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Daily Report #4512

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Old December 21st 07, 05:06 PM posted to sci.astro.hubble
Cooper, Joe
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Posts: 568
Default Daily Report #4512

Note, the next Daily Report won't appear until 12/26

HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science

DAILY REPORT***** # 4512

PERIOD COVERED: UT December 20, 2007 (DOY 354)


ACS/SBC 11145

Probing the Planet Forming Region of T Tauri Stars in Chamaeleon

By studying the inner, planet-forming regions of circumstellar disks
around low-mass pre- main sequence stars we can refine theories of
giant planet formation and develop timescales for the evolution of
disks and their planets. Spitzer infrared observations of T Tauri
stars in the Chamaeleon star-forming region have given us an
unprecedented look at dust evolution in young objects. However,
despite this ground breaking progress in studying the dust in young
disks, the gas properties of the inner disk remain essentially
unknown. Using ACS on HST, we propose to measure the H_2 emission
originating in the innermost disk regions of classical T Tauri stars
in different stages of evolution with the objective of revealing the
timescales of gas dissipation and its relationship to dust evolution.
This proposal is part of a comprehensive effort with approved programs
on Spitzer, Gemini, and Magellan that aim to characterize the state of
gas and dust in disks where planets may already have formed.

ACS/SBC 11199

A Hard Look at Stellar Disks at the Epoch of Planet Formation

We propose to use HST/ACS/SBC and Chandra/ACIS-S3 to observe the high
energy fluxes of 4 stars surrounded by disks in the newly discovered
aggregate 25 Ori, the most populous 10 Myr group known within 500 pc.
Our observations will cover the 1-25A and 1250-2000A bandpasses, and
will complement our optical and Spitzer data for these objects, to
provide essential input to physically-consistent models of disk
structure and chemistry in the age range around 10 Myr, thought to be
a critical period in the planet- forming process. We will be able to
determine the Ne/O ratio and determine if the anomalous metal
abundances observed in X-ray spectra of young stars are an
evolutionary or an environmental effect. Our proposed observations
will double the number of 10 Myr old accreting stars with known high
energy radiation fields, and will be the first FUV observations of low
mass accreting stars in an OB association.

NIC1/NIC2/NIC3 8795

NICMOS Post-SAA calibration - CR Persistence Part 6

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 i mages. Each observation will need its
own CRMAP, as different SAA passages leave different imprints on the
NICMOS detectors.

NIC2 11142

Revealing the Physical Nature of Infrared Luminous Galaxies at 0.3

We aim to determine physical properties of IR luminous galaxies at
0.3z2.7 by requesting coordinated HST/NIC2 and MIPS 70um observations
of a unique, 24um flux- limited sample with complete Spitzer mid-IR
spectroscopy. The 150 sources investigated in this program have S{24um}
0.8mJy and their mid-IR spectra have already provided the majority

targets with spectroscopic redshifts {0.3z2.7}. The proposed
150~orbits of NIC2 and 66~hours of MIPS 70um will provide the physical
measurements of the light distribution at the rest-frame ~8000A and
better estimates of the bolometric luminosity. Combining these
parameters together with the rich suite of spectral diagnostics from
the mid-IR spectra, we will {1} measure how common mergers are among
LIRGs and ULIRGs at 0.3z2.7, and establish if major mergers are the
drivers of z1 ULIRGs, as in the local Universe. {2} study the
co-evolution of star formation and blackhole accretion by
investigating the relations between the fraction of starburst/AGN
measured from mid-IR spectra vs. HST morphologies, L{bol} and z. {3}
obtain the current best estimates of the far- IR emission, thus L{bol}
for this sample, and establish if the relative contribution of mid-to-
far IR dust emission is correlated with morphology {resolved vs.

NIC3 11107

Imaging of Local Lyman Break Galaxy Analogs: New Clues to Galaxy
Formation in the Early Universe

