DAILY REPORT # 4156

HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT # 4156

PERIOD COVERED: UT July 14,15,16, 2006 (DOY 195,196,197)

OBSERVATIONS SCHEDULED

NIC1/NIC2/NIC3 8794

NICMOS Post-SAA calibration - CR Persistence Part 5

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. The keyword 'USEAFTER=date/time' will also be added to
the header of each POST-SAA DARK frame. The keyword must be populated
with the time, in addition to the date, because HST crosses the SAA ~8
times per day so each POST-SAA DARK will need to have the appropriate
time specified, for users to identify the ones they need. Both the raw
and processed images will be archived as POST-SAA DARKSs. Generally we
expect that all NICMOS science/calibration observations started within
50 minutes of leaving an SAA will need such maps to remove the CR
persistence from the science images. Each observation will need its
own CRMAP, as different SAA passages leave different imprints on the
NICMOS detectors.

ACS/HRC 10923

Measuring the size of the close-in transiting extrasolar planet HD
189733b

A new transiting exoplanet was found by our radial velocity search
around the bright K dwarf HD 189733. With an apparent V magnitude of
7.67 and a distance of 19 pc, it is the closest star known with a
transiting extrasolar planet. Moreover, the high radius ratio {Rpl/R ~
0.17} makes it a uniquely favorable target for exoplanet studies. This
planet is set to become the most observed hot Jupiter and a landmark
in the understanding of hot Jupiter structure and formation. We
propose a fundamental observations with the HST: to measure precisely
the size of the transiting planet around HD189733 and the inclination
angle of its orbit. The radius is an important characteristic of the
planet in itself. A precise, model-independent radius determination is
also a necessary prerequisite for further observations of the system
with ground-based large telescopes and Spitzer {e.g. to detect
reflected light and intrinsic infrared light from the planet, to
measure the Rossiter- McLaughlin effect}. This observation requires a
high-accuracy spectrophotometry light curve with ACS in the visible.
Similar observations for the formerly closest transiting planet, HD
209458b, have revealed that the planet was much larger than accounted
for by any model, and undergoing strong evaporation, two observations
that have had a profound impact on our understanding of the structure
of close-in exoplanets and the migration process.

FGS 10912

Trigonometric Calibration of the Distance Scale for Classical Novae

The distance scale for classical novae is important for understanding
the stellar physics of their thermonuclear runaways, their
contribution to Galactic nucleosynthesis, and their use as
extragalactic standard candles. Although it is known that there is a
relationship between their absolute magnitudes at maximum light and
their subsequent rates of decline--the well-known maximum-magnitude
rate-of-decline {MMRD} relation--it is difficult to set the zero-point
for the MMRD because of the very uncertain distances of Galactic
novae. We propose to measure precise trigonometric parallaxes for the
quiescent remnants of the four nearest classical novae. We will use
the Fine Guidance Sensors, which are proven to be capable of measuring
parallaxes with errors of ~0.2 mas, well below what is possible from
the ground.

WFPC2 10767

Further Resolving the Puzzle of Hybrid Star X-rays

Do Alpha TrA {K2II} and Beta Ind {K1II} have previously unrecognized
X-ray active dwarf companions, leading us astray concerning the
coronal properties of the "hybrid-chromosphere" class? Establishing
the true X-ray luminosities of the hybrids is a basis for
understanding magnetic field generation in evolved supergiants, the
driving of their winds, and the seeding of coronal conditions in their
extended outer envelopes. It also bears on the issue of late-type
dwarfs orbiting main sequence B stars, the evolutionary predecessors
of K bright giants. We propose to directly image the putative hybrid
companions using Chandra, with supporting observations from HST/WFPC2.

