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Daily Report #5060



 
 
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Old March 25th 10, 05:10 PM posted to sci.astro.hubble
Bassford, Lynn[_2_]
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Default Daily Report #5060

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5060

PERIOD COVERED: 5am March 24 - 5am March 25, 2010 (DOY 083/09:00z-084/09:00z)

OBSERVATIONS SCHEDULED

ACS/WFC 11995

CCD Daily Monitor (Part 2)

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 320 orbits (20 weeks) from 1 February
2010 to 20 June 2010.

S/C 11550

COS-GTO: X-Ray Binaries

This is a program to obtain UV spectra of soft X-ray transients (SXTs)
in their quiescent states. The target, A0620-00, is an interacting
binary system with a K7V donor star and a 9.7 M_solar black hole
accretor. Our observations will use the COS G140L and STIS G230L modes
to obtain low spectral resolution (R= 1000-2000), broadband (1230-3200
A) spectra of A0620-00. We will also obtain contemporaneous optical
spectra of the system, which varies on time scales of days. The data
will be used to establish the broadband SED of the system and to
measure emission line strengths and widths in the UV. The dereddened
SED will be modeled to determine the structure and temperature of the
accretion disk. The FUV region of the spectrum, which has not been
observed before, will be a key parameter in constraining the
temperature and inner truncation radius of the disk, which is believed
to transition to an advection-dominated accretion flow (ADAF) at large
distances from the black hole in quiescent SXTs. The UV line spectrum,
and in particular the NV 1240 and CIV 1550 transitions, will show
whether C depletions, which have been seen in the NIR spectrum of the
donor star, are present in the accretion disk and whether enhanced N
abundances are also seen, indicative of CNO processing of material
during the evolutionary history of the binary. Comparison of emission
line velocities between the optical HI emission and the ionized UV
metal transitions will also be used to constrain the relative extents
of the photoionized disk chromosphere and the bulk of the disk in
quiescent black hole binaries.

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 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 deg. C to the ambient instrument
temperature (~ +5 deg. 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.

WFC3/IR 11666

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

We propose to use HST/NICMOS 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 11928

WFC3/IR Low-Frequency Flat and Geometric Distortion

Multiple observations of globular cluster Omega Cen at multiple
infrared wavelengths of IR detector will be used to derive filter
dependency of low-frequency sensitivity (L_flat fields) across of IR
detector and its time variation. Additionally, the same data will be
also used to derive filter-dependant geometric distortion of the
detector and its time-dependency.

WFC3/IR/ACS/WFC 11663

Formation and Evolution of Massive Galaxies in the Richest
Environments at 1.5 z 2.0

We propose to image seven 1.5z2 clusters and groups from the IRAC
Shallow Cluster Survey with WFC3 and ACS in order to study the
formation and evolution of massive galaxies in the richest
environments in the Universe in this important redshift range. We will
measure the evolution of the sizes and morphologies of massive cluster
galaxies, as a function of redshift, richness, radius and local
density. In combination with allocated Keck spectroscopy, we will
directly measure the dry merger fraction in these clusters, as well as
the evolution of Brightest Cluster Galaxies (BCGs) over this redshift
range where clear model predictions can be confronted. Finally we will
measure both the epoch of formation of the stellar populations and the
assembly history of that stellar mass, the two key parameters in the
modern galaxy formation paradigm.

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 11919

WFC3 UVIS PSF Wings

The UVIS PSF wings will be evaluated at 5 field points (near the field
center and corners) in two filters (F275W and F625W) to check for
image stability. Subarray images of a moderately bright, isolated star
will be obtained at each field position with a series of increasing
exposure times designed to permit construction of a very high SNR PSF
with dynamic range sufficient to evaluate the wing intensity to 5
arcsec radius. Deep, saturated full field images will also be obtained
at each field point to permit evaluation of the wings at larger radii.
The images will also permit examination of potential straylight
effects, image persistence and electronic cross-talk.

WFC3/UVIS 11732

The Temperature Profiles of Quasar Accretion Disks

We can now routinely measure the size of quasar accretion disks using
gravitational microlensing of lensed quasars. At optical wavelengths
we observe a size and scaling with black hole mass roughly consistent
with thin disk theory but the sizes are larger than expected from the
observed optical fluxes. One solution would be to use a flatter
temperature profile, which we can study by measuring the wavelength
dependence of the disk size over the largest possible wavelength
baseline. Thus, to understand the size discrepancy and to probe closer
to the inner edge of the disk we need to extend our measurements to UV
wavelengths, and this can only be done with HST. For example, in the
UV we should see significant changes in the optical/UV size ratio with
black hole mass. We propose monitoring 5 lenses spanning a broad range
of black hole masses with well-sampled ground based light curves,
optical disk size measurements and known GALEX UV fluxes during Cycles
17 and 18 to expand from our current sample of two lenses. We would
obtain 5 observations of each target in each Cycle, similar to our
successful strategy for the first two targets.

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).

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated.)

HSTARS:

#12228 GSAcq(1,2,1) @083/20:27:16z and REAcqs @ 083/22:03:30z,
083/23:39:22z, 084/01:15:13z and 084/02:51:05z failed to fine lock
backup on FGS 1.

Observations possibly affected: STIS #31-54 Proposal #11550

COMPLETED OPS REQUEST:

#18834-1 Clear GENSLEW Slot-12 for STIS proposal 11550 @ 083/17:08z

COMPLETED OPS NOTES: (None)

SIGNIFICANT EVENTS: (None)

 




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