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WFXRT vs. eROSITA

WFXRT vs. eROSITA. PSF 4-5 arcsec vs 12-14 arcsec Ef.Area 1300 cm2 vs. 2000 cm2 Instr Bkg. Similar. Sensitivity to diffuse emission will be different. Because of different PSF,FOV and observing strategy. WFXRT out to Rvir eROSITA 0.5-0.6 Rvir. Deep Pointings.

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WFXRT vs. eROSITA

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  1. WFXRT vs. eROSITA • PSF 4-5 arcsec vs 12-14 arcsec • Ef.Area 1300 cm2 vs. 2000 cm2 • Instr Bkg. Similar. • Sensitivity to diffuse emission will be different. Because of different PSF,FOV and observing strategy. • WFXRT out to Rvir • eROSITA 0.5-0.6 Rvir

  2. Deep Pointings • 1 MS pointings will reach 1.e-16 cgs in 0.5-2.0 with WFXRT • Comparable to Chandra deep Surveys only on solid angle of 1 sq. deg. Rather than a few sq. arcmin · 1 wfxrt deep pointing Brandt & Hasinger 05

  3. Deep Pointings • 3000 objects per sq. deg. mostly absorbed AGN • About 100 or so above z>4 (distribution of absorption at high z) • X-ray clustering and its evolution. Brandt & Hasinger 05

  4. Deep Pointings • Depth for extended objects: • conservative estimate ~5.e-16 • groups out to z=1.5 • clusters out to z=4 (if there are any)

  5. Deep Pointings & Synergy • Deep Pointings offer the best synergy with TES • the reason is rather obvious: long expo time afford detection of faint lines. a) of the order of ~100 agn emission lines detected. Simultaneous WFXRT detection will allow precise spatial location of AGN. • b) 50-100 detection of group/cluster emission lines. A sizeable fraction of objects detected in WFXRT will also be seen • with TES for these we will get: • redshifit-> Lum • metal abundance • temperature if more than 1 detected (not unlikely)

  6. Deep Pointings & Synergy b) 50-100 detection of group/cluster emission lines. A sizeable fraction of objects detected in WFXRT will also be seen with TES for these we will get I) redshfit-> Lum II) metal abund. III) temperature if more than 1 detected (not unlikely)

  7. MicroCal Bkg. Dominated by emission from unresolved sources. Estimates used so far based on average bkg surface brightness.

  8. MicroCal Bkg. Distribution of total flux due to unresolved sources for a sample of 1.e4 microcal pixels. Distribution is highly asimmetric. Few pixels on which rare bright sources happen to fall contribute in significant way. Excluding these rare pixels will reduce substantially mean bkg.

  9. MicroCal Bkg. Excluding 1/3 of microcal pixels we can reduce bkg. by a factor of about 3. This will improve significantly sensitivity of microcal to diffuse emission extending on large regions of detector. For the brightest 10% pixels microcal data alone should be sufficient to identify and reject high flux pixels. To exlcude others independent estimate of flux from WFXRT where contributing sources are resolved will be important if not vital.

  10. MicroCal Bkg. This will improve significantly sensitivity of microcal to diffuse emission extending on large regions of detector. Typically noise will go down by sqrt(3).

  11. Cluster cores + Outer Reg Making direct velocity measurements of the cluster cores is of great importance to address ICM phsics issues: viscosity/turbulence Cooling/heating problem Subarcmin angular resolution very important. Good obs. Char. Of intermediate and outer regions will be of considerable value in assembling a complete picture

  12. EPIC obs of Perseus Surface Brightness Temperature Long 125 ks uninterrupted observation Not badly contaminated by SP flares After cleaning we have 100 ks for MOS1 100 for MOS2 and 9? for PN. Some 35 million Perseus photons

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