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- Daily Report #5188 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/c7f3738027a79d90?hl=en
- Daily Report #5189 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/a8828a355223a17e?hl=en
- Daily Report #5190 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/752c306d34bcb98e?hl=en
- Daily Report #5191 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/de2241866d1407cf?hl=en
- HST Daily Reports - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/0a078cffe440ca03?hl=en
============================================================================== TOPIC: Daily Report #5188
http://groups google com/group/sci astro hubble/t/c7f3738027a79d90?hl=en
== 1 of 1 == Date: Fri, Sep 24 2010 8:17 am From: "Cooper, Joe"
HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY REPORT #5188
PERIOD COVERED: 5am September 23 - 5am September 24, 2010 (DOY 266/09:00z-267/09:00z)
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: 18924-0 - Genslew for proposal 12312 (slot #1) @ 267/0620z 18925-0 - Genslew for proposal 12312 (slot #2) @ 267/0622z 18926-0 - Genslew for proposal 12312 (slot #3) @ 267/0625z 18927-1 - Genslew for proposal 12312 (slot #4) @ 267/0627z 18928-0 - Genslew for proposal 12312 (slot #5) @ 267/0630z
COMPLETED OPS NOTES: (None)
SCHEDULED SUCCESSFUL
FGS GSAcq 6 6 FGS REAcq 6 6 OBAD with Maneuver 8 8
SIGNIFICANT EVENTS: (None)
OBSERVATIONS SCHEDULED:
ACS/WFC3 11734
The Hosts of High Redshift Gamma-Ray Bursts
Gamma-ray bursts are the most luminous explosive events known, acting as beacons to the high redshift universe Long duration GRBs have their origin in the collapse of massive stars and thus select star forming galaxies across a wide range of redshift Due to their bright afterglows we can study the details of GRB host galaxies via absorption spectroscopy, providing redshifts, column densities and metallicities for galaxies far too faint to be accessible directly with current technology We have already obtained deep ground based observations for many hosts and here propose ACS/WFC3 and WFC3 observations of the fields of bursts at z>3 which are undetected in deep ground based images These observations will study the hosts in emission, providing luminosities and morphologies and will enable the construction of a sample of high-z galaxies with more detailed physical properties than has ever been possible before
STIS/CCD 11845
CCD Dark Monitor Part 2
Monitor the darks for the STIS CCD
STIS/CCD 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
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 12215
Searching for the Missing Low-Mass Companions of Massive Stars
Recent results on binary companions of massive O stars appear to indicate that the distribution of secondary masses is truncated at low masses It thus mimics the distribution of companions of G dwarfs and also the Initial Mass Function (IMF), except that it is shifted upward by a factor of 20 in mass These results, if correct, provide a distribution of mass ratios that hints at a strong constraint on the star-formation process However, this intriguing result is derived from a complex simulation of data which suffer from observational incompleteness at the low-mass end
We propose a snapshot survey to test this result in a very direct way HST WFC3 images of a sample of the nearest Cepheids (which were formerly B stars of ~5 Msun) will search for low-mass companions down to M dwarfs We will confirm any companions as young stars, and thus true physical companions, through follow-up Chandra X-ray images Our survey will show clearly whether the companion mass distribution is truncated at low masses, but at a mass much higher than that of the IMF or G dwarfs
WFC3/UV/ACS/WFC 12311
Multiple Stellar Populations in Galactic Globular Clusters
This is a proposal to bring the unique new properties of WFC3 to bear on the most exciting recent development in stellar populations: multiple generations of stars in globular clusters From our vantage point in the midst of these developments, we feel that the present-day situation merits a concentration on increasing the depth of knowledge in clusters that are already known to have multiple populations, rather than merely increasing the list of clusters with perplexing peculiarities We are therefore proposing to look for a clear splitting of the main sequence (and other sequences) of 47 Tuc, M4, M22, NGC 1851, and NGC 6752, and quantify them The main-sequence study will cast particular light on the question of helium enrichment Coupling the requested F275W data with F814W images available from the archive will allow us to follow the multiple sequences in the color magnitude diagram from the main sequence to the horizontal branch and asymptotic giant branch, and therefore constrain the effects of enhanced He and CNO on their evolution
WFC3/UV/IR 12256
The Ultraviolet and Optical Counterparts of the Intermediate Mass Black Hole Candidate ESO 243-49 HLX-1
We request imaging observations of the record breaking hyper-luminous X-ray source and intermediate mass black hole candidate HLX-1 in the galaxy ESO 243-49, in order to investigate the nature of recent detections of UV emission and an optical counterpart HLX-1 is currently the best candidate for an intermediate mass black hole, the possible building blocks of super-massive black holes found in the centres of galaxies UV emission possibly associated with the X-ray source position was recently detected in lower resolution observations with the Swift and GALEX satellites If this emission can be tied to HLX-1 and is point-like in nature, it will likely be dominated by emission from a hot accretion disc By obtaining UV photometry we will be able to place constraints upon the temperature of the disc and therefore the mass of the black hole The optical counterpart may be related to disc emission, though it is also possible that it is associated with a globular cluster or nucleated dwarf galaxy By obtaining photometry of the counterpart in near-infrared to UV wavelengths we will be able to construct a broad-band SED, which will allow us to place firm constraints on the environment around this intriguing object
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 11914
UVIS Earth Flats
This program is an experimental path finder for Cycle 18 calibration Visible-wavelength flat fields will be obtained by observing the dark side of the Earth during periods of full moon illumination The observations will consist of full-frame streaked WFC3 UVIS imagery: per 22- min total exposure time in a single "dark-sky" orbit, we anticipate collecting 7000 e/pix in F606W or 4500 e/pix in F814W To achieve Poisson S/N > 100 per pixel, we require at least 2 orbits of F606W and 3 orbits of F814W
