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c~ Times-Bold~
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c~ FIRST~
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c~ !OptionFirst~
c~ first-button~
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c~ BACK PAGE~
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15 84 67 92
c~ !OptionBack~
c~ back-button~
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71 212
c~ NEXT PAGE~
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15 83 67 212
c~ !OptionNext~
c~ next-button~
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71 331
c~ LAST~
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15 38 67 331
c~ !OptionLast~
c~ last-button~
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c~ RETURN~
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15 61 25 10
c~ !OptionReturn~
c~ return-button~
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29 91
c~ TOPICS~
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15 55 25 91
c~ !OptionTopics~
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.PT
29 166
c~ INDEX~
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15 47 25 166
c~ !OptionIndex~
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.PT
29 233
c~ HOME~
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15 46 25 233
c~ !OptionHome~
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.PT
29 299
c~ SHOW~
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15 47 25 299
c~ !OptionShow~
c~ show-button~
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29 366
c~ QUIT~
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15 36 25 366
c~ !OptionQuit~
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29 422
c~ REFRESH~
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c~ !Show ~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Faint Object Camera - exploded view~
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18 295 618 10
c~ Faint Object Camera - exploded view~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Faint Object Camera~
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c~ Faint Object Camera~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Faint Object Spectrograph - Exploded view~
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c~ Faint Object Spectrograph - Exploded view~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Faint Object Spectrograph~
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c~ Faint Object Spectrograph~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Fine Guidance Sensors~
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c~ Fine Guidance Sensors~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Goddard Space Flight Center~
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c~ Goddard Space Flight Center~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ High Resolution Spectrograph - exploded view~
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c~ High Resolution Spectrograph - exploded view~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ High Resolution Spectrograph~
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c~ High Resolution Spectrograph~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ High Speed Photometer - exploded view~
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c~ High Speed Photometer - exploded view~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ High Speed Photometer~
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18 191 402 10
c~ High Speed Photometer~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Hubble Space Telescope - Main View~
.PS
18 294 378 10
c~ Hubble Space Telescope - Main View~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Optical Telescope Assembly - diagram~
.PS
18 305 354 10
c~ Optical Telescope Assembly - diagram~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Optical Telescope Assembly~
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18 221 330 10
c~ Optical Telescope Assembly~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Participating Organizations~
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c~ Participating Organizations~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Project Responsibilities~
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c~ Project Responsibilities~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Scientific Instruments~
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18 179 258 10
c~ Scientific Instruments~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Space Telescope Science Institute~
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c~ Space Telescope Science Institute~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Spin the Earth~
.PS
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c~ Spin the Earth~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Stop the Earth~
.PS
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c~ Stop the Earth~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Support Systems Module - Exploded View~
.PS
18 338 162 10
c~ Support Systems Module - Exploded View~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Support Systems Module~
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c~ Support Systems Module~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ The Space Telescope in Orbit~
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c~ The Space Telescope in Orbit~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Why the Hubble Space Telescope?~
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c~ Why the Hubble Space Telescope?~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Wide Field/Planetary Camera - exploded view~
.PS
18 365 66 10
c~ Wide Field/Planetary Camera - exploded view~
c~ default-button~
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c~ Times-Roman~
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c~ Times-Bold~
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c~ Wide Field/Planetary Camera~
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c~ Wide Field/Planetary Camera~
c~ default-button~
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c~ Times-Roman~
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c~ DefinitionPileID~
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c~ Definition~
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c~ DefinitionPileID~
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c~ Definition~
.SN
c~ Faint Object Camera~
.SN
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.SP
86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
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c~ Times-Italic~
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c~ An extremely sensitive camera capable of pinpointing and electronically intensifying dim~
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c~ objects.~
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c~ Times-Bold~
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c~ FULL ENTRY~
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c~ FULL ENTRY~
c~ full-entry-button~
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c~ ContentsPileID~
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c~ Faint Object Camera~
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646 544 0 0
c~ !Show ~
c~ show-background~
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c~ Times-Roman~
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c~ This instrument, being built by the~
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c~ Times-Bold~
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c~ European Space Agency~
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c~ European Space Agency~
c~ default-button~
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c~ Times-Roman~
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c~ ,~
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c~ uses the spatial resolution of the~
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c~ Times-Bold~
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c~ telescope~
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c~ telescope~
c~ default-button~
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c~ Times-Roman~
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c~ to capture images of very~
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c~ faint objects in the universe~
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c~ Times-Bold~
