Date: August 3rd 2010

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Daily Report #5143 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/1e70a960d2b675f4?hl=en
Daily Report #5145 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/7029b87987aae417?hl=en
Daily Report #5146 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/a123696c310ecc61?hl=en
Daily Report #5147 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/2fc8eddc01b07a60?hl=en
Daily Report #5148 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/50d3896ddb20a7ed?hl=en
Daily Report #5149 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/5f2c0a1cedfcb414?hl=en
Daily Report #5150 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/63552440e21bba54?hl=en

============================================================================== TOPIC: Daily Report #5143

http://groups google com/group/sci astro hubble/t/1e70a960d2b675f4?hl=en

== 1 of 1 == Date: Thurs, Jul 22 2010 6:38Ã‚Â am From: "Bassford, Lynn"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5143

PERIOD COVERED: 5am July 21 - 5am July 22, 2010 (DOY 202/09:00z-203/09:00z)

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 7 7 FGS REAcq 9 9 OBAD with Maneuver 3 3

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

STIS/CC 11845

CCD Dark Monitor Part 2

Monitor the darks for the STIS CCD

STIS/CC 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/CC/MA 11668

Cosmo-chronometry and Elemental Abundance Distribution of the Ancient Star HE1523-0901

We propose to obtain near-UV HST/STIS spectroscopy of the extremely metal-poor, highly r-process-enhanced halo star HE 1523-0901, in order to produce the most complete abundance distribution of the heaviest stable elements, including platinum, osmium, and lead These HST abundance data will then be used to estimate the initial abundances of the long-lived radioactive elements thorium and uranium, and by comparison with their observed abundances, enable an accurate age determination of this ancient star The use of radioactive chronometers in stars provides an independent lower limit on the age of the Galaxy, which can be compared with alternative limits set by globular clusters and by analysis from WMAP Our proposed observations of HE1523-0901 will also provide significant new information about the early chemical history of the Galaxy, specifically, the nature of the first generations of stars and the types of nucleosynthetic processes that occurred at the onset of Galactic chemical evolution

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

WFC3/UV/ACS/WFC/IR 12058

A Panchromatic Hubble Andromeda Treasury - I

We propose to image the north east quadrant of M31 to deep limits in the UV, optical, and near-IR HST imaging should resolve the galaxy into more than 100 million stars, all with common distances and foreground extinctions UV through NIR stellar photometry (F275W, F336W with WFC3/UVIS, F475W and F814W with ACS/WFC, and F110W and F160W with WFC3/NIR) will provide effective temperatures for a wide range of spectral types, while simultaneously mapping M31's extinction Our central science drivers are to: understand high-mass variations in the stellar IMF as a function of SFR intensity and metallicity; capture the spatially-resolved star formation history of M31; study a vast sample of stellar clusters with a range of ages and metallicities These are central to understanding stellar evolution and clustered star formation; constraining ISM energetics; and understanding the counterparts and environments of transient objects (novae, SNe, variable stars, x-ray sources, etc ) As its legacy, this survey adds M31 to the Milky Way and Magellanic Clouds as a fundamental calibrator of stellar evolution and star-formation processes for understanding the stellar populations of distant galaxies Effective exposure times are 977s in F275W, 1368s in F336W, 4040s in F475W, 4042s in F814W, 699s in F110W, and 1796s in F160W, including short exposures to avoid saturation of bright sources These depths will produce photon-limited images in the UV Images will be crowding-limited in the optical and NIR, but will reach below the red clump at all radii The images will reach the Nyquist sampling limit in F160W, F475W, and F814W

WFC3/UVI 11615

Hunting for Optical Companions to Binary MSPs in Globular Clusters

Here we present a proposal which exploits the renewed potential of HST after the Service Mission 4 for probing the population of binary Millisecond Pulsars (MSPs) in Globular Clusters In particular we intend to: (1) extend the search for optical counterparts in Terzan 5, by pushing the performance of the WFC3 IR channel to sample the entire MS extension down to M=0 1 Mo; (2) perform a deep multi-band search of MSP companions with the WFC3, in 3 clusters (namely NGC6440, M28 and M5), where recent radio observations have found particularly interesting objects; (3) derive an accurate radial velocity (with STIS) of the puzzling optical companion COM6266B recently discovered by our group, to firmly assess its cluster membership This program is the result of a large collaboration among the three major groups (lead by Freire, Ransom and Possenti) which are performing extensive MSP search in GCs in the radio bands, and our group which has a large experience in performing accurate stellar photometry in crowded environments This collaboration has produced a number of outstanding discoveries In fact, three of the 6 optical counterparts to binary MSP companions known to date in GCs have been discovered by our group The observations here proposed would easily double/triple the existing sample of known MSP companions, allowing the first meaningful approach to the study of the formation, evolution and recycling process of pulsar in GCs Moreover, since most of binary MSPs in GCs are thought to form via stellar interactions in the high density core regions, the determination of the nature of the companion and the incidence of this collisionally-induced population has a significant impact on our knowledge of the cluster dynamics Even more interesting, the study of the optical companions to NSs in GCs allows one to derive tighter constraints (than those obtainable for NS binaries in the Galactic field) on the system properties This has, in turn, an intrinsic importance for fundamental physics, since it offers the opportunity of measuring the mass of the NS and hence constraining the equation of state of matter at the nuclear equilibrium density

WFC3/UVIS 11907

UVIS Cycle 17 Contamination Monitor

The UV throughput of WFC3 during Cycle 17 is monitored via weekly standard star observations in a subset of key filters covering 200-600nm and F606W, F814W as controls on the red end The data will provide a measure of throughput levels as a function of time and wavelength, allowing for detection of the presence of possible contaminants

WFC3/UVIS/IR 11909

UVIS Hot Pixel Anneal

The on-orbit radiation environment of WFC3 will continually generate new hot pixels This proposal performs the procedure required for repairing those hot pixels in the UVIS CCDs During an anneal, the two-stage thermo-electric cooler (TEC) is turned off and the four-stage TEC is used as a heater to bring the UVIS CCDs up to ~20 deg C As a result of the CCD warmup, a majority of the hot pixels will be fixed; previous instruments such as WFPC2 and ACS have seen repair rates of about 80% Internal UVIS exposures are taken before and after each anneal, to allow an assessment of the procedure's effectiveness in WFC3, provide a check of bias, global dark current, and hot pixel levels, as well as support hysteresis (bowtie) monitoring and CDBS reference file generation One IR dark is taken after each anneal, to provide a check of the IR detector

