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 - Theodoros 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 the 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" (PI. 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, 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 DR2full1+ 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, KJL, 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, A48, page 16 of 28

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.

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5 ASTRON, Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD, Dwingeloo, The Netherlands

6 Laboratoire de Physique et Chimie de l'Environnement et de l'Espace, Université d'Orléans / CNRS, 45071 Orléans Cedex 02, France

7 Observatoire Radioastronomique de Nançay, Observatoire de Paris, Université PSL, Université d'Orléans, CNRS, 18330 Nançay, France

8 Dipartimento di Fisica "G. Occhialini", Università degli Studi di Milano-Bicocca, Piazza della Scienza 3, 20126 Milano, Italy

9 INFN, Sezione di Milano-Bicocca, Piazza della Scienza 3, 20126 Milano, Italy

10 INAF – Osservatorio Astronomico di Brera, via Brera 20, 20121 Milano, Italy

11 Institute for Gravitational Wave Astronomy and School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK

12 INAF – Osservatorio Astronomico di Cagliari, via della Scienza 5, 09047 Selargius (CA), Italy

13 Hellenic Open University, School of Science and Technology, 26335 Patras, Greece

14 Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, PR China

15 School of Physics, Faculty of Science, University of East Anglia, Norwich NR4 7TJ, UK

16 Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, 14476 Potsdam, Germany

17 Gran Sasso Science Institute (GSSI), 67100 L'Aquila, Italy

18 INFN, Laboratori Nazionali del Gran Sasso, I67100 Assergi, Italy

19 Università di Cagliari, Dipartimento di Fisica, S.P. Monserrato-Sestu Km 0,700, 09042 Monserrato (CA), Italy

20 Department of Astrophysics/IMAPP, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands

21 School of Physics, Trinity College Dublin, College Green, Dublin 2, D02 PN40, Ireland

22 Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, University of Manchester, Manchester M13 9PL, UK

23 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, PR China

24 E.A. Milne Centre for Astrophysics, University of Hull, Cottingham Road, Kingston-upon-Hull HU6 7RX, UK

25 Centre of Excellence for Data Science, Artificial Intelligence and Modelling (DAIM), University of Hull, Cottingham Road, Kingston-upon-Hull, HU6 7RX, UK

26 Arecibo Observatory, HC3 Box 53995, Arecibo, PR 00612, USA

27 IRFU, CEA, Université Paris-Saclay, 91191 Gif-sur-Yvette, France

28 Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany

29 Ollscoil na Gaillimhe – University of Galway, University Road, Galway H91 TK33, Ireland

30 Laboratoire Univers et Théories LUTh, Observatoire de Paris, Université PSL, CNRS, Université de Paris, 92190 Meudon, France

31 Florida Space Institute, University of Central Florida, 12354 Research Parkway, Partnership 1 Building, Suite 214, Orlando, FL 32826-0650, USA

32 Ruhr University Bochum, Faculty of Physics and Astronomy, Astronomical Institute (AIRUB), 44780 Bochum, Germany

33 Advanced Institute of Natural Sciences, Beijing Normal University, Zhuhai 519087, PR China

<footnote n="1">¹ Institute of Astrophysics, FORTH, N. Plastira 100, 70013 Heraklion, Greece</footnote>

<footnote n="2">² Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany</footnote>

<footnote n="3">³ Université Paris Cité, CNRS, Astroparticule et Cosmologie, 75013 Paris, France</footnote>

<footnote n="4">⁴ Fakultät für Physik, Universität Bielefeld, Postfach 100131, 33501 Bielefeld, Germany</footnote>
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Petit, G. 2009, Proc. Int. Astron. Union, 5, 220

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Rosado, P. A., Sesana, A., & Gair, J. 2015, MNRAS, 451, 2417

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Taylor, J. H. 1992, Philos. Trans. Roy. Soc. London A, 341, 117

Tiburzi, C., Shaifullah, G. M., Bassa, C. G., et al. 2021, A&A, 647, A84

van Cappellen, W. A., Oosterloo, T. A., Verheijen, M. A. W., et al. 2022, A&A, 658, A146

van Kerkwijk, M. H., Bergeron, P., & Kulkarni, S. R. 1996, ApJ, 467, L89

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van Straten, W., Demorest, P., & Osłowski, S. 2012, Astron. Res. Technol., 9, 237

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Zhu, W. W., Desvignes, G., Wex, N., et al. 2019, MNRAS, 482, 3249

5 ASTRON, Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD, Dwingeloo, The Netherlands

6 Laboratoire de Physique et Chimie de l'Environnement et de l'Espace, Université d'Orléans / CNRS, 45071 Orléans Cedex 02, France

7 Observatoire Radioastronomique de Nançay, Observatoire de Paris, Université PSL, Université d'Orléans, CNRS, 18330 Nançay, France

8 Dipartimento di Fisica "G. Occhialini", Università degli Studi di Milano-Bicocca, Piazza della Scienza 3, 20126 Milano, Italy

9 INFN, Sezione di Milano-Bicocca, Piazza della Scienza 3, 20126 Milano, Italy

10 INAF – Osservatorio Astronomico di Brera, via Brera 20, 20121 Milano, Italy

11 Institute for Gravitational Wave Astronomy and School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK

12 INAF – Osservatorio Astronomico di Cagliari, via della Scienza 5, 09047 Selargius (CA), Italy

13 Hellenic Open University, School of Science and Technology, 26335 Patras, Greece

14 Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, PR China

15 School of Physics, Faculty of Science, University of East Anglia, Norwich NR4 7TJ, UK

16 Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, 14476 Potsdam, Germany

17 Gran Sasso Science Institute (GSSI), 67100 L'Aquila, Italy

18 INFN, Laboratori Nazionali del Gran Sasso, I67100 Assergi, Italy

19 Università di Cagliari, Dipartimento di Fisica, S.P. Monserrato-Sestu Km 0,700, 09042 Monserrato (CA), Italy

20 Department of Astrophysics/IMAPP, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands

21 School of Physics, Trinity College Dublin, College Green, Dublin 2, D02 PN40, Ireland

22 Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, University of Manchester, Manchester M13 9PL, UK

23 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, PR China

24 E.A. Milne Centre for Astrophysics, University of Hull, Cottingham Road, Kingston-upon-Hull HU6 7RX, UK

25 Centre of Excellence for Data Science, Artificial Intelligence and Modelling (DAIM), University of Hull, Cottingham Road, Kingston-upon-Hull, HU6 7RX, UK

26 Arecibo Observatory, HC3 Box 53995, Arecibo, PR 00612, USA

27 IRFU, CEA, Université Paris-Saclay, 91191 Gif-sur-Yvette, France

28 Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany

29 Ollscoil na Gaillimhe – University of Galway, University Road, Galway H91 TK33, Ireland

30 Laboratoire Univers et Théories LUTh, Observatoire de Paris, Université PSL, CNRS, Université de Paris, 92190 Meudon, France

31 Florida Space Institute, University of Central Florida, 12354 Research Parkway, Partnership 1 Building, Suite 214, Orlando, FL 32826-0650, USA

32 Ruhr University Bochum, Faculty of Physics and Astronomy, Astronomical Institute (AIRUB), 44780 Bochum, Germany

33 Advanced Institute of Natural Sciences, Beijing Normal University, Zhuhai 519087, PR China

<footnote n="1">¹ Institute of Astrophysics, FORTH, N. Plastira 100, 70013 Heraklion, Greece</footnote>

<footnote n="2">² Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany</footnote>

<footnote n="3">³ Université Paris Cité, CNRS, Astroparticule et Cosmologie, 75013 Paris, France</footnote>

<footnote n="4">⁴ Fakultät für Physik, Universität Bielefeld, Postfach 100131, 33501 Bielefeld, Germany</footnote>
## Appendix A: Dataset versions

The full EPTA DR2 dataset, hereafter referred to as “DR2full”, is the primary source of data for the pulsar timing analyses presented in this paper, as well as the accompanying articles on the single-pulsar noise analysis (EPTA Collaboration & InPTA Collaboration 2023a) and the search for correlated signals in (EPTA Collaboration & InPTA Collaboration 2023b). Apart from the DR2full, additional datasets were created, guided by iterative analyses carried out during the detailed investigation of single pulsar noise models in EPTA Collaboration & InPTA Collaboration (2023a), as well as multiple analyses carried out to search for artefacts and spurious signals in the common signal searches carried out in EPTA Collaboration & InPTA Collaboration (2023b).

The first of these, the ‘DR2full+’, consists of a combination of the DR2full dataset with the first data release of the InPTA (henceforth InPTA-DR1 Tarafdar et al. 2022) for an overlapping set of 10 pulsars, marked with an asterisk in Table 2. This dataset aims to improve the overall sensitivity of the DR2full to DM-variation linked noise-processes. The combination was performed using the ‘narrowband’ TOAs from the InPTA-DR1 for two observing bands centred around 500 MHz and 1460 MHz, respectively. Unlike the EPTA data, the InPTA-DR1 data requires optimisation based on the flux density of the pulsar being observed, as well as, observing setup specific details leading to changes in the number of sub-bands generated, ranging from a minimum of 4 to a maximum of 16. We refer interested readers to Tarafdar et al. (2022) for the full details on the InPTA-DR1 data processing. To combine the InPTA-DR1 data with the EPTA DR2 data, for each pulsar we used the ephemeris produced from the EPTA DR2 dataset and followed the same steps as described in Section 3. Specifically, we fitted for phase offset for each sub-band in the InPTA data individually with respect to the reference system in the EPTA data (see Section 3).

The single-pulsar noise analysis of these additional sets of data are presented in EPTA Collaboration & InPTA Collaboration (2023a). For the ‘DR2full+’ dataset, we performed single-pulsar Bayesian timing analysis following the same description as in Section 3.4, using customised noise models determined by EPTA Collaboration & InPTA Collaboration (2023a). The results of this analysis were later used for the gravitational wave searches presented in EPTA Collaboration & InPTA Collaboration (2023b).

