HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 4151
PERIOD COVERED: UT July 7,8,9, 2006 (DOY 188,189,190)
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/WFC/HRC 11005
Funcional test - MEB2 switch
This is a functional test to be executed after the switch to MEB2.
NIC2 10906
The Fundamental Plane of Massive Gas-Rich Mergers: II. The QUEST QSOs
We propose deep NICMOS H-band imaging of a carefully selected sample
of
23 local QSOs. This program is the last critical element of a
comprehensive investigation of the most luminous mergers in the
nearby
universe, the ultraluminous infrared galaxies {ULIRGs} and the
quasars.
This effort is called QUEST: Quasar / ULIRG Evolutionary STudy. The
high-resolution HST images of the QUEST QSOs will complement an
identical set of images on the ULIRG sample obtained during Cycle 12,
an
extensive set of ground-based data that include long-slit NIR
spectra
from a Large VLT Program, and a large set of mid-infrared spectra from
a
Cycle 1 medium-size program with Spitzer. This unique dataset will
allow
us to derive with unprecedented precision structual, kinematic, and
activity parameters for a large unbiased sample of objects spanning
the
entire ULIRG/QSO luminosity function. These data will refine the
fundamental plane of massive gas-rich mergers and enable us to
answer
the following quesitons: {1} Do ultraluminous mergers form
elliptical
galaxies, and in particular, giant ellipticals? {2} Do ULIRGs evolve
into optical bright QSOs? The results from this detailed study of
massive mergers in the local universe will be relevant to
understanding
the basic physical processes involved in creating massive early-type
host on the one hand, and growing/feeding embedded massive black
holes
on the other, in major galaxy mergers. This is an important question
since 50% of cosmic star formation at high-z and most of the big BHs
appear to be formed in this process.
NIC1 10879
A search for planetary-mass companions to the nearest L dwarfs -
completing the survey
We propose to extend the most sensitive survey yet undertaken for
very
low-mass companions to ultracool dwarfs. We will use NICMOS to
complete
imaging of an all-sky sample of 87 L dwarfs in 80 systems within 20
parsecs of the Sun. The combination of infrared imaging and
proximity
allows us to search for companions with mass ratios q>0.25 at
separations exceeding ~3 AU, while probing companions with q>0.5 at
~1.5
AU separation. This resolution is crucial, since no ultracool
binaries
are known in the field with separations exceeding 15 AU. Fifty L
dwarfs
from the 20-parsec sample have high- resolution imaging, primarily
through our Cycle 13 HST proposal which identified six new binaries,
including an L/T system. Here, we propose to target the remaining 30
dwarfs
ACS/WFC 10824
Measuring the Shape and Orientation of the Galactic Dark-Matter Halo
using Hypervelocity Stars
We propose to obtain high-resolution images of five hypervelocity
stars
in the Galactic halo in order to establish the first-epoch
astrometric
frame for them, as a part of a long-term program to measure precise
proper motions. The origin of these recently discovered stars, all
with
positive radial velocities above 540 km/s, is consistent only with
being
ejected from the deep potential well of the massive black hole at
the
Galactic center. The deviations of their space motions from purely
radial trajectories probe the departures from spherical symmetry of
the
Galactic potential, mainly due to the triaxiality of the dark-matter
halo. Reconstructing the full three-dimensional space motion of the
hypervelocity stars, through astrometric proper motions, provides a
unique opportunity to measure the shape and orientation of the dark
halo. The hypervelocity stars allow measurement of the potential up
to
75 kpc from the center, independently of and at larger distances
than
are afforded by tidal streams of satellite galaxies such as the
Sagittarius dSph galaxy. HVS3 may be associated with the LMC, rather
then the Galactic center, and would therefore present a case for a
supermassive black hole at the center of the LMC. We request one
orbit
with ACS/WFC for each of the five hypervelocity stars to establish
their
current positions relative to background galaxies. We will request a
repeated observation of these stars in Cycle 17, which will
conclusively
measure the astrometric proper motions.
