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Previous: Introduction


Previous: Introduction


Sample Sessions



In this section, examples using PIMMS version 3.0 are shown to illustrate the general feel of PIMMS sessions.

Example 1. Estimating ASCA SIS count rates

*** PIMMS version 3.0 ***
    2000 April 28 release
    (this version does not simulate images)
    Reading mission directory, please wait
* Current model is BREMSSTRAHLUNG, kT=  10.0000 keV; NH =  1.000E+21
   <--- Use 'MODEL' command to change
* By default, input rate is taken to be
 Flux (    2.000-   10.000 keV) in ergs/cm/cm/s
   <--- Use 'FROM' command to change the default
* Simulation product will be
 Count rate in ASCA SIS
   <--- Use 'INSTRUMENT' command to switch to another instrument
PIMMS > go 1 einstein ipc
* For thermal Bremsstrahlung model with kT= 10.0000 keV; NH =  1.000E+21
  and  1.000E+00 cps in EINSTEIN IPC
  (Model normalization =  5.882E-03)
* PIMMS predicts  1.516E+00 cps with ASCA SIS
    [Count rate per single SIS, not per pair, over an entire chip assuming
    a point source at the 1-CCD mode position; within the maximum circular
    extraction region that fits on the default chip, usable rates are
          1.3 (3.2 arcmin radius, SIS-0) and       1.0 (2.5 arcmin, SIS-1)]
* An exposure of      17.42s is required for a 5-sigma detection using optimal
  extraction radius of 5.67 arcmin ( 1.49E+00 src and  6.10E-02 bgd cps)

* Extrapolated to 1998 Dec for S1C3 in 1-CCD mode at 2 SIS temperatures:

  Telemetry is 85.6% full, 10.7% full, 21.4% full, and  2.7% full (nominal)
  Telemetry is  saturated, 12.8% full, 25.7% full, and  3.2% full (warm)
         in    Faint  (M), Faint  (H), Bright (M), and Bright (H) modes
    (S0C1 has lower flickering pixel rate; decide modes based on S1C3)
PIMMS > quit

In this example, the default spectral model is used to estimate the ASCA SIS count rate (which happens to be the default). The only place where user did not use the default set-up was to specify conversion from Einstein IPC count rate. PIMMS not only reports the total SIS count rate but also count rates in the typical extraction regions for SIS-0 and SIS-1, and information on telemetry saturation and recommendations on suitable data modes.

Example 2. Estimating XTE count rates I

*** PIMMS version 3.0 ***
    2000 April 28 release
    (this version does not simulate images)
    Reading mission directory, please wait
* Current model is BREMSSTRAHLUNG, kT=  10.0000 keV; NH =  1.000E+21
   <--- Use 'MODEL' command to change
* By default, input rate is taken to be
 Flux (    2.000-   10.000 keV) in ergs/cm/cm/s
   <--- Use 'FROM' command to change the default
* Simulation product will be
 Count rate in ASCA SIS
   <--- Use 'INSTRUMENT' command to switch to another instrument
PIMMS > from exosat me
PIMMS > inst xte pca
PIMMS > mo rs 1 5e19
WARNING - this version of PIMMS has a grid of  59 Raymond-Smith plasma models
      from log T of  5.60; kT =  0.034
        to log T of  8.50; kT = 27.250
          choosing the nearest one, hope that's okay
         New temperature is  0.967 keV (log T is  7.05)
PIMMS > go 1
* For Raymond Smith model with kT= 0.9669 keV (logT= 7.05); NH =  5.000E+19
  and  1.000E+00 cps in EXOSAT ME
  (Model normalization =  2.196E-02)
* PIMMS predicts  2.100E-01 cps with XTE PCA
ERROR:: non-overlapping energy ranges of model and calibration
ERROR:: non-overlapping energy ranges of model and calibration
   (Count rate is per PCU)

%%%        With 3 PCUs operational:
           (Use these numbers in RPS)

PIMMS predicts     0.630 cps from the source plus    91.380 background cps
5-sigma detection will be achieved in 5.80E+03s
(but undetectable with 1% systematic uncertainties in bgd)

Results in the 6 canonical XTE PCA bands are:

