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arxiv: 2606.01644 · v1 · pith:GQ7AZ7XInew · submitted 2026-06-01 · 🌌 astro-ph.IM · astro-ph.CO

The Murchison Widefield Array Phase III upgrade: Sensitivity Doubled, Number of Baselines Quadrupled, Flexibility Enhanced, and EoR Observations Optimised

S.J. Tingay , M. Johnston-Hollitt , R.B. Wayth , T.A. Booler , J. Jones , Y. Wu , J. Gan , G. Sleap
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A. McPhail C. Wintle A. Williams C.J. Phillips L. Verduyn D. Emrich P. Giersch C.J. Riseley S. Duchesne C.M. Trott D. Null B.W. Myers C.D. Nunhokee N. Barry L. Dressler J. Ducharme B. Hazelton M. Lee E. Lilleskov M. Morales J. Pober Zhiqiang Shen Xiang-ping Wu Xiaoyu Hong M.D. Filipovi\'c S.E. Tremblay M. Walker
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classification 🌌 astro-ph.IM astro-ph.CO
keywords Murchison Widefield Arrayradio interferometryEpoch of Reionisationdigital receiverstelescope upgrade
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The pith

The Murchison Widefield Array Phase III upgrade doubles sensitivity by enabling full correlation of all 256 antenna tiles.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper describes the completion of the Phase III upgrade to the Murchison Widefield Array, which includes new digital receivers. These receivers allow the array to correlate signals from all 256 antenna tiles simultaneously, removing the previous limitation to 128 tiles. This change doubles the maximum instantaneous sensitivity and quadruples the number of interferometric baselines. The upgrade optimizes the telescope for Epoch of Reionisation observations and increases operational flexibility. It also prepares for future integration with the SKA-Low facility.

Core claim

The new digital receivers complement the existing ones such that the MWA now supports the full correlation of all 256 antenna tiles, releasing the prior constraint of correlating only 128 tiles at a time.

What carries the argument

The new fleet of digital receivers integrated with the MWAX correlator, which enables processing all 256 tiles.

Load-bearing premise

The new digital receivers integrate successfully with the existing receivers and MWAX correlator to deliver the performance gains without failures or losses.

What would settle it

If measurements after the upgrade show that the sensitivity remains the same as before or the number of usable baselines does not increase, the claim of doubled sensitivity and quadrupled baselines would be falsified.

Figures

Figures reproduced from arXiv: 2606.01644 by A. McPhail, A. Williams, B. Hazelton, B.W. Myers, C.D. Nunhokee, C.J. Phillips, C.J. Riseley, C.M. Trott, C. Wintle, D. Emrich, D. Null, E. Lilleskov, G. Sleap, J. Ducharme, J. Gan, J. Jones, J. Pober, L. Dressler, L. Verduyn, M.D. Filipovi\'c, M. Johnston-Hollitt, M. Lee, M. Morales, M. Walker, N. Barry, P. Giersch, R.B. Wayth, S. Duchesne, S.E. Tremblay, S.J. Tingay, T.A. Booler, Xiang-Ping Wu, Xiaoyu Hong, Y. Wu, Zhiqiang Shen.