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c~ (fig. 1)~
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c~ (fig. 1)~
c~ default-button~
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c~ Times-Roman~
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c~ .~
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c~ It is expected to be able to detect stars as faint as the 28th~
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c~ magnitude and will easily pick out stars of magnitude 24, which is~
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c~ about the best a large ground observatory can now do. Magnitude is a~
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c~ designation of brightness - the lower the number, the brighter the~
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c~ object. The dimmest star the average person can see with the naked~
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c~ eye are magnitude 6. The planet Venus is magnitude -4.~
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c~ The Faint Object Camera has a basic focal ratio of f/96 and is~
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c~ capable of observing faint objects or extended structures near bright~
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c~ sources. This device will have four~
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c~ Times-Bold~
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c~ filter wheels~
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c~ filter wheels~
c~ default-button~
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c~ , each containing a~
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c~ variety of filters in 12 positions, which can be inserted in the optical~
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c~ path.~
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c~ The system works by gathering and focusing incoming feeble~
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c~ starlight on an electronic image intensifier. The intensifier's output is~
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c~ scanned by a vidicon camera tube and an image consisting of 250,000~
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c~ picture elements is obtained. Exposure times for very faint objects~
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c~ could run as long as ten hours.~
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c~ An f/48 focal ratio camera system will permit the camera to~
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c~ !Show ~
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c~ Times-Roman~
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c~ operate in a~
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c~ Times-Bold~
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c~ spectrographic~
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c~ spectrographic~
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c~ Times-Roman~
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c~ mode which is ideal for studying the~
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c~ structure and dynamics of the center regions of galaxies, the area~
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c~ where black holes are thought to occur. Thus the Faint Object~
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c~ Camera serves as a third, general-purpose spectrograph. This mode of~
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c~ operation will employ fourteen insertable filters.~
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c~ Faint Object Camera - exploded view~
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c~ !Full-Entry ~
c~ full-entry-background~
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c~ Times-Italic~
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c~ A diagram of the Faint Object Camera with labeled components.~
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86 544 0 0
c~ !Full-Entry ~
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c~ Times-Italic~
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c~ An instrument capable of analyzing the wavelength distribution, from ultraviolet through~
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c~ visible, of light from faint sources~
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c~ Times-Bold~
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c~ FULL ENTRY~
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c~ FULL ENTRY~
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c~ Faint Object Spectrograph~
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c~ !Show ~
c~ show-background~
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c~ Times-Roman~
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c~ The Faint Object Spectrograph~
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c~ Times-Bold~
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c~ (fig. 2)~
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c~ (fig. 2)~
c~ default-button~
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c~ Times-Roman~
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c~ is a versatile instrument~
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c~ that can obtain the spectra of extremely faint astronomical objects in~
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c~ the ultraviolet and visible wavebands. A spectrum is a distribution of~
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c~ colors, or wavelengths, created by passing a beam of light through a~
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c~ prism.~
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c~ A spectrum reveals the nature of the source we are viewing. We~
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c~ can tell whether it is hot or cold, dense or rarified, and even its~
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c~ chemical composition. Analysis of the spectrum also yield the~
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c~ remoteness and relative velocity of the object being studied.~
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c~ The spectrograph works by picking up the image of a star, galaxy,~
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c~ interstellar dust cloud or other object that appears on the~
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c~ Times-Bold~
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c~ telescope's~
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c~ telescope's~
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c~ focal plane as a point of light. Then, via a system of~
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c~ Times-Bold~
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c~ optical mirrors~
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c~ optical mirrors~
c~ default-button~
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c~ Times-Roman~
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c~ and~
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c~ Times-Bold~
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c~ gratings~
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c~ gratings~
c~ default-button~
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c~ Times-Roman~
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c~ that work like prisms, the light beam is spread out, from~
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c~ ultraviolet through the visible.~
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c~ The fanned-out beam is recorded on an imaging device called a~
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c~ Times-Bold~
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c~ digicon detector~
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c~ digicon detector~
c~ default-button~
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c~ Times-Roman~
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c~ , which counts the photons of light in each region of~
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c~ the beam. The resulting spectrogram is then transmitted to Earth for~
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c~ study.~
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c~ Faint Object Spectrograph - Exploded view~
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86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
