SPEX Reference manual (PDF) - SRON

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8 Introduction 1.2.2 Sky sectors First, the relevant part of the sky is subdivided into sectors, each sector corresponding to a particular region of the source, for example a circular annulus centered around the core of a cluster, or an arbitrarily shaped piece of a supernova remnant, etc. A sector may also be a point-like region on the sky. For example if there is a bright point source superimposed upon the diffuse emission of the cluster, we can define two sectors: an extended sector for the cluster emission, and a point-like sector for the point source. Both sectors might even overlap, as this example shows! Another example: the two nearby components of the close binary α Centauri observed with the XMM -Newton instruments, with overlapping point-spread-functions of both components. In that case we would have two point-like sky sectors, each sector corresponding to one of the double star’s components. The model spectrum for each sky sector may and will be different in general. For example, in the case of an AGN superimposed upon a cluster of galaxies, one might model the spectrum of the point-like AGN sector using a power law, and the spectrum from the surrounding cluster emission using a thermal plasma model. 1.2.3 Detector regions The observed count rate spectra are extracted in practice in different regions of the detector. It is necessary here to distinguish clearly the (sky) sectors and (detector) regions. A detector region for the XMM EPIC camera would be for example a rectangular box, spanning a certain numberof pixels in the x- and y-directions. It may also beacircular or annular extraction region centered around a particular pixel of the detector, or whatever spatial filter is desired. For the XMM RGS it could be a specific ”banana” part of the detector-coordinate CCD pulse-height plane (z,E). Note that the detector regions need not to coincide with the sky sectors, neither should their number to be equal! A good example of this is again the example of an AGN superimposed upon a cluster of galaxies. The sky sector corresponding to the AGN is simply a point, while, for a finite instrumental psf, its extraction region at the detector is for example a circular region centered around the pixel corresponding to the sky position of the source. Also, one could observe the same source with a number of different instruments and analyse the data simultaneously. In this case one would have only one sky sector but more detector regions, namely one for each participating instrument. 1.3 Different types of spectral components In aspectral model SPEX uses two different types of components, called additive and multiplicative components respectively. Additive components have a normalisation that determines the flux level. Multiplicative components operate on additive components. A delta line or a power law are typical examples of additive components. Interstellar absorption is a typical example of multiplicative components. The redshift component is treated as a multiplicative component, since it operates on additive components. Additive components can be divided into two classes: simple components (like power law, blackbody etc.) and plasma components, that use our atomic code. For the plasma components it is possible to plot or list specific properties, while for the simple models this is not applicable.
1.3 Different types of spectral components 9 Multiplicative components can be divided into 3 classes. First, there are the absorption-type components, like interstellar absorption. These components simply are an energy-dependent multiplication of the original source spectrum. SPEX has both simple absorption components as well as absorption components based upon our plasma code. The second class consists of shifts: redshift (either due to Doppler shifts or due to cosmology) is the prototype of this. The third class consists of convolution-type operators. An example is Gaussian velocity broadening. For more information about the currently defined spectral components in SPEX, see chapter 3.
Page 1: SPEX Reference Manual Jelle Kaastra
Page 4 and 5: 4 CONTENTS 2.29 System . . . . . .
Page 6 and 7: 6 CONTENTS 6.6 Rgsvprof . . . . . .
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 data delete inst
Page 20 and 21: 20 Syntax overview dem mult #i - Do
Page 22 and 23: 22 Syntax overview distance show -
Page 24 and 25: 24 Syntax overview Examples elim 0.
Page 26 and 27: 26 Syntax overview There is yet ano
Page 28 and 29: 28 Syntax overview ignore 1:8 unit
Page 30 and 31: 30 Syntax overview written to this
Page 32 and 33: 32 Syntax overview eV, keV, Å, as
Page 34 and 35: 34 Syntax overview (Z = 7), ... Ni
Page 36 and 37: 36 Syntax overview plot view x1 #r
Page 38 and 39: 38 Syntax overview plot model lw #i
Page 40 and 41: 40 Syntax overview 2.25 Shiftplot:
Page 42 and 43: 42 Syntax overview 2.27 Step: Grid
Page 44 and 45: 44 Syntax overview system exe #a -
Page 46 and 47: 46 Syntax overview Update: several
Page 48 and 49: 48 Syntax overview Also the totals
Page 50 and 51: 50 Spectral Models Table 3.1: Avail
Page 52 and 53: 52 Spectral Models nr name chemical
Page 54 and 55: 54 Spectral Models (cf. Rybicky & L
Page 56 and 57: 56 Spectral Models 3.6.5 Abundances
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58 Spectral Models 3.8 dabs: dust a
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60 Spectral Models 3.11 Dem: Differ
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62 Spectral Models • ... • last
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64 Spectral Models f9 - Transmissio
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66 Spectral Models 3.22 Neij: Non-E
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68 Spectral Models Warning: By defa
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70 Spectral Models seeing equal con
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72 Spectral Models • type=4: b 1
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74 Spectral Models v - Velocity bro
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76 Spectral Models For more informa
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78 More about spectral models Slab
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80 More about spectral models depth
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82 More about spectral models grid
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84 More about spectral models The e
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86 More about plotting Table 5.1: A
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88 More about plotting 5.5 Plot tex
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90 More about plotting Table 5.4: S
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92 More about plotting Table 5.5: x
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94 More about plotting the plot wil
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96 More about plotting
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98 Auxilary programs Property Spect
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100 Auxilary programs Property Resp
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102 Auxilary programs 15. Optional:
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104 Auxilary programs 6.3 RGS fluxc
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106 Auxilary programs This redistri
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108 Auxilary programs 6.6.1 Theory
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110 Response matrices models. Since
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112 Response matrices Table 7.1: We
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114 Response matrices Table 7.2: Sc
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116 Response matrices since the lar
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118 Response matrices Figure 7.1: D
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120 Response matrices Figure 7.3: R
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122 Response matrices 7.4 Model bin
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124 Response matrices In this secti
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126 Response matrices The resulting
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128 Response matrices where w 1 and
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130 Response matrices spectrumextra
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132 Response matrices may be helpfu
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134 Response matrices 1. The OGIP r
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136 Response matrices Table 7.9: Se
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138 Response matrices could be the
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140 Response matrices Table 7.13: R
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142 Response matrices Figure 7.8: B
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144 Response matrices Figure 7.9: B
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146 Installation and testing
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148 Acknowledgements
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150 BIBLIOGRAPHY [1989] Kaastra, J.
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