The second data release from the European Pulsar Timing Array: I. The dataset and timing analysis

J. Antoniadis; S. Babak; A. -S. Bak Nielsen; C. G. Bassa; A. Berthereau; M. Bonetti; E. Bortolas; P. R. Brook; M. Burgay; R. N. Caballero; A. Chalumeau; D. J. Champion; S. Chanlaridis; S. Chen; I. Cognard; G. Desvignes; M. Falxa; R. D. Ferdman; A. Franchini; J. R. Gair; B. Goncharov; E. Graikou; J. -M. Grießmeier; L. Guillemot; Y. J. Guo; H. Hu; F. Iraci; D. Izquierdo-Villalba; J. Jang; J. Jawor; G. H. Janssen; A. Jessner; R. Karuppusamy; E. F. Keane; M. J. Keith; M. Kramer; M. A. Krishnakumar; K. Lackeos; K. J. Lee; K. Liu; Y. Liu; A. G. Lyne; J. W. McKee; R. A. Main; M. B. Mickaliger; I. C. Nitu; A. Parthasarathy; B. B. P. Perera; D. Perrodin; A. Petiteau; N. K. Porayko; A. Possenti; H. Quelquejay Leclere A. Samajdar; S. A. Sanidas; A. Sesana; G. Shaifullah; L. Speri; R. Spiewak; B. W. Stappers; S. C. Susarla; G. Theureau; C. Tiburzi; E. van der Wateren; A. Vecchio; V. Venkatraman Krishnan; J. P. W. Verbiest; J. Wang; L. Wang; Z. Wu

doi:10.1051/0004-6361/202346841

The second data release from the European Pulsar Timing Array: I. The dataset and timing analysis

J. Antoniadis, S. Babak, A. -S. Bak Nielsen, C. G. Bassa, A. Berthereau, M. Bonetti, E. Bortolas, P. R. Brook, M. Burgay, R. N. Caballero, A. Chalumeau, D. J. Champion, S. Chanlaridis, S. Chen, I. Cognard, G. Desvignes, M. Falxa, R. D. Ferdman, A. Franchini, J. R. GairB. Goncharov, E. Graikou, J. -M. Grießmeier, L. Guillemot, Y. J. Guo, H. Hu, F. Iraci, D. Izquierdo-Villalba, J. Jang, J. Jawor, G. H. Janssen, A. Jessner, R. Karuppusamy, E. F. Keane, M. J. Keith, M. Kramer, M. A. Krishnakumar, K. Lackeos, K. J. Lee, K. Liu, Y. Liu, A. G. Lyne, J. W. McKee, R. A. Main, M. B. Mickaliger, I. C. Nitu, A. Parthasarathy, B. B. P. Perera, D. Perrodin, A. Petiteau, N. K. Porayko, A. Possenti, H. Quelquejay Leclere A. Samajdar, S. A. Sanidas, A. Sesana, G. Shaifullah, L. Speri, R. Spiewak, B. W. Stappers, S. C. Susarla, G. Theureau, C. Tiburzi, E. van der Wateren, A. Vecchio, V. Venkatraman Krishnan, J. P. W. Verbiest, J. Wang, L. Wang, Z. Wu

Physics and Astronomy

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Abstract

Pulsar timing arrays offer a probe of the low-frequency gravitational wave spectrum (1 - 100 nanohertz), which is intimately connected to a number of markers that can uniquely trace the formation and evolution of the Universe. We present the dataset and the results of the timing analysis from the second data release of the European Pulsar Timing Array (EPTA). The dataset contains high-precision pulsar timing data from 25 millisecond pulsars collected with the five largest radio telescopes in Europe, as well as the Large European Array for Pulsars. The dataset forms the foundation for the search for gravitational waves by the EPTA, presented in associated papers. We describe the dataset and present the results of the frequentist and Bayesian pulsar timing analysis for individual millisecond pulsars that have been observed over the last ~25 years. We discuss the improvements to the individual pulsar parameter estimates, as well as new measurements of the physical properties of these pulsars and their companions. This data release extends the dataset from EPTA Data Release 1 up to the beginning of 2021, with individual pulsar datasets with timespans ranging from 14 to 25 years. These lead to improved constraints on annual parallaxes, secular variation of the orbital period, and Shapiro delay for a number of sources. Based on these results, we derived astrophysical parameters that include distances, transverse velocities, binary pulsar masses, and annual orbital parallaxes.

Original language	English
Article number	A48
Number of pages	28
Journal	Astronomy and Astrophysics
Volume	678
DOIs	https://doi.org/10.1051/0004-6361/202346841
Publication status	Published - 3 Oct 2023