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c~ Times-Italic~
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c~ A diagram of the Faint Object Spectrograph with labeled components.~
.PS
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c~ Times-Bold~
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44 10
c~ FULL ENTRY~
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15 92 40 10
c~ FULL ENTRY~
c~ full-entry-button~
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c~ Times-Italic~
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c~ Faint Object Spectrograph - Exploded view~
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646 544 0 0
c~ !Show ~
c~ show-background~
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c~ Times-Roman~
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17 10
c~ Faint Object Spectrograph - Exploded view~
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c~ Definition~
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c~ Definition~
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c~ Fine Guidance Sensors~
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86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
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c~ Times-Italic~
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c~ Instruments used to locate and lock on to a target object, maintaining position of the~
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c~ telescope relative to the target.~
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c~ Times-Bold~
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c~ FULL ENTRY~
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c~ FULL ENTRY~
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c~ Times-Italic~
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c~ Fine Guidance Sensors~
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646 544 0 0
c~ !Show ~
c~ show-background~
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c~ Times-Roman~
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c~ Because of the very high spatial reolution of the Space Telescope~
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c~ great pointing stability is required. Two of the fine guidance sensors~
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c~ will be used to locate and lock on to a target while the third is free to~
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c~ view and precisely measure the relative positions of other stars in the~
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c~ vicinity.~
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c~ The three fine guidance sensors are expected to produce distance~
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c~ measurements ten times more accurate than those done from~
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c~ Times-Bold~
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c~ Earth~
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c~ Earth~
c~ default-button~
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c~ Times-Roman~
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c~ .~
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c~ The sensors work through a complex system of mirrors and light~
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c~ detectors to locate the position of a star against a background of~
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c~ other stars. In measuring the distance to a star,~
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c~ Times-Bold~
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c~ ground controllers~
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c~ ground controllers~
c~ default-button~
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c~ Times-Roman~
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c~ will focus the sensors on a foreground star to transmit its position~
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c~ relative to the stars in the background. Similar measurements are~
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c~ made about six months later. Changes will indicate the distance of~
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c~ the star from the~
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c~ Times-Bold~
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c~ earth~
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c~ earth~
c~ default-button~
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c~ Times-Roman~
.UF
238 191
c~ .~
.PS
.EL
.SL
.EL
.SL
190 40
c~ The precise measurement of star positions is called astrometry.~
.PS
.EL
.SL
166 10
c~ Information provided by the fine guidance sensors will assist in~
.PS
.EL
.SL
142 10
c~ resolving the open-versus-closed universe question.~
.PS
.EL
.EP
c~ DefinitionPileID~
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c~ Definition~
.SN
c~ ContentsPileID~
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on
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c~ DefinitionPileID~
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c~ Definition~
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c~ Goddard Space Flight Center~
.SN
.ZP
.SP
86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
.PT
.SL
16
c~ Times-Italic~
.UF
65 10
c~ NASA center in Greenbelt, MD which will operate the Hubble Space Telescope once it is~
.PS
.EL
.SL
44 10
c~ in orbit.~
.PS
.EL
.SL
16
c~ Times-Bold~
.UF
23 10
c~ FULL ENTRY~
.PS
15 92 19 10
c~ FULL ENTRY~
c~ full-entry-button~
.PT
16
c~ Times-Italic~
.UF
.EL
.EP
c~ ContentsPileID~
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.SN
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c~ !Show ~
c~ show-background~
.PT
.SL
18
c~ Times-Roman~
.UF
.EL
.SL
.EL
.SL
574 40
c~ Once the Space Shuttle carries the~
.PS
18
c~ Times-Bold~
.UF
574 306
c~ Hubble Space Telescope~
.PS
18 190 570 306
c~ Hubble Space Telescope~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
574 501
c~ into~
.PS
.EL
.SL
550 10
c~ orbit, project personnel at Goddard will operate the satellite through~
.PS
.EL
.SL
526 10
c~ the Space Telescope Operations Control Center (STOCC), located at~
.PS
.EL
.SL
502 10
c~ Goddard.~
.PS
.EL
.SL
.EL
.SL
454 40
c~ The STOCC is the largest and most complex control center for a~
.PS
.EL
.SL
430 10
c~ scientific satellite to date, and will enable astronomers to utlilize the~
.PS
18
c~ Times-Bold~
.UF
.EL
.SL
406 10
c~ Hubble Space Telescope~
.PS
18 190 402 10
c~ Hubble Space Telescope~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
406 205
c~ much like a ground observatory. The~
.PS
.EL
.SL
382 10
c~ astronomers typically will work at the~
.PS
18
c~ Times-Bold~
.UF
382 298
c~ Space Telescope Science~
.PS
18 191 378 298
c~ Space Telescope Science~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
.EL
.SL
358 10
c~ Institute in Baltimore. They will send their observing requests to the~
.PS
.EL
.SL
334 10
c~ STOCC where the Hubble Space Telescope's controllers will program~
.PS
.EL
.SL
310 10
c~ the observations. The data and images obtained by the Telescope's~
.PS
.EL
.SL
286 10
c~ instruments then will be transmitted to the STOCC and on to the~
.PS
18
c~ Times-Bold~
.UF
.EL
.SL
262 10
c~ Space Telescope Science Institute~
.PS
18 266 258 10
c~ Space Telescope Science Institute~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
262 281
c~ , where astronomers will study~
.PS
.EL
.SL
238 10
c~ the information and present their findings to the world community.~
.PS
.EL
.SL
.EL
.SL
190 40
c~ It is expected that the STOCC will operate 24 hours per day and~
.PS
.EL
.SL
166 10
c~ provide a schedule of 3,500 hours of observing time annually. By~
.PS
.EL
.SL
142 10
c~ comparison, ground observatories, which can operate only during the~
.PS
.EL
.SL
118 10
c~ night, offer just 2000 hours of observing time per year.~
.PS
.EL
.EP
c~ DefinitionPileID~
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c~ Definition~
.SN
c~ ContentsPileID~
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c~ DefinitionPileID~
.ULP
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c~ Definition~
.SN
c~ High Resolution Spectrograph~
.SN
.ZP
.SP
86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
.PT
.SL
16
c~ Times-Italic~
.UF
65 10
c~ An instrument capable of obtaining the ultraviolet spectra of individual objects in~
.PS
.EL
.SL
44 10
c~ crowded fields.~
.PS
.EL
