Date: March 2nd 2010

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Daily Rpt #5041 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/78381ed261071750?hl=en
Daily Report #5042 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/61953409a903ab5a?hl=en

============================================================================== TOPIC: Daily Rpt #5041

http://groups google com/group/sci astro hubble/t/78381ed261071750?hl=en

== 1 of 1 == Date: Sat, Feb 27 2010 4:07Â am From: "Bassford, Lynn"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5041

PERIOD COVERED: 5am February 25 - 5am February 26, 2010 (DOY 056/10:00z-057/10:00z)

OBSERVATIONS SCHEDULED

ACS/WFC 11995

CCD Daily Monitor (Part 2)

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 320 orbits (20 weeks) from 1 February 2010 to 20 June 2010

NIC2/WFC3/IR 11548

Infrared Imaging of Protostars in the Orion A Cloud: The Role of Environment in Star Formation

We propose NICMOS and WFC3/IR observations of a sample of 252 protostars identified in the Orion A cloud with the Spitzer Space Telescope These observations will image the scattered light escaping the protostellar envelopes, providing information on the shapes of outflow cavities, the inclinations of the protostars, and the overall morphologies of the envelopes In addition, we ask for Spitzer time to obtain 55-95 micron spectra of 75 of the protostars Combining these new data with existing 3 6 to 70 micron photometry and forthcoming 5-40 micron spectra measured with the Spitzer Space Telescope, we will determine the physical properties of the protostars such as envelope density, luminosity, infall rate, and outflow cavity opening angle By examining how these properties vary with stellar density (i e clusters vs groups vs isolation) and the properties of the surrounding molecular cloud; we can directly measure how the surrounding environment influences protostellar evolution, and consequently, the formation of stars and planetary systems Ultimately, this data will guide the development of a theory of protostellar evolution

STIS/CCD 11844

CCD Dark Monitor Part 1

The purpose of this proposal is to monitor the darks for the STIS CCD

STIS/CCD 11846

CCD Bias Monitor-Part 1

The purpose of this proposal is to monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4, to build up high-S/N superbiases and track the evolution of hot columns

STIS/CCD/MA1/MA2 11616

The Disks, Accretion, and Outflows (DAO) of T Tau Stars

Classical T Tauri stars undergo magnetospheric accretion, power outflows, and possess the physical and chemical conditions in their disks to give rise to planet formation Existing high resolution FUV spectra verify that this spectral region offers unique diagnostics of these processes, which have the potential to significantly advance our understanding of the interaction of a star and its accretion disk To date the limited results are intriguing, with dramatic differences in kinematic structure in lines ranging from C IV to H2 among the few stars that have been observed We propose to use HST/COS to survey the disks, outflows, and accretion (the DAO) of 26 CTTS and 6 WTTS in the FUV at high spectral resolution A survey of this size is essential to establish how properties of accretion shocks, winds and disk irradiation depend on disk accretion rate Specifically, our goals are to (1) measure the radiation from and understand the physical properties of the gas very near the accretion shock as a function of accretion rate using emission line profiles of hot lines (C IV, Si IV, N V, and He II); (2) measure the opacity, velocity, and temperature at the base of the outflow to constrain outflow models using wind absorption features; and (3) characterize the radiation incident on disks and protoplanetary atmospheres using H2 line and continuum emission and reconstructed bright Ly-alpha line emission

WFC3/ACS/IR 11563

Galaxies at z~7-10 in the Reionization Epoch: Luminosity Functions to <0 2L* from Deep IR Imaging of the HUDF and HUDF05 Fields

