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- Daily Report #5012 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/3df9a0db04202e38?hl=en
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============================================================================== TOPIC: Daily Report #5012
http://groups google com/group/sci astro hubble/t/3df9a0db04202e38?hl=en
== 1 of 1 == Date: Thurs, Jan 14 2010 6:27Â am From: "Bassford, Lynn"
HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY REPORT #5012
PERIOD COVERED: 5am January 13 - 5am January 14, 2010 (DOY 013/10:00z-014/10:00z)
OBSERVATIONS SCHEDULED
ACS/WFC3 11879
CCD Daily Monitor (Part 1)
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 352 orbits (22 weeks) from 31 August 2009 to 31 January 2010
NIC2/WFC3/IR 11548
Infrared Imaging of Protostars in the Orion A Cloud: The Role of Environment in Star Formation
We propose NICMOS and WFC3/IR observations of a sample of 252 protostars identified in the Orion A cloud with the Spitzer Space Telescope These observations will image the scattered light escaping the protostellar envelopes, providing information on the shapes of outflow cavities, the inclinations of the protostars, and the overall morphologies of the envelopes In addition, we ask for Spitzer time to obtain 55-95 micron spectra of 75 of the protostars Combining these new data with existing 3 6 to 70 micron photometry and forthcoming 5-40 micron spectra measured with the Spitzer Space Telescope, we will determine the physical properties of the protostars such as envelope density, luminosity, infall rate, and outflow cavity opening angle By examining how these properties vary with stellar density (i e clusters vs groups vs isolation) and the properties of the surrounding molecular cloud; we can directly measure how the surrounding environment influences protostellar evolution, and consequently, the formation of stars and planetary systems Ultimately, this data will guide the development of a theory of protostellar evolution
STIS/CCD 11844
CCD Dark Monitor Part 1
The purpose of this proposal is to monitor the darks for the STIS CCD
STIS/CCD 11846
CCD Bias Monitor-Part 1
The purpose of this proposal is to 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/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/ACS/IR 11142
Revealing the Physical Nature of Infrared Luminous Galaxies at
0
3 We aim to determine physical properties of IR luminous galaxies at
0
3 WFC3/ACS/IR 11235 HST NICMOS Survey of the Nuclear Regions of Luminous Infrared Galaxies
in the Local Universe At luminosities above 10^11
4 L_sun, the space
density of far-infrared selected galaxies exceeds that of optically
selected galaxies
These `luminous infrared galaxies' (LIRGs) are
primarily interacting or merging disk galaxies undergoing enhanced
star formation and Active Galactic Nuclei (AGN) activity, possibly
triggered as the objects transform into massive S0 and elliptical
merger remnants
We propose NICMOS NIC2 imaging of the nuclear regions
of a complete sample of 88 L_IR > 10^11
4 L_sun luminous infrared
galaxies in the IRAS Revised Bright Galaxy Sample (RBGS: i
e
, 60
micron flux density > 5
24 Jy)
This sample is ideal not only in its
completeness and sample size, but also in the proximity and brightness
of the galaxies
The superb sensitivity and resolution of NICMOS NIC2
on HST enables a unique opportunity to study the detailed structure of
the nuclear regions, where dust obscuration may mask star clusters,
AGN, and additional nuclei from optical view, with a resolution
significantly higher than possible with Spitzer IRAC
This survey thus
provides a crucial component to our study of the dynamics and
evolution of IR galaxies presently underway with Wide-Field, HST
ACS/WFC3, and Spitzer IRAC observations of these 88 galaxies
Imaging
will be done with the F160W filter (H-band) to examine as a function
of both luminosity and merger stage: (i) the luminosity and
distribution of embedded star clusters, (ii) the presence of optically
obscured AGN and nuclei, (iii) the correlation between the
distribution of 1
6 micron emission and the mid-IR emission as
detected by Spitzer IRAC, (iv) the evidence of bars or bridges that
may funnel fuel into the nuclear region, and (v) the ages of star
clusters for which photometry is available via ACS/WFC3 observations
The NICMOS data, combined with the HST ACS, Spitzer, and GALEX
observations of this sample, will result in the most comprehensive
study of merging and interacting galaxies to date
WFC3/ACS/UVIS 11603 A Comprehensive Study of Dust Formation in Type II Supernovae with
HST, Spitzer, and Gemini The recent discovery of three extremely bright Type II SNe, (2007it,
2007oc, 2007od) gives us a unique opportunity to combine observations
with HST, Spitzer, and Gemini to study the little understood dust
formation process in Type II Sne
Priority 1 Spitzer Cycle 5 and band
1 Gemini 2008A time has already been approved for this project
Since
late-time Type II Sne are faint and tend to be in crowded fields, we
