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This model calculates the transmission of the interstellar medium using the
description of the ISM absorption of Rumph, Bowyer, & Vennes 1994, AJ 107,
2108. It includes neutral He autoionization features.
Between 1.2398 and 43.655 Angstroms (i.e. in the 0.28-10 keV range) the model also
accounts for metals as described in Morrison & MacCammon 1983, ApJ 270,
119.
The code uses the best available photoionization cross-sections to date
from the atomic data literature and combines them in an arbitrary mixture of
the three ionic species: HI, HeI, and HeII.
The model assumes that the data are expressed in Angstroms.
This model provided courtesy of Pat Jelinsky.
atten Parameters
| 1 |
hcol |
N(HI) column (atoms cm^-2) |
| 2 |
heiRatio |
N(HeI)/N(HI) |
| 3 |
heiiRatio |
N(HeII)/N(HI) |
- py.sherpa
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bbody,
bbodyfreq,
beta1d,
beta2d,
box1d,
box2d,
bpl1d,
const1d,
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poisson,
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powlaw1d,
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schechter,
sin,
sqrt,
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steplo1d,
tablemodel,
tan,
xs,
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xsapec,
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xsbexrav,
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xsbkn2pow,
xsbknpower,
xsbmc,
xsbremss,
xsbvapec,
xsc6mekl,
xsc6pmekl,
xsc6pvmkl,
xsc6vmekl,
xscabs,
xscemekl,
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xscflow,
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xscompls,
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xscompst,
xscomptt,
xsconstant,
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xscyclabs,
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xslaor,
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xsvnei,
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xsvraymond,
xsvsedov,
xswabs,
xswndabs,
xsxion,
xszbbody,
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xszpcfabs,
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xszpowerlw,
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xszsmdust,
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xszvarabs,
xszvfeabs,
xszvphabs,
xszwabs,
xszwndabs
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