Dublin Core The Dublin Core metadata element set is common to all Omeka records, including items, files, and collections. For more information see, http://dublincore.org/documents/dces/. Title A name given to the resource Faculty Publications Article Faculty Publications -Articles Dublin Core The Dublin Core metadata element set is common to all Omeka records, including items, files, and collections. For more information see, http://dublincore.org/documents/dces/. Creator An entity primarily responsible for making the resource Nobleson, K.; Dwivedi, Churchil; Desai, Shantanu; Joshi, Bhal Chandra; Grover, Himanshu; Deb, Debabrata; Vyasraj, Vaishnavi; Vara, Kunjal; Tahbildar, Hemanga; Susobhanan, Abhimanyu; Surnis, Mayuresh; Srivastava, Aman; Sardana, Shubhit; Takahashi, Keitaro; Amarnath; Arumugam, P.; Bagchi, Manjari; Batra, Neelam Dhanda; Chakraborty, Manoneeta; Chowdhury, Shaswata; Jacob, Shebin Jose; Jose, Jibin; Kala, Shubham; Kato, Ryo; Krishnakumar, M.A.; Meena, Kuldeep; Paladi, Avinash Kumar; Pandian, Arul; Rai, Kaustubh; Rana, Prerna; Singh, Manpreet; Singha, Jaikhomba; Shukla, Adya; Tarafdar, Pratik; Thiagraj, Prabu; Zuraiq, Zenia Title A name given to the resource The indian pulsar timing array data release 2: II. Customised single-pulsar noise analysis and noise budget Date A point or period of time associated with an event in the lifecycle of the resource 01-01-2026 Source A related resource from which the described resource is derived Journal of High Energy Astrophysics;Volume;53;Issue;;Article No.;100594; Identifier An unambiguous reference to the resource within a given context <a href="https://doi.org/10.1016/j.jheap.2026.100594" target="_blank" rel="noreferrer noopener">https://doi.org/10.1016/j.jheap.2026.100594</a> <br /><br /><a href="https://www.scopus.com/pages/publications/105033285648?origin=resultslist" target="_blank" rel="noreferrer noopener">https://www.scopus.com/pages/publications/105033285648?origin=resultslist</a> Coverage The spatial or temporal topic of the resource, the spatial applicability of the resource, or the jurisdiction under which the resource is relevant Nobleson K., International Research Organization for Advanced Science and Technology, Faculty of Advanced Science and Technology, Kumamoto University, 2-39-1 Kurokami, Kumamoto, Kumamoto City, 860-8555, Japan; Dwivedi C., Astronomy and Astrophysics Division, Physical Research Laboratory, Thaltej Campus, Thaltej, Gujarat, Ahmedabad, 380059, India; Desai S., Department of Physics, IIT Hyderabad, Telangana, Kandi, 502284, India; Joshi B.C., National Centre for Radio Astrophysics, SP Pune University Campus, Maharashtra, Pune, 411007, India, Department of Physics, Indian Institute of Technology Roorkee, Uttarakhand, Roorkee, 247667, India; Grover H., Department of Physics, Indian Institute of Technology Roorkee, Uttarakhand, Roorkee, 247667, India; Deb D., Centre for Space Research, North-West University, Private Bag X6001, Potchefstroom, 2520, South Africa; Vyasraj V., Department of Physics, IIT Hyderabad, Telangana, Kandi, 502284, India; Vara K., Department of Physics, Indian Institute of Science Education and Research, Bhauri Bypass Road, Madhya Pradesh, Bhopal, 462066, India; Tahbildar H., Department of Physics, Indian Institute of Science Education and Research, Bhauri Bypass Road, Madhya Pradesh, Bhopal, 462066, India; Susobhanan A., School of Physics, Indian Institute of Science Education and Research Thiruvananthapuram, Maruthamala PO, Kerala, Thiruvananthapuram, 695551, India; Surnis M., Department of Physics, Indian Institute of Science Education and Research, Bhauri Bypass Road, Madhya Pradesh, Bhopal, 462066, India; Srivastava A., Department of Physics, IIT Hyderabad, Telangana, Kandi, 502284, India, Department of Physics, GLA University, Uttar Pradesh, Mathura, 281406, India; Sardana S., Department of Physics, Indian Institute of Science Education and Research, Bhauri Bypass Road, Madhya Pradesh, Bhopal, 462066, India; Takahashi K., International Research Organization for Advanced Science and Technology, Faculty of Advanced Science and Technology, Kumamoto University, 2-39-1 Kurokami, Kumamoto, Kumamoto City, 860-8555, Japan; Amarnath, Raman Research Institute, Karnataka, Bengaluru, 560080, India; Arumugam P., Department of Physics, Indian Institute of Technology Roorkee, Uttarakhand, Roorkee, 247667, India; Bagchi M., The Institute of Mathematical Sciences, C.I.T. Campus, Taramani, Tamilnadu, Chennai, 600113, India, Homi Bhabha National Institute, Training School Complex, Anushakti Nagar, Maharashtra, Mumbai, 400094, India; Batra N.D., Indian Institute of Technology, Delhi, Hauz Khas, New Delhi, 110016, India; Chakraborty