HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT      #4944

PERIOD COVERED: 5am October 2 - 5am October 5, 2009 (DOY 275/09:00z-278/09:00z)

OBSERVATIONS SCHEDULED

NIC1/NIC2/NIC3 8795

NICMOS Post-SAA Calibration - CR Persistence Part 6

This is 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 'Use After' 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 darks. 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.

NIC1/NIC2/NIC3 11947

Extended Dark Monitoring

This program takes a series of darks to obtain darks (including

amplifier glow, dark current, and shading profiles) for all three

cameras in the read-out sequences used in Cycle 17. A set of 12 orbits

will be observed every two months for a total of 72 orbits for a 12

month Cycle 17. This is a continuation of Cycle 16 program 11330 scaled

down by ~80%.

The first orbit (Visit A0) should be scheduled in the NICMOS SMOV after

the DC Transfer Test (11406) and at least 36h before the Filter Wheel

Test (11407). Data download using fast track.

The following 28 orbits (visit A1-N2) should be scheduled AFTER the SMOV

Proposal 11407 (Filter Wheel Test). This is done in order to monitor the

dark current following an adjustment of the NCS set-point. These visits

should be executed until the final temperature is reached during SMOV.

WFC3/IR 11936

IR Grism Flux Calibration

This program will determine image displacement, spectral trace and flux

calibration for the IR G102 and G141 grisms as a function of spatial

position within the field of view. The HST flux standard GD71 will be

observed in a 9-point pattern in the IR field of view, which will

provide the necessary image displacement, spectral trace, and throughput

measurements.

WFC3/IR/S/C 11929

IR Dark Current Monitor

Analyses of ground test data showed that dark current signals are more

reliably removed from science data using darks taken with the same

exposure sequences as the science data, than with a single dark current

image scaled by desired exposure time. Therefore, dark current images

must be collected using all sample sequences that will be used in

science observations. These observations will be used to monitor changes

in the dark current of the WFC3-IR channel on a day-to-day basis, and to

build calibration dark current ramps for each of the sample sequences to

be used by GOs in Cycle 17. For each sample sequence/array size

combination, a median ramp will be created and delivered to the

calibration database system (CDBS).

WFC3/IR 11926

IR Zero Points

We will measure and monitor the zeropoints through the IR filters using

observations of the white dwarf standard stars, GD153, GD71 and GD191B2B

and the solar analog standard star, P330E. Data will be taken monthly

during Cycle 17. Observations of the star cluster, NGC 104, are made

twice to check color transformations. We expect an accuracy of 2% in the

wide filter zeropoints relative to the HST photometric system, and 5% in

the medium- and narrow-band filters.

WFC3/UVIS 11924

WFC3/UVIS External and Internal CTE Monitor

CCD detector Charge Transfer Inefficiency (CTI)-induced losses in

photometry and astrometry will be measured using observations of the

rich open cluster NGC6791 and with the EPER (Extended Pixel Edge

Response) method using tungsten lamp flat field exposures. Although we

do not expect to see CTE effects at the outset of Cycle 17, this CTE

monitoring program is the first of a multi-cycle program to monitor and

establish CTE-induced losses with time. We expect to measure CTE effects

with a precision comparable to the ACS measurements.

WFC3/UVIS 11908

Cycle 17: UVIS Bowtie Monitor

Ground testing revealed an intermittent hysteresis type effect in the

UVIS detector (both CCDs) at the level of ~1%, lasting hours to days.

Initially found via an unexpected bowtie-shaped feature in flatfield

ratios, subsequent lab tests on similar e2v devices have since shown

that it is also present as simply an overall offset across the entire

CCD, i.e., a QE offset without any discernable pattern. These lab tests

have further revealed that overexposing the detector to count levels

several times full well fills the traps and effectively neutralizes the

bowtie. Each visit in this proposal acquires a set of three 3x3 binned

internal flatfields: the first unsaturated image will be used to detect

any bowtie, the second, highly exposed image will neutralize the bowtie

if it is present, and the final image will allow for verification that

the bowtie is gone.

