Daily Rpt #4601
Bassford, Lynn
DAILY REPORT # 4601
PERIOD COVERED: 5am April 30 - 5am May 01, 2008 (DOY 121/0900z - 122/0900z)
OBSERVATIONS SCHEDULED
ACS/SBC 11131
Star formation at large radii in cooling flow brightest cluster galaxies
We propose to take deep ACS FUV images of the bright central galaxies in two
powerful cooling flow clusters for which we have VLT UBR images, with the
object of determining whether the UV excesses we observe at large radii
(>15kpc) are caused by young stars, ultrahot (WR) stars, or an as yet
unknown source. Current models of excess UV light at the AGN-dominated
centers of these galaxies cannot easily be extended to large radii. New
understanding of star formation in these clusters will be directly
applicable to scenarios of galaxy formation in the early universe.
ACS/SBC 11220
Mapping the FUV Evolution of Type IIn Supernovae
We will use the PR110L prism on the SBC of ACS to map the FUV evolution of
Type IIn supernovae {SNe}. The main goal of this proposal is to measure the
FUV continuum, Ly-a emission line flux, and their evolution to {1} quantify
and interpret Type IIn SN transient event detections at high redshift and
{2} dramatically improve current high redshift Type IIn selection criteria.
We show that the inherent properties of Type IIn SNe facilitate high
redshift detection. We will observe the rest-frame FUV of a sample of eight
0.02 < z < 0.33 Type IIn SNe to directly measure the survival of Ly-alpha
photons in low to intermediate redshift Type IIn SNe environments and
extrapolate the results to high redshift. We will calibrate relationships
such as FUV luminosity vs. emission line flux and measure emission line
evolution vs. FUV light evolution. The intent is to categorize and improve
the utility of Type IIn SNe.
FGS 11210
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.
FGS 11211
An Astrometric Calibration of Population II Distance Indicators
In 2002 HST produced a highly precise parallax for RR Lyrae. That
measurement resulted in an absolute magnitude, M{V}= 0.61+/-0.11, a useful
result, judged by the over ten refereed citations each year since. It is,
however, unsatisfactory to have the direct, parallax-based, distance scale
of Population II variables based on a single star. We propose, therefore, to
obtain the parallaxes of four additional RR Lyrae stars and two Population
II Cepheids, or W Vir stars. The Population II Cepheids lie with the RR
Lyrae stars on a common K-band Period-Luminosity relation. Using these
parallaxes to inform that relationship, we anticipate a zero-point error of
0.04 magnitude. This result should greatly strengthen confidence in the
Population II distance scale and increase our understanding of RR Lyrae star
and Pop II Cepheid astrophysics.
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/WFPC2 11142
Revealing the Physical Nature of Infrared Luminous Galaxies at 0.3<z<2.7
Using HST and Spitzer
We aim to determine physical properties of IR luminous galaxies at 0.3<z<2.7
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 {0.3<z<2.7}. 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 0.3<z<2.7, and establish if major mergers are
the drivers of z>1 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. unresolved}.
WFPC2 11022
WFPC2 Cycle 15 Decontaminations and Associated Observations
This proposal is for the WFPC2 decons. Also included are instrument monitors
tied to decons: photometric stability check, focus monitor, pre- and
post-decon internals {bias, intflats, kspots, & darks}, UV throughput check,
VISFLAT sweep, and internal UV flat check.
WFPC2 11130
AGNs with Intermediate-mass Black Holes: Testing the Black Hole-Bulge
Paradigm, Part II
The recent progress in the study of central black holes in galactic nuclei
has led to a general consensus that supermassive {10^6-10^9 solar mass}
black holes are closely connected with the formation and evolutionary
history of large galaxies, especially their bulge component. Two outstanding
issues, however, remain unresolved. Can central black holes form in the
absence of a bulge? And does the mass function of central black holes extend
below 10^6 solar masses? Intermediate-mass black holes {<10^6 solar masses},
if they exist, may offer important clues to the nature of the seeds of
supermassive black holes. Using the SDSS, our group has successfully
uncovered a new population of AGNs with intermediate-mass black holes that
reside in low-luminosity galaxies. However, very little is known about the
detailed morphologies or structural parameters of the host galaxies
themselves, including the crucial question of whether they have bulges or
not. Surprisingly, the majority of the targets of our Cycle 14 pilot program
have structural properties similar to dwarf elliptical galaxies. The
statistics from this initial study, however, are really too sparse to reach
definitive conclusions on this important new class of black holes. We wish
to extend this study to a larger sample, by using the Snapshot mode to
obtain WFPC2 F814W images from a parent sample of 175 AGNs with
intermediate- mass black holes selected from our final SDSS search. We are
particularly keen to determine whether the hosts contain bulges, and if so,
how the fundamental plane properties of the host depend on the mass of their
central black holes. We will also investigate the environment of this unique
class of AGNs.
