Hubble Space Telescope Daily Report #2944 – 27 Aug 2001
HUBBLE SPACE TELESCOPE
DAILY REPORT #2944
PERIOD COVERED: 0000Z (UTC) 08/24/01 – 0000Z (UTC) 08/27/01
Daily Status Report as of 239/0000Z
1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:
1.1 Completed STIS/CCD/MA2 8569 (A New Survey for Low-Redshift Damped
Lyman-Alpha Lines in QSO MgII Systems)
The Space Telescope Imaging Spectrograph (CCD and MA2) was used to
support studies which have shown that most of the observable neutral gas
mass in the Universe resides in QSO damped LyAlpha {DLA} systems. However,
at low redshift, DLA can only be found by searching in the UV with HST. By
boot-strapping from the MgII statistics, we will be able to further improve
the determination of the low- redshift statistical properties of DLA {their
incidence and cosmological mass density} and open up new opportunities for
studies at low redshift. The observations completed nominally.
1.2 Completed Three Sets of STIS/MA1/MA2 8843 (Cycle 9 MAMA Dark
Measurements)
The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to
perform the routine monitoring of the MAMA detector dark noise. The
proposal completed nominally.
1.3 Completed WF/PC-2 9124 (Mid-UV SNAPSHOT Survey of Nearby
Irregulars: Galaxy Structure and Evolution Benchmark)
The WF/PC-2 was used to investigate the relation between star
formation and the global physical characteristics of galaxies to interpret
the morphologies of distant galaxies in terms of their evolutionary
status. Distant galaxies are primarily observed in their rest frame
mid-ultraviolet. They resemble nearby late-type galaxies, but are they
really physically similar classes of objects? It is proposed to address
this question through a SNAPSHOT survey in the 2 mid-UV filter F300W of 98
nearby late-type, irregular and peculiar galaxies. No problems were reported.
1.4 Completed STIS/MA1/MA2 8917 (MAMA Dispersion Solution Check)
The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to
determine wavelength dispersion solutions on a yearly basis as part of a
long-term monitoring program {implemented as Program 7651 in Cycle 7,
Program 8430 in Cycle 8 and 8859 in Cycle 9}. No anomalous activity was
reported.
1.5 Completed STIS/CCD/MA1 9098 (The Spectrum and the Light Curve of
the Nearest Millisecond Pulsar)
The Space Telescope Imaging Spectrograph (CCD and MA1) was used to
observe PSR J0437–4715 that is the nearest and the brightest millisecond
{recycled} pulsar, and the only one that has been well studied at X-ray/EUV
energies, where it has a strong pulsed signal. It is the most promising
candidate for detecting the first optical counterpart of a millisecond
pulsar. Thge observations completed with no reported problems.
1.6 Completed Eleven Sets of WF/PC-2 9244 (POMS Test Proposal: WFII
Parallel Archive Proposal Continuation)
The WF/PC-2 was used to perform a generic target version of the
Archival Pure Parallel program. The program will be used to take parallel
images of random areas of the sky, following the recommendations of the
Parallels Working Group. The observations completed with no anomalous
activity.
1.7 Completed WF/PC-2 9249 (POMS Test Proposal: WFII Backup Parallel
Archive Proposal II)
The WF/PC-2 was used to execute a POMS test proposal designed to
simulate scientific plans. The proposal completed with no reported problems.
1.8 Completed STIS/CCD/MA1 8956 (Pre-SM Calibration)
The Space Telescope Imaging Spectrograph (CCD and MA1) was used in
an exercise to prepare for the SMOV-3B program. Prior to SMOV3B, one
iteration of proposal 8960 {Jitter Test} for WD 2126+734 will be
performed. Also one iteration of 8961 {End of BEA Test} for each new flux
standard {WD 2126+734, WD 0320-539, WD 0710+741, and WD 0214+568} needed to
completely cover all possible Bright Earth Avoidance {BEA} dates will be
exercised. Finally, one extra standard is added {WD 1407-475} to fill the
gap around June when WD 0214+568 is too close to the Sun. This iteration
of the proposal completed with no reported problems.
1.9 Completed 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. As described in 2.1 and HSTAR 8315, the acquisition and the
re-acquisition for this proposal defaulted to fine lock backup on one FGS
only, possibly affecting all observations. Otherwise, the proposal
completed uneventfully.
1.10 Completed WF/PC-2 9138 (Host Galaxies of Gravitationally Lensed
Quasars)
The WF/PC-2 was used to perform imaging studies of quasar host
galaxies at high redshift that are biased toward detecting luminous
hosts. Gravitational lensing combined with optical and near-IR imaging
enhances their detectivity and has nearly doubled the number of known hosts
at z>1. Lens studies have successfully imaged hosts with lower
luminosities at farther distances beneath a larger fraction of quasars than
imaging of non- lensed quasars. We propose deep WFPC2 follow-up imaging of
five lensed systems in the F555W and F814W filters, which offer unique
opportunities for detailed studies of faint, high-redshift, quasar
hosts. As described in 2.1 and HSTAR 8315, the acquisition and the
re-acquisition for this proposal defaulted to fine lock backup on one FGS
only, possibly affecting all observations. Otherwise, the proposal
completed as planned.