The first generations of galaxies were assembled around redshifts z~7-10+, just 500-800 Myr after recombination, in the heart of the reionization of the universe We know very little about galaxies in this period Despite great effort with HST and other telescopes, less than ~15 galaxies have been reliably detected so far at z>7, contrasting with the ~1000 galaxies detected to date at z~6, just 200-400 Myr later, near the end of the reionization epoch WFC3 IR can dramatically change this situation, enabling derivation of the galaxy luminosity function and its shape at z~7-8 to well below L*, measurement of the UV luminosity density at z~7-8 and z~8-9, and estimates of the contribution of galaxies to reionization at these epochs, as well as characterization of their properties (sizes, structure, colors) A quantitative leap in our understanding of early galaxies, and the timescales of their buildup, requires a total sample of ~100 galaxies at z~7-8 to ~29 AB mag We can achieve this with 192 WFC3 IR orbits on three disjoint fields (minimizing cosmic variance): the HUDF and the two nearby deep fields of the HUDF05 Our program uses three WFC3 IR filters, and leverages over 600 orbits of existing ACS data, to identify, with low contamination, a large sample of over 100 objects at z~7-8, a very useful sample of ~23 at z~8-9, and limits at z~10 By careful placement of the WFC3 IR and parallel ACS pointings, we also enhance the optical ACS imaging on the HUDF and a HUDF05 field We stress (1) the need to go deep, which is paramount to define L*, the shape, and the slope alpha of the luminosity function (LF) at these high redshifts; and (2) the far superior performance of our strategy, compared with the use of strong lensing clusters, in detecting significant samples of faint z~7-8 galaxies to derive their luminosity function and UV ionizing flux Our recent z~7 4 NICMOS results show that wide-area IR surveys, even of GOODS-like depth, simply do not reach faint enough at z~7-9 to meet the LF and UV flux objectives In the spirit of the HDF and the HUDF, we will waive any proprietary period, and will also deliver the reduced data to STScI The proposed data will provide a Legacy resource of great value for a wide range of archival science investigations of galaxies at redshifts z~2-9 The data are likely to remain the deepest IR/optical images until JWST is launched, and will provide sources for spectroscopic followup by JWST, ALMA and EVLA

WFC3/ACS/UVIS 11803

Observing Cluster Assembly Around the Massive Cluster RXJ0152-13

We request ACS imaging for groups and filaments in the outskirts of two z=0 8 forming clusters of galaxies These images will be combined with an unparalleled dataset of wide-field spectroscopy from Magellan, with ~2200 confirmed members (~3200 by the summer) of the superstructures surrounding the two clusters We will estimate merger rates and determine the morphological composition of the galaxy populations within the infalling groups and filaments identified in our spectroscopic dataset The HST data are critical to understand how the early-type galaxy fraction remains constant in cluster centers, while clusters double in mass through the steady accretion of lower mass groups One possibility is that the galaxies in the filaments and infalling groups already have predominantly early-type morphologies, while another is that galaxies transform during, and possibly even in connection with, the process of infall Our unique dataset of spectroscopic membership, when combined with the exquisite high- resolution imaging of ACS and WF3, will enable us to witness the accretion of galaxies unto massive clusters and how this process affects their properties

WFC3/IR/S/C 11929

IR Dark Current Monitor

Analyses of ground test data showed that dark current signals are more reliably removed from science data using darks taken with the same exposure sequences as the science data, than with a single dark current image scaled by desired exposure time Therefore, dark current images must be collected using all sample sequences that will be used in science observations These observations will be used to monitor changes in the dark current of the WFC3-IR channel on a day-to-day basis, and to build calibration dark current ramps for each of the sample sequences to be used by Gos in Cycle 17 For each sample sequence/array size combination, a median ramp will be created and delivered to the calibration database system (CDBS)

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

The behavior of the WFC3 UVIS CCD will be monitored daily with a set of full-frame, four-amp bias and dark frames A smaller set of 2Kx4K subarray biases are acquired at less frequent intervals throughout the cycle to support subarray science observations The internals from this proposal, along with those from the anneal procedure (Proposal 11909), will be used to generate the necessary superbias and superdark reference files for the calibration pipeline (CDBS)

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 11 11 FGS REAcq 8 8 OBAD with Maneuver 5 5

SIGNIFICANT EVENTS: (None)

============================================================================== TOPIC: Daily Report #5042

http://groups google com/group/sci astro hubble/t/61953409a903ab5a?hl=en

== 1 of 1 == Date: Mon, Mar 1 2010 7:20Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5042

PERIOD COVERED: 5am February 26 - 5am March 1, 2010 (DOY 057/10:00z-060/10:00z)

OBSERVATIONS SCHEDULED

WFC3/UV 12049

Improve the Measurement of Vesta's Pole Orientation to Support Dawn Mission

NASA?s Dawn spacecraft is scheduled to go into orbit around the main belt asteroid 4 Vesta in July 2011 Currently the project is using a 3-? pole position uncertainty of Vesta of 12? for spacecraft trajectory design We have determined that with an additional set of Hubble observations at Vesta?s next opposition in February 2010, that the pole position uncertainty can be reduced by a factor of 4 This will reduce both cost and risk to the Dawn mission, and is likely to increase the stay time at Vesta and will add to the scientific return of the mission The requested observing window in February 2010 is the last and single best opportunity that can benefit the Dawn mission, but it is before the start of the next HST Cycle

