An original plastic-lens array molded integrally as one block having a function of forming a unit-magnification erect image has been developed. The lens array consists of eight lens devices. The lens device has a roof prism, a reflecting v-groove, and a pair of convex-lens surfaces. A prototype of the lens arrays are arranged side by side. Thickness of the lens array is 4.5 mm, distance between object and image planes is 14.4 mm, array pitch is 1.3 mm, and the effective imaging region is 220 mm. The average modulation transfer function (MTF) at 41 p/mm of the lens array is 76% in the row direction (Y-direction) and 80% in the direction (X-direction) normal to Y-direction. The average F/NO in line-scanning is 1.8. The average irradience unevenness in line-scanning is 17%. The focal depth is +/- 0.6 mm in the area with the MTF being 60% or more. With this prototype a high-resolution image was attained. So, the lens arrays can be applied to imaging devices for use in a compact facsimile, image scanner, LED printer, and so on.

Get PDF Email Share Share with Facebook Tweet This Post on reddit Share with LinkedIn Add to CiteULike Add to Mendeley Add to BibSonomy Get Citation Copy Citation Text Mary Faldon, Roy J. Rosser, and Robert J. Speer, "Low-cost adjustable toroidal mirror," Appl. Opt. 27, 2630-2630 (1988) Export Citation BibTex Endnote (RIS) HTML Plain Text Citation alert Save article

A toroidal relay optic has been used to overcome the problem of damage caused by debris that has limited previous attempts at soft x-ray lithography and contact microscopy using laser-produced plasma sources. Not only is the specimen preserved, but it is now possible to have a vacuum retaining soft x-ray transparent Si(3)N(4) window as a permanent part of the apparatus, greatly simplifying specimen handling. The exposure times are ~2 ns.

Journal of MicroscopyVolume 144, Issue 2 p. RP5-RP6 Biological specimens imaged by soft x-ray contact microscopy using a plasma source produced with a laboratory sized laser R. J. Rosser, R. J. Rosser Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorR. Feder, R. Feder I.B.M., J.T. Watson Research Center, Yorktown Heights, NY 10598, USA Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorA. Ng, A. Ng Physics Department, UBC, Vancouver, Canada, V6T 1Z4 Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorF. Adams, F. Adams Physics Department, UBC, Vancouver, Canada, V6T 1Z4 Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorM. Caldarolo, M. Caldarolo I.B.M., J.T. Watson Research Center, Yorktown Heights, NY 10598, USA Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorP. Celliers, P. Celliers Physics Department, UBC, Vancouver, Canada, V6T 1Z4 Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorP. C. Cheng, P. C. Cheng I.B.M., J.T. Watson Research Center, Yorktown Heights, NY 10598, USA Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorL. Da Silva, L. Da Silva Physics Department, UBC, Vancouver, Canada, V6T 1Z4 Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorD. Parfeniuk, D. Parfeniuk Physics Department, UBC, Vancouver, Canada, V6T 1Z4 Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorR. J. Speer, R. J. Speer Physics Department, SUNY, Stony Brook, NY 11794, USA Blackett Laboratory, Imperial College, London SW7 2BZ, UKSearch for more papers by this author R. J. Rosser, R. J. Rosser Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorR. Feder, R. Feder I.B.M., J.T. Watson Research Center, Yorktown Heights, NY 10598, USA Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorA. Ng, A. Ng Physics Department, UBC, Vancouver, Canada, V6T 1Z4 Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorF. Adams, F. Adams Physics Department, UBC, Vancouver, Canada, V6T 1Z4 Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorM. Caldarolo, M. Caldarolo I.B.M., J.T. Watson Research Center, Yorktown Heights, NY 10598, USA Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorP. Celliers, P. Celliers Physics Department, UBC, Vancouver, Canada, V6T 1Z4 Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorP. C. Cheng, P. C. Cheng I.B.M., J.T. Watson Research Center, Yorktown Heights, NY 10598, USA Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorL. Da Silva, L. Da Silva Physics Department, UBC, Vancouver, Canada, V6T 1Z4 Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorD. Parfeniuk, D. Parfeniuk Physics Department, UBC, Vancouver, Canada, V6T 1Z4 Physics Department, SUNY, Stony Brook, NY 11794, USASearch for more papers by this authorR. J. Speer, R. J. Speer Physics Department, SUNY, Stony Brook, NY 11794, USA Blackett Laboratory, Imperial College, London SW7 2BZ, UKSearch for more papers by this author First published: November 1986 https://doi.org/10.1111/j.1365-2818.1986.tb02792.xCitations: 2AboutPDF ToolsRequest permissionExport citationAdd to favoritesTrack citation ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL No abstract is available for this article. REFERENCES Eason R.W., Cheng P., Feder R., Michette A., Rosser R., O'Neill F., Owadano Y., Rumsby P., and Shaw M., (1986) Optica Acta, vol. 33, No. 4, p 501– 516. Cheng, P.C., Peng, H.B., Feder, R., and McGowan, J.W. (1982) Electron Microscopy (10th. Int. Electron Mic. Proc.), Vol. 1, p 461– 462. Feder R., and Sayre D., (1980) Ann. N. Y. Acad. Sci. 342, p 213. Michette, A. G., Cheng, P. C., Feder, R., O'Neill, F., Owadano, Y., Rosser, R. J., Rumsby, P., and Shaw, M.J., (1986) J. Physics D, 19, p 363– 372. Rosser R.J., Baldwin K.G., Feder R., Bassett D., Cole A., and Eason R.W. (1985a) J. Microscopy, 138, p 310– 320. Rosser R.J., Feder R., Ng, A., and Celliers, P. (1985b) J. Microscopy, 140(1), p RP1. Speer, R.J., Turner, D., Johnson, R.L., Rudolph, D., and Schmahl, G. (1974) Applied Optics, vol. 13, No. 6, p 1258– 1262. Citing Literature Volume144, Issue2November 1986Pages RP5-RP6 ReferencesRelatedInformation

