HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5117

PERIOD COVERED: 5am June 14 - 5am June 15, 2010 (DOY 165/09:00z-166/09:00z)

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports

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

HSTARS:

12302 - GSAcq(1,2,1) scheduled at 166/05:02:06z and REAcqs(1,2,1) at

166/06:33:31z and at 166/08:09:26z all resulted in fine lock backup

(1,0,1) using FGS 1.

Observations possibly affected: COS 16 -21 Proposal ID#11598; WFC3 44, 46, 49

Proposal ID#11700; WFC3 45, 47, 48, 50, 51 Proposal ID#11906; STIS 16 - 17

Proposal ID#11849.

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

SCHEDULED SUCCESSFUL

FGS GSAcq 12 12

FGS REAcq 5 5

OBAD with Maneuver 7 7

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

ACS/SBC 12016

The Stars and Edge-on Disks of PDS 144: An Intermediate-Mass Analog of

Wide T Tauri Multiple Stars

High-Inclination PMS stars are optimally oriented to measure disk size,

height, to detect jets, and to directly probe disk composition. Placing

these data into evolutionary context requires dates for the systems and

measurements of L bol, and extinction. For such stars, X-ray data

provide L x, but also N(H) and the total extinction. FUV data measures L

UV, and constrains the shape of the extinction curve. Recent studies

have suggested that the frequency of Jovian-mass planets is higher for

systems with intermediate-mass stars, due to disk mass or composition.

While suitable low mass YSOs are well-represented in the Chandra and HST

archives, similar data are lacking for higher mass systems. We propose

joint Chandra and HST imaging of PDS 144 to fill this gap.

COS/FUV 11895

FUV Detector Dark Monitor

Monitor the FUV detector dark rate by taking long science exposures

without illuminating the detector. The detector dark rate and spatial

distribution of counts will be compared to pre-launch and SMOV data in

order to verify the nominal operation of the detector. Variations of

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

dependence of dark rate on proximity to the SAA. Dependence of dark rate

as function of time will also be tracked.

COS/FUV/COS/NUV 11598

How Galaxies Acquire their Gas: A Map of Multiphase Accretion and

Feedback in Gaseous Galaxy Halos

We propose to address two of the biggest open questions in galaxy

formation - how galaxies acquire their gas and how they return it to the

IGM - with a concentrated COS survey of diffuse multiphase gas in the

halos of SDSS galaxies at z = 0.15 - 0.35. Our chief science goal is to

establish a basic set of observational facts about the physical state,

metallicity, and kinematics of halo gas, including the sky covering

fraction of hot and cold material, the metallicity of infall and

outflow, and correlations with galaxy stellar mass, type, and color -

all as a function of impact parameter from 10 - 150 kpc. Theory suggests

that the bimodality of galaxy colors, the shape of the luminosity

function, and the mass-metallicity relation are all influenced at a

fundamental level by accretion and feedback, yet these gas processes are

poorly understood and cannot be predicted robustly from first

principles. We lack even a basic observational assessment of the

multiphase gaseous content of galaxy halos on 100 kpc scales, and we do

not know how these processes vary with galaxy properties. This ignorance

is presently one of the key impediments to understanding galaxy

formation in general. We propose to use the high-resolution gratings

G130M and G160M on the Cosmic Origins Spectrograph to obtain sensitive

column density measurements of a comprehensive suite of multiphase ions

in the spectra of 43 z < 1 QSOs lying behind 43 galaxies selected from

the Sloan Digital Sky Survey. In aggregate, these sightlines will

constitute a statistically sound map of the physical state and

metallicity of gaseous halos, and subsets of the data with cuts on

galaxy mass, color, and SFR will seek out predicted variations of gas

properties with galaxy properties. Our interpretation of these data will

be aided by state-of-the-art hydrodynamic simulations of accretion and

feedback, in turn providing information to refine and test such models.

We will also use Keck, MMT, and Magellan (as needed) to obtain optical

spectra of the QSOs to measure cold gas with Mg II, and optical spectra

of the galaxies to measure SFRs and to look for outflows. In addition to

our other science goals, these observations will help place the Milky

Way's population of multiphase, accreting High Velocity Clouds (HVCs)

into a global context by identifying analogous structures around other

galaxies. Our program is designed to make optimal use of the unique

capabilities of COS to address our science goals and also generate a

rich dataset of other absorption-line systems along a significant total

pathlength through the IGM (Delta z ~ 20).

