Figure III.C.1 Lunes are sketched on the celestial sphere. Shaded zone
is not allowed by Sun constraint.
The strategy developed to achieve the goals of multiple
survey coverage on various timescales divided the celestial sphere
into units of half overlapping "lunes" in the ecliptic
coordinate system (Lundy 1984).
Lunes were defined as the area
between two ecliptic meridians 30° apart
The lunes were "painted" by survey scans, one after
the other, as they passed through the viewing window of the telescope.
Figure III.C.2 illustrates the shape of a lune
a plane and, with a very exaggerated focal plane width, how it
was covered by different survey scans each at a fixed cone angle
from the Sun. The first scan in a lune was placed so that it
crossed the ecliptic at the lower longitude boundary of the lune.
Figure III.C.2 Half-overlapping scan swaths (highly exaggerated) fill
a lune with one hours-confirming layer.
Successive scans were laid down at increasing ecliptic longitudes,
each one shifted over by 14.23', that is by half the width of
the focal plane minus a safety margin to account for the pointing
limit cycle of the telescope. The overlap ensured that measurements
of the same area of sky were repeated within a few orbits (for
hours-confirmation) and that the "banana effect"
(Section III.B.8) was not too severe.
The criterion for hours-confirmation
was that the hours-confirming scans had to be made within three
SOPs (34-38 hours) of each other.
Figure III.C.3 A typical days survey coverage (clear regions at
approximately ecliptic longitudes 167° and 347°) is plotted
on a map of the sky in ecliptic coordinates. The two shaded regions
centered on ecliptic longitudes 90° and 270° are forbidden
by the Sun and Earth constraints.
Two lunes in opposite hemispheres were observed simultaneously,
one on the ascending side of the orbit and one on the descending
side. Figure III.C.3 shows a typical day's
survey coverage and
the regions forbidden by the constraints. After a lune was filled,
a second lune in the same hemisphere was started; it overlapped
half of the first lune, ensuring that another hour's-confirming
set of scans was repeated after about one to two weeks, thus providing
the required repetition on the time scale of weeks
Figure III.C.4 The lune coverage scheme is shown for the first two sets
of hours-confirming scans. Each line represents a single hours-confirming
coverage of an entire 30° lune (except short lines at beginning and
end which represent half-lune coverage).
The observing conditions were considerably worse during some
orbits than during others. Orbits that crossed the SAA or contained
a station prime pass were interrupted for significant amounts
of time. When a long interruption occurred, the continuation of
a survey scan was sometimes impossible and a small hole in the
coverage resulted. To minimize such events only the nine (out
of 14) orbits per day least affected by the SAA were used for
the survey scans
Figure III.C.5 A zone of half-circle scans is drawn on the
The survey strategy aimed for four coverages (two sets of
hours-confirming coverages) in the first six months and two coverages
(a third set of hours-confirming coverages) in the second six
months. Any time left over was used to recover survey observations
lost because of the various constraints, to make the necessary
calibration observations and to carry out additional, non-survey,
pointed observations to attain higher sensitivity or spatial resolution.
For the first two weeks of observations (February 10-23, 1983,
SOPs 31-57) half circle scans, which give redundant coverage in
the ecliptic polar areas (Fig. III.C.5), were
used for increased
initial coverage as insurance against an early failure of the
satellite. Subsequently, the more efficient lune method was used
for the rest of the first six months of the survey.
Survey observations were interrupted for up to l4 minutes during SAA passages even after selection of the least affected orbits. When the telescope entered the SAA during a survey scan its scanning motion was halted and it remained pointing at the same point on the celestial sphere until it emerged from the SAA when the scan was restarted with an overlap. During the SAA passage, "bias boost" was applied to the 60 and 100 µm detectors until about three minutes before exit. The internal reference sources were flashed just before entry and just after exit at the end and beginning of survey scans (Section III.B.3). Some SAA passages required so much time that the telescope would have violated the Earth infrared constraint (Section III.B.4) after SAA passage. In such cases it was necessary to leave a hole in the sky coverage and try to recover it with specially prepared short scans in the preceding or succeeding pair of SOPs. The failure to recover all of these holes contributed to the variable depth of sky coverage.
Figure III.C.6.1 The first hours-confirmed coverage is overlaid on a
map of the sky in ecliptic coordinates. The scans converge at the ecliptic
poles. Small, equally spaced holes in the ecliptic plane are due to the lunar
avoidance stragegy and represent gaps in the sky coverage used to generate
the extended emission images. The point source survey was not affected by
Jupiter was avoided by stopping a scan when it reached within
1° of the planet and side stepping by 1° for 2°
of scan before coming back to resume the original scan; hence
the Jupiter avoidance procedure left a 2° square hole on
the sky which needed to be recovered later in the survey.
Figure III.C.6.1-3 clearly show the three
square holes on the ecliptic
at longitude approximately 250° (RA about 17 hrs). Each
was left by one of the three sets of hours-confirming coverages.
There is no residual Jupiter hole when the effect of all the
coverage is added.
Figure III.C.6.2 Same as Figure III.C.6.1,
except for the second hours-confirming coverage.
To avoid the moon in the same way as Jupiter would have
left extremely large holes which would have been difficult to
fill. The policy adopted, therefore, was to stop the survey on
the moon's side of the orbit for the approximately three days
needed for the moon to pass through this approximately 40°
Figure III.C.6.3 Same as Figure III.C.6.1,
except for the third hours-confirming coverage.
To check the photometric calibration the internal reference sources were flashed at the beginning and end of every scan, including scans broken by the SAA. The internal reference sources were themselves regularly checked against an astronomical reference source (Section VI.A).
The scheduling program constrained survey scans to stop at the end of a half-orbit at one of the ecliptic poles. A side effect of this half-orbit design was that on occasions when the satellite had looked back in its orbit to cover a region of sky whose observation had been interrupted by a long SAA passage (Section III.C.4), the scan was cut short by reaching the end of its half-orbit, even though no other constraints had been violated.
Date SOP Event
(All dates are 1983 and given in GMT)
Launch 02h 17m
In Orbit Checkout (Cover on)
Outgassing of satellite
Cover ejection 19h 37m 31 Jan-8 Feb
In Orbit Checkout (Cover off) 9 Feb
SAA contour A (Fig. III.B.6) usage begins
Minisurvey layer 1 Hand made scans
Start first two hours-confirming
coverages using half circles.
Minisurvey layer 2 Hand made scans
Minisurvey layer 3 Hand made scans
Minisurvey layer 4a Hand made scans
Minisurvey layer 4b Hand made scans
Half circle method ended
Lune method started
Moon avoidance radius lowered
from 25° to 20°
SAA contour B (Fig. III.B.6) usage begins
End of first two hours-confirming coverages
Start third hours-confirming coverage
Moon avoidance radius lowered from 20 to 13°
Moon avoidance radius raised from 13 to 20°
First eclipse. Fallback to safety mode
Survey operations resumed 19h 40m
Liquid helium ran out 00h 16m
Last survey scan started 03h 34m
12 µm detector baselines saturated 09h 30m
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