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PARALLEL PROCESSING tools for today's optiker a fringe spacing of about 20 μm in the focal plane. The maximum sepa- ration of the outer mirrors was 6.1 m, so that the smallest measurable an- gular diameter (with λ = 550 nm) was about 0.02 seconds of arc. 3 Again quoting Wood: 7 "The bright star Betelgeuse was the first investigated. This star shows evi- dence of its diameter with the 100- inch telescope if a canvas cover is placed over the instrument, provid- ed with two holes 7 inches in diame- ter and 94 inches apart, the diffrac- tion disk of the star being crossed with faint interference bands. If ei- ther hole is covered the bands disap- pear. If the telescope is pointed at Rigel, however, the bands are clear and strong, showing that Rigel's an- gular diameter is smaller than that of Betelgeuse. With the 20-foot inter- ferometer the bands disappeared en- tirely in the case of Betelgeuse when the mirrors were separated by a dis- tance of 120 inches, while Rigel showed very distinct bands. The an- gular diameter of Betelgeuse was computed as 0.047 second of arc. From the known distance of the star (determined by triangulation), its actual diameter was calculated as 250 million miles (i.e., 300 times the diameter of the sun) or greater than the Earth's orbit about the sun (190 million miles across). Its diameter has been found to vary, howev- er, for at times the mirrors must be sepa- rated by a distance of 14 feet before the fringes disappear. Antares was found to be still larger, having a diameter of 400 mil- lion miles. The mini- mum angular diame- ter measurable with the 20-foot instru- ment is 0.024 second of arc." The majority of the stars are either too dis- tant or too small for the Michelson inter- ferometer to measure their diameter. For example, at the distance of the nearest star (Alpha Centauri) the sun's disk would subtend an angle of only 0.007 s/arc, and to observe the first disappearance of the fringes a mirror separation of 20 m would be necessary. The construction of such a large interferometer would be a difficult undertaking because of the requirement of rigid mechanical connection between the collecting mirrors and the eyepiece. 3 In recent years, the method of Hanbury Brown and Twiss, as well as exten- sions of Michelson's method to ra- dio astronomy have been used for measurements of some of the small- er astronomical objects. 2-4 Biographical note Albert Abraham Michelson (1852- 1931) was born in what was then Germany (now Poland) and emi- grated with his family to the U.S. in 1855. He became professor of physics at the Case School of Ap- plied Science (Cleveland, Ohio), Clark University (Worcester, Mass.), and the University of Chicago (I11.). In 1907, he became the first Ameri- can to receive a Nobel prize. The prize citation reads: "For his optical precision instruments and the spec- troscopic and metrological investi- gations carried out with their aid." References 1. H. Fizeau, C.R. Acad. Sci. Paris 66, 934(1868). 2. L. Mandel and E. Wolf, Optical Coher- ence and Quantum Optics, (Cambridge Univ. Press, London, U.K., 1995). 3. M. Born and E. Wolf, Principles of Optics, 6th ed., (Pergamon Press, Oxford, U.K., 1980). 4. M.V. Klein, Optics, (John Wiley & Sons Inc., New York, N.Y., 1970). 5. The simulations reported in this article were performed by DIFFRACT™, a product of MM Re- search Inc., Tucson, Ariz. 6. One degree is 60 min., and 1 min. is 60 s/arc. One s/arc is the angle subtended by a penny at a distance of 3.5 km. 7. R.W. Wood, Physical Optics, 3rd ed., (reprinted by the Optical Society of America, Washington, D.C., 1988). 8. A.A. Michelson, Phil. Mag. 30, 1 (1890); A.A. Michelson, Nature, Lond. 45, 160 (1891). 9. A.A. Michelson, Astrophys. J. 51, 257 (1920); A.A. Michelson and F.G. Pease, Astrophys. J. 53, 249 (1921). 0PN Contributing Editor Masud Mansuripur is a pro- fessor at the Optical Sciences Center, University of Arizona, Tucson, Ariz.; [email protected]. Electronic Information OSA's Electronic Information Committees MIKE DUNCAN S ome of the most exciting changes in the world today result from ad- vances in electronic communications. It doesn't really matter anymore what you do or where you live, new com- munication technology is almost cer- tainly affecting how you work. For technical professionals the impact is even greater and affects how we learn, how we do research, how we buy, how we publish, and how we communi- cate with colleagues and our profes- sional societies. A number of years ago, OSA realized how important these changes would become to mem- bers and responded by creating com- Figure 7. Michelson's stellar interferometer. The apertures S1 and S 2 are fixed, and the light reaches them after reflection at mirrors M1, M2, M3, and