For UVIS narrowband filters, exposures of 1 sec typically do not saturate on the sunlit Earth, so we will take sunlit Earth flats for three of the more-commonly used narrowband filters in Cycle 17 plus the also-popular long-wavelength quad filters, for which we get four filters at once
Why not use the Sunlit Earth for the wideband visible-light filters? It is too bright in the visible for WFC3 UVIS minimum exposure time of 0 5 sec Similarly, for NICMOS the sunlit-Earth is too bright which saturates the detector too quickly and/or induces abnormal behaviors such as super-shading (Gilmore 1998, NIC 098-011) In the narrowband visible and broadband near- UV its not too bright (predictions in Cox et al 1987 "Standard Astronomical Sources for HST: 6 Spatially Flat Fields " and observations in ACS Program 10050)
Other possibilities? Cox et al 's Section II D addresses many other possible sources for flat fields, rejecting them for a variety of reasons A remaining possibility would be the totally eclipsed moon Such eclipses provide approximately 2 hours (1 HST orbit) of opportunity per year, so they are too rare to be generically useful An advantage of the moon over the Earth is that the moon subtends less than 0 25 square degree, whereas the Earth subtends a steradian or more, so scattered light and light potentially leaking around the shutter presents additional problems for the Earth Also, we're unsure if HST can point 180 deg from the Sun
WFC3/UVIS/IR 11702
Search for Very High-z Galaxies with WFC3 Pure Parallel
WFC3 will provide an unprecedented probe to the early universe beyond
the current redshift frontier
Here we propose a pure parallel program
using this new instrument to search for Lyman-break galaxies at
6
5
(1) We will use both the UVIS and the IR channels, and do not need to seek optical data from elsewhere
(2) Our program will likely triple the size of the probable candidate samples at z~7 and z~8, and will complement other targeted programs aiming at the similar redshift range
(3) Being a pure parallel program, our survey will only make very limited demand on the scarce HST resources More importantly, as the pure parallel pointings will be at random sight-lines, our program will be least affected by the bias due to the large scale structure ("cosmic variance")
(4) We aim at the most luminous LBG population, and will address the bright-end of the luminosity function at z~8 and z~7 We will constrain the value of L* in particular, which is critical for understanding the star formation process and the stellar mass assembly history in the first few hundred million years of the universe
(5) The candidates from our survey, most of which will be the brightest ones that any surveys would be able to find, will have the best chance to be spectroscopically confirmed at the current 8--10m telescopes
(6) We will also find a large number of extremely red, old galaxies at intermediate redshifts, and the fine spatial resolution offered by the WFC3 will enable us constrain their formation history based on the study of their morphology, and hence shed light on their connection to the very early galaxies in the universe
============================================================================== TOPIC: Daily Report #5189
http://groups google com/group/sci astro hubble/t/a8828a355223a17e?hl=en
== 1 of 1 == Date: Mon, Sep 27 2010 9:04 am From: "Cooper, Joe"
HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY REPORT #5189
PERIOD COVERED: 5am September 24 - 5am September 27, 2010 (DOY 267/09:00z-270/09:00z)
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: (None)
COMPLETED OPS NOTES: (None)
SCHEDULED SUCCESSFUL
FGS GSAcq 24 24 FGS REAcq 23 23 OBAD with Maneuver 22 22
SIGNIFICANT EVENTS: (None)
OBSERVATIONS SCHEDULED:
COS/NUV/FUV/STIS/CCD 12312
Hubble Investigation of 103P/Hartley 2 in Support of NASA's DIXI Mission
Comet 103P/Hartley 2 is a small but highly active comet that will pass unusually close to the Earth (0 12 AU) during the fall of 2010, when it will also be visited by NASA's DIXI spacecraft We propose a 15-orbit spectroscopic observing campaign with Hubble, comprised of three 5-orbit visits spanning a 2-month period, to measure the abundances of several key volatiles (CO, CO2, S2) and their possible seasonal variations CO has not yet been detected in 103P, and Hubble may be the only facility capable of doing it Hubble is also uniquely capable of providing confirmation of DIXI's measurements of the CO2 abundance The DIXI flyby is an exceptional opportunity to study the nature of comets, and Hubble will contribute important and unique data to the international campaign supporting this mission
ACS/WFC 12292
SWELLS: Doubling the Number of Disk-dominated Edge-on Spiral Lens Galaxies
The formation of realistic disk galaxies within the LCDM cosmology is still largely an unsolved problem Theory is now beginning to make predictions for how dark matter halos respond to galaxy formation, and for the properties of disk galaxies Measuring the density profiles of dark matter halos on galaxy scales is therefore a strong test for the standard paradigm of galaxy formation, offering great potential for discovery However, the degeneracy between the stellar and dark matter contributions to galaxy rotation curves remains a major obstacle Strong gravitational lensing, when combined with spatially resolved kinematics and stellar population models, can solve this long-standing problem Unfortunately, this joint methodology could not be exploited until recently due to the paucity of known edge-on spiral lenses We have developed and demonstrated an efficient technique to find exactly these systems During supplemental cycle-16 we discovered five new spiral lens galaxies, suitable for rotation curve measurements We propose multi-color HST imaging of 16 candidates and 2 partially-imaged confirmed systems, to measure a sample of eight new edge-on spiral lenses This program will at least double the number of known disk-dominated systems This is crucial for constraining the relative contribution of the disk, bulge and dark halo to the total density profile
WFC3/IR 12217
Spectroscopy of Faint T Dwarf Calibrators: Understanding the Substellar Mass Function and the Coolest Brown Dwarfs
