X-Ray Spectroscopy of Cosmic Sources

Kahn, S. M.; Liedahl, D. A.

doi:10.1007/978-1-4899-1412-5_8

Cited by 7 publications

(4 citation statements)

References 157 publications

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“…Although the semiconductor detectors offer a better energy resolving power than the gas filled detectors and the scintillator detectors, their performance is sometimes still not good enough. In order to reach higher energy resolving powers wavelength-dispersive spectrometers are used [5], such as those based on crystal diffraction. A crystal diffracts X rays because of the regular periodicity of the lattice planes.…”

Section: Crystal-based Spectrometersmentioning

confidence: 99%

“…This process is strongly energy dependent (Γ a ∝ Ω 5 ). Using the low temperature elastic constants for InSb Goldie [74] calculated an anharmonic decay time of 570 µs (1/Ω) 5 , where Ω is the phonon energy in meV. This equation is for the dominant process where one longitudinal phonon splits into two transverse phonons with half the energy of the initial phonon.…”

Section: Thermal Model Of Detectors With Dielectric Absorbersmentioning

confidence: 99%

“…This equation is for the dominant process where one longitudinal phonon splits into two transverse phonons with half the energy of the initial phonon. Next Goldie quotes a total lifetime of the order of 540 µs (1/Ω) 5 , where Ω again is in meV. perfect straight line because the phonons have discrete frequencies (ν D,InSb / 2 n , where n is an integer).…”

Section: Thermal Model Of Detectors With Dielectric Absorbersmentioning

confidence: 99%

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Low temperature y-ray spectrometers based on bulk superconducting and dielectric absorber crystals

Netel

1999

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Chapter 1-Introduction Many areas of research rely on the detection of radiation, in the form of single photons or particles. By measuring the photons or particles coming from an object a lot can be learned about the object under study. In some cases there is a simple need to know the number of photons coming from the source. In cases like this a simple counter, like a Geiger-Mueller survey meter, will suffice. In other cases one want to know the spectral distribution of the photons coming from the source. In cases like that a spectrometer is needed that can distinguish between photons with different energies, like a diffraction or transmission grating. The work presented in this thesis focused on the development of a new generation broad band spectrometer that has a high energy resolving power, combined with a high absorption efficiency for photon energies above 10 keV and up to 500 keV. The spectrometers we are developing are based on low-temperature sensors, like superconducting tunnel junctions or transition edge sensors, that are coupled to bulk absorber crystals. We use the low-temperature sensors because they can offer a significant improvement in energy resolving power, compared to conventional spectrometers. We couple the low-temperature sensors to bulk absorber crystals to increase the absorption efficiency. In this chapter I introduce different types of radiation detectors and spectrometers and areas where they are being used. I also discuss the history and motivation of low-temperature spectrometers and show some of the impressive results that have been achieved in this field over the last few years. Finally I discuss the outline of this thesis.

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Section: Crystal-based Spectrometersmentioning

confidence: 99%

Section: Thermal Model Of Detectors With Dielectric Absorbersmentioning

confidence: 99%

Section: Thermal Model Of Detectors With Dielectric Absorbersmentioning

confidence: 99%

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Low temperature y-ray spectrometers based on bulk superconducting and dielectric absorber crystals

Netel

1999

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“…For example, 1s 2 ,2s 2 ,2p6 ,5f. The orbitals are conventionally listed according to increasing n, then by increasing l, that is, 1s, 2s, 2p, 3s, 3p, 3d, ….. Closed shell configurations may be omitted from the enumeration (see section 4 for Quantum Number definitions).…”

mentioning

confidence: 99%

Simple Spectral Lines Data Model Version 1.0

Osuna¹,

Salgado²,

Guainazzi³

et al.

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This is an IVOA Recommendation. It has been endorsed by the IVOA Executive Committee as an IVOA Recommendation. It is a stable document and may be used as reference material or cited as a normative reference from another document. IVOA's role in making the Recommendation is to draw attention to the specification and to promote its widespread deployment. This enhances the functionality and interoperability inside the Astronomical Community.It is appropriate to reference this document only as a recommended standard that is under review and which may be changed before it is accepted as a full recommendation.

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