HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5139

PERIOD COVERED: 5am July 15 - 5am July 16, 2010 (DOY 196/09:00z-197/09:00z)

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports

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

HSTARS: (None)

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

                                 SCHEDULED      SUCCESSFUL      

FGS GSAcq                         9               9                

FGS REAcq                          9               9                

OBAD with Maneuver          5               5                

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

COS/FUV/STIS/CCD/MA1 11592

Testing the Origin(s) of the Highly Ionized High-Velocity Clouds: A

Survey of Galactic Halo Stars at z>3 kpc

Cosmological simulation predicts that highly ionized gas plays an

important role in the formation and evolution of galaxies and their

interplay with the intergalactic medium. The NASA HST and FUSE missions

have revealed high-velocity CIV and OVI absorption along extragalactic

sightlines through the Galactic halo. These highly ionized high-velocity

clouds (HVCs) could cover 85% of the sky and have a detection rate

higher than the HI HVCs. Two competing, equally exciting, theories may

explain the origin of these highly ionized HVCs: 1) the "Galactic"

theory, where the HVCs are the result of feedback processes and trace

the disk-halo mass exchange, perhaps including the accretion of matter

condensing from an extended corona; 2) the "Local Group" theory, where

they are part of the local warm-hot intergalactic medium, representing

some of the missing baryonic matter of the Universe. Only direct

distance determinations can discriminate between these models. Our group

has found that some of these highly ionized HVCs have a Galactic origin,

based on STIS observations of one star at z<5.3 kpc. We propose an HST

FUV spectral survey to search for and characterize the high velocity NV,

CIV, and SiIV interstellar absorption toward 24 stars at much larger

distances than any previous searches (4<d<21 kpc, 3<|z|<13 kpc). COS

will provide atomic to highly ionized species (e.g.,OI, CII, CIV, SiIV)

that can be observed at sufficient resolution (R~22, 000) to not only

detect these highly ionized HVCs but also to model their properties and

understand their physics and origins. This survey is only possible

because of the high sensitivity of COS in the FUV spectral range.

STIS/CC 11845

CCD Dark Monitor Part 2

Monitor the darks for the STIS CCD.

STIS/CC 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 11999

JWST Calibration from a Consistent Absolute Calibration of Spitzer &

Hubble

Recently, Gordon, Bohlin, et al. submitted a successful Spitzer proposal

for cross calibration of HST and Spitzer. The cross-calibration targets

are stars in three categories: WDs, A-stars, and G-stars. Traditionally,

IR flux standards are extrapolations of stellar models that are tied to

absolute fluxes at shorter wavelengths. HST absolute flux standards are

among the best available with a solid basis that uses pure hydrogen

models of hot WD stars for the SED slopes and is tied to Vega at 5556A

via precise Landolt V-band photometry. Consistently matching models to

our three categories of HST observations along with Spitzer photometry

and the few existing absolute IR flux determinations will provide a

solid basis for JWST flux calibration over its 0.8-30micron range. The

goal of this proposal is to complete the HST observations of the set of

HST/Spitzer cross-calibration stars. Using a variety of standard stars

with three different spectral types will ensure that the final

calibration is not significantly affected by systematic uncertainties.

WFC3/IR 11666

Chilly Pairs: A Search for the Latest-type Brown Dwarf Binaries and the

Prototype Y Dwarf

We propose to use HST/WFC3 to image a sample of 27 of the nearest (< 20

pc) and lowest luminosity T-type brown dwarfs in order to identify and

characterize new very low mass binary systems. Only 3 late-type T dwarf

binaries have been found to date, despite that fact that these systems

are critical benchmarks for evolutionary and atmospheric models at the

lowest masses. They are also the most likely systems to harbor Y dwarf

companions, an as yet unpopulated putative class of very cold (T < 600

K) brown dwarfs. Our proposed program will more than double the number

of T5-T9 dwarfs imaged at high resolution, with an anticipated yield of

~5 new binaries with initial characterization of component spectral

types. We will be able to probe separations sufficient to identify

systems suitable for astrometric orbit and dynamical mass measurements.

We also expect one of our discoveries to contain the first Y-type brown

dwarf. Our proposed program complements and augments ongoing

ground-based adaptive optics surveys and provides pathway science for

JWST.

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/UV 11605

Obtaining the Missing Links in the Test of Very Low Mass Evolutionary

Models with HST

We are proposing for spatially resolved ACS+HRC observations of 11 very

low mass binaries spanning late-M, L and T spectral types in order to

obtain precise effective temperature measurements for each component.

All of our targets are part of a program in which we are measuring

dynamical masses of very low-mass binaries to an unprecedented precision

of 10% (or better). However, without precise temperature measurements,

the full scientific value of these mass measurements cannot be realized.

