Logo

This web portal uses third-party cookies to track visits to the website only, no personal information is collected.

By continuing to use the site you are agreeing to our use of cookies. Learn more

I understand

Use of cookies

This website uses Google Analytics, a web analytics service provided by Google, Inc. (“Google”). Google Analytics uses “cookies”, which are text files placed on your computer, to help the website analyze how users use the site. The information generated by the cookie about your use of the website (including your IP address) will be transmitted to and stored by Google on servers in the United States. The IP address will be truncated before transmission. On our behalf Google will use this information for the purpose of evaluating your use of the website, compiling reports on website activity and providing other services relating to website activity and internet activity in connection with the use of the website. Google will not associate your IP address with any other data held by Google.

If you do not wish to receive a cookie, or if you wish your browser to notify you when you receive a cookie, you may use the option on your web browser to disable cookies. Click on the 'help' section of your browser to learn how to change cookie preferences.

Nuggets Gallery

In this section, you will find illustrations released in the #AthenaNuggets.

Back to Athena Gallery

 

  • Predictions for the redshifts and luminosities of ~600,000 AGN that will be identified with a multilayered 1-year Athena WFI survey, including >400 sources at z > 6, compared to current Chandra and XMM-Newton surveys. Credit: Aird, Comastri et al. 2013 arXiv1306.232. Updated by Andrea Merloni (MPE) (2017). More info
  • Composite of eight stills from the simulation of the tidal disruption of a white dwarf star by an intermediate-mass black hole by Rosswog, Ramirez-Ruiz & Rix (2009, DOI , © AAS. Reproduced with permission) . More info
  • Artistic impression of material falling into a supermassive black hole in the centre of a galaxy (not to scale). Credits: NASA/Aurore Simonnet, Sonoma State University. More info
  • Left: Pictorial representation energy released by the SMBH at the center of the galaxy, via collimated and uncollimated winds. Right: simulation of the X-ray spectrum resulting from a system showing two types of X-ray winds. Credit: ESA/AOES Medialab. More info
  • Spectrum: A simulated X-IFU X-ray spectrum of a medium bright afterglow at z=7, characterized by deep narrow resonant lines of Fe, Si, S, Ar, Mg, from the gas in the environment of the GRB. Background: 100 ks Chandra Deep Field South WFI simulation. Credit: Jonker, O’Brien et al. 2013: arXiv 1306.2336 & WFI Team. Composition: ACO Team. More info
  • Expected abundances measured by Athena in a bright ‘local’ cluster of galaxies. The color bars show which fraction of the element is produced by either core-collapse supernovae (SN cc, green), type Ia supernovae (SNIa, blue) or Asymptotic Giant Branch stars (AGB, red). Credit: J. de Plaa (SRON). More info
  • The Hitomi SXS spectrum of highly-ionized iron ions is superimposed on an enhanced Chandra X-ray image of the Perseus cluster core. The nucleus of NGC1275 is at the centre. The yellow clipped square shows the field of view of the 35 pixel SXS. Credit: A.C. Fabian and Hitomi Collaboration. More info
  • Left: the production of a Mirror Module: ribbed wafers are stacked in an SPO module and 4 are combined in two pairs to form a Mirror Module. Right: front view of the Mirror Assembly Module showing the > 1000 MM required to reach the 2m2 effective area at 1 keV. Credit: R. Willingale and ACO Team. More info
  • Spin as a probe of SMBH growth history. The theoretical expectations for each SMBH growth scenario (dotted histograms) is shown (Berti & Volonteri 2008) and compared to simulated Athena measurements (solid histograms), accounting realistically for all observational errors and spectral complexities. Credit: G. Miniutti. Composition: ACO Team. More info
  • Athena/WFI design drawing showing the main subsystems of the instrument. ICPU stands for 'Instrument Control and Power Distribution Unit'. Date: March 2017; Credit: WFI Team. Composition: ACO Team. More info
  • Reconstructed bulk motion map of the hot gas in a galaxy cluster from a simulated Athena X-ray Field Unit (X-IFU) observation. Courtesy: P. Peille, E. Pointecouteau, V. Biffi, E. Rasia, K. Dolag, S. Borgani, J. Wilms. Composition: ACO Team. More info
