HST Daily Report #3340 (Part 2)
ACS 9454
The Nature of the UV Continuum in LINERs: A Variability Test
LINERs may be the most common AGNs, and the signposts of accretion onto
the massive black holes present in most galaxies. However, the LINER
spectrum is the result of UV excitation, and, in at least some LINERs, a
nuclear cluster of hot stars, rather than an AGN, dominates the
energetics in the UV. Thus, it is still unknown if the UV continuum, or
the optical emission lines it excites, have anything to do with an AGN.
The demographics and accretion physics of low-luminosity AGNs hinge on
this question. We propose to search for variability in a sample of 17
LINERs with compact UV nuclei. Variability can reveal an AGN component
in the UV continuum, even when its light is not dominant. We will test
systematically the handful of non-definitive reports of UV variability,
and potentially quantify the AGN contribution to the UV emission.
Variability in all or most objects will be strong evidence that LINERs
mark dormant AGNs in most galaxies. Alternatively, a general null
detection of variability will suggest that, even in LINERs with
additional AGN signatures, the UV continuum is stellar in origin.
Contemporaneous monitoring with the VLA/VLBA of 11 objects which have
radio cores {five of which we already know are radio-variable} will
reveal the relations between UV and radio variations. The UV-variable
objects will be targeted for future, better-sampled, monitoring.
ACS/WFC/HRC 9445
Gravitational Microlensing in the NGC 3314A-B Galaxy Pair.
The Advanced Camera for Surveys (WFC and HRC) was used to determine the
composition of the dark matter that dominates the masses of galaxies
which is an important unsolved problem.
ACS/WFC/HRC 9696
Hubble Heritage observations of NGC 3370
Hubble Heritage proposes to observe NGC 3370 in conjunction with GO
program 9351 {PI Adam Riess} to use the combined data to produce a three
color image.
HST 9382
A Large Targeted Survey for z < 1.6 Damped Lyman Alpha Lines in SDSS QSO
MgII-FeII Systems.
We have searched the first public release of SDSS QSO spectra for low-z
{z<1.65} metal absorption lines and found over 200 large rest equivalent
width MgII-FeII systems. Previously, we empirically showed that such
systems are good tracers of large neutral gas columns, with ~50% being
classical damped Lyman alpha {DLA} systems {N_HI>=2*10^20 cm^-2}. Here
we propose to follow up a well-defined subset of 79 of them to search
for DLAs with 0.47<z<1.60. Only QSOs brighter than g’=19 were selected.
The QSO emission and DLA absorption redshifts were constrained to
virtually eliminate data loss due to intervening Lyman limit absorption.
Consequently, we expect to discover ~40 new DLAs, which is a three-fold
increase in this redshift interval. This will significantly improve our
earlier low-z DLA statistical results on their incidence, cosmological
mass density, and N_HI distribution. The results will also allow us to
better quantify the empirical DLA — metal-line correlation. With this
improved understanding, the need for follow-up UV spectroscopy will
lessen and, with the release of the final database of SDSS QSO spectra
{an ~25-fold increase}, the number of low-z DLAs could be increased
arbitrarily. Thus, the power of the large and statistically-sound SDSS
database in combination with a proven technique for finding low-z DLAs
will, over the next few years, essentially solve the problem of making
an accurate determination of the cosmic evolution of the neutral gas
component down to z~0.4.
NICMOS 9640
Flats Stability
This calibration proposal is the Cycle 11 NICMOS monthly monitor A
series of camera 1, 2, & 3 flat fields will be obtained to monitor the
health of the cameras.
NICMOS 9423
NICMOS Observations of Transient Infrared Jets in the Galactic
Microquasar GRS1915+105
We propose to use HST/NICMOS to make Target of Opportunity observations
of the galactic microquasar GRS1915+105. This source possesses transient
radio jets which exhibit apparent superluminal motions, and resolved
infrared emission from these jets has been observed in GRS1915+105
{Sams, Eckart, and Sunyaev, 1996; Eikenberry and Fazio, 1996}. Because
the jet ejection events are correlated with X-ray outbursts, we will use
observations of X-ray flares with the Rossi X-Ray Timing Explorer to
trigger the HST observations. We will then monitor GRS1915+105
periodically with NICMOS, obtaining relative astrometry, photometry,
polarimetry, and grism spectroscopy of the jets and the parent object.
