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OCR for page 8
3. THE LST SCIENTIFIC
CONFIGU RATION
The LST is planned as a long·lived orbiling astronomical observatory contain·
In& a 2.4-m Rltchey-Chretien telescope with a focal ratio of f/24. The on-axis
im:lgo is virtually diffrlletion.Jimit. Reaching the sky background will require the "stacking" of
ten or more Individual !mages by ground processing. A key feature of the
Focal Plane Camera is its ability to image a portion of the sky at the same
time any other scientific instrument on the LST is operatin&. This ·~seren·
dipity mode" will produce a collection of high-resolution Un~es that are
expected to reveal very distant cluster> of galaxies, as well as unsuSpected
objects in the ultraviolet.
The other scientific lnstrumenta are contained in four modular axial bays
on the optical and geome1ric axis or the telescope. Foremost amons these
instruments are the Faint Object Spectrograph (Fos) and the Faint Object
Can>era (Foe). The FOS i1 characterized by resolving powers of ~/A~ • 101
and 10' over the wavelength range 1200 A. to 8000 A.. in addition, the design
can incorporate a higher resolution mode ()./A>. • I!f). When ooupled to a
photon-counting detector,the FOS wUI be able to obtain the stigmatic >pee·
trum of a 25th·magnltude st•r (>./A>. • 101 ) in a IO·hour exposure with a
s:ignal·tc>noise ratio or aboul ) 0.
Tile FOC will have two modes of operation at focal ratios of f/48 and f/96.
8
OCR for page 9
Operated at f(96, It Is des~tned to retain the full resolvlna power of the tele·
ocope. For a detector litld of SOO X SOO pilteb, the correspond in& field of
new is small (II arc 10t square). A I().how cumulative txpowre with a
photon-countlna detector wiU yield 10 perocnt photometry on a 28th m"'l'l-
tude nar In a 1()()0,\ band pus. The reeommtnded pbococothode respoJUO
isS-20.
The othtr hilh-priority instlWIXIItl beinl eoruiclered for tht two remalnln&
ulal baya are the Planetary Camera and tht ttt Photomettr. The latttr C0¥<11
tht spectrwn frotn I to IOOOjUD with a ruoiYin&powtr ofabout )Jll). • 10,
obtained by a series of filttrs. A Si:As or Si:P photocoadiJCtor oo~n the
op«trum from I to 30 jllll, while thtlorctr wavelenatha art ruched by the
... of • bolomttcr. Much of the Itt Photomtttr Is cooled to liquid helium
ttrnperaturts by a dewu duigned to last at ltut 1 year In orbit . The t k
Photometer b diffroetion·limited at all wavtltrctlls.
The Plonttary Camero is a 400 X 400 pixel unintendfled onoloa camera
with a allleon photomt1rie rcaponat. When operated at f(96, lu field of view
b 9 arc 1ec square, which is adequate to obtain images of Uranus and Nep-
tune with •I-to-noise ratios in exCC$S of 100. When operated at f/24, the
Planetary Camera is capable of lma&lna hi&hJy rtd-chifted pi axles (z < I)
In one otbltal nl&ht.
F'mally, astrometric observations eon be readily performed ulin& tht fme
1111danoe S)'ll.cm.
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