  • Engineering Model cooler developed for the SAFARI instrument on-board the SPICA satellite. 3D views: Credit F. Bancel (SBT). Composition: ACO Team. More info
  • Right: Artist’s impression of Jupiter’s X-ray aurora and the magnetosphere. Left: Images of Jupiter’s X-ray aurora during varying solar wind conditions in 2011 [Dunn et al. 2016] overlaid on visible images of Jupiter from the Hubble Space Telescope. Credit: JAXA & NASA: STScI/CXC. Composition: ACO Team. More info
  • Artist’s impression of an equatorial accretion disc wind as observed in X-ray binaries and a simulated X-IFU spectrum in the Fe region. Credit: image (Chandra/NASA). Inset: Fig. 2, Motch et al 2013. More info
  • Preliminary spectra of the background in the Athena Instruments. Left - X-IFU background for different configurations of the FPA. Right - WFI background showing contributions from different particle populations. Credit: A. von Kienlin and the WFI team. Composition: ACO Team. More info
  • A multicolour Subaru/FOCAS image of the shell-like bubble MH9-11 around the ultra-luminous X-ray source Holmberg IX X-1. Credit: Grisé et al. 2011, ApJ 734, 23. More info
  • Background: This artist’s impression shows how ULAS J1120+0641, a very distant quasar powered by a black hole with a mass two billion times that of the Sun, may have looked. Credit: ESO/M. Kornmesser. Composition: ACO Team. More info
  • Background: WFI end-to-end M31 simulation. Credit: T. Dauser. Inset: a mosaic of 7 X-IFU pointings of 100ks each that are based on a numerically simulated massive, local galaxy cluster. Credit: E. Cucchetti, E. Pointecouteau, P. Peille & N. Clerc; numerical cluster simulations by E. Rasia, V. Biffi, S. Borgani, and K. Dolag. Compositon: ACO Team. More info
  • SIXTE simulation of a single 100ks Athena/WFI pointing of the Chandra Deep Field South. Galaxy groups and clusters identified in the field are visible as extended red (i.e. soft) sources. Credit: WFI Team. Composition: ACO Team. More info
  • Left: Photograph of a prototype array developed for the X-IFU demonstration unit. Right: Resistance vs temperature curve of a typical TES phase transition. Credit: X-IFU Team. More info
  • Simulated emission of X-rays (pink colors) and radio waves (green) for a portion of a large cosmological simulations. Credit: Vazza et al. 2017. More info
  • Left: predicted number of electron-hole pairs per pixel per read-out time of the WFI generated by UV/Vis photons from early-type stars. Right Panel: FW OBF sample of the WFI imaging detector successfully tested under vibration and acoustic loads. Credit: Marco Barbera. Composition: ACO Team. More info
  • Left: N-body simulation of the cosmic web as traced by galaxies and active galactic nuclei. Credit: Antonis Georgakakis. Right: artistic impression of an AGN. Credit: ESA/NASA. Composition: ACO Team. More info
  • Background: Photograph of the detector plane, showing a kilo-pixel TESs array in the 2x40 FDM testbed. Right: Spectrum of Mn Kalpha complex with a resolution of 1.8 eV FWHM at 1.25 MHz with improved GSFC TESs. Left: Results of the 9 multiplexing demonstration. Credit: Hiroki Akamatsu. Composition: ACO Team. More info
  • Pie: The cosmic budget of ‘ordinary’ matter. Plots: RGS XMM-Newton spectra of 1ES 1553+113. Credits: Pie chart - ESA, Spectra - F. Nicastro, J. Kaastra, Y. Krongold et al. Nature, 558, 406 (2018). Composition: ACO Team. More info
  • Right: artistic vie of a flare due to CME erupted. Credit: NASA. Left: 3D MHD (Magneto Hydro Dinamic) simulation of flaring activity occurring close to a circumstellar disk around a rotating magnetized star.Credit: S. Orlando. Composition: ACO Team. More info
  • Simulated wavelet filtered image of an 80 ks Athena/WFI observation. Credit: Chaoli Zhang, Miriam Ramos-Ceja, Florian Pacaud, Thomas H. Reiprich, and also the SIXTE team. Composition: ACO Team. More info
  • Front: Scheme of DEPFET detector used in the Wide Field Imager (WFI). Background: SIXTE WFI simulations of the galactic center (left) and the CDSF (right). Credit: WFI Team. Composition: ACO Team. More info
  • The distribution of galaxies (left) and X-ray gas (right) predicted by the state-of-the-art computer simulation Illustris. Athena will reveal the properties of the invisible gas that fills the space between galaxies in the cosmic web. Credit: Illustris Collaboration / Illustris Simulation. More info