Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.stsci.edu/hst/foc/documents/tips/tips_19jan95.ps Äàòà èçìåíåíèÿ: Unknown Äàòà èíäåêñèðîâàíèÿ: Tue Feb 5 14:51:33 2013 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: arp 220

SPACETELESCOPESCIENCEINSTITUTE
TIPS
Meeting
19
Jan
1995
R
Jedrzejewski
Summary
of
FOC
Activities
for
the
period
1
Dec
1994
­
19
Jan
1995
Operations .
The
F/96
relay
has
been
operating
nominally.
Proposals
Executed
.
Five
GO/GTO
proposals
were
successfully
executed
with
the
FOC:
5144
Study
of
Optical
Emission
Associated
with
Radio
Jets
and
Hot
Spots
5705
A
Deep
Color­Magnitude
Array
of
NGC
7099:
Cycle
4
Carry­over
5175
Physics
of
Asteroids
­
Cycle
4.
5154
FOC
Observations
of
Elliptical
Galaxies
5420
Color­Magnitude
Diagrams
of
Globular
Clusters
in
M31
.
The
following
CAL
proposals
were
executed
with
the
FOC:
5767
Fall
Heptathlon
5527
FOC
Post­COSTAR
Relative
DQE
Calibration.
5523
Post­COSTAR
FOC/96
Fine
Aperture
Location
5762
FOC
Point­Spread
Function
Monitoring
TIPS
Meeting
19
Jan
1995
R
Jedrzejewski
Summary
of
FOC
Activities
for
the
period
1
Dec
1994
­
19
Jan
1995

SPACETELESCOPESCIENCEINSTITUTE
TIPS
Meeting
19
Jan
1995
R
Jedrzejewski
Summary
of
FOC
Activities
for
the
period
1
Dec
1994
­
19
Jan
1995
Calibration Proposal
5527
lost
last
image.
Image
next
to
last
shows
20%
missing
data
in
form
of
stripes
of
data
drops.
Image
is
still
useful.
Proposal
5523
was
executed
successfully
and
shows
the
astrometric
standard
close
to
the
center.
Images
are
being
analyzed.
Costar
DOB
Move
The
COSTAR
DOB
was
moved
on
January
16th
1994
to
compensate
for
the
scheduled
desorption
move
of
the
OTA
secondary
mirror.
This
keeps
the
FOC
optimally
focussed
for
the
next
2­3
months.
The
DOB
was
moved
from
its
current
position
of
­0.8mm
to
a
new
position
of
­0.1mm.
FOC
images
were
taken
2
days
later
to
verify
the
effectiveness
of
the
move.
A
first
look
appears
to
show
that
everything
worked
fine.

SPACETELESCOPESCIENCEINSTITUTE
TIPS
Meeting
19
Jan
1995
R
Jedrzejewski
Summary
of
FOC
Activities
for
the
period
1
Dec
1994
­
19
Jan
1995
FOC
Phase
II
FOC
Support
All
the
successful
FOC
PIs
have
been
contacted
by
the
LSs.
In
addition
to
the
LS
and
PC
support,
the
FOC
group
is
offering
proactive
technical
support
to
maximize
the
scientific
output
of
the
FOC
programs.
We
have
assigned
to
each
proposal
a
member
of
the
FOC
group,
mainly
on
the
basis
of
scientific
interest.
The
FOC
person
will
read
the
scientific
jus­
tification
of
the
proposal,
and
will
help
the
PI
to
optimize
the
observation
strategy
and
avoid
common
instrument
problems.
Best
Instrument
Choice
Following
the
experience
of
PCs
during
the
TAC
meetings,
The
FOC
group
decided
to
examine
all
the
proposals
approved
to
be
executed
with
WFPC2
to
check
if
they
could
be
better
carried
out
with
the
FOC,
in
the
same
amount
of
time
(eg.
proposals
needing
a
bet­
ter
sampling,
or
UV
capabilities).
Out
of
~
150
WFPC2
proposals,
7
were
singled
out,
which
were
submitted
for
a
second
technical
review
to
the
SIB
Branch
Chief
and
to
the
WFPC2
Instrument
Scientist.
Agreement
was
reached
that
for
four
proposals
the
FOC
may
be
the
most
suitable
instrument
to
carry
out
the
required
science.
The
Director
has
approved
the
strategy:
the
PIs
have
been
contacted,
and
were
given
the
choice
(along

SPACETELESCOPESCIENCEINSTITUTE
TIPS
Meeting
19
Jan
1995
R
Jedrzejewski
Summary
of
FOC
Activities
for
the
period
1
Dec
1994
­
19
Jan
1995
with
all
the
needed
explanations)
to
switch
instrument.
F/48
Camera
The
F/48
relay
was
successfully
switched
on
Day
304
at
8:54
UT
to
execute
a
calibration
program
aimed
at
1)
locating
the
0.06''
slit
in
the
HST
focal
plane
and
2)
characterizing
the
performance
of
the
detector.
The
target
chosen,
NGC1068,
had
been
imaged
with
the
FOC
with
the
F501N
filter,
providing
a
map
in
the
5007å
line
which
could
be
used
to
iden­
tify
features
in
the
long­slit
spectra.
1)
the
first
objective
was
achieved,
with
an
accuracy
of
0.5''.
The
accuracy
is
lower
than
expected
because
the
scans
across
the
target
were
performed
differently
than
planned,
along
the
slit
orientation
rather
than
perpendicular
to
it.
2)
the
most
encouraging
result
here
is
the
behaviour
of
the
background
noise,
which,
although
still
higher
than
nominal,
appeared
to
decrease
as
a
function
of
time
from
HV
switch­on.
This
behaviour
is
exactly
the
opposite
of
what
happened
during
the
previous
tests,
in
which
the
background
noise
increased
with
time
to
reach
saturation
levels
a
few
hrs
after
switch­on.
In
addition,
the
analysis
of
geometric
distortion
across
the
images
gave
also
a
moderately
optimistic
result:
the
geometric
distortion
behaved
much
as
it
did
soon
after
launch.
The
plate
scale
only
changed
by
0.5%
with
a
rotation
of
only
0.23š,
almost
identical
behavior
to
that
seen
during
Cycle
1
observations.
This
would
point
to
a
relative
stability
of
the

SPACETELESCOPESCIENCEINSTITUTE
TIPS
Meeting
19
Jan
1995
R
Jedrzejewski
Summary
of
FOC
Activities
for
the
period
1
Dec
1994
­
19
Jan
1995
detector.
F/48
Camera:
Plans
for
the
Future
The
unexpected
behaviour
of
the
F/48
background
noise
has
prompted
a
revaluation
of
the
testing
strategy
of
the
camera.
An
alternative
theory
has
been
proposed,
invoking
the
presence
of
a
flare
inside
the
tube
itself,
rather
than
a
crack
in
the
potting
around
it.
If
this
theory
is
correct,
the
camera
behaviour
could
keep
improving
with
time.
In
order
to
discern
amongst
the
two
possibilities,
and
ultimately
to
understand
if
the
F/48
is
a
usable
instrument,
we
have
designed
a
more
systematic,
thorough
test,
entirely
intermal,
which
includes
a
sequence
of
darks
and
flat
fields
to
be
taken
after
HV
switch­on
for
a
duration
of
few
hours.
The
exposures
will
be
taken
in
normal
imaging
mode
and
in
histogram
mode,
so
that
we
will
be
able
to
analyze
the
distribution
of
the
events
and
recog­
nize
their
origin.
This
test
will
be
repeated
at
regular
time
intervals
(~
2
months),
in
order
to
accumulate
statistically
significant
data
on
the
problem.