1.11 Completed FGS/1 8616 (Masses of Pre-Main Sequence Binaries)
Fine Guidance Sensor #1 was used to continue mapping the orbits of
young star binaries in the Taurus and Ophiuchus star forming regions. Our
goal is to measure their masses dynamically. This is important because
there are still no low mass young stars with reliably known masses so
calculations of their evolution to the main sequence are
uncalibrated. There were no reported problems.
1.12 Completed Five Sets of STIS/CCD 9285 (POMS Test Proposal: STIS
Non-scripted Parallel Proposal Continuation III)
The Space Telescope Imaging Spectrograph (CCD) was used to make low
galactic latitude, non-scripted parallel observations as part of a POMS
test proposal. The observations were completed as planned, and no
anomalies were reported.
1.13 Completed WF/PC-2 9045 (The Relationship Between Radio Luminosity
and Radio-Loud AGN Host Galaxy Properties)
The WF/PC-2 was used to determine the relationship between the
properties of the host galaxies of radio-loud AGN and their radio
luminosities. Previous studies in this area with the HST have concentrated
on the 3C sample which shows a tight correlation between luminosity and
redshift, such that evolutionary effects cannot be distinguished from those
depending upon radio luminosity. Our sample of 46 radio galaxies at z ~
0.5 comes from four complete, low-frequency-selected samples of radio
sources with differing flux limits. Thus the total sample spans an
unprecedented three orders of magnitude in radio luminosity at a fixed
redshift interval. The proposal completed with no reported problems.
1.14 Completed Five Sets of STIS/CCD 8864 (CCD Dark Monitor-Part 2)
The Space Telescope Imaging Spectrograph (CCD) was used to monitor
the darks for the CCD. The proposal completed nominally.
1.15 Completed Three Sets of STIS/CCD 8865 (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, to build up high-S/N superbiases and track the evolution of hot
columns. The proposal completed with no anomalous activity.
1.16 Completed Two Sets of STIS/CCD/MA1/MA2 9176 (LMC Eclipsing
Binaries with Cepheid Components: The Key to the Extragalactic Distance Scale)
The Space Telescope Imaging Spectrograph (CCD, MA1 and MA2) was
used to determine the distance to the LMC and to observe the Cepheid P-L
that law form the backbone of the Cosmic Distance Scale and the
determination of H_degrees. Unfortunately, in spite of concerted efforts
of many investigators, the zero point of the Cepheid P-L law and the LMC
distance remain controversial and uncertain to ~10-15, using eclipsing
binaries {EBs} as “standard candles” to include two recently discovered
LMC eclipsing binaries {EBs} with Cepheid components. These observations
of these extraordinary systems hold the key to determining simultaneously
the Cepheid P-L zero point and the LMC distance, and to provide a direct
test of the Baade-Wesselink parallax method. There were no reported problems.
1.17 Completed Two Sets of WF/PC-2 8059 (POMS Test Proposal: Targeted
Parallel Archive Proposal)
The WF/PC-2 was used to observe the parallel opportunities
available in the neighborhood of bright galaxies are treated in a slightly
different way from the normal pure parallels. Local Group galaxies offer
the opportunity for a closer look at young stellar
populations. Narrow-band images in F656N can be used both to identify
young stars via their emission lines, and to map the gas distribution in
star-forming regions. The observations completed nominally.
1.18 Completed Five Sets of WF/PC-2 8828 (Cycle 9 Supplemental Darks pt3/3)
The WF/PC-2 was used to obtain three dark frames every day to
provide data for monitoring and characterizing the evolution of hot
pixels. The proposal completed with no reported problems.
1.19 Completed FGS/1 9168 (The Distances to AM CVn Stars)
Fine Guidance Sensor (FGS) #1 was used to determine the parallaxes
and proper motions of the five brightest of the seven known AM CVn
systems. AM CVn systems are binaries where mass is transferred from a
completely hydrogen-deficient, degenerate mass donor to a white dwarf
primary through a helium accretion disk. A better understanding of these
systems is crucial for a number of reasons: (1) to study the late stages of
binary evolution, (2) to study the effect of chemical composition on the
physics of accretion discs, (3) to estimate their contribution to the
Supernovae Ia rate, and (4) to estimate their contribution to the
gravitational radiation background. All observations completed with no
reported problems.
1.20 Completed Two Sets of WF/PC-2 9060 (Photometry of a Statistically
Significant Sample of Kuiper Belt Objects)
The WF/PC-2 was used to propel the physical study of KBOs forward
by performing accurate photometry at V, R, and I on a sample of up to 150
KBOs. The sample is made up of objects that will be observed at thermal
infrared wavelengths by SIRTF and will be used with those data to derive
the first accurate diameters and albedos for a large sample of KBOs. The
observations completed nominally.