Bibliographical note

Acknowledgments:
The European Pulsar Timing Array (EPTA) is a collaboration between European and partner institutes, namely ASTRON (NL), INAF/Osservatorio di Cagliari (IT), Max-Planck-Institut für Radioastronomie (GER), Nançay/Paris Observatory (FRA), the University of Manchester (UK), the University of Birmingham (UK), the University of East Anglia (UK), the University of Bielefeld (GER), the University of Paris (FRA), the University of Milan-Bicocca (IT), the Foundation for Research and Technology, Hellas (GR), and Peking University (CHN), with the aim to provide high-precision pulsar timing to work towards the direct detection of low-frequency gravitational waves. An Advanced Grant of the European Research Council allowed to implement the Large European Array for Pulsars (LEAP) under Grant Agreement Number 227947 (PI: M. Kramer). The EPTA is part of the International Pulsar Timing Array (IPTA); we thank our IPTA colleagues for their support and help with this paper and the external Detection Committee members for their work on the Detection Checklist. Part of this work is based on observations with the 100-m telescope of the Max-Planck-Institut für Radioastronomie (MPIfR) at Effelsberg in Germany. Pulsar research at the Jodrell Bank Centre for Astrophysics and the observations using the Lovell Telescope are supported by a Consolidated Grant (ST/T000414/1) from the UK’s Science and Technology Facilities Council (STFC). I.C.N. is also supported by the STFC doctoral training grant ST/T506291/1. The Nançay radio Observatory is operated by the Paris Observatory, associated with the French Centre National de la Recherche Scientifique (CNRS), and partially supported by the Region Centre in France. We acknowledge financial support from “Programme National de Cosmologie and Galaxies” (PNCG), and “Programme National Hautes Energies” (PNHE) funded by CNRS/INSU-IN2P3-INP, CEA and CNES, France. We acknowledge financial support from Agence Nationale de la Recherche (ANR-18-CE31-0015), France. The Westerbork Synthesis Radio Telescope is operated by the Netherlands Institute for Radio Astronomy (ASTRON) with support from the Netherlands Foundation for Scientific Research (NWO). The Sardinia Radio Telescope (SRT) is funded by the Department of University and Research (MIUR), the Italian Space Agency (ASI), and the Autonomous Region of Sardinia (RAS) and is operated as a National Facility by the National Institute for Astrophysics (INAF). The work is supported by the National SKA programme of China (2020SKA0120100), Max-Planck Partner Group, NSFC 11690024, CAS Cultivation Project for FAST Scientific. This work is also supported as part of the “LEGACY” MPG-CAS collaboration on low-frequency gravitational wave astronomy. J.A. acknowledges support from the European Commission (Grant Agreement number: 101094354). J.A. and S.Cha. were partially supported by the Stavros Niarchos Foundation (SNF) and the Hellenic Foundation for Research and Innovation (H.F.R.I.) under the 2nd Call of the “Science and Society - Action Always strive for excellence – Theodoras Papazoglou” (Project Number: 01431). A.C. acknowledges support from the Paris Île-de-France Region. A.C., A.F., A.Se., A.Sa., E.B., D.I., G.M.S., M.Bo. acknowledge financial support provided under the European Union’s H2020 ERC Consolidator Grant “Binary Massive Black Hole Astrophysics” (B Massive, Grant Agreement: 818691). G.D., K.Li., R.K. and M.K. acknowledge support from European Research Council (ERC) Synergy Grant “BlackHoleCam”, Grant Agreement Number 610058. This work is supported by the ERC Advanced Grant “LEAP”, Grant Agreement Number 227947 (PI M. Kramer). A.V. and P.R.B. are supported by the UK’s Science and Technology Facilities Council (STFC; grant ST/W000946/1). A.V. also acknowledges the support of the Royal Society and Wolfson Foundation. J.P.W.V. acknowledges support by the Deutsche Forschungsgemeinschaft (DFG) through thew Heisenberg programme (Project No. 433075039) and by the NSF through AccelNet award #2114721. N.K.P. is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) – Projektnummer PO 2758/1–1, through the Walter-Benjamin programme. A.Sa. thanks the Alexander von Humboldt foundation in Germany for a Humboldt fellowship for postdoctoral researchers. A.Po., D.P. and M.Bu. acknowledge support from the research grant “iPeska” (P.I. Andrea Possenti) funded under the INAF national call Prin-SKA/CTA approved with the Presidential Decree 70/2016 (Italy). R.N.C. acknowledges financial support from the Special Account for Research Funds of the Hellenic Open University (ELKE-HOU) under the research programme “GRAVPUL” (K.E.-80383/grant agreement 319/10-10-2022: PI N. A. B. Gizani). E.v.d.W., C.G.B. and G.H.J. acknowledge support from the Dutch National Science Agenda, NWA Startimpuls – 400.17.608. B.G. is supported by the Italian Ministry of Education, University and Research within the PRIN 2017 Research Program Framework, n. 2017SYRTCN. L.S. acknowledges the use of the HPC system Cobra at the Max Planck Computing and Data Facility. The work presented here is a culmination of many years of data analysis as well as software and instrument development. In particular, we thank Drs. N. D’Amico, P.C.C. Freire, R. van Haasteren, C. Jordan, K. Lazaridis, P. Lazarus, L. Lentati, O. Löhmer and R. Smits for their past contributions. We also thank Dr. N. Wex for supporting the calculations of the galactic acceleration as well as the related discussions. The EPTA is also grateful to staff at its observatories and telescopes who have made the continued observations possible. Author contributions: The European Pulsar Timing Array: JA, SB, ASBN, CGB, ABe, MBo, EB, PRB, MBu, RNC, AC, DJC, SCha, SChe, IC, GD, MF, RDF, AF, JRG, BG, EG, JMG, LG, YJG, HH, FI, DIV, JJan, JJaw, GHJ, AJ, RK, EFK, MJK, MK, MAK, KLa, KJL, KLi, YL, AGL, JWM, RAM, MBM, ICN, APa, BBPP, DP, APe, NKP, APo, HQL, ASa, SAS, ASe, GS, LS, RS, BWS, SCS, GT, CT, EvdW, AV, VVK, JPWV, JW, LW and ZW. The EPTA is a multi-decade effort and all authors have contributed through conceptualisation, funding acquisition, data-curation, methodology, software and hardware developments as well as (aspects of) the continued running of the observational campaigns, which includes writing and proofreading observing proposals, evaluating observations and observing systems, mentoring students, developing science cases. All authors also helped in (aspects of) verification of the data, analysis and results as well as in finalising the paper draft. Specific contributions from individual EPTA members are listed in the CRediT (https://credit.niso.org/) format below. The Indian Pulsar Timing Array: PA, SA, MB, ABa, SDa, DD, SDe, NDB, CD, YG, SH, BCJ, FK, DK, TK, NK, MAK, YM, KN, AKP, TP, PR, JS, ASr, MS, ASu, KT and PT. InPTA members contributed in uGMRT observations and data reduction to create the InPTA data set which is employed while assembling the DR2full+ and DR2new+ data sets. J.Jan., K.Li., G.M.S. equally share the correspondence of the paper. CRediT statement: Conceptualisation: APa, APo, AV, BWS, CGB, CT, GHJ, GMS, GT, IC, JA, JJan, JPWV, JW, JWM, KJL, KLi, MK. Methodology: APa, AV, DJC, GMS, IC, JA, JJan, JPWV, JWM, KJL, KLi, LG, MK. Software: AC, AJ, APa, CGB, DJC, GMS, IC, JA, JJan, JJaw, JPWV, KJL, KLi, LG, MJK, RK. Validation: AC, APa, CGB, CT, GMS, GT, IC, JA, JJan, JPWV, JWM, KLi, LG. Formal Analysis: APa, CGB, DJC, DP, EvdW, GHJ, GMS, JA, JJan, JPWV, JWM, KLi. Investigation: APa, APo, BWS, CGB, DJC, DP, GMS, GT, IC, JA, JJan, JPWV, JWM, KLi, LG, MBM, MBu, MJK, RK. Resources: APa, APe, APo, BWS, GHJ, GMS, GT, HH, IC, JA, JJan, JPWV, JWM, KJL, KLi, LG, MJK, MK, RK. Data Curation: AC, AJ, APa, BWS, CGB, DJC, DP, EG, EvdW, GHJ, GMS, GT, HH, IC, JA, JJan, JPWV, JWM, KLi, LG, MBM, MBu, MJK, MK, NKP, RK, SChe, YJG. Writing – Original Draft: APa, GMS, JA, JJan, KLi, LG. Writing – Review and Editing: AC, AF, APa, APo, DJC, EB, EFK, GHJ, GMS, GT, JA, JJan, JPWV, JWM, KLi, MK, SChe, VVK. Visualisation: APa, GMS, JA, JJan, KLi. Supervision: APo, ASe, AV, BWS, CGB, DJC, EFK, GHJ, GMS, GT, IC, JA, JPWV, KJL, KLi, LG, MJK, MK, VVK. Project Administration: APo, ASe, AV, BWS, CGB, CT, GHJ, GMS, GT, IC, JJan, JPWV, JWM, KLi, LG, MK. Funding Acquisition: APe, APo, ASe, BWS, GHJ, GT, IC, JA, JJan, LG, MJK, MK. Data Availability: Files containing the TOAs and pulsar timing models can be downloaded from https://epta.pages.in2p3.fr/epta-dr2/. The same site also provides the software environments necessary to recreate the timing analysis presented in this article.