ACS/WFC 10775
An ACS Survey of Galactic Globular Clusters
We propose to conduct an ACS/WFC imaging survey of Galactic globular
clusters. We will construct the most extensive and deepest set of
photometry and astrometry to-date for these systems reaching a main
sequence mass of ~0.2 solar mass with S/N >= 10. We will combine
these
data with archival WFPC2 and STIS images to determine proper motions
for
the stars in our fields. The resultant cleaned cluster CMDs will
allow
us to study a variety of scientific questions. These include [but
are
not limited to] 1} the determination of cluster ages and distances
2}
the construction of main sequence mass functions and the issue of
mass
segregation 3} the internal motions and dynamical evolution of
globular
clusters, and 4} absolute cluster motions, orbits, and the Milky Way
gravitational potential. We anticipate that the unique resource
provided
by the proposed treasury archive will play a central role in the
field
of globular cluster studies for decades, with a stature comparable
to
that of the Hubble Deep Field for high redshift studies.
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/WFC 10753
An Astrometric Calibration Field Near the Ecliptic Pole
This program will obtain deep ACS astrometry of a Large Magellanic
Cloud
star field lying within the planned continuous viewing zone of the
James
Webb Space Telescope, which extends to a 5 degree radius from the
Ecliptic pole. To allow a full astrometric solution to be
calculated,
controlling for distortions within ACS that may be time variable
over
periods of months to years, we will observe our target field at two
distinct roll angles separated by approximately 90 degrees. To help
control for large scale distortions, we will "chop" the
observations in
at least one roll angle, using offsets of order one third the ACS
field
of view.
ACS/WFC 10742
Ramp Filter and Grism Zeroth Order Wavelengths
A calibration of ramp filters on the ACS is obtained through
crossing
the ramp filters with the G800L grism in observations of the
standard
star GD 153. The standard star is also observed through the F606W
filter
and each ramp crossed with a wide-band filter to measure any
filter-wedge offset from the standard grism calibration produced by
crossing a ramp with the grism. The ramp filters chosen for this
first
calibration are those which have been used most extensively by
observers
during the past ACS cycles and can be usefully crossed with the
G800L
grism.
ACS/HRC/WFC 10737
CCD Stability Monitor
This program will verify that the low frequency flat fielding, the
photometry, and the geometric distortion are stable in time and
across
the field of view of the CCD detectors. A moderately crowded stellar
field in the cluster 47 Tuc is observed every three months with the
HRC
{at the cluster core} and WFC {6' West of the cluster core} using
the
full suite of broad and narrow band imaging filters. The positions
and
magnitudes of objects will be used to monitor local and large scale
variations in the plate scale and the sensitivity of the detectors
and
to derive an independent measure of the detector CTE. An additional
orbit is required to compare WFC observations taken at gain 1 with
those
taken at the new default gain 2.
ACS/WFC 10730
External CTE Monitor
Monitor CTE in Cycle 14 for WFC and HRC
ACS/WFC 10630
The Fine Structure of Elliptical Galaxies in Voids
Elliptical galaxies constitute a remarkably homogeneous class of
objects
with a tight color- magnitude relation and a well-defined
Fundamental
Plane. In spite of their bland and symmetrical morphology, they are
characterized by a wealth of structural features {such as nuclear
disks,
dust lanes, shells, blue cores, etc.} which contain important clues
to
their formation history. Little is known about how and if these
sub-structures vary as a function of environment; in fact, due to
the
morphology density relation, our knowledge of ellipticals is
strongly
biased towards overdense regions such as clusters. But what of the
fine
structure of ellipticals in voids? According to theoretical
predictions,
void galaxies should have different merger histories than those in
clusters, which may imply that their fine structure also differs. We
address these issues using the exquisite angular resolution of
HST/ACS
to resolve sub-structures in the most accurately classified sample,
to
date, of truly isolated ellipticals, identified using the 2dFGRS.
