Hubble Space Telescope Daily Report #3025 – 2 Jan 2002
HUBBLE SPACE TELESCOPE
DAILY REPORT #3025
PERIOD COVERED: 0000Z (UTC) 12/27/01 – 0000Z (UTC) 01/02/02
Daily Status Report as of 002/0000Z
1.0 OBSERVATIONS SCHEDULED AND ACCOMPLISHED:
1.1 Completed Four Sets of 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. As documented in HSTAR 8448 and 2.1, the acquisition
for the fourth iteration of this proposal defaulted to fine lock back-up on
one FGS only, possibly affecting the observations in that
iteration. Otherwise, no further problems occurred.
1.2 Completed Twelve Sets of STIS/CCD 8901 (Dark Monitor-Part 1)
The Space Telescope Imaging Spectrograph (CCD) was used to monitor
the darks. There was no anomalous activity.
1.3 Completed Seven Sets of STIS/CCD 8903 (Bias Monitor – Part 1)
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. There were no problems.
1.4 Completed Five Sets of WF/PC-2 8932 (Decontaminations and
Associated Observations Pt. 1/3)
The WF/PC-2 was used for the monthly WFPC2 decons. Also included
are instrument monitors tied to decons: photometric stability check, focus
monitor, pre- and post-decon internals {bias, intflats, kspots, &and
darks}, UV throughput check, VISFLAT sweep, and internal UV flat check. No
problems were reported.
1.5 Completed STIS/CCD 9106 (The Biggest Black Holes)
The Space Telescope Imaging Spectrograph (CCD) was used to perform
searches for supermassive black holes in galaxy centers that have led to
the discoveries that {1} most or all hot galaxies contain massive dark
objects at their centers, presumably black holes; and {2} there is a tight
correlation between the black-hole mass and the luminosity-weighted
velocity dispersion of the hot component of the galaxy. This remarkable
relationship suggests a strong link between black-hole formation, AGN
activity, and galaxy formation, and once it is understood this link should
advance our understanding of all three processes. There were no reported
problems.
1.6 Completed Eighteen Sets of 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. As documented in HSTAR 8448 and 2.1, the
acquisition for the thirteenth iteration of this proposal defaulted to fine
lock back-up on one FGS only, possibly affecting the observations in that
iteration. Otherwise, there were no further reported problems.
1.7 Completed Ten Sets of WF/PC-2 8937 (Cycle 9 Supplemental Darks pt2/3)
The WF/PC-2 was used obtain three dark frames every day to provide
data for monitoring and characterizing the evolution of hot pixels. No
problems were encountered.
1.8 Completed STIS/CCD 8626 (Spatially Resolved Spectroscopy of
APM08279+5255)
The Space Telescope Imaging Spectrograph (CCD) was used to obtain
spatially resolved, high resolution spectra of the z=3.911 BAL quasar, APM
08279+5255. All observations completed nominally.
1.9 Completed Eleven Sets of WF/PC-2 8942 (Cycle 10 Intflat Sweeps and
Linearity Test)
The WF/PC-2 was used to monitor the pixel-to-pixel flatfield
response and provide a linearity check. These intflat sequences are done
once during the year and the images will provide a backup database in the
event of complete failure of the visflat lamp as well as allow monitoring
of the gain ratios. There were no reported problems.
1.10 Completed STIS/MA1 8920 (Cycle 10 MAMA Dark Measurements)
The Space Telescope Imaging Spectrograph (MA1) 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. The proposal completed with no
reported anomalous activity.
