HST Daily Report # 3314
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3314
PERIOD COVERED: DOY 65
OBSERVATIONS SCHEDULED
NICMOS 8791
NICMOS Post-SAA calibration – CR Persistence Part 2
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 DARKSs. 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.
WF/PC-2 9142
The Structure and Physics of Extragalactic Jets.
The WF/PC-2 was used to perform an ongoing investigation into the physics of
jets. It is proposed to obtain polarimetry of the jets of 3C 264 and 3C 78.
NICMOS 9386
Infrared Photometry of a Statistically Significant Sample of KBOs
While the discovery rate of Kuiper Belt objects is accelerating, the
physical
study of this new region of the solar system has been slowed by a lack of
basic
astrophysical data. Photometric observations of the majority of the more
than
400 known KBOs and Centaurs are rudimentary and incomplete, particularly in
the
infrared. The multicolor optical-infrared photometry that exists for a small
subset of KBOs often shows significant discrepancies between observations by
different observers. Their intrinsic faintness puts them at the practical
limits
of ground-based systems. In July 2001 we began what will be the largest
uniform
sample of optical photometry of KBOs with a WFPC2 SNAPSHOT program that will
perform accurate photometry at V, R, and I on a sample of up to 150 targets.
We
seek to greatly enhance the value of this survey by obtaining J and H
photometry
on the same sample using NICMOS. Combined optical and infrared broad band
photometry is a far more powerful tool for physical studies than is either
alone. Our sample includes objects that will be observed at thermal infrared
wavelengths by SIRTF and will be used with those data to derive the first
accurate diameters, albedos, and surface properties for a large sample of
KBOs.
STIS/CCD 9432
The Radio-Loud BAL QSO PKS 1004+13: A Key to Understanding QSO Outflows?
Accretion and outflows drive astrophysical engines on many scales. In
powerful
QSOs, broad absorption lines {BALs} reveal partially-ionized outflows to
~0.1c.
What is the geometry of the flow, its origin, the driving mechanism? Why
are the
most extreme outflows always seen in radio-weak QSOs? Such basic questions
remain unanswered. Plausibly, radiation pressure can drive an equatorial
wind
off the dusty torus or outer accretion disk. Are BAL QSOs seen nearly
edge-on,
as this scenario requires? We don’t know because there is no good
inclination
indicator for these generally radio-weak QSOs. The bright, low-redshift QSO
PKS
1004+13 may be a valuable exception. Its dominant radio lobes imply a near
edge-on view, while low SNR IUE spectra suggest it is a BAL QSO. Indirect
indications that it’s a BAL QSO are: very weak soft X-ray flux, high
scattering
polarization, and unusually weak ionO3. It also shows clear high-ionization
non-BAL absorption with partial continuum coverage. We propose high quality
UV
spectroscopy to confirm its BAL QSO identity. PKS 1004+13 would be only the
second known BAL QSO with powerful radio jets, hence known inclination,
providing a clear test of the outflow geometry, and the only such object at
low
redshift, allowing high SNR, high spatial resolution followup.
ACS 9440
The Composition of Io’s Pele Plume
We propose to determine the composition of Io’s largest volcanic plume,
Pele,
with unprecedented accuracy. This will give us new constraints on the
temperatures, pressures, and magma composition of this volcano, and thus an
improved window into Io’s interior. We will use the proven Jupiter transit
spectroscopy technique, which resulted in the discovery of S_2 gas in the
Pele
plume, but will use exposures that are 4 times longer than in the discovery
observations. This will allow us to accurately measure plume SO_2
abundances,
seen only with low S/N in the discovery observations, and possibly SO, in
addition to S_2, and gives the chance to discover other, currently unknown,
plume components. We will also use ACS to obtain UV and visible images of
the
Pele plume in reflected light prior to Jupiter transit, to constrain the
dust
abundance and particle size in the plume. This will allow refined estimates
of
plume dust/gas ratios and resurfacing rates. We will repeat the observations
four times to build up S/N to even higher levels, and to look for time
variability in both dust and gas abundance and chemistry.
ACS 9450
The lensing galaxy of JVAS B0218+357: determination of H_0
Much effort has been devoted to estimating Hubble’s constant H_0 using
observations of very nearby objects. Gravitational lensing time delays offer
potentially the most accurate method for determining H_0 using observations
on
cosmological scales; it is a very clean method in that little complicated
astrophysics is involved, and it is a single–step method compared to the
traditional multi–step distance ladder. The major problem with most such
determinations in the past has been systematic errors due to uncertainties
in
the lens mass model, leading to 20 Einstein-ring lens system, is the one
system
for which these systematic uncertainties can be reduced very substantially,
and
in particular is unique in that the modeling systematics can be reduced to
the
level of the uncertainties in the measurement of the time delay. The only
requirement left is to be able accurately to locate the center of the
lensing
galaxy. We propose an extremely deep ACS image in I-band of this system for
this
purpose; the prize is a robust 5 {lens mass model}. We have conducted
simulations to estimate the necessary S:N ratio in an ACS observation in
order
to be able to achieve a successful deconvolution of the lens galaxy and
lensed
images with the required accuracy.