<table><caption>Table A.1: Overview of the name designations for the EPTA dataset</caption><thead><tr><th>Dataset</th><th>MJD range</th><th>Notes</th></tr></thead><tbody><tr><td>DR2full</td><td>50360.76 – 59385.10</td><td>Full EPTA DR2 data</td></tr><tr><td>DR2new</td><td>55611.40 – 59385.10</td><td>Data only from the new backends collected in the past 10 yr</td></tr><tr><td>DR2full+</td><td>50360.76 – 59644.16</td><td>DR2full + InPTA DR1 for 10 overlap pulsars</td></tr><tr><td>DR2new+</td><td>55611.40 – 59644.16</td><td>DR2new + InPTA DR1 for 10 overlap pulsars</td></tr></tbody></table>

A significant difference between the EPTA DR1 and DR2 datasets lies in the use of the technique of coherent dedispersion. This allows for a far more accurate modelling of the frequency-

dependent DM delays, leading to the recovery of a sharper profile and thus, improved timing performance. To test the improvements derived from using only coherently dedispersed data, the ‘DR2new’ dataset was created. This dataset spans, approximately, the final 10.3 yr. Similar to the DR2full dataset, we also appended InPTA-DR1 data to the DR2new to produce the ‘DR2new+’ dataset.
## Appendix A: Dataset versions

The full EPTA DR2 dataset, hereafter referred to as “DR2full”, is the primary source of data for the pulsar timing analyses presented in this paper, as well as the accompanying articles on the single-pulsar noise analysis (EPTA Collaboration & InPTA Collaboration 2023a) and the search for correlated signals in (EPTA Collaboration & InPTA Collaboration 2023b). Apart from the DR2full, additional datasets were created, guided by iterative analyses carried out during the detailed investigation of single pulsar noise models in EPTA Collaboration & InPTA Collaboration (2023a), as well as multiple analyses carried out to search for artefacts and spurious signals in the common signal searches carried out in EPTA Collaboration & InPTA Collaboration (2023b).

The first of these, the ‘DR2full+’, consists of a combination of the DR2full dataset with the first data release of the InPTA (henceforth InPTA-DR1 Tarafdar et al. 2022) for an overlapping set of 10 pulsars, marked with an asterisk in Table 2. This dataset aims to improve the overall sensitivity of the DR2full to DM-variation linked noise-processes. The combination was performed using the ‘narrowband’ TOAs from the InPTA-DR1 for two observing bands centred around 500 MHz and 1460 MHz, respectively. Unlike the EPTA data, the InPTA-DR1 data requires optimisation based on the flux density of the pulsar being observed, as well as, observing setup specific details leading to changes in the number of sub-bands generated, ranging from a minimum of 4 to a maximum of 16. We refer interested readers to Tarafdar et al. (2022) for the full details on the InPTA-DR1 data processing. To combine the InPTA-DR1 data with the EPTA DR2 data, for each pulsar we used the ephemeris produced from the EPTA DR2 dataset and followed the same steps as described in Section 3. Specifically, we fitted for phase offset for each sub-band in the InPTA data individually with respect to the reference system in the EPTA data (see Section 3).

The single-pulsar noise analysis of these additional sets of data are presented in EPTA Collaboration & InPTA Collaboration (2023a). For the ‘DR2full+’ dataset, we performed single-pulsar Bayesian timing analysis following the same description as in Section 3.4, using customised noise models determined by EPTA Collaboration & InPTA Collaboration (2023a). The results of this analysis were later used for the gravitational wave searches presented in EPTA Collaboration & InPTA Collaboration (2023b).

<table><caption>Table A.1: Overview of the name designations for the EPTA dataset</caption><thead><tr><th>Dataset</th><th>MJD range</th><th>Notes</th></tr></thead><tbody><tr><td>DR2full</td><td>50360.76 – 59385.10</td><td>Full EPTA DR2 data</td></tr><tr><td>DR2new</td><td>55611.40 – 59385.10</td><td>Data only from the new backends collected in the past 10 yr</td></tr><tr><td>DR2full+</td><td>50360.76 – 59644.16</td><td>DR2full + InPTA DR1 for 10 overlap pulsars</td></tr><tr><td>DR2new+</td><td>55611.40 – 59644.16</td><td>DR2new + InPTA DR1 for 10 overlap pulsars</td></tr></tbody></table>

A significant difference between the EPTA DR1 and DR2 datasets lies in the use of the technique of coherent dedispersion. This allows for a far more accurate modelling of the frequency-

dependent DM delays, leading to the recovery of a sharper profile and thus, improved timing performance. To test the improvements derived from using only coherently dedispersed data, the ‘DR2new’ dataset was created. This dataset spans, approximately, the final 10.3 yr. Similar to the DR2full dataset, we also appended InPTA-DR1 data to the DR2new to produce the ‘DR2new+’ dataset.
## Appendix B: Pulsar Ephemerides

<table><caption>Table B.1: Measured timing model parameters for PSRs J0030+0451, J0613–0200, J0751+1807 and J0900–3144. Here the epoch of spin frequency, sky position and DM are all set to MJD 55000. The definitions of the proper motion terms are: $\mu_{\alpha} = \dot{\alpha} \cos \delta, \mu_{\delta} = \dot{\delta}, \mu_{\lambda} = \dot{\lambda} \cos \beta, \mu_{\beta} = \dot{\beta}$. The components in the red-noise model used in the Bayesian analysis to obtain the timing solution are shown in the last row, where RN, DM, SV stand for achromatic red noise, chromatic red noise for DM variation, and scattering variation, respectively. All of the above apply to all tables in this section.</caption><thead><tr><th>Pulsar Jname</th><th>J0030+0451</th><th>J0613–0200</th><th>J0751+1807</th><th>J0900–3144</th></tr></thead><tbody><tr><td>Right ascension, α (J2000)</td><td>—</td><td>06:13:43.975688(1)</td><td>07:51:09.155329(6)</td><td>09:00:43.953105(8)</td></tr><tr><td>Declination, δ (J2000)</td><td>—</td><td>-02:00:47.22541(4)</td><td>18:07:38.4858(5)</td><td>-31:44:30.8950(1)</td></tr><tr><td>Ecliptic longitude λ (deg)</td><td>8.910356334(10)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Ecliptic latitude β (deg)</td><td>1.4456958(4)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Spin frequency, ν (Hz)</td><td>205.530695938456(2)</td><td>326.6005620234831(4)</td><td>287.457853995106(1)</td><td>90.011841919354(1)</td></tr><tr><td>Spin frequency derivative, ṽ (s<sup>-2</sup>)</td><td>-4.2977(1) × 10<sup>-16</sup></td><td>-1.023017(8) × 10<sup>-15</sup></td><td>-6.43455(6) × 10<sup>-16</sup></td><td>-3.96012(7) × 10<sup>-16</sup></td></tr><tr><td>DM (cm<sup>-3</sup> pc)</td><td>4.331(1)</td><td>38.7759(7)</td><td>30.2457(8)</td><td>75.691(2)</td></tr><tr><td>DM1 (cm<sup>-3</sup> pc yr<sup>-1</sup>)</td><td>0.0002(1)</td><td>-8(2) × 10<sup>-5</sup></td><td>-0.00046(7)</td><td>0.0009(5)</td></tr><tr><td>DM2 (cm<sup>-3</sup> pc yr<sup>-2</sup>)</td><td>-2(2) × 10<sup>-5</sup></td><td>-1.8(6) × 10<sup>-5</sup></td><td>10(20) × 10<sup>-6</sup></td><td>-0.00019(9)</td></tr><tr><td>Proper motion in α, μ<sub>α</sub> (mas yr<sup>-1</sup>)</td><td>—</td><td>1.837(2)</td><td>-2.70(1)</td><td>-1.03(2)</td></tr><tr><td>Proper motion in δ, μ<sub>δ</sub> (mas yr<sup>-1</sup>)</td><td>—</td><td>-10.359(6)</td><td>-13.27(7)</td><td>1.99(2)</td></tr><tr><td>Proper motion in λ, μ<sub>λ</sub> (mas yr<sup>-1</sup>)</td><td>-5.523(5)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Proper motion in β, μ<sub>β</sub> (mas yr<sup>-1</sup>)</td><td>3.1(2)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Parallax, ω (mas)</td><td>3.09(6)</td><td>1.00(5)</td><td>0.85(4)</td><td>—</td></tr><tr><td>Binary model</td><td>—</td><td>T2</td><td>T2</td><td>T2</td></tr><tr><td>Orbital period, P<sub>b</sub> (d)</td><td>—</td><td>1.198512575192(8)</td><td>0.263144270793(3)</td><td>18.7376360584(1)</td></tr><tr><td>Projected semi-major axis, x (s)</td><td>—</td><td>1.09144411(2)</td><td>0.3966135(1)</td><td>17.24880996(4)</td></tr><tr><td>Epoch of ascending node (MJD), T<sub>asc</sub></td><td>—</td><td>53113.79635421(1)</td><td>51800.21586830(2)</td><td>52678.63028838(3)</td></tr><tr><td>x̄ component of the eccentricity, κ</td><td>—</td><td>4.05(4)×10<sup>-6</sup></td><td>2.9(1) × 10<sup>-6</sup></td><td>9.884(5)×10<sup>-6</sup></td></tr><tr><td>ȳ component of the eccentricity, η</td><td>—</td><td>3.50(4)×10<sup>-6</sup></td><td>3(1)×10<sup>-7</sup></td><td>3.484(4)×10<sup>-6</sup></td></tr><tr><td>Orbital period derivative, P̄<sub>b</sub></td><td>—</td><td>3.5(2)×10<sup>-14</sup></td><td>-3.50(5) × 10<sup>-14</sup></td><td>—</td></tr><tr><td>Derivative of x, ẋ</td><td>—</td><td>—</td><td>2(2)×10<sup>-16</sup></td><td>—</td></tr><tr><td>3rd harmonic of Shapiro delay, h<sub>3</sub> (s)</td><td>—</td><td>2.6(2)×10<sup>-7</sup></td><td>1.9(2)×10<sup>-7</sup></td><td>—</td></tr><tr><td>4th harmonic of Shapiro delay, h<sub>4</sub> (s)</td><td>—</td><td>—</td><td>4(23)×10<sup>-9</sup></td><td>—</td></tr><tr><td>Ratio of harmonics amplitude, ζ</td><td>—</td><td>0.69(4)</td><td>—</td><td>—</td></tr><tr><td>Noise model</td><td>RN</td><td>RN, DM</td><td>DM</td><td>RN, DM</td></tr></tbody></table>

The measurements of the pulsar timing parameters obtained from the Bayesian timing analysis are presented in the following pages, in Tables B.1–B.7 for all 25 EPTA DR2 pulsars. The measurement values are the medians of the posterior distributions and the errors denote the 1-σ confidence intervals for the respective parameters.
## Appendix B: Pulsar Ephemerides