============================================================================== TOPIC: Daily Report #5145

http://groups google com/group/sci astro hubble/t/7029b87987aae417?hl=en

== 1 of 1 == Date: Mon, Jul 26 2010 6:05Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5145

PERIOD COVERED: 5am July 23 - 5am July 26, 2010 (DOY 204/09:00z-207/09:00z)

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

12337 - REAcq(2,1,1) scheduled at 205/09:14:55z failed to RGA control at 205/09:21:09z

Observations affected: ACS 102-107 Proposal ID# 11887, WFC3 202 Proposal ID# 11905, WFC3 203-204 Proposal ID# 11929

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

                   SCHEDULED SUCCESSFUL

FGS GSAcq 22 22 FGS REAcq 21 20 OBAD with Maneuver 22 22

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

WFC3/UV/ACS/WFC/IR 12058

A Panchromatic Hubble Andromeda Treasury - I

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

WFC3/IR 12005

Unveiling the Dusty Starburst Galaxy Hosting GRB080607

GRB 080607 at redshift z = 3 0363 is a unique case of a highly extinguished (A_V ~ 3 mag) afterglow that was yet sufficiently bright for high-quality spectroscopy The ISM properties revealed by our afterglow spectrum are unprecedented among GRB host galaxies, including an enormous dust and gas surface mass density (~ 400 M_sun/pc^2), the first detection of CO molecules, and roughly solar metallicity Contrary to the common expectation of GRBs occurring preferentially in low-mass and low-metallicity environments, the observed large metal and dust content, together with the mass-metallicity relation known for z=2-3 galaxies, imply that the host galaxy is massive and intrinsically luminous Identifying the host galaxy of this event is critical for connecting our spectroscopy to the rest of the poorly-understood dark burst population with suppressed optical afterglow light Despite our large investments in optical and NIR imaging at ground-based telescopes to date, the host of GRB 080607 has eluded detection to an unobscured limiting UV luminosity of ~ 0 07 L* The lack of bright emission suggests that the dust seen in the afterglow spectrum reflects the global dust content throughout the host ISM Otherwise, it would imply the presence of highly metal-enriched regions in a low-mass galaxy, challenging the validity of our current understanding of star formation at high redshift

The low sky background and high spatial resolution make HST and WFC3/IR the only instrument available to unveil the morphology and stellar counterpart of the dusty host galaxy of GRB 080607 Here we request Director's Discretionary time to obtain deep near-infrared images of the field surrounding GRB 080607, using WFC3 and the IR channel with the F160W filter The proposed imaging program will allow us to investigate whether the host of GRB 080607 is a dusty luminous galaxy or a faint dwarf galaxy with patchy dust clouds, and to examine the significance of dust enshrouded star formation at z~3

The extraordinary ISM properties observed around GRB 080607 have stimulated a considerable amount of interest not only in the GRB community but also among observers and theorists who study star formation both in the nearby universe and at high redshift We believe the proposed WFC3/IR imaging data will have high impact in the broader astrophysics community

ACS/WFC 11996

CCD Daily Monitor (Part 3)

WFC3/IR 11933

IR Rate Dependent Non-linearity

The NICMOS non-linearity known as the Bohlin Effect has revealed that the apparent flux of a source observed by NICMOS is not a simple, linear function of count rate The effect has been characterized by observations of star clusters observed with and without additional background from the internal lamps As WFC3 lacks internal lamps which can be used to add background, we will rely on the bright Earth limb to provide additional background We will observe a star cluster, 47 Tuc, repeatedly throughout a complete HST orbit which has been chosen to put the closest approach to the bright Earth to be 13 5 degrees, the closest approach allowed while retaining FGS guiding Another set will be done with the BE limb closest approach of 15 5 degrees The observations will be done with the two most commonly used filters, F110W and F160W and at two different bright Earth limb angles to test the linearity of the non-linearity We have also included an orbit on NGC 1850 to repeat the NICMOS field for which the linearity of the field has been established

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/IR 11917

IR Earth Flats Pathfinder

This program is an experimental path finder for Cycle 18 calibration (The WFC3 UVIS version of this is program 11914 and contains additional detail in its description) Infrared-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 IR imagery: per single "dark-sky" orbit, we anticipate achieving Poisson S/N > 100 per pixel in each of three to five exposures, depending on sample sequence (SPARS25 or SPARS50)

Why not use the Sunlit Earth? It is too bright for WFC3 IR full-frame minimum exposure time of 3 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 IR filters the sunlit earth sometimes is faint enough to not saturate immediately, but based upon predictions (Cox et al 1987 "Standard Astronomical Sources for HST: 6 Spatially Flat Fields ") and observations (Gilmore 1998), we consider sunlit Earth unlikely to be successful unless it is twilight

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 prior to the unshuttered exposure presents additional problems for the Earth Also, we're unsure if HST can point 180 deg from the Sun

WFC3/IR 11915

IR Internal Flat Fields

This program is the same as 11433 (SMOV) and depends on the completion of the IR initial alignment (Program 11425) This version contains three instances of 37 internal orbits: to be scheduled early, middle, and near the end of Cycle 17, in order to use the entire 110-orbit allocation

In this test, we will study the stability and structure of the IR channel flat field images through all filter elements in the WFC3-IR channel Flats will be monitored, i e to capture any temporal trends in the flat fields and delta flats produced High signal observations will provide a map of the pixel-to-pixel flat field structure, as well as identify the positions of any dust particles

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)

ACS/WFC3 11887

CCD Stability Monitor

This program will verify that the low frequency flat fielding, the photometry, and the geometric distortion are stable in time and across the field of view of the CCD arrays A moderately crowded stellar field in the cluster 47 Tuc is observed with the ACS (at the cluster core) and WFC3 (6 arcmin West of the cluster core) using the full suite of broad and narrow band imaging filters The positions and magnitudes of objects will be used to monitor local and large scale variations in the plate scale and the sensitivity of the detectors and to derive an independent measure of the detector CTE The UV sensitivity for the SBC and ACS will be addressed in the UV contamination monitor program (11886, PI=Smith)