STIS/MA2/ACS/HRC 9501
Life Cycles of Radio Galaxies
Now, for the first time, we can probe the duration of nuclear activity and
its
duty cycle and the relationship between the growth of the bulge {via a
starburst} and the growth of the BH {via fueling the AGN}. We have
identified a
class of powerful radio galaxy which displays both an outer `older’ radio
source
as well as an inner `younger’ radio source. These `double- doubles’ are
sources
in which the current radio source is propagating outwards through the relic
of
the previous epoch of activity. In 3C 236 we found that repeated episodes of
star formation and radio ejection were indeed temporally linked. We propose
to
obtain images of the host galaxies of 4 additional double-double radio
galaxies
in the NUV with STIS and the R band with ACS/HRC. The proposed HST
observations
will allow us to determine the existence of young star forming regions in
these
double-double sources. Follow up imaging and spectroscopy combined with our
detailed radio imaging, will allow us to use the double-doubles to address
critical questions concerning probe the relationship between star formation
and
AGN fueling, e.g., – Over what time scales do these processes occur ? — are
they short and intense or long and gradual ?
WFPC2 9594
WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt2/3
This dark calibration program obtains 3 dark frames every day to provide
data
for monitoring and characterizing the evolution of hot pixels
STIS 9605
CCD Dark Monitor-Part 1
Monitor the darks for the STIS CCD
STIS 9607
CCD Bias Monitor – Part 1
Monitor the bias in the 1×1, 1×2, 2×1, and 2×2 bin settings at gain=1, and
1×1
at gain = 4, to build up high-S/N superbiases and track the evolution of hot
columns.
STIS 9625
STIS NUV-MAMA Cycle 11 Flats
This program will obtain NUV-MAMA observations of the STIS internal
Deuterium
lamp to construct an NUV flat applicable to all NUV modes
ACS 9657
ACS Internal Flat Field Stability
The flat field stability and characterisation obtained during the ground
calibration and SMOV phases will be tested and verified through a sub-sample
of
the filter set. Only internal exposures with the calibration lamps will be
required.
ACS 9673
CCD Daily Monitor
This program consists of basic tests to monitor, the read noise, the
development
of hot pixels and test for any source of noise in ACS CCD detectors. This
programme will be executed once a day for the entire lifetime of ACS
WFPC2 9676
POMS Test Proposal: WFII parallel archive proposal
This is the generic target version of the WFPC2 Archival Pure Parallel
program.
The program will be used to take parallel images of random areas of the sky,
following the recommendations of the 2002 Parallels Working Group.
NICMOS 9702
NICMOS Parallel Thermal Background
NICMOS Camera 2 pure parallel exposures in the F222M and F237M filters to
establish the stability of the HST+NCS+Instrument thermal emission. This
data
will be compared against the already available Camera 3 measurements in
F222M
which show an increased thermal background.
ACS 9705
M87 Jet
As the nearest galaxy with an optical jet, M87 affords an unparallelled
opportunity to study extragalactic jet phenomena at the highest resolution.
Monitoring of the jet of M87 by Chandra and HST has detected massive
variability
in one knot of M87’s jet. During March-July 2002, knot HST-1 brightened by a
factor of 2 in both X-rays and optical. Following those observations, M87
became
unobservable, as in August-October the Sun approaches to within 5 degrees.
Chandra monitoring resumes in November; however, there are no HST
observations
of M87 scheduled until May 2003. We therefore request five HST observations
during the period November 2002-April 2003, scheduled to correspond with the
Chandra observations. Based on its track record of X-ray variability in the
last
year, and optical variability and superluminal motion {speeds of 6c} since
1994,
we expect continued variability, with comparable timescales. The proposed
observations will monitor the optical morphology, spectrum and magnetic
field
configuration of the jet, and allow us to model the mechanisms responsible
for
this variability, the first seen in a spatially resolved jet. The results of
this investigation are of key importance not only for understanding the
nature
of the X-ray emission of the M87 and its relationship to the lower energy,
radio-optical continuum, but also for understanding flares in blazar jets,
which
are highly variable but where we have never before been able to resolve the
flaring region in the optical or X-rays. Given the SED observed in M87, the
flare emission is probably synchrotron radiation from a fresh particle
injection
threshold. Not only will these observations allow us to check this
hypothesis,
they will allow us to constrain the particle acceleration and loss
timescales as
well as the jet dynamics {which produce and affect the magnetic field
configuration} associated with this flaring component.
STIS 9706
STIS Pure Parallel Imaging Program: Cycle 10
ACS/CAL 9707
Elevated ACS CCD temperature study
behaviour, measurements will be taken with the TEC set points at -71.5C and
-66.7C. Bias and dark frames plus CTE images will be recorded at the normal
operating temperature, -77C, and at the two higher settings
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports of
potential non-nominal performance that will be investigated.)
HSTAR 8948: STIS Tungsten Lamp Failed to Turn On. On day 03/061 (03/02/03)
at
19:57:06 UT, a target acquisition image was taken
with STIS’s CCD. The
third sub-exposure of that image, that is a
through-slit exposure of
0.1 sec in length with the Tungsten lamp ON, did not
show any flux
(other than background noise). Under investigation.
HSTAR 8950: GSacq(1,2,1) results to Finelock Backup (2,0,2). The
GSACQ(1,2,1)
of 066/06:32:55 – 06:40:17 which begun during ZOE,
resulted to Finelock
Backup, at AOS 066/06:49:04 using FGS#2 (2,0,2) due
to SCANSTEP LMT EXC
on FGS#1.Possible observations affected:STIS 87,88
WFPCII 150 thru 160.
The guide star acquisition for this observation was
non-nominal, further
analysis will determine if a repeat observation is
required.
COMPLETED OPS REQs: NONE
OPS NOTES EXECUTED: NONE
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 11 11
FGS REacq 05 05
FHST Update 18 18
LOSS of LOCK
SIGNIFICANT EVENTS: None
