Hubble Space Telescope Daily Report 23 Jun 2002
HUBBLE SPACE TELESCOPE
DAILY REPORT # 3143
PERIOD COVERED: DOY 172-174
OBSERVATIONS SCHEDULED (see HSTARS below for possible observation problems)
ACS/CAL 9558
ACS weekly Test
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.
ACS/HRC/WFC 9292
The Nature of Galaxies at z > 4
The Advanced Camera for Surveys (HRC and WFC) was used to further look into
recent discoveries of a number of galaxies and quasars at redshifts greater
than
5 that has identified the z>5-6 epoch as key to understanding the earliest
formation phases for galaxies. However, establishing the characteristics and
properties of these earliest galaxies is proving to be a particularly
difficult.
They are faint, with I{AB} magnitudes around 26-27. Thus, substantial
investments of time are needed to obtain high S/N images, while ground-based
spectroscopy, even with 8-10 m class telescopes, has provided little more than
redshifts. Establishing the physical properties of these galaxies will be a
challenge for the foreseeable future. However, there is a subset of this high
redshift population that is amenable to more detailed study. These are sources
that have been strongly lensed by low redshift clusters.
ACS/WFC 9584
ACS Default {Archival} Pure Parallel Program II.
The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels.
ACS/WFC 9575
Default {Archival} Pure Parallel Program.
The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in
POMS.
ACS/WFC/HRC 9075
Cosmological Parameters from Type Ia Supernovae at High Redshift.
The Advanced Camera for Surveys (WFC and HRC) was used to obtain a Hubble
diagram of Type Ia supernovae {SNe Ia} that will be of long lasting value as a
record of the expansion history of the universe.
FGS/1 9034
The Masses and Luminosities of Population II Stars.
Fine Guidance Sensor 11R was used to observe the mass-luminosity relation {MLR}
of Population II stars of which very little is currently known. With the advent
of the Hipparcos Catalogue, improved distances to many spectroscopic binaries
known to be Pop II systems are now available. After surveying the
literature and
making reasonable estimates of the secondary masses, we find 13 systems whose
minimum separation should be larger than the resolution limit of FGS #1.
GTO/ACS 9290
The Nature of Galaxies at z > 4.
The Morphological, Photometric, and Spectroscopic Properties of Intermediate
Redshift Cluster.New and fundamental constraints on the evolutionary state of
high redshift clusters will be made by obtaining deep, multiband images
{SDSS g,
r, i, z} over the central 1.5 Mpc regions of seven distant clusters in the
range
0.76 < z < 1.27. In addition, slitless spectroscopy, using the WFC GRISM, will
be performed over the central 750 kpc region of each system galaxy.
NICMOS 9269
NICMOS Parallel Thermal Background
NICMOS Camera 3 pure parallel exposures in the F222M filter will be
obtained for
the entire duration of SMOV to establish the stability of the
HST+NCS+Instrument
thermal emission.
NICMOS 8790
NICMOS Post-SAA calibration – CR Persistence Part 1.
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.
STIS 9618
STIS MAMA Dispersion Solutions
Obtain wavecals just deep enough to constrain wavelength and spatial distortion
maps without overusing the calibration lamp. For the first time on orbit, data
will be obtained at all available central wavelengths. This information will
help constrain global models of STIS optical performance being developed at ECF
and STScI. During the observations, MSM monthly offsets will be set to zero to
complement observations over the past couple of cycles, which occurred at
extreme
monthly offsets. The echelle observations at zero offset will yield dispersion
solutions that are directly applicable to all echelle science data obtained
after monthly offsets are disabled.
STIS 9435
Systematic Search for Rotation at the Base of Outflows from T Tauri Stars
We wish to search for rotation signatures in the initial portion {first 100 AU}
of a sample of outflows emanating from T Tauri stars {TTSs}. This project
originates from our detection of systematic transverse radial velocity
shifts in
STIS spectra of the DG Tau jet {Bacciotti et al., 2002}. The shifts,
observed in
a region where the flow is already collimated, but has not yet manifestly
interacted with its environment, are consistent with the predictions of
magneto-
centrifugal launching models, and may constitute the first observed indication
for rotation in the initial portion of a jet flow. Rotation is a fundamental
ingredient in star formation theories, thus we propose to confirm the above
result by carrying out a systematic survey in similar flows. We plan to
take for
each jet a STIS spectrum in the 6300 — 6800 Angstrom range, with the slit
perpendicular to the flow direction and at a distance of about 0.”3 from the
source {i.e., in our targets, 40 — 70 AU along the jet depending on
inclination
angle}. Since the flows are resolved transversely with HST, the proposed slit
orientation allows for the direct detection of systematic velocity shifts.