Keywords

(Stars:) pulsars: general
(Stars:) pulsars
Gravitational waves
Astronomical instrumentation, methods, and techniques

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AntoniadisJ2023secondFinal published version, 5.54 MBLicence: Creative Commons: Attribution (CC BY)

Astrophysics at the University of Birmingham - Consolidated grant 2022-2025
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Cite this

Antoniadis, J., Babak, S., Nielsen, A. .-S. B., Bassa, C. G., Berthereau, A., Bonetti, M., Bortolas, E., Brook, P. R., Burgay, M., Caballero, R. N., Chalumeau, A., Champion, D. J., Chanlaridis, S., Chen, S., Cognard, I., Desvignes, G., Falxa, M., Ferdman, R. D., Franchini, A., ... Wu, Z. (2023). The second data release from the European Pulsar Timing Array: I. The dataset and timing analysis. Astronomy and Astrophysics, 678, Article A48. https://doi.org/10.1051/0004-6361/202346841

@article{aeb57f9124884de598552234000540f0,

title = "The second data release from the European Pulsar Timing Array: I. The dataset and timing analysis",

abstract = "Pulsar timing arrays offer a probe of the low-frequency gravitational wave spectrum (1 - 100 nanohertz), which is intimately connected to a number of markers that can uniquely trace the formation and evolution of the Universe. We present the dataset and the results of the timing analysis from the second data release of the European Pulsar Timing Array (EPTA). The dataset contains high-precision pulsar timing data from 25 millisecond pulsars collected with the five largest radio telescopes in Europe, as well as the Large European Array for Pulsars. The dataset forms the foundation for the search for gravitational waves by the EPTA, presented in associated papers. We describe the dataset and present the results of the frequentist and Bayesian pulsar timing analysis for individual millisecond pulsars that have been observed over the last ~25 years. We discuss the improvements to the individual pulsar parameter estimates, as well as new measurements of the physical properties of these pulsars and their companions. This data release extends the dataset from EPTA Data Release 1 up to the beginning of 2021, with individual pulsar datasets with timespans ranging from 14 to 25 years. These lead to improved constraints on annual parallaxes, secular variation of the orbital period, and Shapiro delay for a number of sources. Based on these results, we derived astrophysical parameters that include distances, transverse velocities, binary pulsar masses, and annual orbital parallaxes. ",

keywords = "(Stars:) pulsars: general, (Stars:) pulsars, Gravitational waves, Astronomical instrumentation, methods, and techniques",