More than 100 methane brown dwarfs, or T dwarfs, have now been discovered in the local field with 2MASS, SLOAN and UKIDSS, opening up a new area of physics describing objects at 450-1400 K However, very few calibrator objects exist with well established ages and metallicities A very surprising result from the UKIDSS sample (supported by 2MASS and SLOAN) is that the substellar mass function in the local field appears to decline to lower masses, in marked contrast to the rising initial mass function (IMF) observed in young clusters Given that such a difference between the present day IMF and the Galactic time-averaged IMF is unlikely, it is very possible that the apparently falling IMF is an artifact of serious errors in either T model atmospheres or the evolutionary isochrones We propose WFC3 spectroscopy of 4 faint T dwarf calibrators with well established ages and metallicities in the Pleiades and Sigma Ori clusters, and 2 faint field T dwarfs from UKIDSS for comparison These spectra will constitute vital calibration data for T dwarf atmospheres with a wide range of surface gravities, which will be used to test and improve the model atmospheres They will also aid preparation for future spectroscopy of the much larger numbers of field T dwarfs to soon be found by VISTA and WISE These new surveys will permit a more precise measurement of the mass function and detection of even cooler objects
COS/NUV 12042
COS-GTO: Pluto
We seek to measure Pluto's albedo below 2100, to better constrain surface composition COS observations will provide a substantial improvement in the S/N of Pluto spectra from <1800 to 2100 Accumulation of past HST/FOS spectra yields extremely low S/N below 2000 (S/N of only 1-3 in 100 bins; Krasnopolsky 2001) We expect to achieve S/N=5 at 1950 with 10 binning In addition to spectrally broad albedo measurements, these observations could reveal line or molecular band emission, such as C I 1931 or CO 1993
WFC3/UVIS 12018
Ultra-Luminous X-Ray Sources in the Most Metal-Poor Galaxies
There is growing observational and theoretical evidence to suggest that Ultra-Luminous X-ray sources (ULX) form preferentially in low metallicity environments Here we propose a survey of 27 nearby (< 30Mpc) star-forming Extremely Metal Poor Galaxies (Z<5% solar) There are almost no X-ray observations of such low abundance galaxies (3 in the Chandra archive) These are the most metal-deficient galaxies known, and a logical place to find ULX if they favor metal-poor systems We plan to test recent population synthesis models which predict that ULX should be very numerous in metal-poor galaxies We will also test the hypothesis that ULX form in massive young star clusters, and ask for HST time to obtain the necessary imaging data
ACS/WFC 11996
CCD Daily Monitor (Part 3)
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 308 orbits (19 25 weeks) from 21 June 2010 to 1 November 2010
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 11914
UVIS Earth Flats
This program is an experimental path finder for Cycle 18 calibration Visible-wavelength flat fields will be obtained by observing the dark side of the Earth during periods of full moon illumination The observations will consist of full-frame streaked WFC3 UVIS imagery: per 22- min total exposure time in a single "dark-sky" orbit, we anticipate collecting 7000 e/pix in F606W or 4500 e/pix in F814W To achieve Poisson S/N > 100 per pixel, we require at least 2 orbits of F606W and 3 orbits of F814W
For UVIS narrowband filters, exposures of 1 sec typically do not saturate on the sunlit Earth, so we will take sunlit Earth flats for three of the more-commonly used narrowband filters in Cycle 17 plus the also-popular long-wavelength quad filters, for which we get four filters at once
Why not use the Sunlit Earth for the wideband visible-light filters? It is too bright in the visible for WFC3 UVIS minimum exposure time of 0 5 sec Similarly, for NICMOS the sunlit-Earth is too bright which saturates the detector too quickly and/or induces abnormal behaviors such as super-shading (Gilmore 1998, NIC 098-011) In the narrowband visible and broadband near- UV its not too bright (predictions in Cox et al 1987 "Standard Astronomical Sources for HST: 6 Spatially Flat Fields " and observations in ACS Program 10050)
Other possibilities? Cox et al 's Section II D addresses many other possible sources for flat fields, rejecting them for a variety of reasons A remaining possibility would be the totally eclipsed moon Such eclipses provide approximately 2 hours (1 HST orbit) of opportunity per year, so they are too rare to be generically useful An advantage of the moon over the Earth is that the moon subtends less than 0 25 square degree, whereas the Earth subtends a steradian or more, so scattered light and light potentially leaking around the shutter presents additional problems for the Earth Also, we're unsure if HST can point 180 deg from the Sun
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)
STIS/CCD 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 11845
CCD Dark Monitor Part 2
Monitor the darks for the STIS CCD
FGS 11787
Dynamical Masses and Radii of Four White Dwarf Stars
This proposal uses the FGS1R in Trans mode to resolve a pair of double degenerate binary systems (WD1639+153 and WD 1818+26) in order to determine their orbital elements In addition, the binaries and several nearby field stars are observed by FGS1R in Pos mode to establish the local inertial reference frame of each binary, as well as its parallax and proper motion This will allow for a direct measurement of the distance, which yields the intrinsic luminosity, and when combined with the spectroscopic estimates of the T_eff, the radius of each of the four WD stars When combined with the orbital elements, this leads to a dynamical mass measurement for each WD, and a four calibration points of the WD mass-radius relation
ACS/WFC3 11735
The LSD Project: Dynamics, Merging and Stellar Populations of a Sample of Well-Studied LBGs at z~3
A large observational effort with the ground-based ESO/VLT telescopes allowed us to obtain deep, spatially-resolved, near-IR spectra of complete sample of 11 Lyman-Break Galaxies at z~3 1 These observations were used to obtain, for the first time, the metallicity and the dynamical properties of a sample of objects that, albeit small, is representative of the total population of the LBGs We propose to use HST to obtain high-resolution optical and near-IR images of this sample of LBGs in order to study the broad-band morphology and the stellar light distribution of these galaxies These images, exploiting the superior spatial resolution of HST images and the low-background : 1- will allow a precise measure of the dynamical mass from the velocity field derived with spectroscopy; 2- will permit a comparison of the distribution of star formation (from the line emission) with the underlying stellar population, and, 3- will be used to check if the complex velocity field and the multiple line-emitting regions detected in most targets can be ascribed to on-going mergers This accurate study will shed light on a number of unsolved problems still affecting the knowledge of the LBGs
ACS/WFC3 11734
The Hosts of High Redshift Gamma-Ray Bursts
