Date: July 9th 2010

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

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Today's topics:

Daily Report #5124 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/4532b1d5c0f6bc7b?hl=en
Daily Report #5127 (Corrected Copy) - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/88a0865506c45304?hl=en
Daily Report #5128 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/3187178a9d006d8e?hl=en
Daily Report #5129 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/58a94e99b9164f52?hl=en
Daily Rpt #5130 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/9c29de6a00b14599?hl=en
Daily Report #5131 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/281257e189d3364f?hl=en
Daily Report #5132 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/307376947064247e?hl=en
Daily Report #5133 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/ea6bde3c325bdc49?hl=en

============================================================================== TOPIC: Daily Report #5124

http://groups google com/group/sci astro hubble/t/4532b1d5c0f6bc7b?hl=en

== 1 of 1 == Date: Thurs, Jun 24 2010 6:57Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5124

PERIOD COVERED: 5am June 23 - 5am June 24, 2010 (DOY 174/09:00z-175/09:00z)

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 9 9 OBAD with Maneuver 6 6

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

ACS/WFC 11655

Dynamics of the Galactic Bulge/bar

We request second-epoch ACS observations of four star fields in the Galactic bar These will allow us to measure proper motions for tens of thousands of stars well below the turnoff, to construct a dynamical model for the bulge/bar (in combination with data already in hand from other HST fields, and from VLT spectroscopy), and hence to take a unique look at the internal dynamical structure of the central regions of our Galaxy By relating the kinematics with stellar population we can elucidate the formation history of the bulge and bar, and their relation to the surrounding Galactic disk This is a resubmission of an approved Cycle 15 proposal that was hit by the ACS malfunction

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

COS/FUV 11541

COS-GTO: Cool, Warm, and Hot Gas in the Cosmic Web and in Galaxy Halos

COS G130M and G160M 20, 000 resolution observations will be obtained for 17 QSOs to study cool, warm and hot gas in the cosmic web and in galaxy halos 5 QSOs with z from 0 177 to 0 574 and sum z = 1 68 will be observed with S/N = 40-50 per resolution element 12 QSOs with z = 0 286 to 0 669 and sum z = 5 57 will be observed with S/N = 30-40 The observations will allow a wide range of IGM studies including determining the frequency of occurrence of the different types of absorption systems detected, along with studies of the physical conditions and elemental abundances in the different systems Special emphasis will be given to a study of the properties of highly ionized IGM as traced by O VI, O V, O IV, N V, and C IV The high S/N of the observations will allow a search for broad Lyman alpha absorption and weak metal line absorption that can be crucial for the evaluation of physical conditions and elemental abundances Supporting ground based observations will allow studies of the association of the absorbers with galaxy structures along the 17 lines of sight The overall goal of the program will be to obtain the information that will allow an assessment of the baryonic content of the IGM as revealed by UV and EUV absorption lines seen in the spectra of QSOs

COS/NUV/FUV 11698

The Structure and Dynamics of Virgo's Multi-Phase Intracluster Medium

The dynamical flows of the intracluster medium (ICM) are largely unknown We propose to map the spatial and kinematic distribution of the warm ICM of the nearby Virgo cluster using the Cosmic Origins Spectrograph 15 sightlines at a range of impact parameters within the virial radius of the cluster (0 2 - 1 7 Mpc) will be probed for Lyman-alpha absorption and the data compared to blind HI, dust and x-ray surveys to create a multi-phase map of the cluster's ICM Absorption line sightlines are commonly 40-100 kpc from a galaxy, allowing the flow of baryons between galaxies and the ICM to be assessed The velocity distribution of the absorbers will be directly compared to simulations and used to constrain the turbulent motions of the ICM This proposal will result in the first map of a cluster's warm ICM and provide important tests for our theoretical understanding of cluster formation and the treatment of gas cooling in cosmological simulations

STIS/CC 11693

Follow-up Observations of Debris Disks around Two Solar-Type Stars

Circumstellar debris disks offer direct views into the structure of extrasolar planetary systems Their constituent dust, seen in scattered light and thermal emission, is created by the collisions of asteroidal and cometary parent bodies The distribution of this dust provides information on the location of the parent bodies, and can be strongly affected by planetary perturbations Dynamical signatures of planets can include asymmetries, warps, central clearings, and radial gaps in a disk, and thus are key features to search for in resolved images Following up recent Spitzer measurements, we have now detected two new, nearby debris disks in scattered light Our initial ACS F606W coronagraphic images show faint ringlike structures around the solar-type stars HD 10647 (F9V) and HD 207129 (G0V); both are also spatially resolved in Spitzer/MIPS 70 micron images The HD 10647 disk, seen close to edge-on, represents the first disk ever imaged in scattered light around a star known to have a radial velocity planet The inclined ring around HD 207129 is the faintest disk ever imaged in scattered light, and seems in the MIPS image to be asymmetric like the eccentric ring around Fomalhaut We propose to obtain deep ACS coronagraphic images of these two disks Our goals are to get definitive measurements of the dust spatial distributions (including disk asymmetries and sharpness of the ring edges), and measure the overall F606W-F814W color of each disk in order to constrain the dust properties The results will be a definitive exploration of the Kuiper belts of two nearby, Sun-like stars NOTE: HD 207129 was deleted from this program

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/MA1/MA2 11860

MAMA Spectroscopic Sensitivity and Focus Monitor

The purpose of this proposal is to monitor the sensitivity of each MAMA grating mode to detect any change due to contamination or other causes, and to also monitor the STIS focus in a spectroscopic and an imaging mode