ACS/WFC 10629
Are Field OB Stars Alone?
This SNAP program offers an inexpensive, simple program to search
for
low-mass companions of field OB stars. Do field OB stars exist in
true
isolation, as suggested by a recent Galactic study, or are they the
tip
of the iceberg on a small cluster of low-mass stars as predicted by
the
cluster mass function and stellar IMF? Short ACS/WFC V and I
observations proposed here may easily resolve this issue for field
OB
stars in the Small Magellanic Cloud. Truly isolated OB stars represent
a
theoretical challenge and variation from clusters, in mode of star
formation, and have important consequences for our understanding of
the
field stellar population in galaxies. Small clusters around the field
OB
stars, on the other hand, may confirm the universality of the
stellar
clustering law and IMF.
ACS/WFC 10567
Securing the Faint-End Galaxy Luminosity Function with Surface
Brightness Fluctuation Distances
The history of the formation of galaxies must leave an imprint in
the
properties of the mass function of collapsed objects and in it's
observational manifestation the luminosity function. At present the
faint end of the luminosity function of galaxies is poorly known.
Accurate knowledge of the luminosity function over the full range of
galaxy clustering scales would provide serious constraints on both
initial cosmological conditions and modulating astrophysical
processes.
Wide field imaging surveys with large groundbased telescopes now
provide
the capability to identify dwarf galaxy candidates to very faint
levels.
However distances to these candidates are needed to overcome the
omnipresent problem of group membership uncertainties and to
establish
the intrinsic properties of the faint end of the luminosity
function.
Single orbit observations with HST ACS can provide adequate
distances
via the surface brightness fluctuation method for targets in this
program, resulting in the best definition ever of the luminosity
function to M_R=-11 in a specific environment.
ACS/HRC 10542
Charting the Sparkling Star Formation in NGC346
New, stunning V, I images of the youngest and most massive star
forming
region NGC 346, in the Small Magellanic Cloud, have been recently
obtained with the HST/ACS. They reveal a myriad of small compact
clusters: some are still embedded in dust, possibly connected by gas
and
dust filaments. We also discover a rich population of pre-main
sequence
low mass stars {~3 -0.6 Mo} mainly distributed in the body of NGC
346
and in these compact clusters, which formed with the central cluster
{~5My ago}, but have not reached the main sequence yet. The
immediate
question that emerges is: how did star formation occur in this
region?
Is there evidence for an age spread among these clusters, that could
be
indicative of sequential star formation? We are, therefore,
requesting
an immediate follow up investigation with the ACS/HRC to perform a
comprehensive UV/U study of the ten largest clusters identified in
the
NGC 346 region, with the objective of determining, in combination
with
the already available deep V, I data, their mass function, their
upper
mass cut-off, whether mass segregation is present, whether there are
age
variations, and what is the impact of the stellar feedback, with the
final aim to establish how star formation has occured and progressed
in
this low metallicity environment.
NIC2/ACS/WFC/WFPC 10532 2 Kinematics and morphology of the most
massive
field disk galaxies at z>1
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.
ACS/HRC 10516
Host Galaxies of Reverberation-Mapped AGNs
We propose to obtain unsaturated ACS high-resolution images of four
reverberation- mapped active galactic nuclei in order to remove the
point-like nuclear light from each image, thus yielding a
"nucleus-free"
image of the host galaxy. This will allow investigation of host
galaxy
properties: our particular interest is determination of the
host-galaxy
starlight contribution to the reverberation-mapping observations.
This
is necessary {1} for accurate determination of the relationship
between
the AGN nuclear continuum flux and the size of the broad Balmer-line
emitting regions of AGNs, which is important because this
relationship
is used in estimating black hole masses for large samples of QSOs,
and
{2} for accurate determination of the bolometric luminosity of the
AGN
proper. In a Cycle 12 SNAP program, we obtained images of 14 of the
36
reverberation-mapped AGNs for this purpose. This additional request
is
to complete this program through observations of the four important
remaining sources.