Gamma-ray bursts are the most luminous explosive events known, acting as beacons to the high redshift universe Long duration GRBs have their origin in the collapse of massive stars and thus select star forming galaxies across a wide range of redshift Due to their bright afterglows we can study the details of GRB host galaxies via absorption spectroscopy, providing redshifts, column densities and metallicities for galaxies far too faint to be accessible directly with current technology We have already obtained deep ground based observations for many hosts and here propose ACS/WFC3 and WFC3 observations of the fields of bursts at z>3 which are undetected in deep ground based images These observations will study the hosts in emission, providing luminosities and morphologies and will enable the construction of a sample of high-z galaxies with more detailed physical properties than has ever been possible before
COS/FUV 11619
Definitive ISM Abundances through Low-mass X-ray Binaries as Lighthouses
We propose observations of the UV spectra of two low-mass X-ray binaries (Sco X-1 and Cyg X-2) with existing Chandra X-Ray Observatory (CXO) data From the X-ray data we will measure total (phase-independent) column densities of O, Ne, and Fe From the UV data we will determine gas-phase column densities of H and O The data in conjunction will allow us to make unique measurements of the total interstellar abundances of oxygen, neon, and iron, and direct measurements of the dust-phase abundances of O and Fe
WFC3/UV 11605
Obtaining the Missing Links in the Test of Very Low Mass Evolutionary Models with HST
We are proposing for spatially resolved ACS+HRC observations of 11 very low mass binaries spanning late-M, L and T spectral types in order to obtain precise effective temperature measurements for each component All of our targets are part of a program in which we are measuring dynamical masses of very low-mass binaries to an unprecedented precision of 10% (or better) However, without precise temperature measurements, the full scientific value of these mass measurements cannot be realized Together, mass and temperature measurements will allow us to distinguish between brown dwarf evolutionary models that make different assumptions about the interior and atmospheric structure of these ultra-cool objects While dynamical masses can be obtained from the ground in the near-IR, obtaining precise temperatures require access to optical data which, for these sub-arcsecond binaries, can only be obtained from space with Hubble
WFC3/ACS/IR 11600
Star Formation, Extinction, and Metallicity at 0
7 The global star formation rate (SFR) is ~10x higher at z=1 than today
This could be due to drastically elevated SFR in some fraction of
galaxies, such as mergers with central bursts, or a higher SFR across
the board
Either means that the conditions in z=1 star forming
galaxies could be quite different from local objects
The next step
beyond measuring the global SFR is to determine the dependence of SFR,
obscuration, metallicity, and size of the star-forming region on
galaxy mass and redshift
However, SFR indicators at z=1 typically
apply local calibrations for UV, [O II] and far-IR, and do not agree
with each other on a galaxy-by-galaxy basis
Extinction, metallicity,
and dust properties cause uncontrolled offsets in SFR calibrations
The great missing link is Balmer H-alpha, the most sensitive probe of
SFR
We propose a slitless WFC3/G141 IR grism survey of GOODS-N, at 2
orbits/pointing
It will detect Ha+[N II] emission from 0
7 ACS/WFC3 11593 Dynamical Masses of the Coolest Brown Dwarfs T dwarfs are excellent laboratories to study the evolution and the
atmospheric physics of both brown dwarfs and extrasolar planets
To
date, only a single T dwarf binary has a dynamical mass determination,
and more are sorely needed
The prospects of measuring more dynamical
masses over the next decade are limited to 6 known short-period T
dwarf binaries
We propose here to obtain Long-Term HST/ACS monitoring
for the 3 of the 6 binaries which cannot be resolved with AO from the
ground
Upon completion, our program will substantially increase the
number of T dwarf dynamical mass measurements and thereby provide key
benchmarks for testing theoretical models of ultracool objects
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 ACS/SBC/COS/NUV/FUV 11579 The Difference Between Neutral- and Ionized-Gas Metal Abundances in
Local Star-Forming Galaxies with COS The metallicity of galaxies and its evolution with redshift is of
paramount importance for understanding galaxy formation
Abundances in
the interstellar medium (ISM) are typically determined using
emission-line spectroscopy of HII regions
However, since HII regions
are associated with recent SF they may not have abundances typical for
the galaxy as a whole
This is true in particular for star-forming
galaxies (SFGs), in which the bulk of the metals may be contained in
the neutral gas
It is therefore important to directly probe the metal
abundances in the neutral gas
This can be done using absorption lines
in the Far UV
We have developed techniques to do this in SFGs, where
the absorption is measured for sightlines toward bright SF regions
within the galaxy itself
We have successfully applied this technique
to a sample of galaxies observed with FUSE
The results have been very
promising, suggesting in I Zw 18 that abundances in the neutral gas
may be up to 0
5 dex lower than in the ionized gas
However, the
interpretation of the FUSE data is complicated by the very large FUSE
aperture (30 arcsec), the modest S/N, and the limited selection of
species available in the FUSE bandpass
The advent of COS on HST now
allows a significant advance in all of these areas
We will therefore
obtain absorption line spectroscopy with G130M in the same sample for
which we already have crude constraints from FUSE
We will obtain
ACS/SBC images to select the few optimal sightlines to target in each
galaxy
The results will be interpreted through line-profile fitting
to determine the metal abundances constrained by the available lines
The results will provide important new insights into the metallicities
of galaxies, and into outstanding problems at high redshift such as
the observed offset between the metallicities of Lyman Break Galaxies
and Damped Lyman Alpha systems
==============================================================================
TOPIC: Daily Report #5190 == 1 of 1 ==
Date: Tues, Sep 28 2010 8:03 am
From: "Cooper, Joe" HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science DAILY REPORT #5190 PERIOD COVERED: 5am September 26 - 5am September 27, 2010 (DOY 270/00:00z-270/23:59z) 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: (None) COMPLETED OPS NOTES: (None) FGS GSAcq 13 13
FGS REAcq 05 05
OBAD with Maneuver 11 11 SIGNIFICANT EVENTS: (None) OBSERVATIONS SCHEDULED: ACS/WFC 11996 CCD Daily Monitor (Part 3) 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 308 orbits (19