These observations will allow us to greatly increase our understanding
of the jets’ radiative mechanisms and physical conditions, and their
evolution with time. We require the capabilities of HST and NICMOS due
to the small angular separations between the jets and the parent object
{increasing from ~ 0.1 to ~ 0.8 arcsec over the span of the TOO
observations} and the high reddening towards GRS1915+105 {A_V ~ 30 mag}.
NICMOS 9702
NICMOS Parallel Thermal Background
NICMOS Camera 2 pure parallel exposures in the F222M and F237M filters
to establish the stability of the HST+NCS+Instrument thermal emission.
This data will be compared against the already available Camera 3
measurements in F222M which show an increased thermal background.
NICMOS 8791
NICMOS Post-SAA calibration – CR Persistence Part 2
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.
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.
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 9608
CCD Bias Monitor – Part 2
Monitor the bias in the 1×1, 1×2, 2×1, and 2×2 bin settings at gain=1,
and 1×1 at gain = 4, to build up high-S/N superbiases and track the
evolution of hot columns.
STIS 9606
CCD Dark Monitor-Part 2
Monitor the darks for the STIS CCD.
STIS 9509
Probing the Distance and Structure of the LMC Using Eclipsing Binaries:
STIS
The distance to the LMC is crucial to calibrating the Cosmic Distance
Scale but remains controversial and uncertain despite the efforts of
many investigators. We have shown that the analysis of eclipsing binary
{EB} systems has the potential to resolve this controversy. We have
determined accurate distances to three eclipsing binaries in the LMC.
Two EBs in the LMC bar, HV 2274 and EROS 1044, yield a consistent
distance of 46.0+/-1.2 kpc for the bar itself. A third system, HV 982,
is located at a greater distance {50.2+/-1.2 kpc}, which is similar to
that of the nearby SN 1987A {51.4+/-1.2 kpc}. These results may suggest
a significant depth to the LMC populations but a larger stellar sample
is needed to verify this. The distances of the program stars were
derived from ground-based light curves, HST or CTIO radial velocity
data, and HST UV/optical spectrophotometry. We propose HST/STIS
low-resolution spectra of seven LMC EBs for which we already have radial
velocity and light curves. This will permit us to complete the analysis
and derive accurate {to ~3%} individual distances. HST/STIS spectroscopy
{covering 115-800nm} is a key dataset because it provides Teff, Fe/H,
and A_lambda. The ensemble of targets, in addition to nailing down the
distance to the LMC, will provide fundamental stellar properties and a
detailed probe of the structure and spatial extent of this important
galaxy, in particular its line-of-sight depth.
STIS 9633
STIS parallel archive proposal – Nearby Galaxies – Imaging and
Spectroscopy
Using parallel opportunities with STIS which were not allocated by the
TAC, we propose to obtain deep STIS imagery with both the Clear {50CCD}
and Long-Pass {F28X50LP} filters in order to make color-magnitude
diagrams and luminosity functions for nearby galaxies. For local group
galaxies, we also include G750L slitless spectroscopy to search for
e.g., Carbon stars, late M giants and S-type stars. This survey will be
useful to study the star formation histories, chemical evolution, and
distances to these galaxies. These data will be placed immediately into
the Hubble Data Archive.
STIS 9706
STIS Pure Parallel Imaging Program: Cycle 10
This is the default archival pure parallel program for STIS during cycle
10.
STIS 9507
STIS/UV snapshot survey of bright AGN
We propose a UV spectroscopic snapshot survey of bright AGN, quadrupling
the number of Seyferts UV spectra and adding dozens of new quasars,
aimed at the following goals: beginenumerate em Finding the relationship
between the intrinsic luminosity of the AGN and the maximum velocity
{and width} of the outflow emanating from it, and determining the
frequency of outflows in low-z AGN as a function of luminosity. em
Surveying IGM absorption line systems in numerous new sight-lines. em
Identifying promising targets for observations with the future highly
sensitive Cosmic Origin Spectrograph. endenumerate A 35-minute snapshot
with exposures in either the G140L or G230L will yield spectra with a
minimum S/N > 15 per resolution element at all wavelengths for all our
potential targets. This will allow us to be sensitive to absorption
lines to a limiting equivalent width of 0.3 Angstrom at the 3 Sigma
level. In order to facilitate rapid observational followup, we waive the
data proprietary period entirely.