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/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/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/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 #5127 (Corrected Copy)

http://groups google com/group/sci astro hubble/t/88a0865506c45304?hl=en

== 1 of 1 == Date: Tues, Jun 29 2010 9:41Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5127

PERIOD COVERED: 5am June 28 - 5am June 29, 2010 (DOY 179/09:00z-180/09:00z)

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

12314 - GSAcq(2,1,1) @179/20:48:02z and REAcqs(2,1,1) @179/22:23:59z and 179/23:59:50z failed to RGA Hold due to search radius limit exceeded on FGS2 REAcq(2,1,1) @180/01:35:40z was successful

Observations affected: COS #8-11 Proposal ID#11705, WFC3 #70-77 Proposal ID#11696, STIS #14-16 Proposal #11847 and WFC3 #78-79 Proposal #11905

COMPLETED OPS REQUEST:

18568-1 - LBBIAS Updates for Extended Gyro Guiding Intervals @ 179/21:36z, & 180/00:49z

COMPLETED OPS NOTES: (None)

                   SCHEDULED SUCCESSFUL

FGS GSAcq 5 4 FGS REAcq 9 7 OBAD with Maneuver 4 4

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/NUV 11705

Physical Properties of Quasar Outflows: From BALs to Mini-BALs

Accretion disk outflows are important components of quasar environments They might play a major role in facilitating accretion, regulating star formation in the host galaxies and distributing metals to the surrounding gas They reveal themselves most conspicuously via broad absorption lines (BALs), but they appear even more frequently in other guises such as the weaker and narrower "mini-BALs " How are these diverse outflow features related? Are mini-BALs really just "mini" versions of the BALs, or do they represent a fundamentally different type of outflow, with different degrees of ionization, column densities, mass loss rates, physical origins, etc ?

We propose HST-COS spectroscopy to make the first quantitative assessment of the outflow physical conditions across the full range of weak/narrow mini-BALs to strong/broad BALs Our strategy is to measure key diagnostic lines (SVI, OVI, CIII, SIV, PV, etc ) at 930A - 1130A (rest- frame) in a sample of 7 outflow quasars with known mini-BALs through weak BALs We will then 1) combine the COS data with ground-based spectra of the same quasars to include more lines (CIV, SiIV) at longer wavelengths, and 2) include in our analysis a nearly identical UV/optical dataset obtained previously for a sample of quasars with strong BALs Our study of this combined dataset will be an essential next step toward a more global understanding of quasar outflows

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

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 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

STIS/CCD/FGS 11848

CCD Read Noise Monitor

This proposal measures the read noise of all the amplifiers (A, B, C, D) on the STIS CCD using pairs of bias frames Full-frame and binned observations are made in both Gain 1 and Gain 4, with binning factors of 1x1, 1x2, 2x1, and 2x2 All exposures are internals Pairs of visits are scheduled monthly for the first four months and then bi-monthly after that

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/UV 12243

Determining the Size and Shape of Dwarf Planet Haumea from a Mutual Event

The history of Haumea is closely intertwined with several unanswered questions relating to the formation and evolution of the outer solar system Understanding Haumea and its satellites gives us unique insights on the physics of KBO collisions, tides, surfaces, and interiors Yet, the most important physical properties of this dwarf planet, its density and shape, remain only weakly constrained by degenerate light curve inversions The existence of mutual events between Haumea and its inner satellite, Namaka, provide a rare opportunity to measure Haumea's size, shape, density, albedo, and spin orientation with HST photometry These observations also constrain the size of Namaka, the orbits of both satellites, and, through resolved photometry, the totally unexpected rapid rotation of the outer satellite, Hi'iaka After extensive attempts at ground-based observations, it is clear that only HST photometry is capable of securely observing and characterizing a Haumea-Namaka mutual event The proposed observations will observe the ~5-hour transit and shadowing of Haumea by Namaka on June 28, 2010 with high signal-to-noise using straightforward photometric observations with WFC3

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/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

============================================================================== TOPIC: Daily Report #5128

http://groups google com/group/sci astro hubble/t/3187178a9d006d8e?hl=en

== 1 of 1 == Date: Wed, Jun 30 2010 8:41Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5128

PERIOD COVERED: 5am June 29 - 5am June 30, 2010 (DOY 180/09:00z-181/09:00z)

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

FOR DOY 165

12315 - GSAcq(1,2,1) at 165/05:17:55z required two attempts to achieve FL-DV on FGS1 The initial attempt resulted in scan step limit exceeded The acq was successful

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

                  SCHEDULED SUCCESSFUL

FGS GSAcq 6 6 FGS REAcq 8 8 OBAD with Maneuver 4 4

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

ACS/SBC 11886

UV Contamination Monitor

The observations consist of imaging and spectroscopy with SBC and HRC of the cluster NGC 6681 in order to monitor the temporal evolution of the UV sensitivity of the SBC and the HRC

COS/NUV 11705

Physical Properties of Quasar Outflows: From BALs to Mini-BALs

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/ACS/UVIS 11684

The First Proper Motion Measurement for M31: Dynamics and Mass of the Local Group