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

COS/FUV 12011

Magnetic Heating of the Outer Atmospheres of Very Low Mass Dwarfs

The detections of FUV and X-ray emissions from very low mass stars and brown dwarfs have confirmed that stellar magnetic activity can survive even at these low stellar masses The emissions are qualitatively similar to those from active stars, despite the dramatic differences between the characteristics of an ultracool (>M7) stellar atmosphere and those of earlier type cool stars It is currently an open question how the structures and magnetic heating which exists in these very low mass stars compare with those seen in higher mass active stars We propose to take Chandra and HST/COS spectra of two nearby active very low mass stars in order to determine the effect that these large-scale fields have on transition region and coronal structures

ACS/WFC 11995

CCD Daily Monitor (Part 2)

WFC3/IR/S/C 11929

IR Dark Current 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 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 11905

WFC3 UVIS CCD Daily Monitor

FGS 11875

Monitoring FGS2R2 Distortion and Alignment After SMOV4

This proposal monitors changes in the FGS2R2 distortion and alignment after SMOV4 by observing selected stars in M35 in Position mode Data from each epoch are compared to track changes in FGS2R2 When the rate of change becomes sufficiently slow, FGS2R2 will be cleared for a mini-OFAD and FGS-FGS alignment calibration (carried out in another phase 2 proposal)

FGS 11871

Long Term Stability of FGS1R in Position Mode

This proposal resumes the Long Term Monitoring of FGS1R in Position Mode using stars in M35 that are a subset of the FGS "OFAD catalog" using both the "fall" and "spring" seasons (the spring orient was not available under two gyro mode) The data acquired by this proposal are used to update the FGS1R "rhoA & kA" parameters that are associated with the OFAD solution that is applicable at the observation's epoch These values are critical to support sub-milli arcsecond astrometry with FGS1R

This particular proposal also include a FGS3 visit to M35 for post SM4 verification of its calibration status

STIS/CCD 11846

CCD Bias Monitor-Part 1

The purpose of this proposal is to monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4, to build up high-S/N superbiases and track the evolution of hot columns

STIS/CCD 11844

CCD Dark Monitor Part 1

The purpose of this proposal is to monitor the darks for the STIS CCD

WFC3/UVIS/IR 11835

The Multi-Faceted X-Ray Activity of Low-Redshift Active Galaxies

We propose ACIS-I observations of Chandra-unobserved low-redshift 3CRR active galaxies and their environments The data will complete Chandra observations of 3CRR at z < 0 1, making the sample useful for statistical studies Only Chandra can resolve the multiple components of these sources, as is needed for an improved understanding of source physics and gas heating The imaging and spectroscopy of cores, jets, hot spots, and atmospheres will be of permanent legacy value We will use the data to investigate particle acceleration, interactions between radio plasma and the ISM and IGM, the emission mechanisms of hot spots, and AGN fueling Comparison with our complete Spitzer coverage and HST images will aid interpretation The dataset will be made public immediately

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

COS/NUV/FUV 11727

UV Spectroscopy of Local Lyman Break Galaxy Analogs: New Clues to Galaxy Formation in the Early Universe

Much of our information about galaxy evolution and the interaction between galaxies and the IGM at high-z has been provided by the Lyman Break Galaxies (LBGs) However, it is difficult to investigate these faint and distant objects in detail To address this, we have used the GALEX All-Sky Imaging Survey and the SDSS to identify for the first time a rare population of low- redshift galaxies with properties remarkably similar to the high-redshift LBGs These local "Lyman Break Analogs" (LBAs) resemble LBGs in terms of morphology, size, UV luminosity, star formation rate, UV surface brightness, stellar mass, velocity dispersion, metallicity, and dust content We are assembling a wide range of data on these objects with the goal of using them as local laboratories for better understanding the relevant astrophysical processes in LBGs These data include HST imaging (95 orbits in Cy15 and 16), Spitzer photometry and spectroscopy, Chandra and XMM X-ray imaging and spectroscopy, and near-IR integral field spectroscopy (VLT, Keck, and Gemini) In this proposal we are requesting the most important missing puzzle piece: far-UV spectra with a signal-to-noise and spectral resolution significantly better than available for typical LBGs We will use these spectra to study the LBA's galactic winds, probe the processes that regulate the escape of Ly-a and Lyman continuum radiation, determine chemical abundances for the stars and gas, and constrain the form of the high-end of the Initial Mass Function Adding these new COS data will give us vital information about these extraordinary sites of star formation in the local universe In so-doing it will also shed new light on the processes that led to the formation of stars, the building of galaxies, and the enrichment and heating of the IGM in the early universe