ACS/WFC 10760

Black Hole X-ray Novae in M31

We have been carring out a Chandra {GO+GTO} and HST {GO} program to
find Black Hole X-ray Nova {BHXN} and their optical counterparts in
M31 for several years. To date we have found 2 dozen BHXN and 3 HST
optical counterparts for these BHXN. Our results suggest a rather high
ratio of BH to neutron star {NS} binaries, or a high duty cycle for
the BHXN. We propose to continue this program, with the goal of
determining the orbital period distribution and duty cycles of these
BHXN. Current results yield 3 orbital periods and 2 upper limits. Our
proposed observations will ~double the total number of periods and
therefore yield sufficient numbers to make a first approximation of
the orbital period distribution. The orbital period distribution is
the fundamental observable parameter any binary stellar evolution
models must match, and the duty cycle is very poorly known but
directly influences the binary lifetime. M31 is the only galaxy in
which this extra- galactic study of BHXN is feasible.

ACS/HRC/WFC 10758

ACS CCDs daily monitor

This program consists of a set of basic tests to monitor, the read
noise, the development of hot pixels and test for any source of noise
in ACS CCD detectors. The files, biases and dark will be used to
create reference files for science calibration. This programme will be
for the entire lifetime of ACS. Changes from cycle 13:- The default
gain for WFC is 2 e-/DN. As before bias frames will be collected for
both gain 1 and gain 2. Dark frames are acquired using the default
gain {2}. This program cover the period May, 31 2006- Oct, 1-2006. The
first half of the program has a different proposal number: 10729.

ACS/HRC 10738

Earth Flats

Sky flats will be obtained by observing the bright Earth with the HRC
and WFC. These observations will be used to verify the accuracy of the
flats currently in the pipeline and to monitor any changes. Weekly
coronagraphic monitoring is required to assess the changing position
of the spots.

ACS/HRC/WFC 10733

CCD Hot Pixel Annealing

Hot pixel annealing will continue to be performed once every 4 weeks.
The CCD TECs will be turned off and heaters will be activated to bring
the detector temperatures to about +20C. This state will be held for
approximately 6 hours, after which the heaters are turned off, the
TECs turned on, and the CCDs returned to normal operating condition.
To assess the effectiveness of the annealing, a bias and four dark
images will be taken before and after the annealing procedure for both
WFC and HRC. The HRC darks are taken in parallel with the WFC darks.
The charge transfer efficiency {CTE} of the ACS CCD detectors declines
as damage due to on-orbit radiation exposure accumulates. This
degradation has been closely monitored at regular intervals, because
it is likely to determine the useful lifetime of the CCDs. We combine
the annealling activity with the charge transfer efficiency monitoring
and also merge into the routine dark image collection. To this end,
the CTE monitoring exposures have been moved into this proposal . All
the data for this program is acquired using internal targets {lamps}
only, so all of the exposures should be taken during Earth occultation
time {but not during SAA passages}. This program emulates the ACS
pre-flight ground calibration and post-launch SMOV testing {program
8948}, so that results from each epoch can be directly compared.
Extended Pixel Edge Response {EPER} and First Pixel Response {FPR}
data will be obtained over a range of signal levels for both the Wide
Field Channel {WFC}, and the High Resolution Channel {HRC}.

NIC1 10725

Photometric Stability

This NICMOS calibration proposal carries out photometric monitoring
observations during Cycle 14. The format of the program is similar to
that of the Cycle 12 program 9995 and Cycle 13 program 10381, but a
few modifications were made. Provisions had to be made to adopt to
2-gyro mode {G191B2B was added as extra target to provide target
visibility through most of the year}. Where before 4 or 7 dithers were
made in a filter before we moved to the next filter, now we observe
all filters at one position before moving to the next dither position.
While the previous method was chosen to minimize the effect of
persistence, we now realize that persistence is connected to charge
trapping and by moving through the filter such that the count rate
increases, we reach equilibrium more quickly between charge being
trapped and released. We have also increased exposure times where
possible to reduce the charge trapping non-linearity effects.

