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============================================================================== TOPIC: Daily Report #5013
http://groups google com/group/sci astro hubble/t/ad8c8c90ee01f20b?hl=en
== 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
==============================================================================
TOPIC: Daily Report #5014 == 1 of 1 ==
Date: Tues, Jan 19 2010 9:40Â am
From: "Bassford, Lynn" HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science DAILY REPORT #5014 PERIOD COVERED: 5am January 15 - 5am January 19, 2010 (DOY 015/10:00z-
019/10:00z) OBSERVATIONS SCHEDULED 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 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 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)
COS/FUV 11895 FUV Detector Dark Monitor The purpose of this proposal is to monitor the FUV detector dark rate
by taking long science exposures without illuminating the detector
The detector dark rate and spatial distribution of counts will be
compared to pre-launch and SMOV data in order to verify the nominal
operation of the detector
Variations of count rate as a function of
orbital position will be analyzed to find dependence of dark rate on
proximity to the SAA
Dependence of dark rate as function of time will
also be tracked
COS/NUV 11894 NUV Detector Dark Monitor The purpose of this proposal is to measure the NUV detector dark rate
by taking long science exposures with no light on the detector
The
detector dark rate and spatial distribution of counts will be compared
to pre-launch and SMOV data in order to verify the nominal operation
of the detector
Variations of count rate as a function of orbital
position will be analyzed to find dependence of dark rate on proximity
to the SAA
Dependence of dark rate as function of time will also be
tracked
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
STIS/MA1/MA2 11857 STIS Cycle 17 MAMA Dark Monitor This proposal monitors the behavior of the dark current in each of the
MAMA detectors
The basic monitor takes two 1380s ACCUM darks each week with each
detector
However, starting Oct 5, pairs are only included for weeks
that the LRP has external MAMA observations planned
The weekly pairs
of exposures for each detector are linked so that they are taken at
opposite ends of the same SAA free interval
This pairing of exposures
will make it easier to separate long and short term temporal
variability from temperature dependent changes
For both detectors, additional blocks of exposures are taken once
every six months
These are groups of five 1314s FUV-MAMA Time-Tag
darks or five 3x315s NUV ACCUM darks distributed over a single
SAA-free interval
This will give more information on the brightness
of the FUV MAMA dark current as a function of the amount of time that
the HV has been on, and for the NUV MAMA will give a better measure of
the short term temperature dependence
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 11844 CCD Dark Monitor Part 1 The purpose of this proposal is to monitor the darks for the STIS CCD
WFC3/ACS/UVIS 11803 Observing Cluster Assembly Around the Massive Cluster RXJ0152-13 We request ACS imaging for groups and filaments in the outskirts of
two z=0
8 forming clusters of galaxies
These images will be combined
with an unparalleled dataset of wide- field spectroscopy from
Magellan, with ~2200 confirmed members (~3200 by the summer) of the
superstructures surrounding the two clusters
We will estimate merger
rates and determine the morphological composition of the galaxy
populations within the infalling groups and filaments identified in
our spectroscopic dataset
The HST data are critical to understand how
the early-type galaxy fraction remains constant in cluster centers,
while clusters double in mass through the steady accretion of lower
mass groups
One possibility is that the galaxies in the filaments and
infalling groups already have predominantly early-type morphologies,
while another is that galaxies transform during, and possibly even in
connection with, the process of infall
Our unique dataset of
spectroscopic membership, when combined with the exquisite
high-resolution imaging of ACS and WF3, will enable us to witness the
accretion of galaxies unto massive clusters and how this process
affects their properties
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
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/ACS/IR 11677 Is 47 Tuc Young? Measuring its White Dwarf Cooling Age and Completing
a Hubble Legacy With this proposal we will firmly establish the age of 47 Tuc from its
cooling white dwarfs
47 Tuc is the nearest and least reddened of the
metal-rich disk globular clusters
It is also the template used for
studying the giant branches of nearby resolved galaxies
In addition,
the age sensitive magnitude spread between the main sequence turnoff
and horizontal branch is identical for 47 Tuc, two bulge globular
clusters and the bulge field population
A precise relative age
constraint for 47 Tuc, compared to the halo clusters M4 and NGC 6397,
both of which we recently dated via white dwarf cooling, would
therefore constrain when the bulge formed relative to the old halo
globular clusters
Of particular interest is that with the higher