COS/NUV 11538

COS-GTO: Imaging of Mid-UV Emissions from Io in Eclipse

The atmosphere and corona of Jupiter's volcanic moon Io emit light at a

wide variety of wavelengths, from FUV neutral O and S lines to SO

emission at 1.7 microns. These emissions provide important constraints

on the distribution and chemistry of Io's atmosphere, and Io's

interaction with the Jovian magnetosphere. The neutral O and S FUV

emissions, shortward of 2000?, have been imaged extensively by HST/STIS

and visible emissions (from neutral Na, K and O line emission, and SO2

continuum emission) have been imaged by the Galileo, Cassini, and New

Horizons spacecraft, but the spatial distribution of emissions in the

2000-3000? region, thought to be dominated by SO2 electron impact

continuum emission, has not yet been determined. Earlier long-slit

observations with STIS indicated strong concentration of 2800? emission

over the active volcano Prometheus (Jessup et al. 2004), suggesting

local volcanic control, but Cassini images suggest that the SO2

continuum seen at longer wavelengths is instead concentrated over the

sub-Jovian and anti-Jovian points where there are magnetic connections

between Io and the Jovian magnetosphere- the anti-Jovian point is close

to Prometheus. A series of 200-second integrations taken in Jupiter

eclipse should determine whether emission is concentrated over volcanos

or over the sub-Jovian point, and should be able to observe motion of

the emission due to changing magnetic field orientation if it is

magnetically controlled. This observation will also provide experience

in the use of COS in imaging mode.

COS/NUV 11894

NUV Detector Dark Monitor

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 and SMOV data in

order to verify the nominal operation of the detector. Variations of

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

dependence of dark rate on proximity to the SAA. Dependence of dark rate

as function of time will also be tracked.

S/C/WFC3/IR 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).

STIS/CCD 11721

Verifying the Utility of Type Ia Supernovae as Cosmological Probes:

Evolution and Dispersion in the Ultraviolet Spectra

The study of distant type Ia supernova (SNe Ia) offers the most

practical and immediate discriminator between popular models of dark

energy. Yet fundamental questions remain over possible

redshift-dependent trends in their observed and intrinsic properties.

High quality Keck spectroscopy of a representative sample of 36

intermediate redshift SNe Ia has revealed a surprising, and unexplained,

diversity in their rest-frame UV fluxes. One possible explanation is

hitherto undiscovered variations in the progenitor metallicity.

Unfortunately, this result cannot be compared to local UV data as only

two representative SNe Ia have been studied near maximum light. Taking

advantage of two new `rolling searches' and the restoration of STIS, we

propose a non-disruptive TOO campaign to create an equivalent comparison

local sample. This will allow us to address possible evolution in the

mean UV spectrum and its diversity, an essential precursor to the study

of SNe beyond z~1.

STIS/CCD 11818

NICMOS confirmation of an extrasolar planet candidate directly detected

with ACS

With ACS/HRC coronagraphy, we have achieved the direct detection of a

planet candidate in F606W and F814W around a bright nearby star with a

debris belt. The planet candidate, Fomalhaut b, lies 18 astronomical

units interior to the dust belt and we detect counterclockwise orbital

motion in observations separated by 1.75 years. The candidate has mass

no greater than three Jupiter masses based on an analysis of its

luminosity and the dynamical argument that a significantly more massive

object would disrupt the dust belt. Using recent model predictions for

100-300 Myr old planetary atmospheres, the planet candidate has a

temperature of ~400 K and a mass 1.6 - 3.4 M_J. Variability at optical

wavelengths suggests additional sources of luminosity such as H-alpha

emission or the episodic accretion of cometary material. Here we propose

follow-up observations with HST/STIS c oronagraphy. We employ an

observing strategy that is identical to the one used for the detection

using ACS/HRC coronagraphy. The key goal is recovery of Fomalhaut b in a

third epoch that will also provide crucial astrometric information to

determine its orbit. From the new orbit estimate and models of dynamical

interactions with the surrounding debris belt, we aim to further

constrain the mass of Fomalhaut b and the evolutionary history of the

system.

STIS/CCD 11845

CCD Dark Monitor Part 2

Monitor the darks for the STIS CCD.

