The Hot and Energetic Universe: The X-ray Integral Field Unit (X-IFU) for Athena+

D. Barret; J. W. den Herder; L. Piro; L. Ravera; R. Den Hartog; C. Macculi; X. Barcons; M. Page; S. Paltani; G. Rauw; J. Wilms; M. Ceballos; L. Duband; L. Gottardi; S. Lotti; J. de Plaa; E. Pointecouteau; C. Schmid; H. Akamatsu; D. Bagliani; S. Bandler; M. Barbera; P. Bastia; M. Biasotti; M. Branco; A. Camon; C. Cara; B. Cobo; L. Colasanti; J. L. Costa-Kramer; L. Corcione; W. Doriese; J. M. Duval; L. Fabrega; F. Gatti; M. de Gerone; P. Guttridge; R. Kelley; C. Kilbourne; J. van der Kuur; T. Mineo; K. Mitsuda; L. Natalucci; T. Ohashi; P. Peille; E. Perinati; C. Pigot; G. Pizzigoni; C. Pobes; F. Porter; E. Renotte; J. L. Sauvageot; S. Sciortino; G. Torrioli; L. Valenziano; D. Willingale; C. de Vries; H. van Weers

arXiv · 1308.6784

The Hot and Energetic Universe: The X-ray Integral Field Unit (X-IFU) for Athena+

View original source ↗Read source document ↗Export metadata ↓

Abstract

The Athena+ mission concept is designed to implement the Hot and Energetic Universe science theme submitted to the European Space Agency in response to the call for White Papers for the definition of the L2 and L3 missions of its science program. The Athena+ science payload consists of a large aperture high angular resolution X-ray optics and twelve meters away, two interchangeable focal plane instruments: the X-ray Integral Field Unit (X-IFU) and the Wide Field Imager (WFI). The X-IFU is a cryogenic X-ray spectrometer, based on a large array of Transition Edge Sensors (TES), offering 2.5 eV spectral resolution, with ~5" pixels, over a field of view of 5 arc minutes in diameter. In this paper, we briefly describe the Athena+ mission concept and the X-IFU performance requirements. We then present the X-IFU detector and readout electronics principles, the current design of the focal plane assembly, the cooling chain and review the global architecture design. Finally, we describe the current performance estimates, in terms of effective area, particle background rejection, count rate capability and velocity measurements. Finally, we emphasize on the latest technology developments concerning TES array fabrication, spectral resolution and readout performance achieved to show that significant progresses are being accomplished towards the demanding X-IFU requirements.

Explore related subjects

astro-ph.IM

Keep this discovery

BibTeX RIS

D. Barret, J. W. den Herder, L. Piro, L. Ravera, R. Den Hartog, C. Macculi, X. Barcons, M. Page, S. Paltani, G. Rauw, J. Wilms, M. Ceballos, L. Duband, L. Gottardi, S. Lotti, J. de Plaa, E. Pointecouteau, C. Schmid, H. Akamatsu, D. Bagliani, S. Bandler, M. Barbera, P. Bastia, M. Biasotti, M. Branco, A. Camon, C. Cara, B. Cobo, L. Colasanti, J. L. Costa-Kramer, L. Corcione, W. Doriese, J. M. Duval, L. Fabrega, F. Gatti, M. de Gerone, P. Guttridge, R. Kelley, C. Kilbourne, J. van der Kuur, T. Mineo, K. Mitsuda, L. Natalucci, T. Ohashi, P. Peille, E. Perinati, C. Pigot, G. Pizzigoni, C. Pobes, F. Porter, E. Renotte, J. L. Sauvageot, S. Sciortino, G. Torrioli, L. Valenziano, D. Willingale, C. de Vries, H. van Weers. 2013-08-30. The Hot and Energetic Universe: The X-ray Integral Field Unit (X-IFU) for Athena+. https://arxiv.org/abs/1308.6784

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

The EDD Radio Astronomy Backend Framework

Modern digital radio astronomy receivers produce increasingly wide-bandwidth, high bit-rate data streams that necessitate the development of flexible, scalable, and maintainable backend processing and recording systems. Historically, such backend instrumentation has been tightly coupled to telescope observing modes, limiting reuse between observatories and science cases. We present the Effelsberg Direct Digitisation (EDD) backend framework, a software-defined architecture for constructing real-time radio astronomy backends on commodity off-the-shelf computing infrastructure. We describe its design, implementation, supported observing modes, and operational deployments. EDD separates a common core framework from plugin-provided observing capabilities. The core provides orchestration, telescope interfaces, pipeline lifecycle management, monitoring, and deployment tooling, while plugins implement processing pipelines for specific observing modes. The framework is designed to support both single-dish and interferometric instruments through site-specific configuration and plugin selection. EDD currently supports spectroscopy and spectropolarimetry, pulsar timing and searching, baseband recording, very long baseline interferometry, correlation, and beamforming. Operational deployments include the Effelsberg 100-m telescope, the SKA-MPI prototype dish, the Thai National Radio Telescope, and the ARGOS interferometric prototype array. By separating common services, observing-mode plugins, and site-specific configuration, it allows backend capabilities to be deployed across heterogeneous telescope environments and provides a community resource for broadband radio astronomy instrumentation.

astro-ph.IM↗

arXiv2026

Bayesian Superiority in On/Off analysis

We present a detailed comparison of Bayesian criteria with three non-informative priors - flat, Jeffreys, and scale-invariant - for testing a signal against an unknown background and compare them with the classical frequentist Li-Ma approach in the On/Off problem. We perform Monte Carlo simulations for various background levels and evaluate the Li-Ma and Bayesian criteria by their Type I error rates. We then simulate a nonzero signal and compare the criteria in terms of Type II error rates. We find that the Bayesian criterion with the Jeffreys prior yields lower Type I and Type II error rates than the Li-Ma criterion. In addition, we show that the Bayesian criteria are more robust than the Li-Ma criterion when the background distribution is overdispersed relative to the Poisson distribution.

astro-ph.IM↗

arXiv2026

An RFSoC-based Backend and Timing System for the Balloon-borne Very Long Baseline Interferometry Experiment

We present the design and performance characterization of the digital backend and precision-timing system for the Balloon-borne Very Long Baseline Interferometry Experiment (BVEX), a pathfinder for high-frequency stratospheric VLBI at 22 GHz. The backend uses one of the four 14-bit analog-to-digital converter inputs on an AMD-Xilinx RFSoC 4x2. Although the converters support sampling rates up to 5 GSPS, the flight configuration digitizes the 2-4 GHz intermediate frequency at 4.096 GSPS. CASPER firmware provides both a high-resolution spectrometer for pointing and receiver verification, and a VLBI acquisition chain with two-bit requantization that records at a rate of about 8.2 Gbps. The timestamped data packets are sent over 100 Gigabit Ethernet (GbE) to a 16 TB NVMe array in a storage computer that draws approximately 70-80 W. The timing chain uses a Rakon oven-controlled crystal oscillator as a timing reference while a time-interval counter measures its drift relative to a GPS reference with approximately 60 ps resolution. This is the first deployment of an RFSoC-based VLBI backend and precision-timing system on a stratospheric balloon. Ground tests validated the backend, spectrometer, and timing chain. The August 2025 CSA STRATOS flight ended before reaching the target float altitude because of a balloon failure, and as a result no science observations were obtained. For the planned 2027 reflight, we are developing a conduction-cooled data storage computer with 24 TB of NVMe capacity and a direct data path from the 100 GbE interface to the NVMe array.

astro-ph.IM↗