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 #
4452
PERIOD COVERED: UT September 20, 2007 (DOY 263)
OBSERVATIONS SCHEDULED
ACS/SBC 10840
The FUV fluxes of Tauri stars in
the Taurus molecular cloud
Present and forthcoming ground-based and space surveys of
the T Tauri
stars in the Taurus molecular cloud
will provide information from high
energy stellar and accretion radiation
to low energy solid state and
molecular emission from the disk, making
those stars perfect
laboratories to carry out self-consistent
studies of disk physics and
evolution. We propose to complete this
wealth of information by
obtaining ACS/FUV spectra for a
significant sample of Taurus T Tauri
stars, covering a range of accretion
properties and dust evolutionary
stages. FUV fluxes carry ~ 10 - 100
more energy than X-rays into these
disks and are thus crucial gas
heating agents and key to disk dispersal
by photoevaporation.
These observations are a pre-requisite to interpret
observations with Spitzer, SOFIA, Herschel,
and ALMA, and will become
one of the important legacies of
HST to the star formation community.
ACS/SBC 10872
Lyman Continuum Emission in Galaxies at z=1.2
Lyman continuum photons produced in massive starbursts may
have played a
dominant role in the reionization
of the Universe. Starbursts are
important contributors to the ionizing metagalactic background at lower
redshifts as well. However, their contribution
to the background depends
upon the fraction of ionizing
radiation that escapes from the intrinsic
opacity of galaxies below the Lyman
limit. Current surveys suggest
escape fractions of a few percent, up
to 10%, with very few detections
{as opposed to upper limits}
having been reported. No detections have
been reported in the epochs between
z=0.1 and z=2. We propose to measure
the fraction of escaping Lyman
continuum radiation from 15 luminous
z~1.2 galaxies in the GOODS
fields. Using the tremendous sensitivity of
the ACS Solar- blind Channel, we
will reach AB=30 mag., allowing us to
detect an escape fraction of 1%. We
will correlate the amount of
escaping radiation with the photometric
and morphological properties of
the galaxies. A non-detection in
all sources would imply that QSOs
provide the overwhelming majority of
ionizing radiation at z=1.3, and it
would strongly indicate that the
properties of galaxies at higher
redshift have to be significantly
different for galaxies to dominate
reionization. The deep FUV images will also
be useful for extending the
FUV study of other galaxies in the GOODS fields.
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.
NIC2 11016
NICMOS Flats: narrow and broad filters for NIC1 {+ NIC2,
NIC3 in
parallel}
This proposal obtains sequences of NICMOS narrow band
filter flat fields
for camera 1. In cameras 2 and 3,
parallel observations will allow us to
obtain high S/N flats for all spectral
elements.
NIC3 11064
CYCLE 15 NICMOS SPECTROPHOTOMETRY CALIBRATION PROGRAM
Now that the spectrophotometric
capabilities of the NICMOS grism have
been established, cycle 15
observations are needed to refine the
sensitivity estimates, to check for
sensitivity loss with time, to
improve the accuracy of the linearity
correction, to improve the
secondary flux standards by
re-observation, and to expand the G206 data
set now that the sky subtraction technique
has been shown to produce
useful fluxes for some of the fainter
secondary standards. These faint
secondary IR standards will be a
significant step towards establishing
flux standards for JWST, as well as
for SNAP, Spitzer, and
observe the 3 primary WDs GD71, G191B2b, & GD153 twice each, once at the
beginning and once near the end of the 18
month cycle. To date, we have
only 2 observation of each star,
while the corresponding STIS data set
for these primary standards ranges
from 6 to 23 obs. No observations
exist for GD71 or GD153 with G206, so
that the current G206 sensitivity
is defined solely by G191B2B.