need the high sensitivity and high spatial resolution of ACS and
NICMOS/NIC2 for these observations
This project is motivated by the
recent detection of large amounts of dust in high redshift galaxies
The dust in these high-z galaxies must come from young, massive stars
so Type II Sne could be potential sources
The mechanism and the
efficiency of dust condensation in Type II SN ejecta are not well
understood, largely due to the lack of observational data
We plan to
produce a unique dataset, combining spectroscopy and imaging in the
visible, near- and mid-IR covering the key phase, 400-700 days after
maximum when dust is known to form in the SN ejecta
Therefore, we are
proposing for coordinated HST/NOAO observations (HST ACS, NICMOS/NIC2
& Gemini/GMOS and TReCS) which will be combined with our Spitzer Cycle
5 data to study these new bright Sne
The results of this program will
place strong constraints on the formation of dust seen in young high
redshift (z>5) galaxies
WFC3/IR 11591 Are Low-Luminosity Galaxies Responsible for Cosmic Reionization? Our group has demonstrated that massive clusters, acting as powerful
cosmic lenses, can constrain the abundance and properties of
low-luminosity star-forming sources beyond z~6; such sources are
thought to be responsible for ending cosmic reionization
The large
magnification possible in the critical regions of well-constrained
clusters brings sources into view that lie at or beyond the limits of
conventional exposures such as the UDF
We have shown that the
combination of HST and Spitzer is particularly effective in delivering
the physical properties of these distant sources, constraining their
mass, age and past star formation history
Indirectly, we therefore
gain a valuable glimpse to yet earlier epochs
Recognizing the result
(and limitations) of blank field surveys, we propose a systematic
search through 10 lensing clusters with ACS/F814W and
WFC3/[F110W+F160W] (in conjunction with existing deep IRAC data)
Our
goal is to measure with great accuracy the luminosity function at z~7
over a range of at least 3 magnitude, based on the identification of
about 50 lensed galaxies at 6
5 WFC3/IR 11838 Completing a Flux-limited Survey for X-ray Emission from Radio Jets We will measure the changing flow speeds, magnetic fields, and energy
fluxes in well- resolved quasar jets found in our short-exposure
Chandra survey by combining new, deep Chandra data with radio and
optical imaging
We will image each jet with sufficient sensitivity to
estimate beaming factors and magnetic fields in several distinct
regions, and so map the variations in these parameters down the jets
HST observations will help diagnose the role of synchrotron emission
in the overall SED, and may reveal condensations on scales less than
0
1 arcsec
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/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 11911 UVIS L-Flats and Geometric Distortion Multiple pointing observations of the globular cluster Omega Centauri
(NGC 5139) will be used to measure the filter-dependent low frequency
flat field (L-flat) corrections and stability for a key set of 10
broadband filters used by GO programs
The selected filters are F225W,
F275W, F336W, F390W, F438W, F555W, F606W, F775W, F814W and F850LP
By
measuring relative changes in brightness of a star over different
portions of the detector, we will determine local variations in the
UVIS detector response
The broad wavelength range covered by these observations will allow us
to derive the L- flat correction for the remaining wide, medium and
narrow-band UVIS filters
The same data will also be used to determine
and correct the geometric distortion that affects UVIS data
The broad
wavelength range covered by these observations will allow us to
measure the geometric distortion dependence with wavelength and
filters and to provide the most appropriate correction over the entire
wavelength range provided by UVIS
FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated
) HSTARS: FGS 2 Observations possibly affected: WFC3 #79 Proposal #11905, WFC3 #80-81
Proposal #11929 and ACS #19 Proposal #11603 COMPLETED OPS REQUEST: (None) COMPLETED OPS NOTES: (None) FGS GSAcq 8 8
FGS REAcq 7 7
OBAD with Maneuver 8 8 SIGNIFICANT EVENTS: (None) ==============================================================================
TOPIC: Daily Report #5013 == 1 of 1 ==
Date: Fri, Jan 15 2010 6:54Â am
From: "Bassford, Lynn" HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science DAILY REPORT #5013 PERIOD COVERED: 5am January 14 - 5am January 15, 2010 (DOY 014/10:00z-015/10:00z) OBSERVATIONS SCHEDULED COS/NUV/FUV 11531 COS-GTO: Brown Dwarf Activity COS will obtain ultraviolet spectra of a representative sample of
brown dwarfs to study such questions as: (1) Is the hot gas in the
outer atmospheres of young brown dwarfs heated by accretion? (2) Is
the molecular hydrogen emission due to Lyman-alpha fluorescence or
collisional excitation? (3) Are the older brown dwarfs without disks
low mass analogs of active M dwarfs with flares and transient heating?