We will perform observations to determine the proper motion of the Andromeda galaxy M31, which has been sought for almost a century without success While challenging, this measurement has now become possible due to the availability of existing deep ACS/WFC images of several M31 fields The requested second epoch images will yield the average shift of the M31 stars with respect to compact galaxies in the background Our observing strategy uses six different fields (three primary and three coordinated parallel) with two different instruments (ACS and WFC3) to provide a maximum handle on possible systematic effects The expected result will be sufficiently accurate to: (a) discriminate between different histories for the dynamics of the Local Group; (b) constrain the mass distribution of the Local Group; (c) determine the details of the expected future merger between M31 and the Milky Way; (d) infer the past interaction history between M31 and M33; (e) constrain the internal proper motion kinematics of the M31 spheroid, outer disk, and tidal stream; and (f) obtain a pilot estimate of the M31 distance through the method of rotational parallax

WFC3/IR 11671

Kinematic Reconstruction of the Origin and IMF of the Massive Young Clusters at the Galactic Center

We propose to exploit the wide field capabilities of Wide Field Camera 3 to study star formation at the Galactic center By studying young stars located in the most physically extreme region of our Galaxy, we can test star formation theories, which suggest that such environments should favor high mass stars and, in extreme cases, should suppress star formation entirely Specifically, we will measure the proper motions and photometry of stars over the full extent of the three massive young clusters that have been identified at the Galactic Center (Arches, Quintuplet, and the Young Nuclear Star Cluster) These observations are a factor of ?2000 more efficient than what can be done with ground-based adaptive optics Our goals are two-fold First, we hope to establish the initial sites of star formation in order to obtain an accurate estimate of the conditions that led to the stellar populations within these clusters Answering this question for the Young Nuclear Star Cluster is particularly important as it establishes whether or not star formation can indeed proceed within 0 1 pc of our Galaxy?s supermassive black hole Second, we will measure the IMF in the Arches and Quintuplet, where dynamical evolution is less severe, using proper motions to determine membership and to reveal the tidal radius Probing how the properties of the emergent stellar populations within our Galaxy may be affected by the physical environment in which they arise is an important first step to understanding how they might vary as a function of cosmic time and thereby affect our models of galaxy formation and evolution

WFC3/IR 11696

Infrared Survey of Star Formation Across Cosmic Time

WFC3/IR/S/C 11929

IR Dark Current Monitor

WFC3/UVIS 11630

Monitoring Active Atmospheres on Uranus and Neptune

We propose Snapshot observations of Uranus and Neptune to monitor changes in their atmospheres on time scales of weeks and months, as we have been doing for the past seven years Previous Hubble Space Telescope observations (including previous Snapshot programs 8634, 10170, 10534, and 11156), together with near-IR images obtained using adaptive optics on the Keck Telescope, reveal both planets to be dynamic worlds which change on time scales ranging from hours to (terrestrial) years Uranus equinox occurred in December 2007, and the northern hemisphere is becoming fully visible for the first time since the early 1960s HST observations during the past several years (Hammel et al 2005, Icarus 175, 284 and references therein) have revealed strongly wavelength-dependent latitudinal structure, the presence of numerous visible-wavelength cloud features in the northern hemisphere, at least one very long- lived discrete cloud in the southern hemisphere, and in 2006 the first clearly defined dark spot seen on Uranus Long term ground-based observations (Lockwood and Jerzekiewicz, 2006, Icarus 180, 442; Hammel and Lockwood 2007, Icarus 186, 291) reveal seasonal brightness changes that seem to demand the appearance of a bright northern polar cap within the next few years Recent HST and Keck observations of Neptune (Sromovsky et al 2003, Icarus 163, 256 and references therein) show a general increase in activity at south temperate latitudes until 2004, when Neptune returned to a rather Voyager-like appearance with discrete bright spots rather than active latitude bands Further Snapshot observations of these two dynamic planets will elucidate the nature of long-term changes in their zonal atmospheric bands and clarify the processes of formation, evolution, and dissipation of discrete albedo features

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

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 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 #5129

http://groups google com/group/sci astro hubble/t/58a94e99b9164f52?hl=en

== 1 of 1 == Date: Thurs, Jul 1 2010 8:09Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5129

PERIOD COVERED: 5am June 30 - 5am July 1, 2010 (DOY 181/09:00z-182/09:00z)

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

12319 - REAcq(1,2,1) scheduled at 181/19:43:29z - 19:47:55z required three attempts to achieve FL-DV on FGS-2 The acquisition was successful

Observations possibly affected: ACS 34, 35, Proposal ID#11669

FOR DOY 172

12317 - GSAcq(2,1,1) at 172/14:53:57z required two attempts to achieve CT-DV on FGS2 The acquisition was successful

FOR DOY 178

12318 - GSAcq(2,1,1) at 178/21:01:47z required two attempts to maintain lock The second attempt was successful

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

                  SCHEDULED SUCCESSFUL

FGS GSAcq 7 7 FGS REAcq 7 7 OBAD with Maneuver 3 3

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

ACS/WFC 11996

CCD Daily Monitor (Part 3)

ACS/WFC3 11669

The Origins of Short Gamma-Ray Bursts

During the past decade extraordinary progress has been made in determining the origin of long- duration gamma-ray bursts It has been conclusively shown that these objects derive from the deaths of massive stars Nonetheless, the origin of their observational cousins, short-duration gamma-ray bursts (SGRBs) remains a mystery While SGRBs are widely thought to result from the inspiral of compact binaries, this is a conjecture SGRBs have been found in elliptical galaxies, Abell Clusters, star-forming dwarfs and even an edge-on spiral Whether they primarily result from an old population, a young population, or rapid evolution of binaries in globular clusters remains open