Where
found, we will check for consistency between the sense of rotation observed and
that of the underlying disk through CO interferometric measurements. As a
by-product, estimates of the excitation conditions across the flow {including
ionization fraction} and of the mass outflow rates will be derived.
STIS/CCD 9187
A Lyman Limit Snapshot Survey: The Search for Candidate D/H Absorbers.
The Space Telescope Imaging Spectrograph (CCD) was used to measure D/H in gas
clouds seen against background QSOs. This provides a unique and fundamental
cosmological probe of the baryonic density parameter. To date, most of the QSO
absorption line D/H constraints have been derived at high redshift. In this
proposal the proposers investigate a lower redshift range, because there
are two
potentially crucial advantages to be gained by carrying out D/H measurements at
intermediate redshift. First, the background of HI forest lines is lower and
contamination of the DI feature is significantly reduced. Second, a far larger
sample of very bright QSOs exists.
STIS/CCD 8904
Bias Monitor-Part 2.
The Space Telescope Imaging Spectrograph (CCD) was used to 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 in order
to build up high-S/N superbiases and track the evolution of hot columns.
STIS/CCD 9066
Closing in on the Hydrogen Reionization Edge of the Universe.
The Space Telescope Imaging Spectrograph (CCD) was used in parallel constrain
the Hydrogen reionization edge in emission that marks the transition from a
neutral to a fully ionized IGM at a predicted redshifts.
STIS/CCD 9186
D/H in Lyman Limit Absorbers with Simple Velocity Structure.
The Space Telescope Imaging Spectrograph (CCD) was used to observe the
deuterium
abundance in QSO absorbers that provides a direct measurement of the baryonic
density of the Universe. This proposal will obtain new high resolution data of
two carefully selected, intermediate redshift absorption systems.
STIS/CCD 8902
Dark Monitor-Part 2.
The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks.
STIS/CCD 8895
Far-UV Spectroscopy Of The Disk Around HD 100546.
The Space Telescope Imaging Spectrograph (CCD) was used to perform a one-orbit
program to do long-slit spectroscopy of HD 100546. Lyman-alpha has been seen in
emission in IUE/SWP spectra. This spectra would map the spatial extent of
Lyman-alpha emission and give the spatial orientation of the disk {i.e. which
side is the approaching side}. The proposal completed with no reported
problems.
STIS/CCD 9131
Imaging the Host Galaxies of High Redshift Type Ia Supernovae.
The Space Telescope Imaging Spectrograph (CCD) was used to complete the
snapshot
survey of distant galaxies of known redshift which hosted supernovae {SNe} of
Type Ia found via the Supernova Cosmology Project {SCP}.
STIS/CCD 9148
Light Echos and the Nature of Type Ia Supernovae.
The Space Telescope Imaging Spectrograph (CCD) was used to take STIS snapshot
images of a subset of 43 well observed Type Ia supernovae {SNIa}, most of which
have been discovered in late type galaxies over the last 40 years to make a
systematic search for light echos around SN Ia. STIS will also observe a sample
of 10 SN II and SN Ib/c, which are believed to be the result of massive star
core collapse and, therefore, to be thin-disk population objects, in order to
make an empirical calibration of the accuracy of our method for determining
scale heights. The SN Ia sample will provide a direct as well as accurate
estimate of the scale height of SN Ia which is an important clue to the
progenitors of these events.
STIS/CCD 9088
Next Generation Spectral Library of Stars.
The Space Telescope Imaging Spectrograph (CCD) was used to produce a “Next
Generation” Spectral Library of 600 stars for use in modeling the integrated
light of galaxies and clusters by using the low dispersion UV and optical
gratings of STIS. The library will be roughly equally divided among four
metallicities, very low {Fe/H < -1.5}, low {-1.5 < Fe/H < -0.5}, near-solar
{-0.5 < Fe/H < 0.1}, and super-solar {Fe/H > 0.1}, well-sampling the entire
HR-diagram in each bin. Such a library will surpass all extant compilations and
have lasting archival value, well into the Next Generation Space Telescope
era.
STIS/CCD 9317
Pure Parallel Imaging Program: Cycle 10.
The Space Telescope Imaging Spectrograph (CCD) was used to perform the default
archival pure parallel program for STIS during cycle 10.
STIS/MA1/MA2 8920
Cycle 10 MAMA Dark Measurements.
The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to perform the
routine monitoring of the MAMA detector dark noise, and is the primary means of
checking on health of the MAMA detectors systems through frequent monitoring of
the background count rate.
WF/PC-2 9104
A Study of Proplyds and a Protostellar Condensation at the Center of M20.
