Notice:
Due to the conversion of some ACS WFC or HRC observations into
WFPC2,
or NICMOS observations after the loss of ACS CCD science
capability
in January, there may be an occasional discrepancy between a
proposal's
listed (and correct) instrument usage and the abstract that
follows
it.
HUBBLE
SPACE TELESCOPE - Continuing to collect World Class Science
DAILY
REPORT # 4490
PERIOD
COVERED: UT November 15, 2007 (DOY 319)
OBSERVATIONS
SCHEDULED
NIC1/NIC2/NIC3
8794
NICMOS Post-SAA calibration - CR Persistence Part 5
A
new procedure proposed to alleviate the CR-persistence problem of
NICMOS.
Dark frames will be obtained immediately upon exiting the SAA
contour
23, and every time a NICMOS exposure is scheduled within 50
minutes
of coming out of the SAA. The darks will be obtained in parallel
in
all three NICMOS Cameras. The POST-SAA darks will be non- standard
reference
files available to users with a USEAFTER date/time mark. The
keyword
'USEAFTER=date/time' will also be added to the header of each
POST-SAA
DARK frame. The keyword must be populated with the time, in
addition
to the date, because HST crosses the SAA ~8 times per day so
each
POST-SAA DARK will need to have the appropriate time specified, for
users
to identify the ones they need. Both the raw and processed images
will
be archived as POST-SAA DARKs. Generally we expect that all NICMOS
science/calibration
observations started within 50 minutes of leaving an
SAA
will need such maps to remove the CR persistence from the science
images.
Each observation will need its own CRMAP, as different SAA
passages
leave different imprints on the NICMOS detectors.
NIC3
11191
NICMOS
Imaging of a z>4 High-Redshift Ultraluminous Submillimeter Source
We
propose 16 orbits of deep NICMOS 1.6 um imaging of GOODS850-5, a
unique
z>4 candidate SCUBA source that is bright in the submillimeter
{submm}
but extremely faint at all other wavelengths. GOODS850-5 is a 11
mJy
850 um source discovered in our GOODS- N SCUBA survey. It does not
have
a radio counterpart and its accurate location was recently
determined
with the SMA interferometer. It is not detected by the
GOODS-N
HST ACS imaging and is just above the detection limit of the
ultradeep
Spitzer imaging at 3.6-24 um. Its faint radio flux and its
Spitzer
color suggest a redshift of z>4, and potentially even z>6. It
has
an incredible star formation rate of ~1000 solar mass per year, and
it
can quickly grow into a >10^11 solar mass massive galaxy. Radio faint
submm
sources like GOODS850-5 may be a new population of high-redshift
massive
galaxies that are not picked up by any of the previous optical,
near-IR,
and radio surveys, and therefore it is crucial to obtain the
redshift
of GOODS850-5. However, because of its extreme optical
faintness,
the only way to constrain its redshift is photometric
redshift
with the existing Spitzer photometry and the proposed NICMOS
1.6
um photometry. NICMOS is the only instrument that can provide
information
about its redshift and morphology among all space- based and
ground-based
instruments at all wavelengths. The proposed observation
will
provide unique insight on galaxy evolution and mass assembly at
high
redshift.
WFPC2
11093
Hubble
Heritage Observations of PNe with WFPC2
This
is a proposal for observation of a set of PNe using a common WFPC2
observation
sequence.
WFPC2
11134
WFPC2
Tidal Tail Survey: Probing Star Cluster Formation on the Edge
The
spectacular HST images of the interiors of merging galaxies such as
the
Antennae and NGC 7252 have revealed rich and diverse populations of
star
clusters created over the course of the interaction. Intriguingly,
our
WFPC2 study of tidal tails in these and other interacting pairs has
shown
that star cluster birth in the tails does not follow a similarly
straightforward
evolution. In fact, cluster formation in these
relatively
sparse environments is not guaranteed -- only one of six
tails
in our initial study showed evidence for a significant population
of
young star clusters. The tail environment thus offers the opportunity
to
probe star cluster formation on the edge of the physical parameter
space
{e.g., of stellar and gas mass, density, and pressure} that
permits
it to occur. We propose to significantly extend our pilot sample
of
optically bright, gas-rich tidal tails by a factor of 4 in number to
include
a more diverse population of tails, encompassing major and minor
mergers,
gas-rich and gas-poor tails, as well as early, late, and merged
interaction
stages. With 21 orbits of HST WFPC2 imaging in the F606W and
F814W
filters, we can identify, roughly age-date, and measure sizes of
star
clusters to determine what physical parameters affect star cluster
formation.
WFPC2 imaging has been used effectively in our initial study
of
four mergers, and it will be possible in this program to reach
similar
limits of Mv=-8.5 for each of 16 more tails. With the much
larger
sample we expect to isolate which factors, such as merger stage,
HI
content, and merger mass ratio, drive the formation of star clusters.
FLIGHT
OPERATIONS SUMMARY:
Significant
Spacecraft Anomalies: (The following are preliminary reports
of
potential non-nominal performance that will be investigated.)
HSTARS:
(None)
COMPLETED
OPS REQUEST: (None)
COMPLETED
OPS NOTES: (None)
SCHEDULED
SUCCESSFUL
FGS
GSacq
04
04
FGS
REacq
08
08
OBAD
with Maneuver 24
24
SIGNIFICANT
EVENTS: (None)