author = "J. Antoniadis and S. Babak and Nielsen, {A. -S. Bak} and Bassa, {C. G.} and A. Berthereau and M. Bonetti and E. Bortolas and Brook, {P. R.} and M. Burgay and Caballero, {R. N.} and A. Chalumeau and Champion, {D. J.} and S. Chanlaridis and S. Chen and I. Cognard and G. Desvignes and M. Falxa and Ferdman, {R. D.} and A. Franchini and Gair, {J. R.} and B. Goncharov and E. Graikou and Grie{\ss}meier, {J. -M.} and L. Guillemot and Guo, {Y. J.} and H. Hu and F. Iraci and D. Izquierdo-Villalba and J. Jang and J. Jawor and Janssen, {G. H.} and A. Jessner and R. Karuppusamy and Keane, {E. F.} and Keith, {M. J.} and M. Kramer and Krishnakumar, {M. A.} and K. Lackeos and Lee, {K. J.} and K. Liu and Y. Liu and Lyne, {A. G.} and McKee, {J. W.} and Main, {R. A.} and Mickaliger, {M. B.} and Nitu, {I. C.} and A. Parthasarathy and Perera, {B. B. P.} and D. Perrodin and A. Petiteau and Porayko, {N. K.} and A. Possenti and Samajdar, {H. Quelquejay Leclere A.} and Sanidas, {S. A.} and A. Sesana and G. Shaifullah and L. Speri and R. Spiewak and Stappers, {B. W.} and Susarla, {S. C.} and G. Theureau and C. Tiburzi and Wateren, {E. van der} and A. Vecchio and Krishnan, {V. Venkatraman} and Verbiest, {J. P. W.} and J. Wang and L. Wang and Z. Wu",