One additional orbit will be obtained at the beginning of the cycle will allow a verification of the CCD gain ratios for WFC3 using gain 2 0, 1 4, 1 0, 0 5 and for ACS using gain 4 0 and 2 0 In addition, one subarray exposure with the WFC3 will allow a verification that photometry obtained in full-frame and in sub-array modes are repeatable to better than 1% This test is important for the ACS Photometric Cross-Calibration program (11889, PI=Bohlin) which uses sub-array exposures

STIS/CC 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/CC 11845

CCD Dark Monitor Part 2

Monitor the darks for the STIS CCD

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

WFC3/UVIS 11732

The Temperature Profiles of Quasar Accretion Disks

We can now routinely measure the size of quasar accretion disks using gravitational microlensing of lensed quasars At optical wavelengths we observe a size and scaling with black hole mass roughly consistent with thin disk theory but the sizes are larger than expected from the observed optical fluxes One solution would be to use a flatter temperature profile, which we can study by measuring the wavelength dependence of the disk size over the largest possible wavelength baseline Thus, to understand the size discrepancy and to probe closer to the inner edge of the disk we need to extend our measurements to UV wavelengths, and this can only be done with HST For example, in the UV we should see significant changes in the optical/UV size ratio with black hole mass We propose monitoring 5 lenses spanning a broad range of black hole masses with well-sampled ground based light curves, optical disk size measurements and known GALEX UV fluxes during Cycles 17 and 18 to expand from our current sample of two lenses We would obtain 5 observations of each target in each Cycle, similar to our successful strategy for the first two targets

WFC3/UVIS 11730

Continued Proper Motions of the Magellanic Clouds: Orbits, Internal Kinematics, and Distance

In Cycles 11 and 13 we obtained two epochs of ACS/HRC data for fields in the Magellanic Clouds centered on background quasars We used these data to determine the proper motions of the LMC and SMC to better than 5% and 15% respectively The results had a number of unexpected implications for the Milky Way-LMC-SMC system and received considerable attention in the literature and in the press The implied three-dimensional velocities are larger than previously believed and close to the escape velocity in a standard 10^12 solar mass Milky Way dark halo Our orbit calculations suggest the Clouds may not be bound to the Milky Way or may just be on their first passage, both of which are unexpected in view of traditional interpretations of the Magellanic Stream Alternatively, the Milky Way dark halo may be a factor two more massive than previously believed, which would be surprising in view of other observational constraints Also, the relative velocity between the LMC and SMC was larger than expected, leaving open the possibility that the Clouds may not be bound to each other To further verify and refine our results we requested an additional epoch data in Cycle 16 which is being executed with WFPC2/PC due to the failure of ACS A detailed analysis of one LMC field shows that the field proper motion using all three epochs of data is consistent within 1-sigma with the two- epoch data, thus verifying that there are no major systematic effects in our previous measurements The random errors, however, are only smaller by a factor of 1 4 because of the relatively large errors in the WFPC2 data A prediction for a fourth epoch with measurement errors similar to epochs 1 and 2 shows that the uncertainties will improve by a factor of 3 This will allow us to better address whether the Clouds are indeed bound to each other and to the Milky Way It will also allow us to constrain the internal motions of various populations within the Clouds, and to determine a distance to the LMC using rotational parallax Continuation of this highly successful program is therefore likely to provide important additional insights Execution in SNAPshot mode guarantees maximally efficient use of HST resources

ACS/WFC3 11670

The Host Environments of Type Ia Supernovae in the SDSS Survey

The Sloan Digital Sky Survey Supernova Survey has discovered nearly 500 type Ia supernovae and created a large, unique, and uniform sample of these cosmological tools As part of a comprehensive study of the supernova hosts, we propose to obtain Hubble ACS images of a large fraction of these galaxies Integrated colors and spectra will be measured from the ground, but we require high-resolution HST imaging to provide accurate morphologies and color information at the site of the explosion This information is essential in determining the systematic effects of population age on type Ia supernova luminosities and improving their reliability in measuring dark energy Recent studies suggest two populations of type Ia supernovae: a class that explodes promptly after star-formation and one that is delayed by billions of years Measuring the star-formation rate at the site of the supernova from colors in the HST images may be the best way to differentiate between these classes

WFC3/UVIS/IR 11662

Improving the Radius-Luminosity Relationship for Broad-Lined AGNs with a New Reverberation Sample

The radius-luminosity (R-L) relationship is currently the fundamental basis for all techniques used to estimate black hole masses in AGNs, in both the nearby and distant universe However, the current R-L relationship is based on 34 objects that cover a limited range in black hole mass and luminosity To improve our understanding of black hole growth and evolution, the R-L relationship must be extended to cover a broader range of black hole masses using the technique known as reverberation mapping To this end, we have been awarded an unprecedented 64 nights on the Lick Observatory 3-m telescope between March 24 and May 31, 2008, to spectroscopically monitor 12 AGNs in order to measure their black hole masses To properly determine the luminosities of these 12 AGNs, we must correct them for their host-galaxy starlight contributions using high-resolution images Previous work by Bentz et al (2006) has shown that the starlight correction to AGN luminosity measurements is an essential component to interpreting the R-L relationship The correction will be substantial for each of the 12 sources we will monitor, as the AGNs are relatively faint and embedded in nearby, bright galaxies Starlight corrections are not possible with ground-based images, as the PSF and bulge contributions become indistinguishable under typical seeing conditions, and adaptive optics are not yet operational in the spectral range where the corrections are needed In addition, spectral decompositions are very model-dependent and are limited by the degree of accuracy to which we understand emission processes and stellar populations in galaxies Without correcting for starlight, we will be unable to apply the results of our Spring 2008 campaign to the body of knowledge from previous reverberation mapping work Therefore, we propose to obtain high resolution, high dynamic range images of the host galaxies of the 12 AGNs in our ground-based monitoring sample, as well as one white dwarf which will be used as a PSF model