1.11 Completed STIS/CCD 9126 (Galaxy Mass and the Fate of Luminous,
Blue Compact Galaxies at z~0.6)
The Space Telescope Imaging Spectrograph (CCD) was used to obtain
long-slit spectra for a sample of 6 luminous, blue, compact galaxies
{LBCGs} at z ~ 0.6. Despite being very luminous, LBCGs have velocity
widths Sigma ~ 60 kms and half-light radii r_e ~ 0.5” {or R_e ~
3Kpc}. Small sizes and velocity widths suggest LBCGs are low- mass stellar
systems , while their blue colors, strong emission lines and low M/L-ratios
indicate they are undergoing a major starburst. I f the star-forming
process halts after the current burst, models predict that LBCGs will fade
by ~2-4 magnitudes after a few Gyrs to reach the low luminosities and
surface brightnesses characteristic of spheroidal galaxies. The proposal
completed with no reported problems.
1.12 Completed Six Sets of 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. The proposal completed uneventfully.
1.13 Completed Two Sets of 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.
1.14 Completed Six Sets of WF/PC-2 9118 (Tracing the Cosmic Expansion
to z>1 with Type Ia Supernovae)
The WF/PC-2 was used to observe type Ia supernovae in order to 1.15 Completed Four Sets of WF/PC-2 8941 (Cycle 10 UV Earthflats) The WF/PC-2 was used to monitor flat field stability by obtaining 1.16 Completed STIS/CCD 9110 (A Search for Kuiper Belt Object Satellites) The Space Telescope Imaging Spectrograph (CCD) was used to 1.17 Completed Two Sets of STIS/MA1 8590 (UV Imaging and Spectroscopy The Space Telescope Imaging Spectrograph (MA1) was used to observe 1.18 Completed Three Sets of WF/PC-2 8589 (Orbital Structure and Black The WF/PC-2 was used to observe the stellar orbital structure and 1.19 Completed Three Sets of WF/PC-2 9060 (Photometry of a The WF/PC-2 was used to propel the physical study of KBOs forward 1.20 Completed STIS/CCD 9084 (Physical Parameters of the Erupting The Space Telescope Imaging Spectrograph (CCD) was used to observe 1.21 Completed STIS/CCD 9131 (Imaging the Host Galaxies of High The Space Telescope Imaging Spectrograph (CCD) was used to complete 1.22 Completed STIS/CCD/MA2 9051 (Identifying Damped Lyman-alpha The Space Telescope Imaging Spectrograph (CCD and MA2) was used to 1.23 Completed STIS/CCD/MA2 9119 (Io’s Prometheus Plume, and the The Space Telescope Imaging Spectrograph (CCD and MA2) was used to 1.24 Completed STIS/MA2 8048 (Secular Changes in the Jet of M87) The Space Telescope Imaging Spectrograph (MA2) was to be used to 1.25 Completed STIS/CCD 9148 (Light Echos and the Nature of Type Ia The Space Telescope Imaging Spectrograph (CCD) was used to take 1.26 Completed Nine Sets of STIS/CCD 9285 (POMS Test Proposal: STIS The Space Telescope Imaging Spectrograph (CCD) was used to make low 1.27 Completed WF/PC-2 9320 (Constraining the Highly Eccentric Orbit of The WF/PC-2 was used to observe the Trans Neptunian Object {TNO} 1.28 Completed STIS/CCD/MA1/MA2 9153 (The Black Hole {?} in BG Gem) The Space Telescope Imaging Spectrograph (CCD, MA1 and MA2) was 1.29 Completed Two Sets of FGS/1 8946 (Pre-SM3B Observations for Fine Guidance Sensor #1 was used to monitor the characteristics of 1.30 Completed STIS/CCD 9139 (Variability in the UV Spectrum of 3C 279: The Space Telescope Imaging Spectrograph (CCD) was used to 1.31 Completed Three Sets of WF/PC-2 9257 (Cycle 10 Super-PSF) The WF/PC-2 was used to obtain deep images of the WFPC2 Point 1.32 Completed FGS/1 9407 (Astrometry of a Star Hosting an Extrasolar Fine Guidance Sensor #1 was used to determine the astrometric 1.33 Completed WF/PC-2 9309 (Supernova Search) The WF/PC-2 was used to search for high-redshift supernovae in 1.34 Completed Two Sets of WF/PC-2 8059 (POMS Test Proposal: Targeted The WF/PC-2 was used to observe the parallel opportunities 1.35 Completed Two Sets of WF/PC-2 8940 (Cycle 10 Earth Flats) The WF/PC-2 was used to monitor flatfield stability by obtaining 1.36 Completed STIS/CCD 8914 (Sensitivity Monitor C10) The Space Telescope Imaging Spectrograph (CCD) was used to monitor 1.37 Completed STIS/CCD 9280 (X-Ray Imaging of GPS and CSS Quasars) The Space Telescope Imaging Spectrograph (CCD) was used to conduct 2.0 FLIGHT OPERATIONS SUMMARY: 2.1 Guide Star Acquisitions: Scheduled Acquisitions: 48 Successful: 47 Scheduled Re-acquisitions: 41 Successful: 40 Per HSTAR 8445, the acquisition at 363/195140Z failed when the Per HSTAR 8448, the acquisition at 365/060611Z defaulted to fine 2.2 FHST Updates: Scheduled: 102 Successful: 100 As documented in HSTAR 8447, the full maneuver updates scheduled 2.3 Operations Notes: Using ROP SR-1A, the SSR-1 EDAC error counter was cleared eleven times. The CCS engineering status buffer limits were adjusted six times Per an operations request, telemetry diagnostics were performed at ROP IC-2 was used to turn SSA transmitter #2 on for the interval HSTAR 8444 document the fact that the telemetry point SMAELEXT (the The flight operations team transferred operations to the GSFC There were STIS EMC re-tries at 363/012213Z and at 364/045341Z. In HSTAR 8446 was written when real-time recoverable data was lost A TTR was written for a required re-transmit during a NSSC-1 load Another TTR was generated for a required re-transmit at 365/0918Z The STIS MCE-1 reset at 365/003426Z. The STIS flight software The SSR-3 EDAC error counter was cleared at 365/0925Z, using ROP SR-9A. A TTR was written for a needed re-transmit at 365/2014Z during a The ephemeris table was uplinked at 001/0028Z, using ROP DF-07A. An NSSC-1 status buffer dump was commanded at 001/2111Z as directed 3.0 SIGNIFICANT FORTHCOMING EVENTS: Continuation of normal science observations and calibrations.
provide evidence for an accelerating universe. The case for cosmic
acceleration rests almost entirely on the observation that the observed SN
Ia at z~0.5 are 0.25 magnitudes fainter than expected for a
non-accelerating Universe. It is proposed to follow five SN Ia in the
range 0.95
straightforward way to assess the reliability of the SN Ia
measurements. In addition, if SN Ia are reliable standard candles, the
proposed observations will significantly increase the precision with which
Omega_Lambda and Omega_M are measured. There was no reported anomalous
activity.
sequences of earth streak flats to improve the quality of pipeline flat
fields for the WFPC2 UV filter set. The proposal had no problems.
investigate whether the large number of collisions thought to have taken
place in the primordial Kuiper belt suggest that many Kuiper belt objects
{KBOs} could have suffered binary-forming collisions similar to that which
formed the Pluto — Charon binary. Detection of such KBO satellites would
allow measurement of KBO masses, would help to understand the past
collisional environment of the Kuiper belt, and would give a context to the
otherwise unique-seeming formation of the Pluto — Charon binary. The
proposal completed with no reported problems.
of Luminous Blue Compact Galaxies from z=0 to z=1)
two well-defined samples of low-mass starburst galaxies, one in the local
universe {z<0.1} and another at intermediate redshifts {0.2 < z <
0.7}. Both samples show optical sizes, morphologies, emission line widths,
and luminosities comparable to those of LBGs at z=3, and are therefore
probably the best local analogs and testbeds for further study of
LBGs. Our main goals are to: {1} explore the morphologies, surface
brightness distributions, and half-light radii of nearby starforming
galaxies in the FUV, near Ly-alpha; {2} search for systematic differences
among UV, optical, and near-IR morphologies and structural parameters; {3}
investigate the intrinsic emission and absorption spectra near Ly-alpha of
starbursting dwarf galaxies, with special attention to Ly- alpha profiles
and interstellar and stellar photospheric absorption from Si II, O I, C II,
Si IV, and C IV; {4} measure their FUV-optical colors and dust extinction
properties; and {5} test the hypothesis that low-mass starbursts are the
local counterparts of LBGs. The observation completed normally.