.SL
16
c~ Times-Bold~
.UF
23 10
c~ FULL ENTRY~
.PS
15 92 19 10
c~ FULL ENTRY~
c~ full-entry-button~
.PT
16
c~ Times-Italic~
.UF
.EL
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c~ ContentsPileID~
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c~ ContentsPileID~
.ULP
c~ ContentsPileID~
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c~ High Resolution Spectrograph~
.SN
.SP
646 544 0 0
c~ !Show ~
c~ show-background~
.PT
.SL
18
c~ Times-Roman~
.UF
622 10
c~ The High Resolution Spectrograph~
.PS
18
c~ Times-Bold~
.UF
622 275
c~ (fig. 3)~
.PS
18 51 618 275
c~ (fig. 3)~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
622 331
c~ will be able to use the full~
.PS
.EL
.SL
598 10
c~ resolving capability of the~
.PS
18
c~ Times-Bold~
.UF
598 209
c~ telescope~
.PS
18 71 594 209
c~ telescope~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
598 285
c~ to see much dimmer objects than~
.PS
.EL
.SL
574 10
c~ previous space-born instruments. Although it performs in much the~
.PS
.EL
.SL
550 10
c~ same way as the~
.PS
18
c~ Times-Bold~
.UF
550 136
c~ Faint Object Spectrograph~
.PS
18 213 546 136
c~ Faint Object Spectrograph~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
550 354
c~ , it will be much more~
.PS
.EL
.SL
526 10
c~ accurate because it will be using more light and resolving it into~
.PS
.EL
.SL
502 10
c~ much finer increments. The High Resolution Spectrograph will be~
.PS
.EL
.SL
478 10
c~ looking at only the ultraviolet region of the spectrum, wavelengths~
.PS
.EL
.SL
454 10
c~ that do not reach Earth. This ultraviolet region should provide the~
.PS
.EL
.SL
430 10
c~ most detailed chemical composition information yet obtained on~
.PS
.EL
.SL
406 10
c~ objects in space. The instrument's extremely fine resolution will~
.PS
.EL
.SL
382 10
c~ enable it to pick out individual stars in crowded fields. In addition,~
.PS
.EL
.SL
358 10
c~ binary stars that cannot be differentiated optically will be resolved so~
.PS
.EL
.SL
334 10
c~ that each star can be studied separately. The~
.PS
18
c~ Times-Bold~
.UF
334 349
c~ spectrograph~
.PS
18 104 330 349
c~ spectrograph~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
334 458
c~ will be~
.PS
.EL
.SL
310 10
c~ able to study such objects as supernovae, active galaxies, bright~
.PS
.EL
.SL
286 10
c~ quasars, and even phenomena in our own solar system such as~
.PS
.EL
.SL
262 10
c~ planetary atmospheres, auroral activity, and the presence of~
.PS
.EL
.SL
238 10
c~ deuterium in comets. Deuterium, thought to have been manufactured~
.PS
.EL
.SL
214 10
c~ during the Big Bang, occurs throughout the universe. If found in~
.PS
.EL
.SL
190 10
c~ comets, it will reveal more about the relation of our solar system to~
.PS
.EL
.SL
166 10
c~ the original cataclysmic explosion.~
.PS
.EL
.EP
c~ DefinitionPileID~
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c~ Definition~
.SN
c~ ContentsPileID~
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c~ DefinitionPileID~
.ULP
.ZP
c~ Definition~
.SN
c~ High Resolution Spectrograph - exploded view~
.SN
.ZP
.SP
86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
.PT
.SL
16
c~ Times-Italic~
.UF
65 10
c~ A diagram of the High Resolution Spectrograph with labeled components.~
.PS
.EL
.EP
c~ ContentsPileID~
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.ULP
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c~ Definition~
.SN
c~ High Speed Photometer~
.SN
.ZP
.SP
86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
.PT
.SL
16
c~ Times-Italic~
.UF
65 10
c~ Measures the brightness of an object, either within a particular wavelength or~
.PS
.EL
.SL
44 10
c~ throughout the entire spectrum; detects fluctuations.~
.PS
.EL
.SL
16
c~ Times-Bold~
.UF
23 10
c~ FULL ENTRY~
.PS
15 92 19 10
c~ FULL ENTRY~
c~ full-entry-button~
.PT
16
c~ Times-Italic~
.UF
.EL
.EP
c~ ContentsPileID~
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c~ ContentsPileID~
.ULP
c~ ContentsPileID~
.ULP
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c~ High Speed Photometer~
.SN
.SP
646 544 0 0
c~ !Show ~
c~ show-background~
.PT
.SL
18
c~ Times-Roman~
.UF
.EL
.SL
.EL
.SL
574 40
c~ The High Speed Photometer~
.PS
18
c~ Times-Bold~
.UF
574 258
c~ (fig. 4)~
.PS
18 51 570 258
c~ (fig. 4)~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
574 314
c~ is designed to provide~
.PS
.EL
.SL
550 10
c~ accurate observatons of the total light from an object in space, note~
.PS
.EL
.SL
526 10
c~ any fluctuations in brightness on a time scale down to microseconds,~
.PS
.EL
.SL
502 10
c~ and to detail any fine shapes or structures associated with the light~
.PS
.EL
.SL
478 10
c~ source. These measurements are made over a wide spectral interval,~
.PS
.EL
.SL
454 10
c~ including the ultraviolet.~
.PS
.EL
.SL
.EL
.SL
406 40
c~ It is the simplest instrument of the group, containing no moving~
.PS
.EL
.SL
382 10
c~ parts, and relies entirely on the pinpoint accuracy of the spacecraft's~
.PS
18
c~ Times-Bold~
.UF
.EL
.SL
358 10
c~ fine guidance sensors~
.PS
18 168 354 10
c~ fine guidance sensors~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
358 183
c~ to accomplish its work. After the light of a~
.PS
.EL
.SL
334 10
c~ star or other source is received, a~
.PS
18
c~ Times-Bold~
.UF
334 262
c~ detector~
.PS
18 65 330 262
c~ detector~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
334 332
c~ can measure either the~
.PS
.EL
.SL
310 10
c~ total brightness or the intensity of light within a particular portion of~
.PS
.EL
.SL
286 10
c~ the spectrum.~
.PS
.EL
.SL
.EL
.SL
238 40
c~ The High Speed Photometer, in addition, will transmit accurate~
.PS
.EL
.SL
214 10
c~ information on fluctuation in brightness over time. Detection of~
.PS
.EL
.SL
190 10
c~ rapidly spinning neutron or other compact stars will be possible, as~
.PS
.EL
.SL
166 10
c~ well as detailed data on the shape and structure of the fine spikes or~
.PS
.EL
.SL
142 10
c~ flares often associated with such compact objects.~
.PS
.EL
.SL
.EL
.SL
94 40
c~ The instrument will also be of special value to astronomers in~
.PS
.EL
.SL
70 10
c~ establishing calibration standards for faint stellar objects.~
.PS
.EL
.EP
c~ DefinitionPileID~
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.SN
c~ ContentsPileID~
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c~ DefinitionPileID~
.ULP
.ZP
c~ Definition~
.SN
c~ High Speed Photometer - exploded view~
.SN
.ZP
.SP
86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
.PT
.SL
16
c~ Times-Italic~
.UF
65 10
c~ A diagram of the High Speed Photometer with components labeled.~
.PS
.EL
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.ZP
c~ Definition~
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c~ Hubble Space Telescope - Main View~
.SN
.ZP
.SP
86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
.PT
.SL
16
c~ Times-Italic~
.UF
65 10
c~ A diagram of the telescope with major components labelled.~
.PS
.EL
.SL
16
c~ Times-Bold~
.UF
44 10
c~ FULL ENTRY~
.PS
15 92 40 10
c~ FULL ENTRY~
c~ full-entry-button~
.PT
16
c~ Times-Italic~
.UF
.EL
.EP
c~ ContentsPileID~
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.ULP
c~ ContentsPileID~
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c~ Hubble Space Telescope - Main View~
.SN
.SP
646 544 0 0
c~ !Show ~
c~ show-background~
.PT
.SL
18
c~ Times-Roman~
.UF
.EL
.SL
177 1
c~ telescope - main view~
.PP
468 564 177 1
c~ Faint Object Spectrograph - Exploded view~
c~ Main view -  shape FOS~
.PT
468 564 177 1
c~ Faint Object Camera - exploded view~
c~ Main view -  shape FOC~
.PT
468 564 177 1
c~ High Resolution Spectrograph - exploded view~
c~ Main view -  shape HRS~
.PT
468 564 177 1
c~ High Speed Photometer - exploded view~
c~ Main view -  shape HSP~
.PT
468 564 177 1
c~ Wide Field/Planetary Camera - exploded view~
c~ Main view -  shape WFPC~
.PT
468 564 177 1
c~ Optical Telescope Assembly - diagram~
c~ Main view -  shape OTA~
.PT
468 564 177 1
c~ Fine Guidance Sensors~
c~ Main view -  shape FGS~
.PT
468 564 177 1
c~ High Speed Photometer - exploded view~
c~ Main view -  shape HSP~
.PT
468 564 177 1
c~ Faint Object Spectrograph~
c~ Main view -  word Faint Object Spectrograph~
.PT
468 564 177 1
c~ High Resolution Spectrograph~
c~ Main view -  word High Resolution Spectrograph~
.PT
468 564 177 1
c~ High Speed Photometer~
c~ Main view -  word High Speed Photometer~
.PT
468 564 177 1
c~ Faint Object Camera~
c~ Main view -  word Faint Object Camera~
.PT
468 564 177 1
c~ Wide Field Planetary Camera~
c~ Main view -  word Wide Field Planetary Camera~
.PT
