Example 2. Partial covering absorber
*** PIMMS version 4.0 ***
2010 Feb 17th Release
Reading mission directory, please wait
* Current model is BREMSSTRAHLUNG, kT= 10.0000 keV; NH = 1.000E+21
<--- Use 'MODEL' command to change
and 'PLASMA' command to switch among APEC/mekal/RS
* 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 CHANDRA ACIS-I
<--- Use 'INSTRUMENT' command to switch to another instrument
PIMMS > mo brems 15 3e23 brems 15 1e20 0.1 10 ga 6.5 0.1 250
PIMMS > output partial 0.1 10.0 0.005
PIMMS > inst xmm pn thin
PIMMS > go 0.5 asca sis
* For thermal Bremsstrahlung model with kT= 15.0000 keV; NH = 3.000E+23
+ thermal Bremsstrahlung model with kT= 15.0000 keV; NH = 1.000E+20
( 0.1000 times component 1 at 10.0000 keV)
+ Gaussian model with E= 6.5000 keV; sigma= 0.1000 keV; NH = 3.000E+23
(Eq.W=250.0000 eV)
and 5.000E-01 cps in ASCA SIS
%!% Integration over the entire chip (not just in the source region) assumed
(Internal model normalization = 1.122E-02)
* PIMMS predicts 3.576E+00 cps with XMM PN THIN
for on-axis observation before dead time correction,
PATTERN=0 only rate assuming a 15 arcsec extraction radius
(the total PATTERN=0 count rate is approx. 47% higher)
WARNING: The pile-up estimate is approximate
% Pile-up and dead-time corrected count rates in 4 energy bands
using various window options are:
Window Pileup Dead Corrected Good Count Rates
Option frac. Time 0.1-0.4 0.4-1.0 1.0-2.5 2.5-10.0 Total
Full 0.939% 7.0% 0.4934 0.6910 0.6684 1.2785 3.2941
FullExtd 4.495% 2.0% 0.5013 0.7020 0.6791 1.2989 3.3466
Large 0.540% 9.0% 0.4848 0.6789 0.6567 1.2561 3.2363
Small 0.017% 29.0% 0.3802 0.5324 0.5150 0.9852 2.5383
Timing ------- 1.5% 0.5276 0.7388 0.7146 1.3670 3.5220
Burst ------- 97.0% 0.0161 0.0225 0.0218 0.0416 0.1073
% Any pile-up predictions over 10% are highly uncertain
PIMMS> quit
This example shows how to set up a spectrum suffering from partial
covering absorption. In addition, a Gaussian is added which has
a different syntax: the three parameters are the line energy (keV),
the physical width (keV), and the equivalent width (eV). Absorbing
column is assumed to be the same as the first component (it can
be specified explicitly, as the third parameter before the equivalent
width).
Example 3. A redshifte example
*** PIMMS version 4.0 ***
2010 Feb 17th Release
Reading mission directory, please wait
* Current model is BREMSSTRAHLUNG, kT= 10.0000 keV; NH = 1.000E+21
<--- Use 'MODEL' command to change
and 'PLASMA' command to switch among APEC/mekal/RS
* 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 CHANDRA ACIS-I
<--- Use 'INSTRUMENT' command to switch to another instrument
PIMMS > mo pl 1.7 3e23 ga 6.4 0.2 150 plasma 1.2 1.0 0.0 1.0 2.5 z 0.01 8e19
NOTE: This version of PIMMS has a grid of 59x 5 grid of APEC models
from kT= 0.034 keV (logT= 5.60) to kT=27.250 keV (logT= 8.50)
and abundances from 0.20 to 1.00
Selected temperature is 1.217 keV (log T is 7.15)
and selected abundance is 1.0
PIMMS > output agn_sb 0.1 10.0 0.01
PIMMS > inst chandra acis-s
PIMMS > go 1e-11
* For power law model with photon index = 1.7000; NH = 3.000E+23
+ Gaussian model with E= 6.4000 keV; sigma= 0.2000 keV; NH = 3.000E+23
(Eq.W=150.0000 eV)
+ PLASMA (APEC) model with
kT= 1.2172keV (logT= 7.15), Abund=1.0; NH = 0.000E+00
( 1.0000 times component 1 at 2.5000 keV)
...redshifted with z= 0.0100 and a Galactic Nh= 8.000E+19
and a flux ( 2.000- 10.000keV) of 1.000E-11 ergs/cm/cm/s
(Internal model normalization = 7.355E-03)
* PIMMS predicts 1.711E-01 cps with CHANDRA ACIS-S
% Pileup estimate for ACIS:
Pile-up is tolerable (10.0 %) at a frame-time of 1.546 s
PIMMS > quit
In this example, the entire composite model is to be redshifted with z=0.01.
Absorption specified with each component is taken to be intrinsic (i.e.,
also redshifted). Additionally, a Galactic (unredshifted) absorption is
specified. For "unabsorbed" flux, both intrinsic and Galactic absorption
will temporarily be set to 0.
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