WFC3/UVIS 11657

The Population of Compact Planetary Nebulae in the Galactic Disk

We propose to secure narrow- and broad-band images of compact planetary nebulae (PNe) in the Galactic Disk to study the missing link of the early phases of post-AGB evolution Ejected AGB envelopes become PNe when the gas is ionized PNe expand, and, when large enough, can be studied in detail from the ground In the interim, only the HST capabilities can resolve their size, morphology, and central stars Our proposed observations will be the basis for a systematic study of the onset of morphology Dust properties of the proposed targets will be available through approved Spitzer/IRS spectra, and so will the abundances of the alpha- elements We will be able thus to explore the interconnection of morphology, dust grains, stellar evolution, and populations The target selection is suitable to explore the nebular and stellar properties across the galactic disk, and to set constraints on the galactic evolutionary models through the analysis of metallicity and population gradients

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/UVIS 11643

A Timeline for Early-Type Galaxy Formation: Mapping the Evolution of Star Formation, Globular Clusters, Dust, and Black Holes

While considerable effort has been devoted to statistical studies of the origin of the red sequence of galaxies, there has been relatively little direct exploration of galaxies transforming from late to early types Such galaxies are identified by their post-starburst spectra, bulge- dominated, tidally-disturbed morphologies, and current lack of gas We are constructing the first detailed timeline of their evolution onto the red sequence, pinpointing when star formation ends, nuclear activity ceases, globular clusters form, and the bulk of the merging progenitors' dust disappears Here we propose to obtain HST and Chandra imaging of nine galaxies, whose wide range of post-starburst ages we have precisely dated with a new UV-optical technique and for which we were awarded Spitzer time We will address 1) whether the black hole-bulge mass relation arises from nuclear feedback, 2) whether the bimodality of globular cluster colors is due to young clusters produced in galaxy mergers, and 3) what happens to the dust when late types merge to form an early type

WFC3/IR 11631

Binary Brown Dwarfs and the L/T Transition

Brown dwarfs traverse spectral types M, L and T as their atmospheric structure evolves and they cool into oblivion This SNAPSHOT program will obtain WFC3-IR images of 45 nearby late-L and early-T dwarfs to investigate the nature of the L/T transition Recent analyses have suggested that a substantial proportion of late-L and early-T dwarfs are binaries, comprised of an L dwarf primary and T dwarf secondary WFC3-IR observations will let us quantify this suggestion by expanding coverage to a much larger sample, and permitting comparison of the L/T binary fraction against 'normal' ultracool dwarfs Only eight L/T binaries are currently known, including several that are poorly resolved: we anticipate at least doubling the number of resolved systems The photometric characteristics of additional resolved systems will be crucial to constraining theoretical models of these late-type ultracool dwarfs Finally, our data will also be eminently suited to searching for extremely low luminosity companions, potentially even reaching the Y dwarf regime

WFC3/IR 11591

Are Low-Luminosity Galaxies Responsible for Cosmic Reionization?

Our group has demonstrated that massive clusters, acting as powerful cosmic lenses, can constrain the abundance and properties of low-luminosity star-forming sources beyond z~6; such sources are thought to be responsible for ending cosmic reionization The large magnification possible in the critical regions of well-constrained clusters brings sources into view that lie at or beyond the limits of conventional exposures such as the UDF We have shown that the combination of HST and Spitzer is particularly effective in delivering the physical properties of these distant sources, constraining their mass, age and past star formation history Indirectly, we therefore gain a valuable glimpse to yet earlier epochs Recognizing the result (and limitations) of blank field surveys, we propose a systematic search through 10 lensing clusters with ACS/F814W and WFC3/[F110W+F160W] (in conjunction with existing deep IRAC data) Our goal is to measure with great accuracy the luminosity function at z~7 over a range of at least 3 magnitude, based on the identification of about 50 lensed galaxies at 6 5

WFC3/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

WFC3/UV 11556

Investigations of the Pluto System

We propose a set of high SNR observations of the Pluto system that will provide improved lightcurves, orbits, and photometric properties of Nix and Hydra The key photometric result for Nix and Hydra will be a vastly improved lightcurve shape and rotation period to test if the objects are in synchronous rotation or not A second goal of this program will be to retrieve a new epoch of albedo map for the surface of Pluto These observations will also improve masses and in some case densities for the bodies in the Pluto system

============================================================================== TOPIC: Daily Report #5146

http://groups google com/group/sci astro hubble/t/a123696c310ecc61?hl=en

== 1 of 1 == Date: Tues, Jul 27 2010 5:11Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5146

PERIOD COVERED: 5am July 26 - 5am July 27, 2010 (DOY 207/09:00z-208/09:00z)

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 8 8 FGS REAcq 9 9 OBAD with Maneuver 5 5

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

ACS/WFC 11996

CCD Daily Monitor (Part 3)

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/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

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

STIS/CC 11845

CCD Dark Monitor Part 2

Monitor the darks for the STIS CCD

STIS/CC 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 11721

Verifying the Utility of Type Ia Supernovae as Cosmological Probes: Evolution and Dispersion in the Ultraviolet Spectra

The study of distant type Ia supernova (SNe Ia) offers the most practical and immediate discriminator between popular models of dark energy Yet fundamental questions remain over possible redshift-dependent trends in their observed and intrinsic properties High-quality Keck spectroscopy of a representative sample of 36 intermediate redshift SNe Ia has revealed a surprising, and unexplained, diversity in their rest-frame UV fluxes One possible explanation is hitherto undiscovered variations in the progenitor metallicity Unfortunately, this result cannot be compared to local UV data as only two representative SNe Ia have been studied near maximum light Taking advantage of two new `rolling searches' and the restoration of STIS, we propose a non-disruptive TOO campaign to create an equivalent comparison local sample This will allow us to address possible evolution in the mean UV spectrum and its diversity, an essential precursor to the study of SNe beyond z~1

STIS/CCD 11852

STIS CCD Spectroscopic Flats C17

The purpose of this proposal is to obtain pixel-to-pixel lamp flat fields for the STIS CCD in spectroscopic mode

WFC3/UV/ACS/WFC/IR 12055

A Panchromatic Hubble Andromeda Treasury - I

WFC3/UVIS 11707

Detecting Isolated Black Holes through Astrometric Microlensing

This proposal aims to make the first detection of isolated stellar-mass black holes (BHs) in the Milky Way, and to determine their masses Until now, the only directly measured BH masses have come from radial-velocity measurements of X-ray binaries Our proposed method uses the astrometric shifts that occur when a galactic-bulge microlensing event is caused by a BH lens Out of the hundreds of bulge microlensing events found annually by the OGLE and MOA surveys, a few are found to have very long durations (>200 days) It is generally believed that the majority of these long-duration events are caused by lenses that are isolated BHs

