. Hu, S. C. Susarla, M. A. Krishnakumar, G. H. Janssen, O. M. Ulyanov, G. Theureau, Debabrata Deb, F. Jankowski, P. Zarka, Lucas Guillemot, F. Iraci, J. Wang, S. Corbel, J. N. Girard, J-M Grießmeier, K. Nobelson
article en
1 citations

Abstract

Context. Low radio frequency data are highly valuable for enhancing the sensitivity of pulsar timing arrays (PTAs) to propagation effects, such as dispersion measure (DM) variations. These low-frequency observations are particularly sensitive to DM fluctuations and can therefore significantly improve noise characterization in PTA datasets, which is essential for detecting the stochastic gravitational wave background (GWB). Aims. For this work we incorporated for the first time low-frequency observations from LOFAR (100 − 200 MHz) and NenuFAR (30 − 90 MHz) into a PTA context by combining them with the most recent data release from the European and Indian PTAs (in particular, with the subsample labeled DR2new+ , which includes only data from the new backends). This new combined dataset, labeled DR2low , consists of 12 pulsars observed over a time span of ∼11 years, with radio frequencies spanning the range 30 − 2500 MHz. The expanded frequency coverage of DR2low enables us to update and refine the noise models of DR2new+ , and this is crucial in order to increase the PTA sensitivity when searching for the stochastic gravitational wave background, which is the primary goal of PTA observations. This work is a milestone in the integration of low-frequency data into the upcoming third data release of the International PTA, which is posed to achieve the 5 σ detection of the GWB. Methods. We used the pulsar timing software packages L IBSTEMPO and E NTERPRISE to perform a noise analysis of DR2low . At first, we applied a standard noise model including red noise (RN) and time-variable dispersion measure (DMv) as power laws, with Fourier components up to 30 and 100 frequencies, respectively. Next, we performed a fully Bayesian model selection to identify the favored noise model for each pulsar and compute the Bayes factors across all combinations of RN, DMv, and a noise term with a chromatic index of 4 (CN 4 ). Finally, we carried out a detailed analysis on the choice of the chromatic index for CN 4 and the contribution of the solar wind. Results. The comparison between DR2low and DR2new+ using the standard noise model highlights the benefits of including low-frequency data. In particular, the additional frequency coverage improves the constraints on the DM variations and helps disentangle the DM and RN noise components in most pulsars. Through a Bayesian model selection, we found that the RN is required in the final model for 10 out of 12 pulsars, compared to only 5 in the DR2new+ dataset. The improved sensitivity to plasma effects provided by DR2low also favors the identification of significant CN 4 in eight pulsars, while none showed such evidence in DR2new+ . The chromatic index of this process is consistent with four of the five pulsars, while two (PSRs J0030+0451 and J1022+1001) show significant deviations from such a value. We attribute this discrepancy to unmodeled contributions from the solar wind, especially because of the high DM sensitivity of LOFAR and NenuFAR and the high observing cadence provided by these datasets near solar conjunction. A dedicated analysis confirms that the current solar wind model fails to fully capture the observed delay, and residual power is absorbed into the DM component of the model.

Astronomy and AstrophysicsVol. 704
University of Central Florida (US), Tata Institute of Fundamental Research (IN), Centre National de la Recherche Scientifique (FR), Radboud University Nijmegen (NL), National Centre for Radio Astrophysics (IN), National Academy of Sciences of Ukraine (UA), University of Cape Town (ZA), University of Cagliari (IT), Ollscoil na Gaillimhe – University of Galway (IE), Chinese Academy of Sciences (CN), Homi Bhabha National Institute (IN), Bielefeld University (DE), Trinity College (CA), Université Paris Cité (FR), Trinity College Dublin (IE), Commissariat à l'Énergie Atomique et aux Énergies Alternatives (FR), Université Paris Sciences et Lettres (FR), Université Paris-Saclay (FR), Leibniz Institute for Astrophysics Potsdam (DE), Shanghai Astronomical Observatory (CN), Observatoire de Paris (FR), Astrophysique, Instrumentation et Modélisation (FR), Sorbonne Paris Cité (FR), Max Planck Institute for Astrophysics (DE), Institute of Radio Astronomy (UA), CEA Paris-Saclay (FR), Astronomical Institute of the Slovak Academy of Sciences (SK), Istituto Nazionale di Fisica Nucleare, Sezione di Milano Bicocca (IT), Thüringer Landessternwarte Tautenburg (DE), Osservatorio Astronomico di Cagliari (IT), Max Planck Institute for Radio Astronomy (DE), Laboratoire de Physique et Chimie de l’Environnement et de l’Espace (FR), Institute of Mathematical Sciences (IN), Indian Institute of Technology Hyderabad (IN), University of Milano-Bicocca (IT), GLA University (IN), University of Amsterdam (NL), Foundation for Research and Technology Hellas (GR), Ruhr University Bochum (DE), Netherlands Institute for Radio Astronomy (NL), Kumamoto University (JP)
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