view Abstract Citations (94) References (37) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Rocket spectrogram of a solar flare in the 10-100 A region. Acton, L. W. ; Bruner, M. E. ; Brown, W. A. ; Fawcett, B. C. ; Schweizer, W. ; Speer, R. J. Abstract The soft (10-100 A) X-ray spectrum of an M-class solar flare was observed with a high-resolution (0.02 A) rocket-borne spectrograph on 1982 July 13. The spectrum samples an area of 600/sq arcsec on the sun, centered on or near the brightest X-ray feature of the flare. Several hundred emission lines characteristic of temperatures from about 0.5 to 7 x 10 to the 6th K have been photographically recorded. All but three of the stronger lines have been identified. It is argued that previous identification of the line at 17.62 A as iron Ly-alpha is incorrect. Spectral lines from nickel, iron, chromium, calcium, sulphur, silicon, aluminium, magnesium, neon, oxygen, nitrogen, and carbon are tabulated and discussed with extensive reference to earlier work. Absolute line intensities are given and the calibration of the telescope-spectrograph is discussed. Publication: The Astrophysical Journal Pub Date: April 1985 DOI: 10.1086/163125 Bibcode: 1985ApJ...291..865A Keywords: Abundance; Solar Flares; Solar Spectra; Solar X-Rays; Spectrograms; Calibrating; Emission Spectra; Line Spectra; Rocket-Borne Instruments; Solar Temperature; Spectrum Analysis; X Ray Spectra; X Ray Telescopes; Solar Physics full text sources ADS |

Get PDF Email Share Share with Facebook Tweet This Post on reddit Share with LinkedIn Add to CiteULike Add to Mendeley Add to BibSonomy Get Citation Copy Citation Text W. Harris, S. Mrowka, and R. J. Speer, "Linnik interferometer: its use at short wavelengths," Appl. Opt. 21, 1155-1155 (1982) Export Citation BibTex Endnote (RIS) HTML Plain Text Citation alert Save article

The 1933 LINNIK Point Diffraction Interferometer continues to offer new possibilities in non-contacting aspheric grazing incidence mirror testing. In this work we demonstrate the wave-front aberration of a stigmatic Soft X-Ray reflecting optic recorded at progressively shorter wavelengths to a current limit of 313 nm yielding a twofold increase in sensitivity over previously reported measurements.

