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HELP on Simulator

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The BeppoSAX SDC Simulator

• Inclusion of up to 10,000 pointlike sources, each one with its own spectrum.
• inclusion of up to 100 extended sources with brightness distribution following King's profile:
  

  if dist < Cluster_extent

  intensity=surf_brightness*(1.0+dist/core)**(-3.*beta+0.50)

  
  else

  intensity=surf_brightness*(1.0+dist/core)**(-3.*beta+0.50)*exp(-dist/Cluster_extent)

  (dist is the distance from the cluster center)

  XSPEC routines are used for spectral distributions.

  Each source is characterized by a spectral model that can be specified by the user using XSPEC-like syntax.

  The PSF is a function of both position and energy (three psf's are used at different off-axis angles and at three different energy ranges, 9 psf's altogether).

  Vignetting effect applied to all sources and to the cosmic background.

  Output of events files is in fits/ogip format that can be easily analyzed with all major X-ray packages.

The method

Source positions, fluxes and specral shapes

SINGLE TARGET PLUS RANDOM SKY. - The target flux and spectral parameters are input via the WEB from. The random sky is then generated using a LogN-LogS . The sources' spectrum is chosen randomly from a set of predefined spectra. Currently the following spectra and parameters are used
wabs powerlaw 3.E20 1.7 (50% of the sources)
wabs powerlaw 3.E22 2.0 (20% of the sources)
wabs powerlaw 3.E23 2.0 (20% of the sources)
wabs powerlaw 3.E24 2.0 (10% of the sources)

ROSAT FIELD specified by the user by giving a target name or a position in the sky. The position of the sources in the field is taken from a catalog of Rosat sources and the spectrum is fixed to a power law with energy index 0.9 with NH equal to the Galactic value estimated from 21 cm radio data. If the user chooses the WGACAT catalog the spectral shape of the sources is a broken power law where the soft spectral slope is derived from the Rosat hardness ratio (if the slope error is less than 0.5) and the energy slope above 2.5 keV is fixed to 0.9. The random sky from the LogN-LogS is still generated but it is limited to fluxes lower than the faintest source in the rosat field.
LIST OF SOURCE POSITION provided by the user. The list must be in the form of a file for pointlike sources and a file for extended sources . The two files must be submitted through the WEB interface. NOTE that the center of the simulated field is set equal to the coordinates of the FIRST source in the POINTLIKE file list. If you wish to send a list for extended sources only take into account that the image center will be ra=0.0 dec=0.0 unless you are also requesting a ROSAT field centered somewhere.

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The LogN-LogS used to simulate random sources

Currently the LOGN-LogS used to generate random sources is a broken power law with slope at bright fluxes that is based on the ASCA results of Cagnoni et al. 1997 (alpha =1.63) and with a slope at fluxes fainter than 5.e-14 (cgs, 2-10keV) set equal to 1.3. This is consistent with the ASCA results of Georgantopulous et al. 1997 and with the BeppoSAX deep surveys (Giommi et al. 1997).

BeppoSAX LECS -- Calibration files

Field size : 160 (8arcsec) pixels, radius
Response matrix /dat1/calib/lecs/lecs.rmf, /dat1/calib/lecs/lecs_99.arf
Spectral shape and parameters of LogN-LogS sources
wabs powerlaw 3.E20 1.7 (50% of the sources)
wabs powerlaw 3.E22 2.0 (20% of the sources)
wabs powerlaw 3.E23 2.0 (20% of the sources)
wabs powerlaw 3.E24 2.0 (10% of the sources)
Further details can be found in the parameter file (if you are an expert)

BeppoSAX MECS (three units) -- Calibration files

Field size : 200 (8 arcsec) pixels, radius
Response matrix /dat1/calib/mecs/mecs.rmf, /dat1/calib/mecs/mecs_99.arf
Spectral shape and parameters of LogN-LogS sources
wabs powerlaw 3.E20 1.7 (50% of the sources)
wabs powerlaw 3.E22 2.0 (20% of the sources)
wabs powerlaw 3.E23 2.0 (20% of the sources)
wabs powerlaw 3.E24 2.0 (10% of the sources)

Further details can be found in the parameter file (if you are an expert)

BeppoSAX MECS (two units) -- Calibration files

Field size : 200 (8 arcsec) pixels, radius
Response matrix /dat1/calib/mecs23/mecs23.rmf, /dat1/calib/mecs23/mecs23_99.arf
Spectral shape and parameters of LogN-LogS sources
wabs powerlaw 3.E20 1.7 (50% of the sources)
wabs powerlaw 3.E22 2.0 (20% of the sources)
wabs powerlaw 3.E23 2.0 (20% of the sources)
wabs powerlaw 3.E24 2.0 (10% of the sources)

Further details can be found in the parameter file (if you are an expert)

Jet-X CCD -- Calibration files

Field size : 430x320 (4 arcsec) pixels
Response matrix /dat1/calib/jetx/rmf4.rsp
Spectral shape and parameters of LogN-LogS sources
wabs powerlaw 3.E20 1.7 (50% of the sources)
wabs powerlaw 3.E22 2.0 (20% of the sources)
wabs powerlaw 3.E23 2.0 (20% of the sources)
wabs powerlaw 3.E24 2.0 (10% of the sources)

Further details can be found in the parameter file (if you are an expert)

XMM EPIC -- Calibration files

Field size : 400x400 (4 arcsec) pixels
Response matrix /dat1/calib/xmm/epic.rmf, /dat1/calib/xmm/epic_mos00.arf
Spectral shape and parameters of LogN-LogS sources
wabs powerlaw 3.E20 1.7 (50% of the sources)
wabs powerlaw 3.E22 2.0 (20% of the sources)
wabs powerlaw 3.E23 2.0 (20% of the sources)
wabs powerlaw 3.E24 2.0 (10% of the sources)

Further details can be found in the parameter file (if you are an expert)

AXAF ACIS -- Calibration files

Field size : 512x512 (1 arcsec) pixels
Response matrix /dat1/calib/axaf/acis1.rsp
Spectral shape and parameters of LogN-LogS sources
wabs powerlaw 3.E20 1.7 (50% of the sources)
wabs powerlaw 3.E22 2.0 (20% of the sources)
wabs powerlaw 3.E23 2.0 (20% of the sources)
wabs powerlaw 3.E24 2.0 (10% of the sources)

Further details can be found in the parameter file (if you are an expert)

Future improvements