Figure 1
Figure 1. Figure 1: The “Phase II Compact” array configuration (u, v) coverage. progress and mature, it is likely that further configurations will be made available, and ultimately fully user-defined configura￾tions. The initial five configurations are listed below and briefly described with example snapshot (u, v) coverages. In all cases, the (u, v) coverages are presented for a single time point, for a zenith pointing, for … view at source ↗
Figure 5
Figure 5. Figure 5: The “Full Array” array configuration (u, v) coverage. The Phase III array is marked by two significant evolutions, and a number of enabling changes to supporting sub-systems and infrastructure. The first significant development is the replace￾ment of the original, Phase I, correlator Ord et al. (2015) with the MWAX correlator Morrison et al. (2023). Implementation of the MWAX correlator (following a standa… view at source ↗
Figure 4
Figure 4. Figure 4: The “Phase I plus Hexes” array configuration (u, v) coverage. 2.5. Full Array This configuration realises the full 256 tile array (all available tiles) utilising critically sampled receivers, for maximum angular resolu￾tion, maximum sensitivity, and maximum (u, v) coverage ( [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 6
Figure 6. Figure 6: The five different signal path implementations (C1 – C5) that exist in the Phase III array. Phase III additions are shown in green. 4.1. Shanghai Astronomical Observatory (SHAO) receivers The SHAO receivers were designed and developed in collabora￾tion with the Shanghai Astronomical Observatory (SHAO) which contributed 16 units in total towards the MWA Phase III upgrade. They were designed to be a standalo… view at source ↗
Figure 8
Figure 8. Figure 8: The as-built NI receiver, showing the simple nature of the COTS equip￾ment and the straightforward packaging, in contrast to bespoke systems. Msps), a trigger input used for 1PPS synchronisation, a 1 Gb Ethernet port for M&C, and a 10 Gb Ethernet SFP+ port. A full NI receiver is comprised of eight individual FlexRIO modules that are physically housed in a 4U rack mountable enclosure alongside supporting ha… view at source ↗
Figure 7
Figure 7. Figure 7: SHAO receiver schematic (top panel) and as-built hardware (bottom panel). of the firmware that is programmed onto the FPGA when transi￾tioning between modes. The management of the FPGA firmware and configuration is handled by the on-board CPU which runs a lightweight Linux distribution (PetaLinux) and custom software that interacts with the MWA M&C system. 4.2. National Instruments (NI) receivers The Natio… view at source ↗
Figure 10
Figure 10. Figure 10: RF shielded cabinet. Left panel, cabinet open. Middle panel, cabinet closed. Right panel, cabinet installed inside environmental enclosure [PITH_FULL_IMAGE:figures/full_fig_p009_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: A rendering of the RF shielded cabinet inside the environmental enclo￾sure. inputs, and waveguides for ingress of fibre optic cables. The air￾conditioning plant that maintains the operating temperature within the cabinet is positioned at the other end. This end features a hinged door that allows the air-conditioning plant to be installed and removed. The exterior of this door features honeycomb RF gaskets… view at source ↗
Figure 12
Figure 12. Figure 12: Cabinet control unit. 4.4. Supporting subsystems A range of subsystems are required to support the primary ele￾ments of the new receivers, including devices to manage, control, and monitor the receivers, as well as devices to integrate the receivers into the wider MWA system architecture. In this section, we briefly describe these supporting subsystems. 4.4.1. Cabinet control unit Internal environmental m… view at source ↗
Figure 13
Figure 13. Figure 13: Phase III MWA clock and timing distribution architecture [PITH_FULL_IMAGE:figures/full_fig_p011_13.png] view at source ↗
Figure 15
Figure 15. Figure 15: Upper image: Cross sectional view of Power distribution and shielding module. Mains power is supplied through socket at (1) and across to a rail at (1A), inline noise filter at (2), and two IEC outlets at (3). Middle image: Populated power filter and distribution module with RF gasket fitted. Lower image: Enclosed Power filtering and distribution module with managed, networked AC power rails attached. The… view at source ↗
Figure 16
Figure 16. Figure 16: Top image: Design drawing of built rack mount solution. Bottom image: (top portion of image) two BFC PSU (silver boxes) connected with two banks of eight DoC PCBs via ribbon cable and coaxial cables. The bottom of the picture shows the CCU. This image demonstrates the constrained environment for airflow movement. from aliasing across the full 1.28 MHz coarse channel bandwidth, removing the band edge artif… view at source ↗
Figure 18
Figure 18. Figure 18: Top panel: Coax tile configuration. Bottom panel: Phase III converted RFoF tile configuration. Phase III additions are shown in green [PITH_FULL_IMAGE:figures/full_fig_p016_18.png] view at source ↗
Figure 19
Figure 19. Figure 19: Design drawing of the Tile Interface Unit [PITH_FULL_IMAGE:figures/full_fig_p016_19.png] view at source ↗
Figure 20
Figure 20. Figure 20: Design drawing of the Pad Power Supply Unit. deg.) in the 167 - 197 MHz frequency range. The data were iden￾tically processed with calibration and peeling using Hyperdrive Jordan et al. (2025) and the power spectra estimated with CHIPS Trott et al. (2016), following, for example, Nunhokee et al. (2025). As can be seen in the Figure, the so-called EoR window is filled with a uniform noise-like signal for t… view at source ↗
Figure 21
Figure 21. Figure 21: Two dimensional EoR power spectra, from Phase I/II data (left) and preliminary Phase III data (right), showing the improvements to the k∥ modes due to removal of aliasing artifacts from coarse channel edges. In both cases, one hour of data is used, from the east-west oriented polarisation visibilities obtained from observations of the EOR0 field (RA = 0 h, Dec = -27 deg.) in the 167 - 197 MHz frequency ra… view at source ↗
Figure 22
Figure 22. Figure 22: MWA (blue) and SKA-Low AA2 (black) (u, v) coverages for a single frequency at 150 MHz and for a zenith pointed snapshot. Top: full (u, v) coverages. Bottom: zoomed in (u, v) coverages. Acknowledgements We thank the anonymous referee for a close reading of the paper, and for offering comments that assisted in providing addi￾tional clarity for non-expert readers. This scientific work uses data obtained from… view at source ↗
read the original abstract

