SPEX User's Manual - SRON

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50 Spectral Models acronym pow delt gaus bb mbb dbb cie neij sed chev soli band pdem cf wdem dem refl file reds vgau vblo vpro lpro laor absm euve hot slab xabs warm knak Table 3.1: Available spectral components description additive components: Power law Delta line Gaussian line Blackbody Modified blackbody Accretion disk blackbody Collisional ionisation equilibrium spectrum Non-equilibrium ionisation spectrum Sedov adiabatic SNR model Chevalier adiabatic SNR model with reverse shock Solinger isothermal SNR model Band isothermal SNR model with reverse shock Differential emission measure model, polynomials Isobaric cooling flow model Power law differential emission measure with high T cut-off Differential emission measure model, for DEM analysis Reflection model of Zycki Table model from file multiplicative components, shifts: Redshift model multiplicative components, convolutions: Gaussian velocity profile Square velocity profile Arbitrary velocity profile (needs input file) Spatial profile modeling for RGS (needs input file) Laor relativistic line profile multiplicative components, absorption/transmission: Morrison & McCammon ISM absorption EUVE absorption model Rumph et al. (H+He) SPEX absorption by plasma in CIE absorption by a slab with adjustable ionic columns absorption by a slab in photoionization equilibrium absorption by a slab with continuous distribution in ionization transmission piecewise power law where now E is the photon energy in keV, T the temperature in keV and e is the elementary charge in Coulomb. Inserting numerical values and multiplying by the emitting area A, we get N(E) = 9.883280 × 10 7 E 2 A/(e E/T − 1) (3.3) where N(E) is the photon spectrum in units of 10 44 photons/s/keV and A the emitting area in 10 16 m 2 . The parameters of the model are: norm - Normalisation A (the emitting area, in units of 10 16 m 2 . Default value: 1. t - The temperature T in keV. Default value: 1 keV.
3.4 Cf: isobaric cooling flow differential emission measure model 51 3.4 Cf: isobaric cooling flow differential emission measure model This model calculates the spectrum of a standard isobaric cooling flow. The differential emission measure distribution dY (T)/dT for the isobaric cooling flow model can be written as D(T) ≡ dY (T)/dT = 5Ṁk 2µm H Λ(T), (3.4) where Ṁ is the mass deposition rate, k is Boltzmann’s constant, µ the mean molecular weight (0.618 for a plasma with 0.5 times solar abundances), m H is the mass of a hydrogen atom, and Λ(T) is the cooling function. We have calculated the cooling function Λ using our own SPEX code for a grid of temperatures and for 0.5 times solar abundances. The spectrum is evaluated by integrating the above differential emission measure distribution between a lower temperature boundary T 1 and a high temperature boundary T n . We do this by creating a temperature grid with n bins and calculating the spectrum for each temperature. Warning: Take care that n is not too small in case the relevant temperature is large; on the other hand if n is large, the computational time increases. Usually a spacing with temperature differences between adjacent bins of 0.1 (in log) is sufficient and optimal. Warning: The physical relevance of this model is a matter of debate The parameters of the model are: norm - The mass deposition rate Ṁ in M ⊙ yr −1 t1 - Lower temperature cut-off temperature T 1 . Default: 0.1 keV. tn - Upper temperature cut-off temperature T n . Default: 1 keV. nr - Number of temperature bins n used in the integration. Default value: 16 p - Slope p = 1/α. Default: 0.25 (α = 4). cut - Lower temperature cut-off, in units of T max . Default value: 0.1. The following parameters are the same as for the cie-model: ed - Electron density in 10 20 m −3 it - Ion temperature in keV vmic - Micro turbulent velocity in km/s ref - Reference element 01. . .30 - Abundances of H to Zn file - Filename for the nonthermal electron distribution 3.5 Cie: collisional ionisation equilibrium model This model calculates the spectrum of a plasma in collisional ionisation equilibrium (CIE). It consists essentially of two steps, first a calculation of the ionisation balance and then the calculation of the X-ray spectrum. The basis for this model is formed by the mekal model, but several updates have been included. 3.5.1 Temperatures Some remarks should be made about the temperatures. SPEX knows three temperatures that are used for this model. First there is the electron temperature T e . This is usually referrred to as ”the” temperature of the plasma. It determines the continuum shape and line emissivities and the resulting spectrum is most sensitive to this. Secondly, there is the ion temperature T i . This is only important for determining the line broadening, since this depends upon the thermal velocity of the ions (which is determined both by T i and the atomic mass of the ion). Only in high resolution spectra the effects of the ion temperature can be seen.