WFC3/IR 11719

A Calibration Database for Stellar Models of Asymptotic Giant Branch Stars

Studies of galaxy formation and evolution rely increasingly on the interpretation and modeling of near-infrared observations At these wavelengths, the brightest stars are intermediate mass asymptotic giant branch (AGB) stars These stars can contribute nearly 50% of the integrated luminosity at near infrared and even optical wavelengths, particularly for the younger stellar populations characteristic of high-redshift galaxies (z>1) AGB stars are also significant sources of dust and heavy elements Accurate modeling of AGB stars is therefore of the utmost importance

The primary limitation facing current models is the lack of useful calibration data Current models are tuned to match the properties of the AGB population in the Magellanic Clouds, and thus have only been calibrated in a very narrow range of sub-solar metallicities Preliminary observations already suggest that the models are overestimating AGB lifetimes by factors of 2-3 at lower metallicities At higher (solar) metallicities, there are no appropriate observations for calibrating the models

We propose a WFC3/IR SNAP survey of nearby galaxies to create a large database of AGB populations spanning the full range of metallicities and star formation histories Because of their intrinsically red colors and dusty circumstellar envelopes, tracking the numbers and bolometric fluxes of AGB stars requires the NIR observations we propose here The resulting observations of nearby galaxies with deep ACS imaging offer the opportunity to obtain large (100-1000's) complete samples of AGB stars at a single distance, in systems with well-constrained star formation histories and metallicities

WFC3/UVIS 11714

Snapshot Survey for Planetary Nebulae in Local Group Globular Clusters

Planetary nebulae (PNe) in globular clusters (GCs) raise a number of interesting issues related to stellar and galactic evolution The number of PNe known in Milky Way GCs, four, is surprisingly low if one assumes that all stars pass through a PN stage However, it is likely that the remnants of stars now evolving in galactic GCs leave the AGB so slowly that any ejected nebula dissipates long before the star becomes hot enough to ionize it Thus there should not be ANY PNe in Milky Way GCs--but there are four! It has been suggested that these Pne are the result of mergers of binary stars within GCs, i e , that they are descendants of blue stragglers The frequency of occurrence of PNe in external galaxies poses more questions, because it shows a range of almost an order of magnitude

I propose a SNAPshot survey aimed at discovering PNe in the GC systems of Local Group galaxies outside the Milky Way These clusters, some of which may be much younger than their counterparts in our galaxy, might contain many more PNe than those of our own galaxy I will use the standard technique of emission-line and continuum imaging, which easily discloses PNe This proposal continues a WFPC2 program started in Cycle 16, but with the more powerful WFC3 As a by-product, the survey will also produce color-magnitude diagrams for numerous clusters for the first time, reaching down to the horizontal branch

ACS/WFC/WFC3/UV 11711

A Definitive Distance to the Coma Core Ellipticals

As the richest galaxy cluster in the local universe (cz < 10, 000 km/s), the Coma cluster continues to serve as the standard of comparison for numerous studies of galaxy properties and scaling relations in clusters The central importance of Coma has been recognized with two recent HST large programs: a Treasury survey to study the dwarf galaxy population by imaging 82 different ACS/WFC pointings, and a program to measure Cepheid distances to two spiral galaxies projected within the Coma core region An accurate distance to the Coma core is essential for comparing the galaxy luminosities and sizes to nearby galaxies in Virgo and Fornax, while an accurate peculiar velocity is needed for correctly tying to more distant clusters However, experience dictates that Cepheid distances to clusters must be carefully verified against accurate measurements to the dominant early-type population, especially for such an unprecedented effort as the Coma Cepheid search (the completion of which remains uncertain) We propose to measure highly accurate (3-4% internal error per galaxy) SBF distances to the two giant Coma core ellipticals The reliability of the SBF method with the ACS/WFC has been repeatedly demonstrated, and it is so efficient that it requires only 3% of the number of orbits dedicated to the two current large Coma programs The precise ACS SBF Coma core distance will also provide a good constraint on the Coma peculiar velocity, thus improving the accuracy of comparisons to distant clusters Finally, our program will answer some longstanding puzzles surrounding the rich globular cluster population in the core of this archetypal galaxy cluster