STIS 9441
Zinc Abundances in Damped Ly-Alpha Systems at z < 0.5: A Missing Link in
the Chemical History of Galaxies
The evolution of metallicity in damped Lyman alpha {DLA} quasar
absorption systems is an important constraint on the global star
formation history of the universe, but remains a big puzzle at present.
The H I column density weighted mean metallicity in DLAs is expected to
rise to solar values at low redshifts, based on cosmic chemical
evolution models, because the mass-weighted mean metallicity of local
galaxies is near- solar. However, current DLA abundance studies are
highly uncertain and cannot distinguish between evolution and no
evolution in the mean metallicity at redshifts 0.4 < z < 3.5. The
existing data are particularly incomplete because no Zn measurements
exist for z < 0.4, and only 2 exist for z < 0.5, which spans the past
35-45 % of the age of the universe. To pin down the cosmic
age-metallicity relation all the way to the present epoch, we propose to
measure Zn abundances in five DLAs at 0.1 < z < 0.5. We propose to use
HST STIS because it is the only existing instrument that can measure the
necessary UV lines. Our observations will clearly distinguish between no
metallicity evolution vs. the predicted evolution. Our data will also
provide Cr measurements, which will help to estimate the dust abundance.
The proposed observations are crucial for tying together the absorption
and emission histories of gas and stars in galaxies and for clarifying
the relation of DLAs to present-day galaxies.
STIS/CCD/MA1 9357
Towards a global understanding of accretion physics –, Clues from an UV
spectroscopic survey of cataclysmic variables
Accretion inflows and outflows are fundamental phenomena in a wide
variety of astrophysical environments, such as Young Stellar Objects,
galactic binaries, and AGN. Observationally, cataclysmic variables {CVs}
are particularly well suited for the study of accretion processes. We
propose to carry out a STIS UV spectroscopic snapshot survey of CVs that
fully exploits the diagnostic potential of these objects for our
understanding of accretion physics. This survey will provide an
homogenous database of accretion disc and wind outflow spectra covering
a wide range of mass transfer rates and binary inclinations. We will
analyse these spectra with state-of-the-art accretion disc model spectra
{SYNDISK}, testing our current knowledge of the accretion disc
structure, and, thereby, providing new insight into the so far not well
understood process of viscous dissipation. We will use our parameterised
wind model PYTHON for the analysis of the radiation driven accretion
disc wind spectra, assessing the fundamental question whether the mass
loss rate correlates with the disc luminosity. In addition, our survey
data will identify a number of systems in which the white dwarf
significantly contributes to the UV flux, permitting an analysis of the
impact of mass accretion on the evolution of these compact stars. This
survey will at least double, if not triple, the number of high-quality
accretion disc / wind outflow / accreting white dwarf spectra, and we
waive our proprietary rights to permit a timely use of this database.
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.
STIS/MA2 9465
The Cosmic Carbon Budget
Gaseous carbon drives the chemistry of, and is an important coolant in
interstellar clouds. In solid form, carbon is the second most abundant
element in interstellar dust, the key element contributing to
interstellar extinction, and the dominant heat source in some
interstellar clouds. Given the fundamental importance of this element to
interstellar cloud physics, it is surprising that only 8 measurements of
gas- phase carbon abundances exist for neutral clouds; 7 are in diffuse
clouds where the least amount of chemistry and dust incorporation are
expected. The single measurement in a translucent cloud suggests a C
abundance that differs from the diffuse clouds, but the measurement
uncertainties make this difference statistically insignificant. We,
therefore, have no information about carbon’s behavior in translucent
clouds, regions dense enough for chemistry and dust growth to be
important but low enough extinction so that UV spectroscopy is possible
{unlike for molecular clouds}. We propose to measure total gas-phase C
abundances in 6 translucent clouds with our principal scientific goals
being to 1} accurately determine the fraction of carbon in the gas and
dust phases in environments bridging the gap between diffuse and
molecular clouds 2} determine the relative depletions of C and O in
neutral clouds with known O-depletion enhancements and 3} explore how
the interstellar gas-phase C/H is related to extinction variations.
