Hubble Space Telescope Daily Report #3176 – 12 Aug 2002

HUBBLE SPACE TELESCOPE

DAILY REPORT        # 3176
PERIOD COVERED: DOY 221-223
OBSERVATIONS SCHEDULED (see HSTARS below for possible observation problems)
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.
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.
ACS 9665
Extreme Red Stars
ACS provides unprecedented sensitivity in the far red, this coupled with

recent

astronomical pushes to ever cooler objects {e.g. new classifications for L

and T

stellar dwarfs, and extremely high redshift galaxies} increases the need for

extending the photometric calibration to include such objects. We propose

observations of 4 stellar objects for which excellent ground based optical

and

near-IR data exist that span V-I colors of 4.5 at M7 to > 6.0 at L5.
ACS 9395
Is Bulge Formation Still Going-On? An ACS Survey of Pseudo-Bulges
Pseudo-bulges, i.e., bulges with an exponential light profile, have been

unveiled in the centers of many intermediate-type disks. Their structural

similarity with the disks provides support to theoretical scenarios in which

bulges may form due to secular evolution processes within the host disks. If

at

play, these processes would likely be active throughout a large fraction of

cosmic history down to our days: `young' bulges should exist. Our previous

HST

WFPC2 and NICMOS survey of ~100 spirals has provided V-H colors for 11 Sb-Sc

pseudo-bulges, and these could be interpreted as suggestive of relatively

young

stellar ages. Furthermore, dense nuclei have been discovered in these

pseudo-bulges, and their V-H colors may imply stellar masses sufficiently

large

to activate the formation of the pseudo- bulge by means of dynamical

dissolution

of progenitor bars. However, the V-H color, on its own, is fully degenerate

towards stellar ages, metallicities and masses, as well as dust content. We

therefore propose to use ACS to observe the 11 pseudo-bulges of our combined

WFPC2 and NICMOS sample in the F330W, F435W, and F814W filters. Extending

the

wavelength baseline to the bluer passbands is essential to break the

mass-age-metallicity-dust degeneracy, and will provide far more accurate

estimates for the stellar population properties of the pseudo-bulges and

their

nuclei. Proving the existence of `young' bulges in the local Universe would

have

a big impact in our understanding of the formation of the Hubble sequence.
ACS 9563
Preliminary ACS Sensitivity
A spectrophotometric standard star is observed through a popular subset of

filters of each camera to assess the sensitivity of the instrument. The star

is

placed at the centre of the aperture, and two images are taken through each

filter. This programme is based on proposal 9020 designed for SMOV. There

are

three groups of visits, numbered respectively 1 through 3, 4 through 6 and 7

through 9. The three visits in each group must be executed about one month

apart

from one another, as indicated in the visit requirements. The first visit in

each group {namely visits 1, 4 and 7} ought to be scheduled during the month

of

July 2002. During SMOV the standard star GD71 could be used, which is not

visible during the Cycle 11 interim calibration period. We have selected

GRW+705824 instead. The latter is a WD slightly brighter than GD71 in V but

with

very similar spectral properties. The exposure times with this object have

been

selected to reach, on average, SNR~350 in the central pixel for broad band

filters.
ACS 9425
The Great Observatories Origins Deep Survey: Imaging with ACS
We propose a Treasury program of ACS imaging as part of the Great

Observatories

Origins Deep Survey {GOODS}, covering 320{square}', or 32* the area of the

two

original WFPC2 HDFs, to within 0.5--0.8 mag of their depth in four ACS

bands,

BViz. The two GOODS fields, the Hubble Deep Field North and Chandra Deep

Field

South, are the premier deep survey areas from X-- ray to radio wavelengths.

ACS

data will provide unique angular resolution, sensitivity, and wavelength

coverage to close the gap between the deepest Chandra and SIRTF

observations.

