Hubble Space Telescope Daily Report # 3183 – 21 Aug 2002

HUBBLE SPACE TELESCOPE

DAILY REPORT        # 3183
PERIOD COVERED: DOY 232
OBSERVATIONS SCHEDULED (see HSTARS below for possible observation problems)
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/CCD 8902
Dark Monitor-Part 2.
The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks.
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/MA1/MA2 8920
Cycle 10 MAMA Dark Measurements.
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.
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.
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.
FGS 9347
FGS Astrometry of the Extrasolar Planet of Epsilon Eridani
We propose observations with HST/FGS in Position Mode to determine the

astrometric elements {perturbation orbit semimajor axis and inclination} of the

candidate extra-solar planet around the K2 V star Epsilon Eridani that has been

detected by Doppler spectroscopy. These observations will also permit us to

determine the actual mass of the planet by providing the sin{i} factor

which can

not be determined with the radial velocity method. High precision radial

velocity {RV} measurements spanning the years 1980.8–2000.0 for the nearby

{3.22 pc} star Epsilon Eri show convincing variations with a period of ~ 7 yrs.

These data represent a combination of six independent data sets taken with four

different telescopes. A least squares orbital solution using robust estimation

yields orbital parameters of period, P = 6.9 yrs, velocity K- amplitude = 19

m/s, eccentricity e = 0.6, projected companion mass M_B sin{i} = 0.83

M_Jupiter.

An estimate of the inclination yields a perturbation semi-major axis, Alpha =

0arcs0022, easily within the reach of HST/FGS astrometry.
NICMOS 9360
Paschen-alpha Imaging of a SIRTF-Selected Nearby Galaxy Sample
We propose to carry out a NICMOS snapshot survey in the Paschen-alpha {PAlpha}

emission line and H-band of the sample of galaxies being observed at 3.5 — 160

microns as part of SIRTF Nearby Galaxies Survey {SINGS} and a related

guaranteed

time survey of starburst galaxies. The PAlpha images, accessible only from HST,

will be combined with groundbased HAlpha imaging to measure the extinction in

the star-forming centers of these galaxies, and obtain robust, extinction-

corrected maps of the massive star formation rate {SFR}. The PAlpha data by

themselves will provide reliable `extinction- free’ SFRs, and a

cross-calibration of the {dust–affected} HAlpha– and UV–based SFRs. The

PAlpha–based SFR measurements will extend the SFR-vs.-gas density law

{Schmidt–law} to surface densities at least 30 times higher than what is

accessible using HAlpha–based SFR measurements alone, bridging the gap between

normal galaxies and IR–luminous starbursts. Furthermore, the combination

of the

HST PAlpha images with the SIRTF images and spectra, as well as ancillary

ground–based UBVRIJHK images and GALEX UV images being obtained as part of the

SINGS project, will provide a definitive study of the radiative transfer of

starlight and dust heating in star–forming galaxies. The processed NICMOS

images will be incorporated into the public SINGS Legacy Data Archive, to

enable

scores of follow-up studies by the astronomical community at large.
NICMOS 9366
H_2 Imaging of Proto-Planetary Nebulae: Probing the Dynamics and Morphology
H_2 emission provides an excellent probe of the physical conditions in

planetary

nebulae {PNs} and also in proto- planetary nebulae {PPNs}, objects in

transition

between the asymptotic giant branch {AGB} and PN phases. It is thought that the

shaping of the PN occurs when a fast wind interacts with the remnant of the AGB

progenitor during the PPN phase. The study of shock-excited H_2 in PPNs will

allow us to study this process. We request HST/NICMOS H_2 and complementary K

and H broad-band images of 13 PPNs with a range of spectral types of the

central

star. We presently have very high- resolution {~100, 000} H_2 spectra for 7 of

these, which we will use with the high-resolution images to study the velocity

structure of the fast wind. We will also explore the relationship between the

presence of H_2 and a bipolar shape for the nebula, as has been found in PNs.

However, the role of the equatorial torus is expected to be different in these

two cases, and in the PPNs it is expected to collimate the wind rather than

shield the molecules. Thus the H_2 in the PPNs is expected at the ends of the

lobes rather than in the torus. Radiatively-excited H_2 emission appears to be

common in PPNs with central stars of B spectral types; this appears to be a

transitional stage in the evolution of the H_2 in the nebula which these images

will help us to better understand.
SNAP/STIS 9434
A SNAPSHOT Survey of the Hot Interstellar Medium
We propose to obtain SNAPSHOT STIS echelle observations of key tracers of hot