WFC3/UVIS 11907

UVIS Cycle 17 Contamination Monitor

The UV throughput of WFC3 during Cycle 17 is monitored via weekly

standard star observations in a subset of key filters covering 200-600nm

and F606W, F814W as controls on the red end. The data will provide a

measure of throughput levels as a function of time and wavelength,

allowing for detection of the presence of possible contaminants.

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

The behavior of the WFC3 UVIS CCD will be monitored daily with a set of

full-frame, four-amp bias and dark frames. A smaller set of 2Kx4K

subarray biases are acquired at less frequent intervals throughout the

cycle to support subarray science observations. The internals from this

proposal, along with those from the anneal procedure (Proposal 11909),

will be used to generate the necessary superbias and superdark reference

files for the calibration pipeline (CDBS).

ACS/WFC3 11882

CCD Hot Pixel Annealing

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 the Wide Field

Channel (WFC). The High Resolution Channel (HRC) visits have been

removed since it could not be repaired during SM4.

ACS/WFC3 11879

CCD Daily Monitor (Part 1)

This program comprises basic tests for measuring the read noise and dark

current of the ACS WFC and for tracking the growth of hot pixels. The

recorded frames are used to create bias and dark reference images for

science data reduction and calibration. This program will be executed

four days per week (Mon, Wed, Fri, Sun) for the duration of Cycle 17. To

facilitate scheduling, this program is split into three proposals. This

proposal covers 352 orbits (22 weeks) from 31 August 2009 to 31 January

2010.

WFC3/ACS/UVIS 11877

HST Cycle 17 and Post-SM4 Optical Monitor

This program is the Cycle 17 implementation of the HST Optical

Monitoring Program.

The 36 orbits comprising this proposal will utilize ACS (Wide Field

Channel) and WFC3 (UVIS Channel) to observe stellar cluster members in

parallel with multiple exposures over an orbit. Phase retrieval

performed on the PSF in each image will be used to measure primarily

focus, with the ability to explore apparent coma, and astigmatism

changes in WFC3.

The goals of this program are to: 1) monitor the overall OTA focal

length for the purposes of maintaining focus within science tolerances

2) gain experience with the relative effectiveness of phase retrieval on

WFC3/UVIS PSFs 3) determine focus offset between the imagers and

identify any SI-specific focus behavior and dependencies

If need is determined, future visits will be modified to interleave

WFC3/IR channel and STIS/CCD focii measurements.

STIS/CCD 11846

CCD Bias Monitor-Part 1

The purpose of this proposal is to monitor the bias in the 1x1, 1x2,

2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4, to build up

high-S/N superbiases and track the evolution of hot columns.

STIS/CCD 11844

CCD Dark Monitor Part 1

The purpose of this proposal is to monitor the darks for the STIS CCD.

WFC3/IR 11838

Completing a Flux-limited Survey for X-ray Emission from Radio Jets

We will measure the changing flow speeds, magnetic fields, and energy

fluxes in well- resolved quasar jets found in our short-exposure Chandra

survey by combining new, deep Chandra data with radio and optical

imaging. We will image each jet with sufficient sensitivity to estimate

beaming factors and magnetic fields in several distinct regions, and so

map the variations in these parameters down the jets. HST observations

will help diagnose the role of synchrotron emission in the overall SED,

and may reveal condensations on scales less than 0.1 arcsec.

FGS 11788

The Architecture of Exoplanetary Systems

Are all planetary systems coplanar? Concordance cosmogony makes that

prediction. It is, however, a prediction of extrasolar planetary system

architecture as yet untested by direct observation for main sequence

stars other than the Sun. To provide such a test, we propose to carry

out FGS astrometric studies on four stars hosting seven companions. Our

understanding of the planet formation process will grow as we match not

only system architecture, but formed planet mass and true distance from

the primary with host star characteristics for a wide variety of host

stars and exoplanet masses.