468 564 177 1
c~ Support Systems Module~
c~ Main view -  word Support System module~
.PT
.EL
.EP
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.SN
c~ ContentsPileID~
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.ULP
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c~ Definition~
.SN
c~ Optical Telescope Assembly~
.SN
.ZP
.SP
86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
.PT
.SL
16
c~ Times-Italic~
.UF
65 10
c~ The central component of the Hubble Space Telescope, consisting of a 94 inch (2.4 m)~
.PS
.EL
.SL
44 10
c~ reflecting Cassegrain telescope and supporting structures.~
.PS
.EL
.SL
16
c~ Times-Bold~
.UF
23 10
c~ FULL ENTRY~
.PS
15 92 19 10
c~ FULL ENTRY~
c~ full-entry-button~
.PT
16
c~ Times-Italic~
.UF
.EL
.EP
c~ ContentsPileID~
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c~ ContentsPileID~
.ULP
c~ ContentsPileID~
.ULP
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c~ Optical Telescope Assembly~
.SN
.SP
646 544 0 0
c~ !Show ~
c~ show-background~
.PT
.SL
18
c~ Times-Roman~
.UF
622 10
c~ The Optical Telescope Assembly~
.PS
18
c~ Times-Bold~
.UF
622 261
c~ (fig. 5)~
.PS
18 51 618 261
c~ (fig. 5)~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
622 317
c~ will mount a 94-inch (2.4~
.PS
.EL
.SL
598 10
c~ m) reflecting cassegrain-type telescope, consisting of a paraboloidal~
.PS
.EL
.SL
574 10
c~ primary mirror and a hyperboloidal secondary mirror. The optical~
.PS
.EL
.SL
550 10
c~ effect is the same as that of a telephoto lens. Light beams enter the~
.PS
.EL
.SL
526 10
c~ open end of the telescope and strike the~
.PS
18
c~ Times-Bold~
.UF
526 312
c~ primary mirror~
.PS
18 124 522 312
c~ primary mirror~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
526 441
c~ at the rear.~
.PS
.EL
.SL
502 10
c~ The parabolic shape of the primary mirror causes the beams to~
.PS
.EL
.SL
478 10
c~ converge upon the~
.PS
18
c~ Times-Bold~
.UF
478 153
c~ secondary mirror~
.PS
18 138 474 153
c~ secondary mirror~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
478 296
c~ . The secondary mirror's~
.PS
.EL
.SL
454 10
c~ hyperbolic shape aligns the beams in parallel and bounces them back~
.PS
.EL
.SL
430 10
c~ through a hole in the center of the primary mirror. The~
.PS
18
c~ Times-Bold~
.UF
.EL
.SL
406 10
c~ scientific instruments~
.PS
18 173 402 10
c~ scientific instruments~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
406 188
c~ are positioned behind the primary mirror~
.PS
.EL
.SL
382 10
c~ where they can be moved into the path of the reflected light. The~
.PS
18
c~ Times-Bold~
.UF
.EL
.SL
358 10
c~ primary mirror~
.PS
18 124 354 10
c~ primary mirror~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
358 139
c~ is made of ultra-low expansion titanium silicate~
.PS
.EL
.SL
334 10
c~ glass with an aluminum-magnesium fluoride coating. To reduce~
.PS
.EL
.SL
310 10
c~ weight, the front and back plates are fused to a honeycomb core. The~
.PS
.EL
.SL
286 10
c~ mirror will be heated during operation to 70 degrees F to minimize~
.PS
.EL
.SL
262 10
c~ variations from its original accuracy. This heat will come from~
.PS
.EL
.SL
238 10
c~ electrical strip heaters, powered by the~
.PS
18
c~ Times-Bold~
.UF
238 303
c~ solar arrays~
.PS
18 94 234 303
c~ solar arrays~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
238 402
c~ , which will~
.PS
.EL
.SL
214 10
c~ radiate to the back of the mirror. The~
.PS
18
c~ Times-Bold~
.UF
214 300
c~ orientation~
.PS
18 89 210 300
c~ orientation~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
214 394
c~ and~
.PS
18
c~ Times-Bold~
.UF
.EL
.SL
190 10
c~ stabilization control~
.PS
18 160 186 10
c~ stabilization control~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
190 175
c~ system of the telescope can point with an~
.PS
.EL
.SL
166 10
c~ accuracy of 0.01 arc second and can hold onto a target for extended~
.PS
.EL
.SL
142 10
c~ periods within 0.007 arc-second. This angle would translate into a~
.PS
.EL
.SL
118 10
c~ distance slightly larger than the diameter of a dime if the telescope~
.PS
.EL
.SL
94 10
c~ were 500 miles away. Such accuracy is necessary in order to study~
.PS
.EL
.SL
70 10
c~ very faint objects, some of which require exposures of 10 hours or~
.PS
.EL
.SL
46 10
c~ more. The telescope can be turned and changed from one direction to~
.PS
.EL
.SL
22 10
c~ another at a rate of 90 degrees in 20 minutes.~
.PS
.EL
.EP
c~ DefinitionPileID~
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.ZP
c~ Definition~
.SN
c~ ContentsPileID~
.ULP
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on
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c~ DefinitionPileID~
.ULP
.ZP
c~ Definition~
.SN
c~ Optical Telescope Assembly - diagram~
.SN
.ZP
.SP
86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
.PT
.SL
16
c~ Times-Italic~
.UF
65 10
c~ A diagram of the Optical Telescope Assembly.~
.PS
.EL
.SL
16
c~ Times-Bold~
.UF
44 10
c~ FULL ENTRY~
.PS
15 92 40 10
c~ FULL ENTRY~
c~ full-entry-button~
.PT
16
c~ Times-Italic~
.UF
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c~ For a description of the participating organizations and their responsibilities, see article.~
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c~ The~
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c~ Hubble Space Telescope~
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c~ is truly a cooperative effort~
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c~ .~
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c~ Each of the following organizations has distinct responsibilities:~
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c~ - NASA's Office of Space Science and Applications,~
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c~ Space Telescope Program.~
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c~ - Marshall Space Flight Center, Huntsville, AL, is the leading~
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c~ NASA center for the Hubble Space Telescope, providing day-to-day~
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c~ management of the project. Marshall also directs the construction~
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c~ and integration of the telescope and spacecraft systems.~
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c~ for development of the Telescope's four American-contributed~
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c~ European nations, is responsible for developing the~
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c~ , one of five~
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c~ aboard~
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c~ the Hubble Space Telescope. ESA is also developing the~
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c~ which power the spacecraft and will provide a small resident staff to~
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c~ Space Telescope Science Institute~
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c~ in Baltimore.~
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c~ France, West Germany, Ireland, Italy, the Netherlands, Spain,~
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c~ include Austria and Norway.~
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c~ - Johnson Space Center in Houston, Texas, will launch the~
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c~ - Kennedy Space Center, Florida, is also involved in Space~
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c~ Shuttle launch operations.~
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c~ - The Association of Universities for Research in Astronomy~
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c~ contract to NASA's~
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c~ includes: University of Arizona, California Institute of Technology,~
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c~ University of California at Berkeley, University of Chicago,~
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c~ University of Colorado, Harvard, University of Hawaii, University of~
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c~ Illinois, Indiana University, Johns Hopkins University, Massachusetts~
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c~ Institute of Technology, University of Michigan, Ohio State,~
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c~ Princeton, University of Texas at Austin, University of Wisconsin,~
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c~ and Yale.~