25 weeks) from 21 June
2010 to 1 November 2010
ACS/WFC 12209 A Strong Lensing Measurement of the Evolution of Mass Structure in
Giant Elliptical Galaxies The structure and evolution of giant elliptical galaxies provide key
quantitative tests for the theory of hierarchical galaxy formation in
a cold dark matter dominated universe
Strong gravitational lensing
provides the only direct means for the measurement of individual
elliptical galaxy masses beyond the local universe, but there are
currently no large and homogeneous samples of strong lens galaxies at
significant cosmological look-back time
Hence, an accurate and
unambiguous measurement of the evolution of the mass-density structure
of elliptical galaxies has until now been impossible
Using
spectroscopic data from the recently initiated Baryon Oscillation
Spectroscopic Survey (BOSS) of luminous elliptical galaxies at
redshifts from approximately 0
4 to 0
7, we have identified a large
sample of high-probability strong gravitational lens candidates at
significant cosmological look-back time, based on the detection of
emission-line features from more distant galaxies along the same lines
of sight as the target ellipticals
We propose to observe 45 of these
systems with the ACS-WFC in order to confirm the incidence of lensing
and to measure the masses of the lens galaxies
We will complement
these lensing mass measurements with stellar velocity dispersions from
ground-based follow-up spectroscopy
In combination with similar data
from the Sloan Lens ACS (SLACS) Survey at lower redshifts, we will
directly measure the cosmic evolution of the ratio between lensing
mass and dynamical mass, to reveal the structural explanation for the
observed size evolution of elliptical galaxies (at high mass)
We will
also measure the evolution of the logarithmic mass-density profile of
massive ellipticals, which is sensitive to the details of the merging
histories through which they are assembled
Finally, we will use our
lensing mass-to-light measurements to translate the BOSS galaxy
luminosity function into a mass function, and determine its evolution
in combination with data from the original Sloan Digital Sky Survey
ACS/WFC 12210 SLACS for the Masses: Extending Strong Lensing to Lower Masses and
Smaller Radii Strong gravitational lensing provides the most accurate possible
measurement of mass in the central regions of early-type
galaxies(ETGs)
We propose to continue the highly productive Sloan
Lens ACS (SLACS) Survey for strong gravitational lens galaxies by
observing a substantial fraction of 135 new ETG gravitational-lens
candidates with HST-ACS WFC F814W Snapshot imaging
The proposed
target sample has been selected from the seventh and final data
release of the Sloan Digital Sky Survey, and is designed to complement
the distribution of previously confirmed SLACS lenses in lens-galaxy
mass and in the ratio of Einstein radius to optical half-light radius
The observations we propose will lead to a combined SLACS sample
covering nearly two decades in mass, with dense mapping of enclosed
mass as a function of radius out to the half-light radius and beyond
With this longer mass baseline, we will extend our lensing and
dynamical analysis of the mass structure and scaling relations of ETGs
to galaxies of significantly lower mass, and directly test for a
transition in structural and dark-matter content trends at
intermediate galaxy mass
The broader mass coverage will also enable
us to make a direct connection to the structure of well-studied nearby
ETGs as deduced from dynamical modeling of their line-of-sight
velocity distribution fields
Finally, the combined sample will allow
a more conclusive test of the current SLACS result that the intrinsic
scatter in ETG mass-density structure is not significantly correlated
with any other galaxy observables
The final SLACS sample at the
conclusion of this program will comprise approximately 130 lenses with
known foreground and background redshifts, and is likely to be the
largest confirmed sample of strong-lens galaxies for many years to
come
ACS/WFC3 11882 CCD Hot Pixel Annealing This program continues the monthly anneal that has taken place every
four weeks for the last three cycles
We now obtain WFC biases and
darks before and after the anneal in the same sequence as is done for
the ACS daily monitor (now done 4 times per week)
So the anneal
observation supplements the monitor observation sets during the
appropriate week
Extended Pixel Edge Response (EPER) and First Pixel
Response (FPR) data will be obtained over a range of signal levels for
the Wide Field Channel (WFC)
This program emulates the ACS pre-flight
ground calibration and post-launch SMOV testing (program 8948), so
that results from each epoch can be directly compared
The High
Resolution Channel (HRC) visits have been removed since it could not
be repaired during SM4
This program also assesses the read noise, bias structure, and
amplifier cross-talk of ACS/WFC using the GAIN=1
4 A/D conversion
setting
This investigation serves as a precursor to a more
comprehensive study of WFC performance using GAIN=1
4
COS/FUV 11895 FUV Detector Dark Monitor 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/FUV 11897 FUV Spectroscopic Sensitivity Monitoring The purpose of this proposal is to monitor sensitivity in each FUV
grating mode to detect any changes due to contamination or other
causes
COS/FUV 11997 FUV Internal/External Wavelength Scale Monitor This program monitors the offsets between the wavelength scale set by
the internal wavecal versus that defined by absorption lines in
external targets
This is accomplished by observing two external
targets in the SMC: SK191 with G130M and G160M and Cl* NGC 330 ROB B37
with G140L (SK191 is too bright to be observed with G140L)
The
cenwaves observed in this program are a subset of the ones used during
Cycle 17
Observing all cenwaves would require a considerably larger
number of orbits
Constraints on scheduling of each target are placed
so that each target is observed once every ~2-3 months
Observing the
two targets every month would also require a considerably larger
number of orbits
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
COS/NUV 11896 NUV Spectroscopic Sensitivity Monitoring The purpose of this proposal is to monitor sensitivity of each NUV
grating mode to detect any changes due to contamination or other
causes
COS/NUV 12041 COS-GTO: Io Atmosphere/STIS We will use six HST orbits with COS to observe the disk-integrated
longitudinal distribution of Io's atmosphere, and ten HST orbits with
STIS to provide complementary disk-resolved information at key
locations
We wil use the COS G225M grating to observe four SO2