Here we propose to employ two related sets of observations which may dramatically advance our understanding of short bursts The first is a variant of a technique that we pioneered and used to great effect in elucidating the origins of long-duration bursts We will examine a statistical sample of hosts and measure the degree to which SGRB locations trace the red or blue light of their hosts, and thus old or young stellar populations This will allow us to study the demographics of the SGRB population in a manner largely free of the distance dependent selection effects which have so far bedeviled this field In the second line of attack we will use two targets of opportunity to obtain extremely precise positions of up to two nearby bursts -- one on a star-forming galaxy and the other on a elliptical Observation of the star-formation galaxy could link at least some bursts directly to a young population; however, a discovery in later images of a globular cluster at the site of the explosion in an elliptical would provide revolutionary evidence that SGRBs are formed from compact binaries

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/ACS/IR 11597

Spectroscopy of IR-Selected Galaxy Clusters at 1 < z < 1 5

We propose to obtain WFC3 G141 and G102 slitless spectroscopy of galaxy clusters at 1 < z < 1 5 that were selected from the IRAC survey of the Bootes NDWFS field Our IRAC survey contains the largest sample of spectroscopically confirmed clusters at z > 1 The WFC3 grism data will measure H-alpha to determine SFR, and fit models to the low resolution continua to determine stellar population histories for the brighter cluster members, and redshifts for the red galaxies too faint for ground-based optical spectroscopy

WFC3/UV/ACS/WFC 11739

Multiple Stellar Generations in the Unique Globular Clusters NGC 6388 and NGC 6441

Over the last few years HST observations have resulted in one of the most exciting and unexpected developments in stellar population studies: the discovery of multiple generations of stars in several globular clusters The finding of multiple main sequences in the massive clusters NGC 2808 and Omega Centauri, and multiple subgiant branches in NGC 1851, M54, and NGC 6388 has challenged the long-held paradigm that globular clusters are simple stellar populations Even more surprising, given the spectroscopic and photometric constraints, the only viable explanation for the main sequence splitting appears to be Helium enrichment, up to an astonishingly high Y=0 4 The conditions under which certain globulars experience the formation of multiple stellar generations remain mysterious, and even more so the helium-enrichment phenomenon Such an enrichment has important implications for chemical-enrichment, star-formation, and stellar-evolution scenarios, in star clusters and likely elsewhere To properly constrain the multiple main sequence phenomenon, it is important to determine its extent among GCs: is it limited to Omega Cen and NGC2808, or is it more common? We propose deep WFC3 optical/IR imaging of NGC 6388 and 6441, the two globular clusters that are most likely to host multiple, helium-enriched populations Our simulations of WFC3 performance suggest that we will be able to detect even the main sequence splittings caused by small He differences (Delta Y <0 03)

WFC3/UVIS 11697

Proper Motion Survey of Classical and SDSS Local Group Dwarf Galaxies

Using the superior resolution of HST, we propose to continue our proper motion survey of Galactic dwarf galaxies The target galaxies include one classical dwarf, Leo II, and six that were recently identified in the Sloan Digital Sky Survey data: Bootes I, Canes Venatici I, Canes Venatici II, Coma Berenices, Leo IV, and Ursa Major II We will observe a total of 16 fields, each centered on a spectroscopically-confirmed QSO Using QSOs as standards of rest in measuring absolute proper motions has proven to be the most accurate and most efficient method HST is our only option to quickly determine the space motions of the SDSS dwarfs because suitable ground-based imaging is only a few years old and such data need several decades to produce a proper motion The two most distant galaxies in our sample will require time baselines of four years to achieve our goal of a 30-50 km/s uncertainty in the tangential velocity; given this and the finite lifetime of HST, it is imperative that first-epoch observations be taken in this cycle The SDSS dwarfs have dramatically lower surface brightnesses and luminosities than the classical dwarfs Proper motions are crucial for determining orbits of the galaxies and knowing the orbits will allow us to test theories for the formation and evolution of these galaxies and, more generally, for the formation of the Local Group

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

WFC3/UVIS 11911

UVIS L-Flats and Geometric Distortion

Multiple pointing observations of the globular cluster Omega Centauri (NGC 5139) will be used to measure the filter-dependent low frequency flat field (L-flat) corrections and stability for a key set of 10 broadband filters used by GO programs The selected filters are F225W, F275W, F336W, F390W, F438W, F555W, F606W, F775W, F814W and F850LP By measuring relative changes in brightness of a star over different portions of the detector, we will determine local variations in the UVIS detector response

The broad wavelength range covered by these observations will allow us to derive the L-flat correction for the remaining wide, medium and narrow-band UVIS filters The same data will also be used to determine and correct the geometric distortion that affects UVIS data The broad wavelength range covered by these observations will allow us to measure the geometric distortion dependence with wavelength and filters and to provide the most appropriate correction over the entire wavelength range provided by UVIS

WFC3/UVIS/IR 11662

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

WFC3/UVIS/IR 11700

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

============================================================================== TOPIC: Daily Rpt #5130

http://groups google com/group/sci astro hubble/t/9c29de6a00b14599?hl=en

== 1 of 1 == Date: Fri, Jul 2 2010 9:05Ã‚Â am From: "Bassford, Lynn"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5130

PERIOD COVERED: 5am July 1 - 5am July 2, 2010 (DOY 182/09:00z-183/09:00z)

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 4 4 FGS REAcq 12 12 OBAD with Maneuver 4 4

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

ACS/WFC3 11586

Exceptional Galactic Halo Globular Clusters and the Second Parameter

We propose to obtain deep ACS-WFC images of six globular clusters (five of which have no previous HST photometry) that reside in the Galactic halo, where the second parameter effect is most pronounced These globular clusters are among the least studied in the Galaxy and yet, from the perspective of the second parameter phenomenon, the most intriguing