M4. The inner mirrors M3 and M 4 are fixed, while the outer mirrors M1 and M 2 can be moved sym- metrically in the direction joining S1 and S2. If the optical paths M 1 M 3 S 1 and M 2 M 4 S 2 are maintained equal, the optical path difference for light from a distant point source is the same at S1 and S2 as at M1 and M 2 , so that the outer mirrors play the part of the movable apertures in the Fizeau method. A plane parallel glass plate C1 which could be inclined in any direction, is used to maintain the geometrical pencils from S 1 and S 2 in coincidence in the focal plane. A second plane parallel glass plate C 2 , of variable thickness, is used to com- pensate inequalities of the optical paths M1M3S1 and M2M4S2. (Adapted from Born and Wolf. 3 ) Optics & Photonics News/January 1998 43
Transcript of OSA's Electronic Information Committees
PARALLEL PROCESSING tools for today's optiker
a fringe spacing of about 20 μ m in the focal plane. The maximum separation of the outer mirrors was 6.1 m, so that the smallest measurable angular diameter (with λ = 550 nm) was about 0.02 seconds of arc. 3
A g a i n q u o t i n g W o o d : 7 " T h e bright star Betelgeuse was the first investigated. This star shows evidence of its diameter with the 100-inch telescope if a canvas cover is placed over the instrument, provided with two holes 7 inches in diameter and 94 inches apart, the diffraction disk of the star being crossed with faint interference bands. If either hole is covered the bands disappear. If the telescope is pointed at Rigel, however, the bands are clear and strong, showing that Rigel's angular diameter is smaller than that of Betelgeuse. With the 20-foot interferometer the bands disappeared entirely in the case of Betelgeuse when the mirrors were separated by a distance o f 120 inches, whi le Rigel showed very distinct bands. The angular diameter o f Betelgeuse was computed as 0.047 second of arc. From the known distance of the star (determined by triangulation), its actual diameter was calculated as 250 million miles (i.e., 300 times the diameter of the sun) or greater than
the Earth 's o rb i t about the sun (190 mill ion miles across). Its diameter has been found to vary, however, for at t imes the mirrors must be separated by a distance of 14 feet before the f r inges d isappear . Antares was found to be still larger, having a diameter of 400 mi l lion miles. The minim u m angular diameter measurable with the 20- foot i n s t r u ment is 0.024 second of arc."
The majority of the stars are either too distant or too small for the Michelson inter
ferometer to measure their diameter. For example, at the distance of the nearest star (Alpha Centauri ) the sun's disk would subtend an angle of only 0.007 s/arc, and to observe the first disappearance of the fringes a mirror separation of 20 m would be necessary. The construction o f such a large interferometer would be a difficult undertaking because of the requirement of rigid mechanical connection between the collecting mirrors and the eyepiece.3 In recent years, the m e t h o d o f H a n b u r y Brown and Twiss, as well as extensions of Michelson's method to radio astronomy have been used for measurements of some of the smaller astronomical objects.2 - 4
Biographical note Albert Abraham Michelson (1852-1931) was born in what was then Germany (now Poland) and emi grated with his family to the U.S. in 1855. H e became pro fessor o f physics at the Case School of A p pl ied Science (Cleveland, O h i o ) , Clark University (Worcester, Mass.), and the University of Chicago (I11.). In 1907, he became the first Amer i can to receive a Nobel prize. The prize citation reads: "For his optical precision instruments and the spec
troscopic and metrological investigations carried out with their aid."
References 1. H. Fizeau, C.R. Acad. Sci. Paris 66,
934(1868). 2. L. Mandel and E. Wolf, Optical Coher
ence and Quantum Optics, (Cambridge Univ. Press, London, U.K., 1995).
3. M. Born and E. Wolf, Principles of Optics, 6th ed., (Pergamon Press, Oxford, U.K., 1980).
4. M.V. Klein, Optics, (John Wiley & Sons Inc., New York, N.Y., 1970).
5. The simulations reported in this article were performed by DIFFRACT™, a product of MM Research Inc., Tucson, Ariz.
6. One degree is 60 min., and 1 min. is 60 s/arc. One s/arc is the angle subtended by a penny at a distance of 3.5 km.
7. R.W. Wood, Physical Optics, 3rd ed., (reprinted by the Optical Society of America, Washington, D.C., 1988).
8. A.A. Michelson, Phil. Mag. 30, 1 (1890); A.A. Michelson, Nature, Lond. 45, 160 (1891).
9. A.A. Michelson, Astrophys. J. 51, 257 (1920); A.A. Michelson and F.G. Pease, Astrophys. J. 53, 249 (1921).
0PN Contributing Editor Masud Mansuripur is a professor at the Optical Sciences Center, University of Arizona, Tucson, Ariz.; [email protected].