Together, mass and temperature measurements will allow us to distinguish

between brown dwarf evolutionary models that make different assumptions

about the interior and atmospheric structure of these ultra-cool

objects. While dynamical masses can be obtained from the ground in the

near-IR, obtaining precise temperatures require access to optical data

which, for these sub-arcsecond binaries, can only be obtained from space

with Hubble.

WFC3/UV/ACS/WFC/IR 12057

A Panchromatic Hubble Andromeda Treasury - I

We propose to image the north east quadrant of M31 to deep limits in the

UV, optical, and near-IR. HST imaging should resolve the galaxy into

more than 100 million stars, all with common distances and foreground

extinctions. UV through NIR stellar photometry (F275W, F336W with

WFC3/UVIS, F475W and F814W with ACS/WFC, and F110W and F160W with

WFC3/NIR) will provide effective temperatures for a wide range of

spectral types, while simultaneously mapping M31's extinction. Our

central science drivers are to: understand high-mass variations in the

stellar IMF as a function of SFR intensity and metallicity; capture the

spatially-resolved star formation history of M31; study a vast sample of

stellar clusters with a range of ages and metallicities. These are

central to understanding stellar evolution and clustered star formation;

constraining ISM energetics; and understanding the counterparts and

environments of transient objects (novae, SNe, variable stars, x-ray

sources, etc.). As its legacy, this survey adds M31 to the Milky Way and

Magellanic Clouds as a fundamental calibrator of stellar evolution and

star-formation processes for understanding the stellar populations of

distant galaxies. Effective exposure times are 977s in F275W, 1368s in

F336W, 4040s in F475W, 4042s in F814W, 699s in F110W, and 1796s in

F160W, including short exposures to avoid saturation of bright sources.

These depths will produce photon-limited images in the UV. Images will

be crowding-limited in the optical and NIR, but will reach below the red

clump at all radii. The images will reach the Nyquist sampling limit in

F160W, F475W, and F814W.

WFC3/UVIS 11577

Opening New Windows on the Antennae with WFC3

We propose to use WFC3 to provide key observations of young star

clusters in "The Antennae" (NGC4038/39). Of prime importance is the

WFC3's ability to push the limiting UV magnitude FIVE mag deeper than

our previous WFPC2 observations. This corresponds to pushing the

limiting cluster mass from ~10**5 to ~10**3 solar masses for cluster

ages ~10**8 yrs. In addition, the much wider field of view of the WFC3

IR channel will allow us to map out both colliding disks rather than

just the Overlap Region between them. This will be especially important

for finding the youngest clusters that are still embedded in their

placental cocoons. The extensive set of narrow-band filters will provide

an effective means for determining the properties of shocks, which are

believed to be a primary triggering mechanism for star formation. We

will also use ACS in parallel with WFC3 to observe portions of both the

northern and southern tails at no additional orbital cost. Finally, one

additional primary WFC3 orbit will be used to supplement exisiting HST

observations of the star-forming "dwarf" galaxy at the end of the

southern tail. Hence, when completed we will have full UBVI + H_alpha

coverage (or more for the main galaxy) of four different environments in

the Antennae. In conjunction with the extensive multi- wavelength

database we have collected (both HST and ground based) these

observations will provide answers to fundamental questions such as: How

do these clusters form and evolve? How is star formation triggered? How

do star clusters affect the local and global ISM, and the evolution of

the galaxy as a whole? The Antennae galaxies are the nearest example of

a major disk--disk merger, and hence may represent our best chance for

understanding how mergers form tremendous numbers of clusters and stars,

both in the local universe and during galaxy assembly at high redshift.

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.

WFC3/UVIS 11661

The Black Hole Mass - Bulge Luminosity Relationship for the Nearest

Reverberation-Mapped AGNs

We propose to obtain WFC3 host galaxy images of the eight nearest AGNs

with masses from reverberation mapping, and one star as a PSF model.

These images will allow us to determine with unprecedented accuracy the

bulge luminosities of the host galaxies, a goal which is not achievable

from the ground due to the blurring of the very bright PSF component

under typical, and even very good, seeing conditions. High-resolution

ACS images of the host galaxies of more luminous AGNs reveal that the

black hole mass-bulge luminosity and black hole mass-bulge mass

relationships for AGNs are not well constrained and arise from what

appear to be fundamentally flawed data sets. With the addition of the

images proposed here to our current sample of ACS images, we will be

able to extend our determinations of the black hole mass- bulge

luminosity and black hole mass-bulge mass relationships for AGNs by an

order of magnitude and test our preliminary results for these

fundamentally important relationships against those previously

determined for quiescent galaxies.

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).

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.

NASA office: 301-286-2876

__________________________________________________________
Lynn F. Bassford
Hubble Space Telescope
CHAMP Mission Operations Manager
CHAMP Flight Operations Team Manager
Lockheed Martin Mission Services (LMMS)

"...Hubble is the most significant science instrument of all time in terms of its productivity..."     Scott Altman @12:45pm 5/21/9 STS-125 Senate Subcommittee Hearing