With the best available CMDs only reaching the vicinity of the main sequence turn off at present, the unique sensitivity and resolution of ACS-WFC will yield ages of unprecedented precision for these clusters These data will provide us with new insight into the stellar populations present in the outer Galactic halo and the nature of the second parameter The second parameter plays a critical role in our understanding of the formation and evolution of the Galaxy and the proposed observations will shed new light on this problem and these exceptional clusters

COS/NUV/FUV 11659

Probing the Interior of SN1006

The remnant of SN 1006 is unique among all supernova remnants in having 3 identified background UV sources that can be used to probe cold, otherwise unseen ejecta within the remnant shell We propose high-resolution spectra from COS to obtain spectra of all three of these The brightest of these, the Schweizer-Middleditch star (the only one with extensive previous high-quality UV spectra) shows Si II absorption with an extremely unusual asymmetric profile with a sharp edge on the red end, indicating the velocity of material just entering the reverse shock Our new spectrum can be compared with STIS observations from 1999 to measure definitively the velocity change as the reverse shock eats its way into ever-more- slowly-expanding ejecta One may well ask, however, if this profile is truly representative, and we seek to answer that with a spectrum of a background quasar at a similar distance of the SM star from the projected center, but in a different direction And by investigating the detailed structure of these two sources and a second quasar, we can probe small-scale structure in the ejecta No object other than SN1006 offers a similar opportunity to probe the distribution of ejecta within the remnant of a Type Ia supernova

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/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/MA1/MA2 11839

The Cycles of Alpha Centauri

This is the HST part of a joint Chandra/HST observing program The objective of the HST part is to obtain new UV spectra of both components of the Alpha Centauri binary: the primary ("Alpha Cen A") is a near twin of the Sun, while the companion ("B") is an early K dwarf, slightly less massive, smaller and less luminous than the Sun The orbital period is 80 yr, and the two stars currently are separated by about 8" The Alpha Cen system has been the subject of long term coronal X-ray monitoring by four successive generations of space observatories, and extensive UV measurements were obtained periodically during the IUE era, from the late 1970's to late 1990's The present program will obtain new STIS echelle spectra of both stars, which each were observed in selected wavelength windows by GHRS in the mid-1990's, and Alpha Cen A later by STIS in an extensive high-res program in 1999, although B unfortunately never was recorded by STIS

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 11648

WFC3 Spectroscopy of an X-ray Luminous Galaxy Cluster at z>2

We propose to obtain deep WFC3+G141 grism observations to spectroscopically confirm a remarkable z>2 cluster of galaxy candidate Over a 1000 arcmin^2 field imaged with Spitzer's IRAC we have discovered a compact (<30ÃƒÂ•ÃƒÂ• diameter) concentration of extremely red galaxies with a factor of >40 overdensity over the adjacent field Among these galaxies for which we can derive meaningful photometric redshifts, 17 are consistent with zphot=2-2 5, making it very likely that the concentration is a real cluster at such high redshift This is further supported by a 3 5 sigma detection of extended X-Ray emission on XMM-Newton data, by a likely color magnitude sequence of red galaxies, and by the presence of a giant galaxy consistent with a BCG at the cluster redshift The general faintness of the red galaxies in all optical bands and their high redshifts prevent confirmation of this cluster with ordinary optical spectroscopy The WFC3 camera with G141 grism provides the only way to confirm this record high-z cluster and measure its redshift from spectral breaks typical of old stellar populations Our deep integrations will reveal redshifts for at least 19 ultra-red galaxies in the area and of a similar number of bluer galaxies at the cluster redshift Knowledge of the cluster redshift based on the HST spectra will allow us to reach important scientific aims: find the most distant Xray emitting evolved galaxy cluster, determine membership of the other galaxies from photometric SED analysis, study their stellar population properties, characterize the color-magnitude relation with constraints on the formation redshift The proposed observations will establish a first z>2 benchmark for cluster field comparisons of galaxy formation at this highest redshift and will firmly establish the progenitors of local rich Abell clusters

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/IR/S/C 11929

IR Dark Current Monitor

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

WFC3/UVIS 11908

Cycle 17: UVIS Bowtie Monitor

============================================================================== TOPIC: Daily Report #5131

http://groups google com/group/sci astro hubble/t/281257e189d3364f?hl=en

== 1 of 1 == Date: Tues, Jul 6 2010 6:36Ã‚Â am From: "Bassford, Lynn"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5131

PERIOD COVERED: 5am July 2 - 5am July 6, 2010 (DOY 183/09:00z-187/09:00z)

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 27 27 FGS REAcq 32 32 OBAD with Maneuver 20 20

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

STIS/CCD 11999

JWST Calibration from a Consistent Absolute Calibration of Spitzer & Hubble

Recently, Gordon, Bohlin, et al submitted a successful Spitzer proposal for cross calibration of HST and Spitzer The cross-calibration targets are stars in three categories: WDs, A-stars, and G-stars Traditionally, IR flux standards are extrapolations of stellar models that are tied to absolute fluxes at shorter wavelengths HST absolute flux standards are among the best available with a solid basis that uses pure hydrogen models of hot WD stars for the SED slopes and is tied to Vega at 5556A via precise Landolt V-band photometry Consistently matching models to our three categories of HST observations along with Spitzer photometry and the few existing absolute IR flux determinations will provide a solid basis for JWST flux calibration over its 0 8-30micron range The goal of this proposal is to complete the HST observations of the set of HST/Spitzer cross-calibration stars Using a variety of standard stars with three different spectral types will ensure that the final calibration is not significantly affected by systematic uncertainties

