Advanced Telescope for High Energy Astrophysics
|Organization||European Space Agency|
|Launch date||Not chosen|
|Launch vehicle||Ariane V or Atlas V|
|Collecting area||3 square metres (32 sq ft)|
|Focal length||20 metres (66 ft)|
The Advanced Telescope for High ENergy Astrophysics (ATHENA) is a proposed X-ray telescope. It is an ESA forking/rebooting of the International X-ray Observatory (IXO) project planned by NASA, ESA, and JAXA from about 2008 to 2011. In 2011, NASA pulled out. It was a candidate for the first (L1) L-class mission within the ESA Cosmic Vision Programme. It lost to the Jupiter Icy Moon Explorer. It may be a candidade for the next L-class mission.
In the original plan it was to be launched in 2021 as a joint effort by the United States space agency NASA, the European Space Agency (ESA), and the Japan Aerospace Exploration Agency (JAXA). In May 2008, ESA and NASA established a coordination group involving all three agencies, with the intent of exploring a joint mission merging the ongoing XEUS and Constellation-X projects. This proposed the start of a joint study for IXO. IXO faced competition from two other missions, the Europa Jupiter System Mission (EJSM) and the Laser Interferometer Space Antenna (LISA). The mission was estimated to cost €850 million.
Science with IXO 
X-ray observations are crucial for understanding the structure and evolution of the stars, galaxies, and the Universe as a whole. X-ray images reveal hot spots in the Universe—regions where particles have been energized or raised to very high temperatures by strong magnetic fields, violent explosions, and intense gravitational forces. X-ray sources in the sky are also associated with the different phases of stellar evolution such as the supernova remnants, neutron stars, and black holes.
- What happens close to a black hole?
- How did supermassive black holes grow?
- How do large scale structures form?
- What is the connection between these processes?
To address these science questions, IXO will trace orbits close to the event horizon of black holes, measure black hole spin for several hundred active galactic nuclei (AGN), use spectroscopy to characterize outflows and the environment of AGN during their peak activity, search for supermassive black holes out to redshift z = 10, map bulk motions and turbulence in galaxy clusters, find the missing baryons in the cosmic web using background quasars, and observe the process of cosmic feedback where black holes inject energy on galactic and intergalactic scales.
This will allow astronomers to understand better the history and evolution of matter and energy, visible and dark, as well as their interplay during the formation of the largest structures.
Closer to home, IXO observations will constrain the equation of state in neutron stars, black holes spin demographics, when and how elements were created and dispersed into the intergalactic medium, and much more.
To achieve these science goals, IXO requires extremely large collecting area combined with good angular resolution in order to offer unmatched sensitivities for the study of the high-z Universe and for high-precision spectroscopy of bright X-ray sources.
The large collecting area required because, in astronomy, telescopes gather light and produce images by hunting and counting photons. The number of photons collected puts the limit to our knowledge about the size, energy, or mass of an object detected. More photons collected means better images and better spectra, and therefore offers better possibilities for understanding of cosmic processes.
IXO configuration 
The heart of IXO mission is a single large X-ray mirror with up to 3 square meters of collecting area and 5 arcsec angular resolution, which is achieved with an extendable optical bench with a 20 m focal length.
A key feature of the IXO mirror design is a single mirror assembly (Flight Mirror Assembly, FMA), which is optimized to minimize mass while maximizing the collecting area, and an extendible optical bench.
Unlike visible light, X-rays cannot be focused at normal incidence, since the X-ray beams would be absorbed in the mirror. Instead, IXO’s mirrors, like all prior X-ray telescopes, will use grazing incidences, scattering at a very shallow angle. As a result, X-ray telescopes consist of nested cylindrical shells, with their inner surface being the reflecting surface. However, as the goal is to collect as many photons as possible, IXO will have a bigger than 3m diameter mirror.
As the grazing angle is a function inversely proportional to photon energy, the higher-energy X-rays require smaller (less than 2 degrees) grazing angles to be focused. This implies longer focal lengths as the photon energy increases, thus making X-ray telescopes difficult to build if focusing of photons with energies higher than a few keV is desired. For that reason IXO features an extendible optical bench that offers a focal length of 20 m. A focal length of 20 meters was selected for IXO as a reasonable balance between scientific needs for advanced photon collecting capability at the higher energy ranges and engineering constraints. Since no payload fairing is large enough to fit a 20-meter long observatory, thus IXO has a deployable metering structure between the spacecraft bus and the instrument module.
IXO scientific goals require gathering many pieces of information using different techniques such as spectroscopy, timing, imaging, and polarimetry. Therefore, IXO will carry a range of detectors, which will provide complementary spectroscopy, imaging, timing, and polarimetry data on cosmic X-ray sources to help disentangle the physical processes occurring in them.
Two high-resolution spectrometers, a microcalorimeter (XMS or cryogenic imaging spectrograph (CIS)) and a set of dispersive gratings (XGS) will provide high-quality spectra over the 0.1 – 10 keV bandpass where most astrophysically abundant ions have X-ray lines. The detailed spectroscopy from these instruments will enable high-energy astronomers to learn about the temperature, composition, and velocity of plasmas in the Universe. Moreover, the study of specific X-ray spectral features probes the conditions of matter in extreme gravity field, such as around supermassive black holes. Flux variability adds a further dimension by linking the emission to the size of the emitting region and its evolution over time; the high timing resolution spectrometer (HTRS) on IXO will allow these types of studies in a broad energy range and with high sensitivity.
