WFXRT vs' eROSITA

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 zgt4 (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 z1.5
• clusters out to z4 (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-gt 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-gt 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