NIC3/ACS/WFC 10504
Characterizing the Sources Responsible for Cosmic Reionization
Our group has demonstrated the role that massive clusters, acting as
powerful cosmic lenses, can play in constraining the abundance and
properties of low-luminosity star- forming sources beyond z~6; such
sources are thought to be responsible for ending cosmic
reionization.
The large magnification possible in the critical regions of well-
constrained clusters brings sources into view that lie at or beyond
the
limits of conventional exposures such as the UDF, as well as those
in
imaging surveys being undertaken with IRAC onboard Spitzer. We have
shown that the combination of HST and Spitzer is particularly
effective
in delivering the physical properties of these distant sources,
constraining their mass, age and past star formation history.
Indirectly, we therefore gain a valuable glimpse to yet earlier
epochs.
Recognizing the result {and limitations} of the UDF exposure, we
propose
a systematic search through 6 lensing clusters with ACS and NICMOS
for
further z~6-7 sources in conjunction with existing deep IRAC data.
Our
survey will mitigate cosmic variance and extend the search both to
lower
luminosities and, by virtue of the NICMOS/IRAC combination, to
higher
redshift. The goal is to count and characterize representative
sources
at z~6-10 and to delineate the redshift range of activity for the
planning of future observations.
ACS/WFC 10494
Imaging the mass structure of distant lens galaxies
The surface brightness distribution of extended gravitationally
lensed
arcs and Einstein rings contains super-resolved information about
the
lensed object, and, more excitingly, about the smooth and clumpy
mass
distribution of the lens galaxies. The source and lens information
can
non-parametrically be separated, resulting in a direct
"gravitational-mass image" of the inner mass-distribution
of
cosmologically-distant galaxies {Koopmans 2005}. With this goal in
mind,
we propose deep HST ACS-F555W/F814W and NICMOS-F160W imaging of 15
gravitational-lens systems with spatially resolved lensed sources,
selected from the 17 new lens systems discovered by the Sloan Lens
ACS
Survey {Bolton et al. 2004}. Each system has been selected from the
SDSS
and confirmed in a time-efficient HST-ACS snapshot program
{cycle-13};
they show highly-magnified arcs or Einstein rings, lensed by a
massive
early-type lens galaxy. High-fidelity multi-color HST images are
required {not delivered by the 420-sec snapshot images} to isolate
these
lensed images {properly cleaned, dithered and extinction-corrected}
from
the lens galaxy surface brightness distribution, and apply our
"gravitational-mass imaging" technique. The sample of galaxy
mass
distributions - determined through this method from the arcs and
Einstein ring HST images - will be studied to: {i} measure the
smooth
mass distribution of the lens galaxies {Dark and luminous mass are
separated using the HST images and the stellar M/L values derived from
a
joint stellar-dynamical analysis of each system}; {ii} quantify
statistically and individually the incidence of mass-substructure
{with
or without obvious luminous counter-parts such as dwarf galaxies}.
Since
dark-matter substructure should be considerably more prevalent at
higher
redshift, both results provide a direct test of this prediction of
the
CDM hierarchical structure-formation model.
ACS/HRC 10396
Star Clusters, Stellar Populations, and the Evolution of the Small
Magellanic Cloud
As the closest star forming dwarf galaxy, the SMC is the preferred
location for detailed studies of this extremely common class of
objects.
