Diffuse Hot Gas in Galaxy Clusters at High Spatial and Spectral Resolution
Abstract
Power spectra of density fluctua4ons can be measured down to few ”.
Velocity spectrum can be measured down to scales ~3 4mes larger
Marginally resolved mean free path (in veloci4es).
Signs of the spectrum steepening should be present at scales larger than m.f.p.
Depends on the calibration of gain (of pixels) and uniformity of QE.
The mass of the cold gas (at any T, even if it not visible) can be measured
via fluorescent iron line at 6.4 keV.
- Publication:
-
X-Ray Vision Workshop: Probing the Universe in Depth and Detail with the X-Ray Surveyor
- Pub Date:
- October 2015
- DOI:
- 10.5281/zenodo.47424
- Bibcode:
- 2015xrvw.confE..16C
- Keywords:
-
- Galaxy clusters;
- Zenodo community xrayvision