The WF/PC-2 was used to observe the Trifid nebula {M20} that is a well-known
prominent optical HII region trisected by bands of obscuring dust lanes and
excited by an O7.5 star HD 164492A. Our recent study of near-IR ground-based
observations of this region at J, H, K and L show all seven components of HD
164492 {A to G} identified optically. Our sub-arcsecond radio continuum VLA and
ground- based observations of M20 also show free-free emission from three
stellar sources {B, C and D} and a bright rim outlining a protostellar
condensation {TC1} lying close to the O7V star {HD 164492A} at the center
of the
nebula. Based on a number of strong arguments, these stars have disks
associated
with them and their envelopes are photoionized externally by the UV radiation
from the hot central star, HD 164492A. These proposed WFPC2 observations are
intended to search for neutral protoplanetary disks “proplyds”, to study the
optically bright rim of ionized gas associated with TC1 for signs of star
formation, and to make a detailed subarcsecond determination of extinction
toward the dust lanes of M20 using HAlpha and 6cm data.
WF/PC-2 9050
Outflow Collimation in Bipolar Symbiotic Nebulae.
The WF/PC-2 was used to observe flow collimation in evolved stars that is
neither expected nor understood. Classical theories of stellar evolution do not
predict and cannot explain this bipolarity. More exotic concepts {binary
interactions, spun-up atmospheres, poloidal or toroidal magnetized winds} have
been proposed, but observations are yet to verify or falsify any of their
predictions. This proposal will probe the near-nuclear morphology and
kinematics
of four bright, low-extinction targets whose large-scale structure is highly
bipolar. The goal is to provide a detailed description of the circumnuclear
outflows, to uncover the physical structure and nature of the collimator,
and to
evaluate the speculative collimation mechanisms. The bright nucleus has
hampered
efforts to explore the nebular collimators that lie close to the star, so we’ll
use STIS to disperse the nuclear light and, thus, to avoid its glare. A
secondary goal is to obtain second-epoch WFPC2 images of all targets.
WF/PC-2 9318
POMS Test Proposal: WFII Parallel Archive Proposal Continuation.
The WF/PC-2 was used to perform the generic target version of the WFPC2
Archival
Pure Parallel program. The program was used to take parallel images of random
areas of the sky, following the recommendations of the Parallels Working
Group.
WFPC2 8938
WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3.
This dark calibration program obtains 3 dark frames every day to provide data
for monitoring and characterizing the evolution of hot pixels.
FLIGHT OPERATIONS SUMMARY
HSTARs:
8709 – NBOOTSAA CCL skip FOM commanding @170/1929zDuring recovery of NICMOS
from SUSPEND, the CCL NBOOTSAA skipped the FOM homing commands.
SISE advised FC to continue with commanding and OPS
Request#16791 was
modified to omit last step (position FOM, since already in
correct location)
with STScI Commanding concurrence. Note from SI SE: This HSTAR
does not
point towards an anomaly. It simply tracks changes that should
be made to
a CCL used in the NICMOS recovery from suspend. Summary: a
telemetry check
in the CCL needs to be moved up to allow more samples (major
frames) prior
to homing the FOM. At its’ current position, there is a
possibility that
the telemetry check may get inaccurate data. We are also talking
about
adding a check to the COP for the FOM temperatures prior to
executing this CCL.
Under investigation.
8710 – NBOOTSAA CCL skip FOM commanding @170/1929z (********HSTAR 8710
Rejected*****)
8711 – BAY 6 TEMP SENSOR (TB6AESB) OOL LIMITS @172/1446z. Between
2002/172/14:46:16Z
and 2002/172/15:20:00Z mnemonic TB6AESB (bay 6 aft ES bulkhead)
violated its
upper red temperature OOL high= 20.4354 deg C intermittently, and
can be seen
in attachments. PRD LIMITS -50.0/20.0 deg C. Y/R High Limit is
+20.0 deg C.
TCS on call notified. Last reported ref. HSTAR #8451. Under
investigation.
8712 – Bay 5 forward bulkhead temperature out of limit @172/2244z.Bay 5 ES
Forward
Bulkhead temperature TB5ESB broke limit briefly from 22:43:46 to
22:43:58,
again from 22:44:04 to 22:51:04, and from 22:51:16 to 22:51:34,
each time with
a maximum value of 25.1561 DegC, limit is 25.0 DegC. On call TCS
engineer
notified. Under investigation.
COMPLETED OPS REQs: None
OPS NOTES EXECUTED:
1006-3 – AXIAL link2 Temp Limit Change @172/1335z
1014-1 – Main Baffle 3 Limit Adjust Closed(EMNBF3T Lim Restored) @174/0100z
1008-0 – Raise Battery 3 Upper Temp limit Closed(Lim Restored to 3.0deg)
@174/2049z
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 19 19
FGS REacq 28 28
FHST Update 40 40
LOSS of LOCK None
SIGNIFICANT EVENTS:
Reconditioned ESTR @ 175/00:45Z (ROP RD-7A).