WFC3/UVIS/IR 11702

Search for Very High-z Galaxies with WFC3 Pure Parallel

WFC3 will provide an unprecedented probe to the early universe beyond the current redshift frontier Here we propose a pure parallel program using this new instrument to search for Lyman-break galaxies at 6 520deg) that last for 4 orbits and longer, resulting a total survey area of about 140~230 square arcminute Based on our understanding of the new HST parallel observation scheduling process, we believe that the total number of long-duration pure parallel visits in Cycle 17 should be sufficient to accommodate our program We waive all proprietary rights to our data, and will also make the enhanced data products public in a timely manner

(1) We will use both the UVIS and the IR channels, and do not need to seek optical data from elsewhere

(2) Our program will likely triple the size of the probable candidate samples at z~7 and z~8, and will complement other targeted programs aiming at the similar redshift range

(3) Being a pure parallel program, our survey will only make very limited demand on the scarce HST resources More importantly, as the pure parallel pointings will be at random sight-lines, our program will be least affected by the bias due to the large scale structure ("cosmic variance")

(4) We aim at the most luminous LBG population, and will address the bright-end of the luminosity function at z~8 and z~7 We will constrain the value of L* in particular, which is critical for understanding the star formation process and the stellar mass assembly history in the first few hundred million years of the universe

(5) The candidates from our survey, most of which will be the brightest ones that any surveys would be able to find, will have the best chance to be spectroscopically confirmed at the current 8--10m telescopes

(6) We will also find a large number of extremely red, old galaxies at intermediate redshifts, and the fine spatial resolution offered by the WFC3 will enable us constrain their formation history based on the study of their morphology, and hence shed light on their connection to the very early galaxies in the universe

COS/FUV 11687

SNAPing Coronal Iron

This is a Snapshot Survey to explore two forbidden lines of highly ionized iron in late-type coronal sources Fe XII 1349 (T~ 2 MK) and Fe XXI 1354 (T~ 10 MK) -- well known to Solar Physics -- have been detected in about a dozen cool stars, mainly with HST/STIS The UV coronal forbidden lines are important because they can be observed with velocity resolution of better than 15 km/s, whereas even the state-of-the-art X-ray spectrometers on Chandra can manage only 300 km/s in the kilovolt band where lines of highly ionized iron more commonly are found The kinematic properties of hot coronal plasmas, which are of great interest to theorists and modelers, thus only are accessible in the UV at present The bad news is that the UV coronal forbidden lines are faint, and were captured only in very deep observations with STIS The good news is that 3rd-generation Cosmic Origins Spectrograph, slated for installation in HST by SM4, in a mere 25 minute exposure with its G130M mode can duplicate the sensitivity of a landmark 25-orbit STIS E140M observation of AD Leo, easily the deepest such exposure of a late-type star so far Our goal is to build up understanding of the properties of Fe XII and Fe XXI in additional objects beyond the current limited sample: how the lineshapes depend on activity, whether large scale velocity shifts can be detected, and whether the dynamical content of the lines can be inverted to map the spatial morphology of the stellar corona (as in "Doppler Imaging'') In other words, we want to bring to bear in the coronal venue all the powerful tricks of spectroscopic remote sensing, well in advance of the time that this will be possible exploiting the corona's native X-ray radiation The 1290-1430 band captured by side A of G130M also contains a wide range of key plasma diagnostics that form at temperatures from below 10, 000 K (neutral lines of CNO), to above 200, 000 K (semi-permitted O V 1371), including the important bright multiplets of C II at 1335 and Si IV at 1400; yielding a diagnostic gold mine for the subcoronal atmosphere Because of the broad value of the SNAP spectra, beyond the coronal iron project, we waive the normal proprietary rights

