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Summary of SPEX models
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Under construction!

A complete list of models can be found in [to be completed]. This file is a
summary of which models are present, with comments on those most likely to 
be used by members of this group.

Model		usage

pow		Power law: the normalisation is in 1E44 ph/s/keV at 1keV.
		To convert from xspec normalisation to spex normalisation,
		use the following formula:
		
		n_s = ((n_x)*4*Pi*(d)^2)/1E44
		
		where:	n_s = spex norm
			n_x = xspec norm
			d = distance to source in cm
			
delt		delta function: normalisation is in units of 1E44 photons/s

gaus		gaussian: normalisation is in units of 1E44 photons/s

bb		blackbody

mbb		modified black body

cie		collisional ionisation equilibrium

neij		non-equilibrium ionisation

sed		SNR model

chev		SNR model

ham		SNR model

soli		SNR model

band		SNR model

pdem		stellar?

cf		cooling flow

dem		differential emission measure analysis

clus		cluster

reds		redshift

vgau		?

vblo 		?

vpro		?

lpro		scaling factor?

absm		cold galactic absorption: equivalent to wabs in xspec. 
		The hydrogen column is in 1E28/m^2 = 1E24/cm^2
		
euve		EUV absorption?

hot		absorption by a hot cie (collisional ionisation equilibrium)
		medium

slab		warm absorber model: applies photoionised absorption by a slab of hot gas to 
		the spectral continuum. The columns of individual ions are specified separately. 

knak		?

laor		general relativistic broadening: this is multiplicative, and
		can be applied to any appropriate component (e.g. delta 
		function, gaussian, or even the whole spectrum, although this 
		increases computation time)

xabs		warm absorber model: applies absorption by a given column of photoionised gas 
		at a given set of elemental abundances and a given ionisation parameter to the 
		continuum.

refl		reflection model.