We propose that a series of FGS astrometric observations with

demonstrated 1 millisecond of arc per-observation precision can

establish the degree of coplanarity and component true masses for four

extrasolar systems: HD 202206 (brown dwarf+planet); HD 128311

(planet+planet), HD 160691 = mu Arae (planet+planet), and HD 222404AB =

gamma Cephei (planet+star). In each case the companion is identified as

such by assuming that the minimum mass is the actual mass. For the last

target, a known stellar binary system, the companion orbit is stable

only if coplanar with the AB binary orbit.

STIS/CCD/MA1 11737

The Distance Dependence of the Interstellar N/O Abundance Ratio: A Gould

Belt

The degree of elemental abundance homogeneity in the interstellar medium

is a function of the enrichment and mixing processes that govern

galactic chemical evolution. Observations of young stars and the

interstellar gas within ~500 pc of the Sun have revealed a local ISM

that is so well-mixed it is having an impact on ideas regarding the

formation of extrasolar planets. However, the situation just beyond the

local ISM is not so clear. Sensitive UV absorption line measurements

have recently revealed a pattern of inhomogeneities in the interstellar

O, N, and Kr gas-phase abundances at distances of ~500 pc and beyond

that appear nucleosynthetic in origin rather than due to dust depletion.

In particular, based on a sample of 13 sightlines, Knauth et al. (2006)

have found that the nearby stars (d < 500 pc) exhibit a mean

interstellar N/O abundance ratio that is significantly higher (0.18 dex)

than that toward the more distant stars. Interestingly, all of their

sightlines lie in the sky vicinity of the Gould Belt of OB associations,

molecular clouds, and diffuse gas encircling the Sun at a distance of

~400 pc. Is it possible that mixing processes have not yet smoothed out

the recent ISM enrichment by massive stars in the young Belt region? By

measuring the interstellar N/O ratios in a strategic new sample of

sightlines with STIS, we propose to test the apparent N/O homogeneity

inside the Gould Belt and determine if the apparent decline in the N/O

ratio with distance is robust and associated with the Belt region.

WFC3/UVIS 11729

Photometric Metallicity Calibration with WFC3 Specialty Filters

The community has chosen to include several filters in the WFC3 filter

complement that have been designed to allow fairly precise estimates of

stellar metallicities, and many science programs are enabled by this

capability. Since these filters do not exactly match those used for this

purpose on the ground, however, the mapping of stellar colors to stellar

metallicities needs to be calibrated. We propose to achieve this

calibration through observations of five stellar clusters with well

known metallicities. We will calibrate several different filter

calibrations which will allow future users to determine what filter

combination best meets their science needs.

WFC3/UVIS 11714

Snapshot Survey for Planetary Nebulae in Local Group Globular Clusters

Planetary nebulae (PNe) in globular clusters (GCs) raise a number of

interesting issues related to stellar and galactic evolution. The number

of PNe known in Milky Way GCs, four, is surprisingly low if one assumes

that all stars pass through a PN stage. However, it is likely that the

remnants of stars now evolving in galactic GCs leave the AGB so slowly

that any ejected nebula dissipates long before the star becomes hot

enough to ionize it. Thus there should not be ANY PNe in Milky Way

GCs--but there are four! It has been suggested that these PNe are the

result of mergers of binary stars within GCs, i.e., that they are

descendants of blue stragglers. The frequency of occurrence of PNe in

external galaxies poses more questions, because it shows a range of

almost an order of magnitude.

I propose a SNAPshot survey aimed at discovering PNe in the GC systems

of Local Group galaxies outside the Milky Way. These clusters, some of

which may be much younger than their counterparts in our galaxy, might

contain many more PNe than those of our own galaxy. I will use the

standard technique of emission-line and continuum imaging, which easily

discloses PNe. This proposal continues a WFPC2 program started in Cycle

16, but with the more powerful WFC3. As a by-product, the survey will

also produce color-magnitude diagrams for numerous clusters for the

first time, reaching down to the horizontal branch.