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c~ Support Systems Module~
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c~ Optical Telescope Assembly~
c~ resp. - word optical telescope assembly~
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c~ Faint Object Camera~
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c~ The wide field/planetary and faint object cameras, the faint object and high resolution~
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c~ The five scientific instruments, four American and one European,~
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c~ are located behind the primary mirror, at the focal plane, where they~
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c~ can pick up light reflected from the telescope. They are the~
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c~ , the~
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c~ , the latter provided by the~
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c~ . In addition, the~
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c~ instrument. Each instrument is housed in a separate module and will~
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c~ The center for scientific activities associated with the Hubble Space Telescope.~
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c~ The Space Telescope Science institute, opened in 1983 and operated~
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c~ , will be the center~
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c~ for all aspects of science activities associated with the observatory.~
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c~ The Space Telescope Science Institute will manage the planning and~
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c~ implementation of research projects, provide a facility for~
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c~ astronomers using the Hubble Space Telescope, and collect, analyze,~
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c~ and disseminate the data obtained. Following a nationwide~
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c~ competition, management responsibility for the Space Telescope~
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c~ Science Institute was given to the assoication of Universities for~
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c~ , a federation of 17 major U.S.~
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c~ independent agent outside of NASA which is directly responsible to~
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c~ the community of current and potential users.~
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c~ also manages~
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c~ major observatories at Kitt Peak in Arizona, Sacramento Peak in~
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c~ New Mexico, and Cerro Tololo in Chile.~
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c~ The structures and equipment which provide power, communications, orientation, and~
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c~ control to the Space Telescope.~
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c~ The Support Systems Module~
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c~ (fig. 7)~
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c~ (fig. 7)~
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c~ will enclose the~
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c~ Optical Telescope Assembly~
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c~ and~
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c~ Times-Bold~
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c~ scientific instruments~
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c~ scientific instruments~
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c~ and will~
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c~ provide all interfaces with the Shuttle orbiter.~
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c~ The module has four main sections: the light shield, the forward~
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c~ shell, the equipment section, and the aft shroud. These four pieces fit~
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c~ together like stacked cannisters to enclose the telescope assembly and~
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c~ scientific instruments.~
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c~ The~
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c~ aperture door~
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c~ aperture door~
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c~ , which also serves as a light shield, is located~
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c~ at the front of the Support Systems Module. The telescope must be~
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c~ shielded from the Sun, Earth, and Moon so that the scientific~
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c~ instruments are not damaged by a flood of light. While in operation,~
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c~ the telescope will not be turned to within 50 degrees of the Sun,~
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c~ precluding observations of the planet Mercury. Internal~
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c~ baffles~
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c~ in the~
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c~ Support Systems Module door and just below the~
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c~ secondary mirror~
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c~ prevent scattered light from degrading the focal plane image.~
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c~ Just behind the light shield and the forward shell is the equipment~
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c~ section of the spacecraft. This doughnut-shaped section is made up of~
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c~ 10 compartments that house the electronic and control modules.~
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c~ Access to many of these modules will be easy as most compartments~
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c~ open from the outside via a hatch or access door. An astronaut can~
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c~ open a hatch, disconnect a module from its plug-in compartment,~
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c~ and insert a new module, all without disturbing the other instruments~
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c~ in the spacecraft.~
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c~ The~
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c~ Times-Bold~
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c~ aft~
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c~ aft~
c~ default-button~
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c~ Times-Roman~
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c~ shroud fits over the section containing the~
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c~ Times-Bold~
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c~ scientific instruments~
c~ default-button~
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18
c~ Times-Roman~
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c~ and the~
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18
c~ Times-Bold~
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c~ fine guidance sensors~
.PS
18 168 570 250
c~ fine guidance sensors~
c~ default-button~
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c~ Times-Roman~
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c~ . Access~
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c~ covers on this shroud enable astronauts to get at the instruments and~
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c~ sensors for removal or maintenance.~
.PS
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c~ Handrails and portable foot restraints are fixed on the external~
.PS
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c~ surface to permit astronauts to perform their maintenance and~
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c~ refurbishment tasks. Four~
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18
c~ Times-Bold~
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c~ magnetic torquers~