<table><caption>Table B.1: Measured timing model parameters for PSRs J0030+0451, J0613–0200, J0751+1807 and J0900–3144. Here the epoch of spin frequency, sky position and DM are all set to MJD 55000. The definitions of the proper motion terms are: $\mu_{\alpha} = \dot{\alpha} \cos \delta, \mu_{\delta} = \dot{\delta}, \mu_{\lambda} = \dot{\lambda} \cos \beta, \mu_{\beta} = \dot{\beta}$. The components in the red-noise model used in the Bayesian analysis to obtain the timing solution are shown in the last row, where RN, DM, SV stand for achromatic red noise, chromatic red noise for DM variation, and scattering variation, respectively. All of the above apply to all tables in this section.</caption><thead><tr><th>Pulsar Jname</th><th>J0030+0451</th><th>J0613-0200</th><th>J0751+1807</th><th>J0900-3144</th></tr></thead><tbody><tr><td>Right ascension, α (J2000)</td><td>—</td><td>06:13:43.975688(1)</td><td>07:51:09.155329(6)</td><td>09:00:43.953105(8)</td></tr><tr><td>Declination, δ (J2000)</td><td>—</td><td>-02:00:47.22541(4)</td><td>18:07:38.4858(5)</td><td>-31:44:30.8950(1)</td></tr><tr><td>Ecliptic longitude λ (deg)</td><td>8.910356334(10)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Ecliptic latitude β (deg)</td><td>1.4456958(4)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Spin frequency, ν (Hz)</td><td>205.530695938456(2)</td><td>326.6005620234831(4)</td><td>287.457853995106(1)</td><td>90.011841919354(1)</td></tr><tr><td>Spin frequency derivative, ṽ (s<sup>-2</sup>)</td><td>-4.2977(1) × 10<sup>-16</sup></td><td>-1.023017(8) × 10<sup>-15</sup></td><td>-6.43455(6) × 10<sup>-16</sup></td><td>-3.96012(7) × 10<sup>-16</sup></td></tr><tr><td>DM (cm<sup>-3</sup> pc)</td><td>4.331(1)</td><td>38.7759(7)</td><td>30.2457(8)</td><td>75.691(2)</td></tr><tr><td>DM1 (cm<sup>-3</sup> pc yr<sup>-1</sup>)</td><td>0.0002(1)</td><td>-8(2) × 10<sup>-5</sup></td><td>-0.00046(7)</td><td>0.0009(5)</td></tr><tr><td>DM2 (cm<sup>-3</sup> pc yr<sup>-2</sup>)</td><td>-2(2) × 10<sup>-5</sup></td><td>-1.8(6) × 10<sup>-5</sup></td><td>10(20) × 10<sup>-6</sup></td><td>-0.00019(9)</td></tr><tr><td>Proper motion in α, μ<sub>α</sub> (mas yr<sup>-1</sup>)</td><td>—</td><td>1.837(2)</td><td>-2.70(1)</td><td>-1.03(2)</td></tr><tr><td>Proper motion in δ, μ<sub>δ</sub> (mas yr<sup>-1</sup>)</td><td>—</td><td>-10.359(6)</td><td>-13.27(7)</td><td>1.99(2)</td></tr><tr><td>Proper motion in λ, μ<sub>λ</sub> (mas yr<sup>-1</sup>)</td><td>-5.523(5)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Proper motion in β, μ<sub>β</sub> (mas yr<sup>-1</sup>)</td><td>3.1(2)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Parallax, ω (mas)</td><td>3.09(6)</td><td>1.00(5)</td><td>0.85(4)</td><td>—</td></tr><tr><td>Binary model</td><td>—</td><td>T2</td><td>T2</td><td>T2</td></tr><tr><td>Orbital period, P<sub>b</sub> (d)</td><td>—</td><td>1.198512575192(8)</td><td>0.263144270793(3)</td><td>18.7376360584(1)</td></tr><tr><td>Projected semi-major axis, x (s)</td><td>—</td><td>1.09144411(2)</td><td>0.3966135(1)</td><td>17.24880996(4)</td></tr><tr><td>Epoch of ascending node (MJD), T<sub>asc</sub></td><td>—</td><td>53113.79635421(1)</td><td>51800.21586830(2)</td><td>52678.63028838(3)</td></tr><tr><td>x̄ component of the eccentricity, κ</td><td>—</td><td>4.05(4)×10<sup>-6</sup></td><td>2.9(1) × 10<sup>-6</sup></td><td>9.884(5)×10<sup>-6</sup></td></tr><tr><td>ȳ component of the eccentricity, η</td><td>—</td><td>3.50(4)×10<sup>-6</sup></td><td>3(1)×10<sup>-7</sup></td><td>3.484(4)×10<sup>-6</sup></td></tr><tr><td>Orbital period derivative, P̄<sub>b</sub></td><td>—</td><td>3.5(2)×10<sup>-14</sup></td><td>-3.50(5) × 10<sup>-14</sup></td><td>—</td></tr><tr><td>Derivative of x, ẋ</td><td>—</td><td>—</td><td>2(2)×10<sup>-16</sup></td><td>—</td></tr><tr><td>3rd harmonic of Shapiro delay, h<sub>3</sub> (s)</td><td>—</td><td>2.6(2)×10<sup>-7</sup></td><td>1.9(2)×10<sup>-7</sup></td><td>—</td></tr><tr><td>4th harmonic of Shapiro delay, h<sub>4</sub> (s)</td><td>—</td><td>—</td><td>4(23)×10<sup>-9</sup></td><td>—</td></tr><tr><td>Ratio of harmonics amplitude, ζ</td><td>—</td><td>0.69(4)</td><td>—</td><td>—</td></tr><tr><td>Noise model</td><td>RN</td><td>RN, DM</td><td>DM</td><td>RN, DM</td></tr></tbody></table>