STIS/CCD/MA1/MA2 11690

EG And: Providing the Missing Link Required for Modeling Red Giant

Mass-Loss

For the majority of red giant stars, the basic mass-loss processes at

work are unknown. Indeed, for stars of spectral types between K0 III and

M5-M6 III, much remains unknown about the regions above the visible

photosphere and the transportation of the processed material outwards to

the ISM. Eclipsing symbiotic binary systems, consisting of an evolved

giant in orbit with a white dwarf, provide an opportunity to take

advantage of the finite size of the hot component to probe different

levels of the chromosphere and wind acceleration region in absorption.

This provides spatially resolved thermal, ionization and dynamic

information on the wind which can then be compared against predictions

of hydrodynamical stellar atmosphere codes. The symbiotic binary EG And

can be considered as a Rosetta Stone for understanding the winds of

these objects. The system is ideal on a number of counts for utilizing

the ultraviolet eclipse of the white dwarf (WD) component to probe,

layer-by-layer, the thermal and dynamic conditions at the very base of

the wind and chromosphere of the RG. This information is vital for

constraining, testing and calibrating the new generation of cool giant

wind+chromosphere models and is not possible to obtain for isolated RGs.

This team has studied the UV eclipses of this system in depth and

detail, however in order to definitively constrain the wind acceleration

profile and identify the location of the temperature rise just above the

photosphere, we require 4 STIS E140M observations of EG And at specific

orbital phases. We are also requesting a E230M observation of an

isolated spectral standard, corresponding to the RG in the binary, which

will help place the EG And results into the context of the general RG

population from analysis of the MgII wind diagnostic lines.

WFC3/UVIS/IR 11685

Supermassive Neutron Stars or Odd Binaries: Searching for Companions to

Pulsars NGC 6440B and Terzan 5J

Recent sensitive pulsar searches of globular clusters uncovered four

pulsars with very high inferred masses, between 1.7 and 2.7 solar

masses. These strongly constrain the behavior of matter in the

ultra-dense interiors of neutron stars, since for most models such

massive neutron stars could not exist. All four masses are inferred from

the measured advance of periastron with time, under the assumption that

it is due to General Relativity only. Here, we propose to test whether

part of the observed periastron advance could be induced by the

quadrupole moment of a suitably large, rotationally distorted companion.

We infer the radii such companions need to have and show that they would

be relatively bright, easily detectable with HST. For one pulsar, M 5B,

we find a plausible candidate counterpart in archival data. We propose

to use 2 orbits with WFC3 to search for suitably large counterparts to

two of the other systems, including the one with the highest inferred

mass.

WFC3/UVIS 11657

The Population of Compact Planetary Nebulae in the Galactic Disk

We propose to secure narrow- and broad-band images of compact planetary

nebulae (PNe) in the Galactic Disk to study the missing link of the

early phases of post-AGB evolution. Ejected AGB envelopes become PNe

when the gas is ionized. PNe expand, and, when large enough, can be

studied in detail from the ground. In the interim, only the HST

capabilities can resolve their size, morphology, and central stars. Our

proposed observations will be the basis for a systematic study of the

onset of morphology. Dust properties of the proposed targets will be

available through approved Spitzer/IRS spectra, and so will the

abundances of the alpha-elements. We will be able thus to explore the

interconnection of morphology, dust grains, stellar evolution, and

populations. The target selection is suitable to explore the nebular and

stellar properties across the galactic disk, and to set constraints on

the galactic evolutionary models through the analysis of metallicity and

population gradients.