To test this hypothesis, we will carry out high-precision astrometry of 5 long-duration events, using the ACS/HRC camera The expected astrometric signal from a BH lens is >1 4 mas, at least 7 times the demonstrated astrometric precision attainable with the HRC

This proposal will thus potentially lead to the first unambiguous detection of isolated stellar-mass BHs, and the first direct mass measurement for isolated stellar-mass BHs through any technique Detection of several BHs will provide information on the frequency of BHs in the galaxy, with implications for the slope of the IMF at high masses, the minimum mass of progenitors that produce BHs, and constraints on theoretical models of BH formation

WFC3/UVIS 11903

UVIS Photometric Zero Points

This proposal obtains the photometric zero points in 53 of the 62 UVIS/WFC3 filters: the 18 broad-band filters, 8 medium-band filters, 16 narrow-band filters, and 11 of the 20 quad filters (those being used in cycle 17) The observations will be primary obtained by observing the hot DA white dwarf standards GD153 and G191-B2B A redder secondary standard, P330E, will be observed in a subset of the filters to provide color corrections Repeat observations in 16 of the most widely used cycle 17 filters will be obtained once per month for the first three months, and then once every second month for the duration of cycle 17, alternating and depending on target availability These observations will enable monitoring of the stability of the photometric system Photometric transformation equations will be calculated by comparing the photometry of stars in two globular clusters, 47 Tuc and NGC 2419, to previous measurements with other telescopes/instruments

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

============================================================================== TOPIC: Daily Report #5147

http://groups google com/group/sci astro hubble/t/2fc8eddc01b07a60?hl=en

== 1 of 1 == Date: Wed, Jul 28 2010 8:12Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5147

PERIOD COVERED: 5am July 27 - 5am July 28, 2010 (DOY 208/09:00z-209/09:00z)

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

12342 - REAcq(2,1,1) at 209/06:54:02z resulted in a "scan step limit exceeded" error in FGS2 on the first attempt The REAcq went on to succeed on the second attempt

Observations possibly affected WFC 73-75, Proposal ID#11700; COS 45, Proposal ID#11598

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

                  SCHEDULED SUCCESSFUL

FGS GSAcq 7 7 FGS REAcq 8 8 OBAD with Maneuver 4 4

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

COS/NUV/FUV 11598

How Galaxies Acquire their Gas: A Map of Multiphase Accretion and Feedback in Gaseous Galaxy Halos

We propose to address two of the biggest open questions in galaxy formation - how galaxies acquire their gas and how they return it to the IGM - with a concentrated COS survey of diffuse multiphase gas in the halos of SDSS galaxies at z = 0 15 - 0 35 Our chief science goal is to establish a basic set of observational facts about the physical state, metallicity, and kinematics of halo gas, including the sky covering fraction of hot and cold material, the metallicity of infall and outflow, and correlations with galaxy stellar mass, type, and color - all as a function of impact parameter from 10 - 150 kpc Theory suggests that the bimodality of galaxy colors, the shape of the luminosity function, and the mass-metallicity relation are all influenced at a fundamental level by accretion and feedback, yet these gas processes are poorly understood and cannot be predicted robustly from first principles We lack even a basic observational assessment of the multiphase gaseous content of galaxy halos on 100 kpc scales, and we do not know how these processes vary with galaxy properties This ignorance is presently one of the key impediments to understanding galaxy formation in general We propose to use the high-resolution gratings G130M and G160M on the Cosmic Origins Spectrograph to obtain sensitive column density measurements of a comprehensive suite of multiphase ions in the spectra of 43 z < 1 QSOs lying behind 43 galaxies selected from the Sloan Digital Sky Survey In aggregate, these sightlines will constitute a statistically sound map of the physical state and metallicity of gaseous halos, and subsets of the data with cuts on galaxy mass, color, and SFR will seek out predicted variations of gas properties with galaxy properties Our interpretation of these data will be aided by state-of-the-art hydrodynamic simulations of accretion and feedback, in turn providing information to refine and test such models We will also use Keck, MMT, and Magellan (as needed) to obtain optical spectra of the QSOs to measure cold gas with Mg II, and optical spectra of the galaxies to measure SFRs and to look for outflows In addition to our other science goals, these observations will help place the Milky Way's population of multiphase, accreting High Velocity Clouds (HVCs) into a global context by identifying analogous structures around other galaxies Our program is designed to make optimal use of the unique capabilities of COS to address our science goals and also generate a rich dataset of other absorption-line systems

ACS/WFC3 11670

The Host Environments of Type Ia Supernovae in the SDSS Survey

COS/NUV/S/C/FUV 12082

Extending COS/G130M Coverage Down to 905A With Two New Central Wavelengths

These exploratory observations will provide sensitivity, wavelength range, and resolution measurements for two new COS FUV G130M central wavelength settings These new settings will extend COS/G130M coverage down to 905? in two new bandpasses; 1021-1171? (BLUE) and 905-1055? (Ultra-BLUE) The modes are chosen to provide continuous coverage from 905? to the existing coverage in the G130M/1291? setting with approximately 30? of overlap in each mode for cross-calibration purposes No focus adjustments will be made for these settings, as this is deemed an unnecessary risk to COS

These new modes have the potential to provide greater than FUSE sensitivity at moderate (3, 000-5, 000) resolution

Three WD targets are defined;

1) GD50 (GSC-04717-00588; a well observed standard WD) 2) WD0320-539 (GSC-08493-00891, one of the targets used in exploring the G140L sensitivity), 3) REJ0503-289 (WD-5001-289 = GSC-04717-00588, a hot EUVE bright WD)

But only target 2) is used at this time

In the observations section, G130M/1291A is a placeholder for the BLUE and Super-BLUE settings

