ATHENA - in a nutshell - Athena
ATHENA in brief
The selection process for the second Large mission ( L2 ) began in March 2013, when ESA issued a call to the European science community to suggest the scientific themes to be pursued by the Cosmic Vision programme's second and third Large missions.
In November 2013, the theme of "the Hot and energetic Universe" was selected for L2, with "the gravitational Universe" (now LISA) selected for L3. Athena is due to launch in the early 2030s, with possible optimisation during the implementation phase under study.
Now officially selected for L2, Athena is currently in Phase B1 Study. Once the mission design and costing have been completed, it will eventually be proposed for 'adoption' in 2022, before the start of construction.
By combining a large X-ray telescope with state-of-the-art scientific instruments, Athena will address key questions in astrophysics, including: how and why does ordinary matter assemble into the galaxies and galactic clusters that we see today? How do black holes grow and influence their surroundings?
The black holes which lurk at the centre of almost all galaxies play a fundamental role in their formation and evolution.To investigate this connection, Athena will observe X-ray emission from very hot material just before it is swallowed by a black hole, measuring distortions due to gravitational light-bending and time-delay effects in this extreme environment. Athena will also be able to determine the spin of the black hole itself.
Athena's powerful instruments will also allow unprecedented studies of a wide range of astronomical phenomena. These include distant gamma-ray bursts, the hot gas found in the space around clusters of galaxies, the magnetic interplay between exoplanets and their parent stars, Jupiter's auroras and comets in our own Solar System.
Athena is also a powerful, general-purpose observatory, able to address a wide range of current astrophysical topics
The Athena mission concept was proposed by the community consortium, and will be studied in detail by ESA.
The instruments comprise
— the X-ray Integral Field Unit (X-IFU) a cryogenic imaging spectrometer covering the 0.3 to 10 keV energy range with unprecedented energy resolution, over a field of view a few arcminutes across
— the Wide Field Imager (WFI) covering the 0.1 to 12 keV energy range, based on a silicon active pixel sensor. It features a large field of view, excellent spatial and energy resolution and count rate capabilities up to the Crab regime (2-10 keV flux ~10-8 erg cm-2 s-1).
During each sky observation one of the two instruments will be placed in the focal plane of the X-ray telescope (focal length ~12m limited by the launcher fairing).
This mirror provides:
— effective area of at least 1.4 m2 at 1 keV
— angular resolution of 5 arc seconds Half Energy Width (HEW) at <7 keV
— field of view diameter >40 arc minutes
This combination of large area, high angular resolution and large field of view are made possible using the Silicon Pore Optics (SPO) technology developed by ESA and Cosine Measurement Systems over the last decade.
SPO utilises commercially available Si wafers which have surface figure and roughness quality ideally suited to X-ray optics applications.
Athena is currently baselined to be launched into a halo orbit at the Sun-Earth L1 (1st Lagrangian) point, which provides for high observing efficiency, uninterrupted observations, and a benign thermal environment.