Supported by extensive imaging and spectroscopy from the VLT, Keck, Subaru,

NOAO, Gemini, VLA, JCMT, and other facilities, the combined GOODS data set

will

make it possible to map the evolution of the Hubble sequence with redshift,

reconstruct the history of galaxy mass assembly, star formation and nuclear

activity from the epoch of reionization to the present, trace the growth of

density perturbations via cosmic shear, and, with properly phased z--band

observations, detect ~ 12 Type Ia supernovae at 1.2<z<1.8 to test the cosmic

acceleration and the presence of dark energy. All HST, SIRTF, Chandra, and

supporting GOODS data are non-- proprietary, with science--quality images

and

catalogs released on a timescale of months. This will constitute the

deepest,

largest, and most uniform panchromatic data set ever assembled to study the

distant universe.
ACS 9396
Young Cluster Systems in Two Super-Gas- Rich Mergers: Arp 220 and Arp 299
Massive young star clusters are found in large numbers within the mergers of

massive, gas-rich disk galaxies. The most outstanding and well studied case

is

in the nearby merging Antennae pair {Whitmore and colleagues}. These

systems may

give us our best hope to see directly the way in which globular clusters

formed

in the uniquely gas-rich protogalactic era of the universe. But, even in the

Antennae, the many hundreds of young clusters have a median mass which is

still

5 to 10 times smaller than the characteristic mass ~ 3 * 10^5 M_odot that

characterizes normal, old-halo globular clusters. To find objects closer to

the

mass range of ``true'' protoglobular clusters, we need mergers which are

still

more gas-rich than the Antennae and in which the gas has been collected into

more massive GMCs. Two excellent candidates are Arp 220 and Arp 299, both of

which are undergoing extremely high star formation rates and have > 10^10

M_odot

of molecular hydrogen compressed into their central few kpc. With the ACS

High

Resolution Camera we will obtain deep UBVI imaging of the active central

regions

of these galaxies, allowing us to trace the luminosities, colors, masses,

and

ages of the young star clusters within them.
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 9379
Near Ultraviolet Imaging of Seyfert Galaxies: Understanding the

Starburst-AGN

Connection
We propose a near-UV snapshot survey of 101 Seyfert galaxies using ACS/HRC

and

the filter F330W, a configuration which is optimal to detect faint star

forming

regions around their nuclei. These images will complement optical and

near-IR

images available in the HST archive, thus providing a panchromatic atlas of

the

inner regions of active galaxies, which we will use to study the

starburst-AGN

connection. The main goals of this proposal are: {1} Determine the frequency

of

circumnuclear starbursts in Seyferts, down to levels which cannot be

observed

from the ground; {2} characterize the observational {fluxes, colors,

structure,

sizes} and intrinsic {luminosities, masses, ages, global star-formation

rate}

properties of these clusters; {3} derive the luminosity functions of young

star

clusters around the nucleus of Seyferts and compare these results with those

from normal and starburst galaxies to determine their survival rate close

to the

AGN; {4} address questions about the relation between AGNs and starbursts,

like

the possible connection between the masses and luminosities of black holes

and

starbursts, and the implications for the evolution of the black holes and

their

host galaxy bulges. By adding UV images to the existing optical and near-IR

ones, this project will create an extremely valuable database for

astronomers

with a broad range of scientific interests, from the properties of the AGN

to

the properties of their host galaxies.
ACS/WFC/HRC 9562
Cycle 11 Internal Flat Field Stability.
The Advance Camera for Surveys (WFC and HRC) was used to obtain flat field

stability and characterization samples of the ACS filter set. Only internal

exposures using the calibration lamps were required.
ACS/WFPC2 9488
Cosmic Shear - with ACS Pure Parallel Observations
The ACS, with greater sensitivity and sky coverage, will extend our ability

to

measure the weak gravitational lensing of galaxy images caused by the large

scale distribution of dark matter. We propose to use the ACS in pure

parallel

{non- proprietary} mode, following the guidelines of the ACS Default Pure

Parallel Program. Using the HST Medium Deep Survey WFPC2 database we have

measured cosmic shear at arc-min angular scales. The MDS image parameters,

in

particular the galaxy orientations and axis ratios, are such that any

residual

corrections due to errors in the PSF or jitter are much smaller than the

measured signal. This situation is in stark contrast with ground-based

observations. We have also developed a statistical analysis procedure to

derive

unbiased estimates of cosmic shear from a large number of fields, each of

which

has a very small number of galaxies. We have therefore set the stage for

measurements with the ACS at fainter apparent magnitudes and smaller, 10

arc-second scales corresponding to larger cosmological distances. We will

adapt

existing MDS WFPC2 maximum likelihood galaxy image analysis algorithms to

work

with the ACS. The analysis would also yield an online database similar to

that

in archive.stsci.edu/mds/
ACS/WFPC2 9481
Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS

Survey

Fields
In anticipation of the allocation of ACS high-latitude imaging survey{s}, we

request a modification of the default pure parallel program for those WFPC2

parallels that fall within the ACS survey field. Rather than duplicate the

red

bands which will be done much better with ACS, we propose to observe in the

near-ultraviolet F300W filter. These data will enable study of the

rest-frame

ultraviolet morphology of galaxies at 0<z<1. We will determine the

morphological

k-correction, and the location of star formation within galaxies, using a

sample

that is likely to be nearly complete with multi-wavelength photometry and

spectroscopic redshifts. The results can be used to interpret observations

of

higher redshift galaxies by ACS.
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 Dopler 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 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.
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.
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.
POMS 9677
POMS Test Proposal: WFII backup parallel archive proposal
This is a POMS test proposal designed to simulate scientific plans.
SNAP 9356
SNAPSHOT survey of the Planetary Nebulae population of the Galactic Bulge
The spectacular structures seen in HST images of planetary nebulae {PNe} are

generally accepted as originating from hydrodynamical interactions between

stellar winds: the interacting-stellar wind model {ISW}. Traditionally, the

shaping is thought to occur after the star becomes hot enough to ionize the

PN.

But recent HST images indicate that the shaping may occur earlier, and the

newer

GISW model puts the shaping during the pre-planetary nebula evolution. The

relative importance of both models is not known: GISW shaping will account

for

some fraction of PNe, but estimates range from 15--100 during the PN phase,

especially for the youngest PNe. We here propose an HST SNAPshot survey of

compact PNe in the Galactic Bulge, to test these predictions. The Bulge

provides

the only PNe population for which progenitor masses are known and nebular

ages

can be measured. In support of these HST measurements we have already

measured

velocity fields and emission line fluxes. The survey will give an unbiassed

sampling of morphologies, and allow evolutionary sequences to be determined

to

test the ISW versus the GISW model. By-products of the survey will be the

determination of nebular masses, diameters and filling factors. We will also

obtain the White Dwarf mass distribution in the Bulge, and the initial-final

mass function for low-mass stars.
STIS/CCD 8904
Bias Monitor-Part 2.
The Space Telescope Imaging Spectrograph (CCD) was used to monitor the bias

in

the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 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 8902
Dark Monitor-Part 2.
The Space Telescope Imaging Spectrograph (CCD) was used to monitor the

darks.
STIS/CCD 8906
Hot Pixel Annealing.
The Space Telescope Imaging Spectrograph (CCD) was used to measure the

effectiveness of the CCD hot pixel annealing process by measuring the dark

current behavior before and after annealing and by searching for any window

contamination effects. In addition, CTE performance is examined by looking

for

traps in a low signal level flat.
STIS/CCD 8928
PSFs at Pseudo-Apertures {Cycle 10}.
The Space Telescope Imaging Spectrograph (CCD) was used to perform

spectroscopic

PSF measurements, performed for the new pseudo-apertures located near CCD

row

900, which are made available to ameliorate CCD CTE losses.
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/CCD/MA2 9166
Fossil Gaseous Halos of Massive Galaxies at z~1.
The Space Telescope Imaging Spectrograph (CCD and MA2) was used to observe

host

galaxies of high-redshift, powerful radio sources that are likely the

progenitors of present-day gE and cD galaxies, and therefore provide

important

laboratories in which to investigate the formation of massive galaxies in

the

early Universe. Many high-redshift radio galaxies exhibit giant, Ly-alpha

halos.