note = "Acknowledgments: The European Pulsar Timing Array (EPTA) is a collaboration between European and partner institutes, namely ASTRON (NL), INAF/Osservatorio di Cagliari (IT), Max-Planck-Institut f{\"u}r Radioastronomie (GER), Nan{\c c}ay/Paris Observatory (FRA), the University of Manchester (UK), the University of Birmingham (UK), the University of East Anglia (UK), the University of Bielefeld (GER), the University of Paris (FRA), the University of Milan-Bicocca (IT), the Foundation for Research and Technology, Hellas (GR), and Peking University (CHN), with the aim to provide high-precision pulsar timing to work towards the direct detection of low-frequency gravitational waves. An Advanced Grant of the European Research Council allowed to implement the Large European Array for Pulsars (LEAP) under Grant Agreement Number 227947 (PI: M. Kramer). The EPTA is part of the International Pulsar Timing Array (IPTA); we thank our IPTA colleagues for their support and help with this paper and the external Detection Committee members for their work on the Detection Checklist. Part of this work is based on observations with the 100-m telescope of the Max-Planck-Institut f{\"u}r Radioastronomie (MPIfR) at Effelsberg in Germany. Pulsar research at the Jodrell Bank Centre for Astrophysics and the observations using the Lovell Telescope are supported by a Consolidated Grant (ST/T000414/1) from the UK{\textquoteright}s Science and Technology Facilities Council (STFC). I.C.N. is also supported by the STFC doctoral training grant ST/T506291/1. The Nan{\c c}ay radio Observatory is operated by the Paris Observatory, associated with the French Centre National de la Recherche Scientifique (CNRS), and partially supported by the Region Centre in France. We acknowledge financial support from “Programme National de Cosmologie and Galaxies” (PNCG), and “Programme National Hautes Energies” (PNHE) funded by CNRS/INSU-IN2P3-INP, CEA and CNES, France. We acknowledge financial support from Agence Nationale de la Recherche (ANR-18-CE31-0015), France. The Westerbork Synthesis Radio Telescope is operated by the Netherlands Institute for Radio Astronomy (ASTRON) with support from the Netherlands Foundation for Scientific Research (NWO). The Sardinia Radio Telescope (SRT) is funded by the Department of University and Research (MIUR), the Italian Space Agency (ASI), and the Autonomous Region of Sardinia (RAS) and is operated as a National Facility by the National Institute for Astrophysics (INAF). The work is supported by the National SKA programme of China (2020SKA0120100), Max-Planck Partner Group, NSFC 11690024, CAS Cultivation Project for FAST Scientific. This work is also supported as part of the “LEGACY” MPG-CAS collaboration on low-frequency gravitational wave astronomy. J.A. acknowledges support from the European Commission (Grant Agreement number: 101094354). J.A. and S.Cha. were partially supported by the Stavros Niarchos Foundation (SNF) and the Hellenic Foundation for Research and Innovation (H.F.R.I.) under the 2nd Call of the “Science and Society - Action Always strive for excellence – Theodoras Papazoglou” (Project Number: 01431). A.C. acknowledges support from the Paris {\^I}le-de-France Region. A.C., A.F., A.Se., A.Sa., E.B., D.I., G.M.S., M.Bo. acknowledge financial support provided under the European Union{\textquoteright}s H2020 ERC Consolidator Grant “Binary Massive Black Hole Astrophysics” (B Massive, Grant Agreement: 818691). G.D., K.Li., R.K. and M.K. acknowledge support from European Research Council (ERC) Synergy Grant “BlackHoleCam”, Grant Agreement Number 610058. This work is supported by the ERC Advanced Grant “LEAP”, Grant Agreement Number 227947 (PI M. Kramer). A.V. and P.R.B. are supported by the UK{\textquoteright}s Science and Technology Facilities Council (STFC; grant ST/W000946/1). A.V. also acknowledges the support of the Royal Society and Wolfson Foundation. J.P.W.V. acknowledges support by the Deutsche Forschungsgemeinschaft (DFG) through thew Heisenberg programme (Project No. 433075039) and by the NSF through AccelNet award #2114721. N.K.P. is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) – Projektnummer PO 2758/1–1, through the Walter-Benjamin programme. A.Sa. thanks the Alexander von Humboldt foundation in Germany for a Humboldt fellowship for postdoctoral researchers. A.Po., D.P. and M.Bu. acknowledge support from the research grant “iPeska” (P.I. Andrea Possenti) funded under the INAF national call Prin-SKA/CTA approved with the Presidential Decree 70/2016 (Italy). R.N.C. acknowledges financial support from the Special Account for Research Funds of the Hellenic Open University (ELKE-HOU) under the research programme “GRAVPUL” (K.E.-80383/grant agreement 319/10-10-2022: PI N. A. B. Gizani). E.v.d.W., C.G.B. and G.H.J. acknowledge support from the Dutch National Science Agenda, NWA Startimpuls – 400.17.608. B.G. is supported by the Italian Ministry of Education, University and Research within the PRIN 2017 Research Program Framework, n. 2017SYRTCN. L.S. acknowledges the use of the HPC system Cobra at the Max Planck Computing and Data Facility. The work presented here is a culmination of many years of data analysis as well as software and instrument development. In particular, we thank Drs. N. D{\textquoteright}Amico, P.C.C. Freire, R. van Haasteren, C. Jordan, K. Lazaridis, P. Lazarus, L. Lentati, O. L{\"o}hmer and R. Smits for their past contributions. We also thank Dr. N. Wex for supporting the calculations of the galactic acceleration as well as the related discussions. The EPTA is also grateful to staff at its observatories and telescopes who have made the continued observations possible. Author contributions: The European Pulsar Timing Array: JA, SB, ASBN, CGB, ABe, MBo, EB, PRB, MBu, RNC, AC, DJC, SCha, SChe, IC, GD, MF, RDF, AF, JRG, BG, EG, JMG, LG, YJG, HH, FI, DIV, JJan, JJaw, GHJ, AJ, RK, EFK, MJK, MK, MAK, KLa, KJL, KLi, YL, AGL, JWM, RAM, MBM, ICN, APa, BBPP, DP, APe, NKP, APo, HQL, ASa, SAS, ASe, GS, LS, RS, BWS, SCS, GT, CT, EvdW, AV, VVK, JPWV, JW, LW and ZW. The EPTA is a multi-decade effort and all authors have contributed through conceptualisation, funding acquisition, data-curation, methodology, software and hardware developments as well as (aspects of) the continued running of the observational campaigns, which includes writing and proofreading observing proposals, evaluating observations and observing systems, mentoring students, developing science cases. All authors also helped in (aspects of) verification of the data, analysis and results as well as in finalising the paper draft. Specific contributions from individual EPTA members are listed in the CRediT (https://credit.niso.org/) format below. The Indian Pulsar Timing Array: PA, SA, MB, ABa, SDa, DD, SDe, NDB, CD, YG, SH, BCJ, FK, DK, TK, NK, MAK, YM, KN, AKP, TP, PR, JS, ASr, MS, ASu, KT and PT. InPTA members contributed in uGMRT observations and data reduction to create the InPTA data set which is employed while assembling the DR2full+ and DR2new+ data sets. J.Jan., K.Li., G.M.S. equally share the correspondence of the paper. CRediT statement: Conceptualisation: APa, APo, AV, BWS, CGB, CT, GHJ, GMS, GT, IC, JA, JJan, JPWV, JW, JWM, KJL, KLi, MK. Methodology: APa, AV, DJC, GMS, IC, JA, JJan, JPWV, JWM, KJL, KLi, LG, MK. Software: AC, AJ, APa, CGB, DJC, GMS, IC, JA, JJan, JJaw, JPWV, KJL, KLi, LG, MJK, RK. Validation: AC, APa, CGB, CT, GMS, GT, IC, JA, JJan, JPWV, JWM, KLi, LG. Formal Analysis: APa, CGB, DJC, DP, EvdW, GHJ, GMS, JA, JJan, JPWV, JWM, KLi. Investigation: APa, APo, BWS, CGB, DJC, DP, GMS, GT, IC, JA, JJan, JPWV, JWM, KLi, LG, MBM, MBu, MJK, RK. Resources: APa, APe, APo, BWS, GHJ, GMS, GT, HH, IC, JA, JJan, JPWV, JWM, KJL, KLi, LG, MJK, MK, RK. Data Curation: AC, AJ, APa, BWS, CGB, DJC, DP, EG, EvdW, GHJ, GMS, GT, HH, IC, JA, JJan, JPWV, JWM, KLi, LG, MBM, MBu, MJK, MK, NKP, RK, SChe, YJG. Writing – Original Draft: APa, GMS, JA, JJan, KLi, LG. Writing – Review and Editing: AC, AF, APa, APo, DJC, EB, EFK, GHJ, GMS, GT, JA, JJan, JPWV, JWM, KLi, MK, SChe, VVK. Visualisation: APa, GMS, JA, JJan, KLi. Supervision: APo, ASe, AV, BWS, CGB, DJC, EFK, GHJ, GMS, GT, IC, JA, JPWV, KJL, KLi, LG, MJK, MK, VVK. Project Administration: APo, ASe, AV, BWS, CGB, CT, GHJ, GMS, GT, IC, JJan, JPWV, JWM, KLi, LG, MK. Funding Acquisition: APe, APo, ASe, BWS, GHJ, GT, IC, JA, JJan, LG, MJK, MK. Data Availability: Files containing the TOAs and pulsar timing models can be downloaded from https://epta.pages.in2p3.fr/epta-dr2/. The same site also provides the software environments necessary to recreate the timing analysis presented in this article.",