Hole in NGC 3379)
the mass of the central black hole in NGC 3379. The proposal completed
with no reported anomalies.
Statistically Significant Sample of Kuiper Belt Objects)
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.
Luminous Blue Variable NGC 2363-V1)
a bright variable star in the giant extragalactic H , ii region NGC 2363
discovered in 1992. Subsequent photometry and high quality spectroscopy of
this star revealed that observers are witnessing a significant event in the
evolution of a massive star, namely a major eruption of a Luminous Blue
Variable {LBV}. It is proposed to obtain high quality STIS spectra of this
star once a year for the next three observing Cycles. The proposal
completed nominally.
Redshift Type Ia Supernovae)
the snapshot survey of distant galaxies of known redshift which hosted
supernovae {SNe} of Type Ia found via the Supernova Cosmology Project
{SCP}. No problems were seen.
Galaxies at z~1)
look for damped Lyman-alpha absorption systems that contain the bulk of the
neutral gas in the Universe in the redshift range z = 0.5 – 5, yet the
nature of the galaxies responsible for the absorption is not well
understood. Only recently have observers found more than a handful of
damped absorbers at redshifts z < 1.5. Using the FIRST Bright Quasar
Survey {FBQS}, with over a 1000 quasars, the proposers have undertaken a
survey to build a complete picture of he nature of the galaxies responsible
for damped Lyman-alpha absorption systems at z~1 and to double the sample
size at this redshift. No problems were encountered.
Composition and Spatial Distribution of Io’s Atmosphere)
obtain the most detailed view yet of Io’s dynamic SO_2 / S_2 atmosphere,
and the first spectroscopic observations of a Prometheus-type plume, to
test models of plume and atmospheric chemistry and dynamics. The proposal
completed as planned.
continue the investigation of the M87 jet by studying proper motions and
structural changes of the jet. The proposal will track secular changes
and motions in the jet and nucleus. As detailed in HSTAR 8445 and 2.1, the
acquisition and re-acquisition for this proposal failed and all four
observations were lost.
Supernovae)
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.
Non-scripted Parallel Proposal Continuation III)
galactic latitude, non-scripted parallel observations as part of a POMS
test proposal. The observations were completed as planned, and no
anomalies were reported.
the Companion of the Binary TNO 1998 WW31 by Observations at its Pericenter)
1998 WW31 that has a satellite. These observations will assess the
ellipticity of the orbit in a definite way, providing an important
constraint to the models proposed for the creation of such a binary
system. No problems were reported.
used to acquire low resolution ultraviolet spectra of the long period black
hole binary candidate BG Geminorum. These spectra allow an unambiguous
test of the nature of the 4.5 M{sun} primary star, which makes no
measurable contribution to the optical spectrum. Detection of a strong
ultraviolet continuum or ultraviolet absorption lines from Si II and Si III
{among others} would indicate a B-type primary; failure to detect these
features or detection of high ionization emission lines would favor a black
hole primary. If it contains a black hole, BG Gem would be the longest
period black hole binary known {by a factor of ten}, challenging current
theories of black hole formation. It would also be the only eclipsing
binary known to contain a black hole, which would provide a unique
laboratory for testing accretion disk models for black hole binary
systems. The proposal completed as planned.
Verification of Operational FGS Calibrations)
the three Fine Guidance Sensors across the boundary of the servicing
mission SM3B. This proposal establishes the pre-SM3B baseline
measurements. No problems were encountered.
