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Introduction
On
UT
2002
November
5-6
and
8-11,
we
used
the
FLAMINGOS
near-infrared
imager
and
spectrograph
on
the
Gemini-South
8m
telescope
at
Cerra
Pach
on
to
demonstrate
its
infrared
spectroscopic
capabilities
(Figs.
1,2).
An
emphasis
was
placed
on
the
unique
multi-object
spectroscopic
(MOS)
mode
of
FLAMINGOS.
The
data
were
obtained
as
a
Gemini-South
Demonstration
Science
Program
and
are
publicly
available.
The
observers
present
were
F.
Barrientos,
A.
Bunker,
P .
Hall,
M.
Ledlow,
N.
Raines,
D.
Stern,
and
J.
Willis.
His
Royal
Highness,
Prince
Andrew,
Duke
of
York,
visited
the
observatory
on
2002
November
7,
preventing
science
observations
that
night.

The
Camera:
FLAMINGOS
FLAMINGOS
{
The
Florida
Multi-object
Imaging
Near-infrared
Grism
Observational
Spectrometer
{
is
a
combination
wide-eld
near-IR
imager
and
multi-object
spectrometer
(MOS),
built
by
R.
Elston
from
the
University
of
Florida.
It
is
the
world's
rst
fully-cryogenic,
near-IR
MOS
spectrometer.
It
is
designed
to
be
a
traveling
visitor
instrument,
spending
Spring/Summer
at
Kitt
Peak
National
Observatory
and
migrating
to
Gemini-South
for
(Northern-
hemisphere)
Fall/Winter.
At
Gemini-South,
the
20482048
science-grade
Hawaii
II
HgCdTe
array
has
a
plate
scale
of
0.08
00
pix
1
,
providing
to
a
2.5
0

2.5
0
eld
of
view
(e.g.,
Fig.
3).
The
liquid
nitrogen-cooled
MOS
plates
have
spectral
resolutions
of
R

350
for
0.47
00
wide
slits,
can
cover
either
J
+H
or
H
+
K
simultaneously
,
and
t

20
targets
with
7.5
00
long
slitlets.
The
MOS
wheel
holds
11
MOS
plates
and
can
be
thermally
cycled
in
less
than
6
hours.

Observations
A
log
of
our
observing
run
is
provided
in
Table
1.
Instrument
problems
led
to
excessively
high
readnoise
for
the
rst
two
nights,
UT
2002
November
5-6.
On
the
third
night,
a
visit
from
his
Royal
Highness
Duke
of
York
(Fig.
4)
closed
down
the
telescope
for
the
night,
allowing
us
to
properly
diagnose
the
problems.
We
traced
the
high
readnoise
to
two
issues:
(1)
on
the
hardware
side,
A/D
lters
which
had
been
installed
to
lower
the
readnoise
were
actually
increasing
it,
so
we
extracted
them;
and
(2)
on
the
software
side,
Fowler
sampling
was
not
functional
for
FLAMINGOS
during
our
observing
run.
For
imaging,
where
the
bright
near-IR
sky
provides
background-limited
data
with
short
exposure
times,
this
was
not
a
problem.
However,
for
spectroscopy ,
the
eect
was
deleterious
in
the
J
and
H
bands.
We
opted
for
30
minute
spectroscopic
integrations
for
the
remainder
of
the
run
so
as
to
achieve
background-limited
data.
The
nal
four
nights
of
the
run
were
more
useful,
though
high
winds
and
poor
seeing
on
UT
2002
November
10
produced
substantial
slit
losses.
Our
scientic
targets
were
a
mixture
of
long
slit
spectra
of
relatively
bright
quasars,
and
MOS
plates
in
the
Chandra
Deep
Field
South
(CDFS),
AKA
the
GOODS
Southern
eld.

Results:
The
Quasars
Long
slit
spectroscopic
targets
for
the
run
focussed
on
relatively
bright
AGNs,
primarily
from
the
Sloan
Digital
Sky
Survey
(SDSS).

We
observed
SDSS
0150
0033
(z
=
1:182)
and
SDSS
2204+0031
(z
=
1:360),
the
two
\mysterious
objects"
from
the
Hall
et
al.
(2002)
atlas
of
unusual
broad
absorption
line
quasars
from
the
SDSS.
Both
are
FIRST
sources
with
S
1:4GHz
of
a
few
mJy .
Optical
spectra
of
both
show
dramatic
drop-os
shortward
of
MgII,
while
the
near-IR
spectra
show
strong
H
emission,
but
no
H,
indicating
substantial
reddening
(Fig.
5).

We
observed
the
z
=
1:464
high-redshift
radio
galaxy
(HzRG;
AKA
radio-
loud
\type-2
quasar")
MP
J2045
6018
(DeBreuck
et
al.
2001,2002;
Fig.
6).
This
K
=
18:0
source
shows
the
narrow
emission
lines
typical
of
HzRGs.
Notably
,
no
broad
component
in
evident
on
the
H
emission
line.

We
observed
the
z
=
5:77
quasar
SDSS
0836+0054
(Fig.
7),
the
third
highest
redshift
quasar
published
currently
(Fan
et
al.
2001).
The
redshift
derived
from
the
optical
spectroscopy
was
overestimated
at
z
=
5:82
due
to
Ly
self-absorption
{
a
familiar
condition
in
high-redshift
objects.

Results:
The
CDFS
MOS
Plates

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