WFC3/UVIS 11650

Mutual Orbits, Colors, Masses, and Bulk Densities of 3 Cold Classical Trans-Neptunian Binaries

Many Trans-Neptunian Objects (TNOs) have been found to be binary or multiple systems As in other astrophysical settings, Trans-Neptunian Binaries (TNBs) offer uniquely valuable information Their mutual orbits allow the direct determination of their system masses, perhaps the most fundamental physical quantity of any astronomical object Their frequency of occurrence and dynamical characteristics provide clues to formation conditions and evolution scenarios affecting both the binaries and their single neighbors Combining masses with sizes, bulk densities can be measured Densities constrain bulk composition and internal structure, key clues to TNO origins and evolution over time Several TNB bulk densities have been determined, hinting at interesting trends But none of them belongs to the Cold Classical sub-population, the one group of TNOs with demonstrably distinct physical characteristics Two top-priority Spitzer programs will soon observe and measure the sizes of 3 Cold Classical TNBs This proposal seeks to determine the mutual orbits and thus masses of these systems, enabling computation of their densities

WFC3/UVIS/IR 11644

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

The eight planets overwhelmingly dominate the solar system by mass, but their small numbers, coupled with their stochastic pasts, make it impossible to construct a unique formation history from the dynamical or compositional characteristics of them alone In contrast, the huge numbers of small bodies scattered throughout and even beyond the planets, while insignificant by mass, provide an almost unlimited number of probes of the statistical conditions, history, and interactions in the solar system To date, attempts to understand the formation and evolution of the Kuiper Belt have largely been dynamical simulations where a hypothesized starting condition is evolved under the gravitational influence of the early giant planets and an attempt is made to reproduce the current observed populations With little compositional information known for the real Kuiper Belt, the test particles in the simulation are free to have any formation location and history as long as they end at the correct point Allowing compositional information to guide and constrain the formation, thermal, and collisional histories of these objects would add an entire new dimension to our understanding of the evolution of the outer solar system While ground based compositional studies have hit their flux limits already with only a few objects sampled, we propose to exploit the new capabilities of WFC3 to perform the first ever large-scale dynamical-compositional study of Kuiper Belt Objects (KBOs) and their progeny to study the chemical, dynamical, and collisional history of the region of the giant planets The sensitivity of the WFC3 observations will allow us to go up to two magnitudes deeper than our ground based studies, allowing us the capability of optimally selecting a target list for a large survey rather than simply taking the few objects that can be measured, as we have had to do to date We have carefully constructed a sample of 120 objects which provides both overall breadth, for a general understanding of these objects, plus a large enough number of objects in the individual dynamical subclass to allow detailed comparison between and within these groups These objects will likely define the core Kuiper Belt compositional sample for years to come While we have many specific results anticipated to come from this survey, as with any project where the field is rich, our current knowledge level is low, and a new instrument suddenly appears which can exploit vastly larger segments of the population, the potential for discovery -- both anticipated and not -- is extraordinary

WFC3/ACS/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/UVIS 11595

Turning Out the Light: A WFC3 Program to Image z>2 Damped Lyman Alpha Systems

We propose to directly image the star-forming regions of z>2 damped Lya systems (DLAs) using the WFC3/UVIS camera on the Hubble Space Telescope In contrast to all previous attempts to detect the galaxies giving rise to high redshift DLAs, we will use a novel technique that completely removes the glare of the background quasar Specifically, we will target quasar sightlines with multiple DLAs and use the higher redshift DLA as a ``blocking filter'' (via Lyman limit absorption) to eliminate all FUV emission from the quasar This will allow us to carry out a deep search for FUV emission from the lower redshift DLA, shortward of the Lyman limit of the higher redshift absorber The unique filter set and high spatial resolution afforded by WFC3/UVIS will then enable us to directly image the lower redshift DLA and thus estimate its size, star- formation rate and impact parameter from the QSO sightline We propose to observe a sample of 20 sightlines, selected primarily from the SDSS database, requiring a total of 40 HST orbits The observations will allow us to determine the first FUV luminosity function of high redshift DLA galaxies and to correlate the DLA galaxy properties with the ISM characteristics inferred from standard absorption-line analysis to significantly improve our understanding of the general DLA population

