Full disk images
Almost all full disk images were taken with slit 2 (1"x300") on Detector A.
(Only images of the S VI time series rastered after 23 Sep 96 were taken on
Detector B.) Their TIF files have 4.2 MB size. The Sun is centered in the
middle of the images. Missing parts of the disk are restored in grey shade up
to the chromospheric limb. Lines below 790 Å are in second order.
The lists give the line, formation temperature, exposure time, raster step size,
photocathode, spectral window (t: complete spectral window was transmitted to
ground, i: spectral window was integrated on-board), and start date/time. -
The Cont 977 image is dominated by blends from C III;
the Cont 1540 image is somewhat blended with the blue wing of Ne VIII. -
The Cont 812 image also contains Cont 804. - The S VI 944 line is blended with
Si VIII. - The first two He I scans of 26 Jun 96 were interrupted in the middle.
A series of 15 images from June 1996 were binned on-board (3 spatial pixels).
TIF images were extended to 1"x1" pixels. - The Fe II 1559 line is blended
with Si I and
relatively strong continuum. - The O V 629 line was originally blended with
Si I, but this effect could be removed. - The scan of 15 Jun 96 was interrupted
15 minutes early because of a Joint Observational Program.
A series of 37 studies was run between March and October 1996, rastering the
full disk in H I and S VI in full spatial resolution. The study was initiated
by Philippe Lemaire (IAS). Usually, the lines H I Ly e 937, S VI 933 and
S VI 944 were observed; their intensities were integrated on board.
Of these studies, one (e.g., 12 May 96) should be used to show full disk plus
details, one (21 Jun 96) has almost 50% data faults, another one (28 Aug 96)
was interrupted in the middle. The remaining 34 studies could be demonstrated
by showing two out of three full disk images each, not necessarily the same two
lines each time.
Whole Sun Month
Between 10 Aug 96 and 09 Sep 96, SUMER study #579 was executed 34 times on
various locations (NE, NW, SE, SW, polar coronal hole boundary, off-limb,
streamer, equatorial coronal hole). The studies were initiated by Don Hassler
(SwRI). Each one consists of an (approx.) 720"x300" scan with a raster step of
1.5" and an exposure time of 60 s in four different spectral windows of 50 px
simultaneously: Around 1238.82 (=> N V), around 1242.01 (=> Fe XII and Cont
1241), around 1249.88 (=> C I, Mg X, Si II, S II), and around 1259.46
(=> O V). The first interval also contains some continuum, but this is sometimes
blended by the very strong and dynamic N V line. The second interval also
contains a N V line, but this is not used. The Fe XII is weak and blended
with chromospheric lines, but the blend could be resolved. The continuum
at 1241 seems to be the most pure of all four intervals, except for maybe
an unknown line with a little limb brightening. The third interval actually
contains two C I lines, which were added; the Si II and S II are blended, but
this could be resolved, too. The fourth interval also contains continuum and a
Si I line, but both are sometimes blended by the strong and dynamic O V line.
Thus, eight different images of the Sun - from the lower chromosphere to the
1.4 million K corona - can be created from each scan, leading to 34 times two
opposite pages in the atlas. - One test run includes Ne VIII 770 and 780, C IV
1548 and 1550, and Si II 1533.