STIS/CC 11845

CCD Dark Monitor Part 2

Monitor the darks for the STIS CCD

STIS/CC 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 11933

IR Rate Dependent Non-linearity

WFC3/IR/S/C 11929

IR Dark Current Monitor

WFC3/UV/ACS/WFC/IR 12055

A Panchromatic Hubble Andromeda Treasury - I

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

WFC3/UVIS/IR 11700

Bright Galaxies at z>7 5 with a WFC3 Pure Parallel Survey

The epoch of reionization represents a special moment in the history of the Universe as it is during this era that the first galaxies and star clusters are formed Reionization also profoundly affects the environment where subsequent generations of galaxies evolve Our overarching goal is to test the hypothesis that galaxies are responsible for reionizing neutral hydrogen To do so we propose to carry out a pure parallel WFC3 survey to constrain the bright end of the redshift z>7 5 galaxy luminosity function on a total area of 176 arcmin^2 of sky Extrapolating the evolution of the luminosity function from z~6, we expect to detect about 20 Lyman Break Galaxies brighter than M_* at z~8 significantly improving the current sample of only a few galaxies known at these redshifts Finding significantly fewer objects than predicted on the basis of extrapolation from z=6 would set strong limits to the brightness of M_*, highlighting a fast evolution of the luminosity function with the possible implication that galaxies alone cannot reionize the Universe Our observations will find the best candidates for spectroscopic confirmation, that is bright z>7 5 objects, which would be missed by small area deeper surveys The random pointing nature of the program is ideal to beat cosmic variance, especially severe for luminous massive galaxies, which are strongly clustered In fact our survey geometry of 38 independent fields will constrain the luminosity function like a contiguous single field survey with two times more area at the same depth Lyman Break Galaxies at z>7 5 down to m_AB=26 85 (5 sigma) in F125W will be selected as F098M dropouts, using three to five orbits visits that include a total of four filters (F606W, F098M, F125W, F160W) optimized to remove low-redshift interlopers and cool stars Our data will be highly complementary to a deep field search for high- z galaxies aimed at probing the faint end of the luminosity function, allowing us to disentangle the degeneracy between faint end slope and M_* in a Schechter function fit of the luminosity function We waive proprietary rights for the data In addition, we commit to release the coordinates and properties of our z>7 5 candidates within one month from the acquisition of each field

============================================================================== TOPIC: Daily Report #5148

http://groups google com/group/sci astro hubble/t/50d3896ddb20a7ed?hl=en

== 1 of 1 == Date: Thurs, Jul 29 2010 8:31Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5148

PERIOD COVERED: 5am July 28 - 5am July 29, 2010 (DOY 209/09:00z-210/09:00z)

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 6 6 FGS REAcq 8 8 OBAD with Maneuver 3 3

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

ACS/WFC 11996

CCD Daily Monitor (Part 3)

COS/NUV/FUV 11598

How Galaxies Acquire their Gas: A Map of Multiphase Accretion and Feedback in Gaseous Galaxy Halos

COS/NUV/FUV 11728

The Impact of Starbursts on the Gaseous Halos of Galaxies

Perhaps the most important (yet uncertain) aspects of galaxy evolution are the processes by which galaxies accrete gas and by which the resulting star formation and black hole growth affects this accreting gas It is believed that both the form of the accretion and the nature of the feedback change as a function of the galaxy mass At low mass the gas comes in cold and the feedback is provided by massive stars At high mass, the gas comes in hot, and the feedback is from an AGN The changeover occurs near the mass where the galaxy population transitions from star-forming galaxies to red and dead ones The population of red and dead galaxies is building with cosmic time, and it is believed that feedback plays an important role in this process: shutting down star formation by heating and/or expelling the reservoir of cold halo gas To investigate these ideas, we propose to use COS far-UV spectra of background QSOs to measure the properties of the halo gas in a sample of galaxies near the transition mass that have undergone starbursts within the past 100 Myr to 1 Gyr The galactic wind associated with the starburst is predicted to have affected the properties of the gaseous halo To test this, we will compare the properties of the halos of the post-starburst galaxies to those of a control sample of galaxies matched in mass and QSO impact parameter Do the halos of the post-starburst galaxies show a higher incidence rate of Ly-Alpha and metal absorption-lines? Are the kinematics of the halo gas more disturbed in the post-starbursts? Has the wind affected the ionization state and/or the metallicity of the halo? These data will provide fresh new insights into the role of feedback from massive stars on the evolution of galaxies, and may also offer clues about the properties of the QSO metal absorption-line systems at high-redshift

COS/NUV/FUV 12086

Generation of 1-D Fixed Pattern Templates

Tests have shown that application of a 1-D fixed pattern template to a COS spectrum can reduce the fixed pattern noise in G130M or G160M spectra to an equivalent S/N of about 30/1 For this to be occur, the template must be derived from data for the same grating and nearly the same central wavelength as the observation This is because each grating has a different cross dispersion profile, and different central wavelengths fall at different cross dispersion detector locations As a result, spectra obtained at each grating and central wavelength setting are derived from different regions of the detectors -- each with their own, unique detector features and grid wire shadows

STIS/CC 11845

CCD Dark Monitor Part 2

Monitor the darks for the STIS CCD

STIS/CC 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 11696

Infrared Survey of Star Formation Across Cosmic Time

We propose to use the unique power of WFC3 slitless spectroscopy to measure the evolution of cosmic star formation from the end of the reionization epoch at z>6 to the close of the galaxy- building era at z~0 3 Pure parallel observations with the grisms have proven to be efficient for identifying line emission from galaxies across a broad range of redshifts The G102 grism on WFC3 was designed to extend this capability to search for Ly-alpha emission from the first galaxies Using up to 250 orbits of pure parallel WFC3 spectroscopy, we will observe about 40 deep (4-5 orbit) fields with the combination of G102 and G141, and about 20 shallow (2-3 orbit) fields with G141 alone

Our primary science goals at the highest redshifts are: (1) Detect Lya in ~100 galaxies with z>5 6 and measure the evolution of the Lya luminosity function, independent of of cosmic variance; 2) Determine the connection between emission line selected and continuum-break selected galaxies at these high redshifts, and 3) Search for the proposed signature of neutral hydrogen absorption at re-ionization At intermediate redshifts we will (4) Detect more than 1000 galaxies in Halpha at 0 5

To identify single-line Lya emitters, we will exploit the wide 0 8--1 9um wavelength coverage of the combined G102+G141 spectra All [OII] and [OIII] interlopers detected in G102 will be reliably separated from true LAEs by the detection of at least one strong line in the G141 spectrum, without the need for any ancillary data We waive all proprietary rights to our data and will make high-level data products available through the ST/ECF