Previous work has demonstrated the use of the LINNIK Point Diffraction Interferometer for the measurement of wavefront error in soft x-ray imaging systems. Operational wave-lengths from 632.8nm (He-Ne) down to 313.1nm (Hg) have been used. This paper describes our extension of the technique to 253.7nm together with a demonstration. of feasibility at 121.6 nm (Hydrogen. Lyman-α), we believe for the first time. Finally the possibility of working at soft X-Ray wavelengths is considered.

We now describe a new sounding rocket payload that has been developed for x-ray spectroscopic studies of the solar corona. The instrument incorporates a grazing incidence Rowland mounted grating spectrograph and an extreme off-axis parabolic sector telescope to isolate regions of the sun of order 1 X10 arc seconds in size. The focal surface of the spectrograph is shared by photographic and photoelectric detection systems, with the latter serving as a part of the rocket pointing system control loop. Fabrication and alignment of the optical system are based on high precision machining and mechanical metrology techniques. The spectrograph covers the 10 to 50 angstrom interval and has a resolution of 16 milliangstroms in the current version. Modifications planned for future flights will improve the resolution to around 5 milliangstroms, permitting line widths to be measured.

A series of 1200 mm−1 square-wave profile toric gratings have been examined for performance under Rowland circle focalization. The gratings were interferographically-recorded with plane waves on 5000 mm × 26.1 mm radii substrates, to yield gold-on-glass gratings without photoresist.

Annals of the New York Academy of SciencesVolume 342, Issue 1 p. 105-115 POLYCHROMATIC SOFT X-RAY IMAGING USING HOLOGRAPHICALLY RECORDED ASPHERIC GRATINGS R. J. Speer, R. J. Speer Blacken Laboratory Imperial College London SW7 2BZ, EnglandSearch for more papers by this authorR. Rosser, R. Rosser Blacken Laboratory Imperial College London SW7 2BZ, EnglandSearch for more papers by this authorS. Mrowka, S. Mrowka Blacken Laboratory Imperial College London SW7 2BZ, EnglandSearch for more papers by this author R. J. Speer, R. J. Speer Blacken Laboratory Imperial College London SW7 2BZ, EnglandSearch for more papers by this authorR. Rosser, R. Rosser Blacken Laboratory Imperial College London SW7 2BZ, EnglandSearch for more papers by this authorS. Mrowka, S. Mrowka Blacken Laboratory Imperial College London SW7 2BZ, EnglandSearch for more papers by this author First published: June 1980 https://doi.org/10.1111/j.1749-6632.1980.tb47212.xAboutPDF ToolsRequest permissionExport citationAdd to favoritesTrack citation ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL Share a linkShare onFacebookTwitterLinked InRedditWechat Volume342, Issue1Ultrasoft X-Ray Microscopy: Its Application to Biological and Physical SciencesJune 1980Pages 105-115 RelatedInformation

The telescope mirror for the X-Ray Spectrograph Spectrometer Telescope System is a sixty degree sector of an extreme off-axis paraboloid of revolution. It was designed fo focus a coronal region 1 by 10 arc seconds in size on the entrance slit of the spectrometer after reflection from the gold surface at a glancing angle of about 2.9 degrees. This paper discusses the design, manufacture, and metrology of the mirror, the methods of precision mechanical metrology used to focus the system, the mounting system which serves to locate the mirror and has proven itself through several vibration tests, and the results of reflection efficiency measurements at 8 and 44 Angstroms, and alignment tolerances and ray trace analysis of the effects of misalignment. The mirror was developed under NASA Contract NAS2-9181.