Page 1: SPEX User’s Manual Jelle Kaastra
Page 4 and 5: 4 CONTENTS 2.29 System . . . . . .
Page 6 and 7: 6 CONTENTS 5.8.3 ASCA SIS0 . . . .
Page 8 and 9: 8 Introduction 1.2.2 Sky sectors Fi
Page 10 and 11: 10 Introduction
Page 12 and 13: 12 Syntax overview Table 2.2: Abund
Page 14 and 15: 14 Syntax overview tcl: the continu
Page 16 and 17: 16 Syntax overview Examples calc -
Page 18 and 19: 18 Syntax overview by averaging the
Page 20 and 21: 20 Syntax overview dem gene #i1 #i2
Page 22 and 23: 22 Syntax overview distance om #r -
Page 24 and 25: 24 Syntax overview Examples elim 0.
Page 26 and 27: 26 Syntax overview This is strictly
Page 28 and 29: 28 Syntax overview Currently these
Page 30 and 31: 30 Syntax overview Syntax The follo
Page 32 and 33: 32 Syntax overview status, range an
Page 34 and 35: 34 Syntax overview par write mypar
Page 36 and 37: 36 Syntax overview plot box col #i
Page 38 and 39: 38 Syntax overview plot type data -
Page 40 and 41: 40 Syntax overview 2.26 Simulate: S
Page 42 and 43: 42 Syntax overview step axis 2 par
Page 44 and 45: 44 Syntax overview Examples use 100
Page 46 and 47: 46 Syntax overview width. On top of
Page 48 and 49: 48 Syntax overview
Page 52 and 53: 52 Spectral Models Finally, we have
Page 54 and 55: 54 Spectral Models where Q is the l
Page 56 and 57: 56 Spectral Models 3. set=3: for R
Page 58 and 59: 58 Spectral Models 3.14 Hot: collis
Page 60 and 61: 60 Spectral Models can be transform
Page 62 and 63: 62 Spectral Models The emission mea
Page 64 and 65: 64 Spectral Models 3.23 Refl: Refle
Page 66 and 67: 66 Spectral Models • type=3: b 1
Page 68 and 69: 68 Spectral Models 4.8, 4.9, 5.0 wi
Page 70 and 71: 70 More about plotting Table 4.1: A
Page 72 and 73: 72 More about plotting 4.4 Plot lin
Page 74 and 75: 74 More about plotting Table 4.2: A
Page 76 and 77: 76 More about plotting 4.6 Plot cap
Page 78 and 79: 78 More about plotting 4.8 Plot axi
Page 80 and 81: 80 More about plotting bin cou cs k
Page 82 and 83: 82 More about plotting
Page 84 and 85: 84 Response matrices models. Since
Page 86 and 87: 86 Response matrices Table 5.1: Wei
Page 88 and 89: 88 Response matrices Table 5.2: Sca
Page 90 and 91: 90 Response matrices since the larg
Page 92 and 93: 92 Response matrices Figure 5.1: Di
Page 94 and 95: 94 Response matrices for the Cauchy
Page 96 and 97: 96 Response matrices bin j of this
Page 98 and 99: 98 Response matrices The approximat
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100 Response matrices particular bi
Page 102 and 103:
102 Response matrices reduced by ab
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104 Response matrices where as befo
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106 Response matrices 5. Determine
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108 Response matrices practical pro
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110 Response matrices Table 5.10: T
Page 112 and 113:
112 Response matrices Table 5.11: F
Page 114 and 115:
114 Response matrices Figure 5.7: B
Page 116 and 117:
116 Response matrices Table 5.15: R
Page 118 and 119:
118 Response matrices
Page 120 and 121:
120 Installation and testing
Page 122 and 123:
122 Acknowledgements
Page 124 and 125:
124 BIBLIOGRAPHY [2003] Peterson, J
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