absorption bands, which can be used to determine SO2 atmospheric
density
Disk-integrated 19 micron observations of the atmosphere
indicate that the anti-Jupiter hemisphere of Io has an atmospheric
density roughly ten times greater than the Jupiter-facing side
(Spencer et al
2005), and mm-wave observations suggest a similar
pattern
However the infrared and mm-wave observations cannot easily
separate atmospheric density from atmospheric temperature, so these
results are model-dependent
Sparse 2100 2300 disk-resolved
observations (McGrath et al
2000, Jessup et al
2004) tell a
consistent story, but do not cover enough of Io's surface to provide
full confirmation of the long-wavelength result
We will therefore
observe Io's disk-integrated atmospheric density at six longitudes,
roughly 30, 90, 150, 210, 270, and 330 W, to confirm the 19 micron
results and improve our ability to model the 19-micron data
With
STIS, we plan disk-resolved 2000-3200 spectroscopy of Io's SO2
atmosphere
Our observations will target low-latitude regions away
from active plumes (in contrast to our Cycle 10 observations (Jessup
et al
2004) which targeted the Prometheus plume), to look for the
effect of plumes on the atmosphere
We will also look at the variation
of low-latitude atmospheric abundance with terrain type, to look for
explanations for the large longitudinal variations in atmospheric
pressure to be studied with COS
Finally, we will look at a variety of
regions at two different times of day to determine the extent of
diurnal variations in the atmosphere, which are expected if the
atmosphere is dominantly supported by frost sublimation
COS/NUV/FUV/WFC3/UV 12248 How Dwarf Galaxies Got That Way: Mapping Multiphase Gaseous Halos and
Galactic Winds Below L* One of the most vexing problems in galaxy formation concerns how gas
accretion and feedback influence the evolution of galaxies
In high
mass galaxies, numerical simulations predict the initial fuel is
accreted through 'cold' streams, after which AGN suppress star
formation to leave galaxies red and gas-poor
In the shallow potential
wells that host dwarf galaxies, gas accretion can be very efficient,
and "superwinds" driven either by hot gas expelled by SNe or momentum
imparted by SNe and hot-star radiation are regarded as the likely
source(s) of feedback
However, major doubts persist about the physics
of gas accretion, and particularly about SN-driven feedback, including
their scalings with halo mass and their influence on the evolution of
the galaxies
While "superwinds" are visible in X-rays near the point
of their departure, they generally drop below detectable
surface-brightness limits at ~ 10 kpc
Cold clumps in winds can be
detected as blue-shifted absorption against the galaxy's own
starlight, but the radial extent of these winds are difficult to
constrain, leaving their energy, momentum, and ultimate fate
uncertain
Wind prescriptions in hydrodynamical simulations are
uncertain and at present are constrained only by indirect
observations, e
g
by their influence on the stellar masses of
galaxies and IGM metallicity
All these doubts lead to one conclusion:
we do not understand gas accretion and feedback because we generally
do not observe the infall and winds directly, in the extended gaseous
halos of galaxies, when it is happening
To do this effectively, we
must harness the power of absorption-line spectroscopy to measure the
density, temperature, metallicity, and kinematics of small quantities
of diffuse gas in galaxy halos
The most important physical
diagnostics lie in the FUV, so this is uniquely a problem for HST and
COS
We propose new COS G130M and G160M observations of 41 QSOs that
probe the gaseous halos of 44 SDSS dwarf galaxies well inside their
virial radii
Using sensitive absorption-line measurements of the
multiphase gas diagnostics Lya, CII/IV, Si II/III/IV, and other
species, supplemented by optical data from SDSS and Keck, we will map
the halos of galaxies with L = 0
02 - 0
3 L*, stellar masses M* =
10^(8-10) Msun, over impact parameter from 15 - 150 kpc
These
observations will directly constrain the content and kinematics of
accreting and outflowing material, provide a concrete target for
simulations to hit, and statistically test proposed galactic superwind
models
These observations will also inform the study of galaxies at
high z, where the shallow halo potentials that host dwarf galaxies
today were the norm
These observations are low-risk and routine for
COS, easily schedulable, and promise a major advance in our
understanding of how dwarf galaxies came to be
STIS/CCD 11845 CCD Dark Monitor Part 2 Monitor the darks for the STIS CCD
STIS/CCD 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
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/U 12015 Rapid Follow-Up Observations of Tidal Disruption Events Discovered by
Pan-STARRS1 We propose for rapid follow-up Chandra TOO ACIS-S observations and
HST/COS NUV imaging and FUV low-resolution spectroscopy of 5 flares
from the tidal disruption of stars by supermassive black holes
discovered in the Pan-STARRS1 Medium Deep Survey
With TOO
observations obtained within a month of the peak of the flare, and 5
months later, we aim to 1) constrain the flare's broadband SED and
bolometric luminosity, 2) follow the decay of the flare and look for
spectral evolution, and 3) place strong limits on the presence of a
persistent AGN nucleus
Tidal disruption events provide a cosmic
laboratory to study the physics of accretion onto black holes, and are
a unique probe of the mass of black holes in the nuclei of distant
galaxies
WFC3/UV 11635 In Search of SNIb/Ic Wolf-Rayet Progenitors and Comparison with Red
Supergiants (SNII Progenitors) in the Giant ScI Spiral M101 We propose to test two of the clearest predictions of the theory of
evolution of massive-star evolution: 1) The formation of Wolf-Rayet
stars depends strongly on these stars' metallicity (Z), with
relatively fewer WR stars forming at lower Z, and 2) Wolf-Rayet stars
die as Type Ib or Ic supernovae
To carry out these tests we propose a
deep, narrowband imaging survey of the massive star populations in the
ScI spiral galaxy M101
Just as important, we will test the hypothesis
that Superclusters like 30 Doradus are always richly populated with WR
stars, and by implication that these complexes are responsible for the
spectral signatures of starburst galaxies
Our previous HST survey of the HII regions in the ScIII galaxy NGC
2403 suggested that the distribution of WR stars and RSG is a
sensitive diagnostic of the recent star-forming history of these large
complexes: young cores of O and WR stars are surrounded by older halos
containing RSG
Theory predicts that this must change with
metallicity; relatively fewer WR stars form at lower Z
A key goal of
our proposal is to directly test this paradigm in a single galaxy,