To extend our view of the high-energy Universe to the hard X-rays and find the most obscured black holes, the wide field imaging & hard X-ray imaging detectors (WFI/HXI) together will image the sky up to 18 arcmin field of view (FOV) with a moderate resolution (<150 eV up to 6 keV and <1 keV (FWHM) at 40 keV.
The detectors will be located on two instrument platforms—the Moveable Instrument Platform (MIP) and the Fixed Instrument Platform (FIP). The Moveable Instrument Platform is needed because an X-ray telescopes cannot be folded as it can be done with visible-spectrum telescopes. Therefore, IXO will use the MIP that holds the following detectors—a wide field imaging & hard X-ray imaging detector, a high-spectral-resolution imaging spectrometer, a high timing resolution spectrometer, and a polarimeter — and rotates them into the focus in turn.
The X-ray Grating Spectrometer will be located on the Fixed Instrument Platform. This is a wavelength-dispersive spectrometer that will provide high spectral resolution in the soft X-ray band. It can be used to determine the properties of the warm-hot-intergalactic medium, outflows from active galactic nuclei, and plasma emissions from stellar coronae.
A fraction of the beam from the mirror will be dispersed to a charge-coupled device (CCD) camera, which will operate simultaneously with the observing MIP instrument and collect instrumental background data, which can occur when an instrument is not in the focal position.
To avoid interfering the very faint astronomical signals with radiation from the telescope, the telescope itself and all its instruments must be kept cold. Therefore, the IXO Instrument Platform features a large shield that blocks the light from the Sun, Earth, and Moon, which otherwise would heat up the telescope, and interfere with the observations.
IXO optics and instrumentation will provide up to 100-fold increase in effective area for high resolution spectroscopy, deep spectral, and microsecond spectroscopic timing with high count rate capability.
The improvement of IXO relative to current X-ray missions is equivalent to a transition from the 200 inch Palomar telescope to a 22 m telescope while at the same time shifting from spectral band imaging to an integral field spectrograph.
Science operations 
IXO will be designed to operate for a minimum of 5 years, with a goal of 10 years, so IXO science operations are anticipated to last from 2021 to 2030.
See also 
- ESA - ATHENA
- Jonathan Amos (2 May 2012). "Esa selects 1bn-euro Juice probe to Jupiter". BBC News Online. BBC. Retrieved 13 May 2012.
- Announcing the International X-ray Observatory (IXO) - NASA
- Announcing the International X-ray Observatory (IXO) - ESA
- The International X-ray Observatory Activity submission in response to the Astro2010 Program Prioritization Panel RFI#1
- IXO Science Performance Requirements on the ESA web site
- IXO - Payload Definition Document
- IXO Mission Concept
- IXO Project Leadership
- "ATHENA technical and programmatic review report". ESA. ESA. 28 February 2012. Retrieved 13 May 2012.
- IXO Science Performance Requirements
- Stellar-Mass Black Holes and Their Progenitors, J. Miller et al.
- The Evolution of Galaxy Clusters Across Cosmic Time, M. Arnaud et al.
- The Missing Baryons in the Milky Way and Local Group, Joel N. Bregman et al.
- Cosmic Feedback from Supermassive Black Holes, Andrew C. Fabian et. al.
- The Behavior of Matter Under Extreme Conditions, F. Paerels et al.
- Spin and Relativistic Phenomena Around Black Holes, L. Brenneman et al.
- Formation of the Elements, John P. Hughes et al.
- IXO effective area plot and resolution plot
- Mechanical Overview of the International X-Ray Observatory, David W. Robinson, IEEE Aerospace Conference, p.3, 2009
- Design Concept for the International X-Ray Observatory Flight Mirror Assembly, Ryan S. McClelland, David W. Robinson, IEEE Aerospace Conference, 2009
- Uniform high spectral resolution demonstrated in arrays of TES x-ray microcalorimeters, Caroline Kilbourne et al., SPIE 2007
- Science with the XEUS High Time Resolution Spectrometer,D. Barret, 2008, Proc. of SPIE Vol. 7011, 70110E
- Treis, J., et al., 2008, Proc. of SPIE Vol. 7021, 70210Z
- XPOL: a photoelectric polarimeter onboard XEUS, Enrico Costa et al., Proceedings of SPIE Astronomical Instrumentation 2008 Conference, 23–28 June 2008 Marseille, France, Vol. 7011–15
- Development of a critical-angle transmission grating spectrometer for the International X-Ray Observatory, Ralf K. Heilmann et al., Proc. of SPIE Vol. 7437 74370G-8, 2009
- NASA International X-Ray Observatory Mission Site
- ESA International X-Ray Observatory Mission Site
- Catherine Cesarsky, International Year of Astronomy 2009 The Universe: Yours to Discover
- IXO documents on the ESA web site
- ESA - XEUS overview
- ESA - Observations: Seeing in X-ray wavelengths
- Astro2010 Decadal Survey
- 2000-2010 Decadal Survey