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c~ magnetic torquers~
c~ default-button~
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c~ , also located on the~
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c~ shroud exterior, work with four reaction wheels within the Support~
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c~ Systems Module equipment section to control the spacecraft's~
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c~ orientation in space. The magnetic torquers are magnetized metal~
.PS
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c~ rods controlled by an onboard computer. A change in their position~
.PS
.EL
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c~ causes the spacecraft to re-align itself in relation to the Earth`s~
.PS
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c~ magnetic field.~
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c~ Electrical power is supplied by onboard batteries, which are~
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c~ charged by the two~
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c~ Times-Bold~
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c~ solar arrays~
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c~ solar arrays~
c~ default-button~
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c~ Times-Roman~
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c~ during the sunlit portion of the~
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c~ telescope's orbit. An average of 2.4 kw is needed to operate the~
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c~ spacecraft and its instruments.~
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c~ DefinitionPileID~
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c~ DefinitionPileID~
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c~ Definition~
.SN
c~ Support Systems Module - Exploded View~
.SN
.ZP
.SP
86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
.PT
.SL
16
c~ Times-Italic~
.UF
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c~ A diagram of the Support Systems Module with components labeled. (the picture doesn't~
.PS
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c~ exist...)~
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c~ DefinitionPileID~
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c~ Definition~
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c~ The Space Telescope in Orbit~
.SN
.ZP
.SP
86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
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16
c~ Times-Italic~
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c~ An artist's conception of the space telescope in orbit.~
.PS
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c~ Times-Bold~
.UF
44 10
c~ FULL ENTRY~
.PS
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c~ FULL ENTRY~
c~ full-entry-button~
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c~ Times-Italic~
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c~ The Space Telescope in Orbit~
.SN
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c~ !Show ~
c~ show-background~
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c~ Times-Roman~
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c~ orbital view~
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509 533 132 5
c~ Hubble Space Telescope - Main View~
c~ orbital view - shape telescope~
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32
c~ Times-Bold~
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c~ Diagram~
.PS
40 123 86 85
c~ Hubble Space Telescope - Main View~
c~ default-button~
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94 296
c~ Introduction~
.PS
40 180 86 296
c~ Introduction article~
c~ default-button~
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c~ Definition~
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c~ Why the Hubble Space Telescope?~
.SN
.ZP
.SP
86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
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c~ Times-Italic~
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c~ A short description of the telescope and its purpose.~
.PS
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16
c~ Times-Bold~
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c~ FULL ENTRY~
.PS
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c~ FULL ENTRY~
c~ full-entry-button~
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c~ Why the Hubble Space Telescope?~
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c~ !Show ~
c~ show-background~
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c~ Times-Roman~
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.SL
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c~ Imagine trying to see the clouds from the bottom of a muddy~
.PS
.EL
.SL
550 10
c~ pond. That is how astronomers describe their view of the stars and~
.PS
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.SL
526 10
c~ planets through the Earth's atmosphere. As advanced as~
.PS
.EL
.SL
502 10
c~ astronomical technology has become, our capabilities will be forever~
.PS
.EL
.SL
478 10
c~ limited by the turbulence and brightness of our atmosphere. Even the~
.PS
.EL
.SL
454 10
c~ finest ground observatories, such as the one at Mt. Palomar,~
.PS
.EL
.SL
430 10
c~ California, are restricted by these conditions. In addition, the~
.PS
.EL
.SL
406 10
c~ selective absorption of the atmosphere, which lets in visible light and~
.PS
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.SL
382 10
c~ radio waves emitted by stars and planets, but excludes most other~
.PS
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358 10
c~ forms of energy, limits our knowledge of celestial bodies.~
.PS
.EL
.SL
.EL
.SL
310 40
c~ To open the universe to observation in infrared, ultraviolet,~
.PS
.EL
.SL
286 10
c~ x-ray, gamma-ray, and cosmic ray energies, NASA launched~
.PS
.EL
.SL
262 10
c~ numerous satellites, each helping to explain different processes behind~
.PS
.EL
.SL
238 10
c~ astronomical phenomena. But, to date, the value of these orbiting~
.PS
.EL
.SL
214 10
c~ observatories has been limited by their relatively small size and~
.PS
.EL
.SL
190 10
c~ limited spectral capability.~
.PS
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.SL
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142 40
c~ Now, for the first time, a ground-sized observatory will be placed~
.PS
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.SL
118 10
c~ in orbit to view the universe in visible and ultraviolet light~
.PS
.EL
.SL
94 10
c~ unobscured by Earth's atmosphere.~
.PS
.EL
.SL
.EL
.SL
46 40
c~ Called the~
.PS
18
c~ Times-Bold~
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46 122
c~ Edwin P. Hubble Space Telescope~
.PS
18 266 42 122
c~ Edwin P. Hubble Space Telescope~
c~ default-button~
.PT
18
c~ Times-Roman~
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46 393
c~ , the new~
.PS
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c~ observatory is a NASA-wide and international~
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18
c~ Times-Bold~
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22 368
c~ cooperative effort~
.PS
18 139 18 368
c~ cooperative effort~
c~ default-button~
.PT
18
c~ Times-Roman~
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22 512
c~ .~
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c~ !Show ~
c~ show-background~
.PT
.SL
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c~ Times-Roman~
.UF
622 10
c~ Its name honors Edwin P. Hubble (1889-1953), who discovered that~
.PS
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.SL
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c~ the universe extends far beyond the Milky Way galaxy.~
.PS
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.SL
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c~ The~
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18
c~ Times-Bold~
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550 75
c~ Hubble Space Telescope~
.PS
18 190 546 75
c~ Hubble Space Telescope~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
550 270
c~ will weigh about 25,000 pounds~
.PS
.EL
.SL
526 10
c~ (11,300 kg) and will have a length of 43 feet (13.1 m) and a diameter~
.PS
.EL
.SL
502 10
c~ of 14 feet (4.26 m). Its major components are an~
.PS
18
c~ Times-Bold~
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c~ optical telescope assembly~
.PS
18 206 474 10
