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Sample Sessions
- Example 1. Estimating ASCA SIS count rates
- Example 2. Estimating XTE count rates I
- Example 3. Estimating XTE count rates II
- Example 4. Estimating ROSAT PSPC count rates
In this section, examples using PIMMS version 3.0 are shown to illustrate the general feel of PIMMS sessions.
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.
This file was last modified on Tuesday, 13-Sep-2005 16:04:36 EDT
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
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 (+1%)
E (keV) (cps) (cps) detection (s)
0- 13 0.00- 6.14 0.612 10.56 746.858 ( 2934.732)
14- 17 6.14- 7.90 0.018 3.46 2.80E+05 (*********)
18- 23 7.90- 10.5 7.81E-04 4.56 1.87E+08 (*********)
24- 35 10.5- 15.8 5.09E-10 7.87 7.60E+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 0.420 cps from the source plus 60.920 background cps
5-sigma detection will be achieved in 8.70E+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 1120.287 ( 4402.101)
14- 17 6.14- 7.90 0.012 2.31 4.20E+05 (*********)
18- 23 7.90- 10.5 5.21E-04 3.04 2.80E+08 (*********)
24- 35 10.5- 15.8 3.39E-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 > model rs 1 1e20
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 = 1.000E+20
and 1.000E+00 cps in EXOSAT ME
(Model normalization = 2.201E-02)
* PIMMS predicts 2.104E-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 0.631 cps from the source plus 91.380 background cps
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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