ACS/WFC 10624

Solving the Mystery of the Short-Hard Gamma-Ray Bursts

Eight years after the afterglow detections that revolutionized studies
of the long-soft gamma-ray bursts, not even one afterglow of a
short-hard GRB has been seen, and the nature of these events has
become one of the most important problems in GRB research. The Swift
satellite, expected to be in full operation throughout Cycle 14, will
report few-arcsecond localizations for short-hard bursts in minutes,
enabling prompt, deep optical afterglow searches for the first time.
Discovery and observation of the first short-hard optical afterglows
will answer most of the critical questions about these events: What
are their distances and energies? Do they occur in distant galaxies,
and if so, in which regions of those galaxies? Are they the result of
collimated or quasi-spherical explosions? In combination with an
extensive rapid-response ground-based campaign, we propose to make the
critical high-sensitivity HST TOO observations that will allow us to
answer these questions. If theorists are correct in attributing the
short-hard bursts to binary neutron star coalescence events, then they
will serve as signposts to the primary targeted source population for
ground-based gravitational-wave detectors, and short-hard burst
studies will have a vital role to play in guiding those observations.

ACS/HRC 10609

Sizes, Shapes, and SEDs: Searching for Mass Segregation in the Super
Star Clusters of Nearby Starburst

We propose to investigate mass segregation and star cluster evolution
and dissolution processes in Super Star Cluster {SSC} populations in a
small sample of nearby starburst galaxies. ACS/HRC and NICMOS images
of these nearby {d 10 Mpc} starbursts can reveal evidence for mass
segregation in the form of variations in size, shape, and color of the
SSCs as a function of wavelength. The compactness of the cluster light
profiles, and hence the stellar mass distributions, is a critical
indicator of the likely fate of an SSC: long life and eventual
evolution into a globular-like cluster, or dissolution. These
observations will allow us to generate spectral energy distributions
{SEDs} for a large sample of the SSCs at all ages and extinctions in
each system. We will combine the SEDs with population synthesis models
and existing ground-based spectra and Spitzer images to estimate ages,
reddenings, and masses thus derive a more complete picture of the
star- formation histories of the galaxies. For the brightest and most
likely virialized among the SSCs we will also constrain their initial
mass functions {IMFs} using high-resolution spectroscopy. Conclusions
about IMFs from this technique require detailed information about the
SSC concentration, light profiles, and virial status, which are only
possible via ACS data. The proposed observations will provide an
extensive and comprehensive data set for a large number of SSCs. By
addressing the issues of mass segregation, evaporation, and
destruction of SSC populations, the proposed observations will provide
strong constraints on theories regarding the processes involved in the
formation and evolution of SSCs and globular clusters. Given the dire
predictions for the lifetime of HST, and its tremendous impact on the
study of SSCs, we feel that the proposed observations not only are
necessary and timely {even urgent} but will also be a fitting { and
possibly final} addition to HST's legacy in the study of starburst
SSCs.

ACS/HRC 10598

ACS Imaging of Fomalhaut: A Rosetta Stone for Debris Disks Sculpted by
Planets

The Sun and roughly 15% of stars are surrounded by dust disks
collisionally replenished by asteroids and comets. Disk structure can
be directly tied to the dynamical influence of more massive bodies
such as planets. For example, planetary perturbations offset the
center of our zodiacal dust disk ~0.01 AU away from the Sun and also
maintain a ~40 AU radius inner edge to our Kuiper Belt. Here we
propose follow-up observation to the first optical detection of
reflected light from dust grains surrounding the nearby star Fomalhaut
using HST/ACS. We find a belt of material between 133 and 158 AU
radius that has a center position offset ~15 AU from the stellar
position, and with a sharp inner edge. A tenuous dust component
interior to the belt is also detected in the southeast. Given
Fomalhaut's proximity to the Sun {7.7 pc}, these images represent the
closest and highest angular resolution view of an extrasolar analog to
our Kuiper Belt. The center of symmetry offset and the sharp inner
edge of Fomalhaut's belt are evidence for planet-mass objects orbiting
the star as predicted by dynamical theory and simulations. We propose
comprehensive follow-up ACS imaging to fully exploit this discovery
and map the disk around its entire circumference with higher
signal-to-noise and at multiple wavelengths. HST/ACS is certainly the
only facility capable of performing this relatively wide field optical
study at high contrast ratios and diffraction-limited resolution. The
Cycle 14 data will provide key measurements of belt width as a
function of azimuth, the scattered light color of the belt versus the
inner dust component, and the azimuthal structure of the belt. These
data will be used to constrain dynamical models of resonances and
shepherding that ultimately elucidate the dynamical properties of
planet-mass objects in the system.