year = "2023",

month = oct,

day = "3",

doi = "10.1051/0004-6361/202346841",

language = "English",

volume = "678",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Antoniadis, J, Babak, S, Nielsen, A-SB, Bassa, CG, Berthereau, A, Bonetti, M, Bortolas, E, Brook, PR, Burgay, M, Caballero, RN, Chalumeau, A, Champion, DJ, Chanlaridis, S, Chen, S, Cognard, I, Desvignes, G, Falxa, M, Ferdman, RD, Franchini, A, Gair, JR, Goncharov, B, Graikou, E, Grießmeier, J-M, Guillemot, L, Guo, YJ, Hu, H, Iraci, F, Izquierdo-Villalba, D, Jang, J, Jawor, J, Janssen, GH, Jessner, A, Karuppusamy, R, Keane, EF, Keith, MJ, Kramer, M, Krishnakumar, MA, Lackeos, K, Lee, KJ, Liu, K, Liu, Y, Lyne, AG, McKee, JW, Main, RA, Mickaliger, MB, Nitu, IC, Parthasarathy, A, Perera, BBP, Perrodin, D, Petiteau, A, Porayko, NK, Possenti, A, Samajdar, HQLA, Sanidas, SA, Sesana, A, Shaifullah, G, Speri, L, Spiewak, R, Stappers, BW, Susarla, SC, Theureau, G, Tiburzi, C, Wateren, EVD, Vecchio, A, Krishnan, VV, Verbiest, JPW, Wang, J, Wang, L & Wu, Z 2023, 'The second data release from the European Pulsar Timing Array: I. The dataset and timing analysis', Astronomy and Astrophysics, vol. 678, A48. https://doi.org/10.1051/0004-6361/202346841

TY - JOUR

T1 - The second data release from the European Pulsar Timing Array

T2 - I. The dataset and timing analysis

AU - Antoniadis, J.

AU - Babak, S.

AU - Nielsen, A. -S. Bak

AU - Bassa, C. G.

AU - Berthereau, A.

AU - Bonetti, M.

AU - Bortolas, E.

AU - Brook, P. R.

AU - Burgay, M.

AU - Caballero, R. N.

AU - Chalumeau, A.

AU - Champion, D. J.

AU - Chanlaridis, S.

AU - Chen, S.

AU - Cognard, I.

AU - Desvignes, G.

AU - Falxa, M.

AU - Ferdman, R. D.

AU - Franchini, A.

AU - Gair, J. R.

AU - Goncharov, B.

AU - Graikou, E.

AU - Grießmeier, J. -M.

AU - Guillemot, L.

AU - Guo, Y. J.

AU - Hu, H.

AU - Iraci, F.

AU - Izquierdo-Villalba, D.

AU - Jang, J.

AU - Jawor, J.

AU - Janssen, G. H.

AU - Jessner, A.

AU - Karuppusamy, R.

AU - Keane, E. F.

AU - Keith, M. J.

AU - Kramer, M.

AU - Krishnakumar, M. A.

AU - Lackeos, K.

AU - Lee, K. J.

AU - Liu, K.

AU - Liu, Y.

AU - Lyne, A. G.

AU - McKee, J. W.

AU - Main, R. A.

AU - Mickaliger, M. B.

AU - Nitu, I. C.

AU - Parthasarathy, A.

AU - Perera, B. B. P.

AU - Perrodin, D.

AU - Petiteau, A.

AU - Porayko, N. K.

AU - Possenti, A.

AU - Samajdar, H. Quelquejay Leclere A.

AU - Sanidas, S. A.

AU - Sesana, A.

AU - Shaifullah, G.

AU - Speri, L.

AU - Spiewak, R.

AU - Stappers, B. W.

AU - Susarla, S. C.

AU - Theureau, G.

AU - Tiburzi, C.

AU - Wateren, E. van der

AU - Vecchio, A.

AU - Krishnan, V. Venkatraman

AU - Verbiest, J. P. W.

AU - Wang, J.

AU - Wang, L.

AU - Wu, Z.

