000			03522nam a2200361 a 4500
001			ebr10514141
003			CaPaEBR
006			m u
007			cr cn|||||||||
008			110706s2011 enka sb 001 0 eng d
010			_z 2011023034
020			_z9780521883733 (hardback)
020			_z9781139157087 (e-book)
040			_aCaPaEBR _cCaPaEBR
035			_a(OCoLC)773036123
050	1	4	_aQB472 _b.H36 2011eb
082	0	4	_a522/.6863 _223
245	0	0	_aHandbook of X-ray astronomy _h[electronic resource] / _cedited by Keith A. Arnaud, Randall K. Smith, and Aneta Siemiginowska.
260			_aCambridge ; _aNew York : _bCambridge University Press, _c2011.
300			_aviii, 197 p. : _bill.
490	1		_aCambridge observing handbooks for research astronomers ; _v7
504			_aIncludes bibliographical references and index.
505	8		_aMachine 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.
520			_a"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"-- _cProvided by publisher.
533			_aElectronic reproduction. _bPalo Alto, Calif. : _cebrary, _d2013. _nAvailable via World Wide Web. _nAccess may be limited to ebrary affiliated libraries.
650		0	_aX-ray astronomy.
655		7	_aElectronic books. _2local
700	1		_aArnaud, Keith A., _d1959-
700	1		_aSmith, Randall K. _q(Randall Knowles), _d1969-
700	1		_aSiemiginowska, Aneta.
710	2		_aebrary, Inc.
830		0	_aCambridge observing handbooks for research astronomers ; _v7.
856	4	0	_uhttp://site.ebrary.com/lib/daystar/Doc?id=10514141 _zAn electronic book accessible through the World Wide Web; click to view
999			_c196599 _d196599