ACS/WFC 10592

An ACS Survey of a Complete Sample of Luminous Infrared Galaxies in
the Local Universe

At luminosities above 10^11.4 L_sun, the space density of far-infrared
selected galaxies exceeds that of optically selected galaxies. These
`luminous infrared galaxies' {LIRGs} are primarily interacting or
merging disk galaxies undergoing enhanced star formation and Active
Galactic Nuclei {AGN} activity, possibly triggered as the objects
transform into massive S0 and elliptical merger remnants. We propose
ACS/WFC imaging of a complete sample of 88 L_IR 10^11.4 L_sun
luminous infrared galaxies in the IRAS Revised Bright Galaxy Sample
{RBGS: i.e., 60 micron flux density 5.24 Jy}. This sample is ideal
not only in its completeness and sample size, but also in the
proximity and brightness of the galaxies. The superb sensitivity,
resolution, and field of view of ACS/WFC on HST enables a unique
opportunity to study the detailed structure of galaxies that sample
all stages of the merger process. Imaging will be done with the F439W
and F814W filters {B and I-band} to examine as a function of both
luminosity and merger state {i} the evidence at optical wavelengths of
star formation and AGN activity and the manner in which instabilities
{bars and bridges} in the galaxies may funnel material to these active
regions, {ii} the relationship between star formation and AGN
activity, and {iii} the structural properties {AGN, bulge, and disk
components} and fundamental parameters {effective radius and surface
brightness} of LIRGs and their similarity with putative evolutionary
byproducts {elliptical, S0 and classical AGN host galaxies}. This HST
survey will also bridge the wavelength gap between a Spitzer imaging
survey {covering seven bands in the 3.6-160 micron range} and a GALEX
UV imaging survey of these galaxies, but will resolve complexes of
star clusters and multiple nuclei at resolutions well beyond the
capabilities of either Spitzer or GALEX. The combined datasets will
result in the most comprehensive multiwavelength study of interacting
and merging galaxies to date.

ACS/WFC 10551

Gamma-Ray Bursts from Start to Finish: A Legacy Approach

The progenitors of long-duration GRBs are now known to be massive
stars. This result lends credence to the collapsar model, where a
rotating massive star ends its life leaving a black hole or a highly
magnetized neutron star, and confirms its essential aspects. The focus
of attention now is on the black hole or magnetar engines that power
the bursts. Somehow these engines create the most highly relativistic
and highly collimated outflows that we know of, through mechanisms
that no current theory can explain. These astrophysical laboratories
challenge our understanding of relativistic shocks, of mechanisms for
extracting energy from a black hole, and of how physics works in
extreme conditions. The launch of Swift is bringing us into a new era,
where we can make broadband observations that will enable us to study
these fascinating physical processes. We propose here an ambitious,
comprehensive program to obtain the datasets that will become the
standard that any successful model for the central engine must
explain. This programs leverages the HST observations to the maximum
extent by our commitment of Swift observations, a Large program at the
VLA, and extensive ground-based optical resources. By studying the
engines and searching for jets in a variety of events, this program
will investigate the conditions necessary for the engine and jet
formation itself.