N1 - Acknowledgments: The European Pulsar Timing Array (EPTA) is a collaboration between European and partner institutes, namely ASTRON (NL), INAF/Osservatorio di Cagliari (IT), Max-Planck-Institut für Radioastronomie (GER), Nançay/Paris Observatory (FRA), the University of Manchester (UK), the University of Birmingham (UK), the University of East Anglia (UK), the University of Bielefeld (GER), the University of Paris (FRA), the University of Milan-Bicocca (IT), the Foundation for Research and Technology, Hellas (GR), and Peking University (CHN), with the aim to provide high-precision pulsar timing to work towards the direct detection of low-frequency gravitational waves. An Advanced Grant of the European Research Council allowed to implement the Large European Array for Pulsars (LEAP) under Grant Agreement Number 227947 (PI: M. Kramer). The EPTA is part of the International Pulsar Timing Array (IPTA); we thank our IPTA colleagues for their support and help with this paper and the external Detection Committee members for their work on the Detection Checklist. Part of this work is based on observations with the 100-m telescope of the Max-Planck-Institut für Radioastronomie (MPIfR) at Effelsberg in Germany. Pulsar research at the Jodrell Bank Centre for Astrophysics and the observations using the Lovell Telescope are supported by a Consolidated Grant (ST/T000414/1) from the UK’s Science and Technology Facilities Council (STFC). I.C.N. is also supported by the STFC doctoral training grant ST/T506291/1. The Nançay radio Observatory is operated by the Paris Observatory, associated with the French Centre National de la Recherche Scientifique (CNRS), and partially supported by the Region Centre in France. We acknowledge financial support from “Programme National de Cosmologie and Galaxies” (PNCG), and “Programme National Hautes Energies” (PNHE) funded by CNRS/INSU-IN2P3-INP, CEA and CNES, France. We acknowledge financial support from Agence Nationale de la Recherche (ANR-18-CE31-0015), France. The Westerbork Synthesis Radio Telescope is operated by the Netherlands Institute for Radio Astronomy (ASTRON) with support from the Netherlands Foundation for Scientific Research (NWO). The Sardinia Radio Telescope (SRT) is funded by the Department of University and Research (MIUR), the Italian Space Agency (ASI), and the Autonomous Region of Sardinia (RAS) and is operated as a National Facility by the National Institute for Astrophysics (INAF). The work is supported by the National SKA programme of China (2020SKA0120100), Max-Planck Partner Group, NSFC 11690024, CAS Cultivation Project for FAST Scientific. This work is also supported as part of the “LEGACY” MPG-CAS collaboration on low-frequency gravitational wave astronomy. J.A. acknowledges support from the European Commission (Grant Agreement number: 101094354). J.A. and S.Cha. were partially supported by the Stavros Niarchos Foundation (SNF) and the Hellenic Foundation for Research and Innovation (H.F.R.I.) under the 2nd Call of the “Science and Society - Action Always strive for excellence – Theodoras Papazoglou” (Project Number: 01431). A.C. acknowledges support from the Paris Île-de-France Region. A.C., A.F., A.Se., A.Sa., E.B., D.I., G.M.S., M.Bo. acknowledge financial support provided under the European Union’s H2020 ERC Consolidator Grant “Binary Massive Black Hole Astrophysics” (B Massive, Grant Agreement: 818691). G.D., K.Li., R.K. and M.K. acknowledge support from European Research Council (ERC) Synergy Grant “BlackHoleCam”, Grant Agreement Number 610058. This work is supported by the ERC Advanced Grant “LEAP”, Grant Agreement Number 227947 (PI M. Kramer). A.V. and P.R.B. are supported by the UK’s Science and Technology Facilities Council (STFC; grant ST/W000946/1). A.V. also acknowledges the support of the Royal Society and Wolfson Foundation. J.P.W.V. acknowledges support by the Deutsche Forschungsgemeinschaft (DFG) through thew Heisenberg programme (Project No. 433075039) and by the NSF through AccelNet award #2114721. N.K.P. is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) – Projektnummer PO 2758/1–1, through the Walter-Benjamin programme. A.Sa. thanks the Alexander von Humboldt foundation in Germany for a Humboldt fellowship for postdoctoral researchers. A.Po., D.P. and M.Bu. acknowledge support from the research grant “iPeska” (P.I. Andrea Possenti) funded under the INAF national call Prin-SKA/CTA approved with the Presidential Decree 70/2016 (Italy). R.N.C. acknowledges financial support from the Special Account for Research Funds of the Hellenic Open University (ELKE-HOU) under the research programme “GRAVPUL” (K.E.-80383/grant agreement 319/10-10-2022: PI N. A. B. Gizani). E.v.d.W., C.G.B. and G.H.J. acknowledge support from the Dutch National Science Agenda, NWA Startimpuls – 400.17.608. B.G. is supported by the Italian Ministry of Education, University and Research within the PRIN 2017 Research Program Framework, n. 2017SYRTCN. L.S. acknowledges the use of the HPC system Cobra at the Max Planck Computing and Data Facility. The work presented here is a culmination of many years of data analysis as well as software and instrument development. In particular, we thank Drs. N. D’Amico, P.C.C. Freire, R. van Haasteren, C. Jordan, K. Lazaridis, P. Lazarus, L. Lentati, O. Löhmer and R. Smits for their past contributions. We also thank Dr. N. Wex for supporting the calculations of the galactic acceleration as well as the related discussions. The EPTA is also grateful to staff at its observatories and telescopes who have made the continued observations possible. Author contributions: The European Pulsar Timing Array: JA, SB, ASBN, CGB, ABe, MBo, EB, PRB, MBu, RNC, AC, DJC, SCha, SChe, IC, GD, MF, RDF, AF, JRG, BG, EG, JMG, LG, YJG, HH, FI, DIV, JJan, JJaw, GHJ, AJ, RK, EFK, MJK, MK, MAK, KLa, KJL, KLi, YL, AGL, JWM, RAM, MBM, ICN, APa, BBPP, DP, APe, NKP, APo, HQL, ASa, SAS, ASe, GS, LS, RS, BWS, SCS, GT, CT, EvdW, AV, VVK, JPWV, JW, LW and ZW. The EPTA is a multi-decade effort and all authors have contributed through conceptualisation, funding acquisition, data-curation, methodology, software and hardware developments as well as (aspects of) the continued running of the observational campaigns, which includes writing and proofreading observing proposals, evaluating observations and observing systems, mentoring students, developing science cases. All authors also helped in (aspects of) verification of the data, analysis and results as well as in finalising the paper draft. Specific contributions from individual EPTA members are listed in the CRediT (https://credit.niso.org/) format below. The Indian Pulsar Timing Array: PA, SA, MB, ABa, SDa, DD, SDe, NDB, CD, YG, SH, BCJ, FK, DK, TK, NK, MAK, YM, KN, AKP, TP, PR, JS, ASr, MS, ASu, KT and PT. InPTA members contributed in uGMRT observations and data reduction to create the InPTA data set which is employed while assembling the DR2full+ and DR2new+ data sets. J.Jan., K.Li., G.M.S. equally share the correspondence of the paper. CRediT statement: Conceptualisation: APa, APo, AV, BWS, CGB, CT, GHJ, GMS, GT, IC, JA, JJan, JPWV, JW, JWM, KJL, KLi, MK. Methodology: APa, AV, DJC, GMS, IC, JA, JJan, JPWV, JWM, KJL, KLi, LG, MK. Software: AC, AJ, APa, CGB, DJC, GMS, IC, JA, JJan, JJaw, JPWV, KJL, KLi, LG, MJK, RK. Validation: AC, APa, CGB, CT, GMS, GT, IC, JA, JJan, JPWV, JWM, KLi, LG. Formal Analysis: APa, CGB, DJC, DP, EvdW, GHJ, GMS, JA, JJan, JPWV, JWM, KLi. Investigation: APa, APo, BWS, CGB, DJC, DP, GMS, GT, IC, JA, JJan, JPWV, JWM, KLi, LG, MBM, MBu, MJK, RK. Resources: APa, APe, APo, BWS, GHJ, GMS, GT, HH, IC, JA, JJan, JPWV, JWM, KJL, KLi, LG, MJK, MK, RK. Data Curation: AC, AJ, APa, BWS, CGB, DJC, DP, EG, EvdW, GHJ, GMS, GT, HH, IC, JA, JJan, JPWV, JWM, KLi, LG, MBM, MBu, MJK, MK, NKP, RK, SChe, YJG. Writing – Original Draft: APa, GMS, JA, JJan, KLi, LG. Writing – Review and Editing: AC, AF, APa, APo, DJC, EB, EFK, GHJ, GMS, GT, JA, JJan, JPWV, JWM, KLi, MK, SChe, VVK. Visualisation: APa, GMS, JA, JJan, KLi. Supervision: APo, ASe, AV, BWS, CGB, DJC, EFK, GHJ, GMS, GT, IC, JA, JPWV, KJL, KLi, LG, MJK, MK, VVK. Project Administration: APo, ASe, AV, BWS, CGB, CT, GHJ, GMS, GT, IC, JJan, JPWV, JWM, KLi, LG, MK. Funding Acquisition: APe, APo, ASe, BWS, GHJ, GT, IC, JA, JJan, LG, MJK, MK. Data Availability: Files containing the TOAs and pulsar timing models can be downloaded from https://epta.pages.in2p3.fr/epta-dr2/. The same site also provides the software environments necessary to recreate the timing analysis presented in this article.