WFC3/UVIS 11594

A WFC3 Grism Survey for Lyman Limit Absorption at z=2

We propose to conduct a spectroscopic survey of Lyman limit absorbers at redshifts 1 8 < z < 2 5, using WFC3 and the G280 grism This proposal intends to complete an approved Cycle 15 SNAP program (10878), which was cut short due to the ACS failure We have selected 64 quasars at 2 3 < z < 2 6 from the Sloan Digital Sky Survey Spectroscopic Quasar Sample, for which no BAL signature is found at the QSO redshift and no strong metal absorption lines are present at z

2 3 along the lines of sight The survey has three main observational goals First, we will determine the redshift frequency dn/dz of the LLS over the column density range 16 0 < log(NHI) < 20 3 cm^-2 Second, we will measure the column density frequency distribution f(N) for the partial Lyman limit systems (PLLS) over the column density range 16 0 < log(NHI) < 17 5 cm^-2 Third, we will identify those sightlines which could provide a measurement of the primordial D/H ratio By carrying out this survey, we can also help place meaningful constraints on two key quantities of cosmological relevance First, we will estimate the amount of metals in the LLS using the f(N), and ground based observations of metal line transitions Second, by determining f(N) of the PLLS, we can constrain the amplitude of the ionizing UV background at z~2 to a greater precision This survey is ideal for a snapshot observing program, because the on-object integration times are all well below 30 minutes, and follow-up observations from the ground require minimal telescope time due to the QSO sample being bright

WFC3/ACS/IR 11584

Resolving the Smallest Galaxies with ACS

An order of magnitude more dwarf galaxies are expected to inhabit the Local Group, based on currently accepted galaxy formation models, than have been observed This discrepancy has been noted in environments ranging from the field to rich clusters, with evidence emerging that lower density regions contain fewer dwarfs per giant than higher density regions, in further contrast to model predictions However, there is no complete census of the faintest dwarf galaxies in any environment The discovery of the smallest and faintest dwarfs is hampered by the limitations in detecting such compact or low surface brightness galaxies, and this is compounded by the great difficulty in determining accurate distances to, or ascertaining group membership for, such faint objects The M81 group provides a powerful means for establishing membership for faint galaxies in a low density region With a distance modulus of 27 8, the tip of the red giant branch (TRGB) appears at I ~ 24, just within the reach of ground based surveys We have completed a 65 square degree survey in the region around M81 with the CFHT/MegaCam Half of our survey was completed before Cycle 16 and we were awarded time with WFPC2 to observe 15 new candidate dwarf galaxy group members in F606W and F814W bands in order to construct color-magnitude diagrams from which to measure accurate TRGB distances and determine star formation and metallicity histories The data obtained show that 8 - 9 of these objects are galaxies at the same distance as M81 In completing our survey, we have discovered an additional 8 candidate galaxies we propose to image with ACS in order to measure TRGB distances and establish membership We also wish to re-observe our smallest candidate group member and a tidal dwarf candidate with deeper observations made possible with ACS Once membership has been established for this second set of candidates, we will have a complete census of the dwarf galaxy population in the M8 group to M_r ~ -10, allowing us to obtain a firm measurement of the luminosity function faint-end slope, and, combined with previous HST data, to provide a complete inventory of the age and abundance properties for the collapsed core of the M81 group

WFC3/UVIS 11565

A Search for Astrometric Companions to Very Low-Mass, Population II Stars

We propose to carry out a Snapshot search for astrometric companions in a subsample of very low-mass, halo subdwarfs identified within 120 parsecs of the Sun These ultra-cool M subdwarfs are local representatives of the lowest-mass H burning objects from the Galactic Population II The expected 3-4 astrometric doubles that will be discovered will be invaluable in that they will be the first systems from which gravitational masses of metal-poor stars at the bottom of the main sequence can be directly measured

NIC2/WFC3/IR 11219

Active Galactic Nuclei in Nearby Galaxies: A New View of the Origin of the Radio-Loud Radio- Quiet Dichotomy?