The measurements of the pulsar timing parameters obtained from the Bayesian timing analysis are presented in the following pages, in Tables B.1–B.7 for all 25 EPTA DR2 pulsars. The measurement values are the medians of the posterior distributions and the errors denote the 1-σ confidence intervals for the respective parameters.
<table><caption>Table B.2: Measured timing model parameters for PSRs J1012+5307, J1022+1001, J1024–0719, J1455–3330.</caption><thead><tr><th>Pulsar Jname</th><th>J1012+5307</th><th>J1022+1001</th><th>J1024–0719</th><th>J1455–3330</th></tr></thead><tbody><tr><td>Right ascension, α (J2000)</td><td>10:12:33.437537(2)</td><td>—</td><td>10:24:38.675394(3)</td><td>14:55:47.969872(8)</td></tr><tr><td>Declination, δ (J2000)</td><td>53:07:2.30023(3)</td><td>—</td><td>-07:19:19.43377(8)</td><td>-33:30:46.3803(2)</td></tr><tr><td>Ecliptic longitude λ (deg)</td><td>—</td><td>153.865866923(8)</td><td>—</td><td>—</td></tr><tr><td>Ecliptic latitude β (deg)</td><td>—</td><td>-0.063926(8)</td><td>—</td><td>—</td></tr><tr><td>Spin frequency, ν (Hz)</td><td>190.2678344415654(2)</td><td>60.7794479566973(2)</td><td>193.715683448548(2)</td><td>125.200243244993(2)</td></tr><tr><td>Spin frequency derivative, ṽ (s<sup>-2</sup>)</td><td>-6.20041(2) × 10<sup>-16</sup></td><td>-1.60094(1) × 10<sup>-16</sup></td><td>-6.9593(2) × 10<sup>-16</sup></td><td>-3.8097(1) × 10<sup>-16</sup></td></tr><tr><td>Second spin frequency derivative, ṽ (s<sup>-3</sup>)</td><td>—</td><td>—</td><td>-3.57(7) × 10<sup>-27</sup></td><td>—</td></tr><tr><td>DM (cm<sup>-3</sup> pc)</td><td>9.0211(4)</td><td>10.2580(9)</td><td>6.4885(10)</td><td>13.569(3)</td></tr><tr><td>DM1 (cm<sup>-3</sup> pc yr<sup>-1</sup>)</td><td>0.00012(1)</td><td>-0.00016(6)</td><td>0.0004(2)</td><td>0.0004(3)</td></tr><tr><td>DM2 (cm<sup>-3</sup> pc yr<sup>-2</sup>)</td><td>1.6(3) × 10<sup>-5</sup></td><td>4.1(9) × 10<sup>-5</sup></td><td>-9(4) × 10<sup>-5</sup></td><td>-4(4) × 10<sup>-5</sup></td></tr><tr><td>Proper motion in α, μ<sub>α</sub> (mas yr<sup>-1</sup>)</td><td>2.624(3)</td><td>—</td><td>-35.277(5)</td><td>7.85(1)</td></tr><tr><td>Proper motion in δ, μ<sub>δ</sub> (mas yr<sup>-1</sup>)</td><td>-25.487(4)</td><td>—</td><td>-48.23(1)</td><td>-1.98(4)</td></tr><tr><td>Proper motion in λ, μ<sub>λ</sub> (mas yr<sup>-1</sup>)</td><td>—</td><td>-15.916(4)</td><td>—</td><td>—</td></tr><tr><td>Proper motion in β, μ<sub>β</sub> (mas yr<sup>-1</sup>)</td><td>—</td><td>-18(4)</td><td>—</td><td>—</td></tr><tr><td>Parallax, σ (mas)</td><td>0.90(8)</td><td>1.16(8)</td><td>1.01(4)</td><td>1.3(1)</td></tr><tr><td>Binary model</td><td>T2</td><td>DDH</td><td>—</td><td>T2</td></tr><tr><td>Orbital period, P<sub>b</sub> (d)</td><td>0.604672722921(3)</td><td>7.8051340(2)</td><td>—</td><td>76.17456861(2)</td></tr><tr><td>Projected semi-major axis, x (s)</td><td>0.58181715(6)</td><td>16.7654035(5)</td><td>—</td><td>32.3622232(5)</td></tr><tr><td>Longitude of periastron, ω (deg)</td><td>—</td><td>97.711(8)</td><td>—</td><td>223.458(1)</td></tr><tr><td>Epoch of periastron, T<sub>0</sub> (MJD)</td><td>—</td><td>50246.7172(2)</td><td>—</td><td>48980.1327(3)</td></tr><tr><td>Epoch of ascending node (MJD), T<sub>asc</sub></td><td>50700.08174601(1)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Orbital eccentricity, e</td><td>—</td><td>9.697(1) × 10<sup>-5</sup></td><td>—</td><td>0.000169646(4)</td></tr><tr><td>x̂ component of the eccentricity, κ</td><td>1.18(5) × 10<sup>-6</sup></td><td>—</td><td>—</td><td>—</td></tr><tr><td>ŷ component of the eccentricity, η</td><td>9(5) × 10<sup>-8</sup></td><td>—</td><td>—</td><td>—</td></tr><tr><td>Advance of periastron, ω̂ (deg/yr)</td><td>—</td><td>0.0080(4)</td><td>—</td><td>—</td></tr><tr><td>Orbital period derivative, P̂<sub>b</sub></td><td>5.46(6) × 10<sup>-14</sup></td><td>2.2(1) × 10<sup>-13</sup></td><td>—</td><td>5(2) × 10<sup>-12</sup></td></tr><tr><td>Derivative of x, x̂</td><td>1.5(1) × 10<sup>-15</sup></td><td>1.39(2) × 10<sup>-14</sup></td><td>—</td><td>-1.99(6) × 10<sup>-14</sup></td></tr><tr><td>3rd harmonic of Shapiro delay, h<sub>3</sub> (s)</td><td>9.1(10) × 10<sup>-8</sup></td><td>6.5(2) × 10<sup>-7</sup></td><td>—</td><td>—</td></tr><tr><td>4th harmonic of Shapiro delay, h<sub>4</sub> (s)</td><td>5(1) × 10<sup>-8</sup></td><td>—</td><td>—</td><td>—</td></tr><tr><td>Ratio of harmonics amplitude, ζ</td><td>—</td><td>0.54(1)</td><td>—</td><td>—</td></tr><tr><td>Solar wind electron density, n<sub>sw</sub> (cm<sup>-3</sup>)</td><td>—</td><td>11.1(3)</td><td>—</td><td>—</td></tr><tr><td>Noise model</td><td>RN, DM</td><td>RN, DM</td><td>DM</td><td>RN</td></tr></tbody></table>
<table><caption>Table B.2: Measured timing model parameters for PSRs J1012+5307, J1022+1001, J1024–0719, J1455–3330.</caption><thead><tr><th>Pulsar Jname</th><th>J1012+5307</th><th>J1022+1001</th><th>J1024–0719</th><th>J1455–3330</th></tr></thead><tbody><tr><td>Right ascension, α (J2000)</td><td>10:12:33.437537(2)</td><td>—</td><td>10:24:38.675394(3)</td><td>14:55:47.969872(8)</td></tr><tr><td>Declination, δ (J2000)</td><td>53:07:2.30023(3)</td><td>—</td><td>-07:19:19.43377(8)</td><td>-33:30:46.3803(2)</td></tr><tr><td>Ecliptic longitude λ (deg)</td><td>—</td><td>153.865866923(8)</td><td>—</td><td>—</td></tr><tr><td>Ecliptic latitude β (deg)</td><td>—</td><td>-0.063926(8)</td><td>—</td><td>—</td></tr><tr><td>Spin frequency, ν (Hz)</td><td>190.2678344415654(2)</td><td>60.7794479566973(2)</td><td>193.715683448548(2)</td><td>125.200243244993(2)</td></tr><tr><td>Spin frequency derivative, ṽ (s<sup>-2</sup>)</td><td>-6.20041(2) × 10<sup>-16</sup></td><td>-1.60094(1) × 10<sup>-16</sup></td><td>-6.9593(2) × 10<sup>-16</sup></td><td>-3.8097(1) × 10<sup>-16</sup></td></tr><tr><td>Second spin frequency derivative, ṽ (s<sup>-3</sup>)</td><td>—</td><td>—</td><td>-3.57(7) × 10<sup>-27</sup></td><td>—</td></tr><tr><td>DM (cm<sup>-3</sup> pc)</td><td>9.0211(4)</td><td>10.2580(9)</td><td>6.4885(10)</td><td>13.569(3)</td></tr><tr><td>DM1 (cm<sup>-3</sup> pc yr<sup>-1</sup>)</td><td>0.00012(1)</td><td>-0.00016(6)</td><td>0.0004(2)</td><td>0.0004(3)</td></tr><tr><td>DM2 (cm<sup>-3</sup> pc yr<sup>-2</sup>)</td><td>1.6(3) × 10<sup>-5</sup></td><td>4.1(9) × 10<sup>-5</sup></td><td>-9(4) × 10<sup>-5</sup></td><td>-4(4) × 10<sup>-5</sup></td></tr><tr><td>Proper motion in α, μ<sub>α</sub> (mas yr<sup>-1</sup>)</td><td>2.624(3)</td><td>—</td><td>-35.277(5)</td><td>7.85(1)</td></tr><tr><td>Proper motion in δ, μ<sub>δ</sub> (mas yr<sup>-1</sup>)</td><td>-25.487(4)</td><td>—</td><td>-48.23(1)</td><td>-1.98(4)</td></tr><tr><td>Proper motion in λ, μ<sub>λ</sub> (mas yr<sup>-1</sup>)</td><td>—</td><td>-15.916(4)</td><td>—</td><td>—</td></tr><tr><td>Proper motion in β, μ<sub>β</sub> (mas yr<sup>-1</sup>)</td><td>—</td><td>-18(4)</td><td>—</td><td>—</td></tr><tr><td>Parallax, σ (mas)</td><td>0.90(8)</td><td>1.16(8)</td><td>1.01(4)</td><td>1.3(1)</td></tr><tr><td>Binary model</td><td>T2</td><td>DDH</td><td>—</td><td>T2</td></tr><tr><td>Orbital period, P<sub>b</sub> (d)</td><td>0.604672722921(3)</td><td>7.8051340(2)</td><td>—</td><td>76.17456861(2)</td></tr><tr><td>Projected semi-major axis, x (s)</td><td>0.58181715(6)</td><td>16.7654035(5)</td><td>—</td><td>32.3622232(5)</td></tr><tr><td>Longitude of periastron, ω (deg)</td><td>—</td><td>97.711(8)</td><td>—</td><td>223.458(1)</td></tr><tr><td>Epoch of periastron, T<sub>0</sub> (MJD)</td><td>—</td><td>50246.7172(2)</td><td>—</td><td>48980.1327(3)</td></tr><tr><td>Epoch of ascending node (MJD), T<sub>asc</sub></td><td>50700.08174601(1)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Orbital eccentricity, e</td><td>—</td><td>9.697(1) × 10<sup>-5</sup></td><td>—</td><td>0.000169646(4)</td></tr><tr><td>x̂ component of the eccentricity, κ</td><td>1.18(5) × 10<sup>-6</sup></td><td>—</td><td>—</td><td>—</td></tr><tr><td>ŷ component of the eccentricity, η</td><td>9(5) × 10<sup>-8</sup></td><td>—</td><td>—</td><td>—</td></tr><tr><td>Advance of periastron, ω̂ (deg / yr)</td><td>—</td><td>0.0080(4)</td><td>—</td><td>—</td></tr><tr><td>Orbital period derivative, P̂<sub>b</sub></td><td>5.46(6) × 10<sup>-14</sup></td><td>2.2(1) × 10<sup>-13</sup></td><td>—</td><td>5(2) × 10<sup>-12</sup></td></tr><tr><td>Derivative of x, x̂</td><td>1.5(1) × 10<sup>-15</sup></td><td>1.39(2) × 10<sup>-14</sup></td><td>—</td><td>-1.99(6) × 10<sup>-14</sup></td></tr><tr><td>3rd harmonic of Shapiro delay, h<sub>3</sub> (s)</td><td>9.1(10) × 10<sup>-8</sup></td><td>6.5(2) × 10<sup>-7</sup></td><td>—</td><td>—</td></tr><tr><td>4th harmonic of Shapiro delay, h<sub>4</sub> (s)</td><td>5(1) × 10<sup>-8</sup></td><td>—</td><td>—</td><td>—</td></tr><tr><td>Ratio of harmonics amplitude, ζ</td><td>—</td><td>0.54(1)</td><td>—</td><td>—</td></tr><tr><td>Solar wind electron density, n<sub>sw</sub> (cm<sup>-3</sup>)</td><td>—</td><td>11.1(3)</td><td>—</td><td>—</td></tr><tr><td>Noise model</td><td>RN, DM</td><td>RN, DM</td><td>DM</td><td>RN</td></tr></tbody></table>
<table><caption>Table B.3: Measured timing model parameters for PSRs J1600–3053, J164+2224, J1713+0747 and J1730–2304.</caption><thead><tr><th>Pulsar Jname</th><th>J1600-3053</th><th>J1640+2224</th><th>J1713+0747</th><th>J1730-2304</th></tr></thead><tbody><tr><td>Right ascension, α (J2000)</td><td>16:00:51.903339(2)</td><td>16:40:16.744850(2)</td><td>17:13:49.5331917(3)</td><td>—</td></tr><tr><td>Declination, δ (J2000)</td><td>-30:53:49.37555(7)</td><td>22:24:08.84119(5)</td><td>07:47:37.49258(1)</td><td>—</td></tr><tr><td>Ecliptic longitude λ (deg)</td><td>—</td><td>—</td><td>—</td><td>263.18603136(1)</td></tr><tr><td>Ecliptic latitude β (deg)</td><td>—</td><td>—</td><td>—</td><td>0.188871(4)</td></tr><tr><td>Spin frequency, ν (Hz)</td><td>277.9377069896062(8)</td><td>316.123979331869(2)</td><td>218.8118404171605(2)</td><td>123.110287147370(2)</td></tr><tr><td>Spin frequency derivative, ˙ν (s<sup>-2</sup>)</td><td>-7.33880(3) × 10<sup>-16</sup></td><td>-2.8156(1) × 10<sup>-16</sup></td><td>-4.08385(2) × 10<sup>-16</sup></td><td>-3.05916(6) × 10<sup>-16</sup></td></tr><tr><td>DM (cm<sup>-3</sup> pc)</td><td>52.3243(4)</td><td>18.426(1)</td><td>15.9918(1)</td><td>9.618(2)</td></tr><tr><td>DM1 (cm<sup>-3</sup> pc yr<sup>-1</sup>)</td><td>-3(10) × 10<sup>-5</sup></td><td>0.0003(1)</td><td>1(14)×10<sup>-6</sup></td><td>0.0004(2)</td></tr><tr><td>DM2 (cm<sup>-3</sup> pc yr<sup>-2</sup>)</td><td>4(3)×10<sup>-5</sup></td><td>-5(2) × 10<sup>-5</sup></td><td>-6(3) × 10<sup>-6</sup></td><td>-2(40) × 10<sup>-6</sup></td></tr><tr><td>Proper motion in α, μ<sub>α</sub> (mas yr<sup>-1</sup>)</td><td>-0.943(3)</td><td>2.102(4)</td><td>4.9215(8)</td><td>—</td></tr><tr><td>Proper motion in δ, μ<sub>δ</sub> (mas yr<sup>-1</sup>)</td><td>-6.92(1)</td><td>-11.333(7)</td><td>-3.920(2)</td><td>—</td></tr><tr><td>Proper motion in λ, μ<sub>λ</sub> (mas yr<sup>-1</sup>)</td><td>—</td><td>—</td><td>—</td><td>20.236(5)</td></tr><tr><td>Proper motion in β, μ<sub>β</sub> (mas yr<sup>-1</sup>)</td><td>—</td><td>—</td><td>—</td><td>-4.4(1.8)</td></tr><tr><td>Parallax, ω (mas)</td><td>0.72(2)</td><td>0.8(2)</td><td>0.88(1)</td><td>2.08(6)</td></tr><tr><td>Binary model</td><td>T2</td><td>DDH</td><td>T2</td><td>—</td></tr><tr><td>Orbital period, P<sub>b</sub> (d)</td><td>14.3484635(2)</td><td>175.460664578(9)</td><td>67.8251309746(7)</td><td>—</td></tr><tr><td>Projected semi-major axis, x (s)</td><td>8.8016540(1)</td><td>55.3297193(4)</td><td>32.34241947(4)</td><td>—</td></tr><tr><td>Longitude of periastron, ω (deg)</td><td>181.819(3)</td><td>50.7326(2)</td><td>176.2000(4)</td><td>—</td></tr><tr><td>Epoch of periastron, T<sub>0</sub> (MJD)</td><td>52506.3733(1)</td><td>51626.17953(9)</td><td>48741.97387(7)</td><td>—</td></tr><tr><td>Orbital eccentricity, e</td><td>0.000173728(2)</td><td>0.000797277(3)</td><td>7.49405(2)×10<sup>-5</sup></td><td>—</td></tr><tr><td>Advance of periastron, ω̇ (deg/yr)</td><td>0.0036(1)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Orbital period derivative, ˙P<sub>b</sub></td><td>3.6(3)×10<sup>-13</sup></td><td>9(2)×10<sup>-12</sup></td><td>2.6(7)×10<sup>-13</sup></td><td>—</td></tr><tr><td>Derivative of x, ˙x</td><td>-3.55(6) × 10<sup>-15</sup></td><td>1.12(4)×10<sup>-14</sup></td><td>—</td><td>—</td></tr><tr><td>Sine of inclination angle, sin i</td><td>0.906(6)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Companion mass, M<sub>c</sub> (M<sub>☉</sub>)</td><td>0.29(2)</td><td>—</td><td>0.296(3)</td><td>—</td></tr><tr><td>3rd harmonic of Shapiro delay, h<sub>3</sub> (s)</td><td>—</td><td>3.8(2)×10<sup>-7</sup></td><td>—</td><td>—</td></tr><tr><td>Ratio of harmonics amplitude, ζ</td><td>—</td><td>0.75(4)</td><td>—</td><td>—</td></tr><tr><td>Longitude of ascending node, Ω (deg)</td><td>—</td><td>—</td><td>91.1(5)</td><td>—</td></tr><tr><td>Inclination angle, i (deg)</td><td>—</td><td>—</td><td>71.3(2)</td><td>—</td></tr><tr><td>Noise model</td><td>RN, DM, SV</td><td>DM</td><td>RN, DM</td><td>DM</td></tr></tbody></table>

