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EPTA meeting 2025 @ SISSA

Nov 17 – 21, 2025
SISSA (Main building)
Europe/Rome timezone

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Contribution List

33 out of 33 displayed
  1. 14. MPIfR
    Jędrzej Jawor (MPIfR)
    11/18/25, 2:15 PM
  2. 15. Manchester/Birmingham
    Bhavnesh Bhat (University of Manchester)
    11/18/25, 2:30 PM
  3. 16. FORTH
    John Antoniadis
    11/18/25, 2:45 PM
  4. 18. ASTRON
    Aditya Parthasarathy (ASTRON)
    11/18/25, 3:15 PM
  5. 19. Nançay/Orléans
    Gilles Theureau (Orléans)
    11/18/25, 3:45 PM
  6. 20. Shanghai
    Kuo Liu (SHAO)
    11/18/25, 4:00 PM
  7. 22. MPTA
    Kathrin Grunthal (MPIfR)
    11/18/25, 4:15 PM
  8. 23. Milan
    Alberto Sesana (Universita` di Milano Bicocca)
    11/18/25, 4:30 PM
  9. 7. InPTA Updates: DR2 and beyond
    Pratik Tarafdar (INAF-OAC)
    11/18/25, 4:45 PM

    The Indo-Japanese collaboration InPTA recently published its second data release making high-precision dispersion measures and timing solutions available for 27 millisecond pulsars across a 7 year time baseline, spanning simultaneous frequency coverage of 300-500 MHz and 1260-1460 MHz uGMRT receivers. This data is being combined with global PTA datasets for the upcoming IPTA DR3. The talk...

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  10. 25. PPTA - Update
    Andrew Zic
    11/19/25, 9:05 AM
  11. 26. CPTA - update
    Siyuan Chen
    11/19/25, 9:20 AM
  12. 31. Updated constraint on the GWB amplitude from the gamma-ray PTA
    Serena Valtolina
    11/19/25, 9:35 AM
  13. 11. Long term pulse profile variability in millisecond pulsars
    Bhavnesh Bhat (University of Manchester)
    11/19/25, 9:50 AM

    Pulsars generally exhibit stable integrated pulse profiles, making them
    powerful tools for precision timing experiments. While short-term vari-
    ability, such as mode-changing and nulling, is known in young pulsars,
    studies suggest that long-term profile changes may also occur, potentially
    correlated with the spin-down rate. Millisecond pulsars (MSPs), typi-
    cally more stable, have shown...

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  14. 9. Building a pulsar timing pipeline for ARGOS
    Samuel Gullin (Argos / Forth / Univerity of Crete)
    11/19/25, 10:05 AM

    ARGOS-CDS is the design study phase for the planned ARGOS telescope, a leading-edge, low-cost radio interferometer to be built in Europe. It will perform continuous wide-field monitoring in between 1 GHz and 3 GHz, and high-cadence, high-SNR observations of all PTA pulsars as the most sensitive instrument in the EPTA.

    The pulsar science pipeline, arpa, for ARGOS is being developed as new,...

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  15. 32. Session Introduction
    Sara Manzini (APC - Université Paris Cité)
    11/19/25, 10:40 AM
  16. 4. Data span and frequency coverage requirements for robust detection and inference in PTAs - A case study with EPTA DR2
    irene ferranti (University of Milano-Bicocca)
    11/19/25, 10:45 AM

    Pulsar Timing Arrays (PTAs) are approaching the sensitivity required to make a 5-σ detection of the nanohertz stochastic gravitational wave background (GWB), making it crucial to develop a comprehensive understanding of our data and of the outcomes of our analysis pipelines. Thus, it becomes essential to understand a counterintuitive feature revealed in the recent results from the European...

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  17. 27. Impact of DM noise modeling on the GWB search
    Danilo Zecca (Università del Salento)
    11/19/25, 11:00 AM

    Building on Iraci et al. (2024), we study the impact of our main modelling routines to mitigate the effects of the ionized interstellar medium during the search for the Gravitational Wave Background (GWB) with Pulsar Timing Arrays (PTAs). To this scope, we use synthetic PTA datasets and model the DM variations as Gaussian Processes (DM GP) using the Enterprise software to test the consistency...

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  18. 13. Modeling Non-Gaussianities using Gaussian Mixture Models
    Mikel Falxa (Università di Milano Bicocca)
    11/19/25, 11:15 AM

    In Pulsar Timing Array (PTA) data analysis, noise is typically assumed to be Gaussian, and the marginalized likelihood has a well-established analytical form derived within the framework of Gaussian processes. However, this Gaussianity assumption may break down for certain classes of astrophysical and cosmological signals, particularly for a gravitational wave background (GWB) generated by a...

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  19. 28. Optimizing gravitational-wave sky maps for PTAs
    Kathrin Grunthal (MPIfR)
    11/19/25, 11:30 AM

    Gravitational-wave sky maps are a key tool for understanding the origin of the gravitational-wave background (GWB) signal in PTA data sets. Moreover, as they depict the gravitational-wave power sky distribution is, close-by supermassive-black-hole binaries are potentially revealed as hot-spots on these maps. A crucial factor for the identification of these hot-spots and the resulting level of...