c~ optical telescope assembly~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
478 221
c~ , five~
.PS
18
c~ Times-Bold~
.UF
478 263
c~ scientific instruments~
.PS
18 173 474 263
c~ scientific instruments~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
478 441
c~ , and a~
.PS
18
c~ Times-Bold~
.UF
.EL
.SL
454 10
c~ support systems module~
.PS
18 193 450 10
c~ support systems module~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
454 208
c~ .~
.PS
.EL
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c~ DefinitionPileID~
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c~ Definition~
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c~ ContentsPileID~
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c~ DefinitionPileID~
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c~ Definition~
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c~ Wide Field/Planetary Camera~
.SN
.ZP
.SP
86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
.PT
.SL
16
c~ Times-Italic~
.UF
65 10
c~ A camera that can take photographs either in "wide-field" or "planetary" mode. The~
.PS
.EL
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c~ resulting images are transmitted by radio to Earth.~
.PS
.EL
.SL
16
c~ Times-Bold~
.UF
23 10
c~ FULL ENTRY~
.PS
15 92 19 10
c~ FULL ENTRY~
c~ full-entry-button~
.PT
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c~ Times-Italic~
.UF
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c~ ContentsPileID~
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c~ ContentsPileID~
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c~ Wide Field/Planetary Camera~
.SN
.SP
646 544 0 0
c~ !Show ~
c~ show-background~
.PT
.SL
18
c~ Times-Roman~
.UF
.EL
.SL
.EL
.SL
574 40
c~ This instrument~
.PS
18
c~ Times-Bold~
.UF
574 165
c~ (fig. 8)~
.PS
18 51 570 165
c~ (fig. 8)~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
574 221
c~ can operate in one of two modes. In~
.PS
.EL
.SL
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c~ "wide field" mode, its focal ratio of f/12.9 will permit examination of~
.PS
.EL
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c~ large areas of space, leading to more accurate plotting of the spatial~
.PS
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c~ relationships of distant objects such as galaxies and quasars.~
.PS
.EL
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c~ High-resolution images of planets within our solar system can be~
.PS
.EL
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454 10
c~ obtained by the planetary camera, which has a focal ratio of f/30.~
.PS
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c~ Images telemetered to Earth by radio will be far better than~
.PS
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c~ pictures produced by ground-based cameras. Pictures of Jupiter, for~
.PS
.EL
.SL
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c~ example, will be comparable to those taken by the two Voyager~
.PS
.EL
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334 10
c~ spacecraft in 1979. Pictures of more distant planets will not be as~
.PS
.EL
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c~ clear as those taken by Voyager, but will be far superior to those~
.PS
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c~ taken from Earth.~
.PS
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238 40
c~ The camera consists of a complex system of instruments and~
.PS
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c~ mirrors. The field of view is split by a~
.PS
18
c~ Times-Bold~
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c~ pyramidal mirror~
.PS
18 141 210 295
c~ pyramidal mirror~
c~ default-button~
.PT
18
c~ Times-Roman~
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214 441
c~ into four~
.PS
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c~ separate areas which are focused onto four~
.PS
18
c~ Times-Bold~
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c~ charge-coupled devices~
.PS
18 183 186 335
c~ charge-coupled devices~
c~ default-button~
.PT
18
c~ Times-Roman~
.UF
190 523
c~ .~
.PS
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c~ These devices have been designed to receive light of low intensity at~
.PS
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c~ very high resolution. A portion of the image is received on each~
.PS
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c~ target plate and is subdivided into 640,000 picture elements (pixels).~
.PS
.EL
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c~ The light intensities of each pixel are transmitted to Earth via~
.PS
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c~ telemetry signals for assembly into images for study. Images can be~
.PS
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c~ created from different spectral bands by directing the light through~
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c~ any one of 50 spectral filters within the camera.~
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c~ Definition~
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c~ Wide Field/Planetary Camera - exploded view~
.SN
.ZP
.SP
86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
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c~ Times-Italic~
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c~ A diagram of the Wide Field and Planetary Camera with components labeled.~
.PS
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c~ Times-Bold~
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c~ FULL ENTRY~
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15 92 40 10
c~ FULL ENTRY~
c~ full-entry-button~
.PT
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c~ ContentsPileID~
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c~ Wide Field/Planetary Camera - exploded view~
.SN
.SP
646 544 0 0
c~ !Show ~
c~ show-background~
.PT
.SL
18
c~ Times-Roman~
.UF
171 10
c~ Wide Field and Planetary Camera - diagram~
.PP
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18
c~ Times-Bold~
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c~ Wide Field/Planetary Camera~
.PS
18 238 147 10
c~ Wide Field/Planetary Camera~
c~ default-button~
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18
c~ Times-Roman~
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c~ Definition~
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c~ Definition~
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c~ Spin the Earth~
.SN
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86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
.PT
.SL
16
c~ Times-Italic~
.UF
21 10
c~ earth~
.PP
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16
c~ Times-Bold~
.UF
4 10
c~ FULL ENTRY~
.PS
15 92 0 10
c~ FULL ENTRY~
c~ full-entry-button~
.PT
16
c~ Times-Italic~
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c~ Spin the Earth~
.SN
.SP
646 544 0 0
c~ !Show ~
c~ show-background~
.PT
.SL
18
c~ Times-Roman~
.UF
622 10
c~ Spin the Earth!~
.PS
581 140
c~ earth~
.PP
55 64 581 140
c~ Stop the Earth~
c~ spin~
.PT
.EL
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c~ DefinitionPileID~
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c~ Definition~
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c~ Definition~
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c~ Stop the Earth~
.SN
.ZP
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86 544 0 0
c~ !Full-Entry ~
c~ full-entry-background~
.PT
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16
c~ Times-Italic~
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c~ earth~
.PP
.EL
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16
c~ Times-Bold~
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4 10
c~ FULL ENTRY~
.PS
15 92 0 10
c~ FULL ENTRY~
c~ full-entry-button~
.PT
16
c~ Times-Italic~
.UF
.EL
.EP
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c~ ContentsPileID~
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c~ ContentsPileID~
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c~ Stop the Earth~
.SN
.SP
646 544 0 0
c~ !Show ~
c~ show-background~
.PT
.SL
18
c~ Times-Roman~
.UF
622 10
c~ Stop the Earth!~
.PS
581 140
c~ earth~
.PP
55 64 581 140
c~ Spin the Earth~
c~ circle-button~
.PT
622 214
c~ I want to get off!~
.PS
.EL
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c~ Definition~
.SN
c~ ContentsPileID~
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\ End compilation of HyperTIES Space Telescope Demo.