ACS/WFC 11996

CCD Daily Monitor (Part 3)

WFC3/IR/S/C 11929

IR Dark Current Monitor

WFC3/IR 11926

IR Zero Points

We will measure and monitor the zeropoints through the IR filters using observations of the white dwarf standard stars, GD153, GD71 and GD191B2B and the solar analog standard star, P330E Data will be taken monthly during Cycle 17 Observations of the star cluster, NGC 104, are made twice to check color transformations We expect an accuracy of 2% in the wide filter zeropoints relative to the HST photometric system, and 5% in the medium- and narrow-band filters

WFC3/IR 11915

IR Internal Flat Fields

WFC3/UVIS 11911

UVIS L-Flats and Geometric Distortion

WFC3/UVIS 11908

Cycle 17: UVIS Bowtie Monitor

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

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 11895

FUV Detector Dark Monitor

COS/NUV 11894

NUV Detector Dark Monitor

ACS/SBC 11886

UV Contamination Monitor

The observations consist of imaging and spectroscopy with SBC and HRC of the cluster NGC 6681 in order to monitor the temporal evolution of the UV sensitivity of the SBC and the HRC

WFC3/ACS/UVIS 11877

HST Cycle 17 and Post-SM4 Optical Monitor

This program is the Cycle 17 implementation of the HST Optical Monitoring Program

The 36 orbits comprising this proposal will utilize ACS (Wide Field Channel) and WFC3 (UVIS Channel) to observe stellar cluster members in parallel with multiple exposures over an orbit Phase retrieval performed on the PSF in each image will be used to measure primarily focus, with the ability to explore apparent coma, and astigmatism changes in WFC3

The goals of this program are to: 1) monitor the overall OTA focal length for the purposes of maintaining focus within science tolerances 2) gain experience with the relative effectiveness of phase retrieval on WFC3/UVIS PSFs 3) determine focus offset between the imagers and identify any SI-specific focus behavior and dependencies

If need is determined, future visits will be modified to interleave WFC3/IR channel and STIS/CCD focii measurements

STIS/CCD 11855

STIS/CCD Spectroscopic Sensitivity Monitor for Cycle 17

Monitor sensitivity of each CCD grating mode to detect any change due to contamination or other causes

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

WFC3/UV/ACS/WFC 11739

Multiple Stellar Generations in the Unique Globular Clusters NGC 6388 and NGC 6441

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/UV/ACS/WFC 11710

The Extreme Globular Cluster System of Abell 1689: The Ultimate Test of Universal Formation Efficiency

The stellar masses of the most luminous galaxies poorly represent the masses of the halos in which they reside However, recent studies of the very rich globular cluster (GC) populations in the centers of galaxy clusters point toward an apparently linear scaling of the number of GCs with the total core mass of the galaxy cluster Thus, unlike for the stars in cD galaxies, GC formation in these systems appears to have proceeded with a roughly universal mass conversion efficiency GCs are also distinct in that their spatial distributions are more extended than the starlight, and recent simulations suggest that they follow the mass density profile of the merged dark matter halos that formed stars at high redshift To provide a definitive test of the universal efficiency hypothesis requires measuring the number of GCs in the most massive galaxy clusters, where the number should be a factor of 5 or more greater than seen in M87 Likewise, the relationship between GCs and mass density can only be tested in systems where the total mass and mass density are well-determined Fortunately, the imaging power of HST brings the GC population of Abell 1689, the most extreme high-mass lensing cluster, into range Estimates of the size of the A1689 GC population from available data suggest an unprecedented 100, 000 GCs, but this number is based on the tip of the iceberg and is extremely uncertain We propose to obtain the first accurate measurement of the number of GCs and their density profile in this extraordinary system - the most massive and most distant GC system ever studied - and thus make the ultimate test of the universal GC formation hypothesis Our deep I-band image will also provide a stringent "null-detection" test of several known z>7 galaxy candidates and improve the mass model of the system by increasing the number of usable lensed background galaxies Finally, we will take deep multi-band parallel observations with WFC3/IR to help in quantifying the abundance of rare faint red objects

WFC3/IR 11696

Infrared Survey of Star Formation Across Cosmic Time

WFC3/UVIS 11661

The Black Hole Mass - Bulge Luminosity Relationship for the Nearest Reverberation-Mapped AGNs

We propose to obtain WFC3 host galaxy images of the eight nearest AGNs with masses from reverberation mapping, and one star as a PSF model These images will allow us to determine with unprecedented accuracy the bulge luminosities of the host galaxies, a goal which is not achievable from the ground due to the blurring of the very bright PSF component under typical, and even very good, seeing conditions High-resolution ACS images of the host galaxies of more luminous AGNs reveal that the black hole mass-bulge luminosity and black hole mass-bulge mass relationships for AGNs are not well constrained and arise from what appear to be fundamentally flawed data sets With the addition of the images proposed here to our current sample of ACS images, we will be able to extend our determinations of the black hole mass- bulge luminosity and black hole mass-bulge mass relationships for AGNs by an order of magnitude and test our preliminary results for these fundamentally important relationships against those previously determined for quiescent galaxies

WFC3/UVIS/IR 11644

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

WFC3/UVI 11615

Hunting for Optical Companions to Binary MSPs in Globular Clusters

Here we present a proposal which exploits the re-newed 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 intrisic 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/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/UVIS 11603