ACS 11603

A Comprehensive Study of Dust Formation in Type II Supernovae with HST,

Spitzer, and Gemini

The recent discovery of three extremely bright Type II SNe, (2007it,

2007oc, 2007od) gives us a unique opportunity to combine observations

with HST, Spitzer, and Gemini to study the little understood dust

formation process in Type II SNe. Priority 1 Spitzer Cycle 5 and band 1

Gemini 2008A time has already been approved for this project. Since

late-time Type II SNe are faint and tend to be in crowded fields, we

need the high sensitivity and high spatial resolution of ACS and

NICMOS/NIC2 for these observations. This project is motivated by the

recent detection of large amounts of dust in high redshift galaxies. The

dust in these high-z galaxies must come from young, massive stars so

Type II SNe could be potential sources. The mechanism and the efficiency

of dust condensation in Type II SN ejecta are not well understood,

largely due to the lack of observational data. We plan to produce a

unique dataset, combining spectroscopy and imaging in the visible, near-

and mid-IR covering the key phase, 400- 700 days after maximum when dust

is known to form in the SN ejecta. Therefore, we are proposing for

coordinated HST/NOAO observations (HST ACS, NICMOS/NIC2 & Gemini/GMOS

and TReCS) which will be combined with our Spitzer Cycle 5 data to study

these new bright SNe. The results of this program will place strong

constraints on the formation of dust seen in young high redshift (z>5)

galaxies.

WFC3/UVIS 11594

A WFC3 Grism Survey for Lyman Limit Absorption at z=2

We propose to conduct a spectroscopic survey of Lyman limit absorbers at

redshifts 1.8 < z < 2.5, using WFC3 and the G280 grism. This proposal

intends to complete an approved Cycle 15 SNAP program (10878), which was

cut short due to the ACS failure. We have selected 64 quasars at 2.3 < z

< 2.6 from the Sloan Digital Sky Survey Spectroscopic Quasar Sample, for

which no BAL signature is found at the QSO redshift and no strong metal

absorption lines are present at z > 2.3 along the lines of sight. The

survey has three main observational goals. First, we will determine the

redshift frequency dn/dz of the LLS over the column density range 16.0 <

log(NHI) < 20.3 cm^-2. Second, we will measure the column density

frequency distribution f(N) for the partial Lyman limit systems (PLLS)

over the column density range 16.0 < log(NHI) < 17.5 cm^-2. Third, we

will identify those sightlines which could provide a measurement of the

primordial D/H ratio. By carrying out this survey, we can also help

place meaningful constraints on two key quantities of cosmological

relevance. First, we will estimate the amount of metals in the LLS using

the f(N), and ground based observations of metal line transitions.

Second, by determining f(N) of the PLLS, we can constrain the amplitude

of the ionizing UV background at z~2 to a greater precision. This survey

is ideal for a snapshot observing program, because the on-object

integration times are all well below 30 minutes, and follow-up

observations from the ground require minimal telescope time due to the

QSO sample being bright.

COS/NUV/FUV/WFC3/UVIS/IR 11534

COS-GTO: Atmosphere of a Transiting Planet

COS observations of a transiting planet at different orbital locations

will be useful in identifying the chemical content, size, temperature,

and flows in the atmosphere of a transiting planet.

STIS/CCD/MA1 11525

COS-GTO: STIS High Resolution Observations of the Local ISM

We shall use bright early-type B stars located within 150pc of the Sun

to probe the absorption properties of the interstellar gas associated

with the local cavity. By utilizing the high sensitivity and high

spectral resolution of the HST-STIS spectrograph we shall be able to

place new detection limits on absorption occurring in any highly ionized

gas associated with the lines of NV, SiIV and CIV that may be present

along these sight-lines within the local cavity. These data will be used

to test current theoretical models that generally predict far higher

absorption column densities than have been previously found. Also, the

high spectral resolution will enable far stricter limits to be placed on

the thermal widths of such highly ionized absorption lines, which

previous observations towards the Loop I region have suggested

anomalously narrow profiles consistent with their formation by either

photo ionization or highly non-equilibrium processes.

