DESCRIPTION |
Online Reference: http://wundow.wustl.edu/clbin/clsearch.pl
Instrument Overview
===================
The Ultraviolet/Visible Camera (UVVIS) has a catadioptic
telescope using fused silica lenses focused onto a
metachrome-coated charge couple device (CCD) imager. Active
wavelength response is limited on the short wavelength end by
the transmission of fused silica and the optical blur of the
lens. Wavelength response on the long end is limited by the
response of the CCD. Six spectral bands can be selected from a
filter wheel which is controlled through the same
serial-addressable synchronous interface (SASI).
The Thomson focal plane array (FPA) used is a frame-transfer
device, accomplishing electronic shuttering by rapidly shifting
the active pixel area into the storage area, pausing for the
13-bit programmable shuttering system integration time, then
rapidly shifting the captured image into a storage buffer from
which the image is read out. Post-FPA electronics allow three
gain states followed by 5 bits of offset that span 248 counts
in the analog regime to augment the basic 8-bit analog/digital
(A/D) conversion. Gain is A/D digitization noise limited, so
proper exposure is critical.
Working against the day side of the Moon as a target, typical
integration times were as short as several milliseconds in the
lowest gain state (1000 electrons/bit) near sub-solar
illumination points at the brighter spectral bands, increasing
to 40 msec near the polar regions in the mid-gain setting for
the weaker 415 and 1000 nanometers (nm) spectral bands. The
UVVIS performance specifications are shown below.
Scientific Objectives
=====================
The primary scientific objective of the UVVIS imaging
instrument was to support lunar mineral mapping investigations.
Pole-to-pole NADIR observations with solar phase angles kept to
less than 30 degrees at mid-latitudes were the predominant
viewing conditions during the two month systematic mapping
phase of the mission. The UVVIS and NIR cameras provided 100%
coverage of the lunar surface in 11 spectral bands ranging in
wavelength from 415 to 2690 nm. Image resolution ranges from
100 meters/pixel at periselene (-28 degrees south latitude for
the first month's observations, +28 degrees the second month)
to 400 meters/pixel at the poles.
Calibration
===========
The radiometric calibration converts the digitized signal
received from the camera (DN value) into a quantity that is
proportional to the radiance reaching the sensor. The
sensitivity of the CCD focal plane array varies across the
field of view but appears to be time invariant during the two
month lunar observation period. The UVVIS camera was
calibrated before launch. Laboratory observations of a flat
field under various operating temperatures and camera operation
modes provides information about the sensitivity of the camera
under expected spaceflight conditions. During inflight
operations, a variety of calibration observations were made
including images of stars with known radiance (Vega) and the
Apollo Landing sites where laboratory spectra of returned lunar
samples have been measured.
Geometric calibration removes optical distortions of the
imaging system. The geometric distortion of the UVVIS camera
has been shown to be minimal (maximum optical distortion does
not exceed 0.1 pixels) and can be satisfactorily modeled by a
radially dependent 2nd order polynomial.
For additional information on the geometric and radiometric
calibration of the Clementine imaging systems, contact the PDS
Imaging Node.
Operational Considerations
==========================
The pole-to-pole lunar observations provided scenes with a
broad range of viewing conditions, ranging from bright
observations near zero phase angle at the equator to very low
light-level observations at the poles. In order to properly
record an observation with an optimal signal-to-noise ratio it
is important to adequately fill the 8-bit (255 levels) dynamic
range of the A/D camera output. The integration time (exposure
time) and the gain and offset settings of the instrument were
adjusted to properly record each image. During the systematic
mapping, the gain state of the camera was normally set to 1 for
the mid-latitude observations and set to 2 (thereby increasing
the sensitivity of the A/D converter) at the higher latitudes.
Integration times were increased as observations approached the
poles. Lunar observations were broken into 10 latitude bins.
Each latitude bin contained fixed gain and offset modes and
integration times for each camera/filter combination.
For the UVVIS camera two observations were made in rapid
succession acquiring both high and low integration-time images
for the same scene. The multiple integration-time imaging was
designed to optimally record both maria materials (dark albedo
material optimally recorded by the high integration-time image)
and highland materials (high albedo materials optimally
recorded by the low integration-time image).
The Clementine orbit was designed to provide overlapping
coverage in both the down-track (~15% overlap) and cross-track
(~10% overlap at the equator) directions. The image overlap is
necessary to geometrically control images in cartographic
applications.
Operational Modes
=================
The UVVIS camera had three operating modes:
1. 13-bit programmable integration time. The range of
integration times (in microseconds) is given by: Integration
Time = [(N+3)*94.5 - 45, N=0,2,3...2**13)].
2. Gain Mode. The gain mode represents the multiplicative
constant applied to the image data passing through the A/D
converter. Three gain state settings were available (1,2,4)
although gain setting 4 was seldom used during lunar
observations.
3. Offset Mode. The offset mode represents the additive
constant applied to the image data passing through the A/D
converter. There were 14 offset mode settings (1-14) although
offset modes 1 and 6 were predominantly used during systematic
lunar observations.
Camera Specifications
=====================
Detectors
---------
Thomson Focal Plane Array
Type : Si Charge Coupled Device
Thomson TH7863-CRU-UV
Pixel format : 288x384
Pixel size : 23x23 microns
Readout rate : 4MHz
Wavelength Sensitivity : 0.3 to 1.1 microns
Field of view : 4.2 deg. x 5.6 deg.
Pixel IFOV : 255 microradians
Point spread : 1.1 to 1.5 pixels
Electronics
-----------
A/D resolution : 8 bits
Frame rate : 10 Hz
Readout time : 27.4 msec
Integration time : 0.2-733 msec
Digitization gain : 150,350,1000 electrons/count
Offset control : 248 gray levels
Power : 4.5 W
Filters
-------
Filter
Wheel Spectral
Position Band
-----------------------------------------------
A : 415nm (plus-or-minus 20 nm bw)
B : 750nm (plus-or-minus 5)
C : 900nm (plus-or-minus 10)
D : 950nm (plus-or-minus 15)
E : 1000nm (plus-or-minus 15)
F : 400 to 950nm broad band
Optics
------
Clear aperture : 46nm
Speed : F/1.96
Mechanical
----------
Mass : 410 grams
Size : 15.5cm x 11.7 cm x 10.4 cm
Filter Wheel System -
Type : 6 position, 90 deg. stepper
motor driven,
Hall Effect Position Sensors -
Step and Settle time : <250ms
Position repeatability : 10mr
Power : 0.15 W quiescent,
11.0 W stepping
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REFERENCES |
Kordas, J.R., I.T. Lewis, R.E. Priest, W.T. White, D.P. Nielsen, H. Park,
B.A. Wilson, M.J. Shannon, A.G. Ledebuhr, and L.D. Pleasance, UV/visible
Camera for the Clementine Mission, Proceedings of the Society of
Photo-optical Instrumentation Engineers (SPIE), 2478, pp. 175-186, 1995.
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