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The final tab is Finishing. For print shops needing information related to bindery and finishing, choices can be made in this dialog box. A special note area is available for custom finishing requests (see Figure 6-27).

For nearby objects z 1 and so d1um ~ dphys ie the objects really are just as far away as they look But more distant objects appear further away (dl um > d phys ) than they really are If the geometry is not flat, this gives an additional effect which can either enhance this trend (hyperbolic geometry) or oppose it (spherical geometry) - see Problem A22 Provided there is no cosmological constant, there are useful analytic forms for the luminosity distance as a function of redshift, related to an equation known as the Mattig equation, but once a cosmological constant is introduced calculations have to be done numerically A detailed account can be found in Peacock's textbook (see Bibliography) Before we can use the luminosity distance in practice, there is a problem to overcome.

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As above, we have changed the subscripts to indicate that the summations run over the orbitals rather than the electrons. The two-electron repulsion integrals Jab and Kab are formally de ned as Jab Kab fa 1 fb 2 fa 1 fb 2 e2 f 1 fb 2 dt1 dt2 r12 a e2 f 2 fb 1 dt1 dt2 r12 a AX25 AX26

A ZipFile object has a debug attribute that you can use to change the level of debug output messages. Most output comes with a value of 3, the least (no output) is with a value of 0, the default.

Ai C and J Wyant, Effect of Spurious Re ection on a Phase Shift Interferometry, Appl Opt, 27, 3039 3045 (1988) Ai C and JC Wyant, Absolute Testing of Flats Decomposed to Even and Odd Functions, Proc SPIE, 1776, 73 83 (1992) Ai C and J Wyant, Effect of Retrore ection on a Phase-Shifting Interferometer, Appl Opt, 32, 3470 3478 (1993) Burge J H, Fizeau Interferometry for Large Convex Surfaces, Proc SPIE, 2536, 127 138 (1995) Deck L, D Stephenson, M Kuchel, and C Evans, Advances in Laser Fizeau Inteferometry for Optical Testing, TOPS, 76, 108 111 (2000) Forman P F, A Note on Possible Errors Due to Thickness Variations in Testing Nominally Parallel Plates, Appl Opt, 3, 646 (1964) Forman P F, The Zygo Interferometer System, Proc SPIE, 192, 41 (1979) Fritz B S.

The luminosity we have described is the total luminosity of the source across all wavelengths (called the bolometric luminosity), but in practice a detector is sensitive only to a particular range of wavelengths The redshifting of light means that the detector is seeing light emitted in a different part of the spectrum, as compared to nearby objects If enough is known about the emission spectrum of the object, a correction can be applied to allow for this which is known as the K-correction, though often its application is an uncertain business The luminosity distance depends on the cosmological model we have under discussion and hence can be used to tell us which cosmological model describes our Universe In particular we can plot the luminosity distance against redshift for different cosmologies, as in Figure A23 (see Problem A2A to find out how to obtain these curves).

, Absolute Calibration of an Optical Flat, Proc SPIE, 433, 123 (1983) Fritz B S, Absolute Calibration of an Optical Flat, Opt Eng, 23, 379 (1984) Grigor ev V A, Va O Zaborov, and P P Ivanov, Use of a Liquid Mirror for the Calibration of an Interferometer, Sov J Opt Technol, 53, 613 (1986) Hariharan P and W H Steel, Fringe Localization Depth: A Comment, Appl Opt, 28, 29 (1989) Karow H H, Interferometric Testing in a Precision Optics Shop: A Review of Testplate Testing, Proc SPIE, 192, 56 (1979) Ketelsen D A and D S Anderson, Optical Testing With Large Liquid Flats, Proc SPIE, 966, 365 (1988) Malacara D and A Cornejo, Testing of Aspherical Surfaces with Newton Fringes, Appl Opt, 9, 837 (1970) Moore R C and F H Slaymaker, Direct Measurement of Phase in a SphericalWave Fizeau Interferometer, Appl.

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