COS/NUV 11466

NUV Detector Dark

The purpose of this proposal is to measure the NUV detector dark rate by

taking long science exposures with no light on the detector. The

detector dark rate and spatial distribution of counts will be compared

to pre-launch data in order to verify the nominal operation of the

detector, and for use in the CalCOS calibration pipeline. Variations of

count rate as a function of orbital position will be analyzed to find

dependence of dark rate on proximity to the SAA.

WFC3/ACS/IR 11359

Panchromatic WFC3 Survey of Galaxies at Intermediate z: Early Release

Science Program for Wide Field Camera 3

The unique panchromatic capabilities of WFC3 will be used to survey the

structure and evolution of galaxies at the peak of the galaxy assembly

epoch. Deep ultraviolet and near-IR imaging and slitless spectroscopy of

existing deep multi-color ACS fields will be used to gauge

star-formation and the growth of stellar mass as a function of

morphology, structure and surrounding density in the critical epoch 1 <

z < 4. Images in the F225W, F275W, and F336W filters will identify

galaxies at z < 1.5 from their UV continuum breaks, and provide

star-formation indicators tied directly to both local and z > 3

populations. Deep near-IR (F125W and F160W) images will probe the

stellar mass function well below 10^9 Msun for mass-complete samples.

Lastly, the WFC3 slitless UV and near-IR grisms will be used to measure

redshifts and star-formation rates from H- alpha and rest-frame UV

continuum slope. This WFC3 ERS program will survey one 4 x 2 mosaic for

a total area of 50 square arcminutes to 5-sigma depths of m_AB = 27 in

most filters from the mid-UV through the near-IR.

This multicolor high spatial resolution data set will allow the user to

gauge the growth of galaxies through star-formation and merging. High

precision photometric and low- resolution spectroscopic redshifts will

allow accurate determinations of the faint-end of the luminosity and

mass functions, and will shed light on merging and tidal disruption of

stellar and gaseous disks. The WFC3 images will also allow detailed

studies of the internal structure of galaxies, and the distribution of

young and old stellar populations. This program will demonstrate the

unique power of WFC3 by applying its many diverse modes and full

panchromatic capability to a forefront problem in astrophysics.

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports

of potential non-nominal performance that will be investigated.)

HSTARS:

12034 - GSAcq(2,3,3) scheduled at 276/09:26:46z failed due to scan step

           limit exceeded on FGS 3.

           Observation affected, NIC 46 Proposal ID# 08795

HSTAR FOR DAY 269

12031 - REAcq(1,2,1) scheduled to start at 269/09:26:53z ran longer

           than allotted (266 sec). Further review shows FGS2 suffer scan step

           limit exceed on its initial FL-WD attempt but succeeded in the 2nd (ie,

           failure path). The take data flag (P4TAKDAT) didn't come up until

           269/09:32:33z.

HSTAR FOR DAY 246

12032 - REAcq(2,1,1) schedule to start @ 2009.246/05:12:35z lost data

           valid on FGS2 during a Profile slew (and the FGS Mailbox (Q4DMRFGS)went

           to PauseExp (246/05:45:21z). LoL was successfully recovered with take data

           flag (P4TAKDAT) back up (246/05:47:57z). No further LoL events occurred prior

           to PCPTERM (246/06:27:16z).

HSTAR FOR DAY 262

12033 - GSAcq(1,2,1) schedule to start @ 262/01:52:41z lost star

           presence and data valid on FGS1 (262/01:56:32z) during a Profile slew with

           both FGSes going to SSM control (262/02:07:47z). LoL was successfully

           recovered with take data flag (P4TAKDAT) back up (262/02:35:39z).

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

                       SCHEDULED      SUCCESSFUL  

FGS GSAcq               28                  27     

FGS REAcq               23                  23                 

OBAD with Maneuver 24                  24                

LOSS of LOCK                                                                  

SIGNIFICANT EVENTS: (None)