Purposes: Refine sensitivities, measure
sens losses. Orbits: 2 for each of 6
visits = 12 2. Re-observe WD1057 &
WD1657 plus another P041C lamp-on visit to improve the
scatter in the
non-lin measurements per Fig. 8 of NIC
ISR 2006-02. The WD stars require
2 orbits each, while the lamp-on
test is done in one. The very faintest
and most crucial standard WD1657
has 2 good visits already, so to
substantially improve the S/N, two visits of
two orbits are needed.
Include G206 for P041C in the lamp-off baseline part of
that orbit.
Orbits: WD1057-2, WD1657-4, P041C-1 --> 7 3. Re-observe
9 secondary
standards to improve S/N of the faint
ones and to include G206 for all
9. BD+17 {3 obs} is not repeated
in this cycle. Four are bright enough
to do in one orbit: VB8,
2M0036+18, P330E, and P177D. Orbits:2*5+4=14
Grand Total orbits over 18 month cycle 15 is 12+6+14=32 {Roelof will
submit the P041C lamp-on visit in a
separate program.}
WFPC2 10915
ACS Nearby Galaxy Survey
Existing HST observations of nearby galaxies comprise a
sparse and
highly non-uniform archive, making
comprehensive comparative studies
among galaxies essentially impossible.
We propose to secure HST's
lasting impact on the study of nearby
galaxies by undertaking a
systematic, complete, and carefully
crafted imaging survey of ALL
galaxies in the Local Universe outside
the Local Group. The resulting
images will allow unprecedented
measurements of: {1} the star formation
history {SFH} of a >100 Mpc^3 volume
of the Universe with a time
resolution of Delta[log{t}]=0.25; {2}
correlations between spatially
resolved SFHs
and environment; {3} the structure and properties of thick
disks and stellar halos; and {4} the
color distributions, sizes, and
specific frequencies of globular and
disk clusters as a function of
galaxy mass and environment. To reach
these goals, we will use a
combination of wide-field tiling and
pointed deep imaging to obtain
uniform data on all 72 galaxies within
a volume-limited sample extending
to ~3.5 Mpc,
with an extension to the M81 group. For each galaxy, the
wide-field imaging will cover out to ~1.5
times the optical radius and
will reach photometric depths of at
least 2 magnitudes below the tip of
the red giant branch throughout the
limits of the survey volume. One
additional deep pointing per galaxy will
reach SNR~10 for red clump
stars, sufficient to recover the
ancient SFH from the color-magnitude
diagram. This proposal will produce
photometric information for ~100
million stars {comparable to the number
in the SDSS survey} and uniform
multi- color images of half a square
degree of sky. The resulting
archive will establish the fundamental
optical database for nearby
galaxies, in preparation for the shift
of high- resolution imaging to
the near-infrared.
WFPC2 11084
Probing the Least Luminous Galaxies in the Local Universe
We propose to obtain deep color-magnitude data of eight
new Local Group
galaxies which we recently discovered:
Andromeda XI, Andromeda XII, and
Andromeda XIII {satellites of M31}; Canes Venatici I, Canes Venatici II,
Hercules, and Leo IV {satellites of the Milky Way}; and
Leo T, a new
"free-floating" Local
Group dwarf spheroidal with evidence for recent
star formation and associated H I
gas. These represent the least
luminous galaxies known at *any* redshift, and are the only accessible
laboratories for studying this extreme
regime of galaxy formation. With
deep WFPC-2 F606W and F814W pointings at their centers, we will
determine whether these objects contain
single or multiple age stellar
populations, as well as whether these
objects display a range of
metallicities.
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 06 06
OBAD with Maneuver
20 20
SIGNIFICANT EVENTS: (None)
-
____________________________________________________________
Lynn F. Bassford
Hubble Space Telescope
CHAMP
CHAMP Flight Operations Team Manager
Lockheed Martin Mission Services (LMMS)
NASA GSFC PH#: 301-286-2876
"The Hubble Space Telescope is the
astronomical observatory and key to unlocking the most cosmic mysteries of the
past, present and future." - 7/26/6