Similar nebulae without associated radio sources have recently been

discovered

in a galaxy overdensity at z = 3.09. The LyAlpha luminosity of these halos

is

comparable to the total X-ray luminosities of low--z X--ray clusters, and

may

reflect the hot, cooling gas reservoir from which the galaxy/cluster is

forming.
WF/PC-2 9091
Evolution of Star Forming Environments in H II Regions.
The WF/PC-2 was used to look for evaporating gaseous globules and silhouette

disks in two young clusters and along one molecular cloud wall.
WFPC2 9393
Dynamics and Cloud Structure of Neptune
A 4-year gap in detailed observation of one of the most active planets in

our

solar system can be ended by our proposed multispectral WFPC2 imaging of

Neptune

over a period of 2 Neptune rotations. Our objectives are {1} mapping the

two-

dimensional distribution of Neptune's discrete cloud features and zonal

bands

with sufficiently dense longitudinal sampling to insure detection of any

Great

Dark Spot, or other major storm system, up to 35degrees N, {2}

characterizing

Neptune's circulation by tracking cloud motions during two densely sampled

half-rotations that ensure reliable target identification, and {4}

characterizing the vertical structure of clouds by imaging with filters that

select varying amounts of Rayleigh scattering and methane absorption and by

capturing their center-to-limb variations during intensely sampled feature

transits. To enhance the characterization of cloud structure we will also

propose coordinated groundbased IRTF and Keck observations,both using

adaptive

optics at near IR wavelengths that provide access to additional strong

methane

and hydrogen absorption bands. The proposed HST observations use the same

filters

as in 1996 and 1998, as well as additional filters, permitting detailed

comparisons with previous observations.
WFPC2 9599
WFPC2 Cycle 11 UV Earth Flats
Monitor flat field stability. This proposal obtains sequences of earth

streak

flats to improve the quality of pipeline flat fields for the WFPC2 UV filter

set. These Earth flats will complement the UV earth flat data obtained

during

cycles 8-10.
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.
WFPC2 8934
WFPC2 Decontaminations and Associated Observations Pt. 3/3
This proposal is 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, & darks}, UV throughput check,

VISFLAT sweep, and internal UV flat check.
FLIGHT OPERATIONS SUMMARY:
HSTARS (For details see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf)
HSTAR 8756:  CCS "G" String HSTPS alarming due to a process count of zero

on nascomd.

                       Under investigation.
HSTAR 8757:  NICMOS TPG reset @ 223/04:18:22Z.  NICMOS 736, 744, 639, 290,

588, and

                      two 604 Status Buffer messages received.  NICMOS was

in the middle of

                      Observation 9396 at time of reset.Under investigation.
HSTAR 8758:  CCS "G" String Backbone Data Server icon flashing red @

223/07:45Z.

                      Under investigation.
HSTAR 8759:  CCS "B" String can not copy config file from "B" String

(permission denied).

                       G. Gibson copied the file over for the FOT, they can

now transfer files

                       from a remote machine. Under investigation.
HSTAR 8760:  - Wing Panel Temperature (B_WPANLT) flagged yellow low

(-81.2765 ?C) for

                      42 seconds (7 samples)  @ 223/20:42:50Z.  Limit is

-80.0 ?C.Under investigation.
COMPLETED OPS REQs:

16817-0 - FN format to cover acquisitions and reacquisitions in SA217 SMS @

223/1811z
OPS NOTES EXECUTED: None
                           SCHEDULED     SUCCESSFUL    FAILURE TIMES

FGS GSacq                20                     20

FGS REacq                26                     26

FHST Update              47                     47

LOSS of LOCK
SIGNIFICANT EVENTS:
NICMOS experienced TPG, Detector 3  reset @ 223/04:18:22Z; similar to one

that

occurred on Day 213.  Unlike Day 213, NICMOS was observing on the detector

that experienced the reset, effecting 895 second multi-accumulator exposure

on Camera 3 which started at 223/04:12Z (Proposal 9484).  Five Status Buffer

messages were issued, first two were the result of the TPG reset, indicating

OOL condition and a TPG reset on Camera 3, respectively.  NICMOS camera was

successfully recovered by SPC and subsequent observations executed as

expected.
HST On-Orbit Checkout of real-time WSC interface scheduled daily 224 - 231

with

GDOC, STOCC Ops (SIMOR), HITT, and CCS using CCS "G" String with CCS

Release 4.0.1

and PRD D06100R2.  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.