M., Department of Astronomy, Astrophysics, and Space Engineering, Indian Institute of Technology Indore, Madhya Pradesh, Indore, 453552, India; Chowdhury S., The Institute of Mathematical Sciences, C.I.T. Campus, Taramani, Tamilnadu, Chennai, 600113, India; Jacob S.J., Department of Physics, Government Brennen College Thalassery Kannur University, Kerala, Kannur, 670106, India; Jose J., Department of Astronomy, Astrophysics, and Space Engineering, Indian Institute of Technology Indore, Madhya Pradesh, Indore, 453552, India; Kala S., The Institute of Mathematical Sciences, C.I.T. Campus, Taramani, Tamilnadu, Chennai, 600113, India; Kato R., Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Tokyo, Mitaka, 181-8588, Japan; Krishnakumar M.A., Radio Astronomy Centre National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Tamilnadu, Udhagamandalam, 643001, India; Meena K., UM-DAE Centre for Excellence in Basic Sciences, University of Mumbai Vidyanagari, Maharashtra, Mumbai, 400098, India; Paladi A.K., Joint Astronomy Programme, Department of Physics, Indian Institute of Science, Karnataka, Bengaluru, 560012, India; Pandian A., Raman Research Institute, Karnataka, Bengaluru, 560080, India, Department of Physics and Electronics, CHRIST (Deemed to be University), Karnataka, Bengaluru, 560029, India; Rai K., Department of Physics, Indian Institute of Science Education and Research, Bhauri Bypass Road, Madhya Pradesh, Bhopal, 462066, India; Rana P., Department of Astronomy, University of Cape Town, Cape Town, 7700, South Africa, High Energy Physics, Cosmology &amp; Astrophysics Theory (HEPCAT) Group, Department of Mathematics and Applied Mathematics, University of Cape Town, Cape Town, 7700, South Africa; Singh M., Department of Physical Sciences, Indian Institute of Science Education and Research (IISER) Mohali, Sector 81, SAS Nagar, Punjab, Mohali, 140306, India; Singha J., High Energy Physics, Cosmology &amp; Astrophysics Theory (HEPCAT) Group, Department of Mathematics and Applied Mathematics, University of Cape Town, Cape Town, 7700, South Africa; Shukla A., Department of Physics, Indian Institute of Technology Roorkee, Uttarakhand, Roorkee, 247667, India; Tarafdar P., INAF - Osservatorio Astronomico di Cagliari, via della Scienza 5, Selargius (CA), 09047, Italy; Thiagraj P., Raman Research Institute, Karnataka, Bengaluru, 560080, India; Zuraiq Z., Department of Physics, Indian Institute of Science, Karnataka, Bengaluru, 560012, India Description An account of the resource We present the results of customised single-pulsar noise analysis of 27 millisecond pulsars from the second data release of the Indian Pulsar Timing Array (InPTA-DR2). We model various stochastic noise sources present in the dataset using stationary Gaussian processes and estimate the noise budget of the InPTA-DR2 using Bayesian inference, involving model selection, Fourier harmonics selection, and parameter estimation for each pulsar. We check the efficacy of our noise characterisation by performing the Anderson-Darling test for Gaussianity on the noise-subtracted residuals. We find that all 11 pulsars with time baseline ? 2.5 yr show Gaussian residuals and do not have evidence for any red noise process in the optimal model, except for PSR J1944 + 0907, which shows presence of DM noise. PSRs J0437 - 4715, J1909 - 3744 and J1939 + 2134 show preference for the most complicated noise model, having achromatic and chromatic red noise processes. Only 4 out of 15 pulsars with time baseline ? 2.5 yr show significant non-Gaussianity in noise-subtracted residuals. We suspect that this may require more advanced methods to model noise processes properly. A comparative study of six pulsars with data removed near solar conjunctions showed deviations from the parameter estimates obtained with the original dataset, indicating potential bias in red noise processes due to unmodeled solar-wind effects. The results presented in this work remain broadly consistent with the InPTA-DR1 noise budget, with better constraints obtained on noise processes for several pulsars and support for achromatic red noise in PSR J1012 + 5307 due to the extended time baseline. 2026 The Author(s). Subject The topic of the resource Gravitational waves; Neutron stars; Pulsar timing arrays; Pulsars Publisher An entity responsible for making the resource available Elsevier B.V. Relation A related resource ISSN: 22144048; Language A language of the resource English Type The nature or genre of the resource Article Rights Information about rights held in and over the resource All Open Access; Green Open Access Format The file format, physical medium, or dimensions of the resource online