<table><caption>Table B.4: Measured timing model parameters for PSRs J1738+0333, J1744–1134, J1751–2857 and J1801–1417.</caption><thead><tr><th>Pulsar Jname</th><th>J1738+0333</th><th>J1744–1134</th><th>J1751–2857</th><th>J1801–1417</th></tr></thead><tbody><tr><td>Right ascension, α (J2000)</td><td>17:38:53.966386(6)</td><td>17:44:29.4075472(8)</td><td>17:51:32.69322(1)</td><td>18:01:51.07336(2)</td></tr><tr><td>Declination, δ (J2000)</td><td>03:33:10.8720(2)</td><td>-11:34:54.69423(6)</td><td>-28:57:46.519(2)</td><td>-14:17:34.527(2)</td></tr><tr><td>Spin frequency, ν (Hz)</td><td>170.937369887100(7)</td><td>245.4261196898081(5)</td><td>255.43611088568(2)</td><td>275.85470899694(1)</td></tr><tr><td>Spin frequency derivative, ˙ν (s<sup>-2</sup>)</td><td>-7.0471(4) × 10<sup>-16</sup></td><td>-5.38156(3) × 10<sup>-16</sup></td><td>-7.3239(8) × 10<sup>-16</sup></td><td>-4.0361(7) × 10<sup>-16</sup></td></tr><tr><td>DM (cm<sup>-3</sup> pc)</td><td>33.767(2)</td><td>3.1379(4)</td><td>42.81(1)</td><td>57.24(1)</td></tr><tr><td>DM1 (cm<sup>-3</sup> pc yr<sup>-1</sup>)</td><td>-0.0014(5)</td><td>-7(3) × 10<sup>-5</sup></td><td>3(99)×10<sup>-5</sup></td><td>0.003(1)</td></tr><tr><td>DM2 (cm<sup>-3</sup> pc yr<sup>-2</sup>)</td><td>1.0(8)×10<sup>-4</sup></td><td>1.7(4)×10<sup>-5</sup></td><td>0.0002(2)</td><td>-0.0003(2)</td></tr><tr><td>Proper motion in α, μ<sub>α</sub> (mas yr<sup>-1</sup>)</td><td>7.09(1)</td><td>18.806(2)</td><td>-7.38(4)</td><td>-10.85(4)</td></tr><tr><td>Proper motion in δ, μ<sub>δ</sub> (mas yr<sup>-1</sup>)</td><td>5.07(3)</td><td>-9.386(10)</td><td>-4.5(4)</td><td>-1.9(3)</td></tr><tr><td>Parallax, ω (mas)</td><td>—</td><td>2.58(3)</td><td>1.1(4)</td><td>0.8(3)</td></tr><tr><td>Binary model</td><td>T2</td><td>—</td><td>T2</td><td>—</td></tr><tr><td>Orbital period, P<sub>b</sub> (d)</td><td>0.35479073997(3)</td><td>—</td><td>110.74646085(1)</td><td>—</td></tr><tr><td>Projected semi-major axis, x (s)</td><td>0.3434302(1)</td><td>—</td><td>32.5282233(8)</td><td>—</td></tr><tr><td>Longitude of periastron, ω (deg)</td><td>—</td><td>—</td><td>45.501(5)</td><td>—</td></tr><tr><td>Epoch of periastron, T<sub>0</sub> (MJD)</td><td>—</td><td>—</td><td>52491.572(2)</td><td>—</td></tr><tr><td>Epoch of ascending node (MJD), T<sub>asc</sub></td><td>52500.1940104(2)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Orbital eccentricity, e</td><td>—</td><td>—</td><td>0.00012792(1)</td><td>—</td></tr><tr><td>ˆx component of the eccentricity, κ</td><td>1.0(7)×10<sup>-6</sup></td><td>—</td><td>—</td><td>—</td></tr><tr><td>ˆy component of the eccentricity, η</td><td>4(6)×10<sup>-7</sup></td><td>—</td><td>—</td><td>—</td></tr><tr><td>Advance of periastron, ω̇ (deg/yr)</td><td>0.0036(1)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Orbital period derivative, ˙P<sub>b</sub></td><td>-3.0(7) × 10<sup>-14</sup></td><td>—</td><td>3.7(2)×10<sup>-14</sup></td><td>—</td></tr><tr><td>Derivative of x, ˙x</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Noise model</td><td>RN</td><td>RN, DM</td><td>DM</td><td>DM</td></tr></tbody></table>
<table><caption>Table B.3: Measured timing model parameters for PSRs J1600–3053, J164+2224, J1713+0747 and J1730–2304.</caption><thead><tr><th>Pulsar Jname</th><th>J1600–3053</th><th>J1640+2224</th><th>J1713+0747</th><th>J1730–2304</th></tr></thead><tbody><tr><td>Right ascension, α (J2000)</td><td>16:00:51.903339(2)</td><td>16:40:16.744850(2)</td><td>17:13:49.5331917(3)</td><td>—</td></tr><tr><td>Declination, δ (J2000)</td><td>-30:53:49.37555(7)</td><td>22:24:08.84119(5)</td><td>07:47:37.49258(1)</td><td>—</td></tr><tr><td>Ecliptic longitude λ (deg)</td><td>—</td><td>—</td><td>—</td><td>263.18603136(1)</td></tr><tr><td>Ecliptic latitude β (deg)</td><td>—</td><td>—</td><td>—</td><td>0.188871(4)</td></tr><tr><td>Spin frequency, ν (Hz)</td><td>277.9377069896062(8)</td><td>316.123979331869(2)</td><td>218.8118404171605(2)</td><td>123.110287147370(2)</td></tr><tr><td>Spin frequency derivative, ˙ν (s<sup>-2</sup>)</td><td>-7.33880(3) × 10<sup>-16</sup></td><td>-2.8156(1) × 10<sup>-16</sup></td><td>-4.08385(2) × 10<sup>-16</sup></td><td>-3.05916(6) × 10<sup>-16</sup></td></tr><tr><td>DM (cm<sup>-3</sup> pc)</td><td>52.3243(4)</td><td>18.426(1)</td><td>15.9918(1)</td><td>9.618(2)</td></tr><tr><td>DM1 (cm<sup>-3</sup> pc yr<sup>-1</sup>)</td><td>-3(10) × 10<sup>-5</sup></td><td>0.0003(1)</td><td>1(14)×10<sup>-6</sup></td><td>0.0004(2)</td></tr><tr><td>DM2 (cm<sup>-3</sup> pc yr<sup>-2</sup>)</td><td>4(3)×10<sup>-5</sup></td><td>-5(2) × 10<sup>-5</sup></td><td>-6(3) × 10<sup>-6</sup></td><td>-2(40) × 10<sup>-6</sup></td></tr><tr><td>Proper motion in α, μ<sub>α</sub> (mas yr<sup>-1</sup>)</td><td>-0.943(3)</td><td>2.102(4)</td><td>4.9215(8)</td><td>—</td></tr><tr><td>Proper motion in δ, μ<sub>δ</sub> (mas yr<sup>-1</sup>)</td><td>-6.92(1)</td><td>-11.333(7)</td><td>-3.920(2)</td><td>—</td></tr><tr><td>Proper motion in λ, μ<sub>λ</sub> (mas yr<sup>-1</sup>)</td><td>—</td><td>—</td><td>—</td><td>20.236(5)</td></tr><tr><td>Proper motion in β, μ<sub>β</sub> (mas yr<sup>-1</sup>)</td><td>—</td><td>—</td><td>—</td><td>-4.4(1.8)</td></tr><tr><td>Parallax, ω (mas)</td><td>0.72(2)</td><td>0.8(2)</td><td>0.88(1)</td><td>2.08(6)</td></tr><tr><td>Binary model</td><td>T2</td><td>DDH</td><td>T2</td><td>—</td></tr><tr><td>Orbital period, P<sub>b</sub> (d)</td><td>14.3484635(2)</td><td>175.460664578(9)</td><td>67.8251309746(7)</td><td>—</td></tr><tr><td>Projected semi-major axis, x (s)</td><td>8.8016540(1)</td><td>55.3297193(4)</td><td>32.34241947(4)</td><td>—</td></tr><tr><td>Longitude of periastron, ω (deg)</td><td>181.819(3)</td><td>50.7326(2)</td><td>176.2000(4)</td><td>—</td></tr><tr><td>Epoch of periastron, T<sub>0</sub> (MJD)</td><td>52506.3733(1)</td><td>51626.17953(9)</td><td>48741.97387(7)</td><td>—</td></tr><tr><td>Orbital eccentricity, e</td><td>0.000173728(2)</td><td>0.000797277(3)</td><td>7.49405(2)×10<sup>-5</sup></td><td>—</td></tr><tr><td>Advance of periastron, ω̇ (deg/yr)</td><td>0.0036(1)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Orbital period derivative, ˙P<sub>b</sub></td><td>3.6(3)×10<sup>-13</sup></td><td>9(2)×10<sup>-12</sup></td><td>2.6(7)×10<sup>-13</sup></td><td>—</td></tr><tr><td>Derivative of x, ˙x</td><td>-3.55(6) × 10<sup>-15</sup></td><td>1.12(4)×10<sup>-14</sup></td><td>—</td><td>—</td></tr><tr><td>Sine of inclination angle, sin i</td><td>0.906(6)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Companion mass, M<sub>c</sub> (M<sub>☉</sub>)</td><td>0.29(2)</td><td>—</td><td>0.296(3)</td><td>—</td></tr><tr><td>3rd harmonic of Shapiro delay, h<sub>3</sub> (s)</td><td>—</td><td>3.8(2)×10<sup>-7</sup></td><td>—</td><td>—</td></tr><tr><td>Ratio of harmonics amplitude, ζ</td><td>—</td><td>0.75(4)</td><td>—</td><td>—</td></tr><tr><td>Longitude of ascending node, Ω (deg)</td><td>—</td><td>—</td><td>91.1(5)</td><td>—</td></tr><tr><td>Inclination angle, i (deg)</td><td>—</td><td>—</td><td>71.3(2)</td><td>—</td></tr><tr><td>Noise model</td><td>RN, DM, SV</td><td>DM</td><td>RN, DM</td><td>DM</td></tr></tbody></table>