WFC3/IR 11915

IR Internal Flat Fields

WFC3/UV/ACS/WFC/IR 12055

A Panchromatic Hubble Andromeda Treasury - I

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

WFC3/UVIS 11908

Cycle 17: UVIS Bowtie Monitor

WFC3/UVIS/IR 11700

Bright Galaxies at z>7 5 with a WFC3 Pure Parallel Survey

============================================================================== TOPIC: Daily Report #5149

http://groups google com/group/sci astro hubble/t/5f2c0a1cedfcb414?hl=en

== 1 of 1 == Date: Fri, Jul 30 2010 8:05Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5149

PERIOD COVERED: 5am July 29 - 5am July 30, 2010 (DOY 210/09:00z-211/09:00z)

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 9 9 FGS REAcq 6 6 OBAD with Maneuver 6 6

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

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

COS/NUV/FUV 12086

Generation of 1-D Fixed Pattern Templates

STIS/CC 11845

CCD Dark Monitor Part 2

Monitor the darks for the STIS CCD

STIS/CC 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

STS/MA/CC 12085

STIS/E230M Observations of HD6655 for Calibration of COS/G230L

This program observes HD 6655, a radial velocity target that is used for calibrating COS/G230L The objective of this program is to get STIS data of this target, with the E230M grating, and then use this observations to derive the offsets between the internal and external COS/G230L wavelength scales

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

WFC3/IR/S/C 11929

IR Dark Current Monitor

WFC3/UV 11554

Luminosity Profiles of Extremely Massive Clusters in NGC 7252

The galactic merger remnant NGC 7252 represents one of the most extreme post-starburst environments in the local universe During the disk-disk merger (~400 Myr ago) this galaxy produced the largest young massive star cluster population known, including two clusters above 10^7 Msun, a factor of 100 more massive than typical globular clusters in the Milky Way We propose ACS-HRC observations of 3 fields in NGC 7252 in order to explore the detailed properties, i e luminosity profiles, of these massive star clusters These observations will be able to test massive cluster formation mechanisms (e g the cluster merger scenario) as well as the possible tidal erosion and truncation of the outer regions of the clusters by the galactic tidal field These observations will compliment our large on-going study using archival HST data, of star cluster profiles outside the Local Group The cluster population in NGC 7252 will extend our sample in cluster mass by an order of magnitude

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

WFC3/UVIS 11908

Cycle 17: UVIS Bowtie Monitor

WFC3/UVIS/IR 11644

A Dynamical-Compositional Survey of the Kuiper Belt: A New Window Into the Formation of the Outer Solar System

============================================================================== TOPIC: Daily Report #5150

http://groups google com/group/sci astro hubble/t/63552440e21bba54?hl=en

== 1 of 1 == Date: Mon, Aug 2 2010 8:30Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5150

PERIOD COVERED: 5am July 30 - 5am August 2, 2010 (DOY 211/09:00z-214/09:00z)

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

12344 - At 213/18:01:57z a COS Dump Timeout Error was received The timeout error occurred during the instrument dump to the SSR This error is received when the timeout alarm at the end of an instrument dump has expired, meaning the dump did not complete in the expected amount of time

Observation possibly affected COS 212, proposal ID# 12086

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

                   SCHEDULED SUCCESSFUL

FGS GSAcq 15 15 FGS REAcq 31 31 OBAD with Maneuver 13 13

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

COS/NUV/FUV 12086

Generation of 1-D Fixed Pattern Templates

S/C 12046

COS FUV DCE Memory Dump

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)

WFC3/IR/S/C 11929

IR Dark Current Monitor

WFC3/UVIS 11924

WFC3/UVIS External and Internal CTE Monitor

CCD detector Charge Transfer Inefficiency (CTI)-induced losses in photometry and astrometry will be measured using observations of the rich open cluster NGC6791 and with the EPER (Extended Pixel Edge Response) method using tungsten lamp flat field exposures Although we do not expect to see CTE effects at the outset of Cycle 17, this CTE monitoring program is the first of a multi-cycle program to monitor and establish CTE-induced losses with time We expect to measure CTE effects with a precision comparable to the ACS measurements

WFC3/IR 11915

IR Internal Flat Fields

WFC3/UVIS 11908

Cycle 17: UVIS Bowtie Monitor

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

WFC3/UV 11904

UVIS Droplets

To characterize the effects of the contamination (i e , droplets) on the UVIS window, we will observe a star cluster in three wide band filters (F225W, F555W, and F814W) as well as a narrow band filter (F502N) and step the stars in the cluster across randomly located droplets The step size is 20 pixels, and we execute a five point line dither for each filter This should provide for observations both on and off the droplets, for the same star Internal flat fields are also obtained, but, due to the high f/# of the internal calibration system, the flats will be of limited utility, but will serve to map and crudely track any changes in the droplets The cluster needs to contain both hot and cool stars, and therefore we select NGC 6752, a nearby globular with a hot horizontal branch Note, although the total population of HB stars may be larger in systems such as NGC 2419, NGC 6715, and NGC 2808, those clusters are much further away and will not provide a high density of stars over the global image (the droplets are located over the entire frame) There will be three visits (initial, 7 days later, and 30 days later), with each visit requiring 4 orbits The total program thus requires 12 orbits total

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

WFC3/ACS 11888

ACS Internal Flat Fields

The stability of the CCD flat fields will be monitored using the calibration lamps and a sub-sample of the filter set High signal observations will be used to assess the stability of the pixel-to-pixel flat field structure and to monitor the position of the dust motes

STIS/CC 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/CC 11845

CCD Dark Monitor Part 2

Monitor the darks for the STIS CCD

COS/NUV/FUV 11741

Probing Warm-Hot Intergalactic Gas at 0 5 < z < 1 3 with a Blind Survey for O VI, Ne VIII, Mg X, and Si XII Absorption Systems

