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

Contributor(s):

Material type: Text

TextSeries: Cambridge observing handbooks for research astronomersPublication details: Cambridge, UK ; New York : Cambridge University Press, 2011.Description: 1 online resource (viii, 197 pages) : illustrationsContent type:

text

Media type:

computer

Carrier type:

online resource

ISBN:

9781139157087
1139157086
9781139160896
1139160893
9781139034234
1139034235
128334095X
9781283340953
9781139158848
1139158848
1107226082
9781107226081
1139159895
9781139159890
9786613340955
6613340952
1139155334
9781139155335

Subject(s):

Genre/Form:

Electronic books.

Additional physical formats: Print version:: Handbook of X-ray astronomy.DDC classification:

522/.6863 23

LOC classification:

QB472 .H36 2011eb

Other classification:

SCI004000

Online resources:

Click here to access online

Contents:

1. Optics / Daniel A. Schwartz -- 2. Detectors / Richard J. Edgar -- 3. Charge-coupled devices / 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, catalogs, and software / Keith Arnaud -- 7. Statistics / Aneta Siemiginowska -- 8. Extended emission / Kip D. Kuntz -- Appendices.

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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Item type	Home library	Collection	Call number	Materials specified	Status	Date due	Barcode
Electronic-Books	OPJGU Sonepat- Campus	E-Books EBSCO			Available

Includes bibliographical references (pages 190-194) and 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