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  20. 30. Cosmic Variance in Anisotropy Searches at Pulsar Timing Arrays
    Mauro Pieroni
    11/19/25, 11:45 AM

    In the context of cosmology, the statistical uncertainty induced by a small sample size is typically referred to as cosmic variance. Several works have considered its relevance in the context of gravitational wave (GW) detection using pulsar timing array (PTA) experiments. In this talk, I will discuss the impact of cosmic variance on the measurement of anisotropies in the GW background using...

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  21. 34. Session Introduction
    Dr Golam Shaifullah (Dipartimento di Fisica ``G. Occhialini", Universit{\'a} degli Studi di Milano-Bicocca, Piazza della Scienza 3, I-20126 Milano, Italy)
    11/19/25, 3:30 PM
  22. 10. Update on LOFAR and NenuFAR
    Mark Brionne (INAF-OACa Cagliari)
    11/19/25, 3:35 PM

    In this talk, we will discuss on the recent updates on LOFAR and NenuFAR.

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  23. 5. Polarization Calibration in LOFAR Beamformed Data
    Caterina Tiburzi (inaf-oac)
    11/19/25, 3:50 PM

    LOFAR’s beamformed mode enables diverse science cases and data collected in this mode proved to be fundamental for the latest EPTA data release, DR2low (Iraci and Chalumeau et al 2025).
    However, polarization analysis in beamformed mode has remained largely out of reach due to the absence of a reliable polarization calibration framework.

    Here, I will present our cutting-edge polarization...

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  24. 21. DR2low and IISM turbulence with LOFAR
    Francesco Iraci (INAF-OAC)
    11/19/25, 4:05 PM

    Low-frequency radio data are highly valuable for studying propagation effects in pulsar signals, such as dispersion measure (DM) variations. In this work, we combine for the first time observations from LOFAR (100–200 MHz) and NenuFAR (30–90 MHz) with EPTA DR2new+ data to build a new dataset, the so-called DR2low. It consists of 12 pulsars observed over a time span of ∼11 years with radio...

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  25. 12. Simulating the IISM to improve PTAs noise modelling
    Ruggero Valdata
    11/19/25, 4:20 PM

    The Ionised interstellar medium (IISM) is a major source of unmodelled noise in Pulsar Timing Array (PTA) data. Spatial effects like scattering and scintillation lead to short-term diffractive and long-term refractive noise. These overlaid with variations in electron density further complicate and bias PTA noise models - directly impacting sensitivity to low-frequency gravitational waves....

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  26. 33. Session Introduction
    irene ferranti (University of Milano-Bicocca)
    11/20/25, 10:25 AM
  27. 3. Constraints on Ultralight Scalar and Dark photon Dark Matter from PPTA-DR3 and EPTA-DR2
    XiaoSong Hu (Beijing Normal University)
    11/20/25, 10:30 AM

    The cold dark matter (CDM) model successfully describes the Universe on large scales, yet faces challenges at sub-galactic scales. Ultralight dark matter (ULDM), with particle masses around $10^{-22}$ eV, offers a promising solution to these small-scale issues. Pulsar timing arrays (PTAs), originally designed to detect nanohertz gravitational waves, also provide a sensitive probe for ULDM...

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  28. 6. Exploring Neural Network Methods for Sky Localisation of PTA sources
    Ludovica Carbone (Università degli Studi di Milano-Bicocca)
    11/20/25, 10:45 AM

    Accurate localisation of continuous gravitational waves (CGWs) from supermassive black hole binaries (SMBHBs) remains one of the key challenges in Pulsar Timing Array (PTA) data analysis. Traditional searches based on the $\mathcal{F}_e$ statistic provide a robust analytic framework, but the resulting sky maps are strongly affected by the PTA antenna pattern, which redistributes signal power...

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  29. 2. Studying eccentric supermassive black hole binaries in PTA
    Sara Manzini (APC - Université Paris Cité)
    11/20/25, 11:00 AM

    The most plausible astrophysical sources for PTA experiments are supermassive black hole binaries (SMBHBs), which emit gravitational waves (GWs) that incoherently superpose to form a stochastic GW background (SGWB). Particularly massive and nearby SMBHBs produce strong signals that may stand out above the GWB. PTAs will observe the early inspiral of these systems at large orbital separations,...

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  30. 29. Constraining Preferred-Frame Effects in Gravity with Binary Pulsars
    Massimo Vaglio (SISSA)
    11/20/25, 11:15 AM

    We constrain Einstein-Aether gravity, a leading alternative to General Relativity that introduces a preferred-frame via a dynamical time-like vector field, using high-precision pulsar timing observations from EPTA. Our analysis incorporates both conservative and dissipative first post-Newtonian corrections and utilizes full times of arrival from multiple pulsars, processed with Vela.jl, a...

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  31. 8. Light Bending Under General Relativity: A study of pulsar blackhole binaries
    Jyotijwal Debnath (INAF Cagliari)
    11/20/25, 11:30 AM

    We present a fully general relativistic formalism to study propagation delays in the radio signals of pulsars in binary systems, arising from the gravitational bending of light. This bending delay is a significant contribution in neutron star–neutron star systems and becomes even more pronounced in neutron star–black hole binaries. Applying our framework to hypothetical neutron star–black hole...

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  32. 17. Sardinia/Cagliari
    Delphine Perrodin (INAF - Osservatorio Astronomico di Cagliari)
    11/20/25, 11:45 AM
  33. 24. InPTA