<table><caption>Table B.4: Measured timing model parameters for PSRs J1738+0333, J1744–1134, J1751–2857 and J1801–1417.</caption><thead><tr><th>Pulsar Jname</th><th>J1738+0333</th><th>J1744–1134</th><th>J1751–2857</th><th>J1801–1417</th></tr></thead><tbody><tr><td>Right ascension, α (J2000)</td><td>17:38:53.966386(6)</td><td>17:44:29.4075472(8)</td><td>17:51:32.69322(1)</td><td>18:01:51.07336(2)</td></tr><tr><td>Declination, δ (J2000)</td><td>03:33:10.8720(2)</td><td>-11:34:54.69423(6)</td><td>-28:57:46.519(2)</td><td>-14:17:34.527(2)</td></tr><tr><td>Spin frequency, ν (Hz)</td><td>170.937369887100(7)</td><td>245.4261196898081(5)</td><td>255.43611088568(2)</td><td>275.85470899694(1)</td></tr><tr><td>Spin frequency derivative, ˙ν (s<sup>-2</sup>)</td><td>-7.0471(4) × 10<sup>-16</sup></td><td>-5.38156(3) × 10<sup>-16</sup></td><td>-7.3239(8) × 10<sup>-16</sup></td><td>-4.0361(7) × 10<sup>-16</sup></td></tr><tr><td>DM (cm<sup>-3</sup> pc)</td><td>33.767(2)</td><td>3.1379(4)</td><td>42.81(1)</td><td>57.24(1)</td></tr><tr><td>DM1 (cm<sup>-3</sup> pc yr<sup>-1</sup>)</td><td>-0.0014(5)</td><td>-7(3) × 10<sup>-5</sup></td><td>3(99)×10<sup>-5</sup></td><td>0.003(1)</td></tr><tr><td>DM2 (cm<sup>-3</sup> pc yr<sup>-2</sup>)</td><td>1.0(8)×10<sup>-4</sup></td><td>1.7(4)×10<sup>-5</sup></td><td>0.0002(2)</td><td>-0.0003(2)</td></tr><tr><td>Proper motion in α, μ<sub>α</sub> (mas yr<sup>-1</sup>)</td><td>7.09(1)</td><td>18.806(2)</td><td>-7.38(4)</td><td>-10.85(4)</td></tr><tr><td>Proper motion in δ, μ<sub>δ</sub> (mas yr<sup>-1</sup>)</td><td>5.07(3)</td><td>-9.386(10)</td><td>-4.5(4)</td><td>-1.9(3)</td></tr><tr><td>Parallax, ω (mas)</td><td>—</td><td>2.58(3)</td><td>1.1(4)</td><td>0.8(3)</td></tr><tr><td>Binary model</td><td>T2</td><td>—</td><td>T2</td><td>—</td></tr><tr><td>Orbital period, P<sub>b</sub> (d)</td><td>0.35479073997(3)</td><td>—</td><td>110.74646085(1)</td><td>—</td></tr><tr><td>Projected semi-major axis, x (s)</td><td>0.3434302(1)</td><td>—</td><td>32.5282233(8)</td><td>—</td></tr><tr><td>Longitude of periastron, ω (deg)</td><td>—</td><td>—</td><td>45.501(5)</td><td>—</td></tr><tr><td>Epoch of periastron, T<sub>0</sub> (MJD)</td><td>—</td><td>—</td><td>52491.572(2)</td><td>—</td></tr><tr><td>Epoch of ascending node (MJD), T<sub>asc</sub></td><td>52500.1940104(2)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Orbital eccentricity, e</td><td>—</td><td>—</td><td>0.00012792(1)</td><td>—</td></tr><tr><td>ˆx component of the eccentricity, κ</td><td>1.0(7)×10<sup>-6</sup></td><td>—</td><td>—</td><td>—</td></tr><tr><td>ˆy component of the eccentricity, η</td><td>4(6)×10<sup>-7</sup></td><td>—</td><td>—</td><td>—</td></tr><tr><td>Advance of periastron, ω̇ (deg/yr)</td><td>0.0036(1)</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Orbital period derivative, ˙P<sub>b</sub></td><td>-3.0(7) × 10<sup>-14</sup></td><td>—</td><td>3.7(2)×10<sup>-14</sup></td><td>—</td></tr><tr><td>Derivative of x, ˙x</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>Noise model</td><td>RN</td><td>RN, DM</td><td>DM</td><td>DM</td></tr></tbody></table>
<table><caption>Table B.5: Measured timing model parameters for PSRs J1804−2717, J1843−1113, J1857+0943 and J1909−3744.</caption><thead><tr><th>Pulsar Jname</th><th>J1804−2717</th><th>J1843−1113</th><th>J1857+0943</th><th>J1909−3744</th></tr></thead><tbody><tr><td>Right ascension, α (J2000)</td><td>18:04:21.13307(1)</td><td>18:43:41.261937(7)</td><td>18:57:36.390620(1)</td><td>19:09:47.4335785(8)</td></tr><tr><td>Declination, δ (J2000)</td><td>−27:17:31.337(3)</td><td>−11:13:31.0684(5)</td><td>09:43:17.20712(4)</td><td>−37:44:14.51579(3)</td></tr><tr><td>Spin frequency, ν (Hz)</td><td>107.031649219533(4)</td><td>541.809745036152(5)</td><td>186.4940783779890(9)</td><td>339.3156872184705(9)</td></tr><tr><td>Spin frequency derivative, ṽ (s<sup>−2</sup>)</td><td>−4.6812(2) × 10<sup>−16</sup></td><td>−2.80559(3) × 10<sup>−15</sup></td><td>−6.20522(4) × 10<sup>−16</sup></td><td>−1.614806(7) × 10<sup>−15</sup></td></tr><tr><td>DM (cm<sup>−3</sup> pc)</td><td>24.688(4)</td><td>59.962(2)</td><td>13.2957(9)</td><td>10.3925(2)</td></tr><tr><td>DM1 (cm<sup>−3</sup> pc yr<sup>−1</sup>)</td><td>0.0005(7)</td><td>−0.0009(3)</td><td>0.00082(7)</td><td>−0.00037(3)</td></tr><tr><td>DM2 (cm<sup>−3</sup> pc yr<sup>−2</sup>)</td><td>−0.00012(9)</td><td>5(8)×10<sup>−5</sup></td><td>−0.00012(2)</td><td>4.1(6)×10<sup>−5</sup></td></tr><tr><td>Proper motion in α, μ<sub>α</sub> (mas yr<sup>−1</sup>)</td><td>2.46(2)</td><td>−1.99(2)</td><td>−2.670(3)</td><td>−9.523(1)</td></tr><tr><td>Proper motion in δ, μ<sub>δ</sub> (mas yr<sup>−1</sup>)</td><td>−16.9(4)</td><td>−3.00(7)</td><td>−5.428(6)</td><td>−35.780(5)</td></tr><tr><td>Parallax, ϖ (mas)</td><td>1.1(3)</td><td>—</td><td>0.89(6)</td><td>0.94(2)</td></tr><tr><td>Binary model</td><td>T2</td><td>—</td><td>T2</td><td>T2</td></tr><tr><td>Orbital period, P<sub>b</sub> (d)</td><td>11.1287119652(3)</td><td>—</td><td>12.32717138285(5)</td><td>1.533449475874(1)</td></tr><tr><td>Projected semi-major axis, x (s)</td><td>7.2814511(1)</td><td>—</td><td>9.23078029(8)</td><td>1.89799110(1)</td></tr><tr><td>Epoch of ascending node (MJD), T<sub>asc</sub></td><td>49610.1749842(2)</td><td>—</td><td>46423.31409197(5)</td><td>56180.8496921865(6)</td></tr><tr><td>x̄ component of the eccentricity, κ</td><td>1.219(3)×10<sup>−5</sup></td><td>—</td><td>−2.1565(9) × 10<sup>−5</sup></td><td>5.4(7)×10<sup>−8</sup></td></tr><tr><td>ȳ component of the eccentricity, η</td><td>−3.177(4) × 10<sup>−5</sup></td><td>—</td><td>2.454(5)×10<sup>−6</sup></td><td>−1.07(4) × 10<sup>−7</sup></td></tr><tr><td>Orbital period derivative, Ṗ<sub>b</sub></td><td>—</td><td>—</td><td>—</td><td>5.09(1)×10<sup>−13</sup></td></tr><tr><td>Derivative of x, ṛ</td><td>—</td><td>—</td><td>—</td><td>−3.6(5) × 10<sup>−16</sup></td></tr><tr><td>Sine of inclination angle, sin i</td><td>—</td><td>—</td><td>0.9989(2)</td><td>0.99831(4)</td></tr><tr><td>Companion mass, M<sub>c</sub> (M<sub>☉</sub>)</td><td>—</td><td>—</td><td>0.258(5)</td><td>0.2048(9)</td></tr><tr><td>Noise model</td><td>DM</td><td>DM</td><td>DM</td><td>RN, DM</td></tr></tbody></table>