M101 being the ideal target
The abundance gradient across M101 (a
factor of 20) suggests that relatively many more WR will be found in
the inner parts of this galaxy than in the outer "suburbs"
Second, we
note that WR stars are predicted to end their lives as core-collapse
or pair-instability supernovae
The WR population in M101 may be
abundant enough for one to erupt as a Type Ib or Ic supernova within a
generation
The clear a priori identification of a WR progenitor would
be a major legacy of HST
Third, we will also determine if
"superclusters", heavily populated by WR stars, are common in M101
It
is widely claimed that such Superclusters produce the integrated
spectral signatures of Starburst galaxies
We will be able to directly
measure the numbers and emission-line luminosities of thousands of
Wolf Rayet stars located in hundreds of M101 Superclusters, and
correlate those numbers against the Supercluster sizes and
luminosities
It is likely (but far from certain) that Supercluster
sizes and emission-line luminosities are driven by their Wolf-Rayet
star content
Our sample will be the largest and best-ever
Supercluster/Wolf Rayet sample, an excellent local proxy for
characterizing starburst galaxies' Superclusters
WFC3/UV 12237 Orbits, Masses, Densities, and Colors of Two Transneptunian Binaries Binaries are the key to learning many crucial bulk properties of
transneptunian objects (TNOs) including their masses
Perhaps the most
interesting mass-dependent property of a TNO is its bulk density,
which provides unique information about its bulk composition and
interior structure
Densities have so far only been measured for a
handful of binary TNO systems
This proposal seeks to determine orbits
and thus masses of two more binary TNOs, both of which are also to be
observed at thermal infrared wavelengths by the Herschel spacecraft
Combining the masses from Hubble with the sizes from Herschel will
enable us to compute their densities
We will also obtain
multi-wavelength photometric colors of the individual components of
each binary system
It is imperative to link colors to the physical
properties measurable in binary systems in order to use the remnant
planetesimals in today's Kuiper belt to learn more about the early
history of our own solar system, and more generally about how
planetesimals form in nebular disks and subsequently evolve
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)
==============================================================================
TOPIC: Daily Report #5191 == 1 of 1 ==
Date: Wed, Sep 29 2010 7:55 am
From: "Bassford, Lynn" HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science DAILY REPORT #5191 PERIOD COVERED: 8:00pm September 27 - 7:59pm September 28, 2010 (DOY 271/00:00z-271/23:59z) 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: (None) COMPLETED OPS NOTES: (None) FGS GSAcq 8 8
FGS REAcq 8 8
OBAD with Maneuver 6 6 SIGNIFICANT EVENTS: (None) OBSERVATIONS SCHEDULED: ACS/WFC3 11882 CCD Hot Pixel Annealing This program continues the monthly anneal that has taken place every
four weeks for the last three cycles
We now obtain WFC biases and
darks before and after the anneal in the same sequence as is done for
the ACS daily monitor (now done 4 times per week)
So the anneal
observation supplements the monitor observation sets during the
appropriate week
Extended Pixel Edge Response (EPER) and First Pixel
Response (FPR) data will be obtained over a range of signal levels for
the Wide Field Channel (WFC)
This program emulates the ACS pre-flight
ground calibration and post-launch SMOV testing (program 8948), so
that results from each epoch can be directly compared
The High
Resolution Channel (HRC) visits have been removed since it could not
be repaired during SM4
This program also assesses the read noise, bias structure, and
amplifier cross-talk of ACS/WFC using the GAIN=1
4 A/D conversion
setting
This investigation serves as a precursor to a more
comprehensive study of WFC performance using GAIN=1
4
COS/NUV/FUV 11535 COS-GTO: Deep Search for an Oxygen Atmosphere on Callisto We plan a deep search for 1304? and 1356? O emission from Callisto, to
detect or place strong limits on the presence of a hypothesized O2
atmosphere on this moon (Liang et al
2005)
Tenuous oxygen
atmospheres on Europa and Ganymede have been detected by HST using
these emission lines, but searches for O emission from Callisto have
not been successful (Strobel et al
2002)
The Liang et al
models
predict O emission at levels comparable to the Strobel et al
upper
limit, so the improved sensitivity of COS may be able to detect the
emission, and thus Callisto's O2 atmosphere, for the first time
S/C 12046 COS FUV DCE Memory Dump Whenever the FUV detector high voltage is on, count rate and current
draw information is collected, monitored, and saved to DCE memory
Every 10 msec the detector samples the currents from the HV power
supplies (HVIA, HVIB) and the AUX power supply (AUXI)
The last 1000
samples are saved in memory, along with a histogram of the number of
occurrences of each current value
In the case of a HV transient (known as a "crackle" on FUSE), where
one of these currents exceeds a preset threshold for a persistence
time, the HV will shut down, and the DCE memory will be dumped and
examined as part of the recovery procedure
However, if the current
exceeds the threshold for less than the persistence time (a
"mini-crackle" in FUSE parlance), there is no way to know without
dumping DCE memory
By dumping and examining the histograms regularly,
we will be able to monitor any changes in the rate of "mini-crackles"
and thus learn something about the state of the detector
STIS/CCD 11845 CCD Dark Monitor Part 2 Monitor the darks for the STIS CCD
STIS/CCD 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
WFC3/IR 12307 A public SNAPSHOT Survey of Gamma-ray Burst Host Galaxies We propose to conduct a public infrared survey of the host galaxies of
Swift selected gamma-ray bursts (GRBs) at z<3
By obtaining deep,
diffraction limited imaging in the IR we will complete detections for
the host galaxies, and in concert with our extensive ground based
afterglow and host programmes will compile a detailed catalog of the
properties of high-z galaxies selected by GRBs
In particular these
observations will enable us to study the colours, luminosities and
morphologies of the galaxies
This in turn informs studies of the
nature of the progenitors and the role of GRBs as probes of star
formation across cosmic history
Ultimately it provides a product of
legacy value which will greatly complement further studies with next
generation facilities such as ALMA and JWST
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 11635 In Search of SNIb/Ic Wolf-Rayet Progenitors and Comparison with Red