interstellar gas {CIV, NV and SiIV} for selected FUSE Team OVI survey targets

with known UV fluxes. By taking advantage of the SNAPSHOT observing mode we

will

efficiently obtain a large number of spectra suitable for the study of the

highly ionized hot component of the interstellar medium {ISM}. Our goals are to

explore the physical conditions in and distribution of such gas, as well as to

explore the nature of the interfaces between the hot ISM and the other

interstellar gas phases. Using inter–comparisons of the various ionic ratios

for CIV, NV, OVI and SiIV, we will be able to discriminate between the various

models for the production of the highly ionized gas in the Galactic ISM. The

survey will also enable detailed studies of regions already known to

contain hot

gas through X-ray emission measurements {e.g., SNRs and radio loops}. The

proposed SNAPSHOT observations will extend our previous Cycle 9 survey {which

was compromised by the STIS side 1 failure}, and should roughly double the

number of stars for which high quality STIS observations of the important hot

gas tracers are available, enabling us to derive a truly global view of the hot

ISM.
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.
GO 9449
UV Spectrum of the Massive X-ray Binary LS 5039
LS 5039 is a massive X-ray binary with non-thermal radio emission, relativistic

jets, and probably high energy Gamma- ray emission. It appears to be one of the

closest of the Galactic microquasars, stellar-sized engines that produce

relativistic jets like extragalactic quasars. We recently discovered that the

system is a 4.1 day binary with a very eccentric orbit {indicating large mass

loss in the supernova event that gave birth to the system}. The companion is

probably a neutron star, but a black hole companion is viable if the system

inclination is small. Here we propose to obtain the first UV observations

of the

binary to determine fundamental properties about the O6.5 V{{f}} optical star

and the mass transfer process. The UV spectrophotometry will allow us to

measure

accurately the interstellar extinction and system distance, and the unreddened

spectrum will provide information on the optical star’s effective temperature,

spectral classification, and surface abundances. The stellar wind lines in the

FUV provide the means to measure the O- star’s wind terminal velocity and mass

loss rate, and these parameters will allow us to determine if the X-ray

luminosity can be generated by wind accretion alone. We plan to observe these

wind lines at both orbital conjunction phases to search for evidence of changes

in the wind structure caused by proximity to the X-ray source’s radiation

field,

accretion disk wind, and jets.
ACS 9472
A Snapshot Survey for Gravitational Lenses among z >= 4.0 Quasars
Over the last few years, the Sloan Digital Sky Survey has revolutionized the

study of high-redshift quasars by discovering over 200 objects with redshift

greater than 4.0, more than doubling the number known in this redshift

interval.

The sample includes eight of the ten highest redshift quasars known. We propose

a snapshot imaging survey of a well-defined sample of 250 z > 4.0 quasars in

order to find objects which are gravitationally lensed. Lensing models

including

magnification bias predict that at least 4% of quasars in a flux-limited sample

at z > 4 will be multiply lensed. Therefore this survey should find of order 10

lensed quasars at high redshift; only one gravitationally lensed quasar is

currently known at z > 4. This survey will provide by far the best sample to

date of high-redshift gravitational lenses. The observed fraction of lenses can

put strong constraints on cosmological models, in particular on the

cosmological

constant Lambda. In addition, magnification bias can significantly bias

estimates of the luminosity function of quasars and the evolution thereof; this

work will constrain how important an effect this is, and thereby give us a

better understanding of the evolution of quasars and black holes at early

epochs, as well as constrain models for black hole formation.
ACS 9480
Cosmic Shear With ACS Pure Parallels
Small distortions in the shapes of background galaxies by foreground mass

provide a powerful method of directly measuring the amount and distribution of

dark matter. Several groups have recently detected this weak lensing by

large-scale structure, also called cosmic shear. The high resolution and

sensitivity of HST/ACS provide a unique opportunity to measure cosmic shear

accurately on small scales. Using 260 parallel orbits in Sloan textiti {F775W}

we will measure for the first time: beginlistosetlength sep0cm

setlengthemsep0cm

setlength opsep0cm em the cosmic shear variance on scales <0.7 arcmin, em the
skewness of the shear distribution, and em the magnification effect. 
endlist Our
measurements will determine the amplitude of the mass power spectrum
sigma_8Omega_m^0.5, with signal-to-noise {s/n} ~ 20, and the mass density
Omega_m with s/n=4. They will be done at small angular scales where non-linear
effects dominate the power spectrum, providing a test of the gravitational
instability paradigm for structure formation. Measurements on these scales are
not possible from the ground, because of the systematic effects induced by PSF
smearing from seeing. Having many independent lines of sight reduces the
uncertainty due to cosmic variance, making parallel observations ideal.

NICMOS 9484

The NICMOS Parallel Observing Program

We propose to manage the default set of pure parallels with NICMOS. Our
experience with both our GO NICMOS parallel program and the public parallel
NICMOS programs in cycle 7 prepared us to make optimal use of the parallel
opportunities. The NICMOS G141 grism remains the most powerful survey tool for
HAlpha emission-line galaxies at cosmologically interesting redshifts. It is
particularly well suited to addressing two key uncertainties regarding the
global history of star formation: the peak rate of star formation in the
relatively unexplored but critical 1<= z <= 2 epoch, and the amount of star
formation missing from UV continuum-based estimates due to high extinction. Our
proposed deep G141 exposures will increase the sample of known HAlpha emission-
line objects at z ~ 1.3 by roughly an order of magnitude. We will also obtain a
mix of F110W and F160W images along random sight-lines to examine the space
density and morphologies of the reddest galaxies. The nature of the extremely
red galaxies remains unclear and our program of imaging and grism spectroscopy
provides unique information

regarding both the incidence of obscured star bursts and the build up of 
stellar
mass at intermediate redshifts. In addition to carrying out the parallel 
program
we will populate a public database with calibrated spectra and images, and
provide limited ground- based optical and near-IR data for the deepest parallel
fields.