<table><caption>Table B.6: Measured timing model parameters for PSRs J1910+1256, J1911+1347, J1918−0642 and J2124−3358.</caption><thead><tr><th>Pulsar Jname</th><th>J1910+1256</th><th>J1911+1347</th><th>J1918−0642</th><th>J2124−3358</th></tr></thead><tbody><tr><td>Right ascension, α (J2000)</td><td>19:10:9.701454(7)</td><td>19:11:55.204694(3)</td><td>19:18:48.033123(3)</td><td>21:24:43.847830(7)</td></tr><tr><td>Declination, δ (J2000)</td><td>12:56:25.4868(2)</td><td>13:47:34.38383(6)</td><td>−06:42:34.8895(1)</td><td>−33:58:44.9196(2)</td></tr><tr><td>Spin frequency, ν (Hz)</td><td>200.658802230113(7)</td><td>216.171227371979(2)</td><td>130.789514123371(1)</td><td>202.793893746013(3)</td></tr><tr><td>Spin frequency derivative, ṽ (s<sup>−2</sup>)</td><td>−3.8969(3) × 10<sup>−16</sup></td><td>−7.9086(1) × 10<sup>−16</sup></td><td>−4.3947(6) × 10<sup>−16</sup></td><td>−8.4590(1) × 10<sup>−16</sup></td></tr><tr><td>DM (cm<sup>−3</sup> pc)</td><td>38.075(5)</td><td>30.989(1)</td><td>26.593(1)</td><td>4.600(3)</td></tr><tr><td>DM1 (cm<sup>−3</sup> pc yr<sup>−1</sup>)</td><td>0.0002(6)</td><td>−0.0010(2)</td><td>−0.0003(2)</td><td>−0.0003(2)</td></tr><tr><td>DM2 (cm<sup>−3</sup> pc yr<sup>−2</sup>)</td><td>−4(10) × 10<sup>−5</sup></td><td>7(4)×10<sup>−5</sup></td><td>2(3)×10<sup>−5</sup></td><td>7(4)×10<sup>−5</sup></td></tr><tr><td>Proper motion in α, μ<sub>α</sub> (mas yr<sup>−1</sup>)</td><td>0.24(2)</td><td>−2.900(5)</td><td>−7.124(5)</td><td>−14.09(1)</td></tr><tr><td>Proper motion in δ, μ<sub>δ</sub> (mas yr<sup>−1</sup>)</td><td>−7.10(3)</td><td>−3.684(9)</td><td>−5.96(2)</td><td>−50.32(3)</td></tr><tr><td>Parallax, ϖ (mas)</td><td>—</td><td>0.40(9)</td><td>0.75(7)</td><td>2.1(1)</td></tr><tr><td>Binary model</td><td>T2</td><td>—</td><td>DDH</td><td>—</td></tr><tr><td>Orbital period, P<sub>b</sub> (d)</td><td>58.466742972(2)</td><td>—</td><td>10.91317774976(7)</td><td>—</td></tr><tr><td>Projected semi-major axis, x (s)</td><td>21.1291048(4)</td><td>—</td><td>8.3504666(2)</td><td>—</td></tr><tr><td>Longitude of periastron, ω (deg)</td><td>106.005(3)</td><td>—</td><td>219.49(4)</td><td>—</td></tr><tr><td>Epoch of periastron, T<sub>0</sub> (MJD)</td><td>52968.4482(5)</td><td>—</td><td>51575.771(1)</td><td>—</td></tr><tr><td>Orbital eccentricity, e</td><td>0.00023024(1)</td><td>—</td><td>2.032(1)×10<sup>−5</sup></td><td>—</td></tr><tr><td>Orbital period derivative, Ṗ<sub>b</sub></td><td>—</td><td>—</td><td>2.6(7)×10<sup>−13</sup></td><td>—</td></tr><tr><td>Derivative of x, ṛ</td><td>−1.5(1) × 10<sup>−14</sup></td><td>—</td><td>—</td><td>—</td></tr><tr><td>3rd harmonic of Shapiro delay, h<sub>3</sub> (s)</td><td>—</td><td>—</td><td>8.2(2)×10<sup>−7</sup></td><td>—</td></tr><tr><td>Ratio of harmonics amplitude, ζ</td><td>—</td><td>—</td><td>0.918(9)</td><td>—</td></tr><tr><td>Noise model</td><td>DM</td><td>DM</td><td>DM</td><td>DM</td></tr></tbody></table>
<table><caption>Table B.5: Measured timing model parameters for PSRs J1804−2717, J1843−1113, J1857+0943 and J1909−3744.</caption><thead><tr><th>Pulsar Jname</th><th>J1804−2717</th><th>J1843−1113</th><th>J1857+0943</th><th>J1909−3744</th></tr></thead><tbody><tr><td>Right ascension, α (J2000)</td><td>18:04:21.13307(1)</td><td>18:43:41.261937(7)</td><td>18:57:36.390620(1)</td><td>19:09:47.4335785(8)</td></tr><tr><td>Declination, δ (J2000)</td><td>−27:17:31.337(3)</td><td>−11:13:31.0684(5)</td><td>09:43:17.20712(4)</td><td>−37:44:14.51579(3)</td></tr><tr><td>Spin frequency, ν (Hz)</td><td>107.031649219533(4)</td><td>541.809745036152(5)</td><td>186.4940783779890(9)</td><td>339.3156872184705(9)</td></tr><tr><td>Spin frequency derivative, ṽ (s<sup>−2</sup>)</td><td>−4.6812(2) × 10<sup>−16</sup></td><td>−2.80559(3) × 10<sup>−15</sup></td><td>−6.20522(4) × 10<sup>−16</sup></td><td>−1.614806(7) × 10<sup>−15</sup></td></tr><tr><td>DM (cm<sup>−3</sup> pc)</td><td>24.688(4)</td><td>59.962(2)</td><td>13.2957(9)</td><td>10.3925(2)</td></tr><tr><td>DM1 (cm<sup>−3</sup> pc yr<sup>−1</sup>)</td><td>0.0005(7)</td><td>−0.0009(3)</td><td>0.00082(7)</td><td>−0.00037(3)</td></tr><tr><td>DM2 (cm<sup>−3</sup> pc yr<sup>−2</sup>)</td><td>−0.00012(9)</td><td>5(8)×10<sup>−5</sup></td><td>−0.00012(2)</td><td>4.1(6)×10<sup>−5</sup></td></tr><tr><td>Proper motion in α, μ<sub>α</sub> (mas yr<sup>−1</sup>)</td><td>2.46(2)</td><td>−1.99(2)</td><td>−2.670(3)</td><td>−9.523(1)</td></tr><tr><td>Proper motion in δ, μ<sub>δ</sub> (mas yr<sup>−1</sup>)</td><td>−16.9(4)</td><td>−3.00(7)</td><td>−5.428(6)</td><td>−35.780(5)</td></tr><tr><td>Parallax, ϖ (mas)</td><td>1.1(3)</td><td>—</td><td>0.89(6)</td><td>0.94(2)</td></tr><tr><td>Binary model</td><td>T2</td><td>—</td><td>T2</td><td>T2</td></tr><tr><td>Orbital period, P<sub>b</sub> (d)</td><td>11.1287119652(3)</td><td>—</td><td>12.32717138285(5)</td><td>1.533449475874(1)</td></tr><tr><td>Projected semi-major axis, x (s)</td><td>7.2814511(1)</td><td>—</td><td>9.23078029(8)</td><td>1.89799110(1)</td></tr><tr><td>Epoch of ascending node (MJD), T<sub>asc</sub></td><td>49610.1749842(2)</td><td>—</td><td>46423.31409197(5)</td><td>56180.8496921865(6)</td></tr><tr><td>x̄ component of the eccentricity, κ</td><td>1.219(3)×10<sup>−5</sup></td><td>—</td><td>−2.1565(9) × 10<sup>−5</sup></td><td>5.4(7)×10<sup>−8</sup></td></tr><tr><td>ȳ component of the eccentricity, η</td><td>−3.177(4) × 10<sup>−5</sup></td><td>—</td><td>2.454(5)×10<sup>−6</sup></td><td>−1.07(4) × 10<sup>−7</sup></td></tr><tr><td>Orbital period derivative, Ṗ<sub>b</sub></td><td>—</td><td>—</td><td>—</td><td>5.09(1)×10<sup>−13</sup></td></tr><tr><td>Derivative of x, ṇ</td><td>—</td><td>—</td><td>—</td><td>−3.6(5) × 10<sup>−16</sup></td></tr><tr><td>Sine of inclination angle, sin i</td><td>—</td><td>—</td><td>0.9989(2)</td><td>0.99831(4)</td></tr><tr><td>Companion mass, M<sub>c</sub> (M<sub>☉</sub>)</td><td>—</td><td>—</td><td>0.258(5)</td><td>0.2048(9)</td></tr><tr><td>Noise model</td><td>DM</td><td>DM</td><td>DM</td><td>RN, DM</td></tr></tbody></table>