NIC2/ACS/WFC/WFPC2 10532

Kinematics and morphology of the most massive field disk galaxies at
z1

We propose to obtain 1 orbit NIC-2 images of a sample of the 15 most
massive galaxies found at $1 z 1.3$. These were culled from over
20, 000 Keck spectra collected as part of DEEP and are unique among
high redshift massive galaxy samples in being kinematically selected.
We intend to test whether these potentially very young galaxies are
likely precursors to massive local disks, assuming no further merging.
NIC-2 images provide rest-frame optical morphologies that will show
whether they are normal disky systems or instead more disturbed
looking objects with multiple subcomponents, mergers, peculiar
structure, etc. NIC-2 provides near-IR resolutions sufficient to
enable measurements of bulges and disks subcomponents. The near-IR
will fill a critical gap in the broad-band SED photometry of the
galaxy and its subcomponents to estimate mean stellar ages and stellar
masses and to assess whether old stellar bulges and disks are in place
at that time. Finally, this sample will yield the first statistically
significant results on the $z 1$ evolution of the Tully-Fisher
relation for massive galaxies. In addition, we propose parallel
observations with ACS WFC {V and I bands} and WFPC2 {I-band}. These
will target up to 700 galaxies at redshifts 0.7 ... 1.2 for which the
DEEP2 survey has obtained precision redshifts and high-resolution
kinematic data. The added HST morphology and color information will
allow a variety of detailed studies on dynamical, structural, and
photometric evolution of galaxies.

NIC2 10510

Morphology of massive early-type galaxies at z1.2: constraining
galaxy formation models

We ask for NICMOS-NIC2 H-band imaging of a sample of 10 massive
early-type galaxies spectroscopically identified at 1.2z1.7. Our aim
is to look for possible relics of merging events of their
formation/evolution in their morphology. The requested observations,
sampling their rest-frame at lambda6500A, would map the mass
distribution of the bulk of their stellar content. The targets have
been revealed by our group on the basis of near-IR spectroscopy
obtained in the framework of a spectroscopic survey of a complete
sample of bright EROs {Ks18.5}. Optical and near-IR photometry is
available for all the targets, and low resolution near-IR spectra have
allowed their identification and redshift measurement. Spectroscopic
and photometric data in our hands show that they have already
assembled stellar masses greater than 3 10^11 solar masses, and that
the mean age of their stellar population is estimated older than 2-3
Gyr for 6 of them and about 1 Gyr for the other 4 galaxies. Thus, they
are among the most luminous and massive evolved galaxies detected so
far at z1. Other data are needed to infer how they have assembled
such high stellar masses, i.e. to trace back their evolution. The
requested observations would allow us to reveal signs of past
interaction/merger event. A smooth r^{1/m} profile, coupled with no
other signs of interaction/merger {disturbed morphology}, would place
the possible merger event of formation 1-2 Gyr before their redshift z
pprox 1.5, i.e. at z 2-3. On the other hand, if signs of recent
merger events will be found, the last merger event forming the local
massive spheroids will be constrained at 1.5 z 2. Thus, the
requested HST observations will allow for the first time to see how
massive early-type galaxies at z pprox 1.5 look like, constraining in
any case the redshift of the possible merging event of their
formation.

ACS/WFC 10496

Decelerating and Dustfree: Efficient Dark Energy Studies with
Supernovae and Clusters

We propose a novel HST approach to obtain a dramatically more useful
"dust free" Type Ia supernovae {SNe Ia} dataset than available with
the previous GOODS searches. Moreover, this approach provides a
strikingly more efficient search-and-follow-up that is primarily
pre-scheduled. The resulting dark energy measurements do not share the
major systematic uncertainty at these redshifts, that of the
extinction correction with a prior. By targeting massive galaxy
clusters at z 1 we obtain a five-times higher efficiency in
detection of Type Ia supernovae in ellipticals, providing a
well-understood host galaxy environment. These same deep cluster
images then also yield fundamental calibrations required for future
weak lensing and Sunyaev-Zel'dovich measurements of dark energy, as
well as an entire program of cluster studies. The data will make
possible a factor of two improvement on supernova constraints on dark
energy time variation, and much larger improvement in systematic
uncertainty. They will provide both a cluster dataset and a SN Ia
dataset that will be a longstanding scientific resource.

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated.)

HSTARS:

10361 - JWCK3P5 out of limit one sample @195/2048z

ACS mnemonic JWCK3P5 (WFC CEB CLOCK 3 +5 volt) flagged out of limit
for one sample at 20:47:47 with a value of 5.3126, limit is 5.30
volts, went back in limit 60 seconds later at 20:48:47. On call SI SE
notified.