quality ACS data on NGC 6397, we are now capable with the technique of
white dwarf cooling of determining ages to an accuracy of +/-0
4 Gyrs
at the 95% confidence level
Ages derived from the cluster turnoff are
not currently capable of reaching this precision
The important role
that 47 Tuc plays in galaxy formation studies, and as the metal-rich
template for the globular clusters, makes the case for a white dwarf
cooling age for this metal-rich cluster compelling
Several recent analyses have suggested that 47 Tuc is more than 2 Gyrs
younger than the Galactic halo
Others have suggested an age similar
to that of the most metal poor globular clusters
The current
situation is clearly uncertain and obviously a new approach to age
dating this important cluster is required
With the observations of 47 Tuc, this project will complete a legacy
for HST
It will be the third globular cluster observed for white
dwarf cooling; the three covering almost the full metallicity range of
the cluster system
Unless JWST has its proposed bluer filters (700
and 900 nm) this science will not be possible perhaps for decades
until a large optical telescope is again in space
Ages for globular
clusters from the main sequence turnoff are less precise than those
from white dwarf cooling making the science with the current proposal
truly urgent
COS/NUV/FUV 11659 Probing the Interior of SN1006 The remnant of SN 1006 is unique among all supernova remnants in
having 3 identified background UV sources that can be used to probe
cold, otherwise unseen ejecta within the remnant shell
We propose
high-resolution spectra from COS to obtain spectra of all three of
these
The brightest of these, the Schweizer-Middleditch star (the
only one with extensive previous high-quality UV spectra) shows Si II
absorption with an extremely unusual asymmetric profile with a sharp
edge on the red end, indicating the velocity of material just entering
the reverse shock
Our new spectrum can be compared with STIS
observations from 1999 to measure definitively the velocity change as
the reverse shock eats its way into ever-more-slowly-expanding ejecta
One may well ask, however, if this profile is truly representative,
and we seek to answer that with a spectrum of a background quasar at a
similar distance of the SM star from the projected center, but in a
different direction
And by investigating the detailed structure of
these two sources and a second quasar, we can probe small-scale
structure in the ejecta
No object other than SN1006 offers a similar
opportunity to probe the distribution of ejecta within the remnant of
a Type Ia supernova
WFC3/UVIS/IR 11644 A Dynamical-Compositional Survey of the Kuiper Belt: A New Window Into
the Formation of the Outer Solar System The eight planets overwhelmingly dominate the solar system by mass,
but their small numbers, coupled with their stochastic pasts, make it
impossible to construct a unique formation history from the dynamical
or compositional characteristics of them alone
In contrast, the huge
numbers of small bodies scattered throughout and even beyond the
planets, while insignificant by mass, provide an almost unlimited
number of probes of the statistical conditions, history, and
interactions in the solar system
To date, attempts to understand the
formation and evolution of the Kuiper Belt have largely been dynamical
simulations where a hypothesized starting condition is evolved under
the gravitational influence of the early giant planets and an attempt
is made to reproduce the current observed populations
With little
compositional information known for the real Kuiper Belt, the test
particles in the simulation are free to have any formation location
and history as long as they end at the correct point
Allowing
compositional information to guide and constrain the formation,
thermal, and collisional histories of these objects would add an
entire new dimension to our understanding of the evolution of the
outer solar system
While ground based compositional studies have hit
their flux limits already with only a few objects sampled, we propose
to exploit the new capabilities of WFC3 to perform the first ever
large-scale dynamical-compositional study of Kuiper Belt Objects
(KBOs) and their progeny to study the chemical, dynamical, and
collisional history of the region of the giant planets
The
sensitivity of the WFC3 observations will allow us to go up to two
magnitudes deeper than our ground based studies, allowing us the
capability of optimally selecting a target list for a large survey
rather than simply taking the few objects that can be measured, as we
have had to do to date
We have carefully constructed a sample of 120
objects which provides both overall breadth, for a general
understanding of these objects, plus a large enough number of objects
in the individual dynamical subclass to allow detailed comparison
between and within these groups
These objects will likely define the
core Kuiper Belt compositional sample for years to come
While we have
many specific results anticipated to come from this survey, as with
any project where the field is rich, our current knowledge level is
low, and a new instrument suddenly appears which can exploit vastly
larger segments of the population, the potential for discovery -- both