<table><caption>Table B.6: Measured timing model parameters for PSRs J1910+1256, J1911+1347, J1918−0642 and J2124−3358.</caption><thead><tr><th>Pulsar Jname</th><th>J1910+1256</th><th>J1911+1347</th><th>J1918−0642</th><th>J2124−3358</th></tr></thead><tbody><tr><td>Right ascension, α (J2000)</td><td>19:10:9.701454(7)</td><td>19:11:55.204694(3)</td><td>19:18:48.033123(3)</td><td>21:24:43.847830(7)</td></tr><tr><td>Declination, δ (J2000)</td><td>12:56:25.4868(2)</td><td>13:47:34.38383(6)</td><td>−06:42:34.8895(1)</td><td>−33:58:44.9196(2)</td></tr><tr><td>Spin frequency, ν (Hz)</td><td>200.658802230113(7)</td><td>216.171227371979(2)</td><td>130.789514123371(1)</td><td>202.793893746013(3)</td></tr><tr><td>Spin frequency derivative, ṽ (s<sup>−2</sup>)</td><td>−3.8969(3) × 10<sup>−16</sup></td><td>−7.9086(1) × 10<sup>−16</sup></td><td>−4.3947(6) × 10<sup>−16</sup></td><td>−8.4590(1) × 10<sup>−16</sup></td></tr><tr><td>DM (cm<sup>−3</sup> pc)</td><td>38.075(5)</td><td>30.989(1)</td><td>26.593(1)</td><td>4.600(3)</td></tr><tr><td>DM1 (cm<sup>−3</sup> pc yr<sup>−1</sup>)</td><td>0.0002(6)</td><td>−0.0010(2)</td><td>−0.0003(2)</td><td>−0.0003(2)</td></tr><tr><td>DM2 (cm<sup>−3</sup> pc yr<sup>−2</sup>)</td><td>−4(10) × 10<sup>−5</sup></td><td>7(4)×10<sup>−5</sup></td><td>2(3)×10<sup>−5</sup></td><td>7(4)×10<sup>−5</sup></td></tr><tr><td>Proper motion in α, μ<sub>α</sub> (mas yr<sup>−1</sup>)</td><td>0.24(2)</td><td>−2.900(5)</td><td>−7.124(5)</td><td>−14.09(1)</td></tr><tr><td>Proper motion in δ, μ<sub>δ</sub> (mas yr<sup>−1</sup>)</td><td>−7.10(3)</td><td>−3.684(9)</td><td>−5.96(2)</td><td>−50.32(3)</td></tr><tr><td>Parallax, ϖ (mas)</td><td>—</td><td>0.40(9)</td><td>0.75(7)</td><td>2.1(1)</td></tr><tr><td>Binary model</td><td>T2</td><td>—</td><td>DDH</td><td>—</td></tr><tr><td>Orbital period, P<sub>b</sub> (d)</td><td>58.466742972(2)</td><td>—</td><td>10.91317774976(7)</td><td>—</td></tr><tr><td>Projected semi-major axis, x (s)</td><td>21.1291048(4)</td><td>—</td><td>8.3504666(2)</td><td>—</td></tr><tr><td>Longitude of periastron, ω (deg)</td><td>106.005(3)</td><td>—</td><td>219.49(4)</td><td>—</td></tr><tr><td>Epoch of periastron, T<sub>0</sub> (MJD)</td><td>52968.4482(5)</td><td>—</td><td>51575.771(1)</td><td>—</td></tr><tr><td>Orbital eccentricity, e</td><td>0.00023024(1)</td><td>—</td><td>2.032(1)×10<sup>−5</sup></td><td>—</td></tr><tr><td>Orbital period derivative, Ṗ<sub>b</sub></td><td>—</td><td>—</td><td>2.6(7)×10<sup>−13</sup></td><td>—</td></tr><tr><td>Derivative of x, ṇ</td><td>−1.5(1) × 10<sup>−14</sup></td><td>—</td><td>—</td><td>—</td></tr><tr><td>3rd harmonic of Shapiro delay, h<sub>3</sub> (s)</td><td>—</td><td>—</td><td>8.2(2)×10<sup>−7</sup></td><td>—</td></tr><tr><td>Ratio of harmonics amplitude, ζ</td><td>—</td><td>—</td><td>0.918(9)</td><td>—</td></tr><tr><td>Noise model</td><td>DM</td><td>DM</td><td>DM</td><td>DM</td></tr></tbody></table>
<table><caption>Table B.7: Measured timing model parameters for PSR J2322+2057.</caption><thead><tr><th>Pulsar Jname</th><th>J2322+2057</th></tr></thead><tbody><tr><td>Right ascension, α (J2000)</td><td>23:22:22.33517(2)</td></tr><tr><td>Declination, δ (J2000)</td><td>20:57:02.6754(6)</td></tr><tr><td>Spin frequency, ν (Hz)</td><td>207.96816335836(1)</td></tr><tr><td>Spin frequency derivative, ṽ (s<sup>-2</sup>)</td><td>-4.1769(7) × 10<sup>-16</sup></td></tr><tr><td>DM (cm<sup>-3</sup> pc)</td><td>13.381(8)</td></tr><tr><td>DM1 (cm<sup>-3</sup> pc yr<sup>-1</sup>)</td><td>-0.0002(10)</td></tr><tr><td>DM2 (cm<sup>-3</sup> pc yr<sup>-2</sup>)</td><td>4(16)×10<sup>-5</sup></td></tr><tr><td>Proper motion in α, μ<sub>α</sub> (mas yr<sup>-1</sup>)</td><td>-18.30(5)</td></tr><tr><td>Proper motion in δ, μ<sub>δ</sub> (mas yr<sup>-1</sup>)</td><td>-14.9(1)</td></tr><tr><td>Noise model</td><td>—</td></tr></tbody></table>
<table><caption>Table B.7: Measured timing model parameters for PSR J2322+2057.</caption><thead><tr><th>Pulsar Jname</th><th>J2322+2057</th></tr></thead><tbody><tr><td>Right ascension, α (J2000)</td><td>23:22:22.33517(2)</td></tr><tr><td>Declination, δ (J2000)</td><td>20:57:02.6754(6)</td></tr><tr><td>Spin frequency, ν (Hz)</td><td>207.96816335836(1)</td></tr><tr><td>Spin frequency derivative, ṽ (s<sup>-2</sup>)</td><td>-4.1769(7) × 10<sup>-16</sup></td></tr><tr><td>DM (cm<sup>-3</sup> pc)</td><td>13.381(8)</td></tr><tr><td>DM1 (cm<sup>-3</sup> pc yr<sup>-1</sup>)</td><td>-0.0002(10)</td></tr><tr><td>DM2 (cm<sup>-3</sup> pc yr<sup>-2</sup>)</td><td>4(16)×10<sup>-5</sup></td></tr><tr><td>Proper motion in α, μ<sub>α</sub> (mas yr<sup>-1</sup>)</td><td>-18.30(5)</td></tr><tr><td>Proper motion in δ, μ<sub>δ</sub> (mas yr<sup>-1</sup>)</td><td>-14.9(1)</td></tr><tr><td>Noise model</td><td>—</td></tr></tbody></table>
Appendix C: Timing residuals

In Figs. C.1–C.5, we present the timing residuals of the 25 pulsars in the EPTA DR2. Residuals both before and after the application of red-noise subtraction are shown.

<figure><img src="image_5.png" /><figcaption>Fig. C.1. Timing residuals of PSRs J0030+0030, J0613−0200, J0751+1807, J0900−3144, J1012+5307. For each pulsar, the residuals before and after subtraction of DM and monochromatic red noise are shown. The squares, circles and triangles represent P-band, L-band and S/C-band observations, respectively (see Table 2 for frequency coverage of each band). The blue/filled and black/unfilled symbols indicate the new backend data and those from EPTA DR1, respectively.</figcaption></figure>
**Appendix C: Timing residuals**

In Figs. C.1–C.5, we present the timing residuals of the 25 pulsars in the EPTA DR2. Residuals both before and after the application of red-noise subtraction are shown.

<figure><img src="image_7.png" /><figcaption>**Fig. C.1.** Timing residuals of PSRs J0030+0030, J0613–0200, J0751+1807, J0900–3144, J1012+5307. For each pulsar, the residuals before and after subtraction of DM and monochromatic red noise are shown. The squares, circles and triangles represent P-band, L-band and S/C-band observations, respectively (see Table 2 for frequency coverage of each band). The blue/filled and black/unfilled symbols indicate the new backend data and those from EPTA DR1, respectively.</figcaption></figure>
<figure><img src="image_6.png" /><figcaption>Fig. C.2. Timing residuals of PSRs J1022+1001, J1024-0719, J1455-3330, J1600-3053, J1640+2224. Figure style is the same as Figure C.1.</figcaption></figure>
<figure><img src="image_8.png" /><figcaption>Fig. C.2. Timing residuals of PSRs J1022+1001, J1024-0719, J1455-3330, J1600-3053, J1640+2224. Figure style is the same as Figure C.1.</figcaption></figure>
<figure><img src="image_7.png" /><figcaption>Fig. C.3. Timing residuals of PSRs J1713+0747, J1730−2304, J1738+0333, J1744−1134, J1751−2857. Figure style is the same as Figure C.1.</figcaption></figure>
<figure><img src="image_9.png" /><figcaption>Fig. C.3. Timing residuals of PSRs J1713+0747, J1730−2304, J1738+0333, J1744−1134, J1751−2857. Figure style is the same as Figure C.1.</figcaption></figure>
<figure><img src="image_8.png" /><figcaption>**Fig. C.4.** Timing residuals of PSRs J1801−1417, J1804−2717, J1843−1113, J1857+0943, J1909−3744. Figure style is the same as Figure C.1.</figcaption></figure>
<figure><img src="image_10.png" /><figcaption>Fig. C.4. Timing residuals of PSRs J1801−1417, J1804−2717, J1843−1113, J1857+0943, J1909−3744. Figure style is the same as Figure C.1.</figcaption></figure>
<figure><img src="image_9.png" /><figcaption>Fig. C.5. Timing residuals of PSRs J1910+1256, J1911+1347, J1918−0642, J2124−3358, J2322+2057. Figure style is the same as Figure C.1.</figcaption></figure>
<figure><img src="image_11.png" /><figcaption>Fig. C.5. Timing residuals of PSRs J1910+1256, J1911+1347, J1918−0642, J2124−3358, J2322+2057. Figure style is the same as Figure C.1.</figcaption></figure>