We describe the latest iteration of upgrades (designated Phase III) to the Murchison Widefield Array (MWA), in the fourth paper in a series that covers the evolution of the telescope from design concept to initial operational facility, and through two major upgrades. As part of the Phase III upgrade of the MWA, we report the completion of work to design, build, and deploy a new fleet of digital receivers that further optimise the MWA for Epoch of Reionisation observations. These receivers complement existing receivers, such that the MWA now supports the full correlation of all 256 antenna tiles currently in the array. This step releases the MWA from the prior constraint of having to correlate only 128 of the 256 tiles at any given time, which means that the maximum instantaneous sensitivity of the MWA is doubled and the maximum number of interferometric baselines is approximately quadrupled. The upgrade is fundamentally enabled by the new MWAX correlator and various other improvements to the MWA sub-systems. In this paper we describe the new digital receivers and the other improvements that result in the Phase III system. A range of operational benefits arise from the upgrade and scientific flexibility is increased. We also comment on the transition from the MWA to the SKA-Low facility near the end of the decade, including a description of some unique science opportunities utilising joint MWA/SKA-Low data during the Science Verification phase of the SKA-Low Array Assembly 2 (AA2) period.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 0 minor

Summary. The manuscript describes the Phase III upgrade to the Murchison Widefield Array (MWA), reporting the completion of new digital receivers that complement existing ones to enable full correlation of all 256 antenna tiles. This removes the prior limit of correlating only 128 tiles, doubling maximum instantaneous sensitivity and approximately quadrupling the number of baselines. The upgrade is enabled by the MWAX correlator and other subsystem improvements; the paper also covers resulting operational benefits, increased flexibility for Epoch of Reionisation observations, and prospects for joint MWA/SKA-Low data during the SKA-Low AA2 Science Verification phase.

Significance. If the upgrade has been successfully deployed as described, the removal of the 128-tile correlation constraint provides a direct and substantial increase in MWA performance for EoR science, with the quadrupled baseline count improving uv-coverage and sensitivity on relevant scales. The work also supplies engineering documentation useful for the community and outlines a practical bridge to SKA-Low operations.

major comments (1)
  1. [Abstract] Abstract and main text: the central claim that the upgrade is complete and delivers doubled sensitivity plus quadrupled baselines is presented without any supporting on-sky measurements, system-temperature verification, baseline-count validation, or error analysis from the integrated MWAX + new-receiver system. This evidence is load-bearing for the performance assertions.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful review and constructive feedback on our manuscript describing the MWA Phase III upgrade. We address the single major comment below.

read point-by-point responses

  1. Referee: [Abstract] Abstract and main text: the central claim that the upgrade is complete and delivers doubled sensitivity plus quadrupled baselines is presented without any supporting on-sky measurements, system-temperature verification, baseline-count validation, or error analysis from the integrated MWAX + new-receiver system. This evidence is load-bearing for the performance assertions.

    Authors: The performance figures quoted in the abstract and main text follow directly from the change in the number of correlated tiles (128 to 256). The number of baselines increases exactly from C(128,2) to C(256,2), a factor of approximately four; the instantaneous sensitivity doubles because twice as many tiles now contribute to every observation. These are deterministic consequences of array size and do not require on-sky data to state as the new maximum capability. The new receivers were designed and tested to match the system temperature of the existing fleet. We agree, however, that empirical on-sky validation, baseline verification, and error analysis of the integrated MWAX + receiver system would strengthen the performance claims. Because the present manuscript is an engineering description of the upgrade deployment, we will revise the abstract and relevant sections to make explicit that the quoted gains are the calculated maximum values based on tile count, and we will add a brief statement that detailed on-sky verification is planned for a follow-up publication. revision: yes

Circularity Check

0 steps flagged

No circularity; purely descriptive engineering report with direct claims

full rationale

The manuscript is a factual report on completed hardware deployment and integration. The central claims (full 256-tile correlation now supported, doubling sensitivity and quadrupling baselines) follow directly from the stated design change and reported success with the MWAX correlator; no equations, fitted parameters, predictions, or self-referential derivations appear. Self-citations to prior papers in the series are present but not load-bearing for the upgrade description. No steps reduce to inputs by construction.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

No mathematical model, free parameters, axioms, or invented entities are invoked; the document is a hardware and operations report.

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Reference graph

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