A simple interferometric method capable of displaying quantitatively the wave front aberration of any image-forming optical system is described. Its application for testing and aligning grazing incidence reflection optics at the same conjugates as those of short-wavelength use is demonstrated. The image-forming wave front from the system being tested is compared with a true spherical wave front generated within the interferometer from a point at the intended focus. The differences are displayed as a fringe pattern superimposed on an image of the exit pupil. Each fringe corresponds to one wavelength of separation between the actual image-forming wave front and the Gaussian reference sphere. The principle originates from a paper by W. P. Linnik published in Russian and German in 1933. A translation is included as an appendix. Four variations on Linnik's design are discussed, one of which avoids the use of transmitting optics and normal incidence reflections altogether and could therefore be used at ultraviolet or soft x-ray wavelengths.

An interferometer is described which allows in situ assessment and alignment of any image forming grazing incidence optic. The fringes are localized in the exit pupil of the X-ray telescope or microscope (either under manufacture or during use) and mark out in units of one wavelength the departure of an actual convergent image forming wavefront from the Gaussian reference sphere. In one variation of the principle the interferometer is comprised of one grazing incidence reflecting surface only. Visible interferograms are shown for two current applications.

We describe a new sounding rocket payload that has been developed for X-ray spectro-scopic studies of the Solar Corona. The instrument incorporates a grazing incidence Row-land mounted grating spectrograph and an extreme off axis paraboloic sector feed system to isolate regions of the sun of order 1 x 10 arc seconds in size. The focal surface of the spectrograph is shared by photographic and photoelectric detection systems, with the latter serving as a part of the rocket pointing system control loop. Fabrication and alignment of the optical system is based on high precision machining and mechanical metrology techniques. The spectrograph covers the 10 to 50 Angstrom interval and has a resolution of 16 milliangstroms in the current version. Modifications planned for future flights will improve the resolution to around 5 milliangstroms, permitting line widths to be measured. The instrument has been developed under the NASA Contract NAS2-9181 and the Lockheed Independent Research Program.

X-ray gratings have been developed for use in the wavelength region of 0.01-20 nm, where it is required to employ a grazing incidence configuration. The gratings have a rectangular profile and radiation is diffracted both from the tops and bottoms of the grooves. They therefore differ from blazed gratings, used at grazing incidence, in that a substantial portion of the grating participates in the diffraction process. A scalar diffraction theory has been developed which demonstrates that grating diffraction efficiency varies periodically with wavelength, pitch, groove depth and incidence angle. The theory can be used to optimize grating parameters for most efficient use in any selected region of the spectrum. The gratings are produced by processing a ruled 300 lines per millimetre master grating, so that surface profile defects introduced by ruling are eliminated. Grating performance has been assessed by means of a specially designed grating analyser in addition to spectrometers and a spectrograph. The experimental results are in qualitative agreement with theory. At very short wavelengths of 0.05 nm and grazing incidence angles of about 5', the diffraction efficiency in the first order is below 1 %. The efficiency rises rapidly to between 5 and 10 % at 0.15 nm and to 20 % in the 1 nm region where the incidence angles are typically a few degrees.

Holographically-formed X-ray reflection grating scan now be constructed with competitive groove efficiency to classically ruled types, down to a short wavelength diffracting limit of several angstroms.The gratings can be generated on any surface capable of intersecting the interference fringe pattern without shadowing. This fact alone brings several new X-ray optical design possibilities within reach, for example, by combining plane construction waves with steep aspheric substrates. The first order imaging theory of the grazing incidence mounting is discussed and compared to measured performance for aberration corrected stigmatic types.A new 5 meter spectrograph has also been constructed with applications in molecular chemistry, laser fusion research and synchro tronspectroscopy. The unit is available with fully prefocussed holographic and classical X-ray grating optics, and uses the precision miniature camera principle of fully interchangeable lenses, but applied, in this case to the entrance slit, grating and detector modules.