STIS/CCD 11847

CCD Bias Monitor-Part 2

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 11849

STIS CCD Hot Pixel Annealing

This purpose of this activity is to repair radiation induced hot pixel

damage to the STIS CCD by warming the CCD to the ambient instrument

temperature and annealing radiation damaged pixels. Radiation damage

creates hot pixels in the STIS CCD Detector. Many of these hot pixels

can be repaired by warming the CCD from its normal operating temperature

near -83 C to the ambient instrument temperature (~ +5 C) for several

hours. The number of hot pixels repaired is a function of annealing

temperature. The effectiveness of the CCD hot pixel annealing process is

assessed by measuring the dark current behavior before and after

annealing and by searching for any window contamination effects.

STIS/CCD/STIS/MA2 11568

A SNAPSHOT Survey of the Local Interstellar Medium: New NUV Observations

of Stars with Archived FUV Observations

We propose to obtain high-resolution STIS E230H SNAP observations of

MgII and FeII interstellar absorption lines toward stars within 100

parsecs that already have moderate or high-resolution far-UV (FUV),

900-1700 A, observations available in the MAST Archive. Fundamental

properties, such as temperature, turbulence, ionization, abundances, and

depletions of gas in the local interstellar medium (LISM) can be

measured by coupling such observations. Due to the wide spectral range

of STIS, observations to study nearby stars also contain important data

about the LISM embedded within their spectra. However, unlocking this

information from the intrinsically broad and often saturated FUV

absorption lines of low-mass ions, (DI, CII, NI, OI), requires first

understanding the kinematic structure of the gas along the line of

sight. This can be achieved with high resolution spectra of high-mass

ions, (FeII, MgII), which have narrow absorption lines, and can resolve

each individual velocity component (interstellar cloud). By obtaining

short (~10 minute) E230H observations of FeII and MgII, for stars that

already have moderate or high-resolution FUV spectra, we can increase

the sample of LISM measurements, and thereby expand our knowledge of the

physical properties of the gas in our galactic neighborhood. STIS is the

only instrument capable of obtaining the required high resolution data

now or in the foreseeable future.

WFC3/IR 11694

Mapping the Interaction between High-Redshift Galaxies and the

Intergalactic Environment

With the commissioning of the high-throughput large-area camera WFC3/IR,

it is possible for the first time to undertake an efficient survey of

the rest-frame optical morphologies of galaxies at the peak epoch of

star formation in the universe. We therefore propose deep WFC3/IR

imaging of over 320 spectroscopically confirmed galaxies between

redshift 1.6 < z < 3.4 in well-studied fields which lie along the line

of sight to bright background QSOs. The spectra of these bright QSOs

probe the IGM in the vicinity of each of the foreground galaxies along

the line of sight, providing detailed information on the physical state

of the gas at large galactocentric radii. In combination with our

densely sampled UV/IR spectroscopy, stellar population models, and

kinematic data in these fields, WFC3/IR imaging data will permit us to

construct a comprehensive picture of the structure, dynamics, and star

formation properties of a large population of galaxies in the early

universe and their effect upon their cosmological environment.

WFC3/IR 11719

A Calibration Database for Stellar Models of Asymptotic Giant Branch

Stars

Studies of galaxy formation and evolution rely increasingly on the

interpretation and modeling of near-infrared observations. At these

wavelengths, the brightest stars are intermediate mass asymptotic giant

branch (AGB) stars. These stars can contribute nearly 50% of the

integrated luminosity at near infrared and even optical wavelengths,

particularly for the younger stellar populations characteristic of

high-redshift galaxies (z>1). AGB stars are also significant sources of

dust and heavy elements. Accurate modeling of AGB stars is therefore of

the utmost importance.

The primary limitation facing current models is the lack of useful

calibration data. Current models are tuned to match the properties of

the AGB population in the Magellanic Clouds, and thus have only been

calibrated in a very narrow range of sub-solar metallicities.

Preliminary observations already suggest that the models are

overestimating AGB lifetimes by factors of 2-3 at lower metallicities.

At higher (solar) metallicities, there are no appropriate observations

for calibrating the models.

We propose a WFC3/IR SNAP survey of nearby galaxies to create a large

database of AGB populations spanning the full range of metallicities and

star formation histories. Because of their intrinsically red colors and

dusty circumstellar envelopes, tracking the numbers and bolometric

fluxes of AGB stars requires the NIR observations we propose here. The

resulting observations of nearby galaxies with deep ACS imaging offer

the opportunity to obtain large (100-1000's) complete samples of AGB

stars at a single distance, in systems with well-constrained star

formation histories and metallicities.

WFC3/IR 11929