A Comprehensive Study of Dust Formation in Type II Supernovae with HST, Spitzer, and Gemini

The recent discovery of three extremely bright Type II SNe, (2007it, 2007oc, 2007od) gives us a unique opportunity to combine observations with HST, Spitzer, and Gemini to study the little understood dust formation process in Type II Sne Priority 1 Spitzer Cycle 5 and band 1 Gemini 2008A time has already been approved for this project Since late-time Type II Sne are faint and tend to be in crowded fields, we need the high sensitivity and high spatial resolution of ACS and NICMOS/NIC2 for these observations This project is motivated by the recent detection of large amounts of dust in high redshift galaxies The dust in these high-z galaxies must come from young, massive stars so Type II Sne could be potential sources The mechanism and the efficiency of dust condensation in Type II SN ejecta are not well understood, largely due to the lack of observational data We plan to produce a unique dataset, combining spectroscopy and imaging in the visible, near- and mid-IR covering the key phase, 400-700 days after maximum when dust is known to form in the SN ejecta Therefore, we are proposing for coordinated HST/NOAO observations (HST ACS, NICMOS/NIC2 & Gemini/GMOS and TReCS) which will be combined with our Spitzer Cycle 5 data to study these new bright Sne The results of this program will place strong constraints on the formation of dust seen in young high redshift (z>5) galaxies

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

WFC3/ACS/IR 11597

Spectroscopy of IR-Selected Galaxy Clusters at 1 < z < 1 5

ACS/WFC3 11586

Exceptional Galactic Halo Globular Clusters and the Second Parameter

ACS/WFC 11582

The Spatial Distribution of Radiation in the Complex ISM of Distant Ultraluminous Galaxies

A significant fraction of energy emitted by galaxies at redshifts when their stars were forming most vigorously, and when their blackholes were growing most powerfully emerges at far-infrared (IR) wavelengths The fraction of this energy generated by the most extreme and luminous objects is also much larger than the equivalent fraction at optical wavelengths Many of the most luminous far-IR sources have been located precisely and unambiguously using deep radio, Spitzer and optical observations, and have spectroscopic identifications using the largest ground-based telescopes Surprisingly, however, the spectra of most of these heavily dust-enshrouded galaxies show prominent Lyman-alpha emission We propose to observe five of the brightest examples at z~2-3 in re-activated ACS ramp filters, to resolve the spatial distribution of this line emission on fine kpc scales, in order to contrast and compare with the underlying ultraviolet (UV) continuum Precise spectroscopic redshifts and the unique rest-UV resolution of HST are both essential to reveal the escape and generation of Lyman-alpha photons in the dusty ISM of these extreme galaxies There is no other way to trace the detailed spatial distirbution of the most excited gas in a galactic wind, along with emission from less-massive star-forming galaxies in associated groups The targets have available HST-resolution ground-based near-IR AO imaging and arcsec-scale images in CO from ground-based mm-wave interferometers, which provide context for spatial structure of evolved stars and the ISM The interplay between restframe UV emission and the ISM in these galaxies has important consequences for understanding the origin of the prodigous luminosity of these systems, and for future observations with JWST and ALMA

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

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

WFC3/ACS/UVIS 11360

Star Formation in Nearby Galaxies

Star formation is a fundamental astrophysical process; it controls phenomena ranging from the evolution of galaxies and nucleosynthesis to the origins of planetary systems and abodes for life The WFC3, optimized at both UV and IR wavelengths and equipped with an extensive array of narrow-band filters, brings unique capabilities to this area of study The WFC3 Scientific Oversight Committee (SOC) proposes an integrated program on star formation in the nearby universe which will fully exploit these new abilities Our targets range from the well-resolved R136 in 30 Dor in the LMC (the nearest super star cluster) and M82 (the nearest starbursting galaxy) to about half a dozen other nearby galaxies that sample a wide range of star-formation rates and environments Our program consists of broad band multiwavelength imaging over the entire range from the UV to the near-IR, aimed at studying the ages and metallicities of stellar populations, revealing young stars that are still hidden by dust at optical wavelengths, and showing the integrated properties of star clusters Narrow-band imaging of the same environments will allow us to measure star-formation rates, gas pressure, chemical abundances, extinction, and shock morphologies The primary scientific issues to be addressed are: (1) What triggers star formation? (2) How do the properties of star-forming regions vary among different types of galaxies and environments of different gas densities and compositions? (3) How do these different environments affect the history of star formation? (4) Is the stellar initial mass function universal or determined by local conditions?

============================================================================== TOPIC: Daily Report #5132

http://groups google com/group/sci astro hubble/t/307376947064247e?hl=en

== 1 of 1 == Date: Wed, Jul 7 2010 9:00Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5132

PERIOD COVERED: 5am July 6 - 5am July 7, 2010 (DOY 187/09:00z-188/09:00z)

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 3 3 FGS REAcq 11 11 OBAD with Maneuver 3 3

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

COS/NUV/ACS/WFC/FUV 11658

Probing the Outer Regions of M31 with QSO Absorption Lines

We propose HST-COS spectroscopy of 10 quasars behind M31 Absorption lines due to MgII, FeII, CIV, and a variety of other lines will be searched for and measured Six quasars lie between 1 and 4 2 Holmberg radii near the major axis on the southwest side, where confusion with Milky Way gas is minimized Two lie even farther out on the southwest side of the major axis One lies within 1 Holmberg radius Two of the 10 pass through M31's high velocity clouds seen in a detailed 21 cm emission map Exposure time estimates were based on SDSS magnitudes and available GALEX magnitudes Thus, using the most well-studied external spiral galaxy in the sky, our observations will permit us to check, better than ever before, the standard picture that quasar metal-line absorption systems such as MgII and CIV arise in an extended gaseous halo/disk of a galaxy well beyond its observable optical radius The observations will yield insights into the nature of the gas and its connection to the very extended stellar components of M31 that have recently been studied Notably the observations have the potential of extending M31's rotation curve to very large galactocentric distances, thereby placing new constrants on M31's dark matter halo