1.21 Completed STIS/CCD/MA1 9137 (Quasar Absorbers and Large Scale
Structure)
The Space Telescope Imaging Spectrograph (CCD and MA1) was used to
perform spectroscopy of 15 bright quasars in a 22 square degree region
that has well-sampled galaxy redshifts. No problems were encountered.
1.22 Completed Two Sets of 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. The proposal completed nominally.
1.23 Completed Two Sets of STIS/CCD 8924 (PSF and LP Filter Curve
Calibration)
The Space Telescope Imaging Spectrograph (CCD) was used in an
attempt to tie down the wavelength dependence of the CCD imaging
sensitivity. To do this, it is necessary to have good photometric imaging
data in both 50CCD and F28X50LP for stars of a variety of colors for which
the spectral energy distribution is known with great accuracy. To fill in
a color gap in the data that meets these requirements, the proposer will
obtain spectra of a late F star for which extensive imaging data is
available, and also will obtain both spectra and deep dithered CCD images
of an early K star. No problems occurred.
1.24 Completed Three Sets of WF/PC-2 8941 (Cycle 10 UV Earthflats)
The WF/PC-2 was used to monitor flat field stability by obtaining
sequences of earth streak flats to improve the quality of pipeline flat
fields for the WFPC2 UV filter set. The proposal had no problems.
1.25 Completed STIS/CCD 9128 (A Snapshot Survey of Absorption Lines
from High Velocity Clouds in the Milky Way)
The Space Telescope Imaging Spectrograph (CCD) was used to search
for Mg II and Mg I absorption from Galactic High Velocity Clouds {HVCs}
along the sightlines of 51 of the brightest QSOs, BL Lacs and Seyfert 2
galaxies in the sky. The observations completed with no rpeorted problems.
1.26 Completed STIS/CCD/MA1/MA2 8857 (MAMA Sensitivity and Focus
Monitor C9)
The Space Telescope Imaging Spectrograph (CCD, MA1 and MA2) was
used to monitor the sensitivity of each MAMA grating mode to detect any
change due to contamination or other causes. There were no problems.
1.27 Completed STIS/CCD/MA1 9154 (Spatial Distribution Of The Gas
Inside The Beta Pic Disk)
The Space Telescope Imaging Spectrograph (CCD and MA1) was used to
investigate the gas and dust disk surrounding Beta Pictoris that will give
clues to the understanding of the late stages of planetary
formation. There was no anomalous activity.
1.28 Completed STIS/CCD 9121 (Evolution of the Host Galaxies in Low-
Power AGN)
The Space Telescope Imaging Spectrograph (CCD) was used to study
the evolution of low-power AGN host galaxies to z~1.3, allowing the direct
study of how the formation and life cycles of radio-loud AGN depend on
intrinsic power. There were no reported problems.
1.29 Completed WF/PC-2 9135 (A New High-Z Galaxy Cluster with
Extraordinary Lensed Arcs From Multiple Sources)
The WF/PC-2 was used to observe strong lensing by a relatively high
redshift {z~0.7} cluster in the Red-Sequence Cluster. This lens system has
more bright arcs, with better cluster azimuthal coverage than examples of
lower z lenses previously imaged. At least 4 separate arcs are detected in
our initial survey data, at 3-4 different cluster-centric radii and hence
likely corresponding to at least 3 different background sources at 3
different redshifts. Moreover, these arcs are relatively bright and hence
redshifts should be readily obtainable using 8m class telescopes. All
observations completed normally.
1.30 Completed WF/PC-2 9267 (Supernova Search)
The WF/PC-2 was used to search for high-redshift supernovae in
GO-observed fields, taking advantage of good first-epoch observations and
of the scheduling opportunities available because STIS is not currently
observing. No anomalous activity was reported.
2.0 FLIGHT OPERATIONS SUMMARY:
2.1 Guide Star Acquisitions:
Scheduled Acquisitions: 21
Successful: 21
The acquisition at 236/143500Z and the re-acquisition at 236/1605Z
defaulted to fine lock backup on FGS-3 only. HSTAR 8315 was written. The
proposals detailed in 1.9 and 1.10 may have been affected.
Scheduled Re-acquisitions: 23
Successful: 23
2.2 FHST Updates:
Scheduled: 51
Successful: 51
2.3 Operations Notes:
Using ROP SR-1A, the SSR EDAC error counter was cleared nine times.
ROP DF-18A was utilized twice to reset the 486 engineering status
buffer.
Two TTRs were written when re-transmits were required at 236/1306Z
and at 236/2010Z during NSSC-1 loads. In each case, SI C&DH errors were
reset per ROP NS-5.
Re-dumps of science data were executed at 238/2336Z and at
238/2338Z as directed by ROP SR-1A.
3.0 SIGNIFICANT FORTHCOMING EVENTS:
GSFC Internal Simulation #13 (Rendezvous/Capture) will occur today,
beginning at 8:00 am and continuing until approximately 6:00 pm.
Continuation of normal science observations and calibrations.
