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Science requirements

A preliminary set of Science requirements for the Athena mission is given here:

Science Requirements
Effective Area (total) 1m2 @ 1.25 keV (goal 1.2)
0.52 @ 6 keV (goal 0.7)
Black hole evolution
Large scale strucure
Cosmic feedback
Strong gravity
Spectral Resolution (FWHM) ΔE = 3 eV (@ 6 keV) within 2x2 arcmin
(goal of 2.5 eV and 4x3 arcmin)
missing baryons
ΔE = 150 eV (@ 6 keV) within 25 arcmin diam
(goal of 125 eV and 30 arcmin)
Black hole evolution & cosmic feedback
Large scale structure
Angular Resolution 10 arc sec HPD (0.1-7 keV)
(goal of 5 arcsec)
Large scale sturcture
Cosmic feedback
Black hole evolution
Count Rate (WFI) 1 Crab with >90% throughput (tbc)
ΔE < 200eV @ 6keV (0.3-10 keV)
Strong gravity
Astrometry 1.5 arcsec at 3σ confidence (tbc) Black hole evolution
Absolute timing 100 µsec Neutron star studies

All information taken from : SciRD_table_29April2011.pdf , prepared by D. Lumb (ESA)

Effective area curves:

Total effective area for the two Athena telescopes combined

Effective area for the XMS calorimeter compared to that of ASTRO-H. In addition to a much larger effective area the Athena XMS has better energy resolution, and 5-10" HEW PSF, compared to 1.5' for the ASTRO-H SXS calorimeter.

Effective area for the Athena Wide Field Imager compared to the XMM-Newton EPIC pn. The Athena WFI also delivers a sharper PSF (5-10" vs 15'), better energy resolution and high count-rate capability.

Vignetting Curve :

A simple vignetting curve for the telescope has been calculated for a radially symmetric version of the telescope design. A more accurate ray tracing for the Owl configuration is required to demonstrate the vignetting accounting for asymmetric effects, expected to introduce a ~10% modulation with azimuth, especially at low energies.

Estimate of vignetting function of the telescope, and estimate of energy dependence. At the extreme corners of the Wide Field Imager the effective area would reduce to ~80% of the on-axis value

Athena Spectroscopy Figure of Merit

© Hochenergiegruppe des MPE
letzte Änderung: 24-Apr-2011, durch Thomas Boller and Joachim Paul

up © Max-Planck-Institut für extraterrestrische Physik