Finally, we also request that the coordinated parallel orbits be allocated to this program so that we may image the resolved stellar content of M31's halo and outer disk

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/ACS/IR 11235

HST NICMOS Survey of the Nuclear Regions of Luminous Infrared Galaxies in the Local Universe

At luminosities above 10^11 4 L_sun, the space density of far-infrared selected galaxies exceeds that of optically selected galaxies These `luminous infrared galaxies' (LIRGs) are primarily interacting or merging disk galaxies undergoing enhanced star formation and Active Galactic Nuclei (AGN) activity, possibly triggered as the objects transform into massive S0 and elliptical merger remnants We propose NICMOS NIC2 imaging of the nuclear regions of a complete sample of 88 L_IR > 10^11 4 L_sun luminous infrared galaxies in the IRAS Revised Bright Galaxy Sample (RBGS: i e , 60 micron flux density > 5 24 Jy) This sample is ideal not only in its completeness and sample size, but also in the proximity and brightness of the galaxies The superb sensitivity and resolution of NICMOS NIC2 on HST enables a unique opportunity to study the detailed structure of the nuclear regions, where dust obscuration may mask star clusters, AGN, and additional nuclei from optical view, with a resolution significantly higher than possible with Spitzer IRAC This survey thus provides a crucial component to our study of the dynamics and evolution of IR galaxies presently underway with Wide-Field, HST ACS/WFC3, and Spitzer IRAC observations of these 88 galaxies Imaging will be done with the F160W filter (H-band) to examine as a function of both luminosity and merger stage: (i) the luminosity and distribution of embedded star clusters, (ii) the presence of optically obscured AGN and nuclei, (iii) the correlation between the distribution of 1 6 micron emission and the mid-IR emission as detected by Spitzer IRAC, (iv) the evidence of bars or bridges that may funnel fuel into the nuclear region, and (v) the ages of star clusters for which photometry is available via ACS/WFC3 observations The NICMOS data, combined with the HST ACS, Spitzer, and GALEX observations of this sample, will result in the most comprehensive study of merging and interacting galaxies to date

WFC3/ACS/UVIS 11360

Star Formation in Nearby Galaxies

WFC3/IR/S/C 11929

IR Dark Current Monitor

WFC3/UV 11556

Investigations of the Pluto System

WFC3/UV/ACS/WFC 11710

The Extreme Globular Cluster System of Abell 1689: The Ultimate Test of Universal Formation Efficiency

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

WFC3/UVIS 11908

Cycle 17: UVIS Bowtie Monitor

============================================================================== TOPIC: Daily Report #5133

http://groups google com/group/sci astro hubble/t/ea6bde3c325bdc49?hl=en

== 1 of 1 == Date: Thurs, Jul 8 2010 7:27Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5133

PERIOD COVERED: 5am July 7 - 5am July 8, 2010 (DOY 188/09:00z-189/09:00z)

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 5 5 FGS REAcq 9 9 OBAD with Maneuver 4 4

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

ACS/WFC 11996

CCD Daily Monitor (Part 3)

COS/FUV 11686

The Cosmological Impact of AGN Outflows: Measuring Absolute Abundances and Kinetic Luminosities

AGN outflows are increasingly invoked as a major contributor to the formation and evolution of supermassive black holes, their host galaxies, the surrounding IGM, and cluster cooling flows Our HST/COS proposal will determine reliable absolute chemical abundances in six AGN outflows, which influences several of the processes mentioned above To date there is only one such determination, done by our team on Mrk 279 using 16 HST/STIS orbits and 100 ksec of FUSE time The advent of COS and its high sensitivity allows us to choose among fainter objects at redshifts high enough to preclude the need for FUSE This will allow us to determine the absolute abundances for six AGN (all fainter than Mrk 279) using only 40 HST COS orbits This will put abundances studies in AGN on a firm footing, an elusive goal for the past four decades In addition, prior FUSE observations of four of these targets indicate that it is probable that the COS observations will detect troughs from excited levels of C III These will allow us to measure the distances of the outflows and thereby determine their kinetic luminosity, a major goal in AGN feedback research

We will use our state of the art column density extraction methods and velocity-dependent photoionization models to determine the abundances and kinetic luminosity Previous AGN outflow projects suffered from the constraints of deciding what science we could do using ONE of the handful of bright targets that were observable With COS we can choose the best sample for our experiment As an added bonus, most of the spectral range of our targets has not been observed previously, greatly increasing the discovery phase space

COS/NUV/ACS/WFC/FUV 11658

Probing the Outer Regions of M31 with QSO Absorption Lines

Finally, we also request that the coordinated parallel orbits be allocated to this program so that we may image the resolved stellar content of M31's halo and outer disk

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/S/C 11929

IR Dark Current Monitor

WFC3/UV/ACS/WFC 11710

The Extreme Globular Cluster System of Abell 1689: The Ultimate Test of Universal Formation Efficiency

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

WFC3/UVIS 11908

Cycle 17: UVIS Bowtie Monitor

==============================================================================

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