Channels  Nominal    Source   BGD   5-sigma    detection will be achieved in 5.78E+03s
(but undetectable with 1% systematic uncertainties in bgd)

Results in the 6 canonical XTE PCA bands are:

Channels  Nominal    Source   BGD   5-sigma    (+1%)
          E (keV)    (cps)    (cps) detection (s)
  0- 13  0.00- 6.14     0.613 10.56  744.286 ( 2894.601)
 14- 17  6.14- 7.90     0.018  3.46 2.78E+05 (*********)
 18- 23  7.90- 10.5  7.83E-04  4.56 1.86E+08 (*********)
 24- 35  10.5- 15.8  5.10E-10  7.87 7.57E+20 (*********)
 36- 49  15.8- 22.1  0.00E+00  8.90 ******** (*********)
 50-249  22.1-116.0  0.00E+00 56.05 ******** (*********)

%%% ...and with 2 PCUs operational:

PIMMS predicts     0.421 cps from the source plus    60.920 background cps
5-sigma detection will be achieved in 8.66E+03s
(but undetectable with 1% systematic uncertainties in bgd)

Results in the 6 canonical XTE PCA bands are:

Channels  Nominal    Source   BGD   5-sigma    (+1%)
          E (keV)    (cps)    (cps) detection (s)
  0- 13  0.00- 6.14     0.408  7.04 1116.429 ( 4341.900)
 14- 17  6.14- 7.90     0.012  2.31 4.18E+05 (*********)
 18- 23  7.90- 10.5  5.22E-04  3.04 2.79E+08 (*********)
 24- 35  10.5- 15.8  3.40E-10  5.24 1.14E+21 (*********)
 36- 49  15.8- 22.1  0.00E+00  5.93 ******** (*********)
 50-249  22.1-116.0  0.00E+00 37.37 ******** (*********)
PIMMS > quit
In this example, the user specified conversion from EXOSAT ME count rate to XTE PCA and used Raymond-Smith models with two different columns. Since PIMMS has a limited grid of Raymond-Smith models, the temperature of the actual model used does not exactly match the request. In addition, Raymond-Smith models are not calculated up to very high energies (where the flux tends to be low) so error messages are displayed to that effect. As with ASCA, PIMMS provides instrument-specific information for the XTE PCA (source and background count rates, and 5-sigma detection times in the entire passband and in the 6 canonical PCA bands with 2 or 3 PCUs operational).

Example 3. Estimating XTE count rates II

*** PIMMS version 3.0 ***
    2000 April 28 release
    (this version does not simulate images)
    Reading mission directory, please wait
* Current model is BREMSSTRAHLUNG, kT=  10.0000 keV; NH =  1.000E+21
   <--- Use 'MODEL' command to change
* By default, input rate is taken to be
 Flux (    2.000-   10.000 keV) in ergs/cm/cm/s
   <--- Use 'FROM' command to change the default
* Simulation product will be
 Count rate in ASCA SIS
   <--- Use 'INSTRUMENT' command to switch to another instrument
PIMMS > from ginga lac both
PIMMS > mo pl 1.5 15 30 1e22
Value of Nh is rather small ---
Assuming that log10(Nh) was given
Warning:: Ignoring extra numerical parameter(s)
PIMMS > inst xte pca
PIMMS > go 500
* For power law model with photon index = 1.5000; NH =  1.000E+15
  and  5.000E+02 cps in GINGA LAC BOTH
  (Model normalization =  1.805E-01)
* PIMMS predicts  1.226E+02 cps with XTE PCA
   (Count rate is per PCU)

%%%        With 3 PCUs operational:
           (Use these numbers in RPS)

PIMMS predicts   367.907 cps from the source plus    91.380 background cps
5-sigma detection will be achieved in    0.085s
(or in    0.085s with 1% systematic uncertainties in bgd)

Results in the 6 canonical XTE PCA bands are:

Channels  Nominal    Source   BGD   5-sigma    (+1%)
          E (keV)    (cps)    (cps) detection (s)
  0- 13  0.00- 6.14   144.709 10.56    0.185 (    0.185)
 14- 17  6.14- 7.90    50.814  3.46    0.526 (    0.526)
 18- 23  7.90- 10.5    58.519  4.56    0.461 (    0.461)
 24- 35  10.5- 15.8    64.826  7.87    0.432 (    0.432)
 36- 49  15.8- 22.1    28.216  8.90    1.165 (    1.166)
 50-249  22.1-116.0    20.823 56.05    4.432 (    4.514)