Supergiants (SNII Progenitors) in the Giant ScI Spiral M101 We propose to test two of the clearest predictions of the theory of
evolution of massive-star evolution: 1) The formation of Wolf-Rayet
stars depends strongly on these stars' metallicity (Z), with
relatively fewer WR stars forming at lower Z, and 2) Wolf-Rayet stars
die as Type Ib or Ic supernovae
To carry out these tests we propose a
deep, narrowband imaging survey of the massive star populations in the
ScI spiral galaxy M101
Just as important, we will test the hypothesis
that Superclusters like 30 Doradus are always richly populated with WR
stars, and by implication that these complexes are responsible for the
spectral signatures of starburst galaxies
Our previous HST survey of the HII regions in the ScIII galaxy NGC
2403 suggested that the distribution of WR stars and RSG is a
sensitive diagnostic of the recent star-forming history of these large
complexes: young cores of O and WR stars are surrounded by older halos
containing RSG
Theory predicts that this must change with
metallicity; relatively fewer WR stars form at lower Z
A key goal of
our proposal is to directly test this paradigm in a single galaxy,
M101 being the ideal target
The abundance gradient across M101 (a
factor of 20) suggests that relatively many more WR will be found in
the inner parts of this galaxy than in the outer "suburbs"
Second, we
note that WR stars are predicted to end their lives as core-collapse
or pair-instability supernovae
The WR population in M101 may be
abundant enough for one to erupt as a Type Ib or Ic supernova within a
generation
The clear a priori identification of a WR progenitor would
be a major legacy of HST
Third, we will also determine if
"superclusters", heavily populated by WR stars, are common in M101
It
is widely claimed that such Superclusters produce the integrated
spectral signatures of Starburst galaxies
We will be able to directly
measure the numbers and emission-line luminosities of thousands of
Wolf Rayet stars located in hundreds of M101 Superclusters, and
correlate those numbers against the Supercluster sizes and
luminosities
It is likely (but far from certain) that Supercluster
sizes and emission-line luminosities are driven by their Wolf-Rayet
star content
Our sample will be the largest and best-ever
Supercluster/Wolf Rayet sample, an excellent local proxy for
characterizing starburst galaxies' Superclusters
WFC3/UV 12348 WFC3/UVIS Charge Injection Test In preparation for making charge injection (CI) available to
observers, this proposal will 1) confirm that the CI performs on-orbit
as it did on the ground, 2) provide an initial assessment of which CI
mode is most effective (10, 17, 25 line or continuous), and 3) obtain
a baseline calibration for each mode
WFC3/UV/IR 11664 The WFC3 Galactic Bulge Treasury Program: Populations, Formation
History, and Planets Exploiting the full power of the Wide Field Camera 3 (WFC3), we
propose deep panchromatic imaging of four fields in the Galactic
bulge
These data will enable a sensitive dissection of its stellar
populations, using a new set of reddening-free photometric indices we
have constructed from broad-band filters across UV, optical, and
near-IR wavelengths
These indices will provide accurate temperatures
and metallicities for hundreds of thousands of individual bulge stars
Proper motions of these stars derived from multi-epoch observations
will allow separation of pure bulge samples from foreground disk
contamination
Our catalogs of proper motions and panchromatic
photometry will support a wide range of bulge studies
Using these photometric and astrometric tools, we will reconstruct the
detailed star-formation history as a function of position within the
bulge, and thus differentiate between rapid- and extended-formation
scenarios
We will also measure the dependence of the stellar mass
function on metallicity, revealing how the characteristic mass of star
formation varies with chemistry
Our sample of bulge stars with
accurate metallicities will include 12 candidate hosts of extrasolar
planets
Planet frequency is correlated with metallicity in the solar
neighborhood; our measurements will extend this knowledge to a remote
environment with a very distinct chemistry
Our proposal also includes observations of six well-studied globular
and open star clusters; these observations will serve to calibrate our
photometric indices, provide empirical population templates, and
transform the theoretical isochrone libraries into the WFC3 filter
system
Besides enabling our own program, these products will provide
powerful new tools for a host of other stellar-population
investigations with HST/WFC3
We will deliver all of the products from
this Treasury Program to the community in a timely fashion
WFC3/UVIS 11729 Photometric Metallicity Calibration with WFC3 Specialty Filters The community has chosen to include several filters in the WFC3 filter
complement that have been designed to allow fairly precise estimates
of stellar metallicities, and many science programs are enabled by
this capability
Since these filters do not exactly match those used
for this purpose on the ground, however, the mapping of stellar colors
to stellar metallicities needs to be calibrated
We propose to achieve
this calibration through observations of five stellar clusters with
well known metallicities
We will calibrate several different filter
calibrations which will allow future users to determine what filter
combination best meets their science needs
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/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
==============================================================================
TOPIC: HST Daily Reports == 1 of 1 ==
Date: Wed, Sep 29 2010 2:15 pm
From: "Paul Scowen" HST Daily Reports For the past decades we have been posting the HST Daily Status Reports to this
newsgroup for interested readers, and those people who use the HST as part of
their daily work both in industry and academia
We have been notified that our usual method for receiving these reports will be
terminated on October 8th
We can still get to the information and post it
here, but there will be more work involved
As such, we have decided it would
be appropriate to determine if there is still a need for the reports to be
published here
If you are a regular reader of this newsgroup (sci
astro
hubble) and would like
to continue to see the HST Daily Reports published here, please email me back
at the email address at the top of this post
Thanks in advance
Paul Scowen
Research Professor, ASU ============================================================================== You received this message because you are subscribed to the Google Groups "sci
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