Using archival HST and Chandra observations of 34 nearby early-type galaxies (drawn from a complete radio selected sample) we have found evidence that the radio-loud/radio-quiet dichotomy is directly connected to the structure of the inner regions of their host galaxies in the following sense: [1] Radio-loud AGN are associated with galaxies with shallow cores in their light profiles [2] Radio-quiet AGN are only hosted by galaxies with steep cusps Since the brightness profile is determined by the galaxy's evolution, through its merger history, our results suggest that the same process sets the AGN flavor This provides us with a novel tool to explore the co-evolution of galaxies and supermassive black holes, and it opens a new path to understand the origin of the radio-loud/radio-quiet AGN dichotomy Currently our analysis is statistically incomplete as the brightness profile is not available for 82 of the 116 targets Most galaxies were not observed with HST, while in some cases the study is obstructed by the presence of dust features We here propose to perform an infrared NICMOS snapshot survey of these 82 galaxies This will enable us to i) test the reality of the dichotomic behavior in a substantially larger sample; ii) extend the comparison between radio-loud and radio-quiet AGN to a larger range of luminosities

WFC3/IR 11208

The Co-Evolution of Spheroids and Black Holes in the Last Six Billion Years

The masses of giant black holes are correlated with the luminosities, masses, and velocity dispersions of the bulges of their host galaxies This empirical correlation of phenomena on widely different scales (from pcs to kpcs) suggests that the formation and evolution of galaxies and central black holes are closely linked In Cycle 13, we have started a campaign to map directly the co-evolution of spheroids and black-holes by measuring in observationally favorable redshift windows the empirical correlations connecting their properties By focusing on Seyfert 1s, where the nucleus and the stars contribute comparable fractions of total light, black hole mass and bulge dispersion are obtained from Keck spectroscopy HST is required for accurate measurement of the non-stellar AGN continuum, the morphology of the galaxy, and the structural parameters of the bulge The results at z=0 36 indicate a surprisingly fast evolution of bulges in the past 4 Gyrs (significant at the 95%CL), in the sense that bulges were significantly smaller for a given black hole mass Also, the large fraction of mergers and disturbed galaxies (4+2 out of 20) identifies gas-rich mergers as the mechanisms responsible for bulge-growth Going to higher redshift - where evolutionary trends should be stronger - is needed to confirm these tantalizing results We propose therefore to push our investigation to the next suitable redshift window z=0 57 (lookback-time 6 Gyrs) Fifteen objects are the minimum number required to map the evolution of the empirical correlations between bulge properties and black-hole mass, and to achieve a conclusive detection of evolution (>99%CL)

WFC3/IR 11189

Probing the Early Universe with GRBs

Cosmology is beginning to constrain the nature of the earliest stars and galaxies to form in the Universe, but direct observation of galaxies at z>6 remains highly challenging due to their scarcity, intrinsically small size, and high luminosity distance GRB afterglows, thanks to their extreme luminosities, offer the possibility of circumventing these normal constraints by providing redshifts and spectral information which couldn't be obtained through direct observation of the host galaxies themselves In addition, the association of GRBs with massive stars means that they are an indicator of star formation, and that their hosts are likely responsible for a large proportion of the ionizing radiation during that era Our collaboration is conducting a campaign to rapidly identify and study candidate very high redshift bursts, bringing to bear a network of 2, 4 and 8m telescopes with near-IR instrumentation Swift has proven capable of detecting faint, distant GRBs, and reporting accurate positions for many bursts in near real-time Here we propose to continue our HST program of targeting GRBs at z~6 and above HST is crucial to this endeavor, allowing us (a) to characterize the basic properties, such as luminosity and color, and in some cases morphologies, of the hosts, which is essential to understanding these primordial galaxies and their relationship to other galaxy populations; and (b) to monitor the late time afterglows and hence compare them to lower-z bursts and test the use of GRBs as standard candles

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

12203 - GSAcq(1,2,1) at 057/22:59:43z and REAcq(1,2,1) at 057/23:36:14z both acquired fine lock backup on FGS 1 due to scan step limit exceeded on FGS 2

Observations possibly affected: WFC3 - 147 148, proposal ID# 11219

12204 - GSAcq(1,2,1) scheduled at 059/22:14:49z resulted in fine lock backup (2,0,2) due to scan step limit exceeded on FGS 1

Observations possibly affected: COS 105 - 109 proposal ID#11687, WFC3 1 proposal ID# 11929

12205 - REAcq(1,2,1) scheduled at 060/06:09:49z required multiple attempts to achieve Coarse Track Data Valid

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

                  SCHEDULED  SUCCESSFUL

FGS GSAcq 31 31 FGS REAcq 19 19 OBAD with Maneuver 21 21

SIGNIFICANT EVENTS: (None)

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