Handbook of X-ray astronomy / edited by Keith A. Arnaud, Randall K. Smith, Aneta Siemiginowska.

Contributor(s):

Material type: Text

TextSeries: Cambridge observing handbooks for research astronomersPublication details: Cambridge ; New York : Cambridge University Press, 2011.Description: viii, 197 p. : ill. ; 24 cmISBN:

9780521883733 (hardback)

Subject(s):

DDC classification:

522/.6863 23

LOC classification:

QB472 .H36 2011

Other classification:

SCI004000

Contents:

Machine generated contents note: 1. X-ray astronomy optics Daniel A. Schwartz; 2. Proportional counters and other detector techniques Richard J. Edgar; 3. CCDs for x-ray astronomy Catherine E. Grant; 4. Data reduction and calibration Keith A. Arnaud and Randall K. Smith; 5. Data analysis Randall K. Smith, Keith A. Arnaud and Aneta Siemiginowska; 6. Archives, surveys, catalogues and software Keith Arnaud; 7. Statistics Aneta Siemiginowska; 8. Analysis of extended emission K. D. Kuntz; Appendices; Index.

Summary: "It may be obvious why visible astronomy utilizes images, but it is illustrative to consider the value of focusing to X-ray astronomy. A list of advantages offered by the best possible two-dimensional angular resolution would include: (i) Resolving sources with small angular separation and distinguishing different regions of the same source. (ii) Using the image morphology to apply intuition in choosing specific models for quantitative fits to the data. (iii) Using as a "collector" to gather photons. This is necessary because X-ray-source fluxes are so low that individual X-ray photons are detected; the weakest sources give less than one photon per day. (iv) Using as a "concentrator," so that the photons from individual sources interact in such a small region of the detector that residual non-X-ray background counts are negligible. (v) Measuring sources of interest and simultaneously determining the contaminating background using other regions of the detector. (vi) Using with dispersive spectrometers such as transmission or reflection gratings to provide high spectral resolution. The Earth's atmosphere completely absorbs cosmic X-rays. Consequently, X-ray observatories must be launched into space; so size, weight, and cost are always important constraints on the design. In practice this leads to a trade-off between the best possible angular resolution and the largest possible collecting area. Realizing an X-ray telescope involves two key issues: reflection of X-rays, and formation of an image"-- Provided by publisher.

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Holdings
Item type	Current library	Call number	Status	Date due	Barcode
Books	Raman Research Institute Library	52-735 ARN (Browse shelf(Opens below))	Checked out	28.03.2024	26611

Includes index.

"It may be obvious why visible astronomy utilizes images, but it is illustrative to consider the value of focusing to X-ray astronomy. A list of advantages offered by the best possible two-dimensional angular resolution would include: (i) Resolving sources with small angular separation and distinguishing different regions of the same source. (ii) Using the image morphology to apply intuition in choosing specific models for quantitative fits to the data. (iii) Using as a "collector" to gather photons. This is necessary because X-ray-source fluxes are so low that individual X-ray photons are detected; the weakest sources give less than one photon per day. (iv) Using as a "concentrator," so that the photons from individual sources interact in such a small region of the detector that residual non-X-ray background counts are negligible. (v) Measuring sources of interest and simultaneously determining the contaminating background using other regions of the detector. (vi) Using with dispersive spectrometers such as transmission or reflection gratings to provide high spectral resolution. The Earth's atmosphere completely absorbs cosmic X-rays. Consequently, X-ray observatories must be launched into space; so size, weight, and cost are always important constraints on the design. In practice this leads to a trade-off between the best possible angular resolution and the largest possible collecting area. Realizing an X-ray telescope involves two key issues: reflection of X-rays, and formation of an image"-- Provided by publisher.

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Handbook of X-ray astronomy / edited by Keith A. Arnaud, Randall K. Smith, Aneta Siemiginowska.