SPEX Reference manual (PDF) - SRON

2.10 Elim: set flux energy limits 23
width #r3. In case the difference between upper and lower energy is not a multiple of the bin width, the
upper boundary of the last bin will be taken as close as possible to the upper boundary (but cannot be
equal to it).
egrid log #r1 #r2 #i [#a] - Create a logarithmic energy grid between #r1 and #r2, in units given by
#a (as listed above). If no unit is given, it is assumed that the limits are in keV. The number of energy
bins is given by #i
egrid log #r1 #r2 step #r3 [#a] - as above, but do not prescribe the number of bins, but the bin
width (in log E) #r3.
egrid read #a - Read the energy grid from file #a.egr
egrid save #a - Save the current energy grid to file #a.egr
Warning: The lower limit of the energy grid must be positive, and the upper limit must always be larger
than the lower limit.
Examples
egrid lin 5 38 step 0.02 a - create a linear energy grid between 5−38 Å, with a step size of 0.02 Å.
egrid log 2 10 1000 - create a logarithmic energy grid with 1000 bins between 2−10 keV.
egrid log 2 10 1000 ev - create a logarithmic energy grid with 1000 bins between 0.002−0.010 keV.
egrid read mygrid - read the energy grid from the file mygrid.egr.
egrid save mygrid - save the current energy grid to file mygrid.egr.
2.10 Elim: set flux energy limits
Overview
SPEX offers the opportunity to calculate the model flux in a given energy interval for the current spectral
model. This information can be viewed when the model parameters are shown (see section 2.21).
For each additive component of the model, the following quantities are listed:
the observedphoton number flux (photonsm −2 s −1 ) at earth, including anyeffects of galacticabsorption
etc.
the observed energy flux (Wm −2 ) at earth, including any effects of galactic absorption etc.
the intrinsic numberof photonsemitted at the source, not diluted byany absorptionetc., in photonss −1 .
the intrinsic luminosity emitted at the source, not diluted by any absorption etc., in W.
The following units can be used to designate the energy or wavelength range: keV (the default), eV, Ryd,
J, Hz, Å, nm.
Syntax
The following syntax rules apply:
elim #r1 #r2 [#a] - Determine the flux between #r1 #r2, in units given by #a, and as listed above.
The default at startup is 2−10 keV. If no unit is given, it is assumed that the limits are in keV.
Warning: When new units or limits are chosen, the spectrum must be re-evaluated (e.g. by giving the
”calc” comand) in order to determine the new fluxes.
Warning: The lower limit must be positive, and the upper limit must always be larger than the lower
limit.