anticipated and not -- is extraordinary
WFC3/ACS/UVIS 11613 GHOSTS: Stellar Outskirts of Massive Spiral Galaxies We propose to continue our highly successful GHOSTS HST survey of the
resolved stellar populations of nearby, massive disk galaxies using
SNAPs
These observations provide star counts and color-magnitude
diagrams 2-3 magnitudes below the tip of the Red Giant Branch of the
outer disk and halo of each galaxy
We will measure the metallicity
distribution functions and stellar density profiles from star counts
down to very low average surface brightnesses, equivalent to ~32 V-mag
per square arcsec
This proposal will substantially improve our unique sampling of galaxy
outskirts
Our targets cover a range in galaxy mass, luminosity,
inclination, and morphology
As a function of these galaxy properties,
this survey provides: - the most extensive, systematic measurement of
radial light profiles and axial ratios of the diffuse stellar halos
and outer disks of spiral galaxies; - a comprehensive analysis of halo
metallicity distributions as function of galaxy type and position
within the galaxy; - an unprecedented study of the stellar metallicity
and age distribution in the outer disk regions where the disk
truncations occur; - the first comparative study of globular clusters
and their field stellar populations
We will use these fossil records of the galaxy assembly process to
test halo formation models within the hierarchical galaxy formation
scheme
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 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/ACS/UVIS/IR 11570 Narrowing in on the Hubble Constant and Dark Energy A measurement of the Hubble constant to a precision of a few percent
would be a powerful aid to the investigation of the nature of dark
energy and a potent "end-to end" test of the present cosmological
model
In Cycle 15 we constructed a new streamlined distance ladder
utilizing high- quality type Ia supernova data and observations of
Cepheids with HST in the near-IR to minimize the dominant sources of
systematic uncertainty in past measurements of the Hubble constant and
reduce its total uncertainty to a little under 5%
Here we propose to
exploit this new route to reduce the remaining uncertainty by more
than 30%, translating into an equal reduction in the uncertainty of
the equation of state of dark energy
We propose three sets of
observations to reach this goal: a mosaic of NGC 4258 with WFC3 in
F160W to triple its sample of long period Cepheids, WFC3/F160W
observations of the 6 ideal SN Ia hosts to triple their samples of
Cepheids, and observations of NGC 5584 the host of a new SN Ia, SN
2007af, to discover and measure its Cepheids and begin expanding the
small set of SN Ia luminosity calibrations
These observations would
provide the bulk of a coordinated program aimed at making the
measurement of the Hubble constant one of the leading constraints on
dark energy
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
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
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/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 NIC2/STIS/CCD 10897 Coronagraphic Imaging of the Submillimeter Debris Disk of a 200Myr-Old
M-Dwarf A recent sub-millimeter survey has unambiguously discovered a new
debris disk around the M0
5 dwarf GJ842
2 which is 200 Myr old
Reanalysis of the IRAS data has shown that there is also a 25 micron
excess toward this star indicating warm dust close to the star
It is
also only the second debris disk found among M-dwarfs that constitute
70 % of the stars in the Galaxy
Collisional and Poynting-Roberston
timescale arguments indicate that the cold grains detected in the
sub-mm are "primordial'', i
e
original grains from the protoplanetary
phase
The disk around GJ842
2 is thus unique in terms of the presence
of dust at such a late stage of evolution and presents two conundrums:
why did it retain so much primordial dust at large distances, and why
does it continue to produce dust close to the star? We propose to
conduct high contrast NICMOS coronagraphic imaging of GJ842
2 to
determine the spatial distribution of the small reflecting grains and
test the various scenarios which might explain the IRAS and sub-mm
data e
g
resonant trapping of dust by planets or ``sandblasting'' by
interstellar medium grains working more aggressively on a low-
luminosity star than on an A-type star like Beta Pic
Also, we would
search for an evolutionary sequence between GJ842
2 and the only other
M-dwarf with a disk resolved by HST, the 10 Myr old AU Mic system
FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated
) HSTARS: 12168 - GSAcq (2,1,1) at 17/12:08:22z, REAcq (2,1,1) at 17/13:31:04z
and and REAcq (2,1,1) at 17/15:03:21z all failed due to Search Radius
Limit on FGS2
Observations affected ACS 83 - 86, WFC3 196 - 201, WF3 202 - 204;
Proposal ID# 11570, 11879 and 11905 12169 - GSAcq (2,1,1) results in fine lock backup (2,0,2) using FGS-2
@ 018/12:56:28z
Observations possibly affected: WFC3 18-21, STIS 15, ACS 21; Proposal
ID# 11548, 11857, 11879 COMPLETED OPS REQUEST: 18799-0 - Real Time OBAD @ 017/1319z COMPLETED OPS NOTES: (None) FGS GSAcq 25 24
FGS REAcq 34 32
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