10362 - EFG1_12T out of limits @194/0450z

EFG1_12T red limit high. SE informed and Ops Note:1500-2 FGS Dome
Temperature Limit Change amended to relect red limit which was not
included in original OpsNote:1500-1

10363 - GSacq(2,1,1) failed to RGA control @198/0530z

GSacq(2,1,1) scheduled at 198/05:26:03 failed to RGA control due to
stop flag (QF2STOPF). The OBAD at 05:08:58 showed errors of V1=0.51,
V2=-8.37, V3=-3.57, RSS=9.12. Observations affected: ACS 23 - 30

10364- GSacq(1,2,1) results in finelock backup @198/0655z

During LOS the GSacq(1,2,1)at 198/06:54:50 resulted in finelock backup
(1,0,1) due to receiving a stop flag(QF2STOPF) on FGS 2. The OBAD at
06:220 showed errors of V1=-12.42, V2=-4.75, V3=2.57, RSS=13.55.
Observations affected: ACS 31 - 33 GSacq(1,2,1) resulted in finelock
backup

COMPLETED OPS REQUEST:
17808-0 Battery Pressure Limits After Battery 3 BCT @195/1428z

17814-0 Disable 486 ESBs 1201 and 1202 after Battery 3 BCT Completed
@195/1602z

17818-0 Battery 3 Capacity Test Script & 5 Battery Pressure Limit COP
@195/1420z

17833-0 - GenSlew for Proposal 10598 slot#9 @195/1824z

17834-0 - GenSlew for Proposal 10598 slot#10 @195/1826z

17835-0 - GenSlew for Proposal 10598 slot#11 @195/1829z

17836-0 - GenSlew for Proposal 10598 slot#12 @195/1831z

17830-0 - Set ACS WFC TEC setpoint to -81.0 deg @196/0445z

17831-1 - Set Up ACS FW memory monitors @196/0557z

17816-0 CONTING Batt 3 Rec: Lower VTFE Curves to K1L4-150mV @196/1403z

17817-0 CONTING Batt 3 Rec: Lower VTFE Curves to K1L4-100mV @196/2002Z

17695-2 Monitor VehConLaw.Integral Path Data via TMDIAG Slot 0
196/1406z,2012z


COMPLETED OPS NOTES:
1506-1 - Battery 3 BCT Limits following test @195/1436z

SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 26 25 198/0530z (HSTAR#10363)
FGS REacq 14 14
OBAD with Maneuver 64 64


SIGNIFICANT EVENTS:

Battery 3 Capacity Final Flash Report

At approximately 2006/195 14:05 GMT (10:05 am local), Battery 3 was
successfully commanded back on-line in FSW. The remainder of the
Battery 3 Reconditioning script was completed at approximately
2006/195 14:30 GMT (10:30 am local). EPS SEs monitored the system for
2 orbits after restoring EPS to a 6-battery FSW configuration and
observed nominal system performance. Battery temperatures are still
cycling within nominal limits with battery 5 the warmest at 2.11 DegC.
EPS SEs will continue to remotely monitor the system throughout the
high sun-time which terminates on July 24th

Lowered VTFE to K1L4-100mv Flash Report

At approximately doy 196/ 930 GMT (530am local), batteries 5 and 6
exceeded the 5.5degC ground temperature limit. Per the battery
temperature contingency, the VTFE was lowered by 100mv to K1L4-100mv
for all batteries at 196/ 14:03 (1003am local). EPS will monitor
remotely for the next 48hours to ensure that battery temperatures
remain below 5.5degC. Per the contingency plan, the VTFE can be
lowered an additional 50mv if necessary to reduce temperatures.

Lowered VTFE to K1L4-150mv Flash Report

At approximately doy 196/ 1900 GMT (SATURDAY, 7/15, 300pm local),
batteries 5 and 6 exceeded the 7degC ground temperature limit. Per the
battery temperature contingency, the VTFE was lowered an additional
50mv to K1L4-150mv for all batteries at 196/ 2000 GMT(4pm local). EPS
will monitor remotely for the next 24hours to ensure that battery
temperatures remain in the range of +5 -to +7degC. An Ops Request to
offline the battery 6 +CC SPA has been generated in the event
additional action is required.