WFPC2 11160
Escape fraction and stellar populations in a highly magnified
Lyman-Break Galaxy
Understanding how star-forming galaxies contribute to cosmic reionization is
one of the frontiers of observational cosmology. A key ingredient in this
issue is measuring the escape fraction of Lyman-continuum photons in high
redshift galaxies (z>3). Gravitationally lensed Lyman-break galaxies (LBGs)
act as important laboratories for studying the resolved physical properties
at sub-kpc scales with high signal-to-noise. Correlating the local escape
fraction with physical parameters derived from stellar population modeling
(such as the star formation rate, age and reddening) will offer new insights
into understanding the physical processes involved with the production of
ionizing photons. We propose here follow-up observations of the "Cosmic
Eye", a remarkable, highly magnified (x 30), Lyman-break galaxy at z~3.07
using WFPC2 and NICMOS. Deep ultraviolet WFPC2 imaging will provide a
detailed study of variations in the escape fraction, while WFPC2 and
NICMOS/NIC2 imaging will complement the current broad-band detections to
allow a precise modeling of the spatially-dependent spectral energy
distribution. This will allow the first comprehensive analysis between the
escape fraction, the local SED and the dynamics of a distant galaxy.
WFPC2 11178
Probing Solar System History with Orbits, Masses, and Colors of
Transneptunian Binaries
The recent discovery of numerous transneptunian binaries {TNBs} opens a
window into dynamical conditions in the protoplanetary disk where they
formed as well as the history of subsequent events which sculpted the outer
Solar System and emplaced them onto their present day heliocentric orbits.
To date, at least 47 TNBs have been discovered, but only about a dozen have
had their mutual orbits and separate colors determined, frustrating their
use to investigate numerous important scientific questions. The current
shortage of data especially cripples scientific investigations requiring
statistical comparisons among the ensemble characteristics. We propose to
obtain sufficient astrometry and photometry of 23 TNBs to compute their
mutual orbits and system masses and to determine separate primary and
secondary colors, roughly tripling the sample for which this information is
known, as well as extending it to include systems of two near-equal size
bodies. To make the most efficient possible use of HST, we will use a Monte
Carlo technique to optimally schedule our observations.
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports of
potential non-nominal performance that will be investigated.)
HSTARS:
11285 - GSacq(1,2,1) failed to RGA control
During LOS the GSacq(1,2,1) scheduled at 122/01:10:43 failed to RGA control
due to search radius limit exceeded on FGS 1. OBAD1 has an RSS value of
1894.84. OBAD2 had and RSS value of 3.44.
At 122/02:54:23 REAcq (1,2,1) scheduled from 02:49:00 - 02:56:20 failed to
RGA control due to Search Radius Limit Exceeded on FGS 1. Pre-acquisition
OBADs had an RSS value of 639.94 and 3.90 arc-seconds respectively. At
02:59:15 received 486 ESB message "a07" C Timeout-Data Valid. Initial
indications show no S-curves in either X or Y axis.
11286 - GSAcq (1,2,1) failed due to Search Radius Limit Exceeded on FGS 1
At 122/04:36:05 GSAcq (1,2,1) scheduled from 04:30:50 - 04:38:09 had failed
due to search radius limit exceeded on FGS 1. At 04:33:18 mnemonic F1SSCEB
indicated Red High @ 10.16V, Upper Limit is set to 10. At 04:36:05 mnemonic
F1SSCEA indicated Red Low @ -10.24V, Lower Limit is set to -10.
Pre-acquisition OBADs RSS values were 1784.65 and 20.29 arc-seconds
respectively. At 04:41:03 received 486 ESB message "a07", FGS Coarse Track
failed - Timed out waiting for data valid. Initial analysis indicates this
acquisition used the same guide star pair as was used in HSTAR 11285. A
total of 9 attempts at course track were observed. FGS 1 PMT counts showed a
high of 9151.00293 @ 04:33:32 and a low of 573.00018 @ 04:33:56.
The REAcq (1,2,1) scheduled at 122/06:05:31 will occur during an LOS
followed by a T2 slew and a new GSAcq prior to AOS. The next scheduled
engineering data dump is 123/00:34:36.
COMPLETED OPS REQUEST: (None)
COMPLETED OPS NOTES: (None)
SCHEDULED SUCCESSFUL
FGS GSacq 09 07
FGS REacq 06 05
OBAD with Maneuver 30 30
SIGNIFICANT EVENTS: (None)