(4) Are young brown dwarfs with disks low mass analogs of classical T
Tauri stars? STIS/CCD 11844 CCD Dark Monitor Part 1 The purpose of this proposal is to monitor the darks for the STIS CCD
STIS/CCD 11846 CCD Bias Monitor-Part 1 The purpose of this proposal is to 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
WFC3/ACS/IR 11142 Revealing the Physical Nature of Infrared Luminous Galaxies at
0
3 We aim to determine physical properties of IR luminous galaxies at
0
3 WFC3/ACS/UVIS 11724 Direct Age Determination of the Local Group dE Galaxies NGC 147 and
NGC 185 The origin of dwarf elliptical (dE) galaxies remains a mystery and the
dE galaxies of the Local Group provide the best opportunity to study
this galaxy class in detail
v We propose to obtain ACS photometry of
main sequence turnoff stars in the M31 dE satellites NGC 147 and NGC
185
Because these galaxies have little to no stars younger than 1
Gyr, resolving the main sequence turnoff is required to directly
quantify their star formation histories
NGC 147 and NGC 185 are the
only two dEs for which a clean measurement is feasible with the HST
This proposal was accepted in Cycle 15, but little data were taken
before the failure of ACS
The main sequence turnoffs of NGC 147 and
NGC 185 are expected to be at an apparent magnitude of V=29; we
request F606W/F814W imaging one half magnitude fainter than this limit
(three magnitudes fainter than the deepest previous dE observations)
Quantifying the ratio of old to intermediate-age stars will allow us
to discriminate between competing models of dE formation
On-going
Keck/DEIMOS spectroscopy of several hundred red giant stars in each of
these two dE galaxies, coupled with dynamical modeling and spectral
synthesis, will complement the ACS measurement by providing
information on chemical abundance patterns, dark matter content and
internal dynamics
The proposed ACS data will be the first to directly
quantify the onset and duration of star formation episodes in dE
galaxies, and will thereby form the cornerstone in what promises to be
the most comprehensive study of this class of galaxies
WFC3/UVIS 11583 The Star Formation Rate In Nearby Elliptical Galaxies Small amounts of star formation in normal elliptical galaxies are
suggested by several results: some surprisingly young ages from
optical line-index dating; cooling X-ray gas; and mid-IR dust
emission
Previously, it was difficult to detect low levels of star
formation, but UV imaging with WFPC3 will permit us to conclusively
identify individual O/B stars in nearby normal ellipticals by their UV
colors and magnitudes
This technique is orders of magnitude more
sensitive than previous methods, allowing detections of star formation
to levels of 1E-4 Msolar/yr
Proof of concept is provided by a very
long UV ACS observation of M87 that revealed many O/B stars
We
propose observations of four normal ellipticals where recent star
formation is likely
This will yield their star formation rates and
the locations of such activity
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
WFC3/UVIS 11911 UVIS L-Flats and Geometric Distortion Multiple pointing observations of the globular cluster Omega Centauri
(NGC 5139) will be used to measure the filter-dependent low frequency
flat field (L-flat) corrections and stability for a key set of 10
broadband filters used by GO programs
The selected filters are F225W,
F275W, F336W, F390W, F438W, F555W, F606W, F775W, F814W and F850LP
By
measuring relative changes in brightness of a star over different
portions of the detector, we will determine local variations in the
UVIS detector response
The broad wavelength range covered by these observations will allow us
to derive the L- flat correction for the remaining wide, medium and
narrow-band UVIS filters
The same data will also be used to determine
and correct the geometric distortion that affects UVIS data
The broad
wavelength range covered by these observations will allow us to
measure the geometric distortion dependence with wavelength and
filters and to provide the most appropriate correction over the entire
wavelength range provided by UVIS
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: COMPLETED OPS NOTES: (None) FGS GSAcq 3 3
FGS REAcq 12 12
OBAD with Maneuver 3 3 SIGNIFICANT EVENTS: Flash Report: Lunar solar eclipse 2010/015 OPS Request #18793 was successfully executed to configure the FSW
processing of CSS data and temporarily disable Rate of Charge (ROC)
safemode test during a series of moon shadows that occurred on GMT day
015 between 04:19z and 08:18z
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