WFPC2 9033
Measuring the mass distribution in the most distant, very X-ray luminous
galaxy cluster known
We propose to obtain a mosaic of deep HST/WFPC2 images to conduct a weak
lensing analysis of the mass distribution in the massive, distant galaxy
cluster ClJ1226.9+3332, recently discovered by us. At z=0.888 this
exceptional system is more X-ray luminous and more distant than both
MS1054.4-0321 and ClJ0152.7-1357, the previous record holders, thus
providing yet greater leverage for cosmological studies of cluster
evolution. ClJ1226.9+3332 differs markedly from all other currently
known distant clusters in that it exhibits little substructure and may
even host a cooling flow, suggesting that it could be the first cluster
to be discovered at high redshift that is virialized. We propose joint
HST and Chandra observations to investigate the dynamical state of this
extreme object. This project will 1} take advantage of HST’s superb
resolution at optical wavelengths to accurately map the mass
distribution within 1.9 h^{-1} 50 Mpc via strong and weak gravitational
lensing, and 2} use Chandra’s unprecedented resolution in the X-ray
waveband to obtain independent constraints on the gas and dark matter
distribution in the cluster core, including the suspected cooling flow
region. As a bonus, the proposed WFPC2 observations will allow us to
test the results by van Dokkum et al. {1998, 1999} on the properties of
cluster galaxies {specifically merger rate and morphologies} at z~0.8
from their HST study of MS1054.4-0321.
WFPC2 9710
POMS Test Proposal: WFII backup parallel archive proposal
This is a POMS test proposal designed to simulate scientific plans.
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.
WFPC2 9709
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 paralell images of random
areas of the sky, following the recommendations of the 2002 Parallels
Working Group.
WFPC2 9594
WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt2/3
This dark calibration program obtains 3 dark frames every day to provide
data for monitoring and characterizing the evolution of hot pixels
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports
of potential non-nominal performance that will be investigated.)
HSTARs:
- 8985 GSACQ(1,3,3) Search Radius Limit Exceeded on both FGS 1 and 3 @ 101/09:06:56z
- 8986 NICMOS Suspends @ 101/13:33:43z
- 8987 ZERO GYRO SAFEMODE ENTRY @ 103/22:21:08z
- 8988 B-String CclParser(on Core Data Server)down @ 104/05:33:04z
COMPLETED OPS REQs:
- 16922-0 Execute ROP NS-9 @ 101/1431z
- 16923-1 NICMOS Suspend Recovery @ 101/2015z
- 16881-1 Contingency Gyro 3 Restart @ 103/2356z (Gyro 3 power on @
- 103/23:51:28z)
- 16924-0 Power on GEA/TAG’s after ZGSP Entry @ 104/00:42:36z
- 16925-0 Dump ESBs @ 104/02:30:39z
- 16927-0 Enable WFPC2 Autorerase @ 104/04:42:24z
- 16928-0 Transition NICMOS to SAAOPER @ 104/04:46:22z
- 16929-2 Real Time Map @ 104/06:55:37z
- 16930-0 Real Time Map @ 104/08:06:45z
- 16931-0 ARU/PRT @ 104/08:28:53z
OPS NOTES EXECUTED:
- 0910-2 SI Console response to MCE Resets after FSW 4.8 is activated @ 101/0910z
- 0924-0 HSTAR Documentation for Guide Star Acq Failure/Loss of Lock @ 101/0906z
- 0900-1 Command Problem @ 102/0425z
- 1096-0 Battery 5 & 6 Temperature Limit Adjustment @ 101/1653z
- 1095-0 Consolidated PCS Limit Modifications @ 103/0651z
SCHEDULED SUCCESSFUL FAILURE TIMES
FGS GSacq 22 21 101/09:06:56z
FGS REacq 23 23
FHST Update 42 42
LOSS of
LOCK
SIGNIFICANT EVENTS:
Transition to SIMOR @ 101/1645z