Currently we can only account for half of the baryons (or less) expected to be found in the nearby universe based on D/H and CMB observations This "missing baryons problem" is one of the highest-priority challenges in observational extragalatic astronomy Cosmological simulations suggest that the baryons are hidden in low-density, shock-heated intergalactic gas in the log T = 5 - 7 range, but intensive UV and X-ray surveys using O VI, O VII, and O VIII absorption lines have not yet confirmed this prediction We propose to use COS to carry out a sensitive survey for Ne VIII and Mg X absorption in the spectra of nine QSOs at z(QSO) > 0 89 For the three highest-redshift QSOs, we will also search for Si XII This survey will provide more robust constraints on the quantity of baryons in warm-hot intergalactic gas at 0 5 < z < 1 3, and the data will provide rich constraints on the metal enrichment, physical conditions, and nature of a wide variety of QSO absorbers in addition to the warm-hot systems By comparing the results to other surveys at lower redshifts (with STIS, FUSE, and from the COS GTO programs), the project will also enable the first study of how these absorbers evolve with redshift at z < 1 By combining the program with follow-up galaxy redshift surveys, we will also push the study of galaxy-absorber relationships to higher redshifts, with an emphasis on the distribution of the WHIM with respect to the large-scale matter distribution of the universe

WFC3/UV/IR 11709

Stretching the Diversity of Cosmic Explosions: The Supernovae of Gamma-ray Bursts

While the association between gamma-ray bursts (GRBs) and massive stars is robust, there is a large diversity of properties among supernovae (SNe) associated with GRBs The converse is also true: Several recent events show that there is a large brightness range among high energy transients associated with SNe As part of a comprehensive program, we propose to use HST in order to search for and characterize the SNe associated with GRB

HST offers the means to cleanly separate the light curve of the GRB afterglow from the supernova, and to remove the contamination from the host galaxy, opening a clear path to the fundamental parameters of the SN, and thence to the progenitor From these observations, we will determine the absolute magnitude at maximum, the shape of the spectral energy distribution, and any change over time of the energy distribution We will also measure the rate of decay of the exponential tail

Merged with the ground-based data that we will obtain for each event, we will be able to compare our data set to models and constrain the energy of the explosion, the mass of the ejecta and the mass of Nickel synthesized during the explosion These results will shed light on the apparent variety of supernovae associated with gamma-ray bursts and X-ray flashes, and on the relation between these SNe and other, more common, types of core-collapse explosions

WFC3/UVIS/IR 11700

Bright Galaxies at z>7 5 with a WFC3 Pure Parallel Survey

WFC3/IR 11696

Infrared Survey of Star Formation Across Cosmic Time

COS/NUV/FUV/STIS/CCD/ 11692 MA1 The LMC as a QSO Absorption Line System

We propose to obtain high resolution, high signal-to-noise observations of QSOs behind the Large Magellanic Clouds These QSOs are situated beyond the star forming disk of the galaxy, giving us the opportunity to study the distribution of metals and energy in regions lacking significant star formation In particular, we will derive the metallicities and study the ionization characteristics of LMC gas at impact parameters 3-17 kpc We will compare our results with high-z QSO absorption line systems

ACS/WFC/WFC3/UV/IR 11691

Using Massive Star Clusters in Merger Remnants To Provide Reference Colors of Intermediate- Age Stellar Populations

Much current research in cosmology and galaxy formation relies on an accurate interpretation of colors of galaxies in terms of their evolutionary state, i e , in terms of ages and metallicities One particularly important topic is the ability to identify early-type galaxies at "intermediate" ages (~ 500 Myr - 5 Gyr), i e , the period between the end of star formation and ~ half the age of the universe Currently, integrated-light studies must rely on population synthesis models which rest upon spectral libraries of stars in the solar neighborhood These models have a difficult time correctly incorporating short-lived evolutionary phases such as thermally pulsing AGB stars, which produce up to 80% of the flux in the near-IR in this age range Furthermore, intermediate-age star clusters in the Local Group do not represent proper templates against which to calibrate population synthesis models in this age range, because their masses are too low to render the effect of stochastic fluctuations due to the number of bright RGB and AGB stars negligible As a consequence, current population synthesis models have trouble reconciling the evolutionary state of high-redshift galaxies from optical versus near-IR colors We propose a simple and effective solution to this issue, namely obtaining high-quality EMPIRICAL colors of massive globular clusters in galaxy merger remnants which span this important age range These colors should serve as relevant references, both to identify intermediate-age objects in the local and distant universe and as calibrators for population synthesis modellers

WFC3/UVIS 11675

Stellar Forensics: A Post-Explosion View of the Progenitors of Core-Collapse Supernovae

Recent studies have used high spatial resolution HST observations of SN sites to identify the progenitors of core-collapse SNe on pre-explosion images These studies have set constraints about the nature of massive stars and their evolution just prior to their explosion as SNe Now, at late-times when the SNe have faded sufficiently, it is possible to return to the sites of these core-collapse SNe to search for clues about the nature of their progenitors We request time to conduct deep, late-time, high-resolution imaging with ACS/HRC of the sites of six core-collapse SNe In this program we aim to: 1) confirm our identifications, that were made with HST pre- explosion images, of the red supergiant progenitors of four Type IIP SNe (1999ev, 2003gd, 2004A and 2005cs), by observing if the objects identified as the progenitors are now missing; 2) place precise constraints on the progenitor of the Type Ic SN 2007gr by studying its host cluster; and 3) confirm our identification of an LBV-like outburst of an unstable WR star as belonging to the progenitor of a Type Ib-n core-collapse SN (2006jc), using broad and narrow- band imaging to search for emission line stars in its locality The deep imaging will also allow to probe the stellar populations in the immediate vicinities of these SNe, that were previously obscured by the progenitors and the bright SNe HST provides the unique combination of high- resolution optical imaging at very faint magnitudes that will facilitate this study

COS/NUV/FUV 11598

How Galaxies Acquire their Gas: A Map of Multiphase Accretion and Feedback in Gaseous Galaxy Halos

WFC3/UVIS 11588

Galaxy-Scale Strong Lenses from the CFHTLS Survey

We aim to investigate the origin and evolution of early-type galaxies using gravitational lensing, modeling the mass profiles of objects over a wide range of redshifts The low redshift (z = 0 2) sample is already in place following the successful HST SLACS survey; we now propose to build up and analyze a sample of comparable size (~50 systems) at high redshift (0 4 < z < 0 9) using HST WFC3 Snapshot observations of lens systems identified by the SL2S collaboration in the CFHT legacy survey

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

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