We therefore propose to use the capabilities of ACS, which provide
an
improvement by an order of magnitude over what is possible with
ground-based optical imaging surveys that are limited by confusion
anddepth, to measure key stellar population parameters in the SMC
from
VI color- magnitude diagrams. Our program focuses on regions where
crowding makes HST essential and includes 7 star clusters and 7
field
star locations. We will measure accurate ages of the clusters, test
stellar evolution models, gain fiducial stellar sequences to use in
fitting the field stars, check the form of the IMF, and
substantially
extend the study of RR Lyrae variables in the key NGC121 SMC
globular
cluster. The field pointings will allow us to reconstruct the star
formation history, look for enhanced star formation that is expected
when the SMC interacts with the LMC and/or Milky Way, and compare
its
main sequence luminosity {and mass} functions with those of the
Milky
Way, LMC, and UMi dwarf spheroidal. This proposal is part of a
coordinated HST and ground-based study of the stellar history and
star
formation processes in the SMC.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary
reports
of potential non-nominal performance that will be investigated.)
HSTARS:
#10346 REacq(2,1,2 ) failed due to search radius limit exceeded @
188/1219z
The
REacq(2,1,2)scheduled at 188/12:15:09 failed at 12:19:58 due to
search
radius limit exceeded on FGS 2. OBAD2 at 12:10:03 showed errors
of
V1=68.13, V2=37.63, V3=57.97, RSS=97.05. ESD a05 (FGS Coarse Track
failed -
Search Radius Limit exceeded) was received. Observations
affected :
ACS 19, ACS 20, NIC 43
#10347 OBAD Failed Identification (ESB 1902) @ 188/2320z
At
188/23:20:04 OBAD1 using FHST-1 and FHST-2 failed. One 486 ESB
message
1902 (OBAD Failed Identification) was received. OBAD1 had (RSS)
value of
130325.87 arcseconds. OBAD success flag (mnemonic GCHACL09)
returned
to the "no success" state(a value of 1). OBAD2 at 188/23:30:39
was
successful
with (RSS) value of 28540.30 arcseconds.
#10348 REacq(1,3,3) Failed to RGA Control @ 188/2334z
The
REacq(1,3,3) scheduled at 188/23:34:59 - 23:43:04 failed to RGA Hold
due to
uncorrected attitude error per Ref HSTAR# 10347. There were no
FGSs
indication flags. Prior GSacq using same star id was successful.
Possible
Observations affected: ACS 38 thru 41.
#10349 GSAcq (2,1,2) failed due to search radius limit exceeded @
190/0631z
GSAcq
(2,1,2) scheduled @ 190/06:28:12-06:35:45 failed due to search
radius
limit exceeded on FGS 1. Received one 486 ESB message a05
(Exceeded
SRL). OBAD #1: V1 -1811.83, V2 1880.49, V3 -2874.30, RSS
3883.37.
OBAD #2: V1 -0.53, V2 5.56, V3 7.14, RSS 9.06. At AOS
(190/07:39:10) OBAD MAP scheduled @ 07:15:32 showed the following:
V1
-55.71, V2
2400.79, V3 -29.66, RSS 2401.62. REAcq 2,1,2 scheduled at
190/08:03:38 failed to RGA hold due to stop flag on FGS-1. Possible
observations effected: ACS 101-131. OBAD MAP @ 08:51:27 = V1
-389.08, V2
4988.63,
V3 -3.54, RSS 5003.78
COMPLETED OPS REQUEST:
#17543-2 Dump OBAD tables after failed OBAD (Generic) @
188/2326z
COMPLETED OPS NOTES: (None)
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS
GSacq
23
22
190/0631z (HSTAR 10349)
FGS
REacq
30
27
188/1215z (HSTAR 10346)
188/2334z (HSTAR 10348)
190/0803z (HSTAR 10349)
OBAD with Maneuver
76
75
188/2320z (HSTAR 10347)
SIGNIFICANT EVENTS: (None)
-Lynn
Lynn F. Bassford
CHAMP HST Missions Operations Manager
Lockheed Martin Technical Operations
GSFC PH#: 301-286-2876
Cell/Voice Mail: 240-603-4873 Text/Pager:
2406034873@messaging.sprintpcs.com
"The Hubble Space Telescope is the Babe Ruth of astronomical
observatories, the Muhammad Ali of cosmic photography
"
- Robert Roy Britt, space.com 7-14-4
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