We have used the ultraviolet all-sky imaging survey currently being
conducted by the Galaxy Evolution Explorer {GALEX} to identify for the
first time a rare population of low- redshift starbursts with
properties remarkably similar to high-redshift Lyman Break Galaxies
{LBGs}. These "compact UV luminous galaxies" {UVLGs} resemble LBGs in
terms of size, SFR, surface brightness, mass, metallicity, kinematics,
dust, and color. The UVLG sample offers the unique opportunity of
investigating some very important properties of LBGs that have
remained virtually inaccessible at high redshift: their morphology and
the mechanism that drives their star formation. Therefore, in Cycle 15
we have imaged 7 UVLGs using ACS in order to 1} characterize their
morphology and look for signs of interactions and mergers, and 2}
probe their star formation histories over a variety of timescales. The
images show a striking trend of small-scale mergers turning large
amounts of gas into vigorous starbursts {a process referred to as
dissipational or "wet" merging}. Here, we propose to complete our
sample of 31 LBG analogs using the ACS/SBC F150LP {FUV} and WFPC2
F606W {R} filters in order to create a statistical sample to study the
mechanism that triggers star formation in UVLGs and its implications
for the nature of LBGs. Specifically, we will 1} study the trend
between galaxy merging and SFR in UVLGs, 2} artificially redshift the
FUV images to z=1-4 and compare morphologies with those in similarly
sized samples of LBGs at the same rest-frame wavelengths in e.g.
GOODS, UDF, and COSMOS, 3} determine the presence and morphology of
significant stellar mass in "pre-burst" stars, and 4} study their
immediate environment. Together with our Spitzer {IRAC+MIPS}, GALEX,
SDSS and radio data, the HST observations will form a unique union of
data that may for the first time shed light on how the earliest major
episodes of star formation in high redshift galaxies came about. This
proposal was adapted from an ACS HRC+WFC proposal to meet the new
Cycle 16 observing constraints, and can be carried out using the
ACS/SBC and WFPC2 without compromising our original science goals.

WFPC2 10915

ACS Nearby Galaxy Survey

Existing HST observations of nearby galaxies comprise a sparse and
highly non-uniform archive, making comprehensive comparative studies
among galaxies essentially impossible. We propose to secure HST's
lasting impact on the study of nearby galaxies by undertaking a
systematic, complete, and carefully crafted imaging survey of ALL
galaxies in the Local Universe outside the Local Group. The resulting
images will allow unprecedented measurements of: {1} the star
formation history {SFH} of a 100 Mpc^3 volume of the Universe with a
time resolution of Delta[log{t}]=0.25; {2} correlations between
spatially resolved SFHs and environment; {3} the structure and
properties of thick disks and stellar halos; and {4} the color
distributions, sizes, and specific frequencies of globular and disk
clusters as a function of galaxy mass and environment. To reach these
goals, we will use a combination of wide-field tiling and pointed deep
imaging to obtain uniform data on all 72 galaxies within a
volume-limited sample extending to ~3.5 Mpc, with an extension to the
M81 group. For each galaxy, the wide-field imaging will cover out to
~1.5 times the optical radius and will reach photometric depths of at
least 2 magnitudes below the tip of the red giant branch throughout
the limits of the survey volume. One additional deep pointing per
galaxy will reach SNR~10 for red clump stars, sufficient to recover
the ancient SFH from the color-magnitude diagram. This proposal will
produce photometric information for ~100 million stars {comparable to
the number in the SDSS survey} and uniform multi- color images of half
a square degree of sky. The resulting archive will establish the
fundamental optical database for nearby galaxies, in preparation for
the shift of high- resolution imaging to the near-infrared.


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


11110 - REacq(2,1,1) results in fine lock backup

During LOS REacq(2,1,1) scheduled at 354/16:11:17 resulted in fine
lock backup using FGS 2, with QF1STOPF and QSTOP flags set on FGS 1.
OBAD 2 showed errors of V1= -8.21, V2= -5.72, V3= -10.63, RSS =

11111 - REAcq(2,1,1) results in fine lock backup (2,0,2) using FGS-2

Upon acquisition of signal at 354/21:19:15, the REAcq(2,1,1) scheduled
at 354/20:58:10 - 21:06:15 had resulted to fine lock backup (2,0,2)
using FGS-2, due to stop flag (QF1STOPF) indication on the primary
FGS-1. Pre-acquisition OBAD1 attitude error correction (RSS) not
available pending future ETR Dump. OBAD2 had (RSS) value of 10.05
arcseconds. Post-acq OBAD/MAP not scheduled.



*********************** SCHEDULED***** SUCCESSFUL

FGS GSacq************** 07***************** 07
FGS REacq************** 08***************** 08
OBAD with Maneuver **** 30***************** 30


Ops Request 18165 was successfully executed at 17:09:26 on day 354
(December 20) to uplink the new value for the Universal Kalman Filter
(UKF) bias states process noise (Qab).

In M2G intervals after the UKF re-start, the UKF attitude estimate
remained within approximately 3 degrees of the commanded vehicle
pointing, despite some adverse magnetic field conditions (e.g. SAA
passages). During telemetry-available F2G and T2G post-OBAD intervals,
the UKF attitude estimate remained within approximately 2 degrees of
the known vehicle pointing.* No innovations or residuals failures or
other anomalous signatures occurred.* Real-time monitoring ended at
354/20:15. PCS will continue to trend UKF performance and assess the
effects of this change.


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