PY - 2023/10/3

Y1 - 2023/10/3

N2 - Pulsar timing arrays offer a probe of the low-frequency gravitational wave spectrum (1 - 100 nanohertz), which is intimately connected to a number of markers that can uniquely trace the formation and evolution of the Universe. We present the dataset and the results of the timing analysis from the second data release of the European Pulsar Timing Array (EPTA). The dataset contains high-precision pulsar timing data from 25 millisecond pulsars collected with the five largest radio telescopes in Europe, as well as the Large European Array for Pulsars. The dataset forms the foundation for the search for gravitational waves by the EPTA, presented in associated papers. We describe the dataset and present the results of the frequentist and Bayesian pulsar timing analysis for individual millisecond pulsars that have been observed over the last ~25 years. We discuss the improvements to the individual pulsar parameter estimates, as well as new measurements of the physical properties of these pulsars and their companions. This data release extends the dataset from EPTA Data Release 1 up to the beginning of 2021, with individual pulsar datasets with timespans ranging from 14 to 25 years. These lead to improved constraints on annual parallaxes, secular variation of the orbital period, and Shapiro delay for a number of sources. Based on these results, we derived astrophysical parameters that include distances, transverse velocities, binary pulsar masses, and annual orbital parallaxes.

AB - Pulsar timing arrays offer a probe of the low-frequency gravitational wave spectrum (1 - 100 nanohertz), which is intimately connected to a number of markers that can uniquely trace the formation and evolution of the Universe. We present the dataset and the results of the timing analysis from the second data release of the European Pulsar Timing Array (EPTA). The dataset contains high-precision pulsar timing data from 25 millisecond pulsars collected with the five largest radio telescopes in Europe, as well as the Large European Array for Pulsars. The dataset forms the foundation for the search for gravitational waves by the EPTA, presented in associated papers. We describe the dataset and present the results of the frequentist and Bayesian pulsar timing analysis for individual millisecond pulsars that have been observed over the last ~25 years. We discuss the improvements to the individual pulsar parameter estimates, as well as new measurements of the physical properties of these pulsars and their companions. This data release extends the dataset from EPTA Data Release 1 up to the beginning of 2021, with individual pulsar datasets with timespans ranging from 14 to 25 years. These lead to improved constraints on annual parallaxes, secular variation of the orbital period, and Shapiro delay for a number of sources. Based on these results, we derived astrophysical parameters that include distances, transverse velocities, binary pulsar masses, and annual orbital parallaxes.

KW - (Stars:) pulsars: general

KW - (Stars:) pulsars

KW - Gravitational waves

KW - Astronomical instrumentation, methods, and techniques

U2 - 10.1051/0004-6361/202346841

DO - 10.1051/0004-6361/202346841

M3 - Article

SN - 0004-6361

VL - 678

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A48

ER -

The second data release from the European Pulsar Timing Array: I. The dataset and timing analysis

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