Electronic Information
OSA's Electronic
Information Committees
MIKE DUNCAN
Some of the most exciting changes in the world today result from ad
vances in electronic communications. It doesn't really matter anymore what you do or where you live, new communication technology is almost certainly affecting how you work. For technical professionals the impact is even greater and affects how we learn, how we do research, how we buy, how we publish, and how we communicate with colleagues and our professional societies. A number of years ago, O S A realized how important these changes would become to members and responded by creating com-
Figure 7. Michelson's stellar interferometer. The apertures S1
and S 2 are fixed, and the light reaches them after reflection at mirrors M1, M2, M3, and M4. The inner mirrors M3 and M 4 are fixed, while the outer mirrors M1 and M 2 can be moved symmetrically in the direction joining S1 and S2. If the optical paths M 1 M 3 S 1 and M 2 M 4 S 2 are maintained equal, the optical path difference for light from a distant point source is the same at S1 and S2 as at M1 and M 2 , so that the outer mirrors play the part of the movable apertures in the Fizeau method. A plane parallel glass plate C1 which could be inclined in any direction, is used to maintain the geometrical pencils from S 1
and S 2 in coincidence in the focal plane. A second plane parallel glass plate C 2 , of variable thickness, is used to compensate inequalities of the optical paths M1M3S1 and M2M4S2. (Adapted from Born and Wolf.3)
Optics & Photonics News/January 1998 43
PARALLEL PROCESSING tools for today's optiker
mittees to advise the Society on the impact of, and the opportunities provided by, new forms of electronic publishing, electronic communication, and digital technology.
The first OSA committee to explicitly deal with these issues was the Publishing Technology Committee (a subcommittee of the Publications Council) whose scope was to ". . . evaluate publication policies pertaining to new-technology-based publications and provide guidance and support in the implementation of new-technology-based publications." Consisting of one chair and nine members, the committee advises OSA on issues relating to the nitty-gritty details of new publishing technologies including C D -ROMs, online journals, electronic submissions, electronic publication formats, electronic archiving, and other issues related to electronic information transmittal.
Electronic champions Currently the Publishing Technology Committee helps keep the Society abreast of changes in the field of electronic publishing, the Internet, and browser technology. The committee identifies 'champions' from committee and OSA membership to help monitor and report on the details of issues such as electronic archiving of information, journal citations, electronic submissions, Java, multimedia, PDF, electronic product pricing, search engines, agent technology,
SGML/HTML/XML, TeX, video conferencing, and online conferences. Three champions and their issues have already been found: Casimer DeCusatis, online conferences; Neal Gallagher, multimedia; and Mike Duncan, search engines and agent technology. Other champions are actively being sought. If you are interested, contact Bob Jopson at [email protected].
Online presence With the advent of the World Wide Web, new opportunities for communication arose, some so radical that they threatened the economic core of many societies by providing alternatives to paper publications. OSA responded by aggressively pursuing two high priority paths: Creating a first class Web site, OpticsNet, and establishing an all-electronic journal, Optics Express.
An implementation committee was formed for Optics Express. After much hard work and in a surprisingly short time, the journal, under the guiding hand of Joe Eberly, debuted in July 1997. The result is a world-class, peer-reviewed optics journal, with an outstandingly short time-to-publication, multimedia capabilities, and easy worldwide access. The Optics Express Implementation Committee, having completed its duties, has been disbanded. Steering of the journal has been taken over by the editor and associate editors.
OpticsNet, an electronic window to most Society activities, was first created simply to give OSA a Web presence. But it was quickly realized that the site had to meet the usual, high-standards for information published by OSA and that it had the potential to be a powerful tool for anyone interested in optics or photonics. An ad-hoc committee was created to, "advise on content, services, access, structure, and policy for the Web site; promote and advise on OpticsNets' potential and opportunities to other OSA committees; and serve as or appoint beta-testers and editors of new and current services." The chair and five members
meet biannually. If you wish to discuss OpticsNet, contact Mike Duncan at [email protected].
Issues discussed by the Optics-Net Committee have included OpticsNet's priority within OSA, the priorities of various components of OpticsNet, the success of the "look and feel" of the site, the appropriateness of advertising, the use of "cookies," tracking (who is coming to the site and from where), and "agent" technology. The committee has appointed Bob Guenther as editor for the links page—the place on OpticsNet that lists useful, optics-related information found on the Internet. He verifies that the links listed point to high quality information and helps to classify the various links by subcategory.
There are still many other issues for the OpticsNet committee to consider. For one thing, OpticsNet is being tied into the new, all-electronic data management system that makes up OSA's Optics InfoBase. What new member services will this enable and how will this affect the delivery of electronic information? Other questions relate to the Technical Homes available on OpticsNet. Who will run them and what kind of information will they contain? Finally, OpticsNet costs money to operate. Where should the money come from? Should OpticsNet charge for certain services?
One of the most satisfying aspects of belonging to OSA is the opportunity to become involved in active committees that have an impact on how the Society is run. The committees discussed above are good examples. All three have helped shape the way the Society does business in the new world of networked, electronic information. And they have done so because of the active interest and involvement of OSA members. Want to help shape the future of your Society? Express an interest. Do something. Get involved!
Mike Duncan, the chair elect of the publications council, is the head of the nonlinear optics section of the Laser Physics Branch at the Naval Research Laboratory; [email protected].
44 Optics & Photonics News/January 1998