Testing Models for the Gamma-Ray Emission in Blazars)
determine whether gamma- rays are produced on the scale of the broad line
region, using multi-epoch UV snapshots of 3C 279 to find and characterize
its LyAlpha variability. This will validate the mirror model for
generating the intense gamma-ray emission from blazars. 3C 279 is the
best-studied blazar from radio to gamma-ray wavelengths, showing frequent
large flares over days to months. Variability in the UV continuum and
LyAlpha will directly reveal any coupling between the jet ionizing flux and
the broad-line region emission, providing clues to the physics and
energetics of all radio-loud AGN. All observations completed without
reported incident.
Spread Function (PSF) in several broadband filters in order to investigate
the 2-dimensional structure in the PSF wings and characterize the change in
structure with varying focus and target color. There were no reported
problems.
Planet: The Mass of Upsilon Andromedae)
elements {perturbation orbit semimajor axis and inclination} produced by
the outermost extra-solar planet orbiting the F8V star Upsilon
Andromedae. These observations will permit us to determine the actual mass
of the planet by providing the presently unknown sin i factor intrinsic to
the radial velocity method which discovered this object. An inclination, i
= 30degrees, within the range of one very low precision determination using
reanalyzed HIPPARCOS intermediate data products, would produce the observed
radial velocity amplitude, K = 66 ms with a companion mass of ~8 M_Jupiter.
Such a mass would induce in Upsilon Andromedae a perturbation semi-major
axis, Alpha = 0arcs0012. The proposed observations will yield a planetary
mass, rather than, as previous investigations have done, only suggest a
planetary mass companion. The proposal completed nominally.
GO-observed fields, taking advantage of good first-epoch observations. All
observations completed nominally.
Parallel Archive Proposal)
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
sequences of Earth streak flats to construct high quality flat fields for
the WF/PC-2 filter set. These flat fields will allow mapping of the OTA
illumination pattern and will be used in conjunction with previous internal
and external flats to generate new pipeline superflats. The proposal
completed without incident.
the sensitivity of each CCD grating mode to detect any change due to
contamination or other causes. The STIS focus is also monitored in an
imaging mode. There was no anomalous activity.
a survey of GPS and CSS radio-loud quasars, by studying their arcsecond
structure in the X-rays, by searching for X-ray jets, and by searching for
signatures of intermittent AGN activity. The proposal completed nominally
search radius limit for both FGS-2 and FGS-3 was exceeded. The subsequent
re-acquisition at 383/200919Z also failed. The proposal described in 1.24
was affected.
lock back-up on FGS-3 only when the scan step limit was exceeded on
FGS-1..The proposals described in 1.1 and 1.6 may have been affected.
for 364/164614Z and 364/164859Z failed due to tracker #3. Subsequent
acquisitions were successful.
per ROP DF-18A.
362/0030Z in order to obtain RWA data.
362/0941Z to 362/1003Z.
MCE-A Electronics temperature) flagged out-of-limits high at 49.09 degC
(the high limit being 49.0 degC). Per agreement with the Systems Engineer,
the ground system limit was adjusted to 51.5 degC.
back-up facility from 363/1200Z to 364/0000Z to allow for repair of the
main power switchgear at the STScI.
each case, ROP NS-12 was used to reset the STIS flight software error counter.
from 364/025615Z to 364/030941Z due to currently unknown CCS problems. The
data was subsequently unsuccessfully recovered by a line outage recorder
playback performed at 365.2340Z.
at 364/1317Z. ROP NS-5 was used at 364/1322Z to reset the SI C&DH error
counter.
during a 486 uplink.
error counter was reset at 365/0043Z per ROP NS-12. MAMA-1 was recovered
at the time of the following high voltage on commanding in the SMS.
NSSC-1 load. The SI C&DH error counter was reset at 365/2020Z per ROP NS-5.
by ROP NS-3.