%%% ...and with 2 PCUs operational:

PIMMS predicts   245.271 cps from the source plus    60.920 background cps
5-sigma detection will be achieved in    0.127s
(or in    0.127s with 1% systematic uncertainties in bgd)

Results in the 6 canonical XTE PCA bands are:

Channels  Nominal    Source   BGD   5-sigma    (+1%)
          E (keV)    (cps)    (cps) detection (s)
  0- 13  0.00- 6.14    96.473  7.04    0.278 (    0.278)
 14- 17  6.14- 7.90    33.876  2.31    0.788 (    0.788)
 18- 23  7.90- 10.5    39.012  3.04    0.691 (    0.691)
 24- 35  10.5- 15.8    43.217  5.24    0.649 (    0.649)
 36- 49  15.8- 22.1    18.810  5.93    1.748 (    1.749)
 50-249  22.1-116.0    13.882 37.37    6.649 (    6.771)
PIMMS > inst xte hexte def
PIMMS > go 500
* For power law model with photon index = 1.5000; NH =  1.000E+15
  and  5.000E+02 cps in GINGA LAC BOTH
  (Model normalization =  1.805E-01)
* PIMMS predicts  3.038E+01 cps with XTE HEXTE DEFAULT
   (Source-only count rate in 1 cluster; BGD rate is 73.1 per cluster)
5-sigma detection will be achieved in      5.4s

Results in the 4 canonical XTE HEXTE bands are:
             (per HEXTE cluster)

  Channels Nominal   Source   BGD   5-sigma
           E (keV)   (cps)    (cps) detection (s)
    5- 29   12-  30    15.2   11.86      4.7
   30- 61   30-  62     8.2   17.93     18.5
   62-125   62- 126     5.6   21.94     45.2
  126-250  126- 250     1.4   21.35    650.8
 (The default 16-s rocking cycle is assumed for detection time)
PIMMS > quit
In this case, a special version of the power law model (with high energy cut-off) is used, by specifying index, cut-off energy and e-folding energy, as well as NH, on the command line. User then calculated PCA and HEXTE count rates for a 500 cps Ginga LAC source.

Example 4. Estimating ROSAT PSPC count rates

*** PIMMS version 3.0 ***
    2000 April 28 release
    (this version does not simulate images)
    Reading mission directory, please wait
* Current model is BREMSSTRAHLUNG, kT=  10.0000 keV; NH =  1.000E+21
   <--- Use 'MODEL' command to change
* By default, input rate is taken to be
 Flux (    2.000-   10.000 keV) in ergs/cm/cm/s 
   <--- Use 'FROM' command to change the default
* Simulation product will be
 Count rate in ASCA SIS
   <--- Use 'INSTRUMENT' command to switch to another instrument
PIMMS > from flux ergs 0.1-4
PIMMS > mo rs06_665 3e19
PIMMS > inst rosat pspc open
PIMMS > go 5e-12
* For model rs06_665; NH =  3.000E+19
   and a flux (  0.100-  4.000keV) of  5.000E-12 ergs/cm/cm/s
  (Model normalization =  1.893E-03)
* PIMMS predicts  6.594E-01 cps with ROSAT PSPC OPEN
PIMMS > inst rosat pspc r6r7
PIMMS > go 5e-12
* For model rs06_665; NH =  3.000E+19
   and a flux (  0.100-  4.000keV) of  5.000E-12 ergs/cm/cm/s
  (Model normalization =  1.893E-03)
* PIMMS predicts  1.330E-01 cps with ROSAT PSPC R6R7
PIMMS > quit
In this example, 0.6 Solar abundance, logT=6.65 Raymond-Smith model with an absorption of 3x1019 cm-2 is used to estimate ROSAT PSPC count rates (total and in 3 combinations of the Snowden R bands) for a 5x10-12 ergs cm-2s-1 source.



Next: Using Multi-component Models

 
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