NICMOS 9485

Completing A Near-Infrared Search for Very Low Mass Companions to Stars within
10 pc of the Sun

Most stars are fainter and less massive than the Sun. Nevertheless, our
knowledge of very low mass {VLM} red dwarfs and their brown dwarf cousins is
quite limited. Unknown are the true luminosity function {LF}, multiplicity
fraction, mass function, and mass-luminosity relation for red and brown dwarfs,
though they dominate the Galaxy in both numbers and total mass. The best way to
constrain these relations is a search for faint companions to nearby stars. 
Such
a search has several advantages over field surveys, including greater
sensitivity to VLM objects and the availability of precise parallaxes from 
which
luminosities and masses can be derived. We propose to complete our four-filter
NICMOS snapshot search for companions to stars within 10 pc. With a 10 sigma
detection limit of M_J ~ 20 at 10 pc, we can detect companions between 10 and
100 AU that are at least 9 mag fainter than the empirical end of the main
sequence and at least 6.5 mag fainter than the brown dwarf Gl 229B. When
completed, our search will be the largest, most sensitive, volume-limited 
search
for VLM companions ever undertaken. Our four-filter search will permit
unambiguous identification of VLM-companion candidates for follow-up
observation. Together with IR speckle and deep imaging surveys, our program 
will
firmly establish the LF for VLM companions at separations of 1-1000 AU and the
multiplicity fraction of all stars within 10 pc.

STIS 9505

The Evolution of Molecular Clouds.

The combined STIS, FUSE and ground-based results will yield information needed
to understand the role of ablation in the evolution of the central clouds.

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 9565

ACS Post-SMOV UV Contamination Monitor

This programme continues the UV sensitivity monitoring campaign {ACS SMOV
proposal 9010} of the HRC and SBC after the end of the SMOV period.

ACS 9567

SBC Dark Current

Dark current measurements will be made for the ACS SBC once a week.

ACS/WFC 9584

ACS Default {Archival} Pure Parallel Program II.

The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels.

WFPC2 9634

POMS Test Proposal: WFII targeted parallel archive proposal

The parallel opportunities available with WFPC2 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. Thus, the filter F656N is added to the four standard filters. Near 
more
distant galaxies, up to about 10 Mpc, we can map the population of globular
clusters; for this purpose, F300W is less useful, and only F450W, F606W, and
F814W will be used.

ACS 9672

Grism/Prism Calibration

A Planetary Nebula in the LMC and two Galactic White Dwarfs are observed 
through
the prisms of the HRC and the SBC to measure: 1} the dispersion of the prisms
and its field dependence; 2} the prisms throughput and its field dependence.
Therefore, these measurements will be carried out at several positions on the
chip including the centre and the corners of the HRC and SBC chips.

WFPC2 9676

POMS Test Proposal: WFII parallel archive proposal

used to take parallel images of random areas of the sky, following the
recommendations of the 2002 Parallels Working Group.

POMS 9677

POMS Test Proposal: WFII backup parallel archive proposal

This is a POMS test proposal designed to simulate scientific plans.

FLIGHT OPERATIONS SUMMARY:

HSTARS (For details see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf)

HSTAR 8766 - Telemetry Bars on "A" string Reads 1  PCS Mnemonic Out of 
Limits @232/0303z
              CCS "A" String Telemetry Bar reads 1 PCS mnemonic OOL @ 
232/03:30Z,
              but when clicked on, there are no mnemonics violated. Under
              investigation.

COMPLETED OPS REQs:
16833-1 - Battery 1 Capacity Test Script @232/1800z (opened at 232/1851z)

OPS NOTES EXECUTED: None

                              SCHEDULED     SUCCESSFUL    FAILURE TIMES
FGS GSacq                  11                      11
FGS REacq                  3                        3
FHST Update                24                      24
LOSS of LOCK

Operations Notes:

SIGNIFICANT EVENTS:

Battery 1 Capacity Test started 232/18:43Z (OR 16833-1).
Discharge began nominally @ 232/22:07Z and is estimated to continue
for 14 - 16 hours.  EPS and SI SEs are monitoring test from the STOCC,
a follow-on Flash Report will issued after discharge is terminate.

NBL 02.3 (FGS 3, NOBL 5 (FF & RMS), STIK, filler - Parazynski,
Williams, Nicollier), Day 3 of 5, 7 am - 5 pm @ JSC NBL

HST On-Orbit Checkout of real-time WSC interface scheduled daily
231 - 238 with GDOC, STOCC Ops (SIMOR), HITT, and CCS using CCS
"G" String with CCS Release 4.0.1 and PRD O06100Q1.  The purpose
of this testing is to verify CCS Release 4.0.1 (IP) capability
to interface through the IP Packet Filters to WSC for real-time
telemetry and commands.