Date: May 4th 2010

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Daily Report #5084 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/556e3a0df7b009c9?hl=en
Daily Report #5086 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/446cbd8ce2c5710c?hl=en
Daily Report #5087 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/15fcdcabcf4e7945?hl=en

============================================================================== TOPIC: Daily Report #5084

http://groups google com/group/sci astro hubble/t/556e3a0df7b009c9?hl=en

== 1 of 1 == Date: Wed, Apr 28 2010 7:36Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5084

PERIOD COVERED: 5am April 27 - 5am April 28, 2010 (DOY 117/09:00z-118/09:00z)

OBSERVATIONS SCHEDULED

ACS/WFC/WFC3/UV 11578

The Extremely Metal-Poor BCD Galaxy DDO 68: a Young Galaxy in the Local Universe ?

A long standing question in astrophysics is the existence of young galaxies, in which stars are now forming for the first time, in the nearby (i e , present-day) universe Such galaxies would be the local analogs of primordial galaxies observed at high redshift The most promising candidates have long been the most metal-poor systems, including dwarf irregulars (dIrrs) and blue compact dwarfs (BCDs) However, in many dIrrs and BCDs studied with HST an old (1 Gyr) underlying stellar population, as traced by red giant branch (RGB) stars, has been unambiguously detected Even in I Zw 18, which is the most-metal poor prototype of the class and long the most controversial case, our group has recently succeeded in detecting an RGB Nonetheless, there remains the possibility that the star formation histories of BCDs/dIrrs vary from galaxy to galaxy, and that truly young galaxies do exist in the local universe A new test of these issues has only recently become possible with the identification of DDO 68 as an extremely metal-poor galaxy with an oxygen abundance equal to that of I Zw 18 (12+(O/H)=7 21) This galaxy is about a factor of 2-3 closer than I Zw 18, which yields the opportunity to avoid the many ambiguities that have plagued studies of I Zw 18 Also, DDO 68 resides in a void, making it more likely that star formation has been suppressed for a very long time We will observe DDO 68 with ACS/WFC in F606W and F814W, plus F658N (Halpha) to correct the broad F606W for gas contamination We will use WFC3 in parallel with the same filters to study radial population gradients Deep color-magnitude diagrams (CMDs) reaching the depth of one magnitude below the predicted RGB tip will be constructed and interpreted based on synthetic CMD fitting These data will determine unambiguously whether DDO 68 has an underlying old (RGB) stellar population or is forming stars for the first time Finding just a single nearby ``young'' galaxy would have profound cosmological implications

COS/NUV/FUV/WFC3/UVIS/IR 11533

COS-GTO: Accretion Flows and Winds of Pre-Main Sequence Stars

COS will obtain spectra of T Tauri stars to study accretion flows and wind absorption features in ultraviolet emission lines Observations of several T Tauri stars with different inclination angles with respect to the line of sight will determine the temperature distributions, flow velocities, and column densities of both inflows and outflows for these stars

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/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/IR 11936

IR Grism Flux Calibration

This program will determine image displacement, spectral trace and flux calibration for the IR G102 and G141 grisms as a function of spatial position within the field of view The HST flux standard GD71 will be observed in a 9-point pattern in the IR field of view, which will provide the necessary image displacement, spectral trace, and throughput measurements

WFC3/IR/S/C 11929

IR Dark Current Monitor

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

WFC3/UV/ACS/WFC 11636

First Resolved Imaging of Escaping Lyman Continuum

The emission from star-forming galaxies appears to be responsible for reionization of the universe at z > 6 However, the models that attempt to describe the detailed impact of high-redshift galaxies on the surrounding inter-galactic medium (IGM) are strongly dependent upon several uncertain parameters Perhaps the most uncertain is the fraction of HI-ionizing photons produced by young stars that escape into the IGM Most attempts to measure this "escape fraction" have produced null results Recently, a small subset of z~3 Lyman Break Galaxies (LBGs) has been found exhibiting large escape fractions It remains unclear however, what differentiates them from other LBGs Several models attempt to explain how such a large fraction of ionizing continuum can escape through the HI and dust in the ISM (eg "chimneys" created by SNe winds, globular cluster formation, etc ), each producing unique signatures which can be observed with resolved imaging of the escaping Lyman continuum To date, there are only six LBGs with individual detections of escaping Lyman continuum at any redshift We propose a single deep, high resolution WFC3/UVIS image of the ionizing continuum (F336W) and the rest-frame UV/optical (F606W/F814W/F160W) of five of these six LBGs with large escape fractions These LBGs have a high surface density and large escape fractions, and lie at the optimal redshift for Lyman continuum imaging with UVIS filters, making our sample especially suitable for follow-up With these data we will discern the mechanisms responsible for producing large escape fractions, and therefore gain insight into the process of reionization

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/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/UVI 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 determin and correct the geometric distotrion 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

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

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

12255 - Following successful GSAcq(2,3,3), a Loss of Lock occurred while guiding with FGS-2, and FGS-3 at 188/04:27:02z Subsequent REAcqs(2,3,3) were successful

Observations possibly affected WFC3 47 Proposal ID#11911, ACS #85, Proposal ID#11995

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

                  SCHEDULED SUCCESSFUL FAILURE TIMES

FGS GSAcq 06 06 FGS REAcq 10 10 OBAD with Maneuver 03 03 LOSS of LOCK 118/04:29:57z

SIGNIFICANT EVENTS: (None)

============================================================================== TOPIC: Daily Report #5086

http://groups google com/group/sci astro hubble/t/446cbd8ce2c5710c?hl=en

== 1 of 1 == Date: Fri, Apr 30 2010 9:27Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5086

PERIOD COVERED: 5am April 29 - 5am April 30, 2010 (DOY 119/09:00z-120/09:00z)

OBSERVATIONS SCHEDULED

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

ACS/WFC 11715

The Luminous Galactic Cepheid RS Puppis: A Geometric Distance from its Nested Light Echoes

RS Puppis is one of the most luminous Cepheids in the Milky Way (P = 41 4 days) and an analog of the bright Cepheids used to measure extragalactic distances An accurate distance would help anchor the zero-point of the bright end of the period-luminosity relation, but at a distance of about 2 kpc it is too far away for a trigonometric parallax with existing instrumentation

RS Pup is unique in being surrounded by a reflection nebula, whose brightness varies as pulses of light from the Cepheid propagate outwards Members of our team have used ground-based imaging of the nebula to derive phase lags in the light variations of individual features in the nebula, and have inferred a seemingly very precise geometric distance to the star However, there is an unavoidable ambiguity involving the cycle counts, which was resolved by assuming that the features lie in the plane of the sky If this assumption is incorrect, a large systematic error would be introduced into the distance measurement

We show that polarimetric imaging using the high spatial resolution of ACS/WFC and its ability to image close to the star can resolve this ambiguity and yield a reliable geometric distance to RS Pup We will also obtain a wide-field multicolor image of the nebula, in order to study its morphology and the mass-loss history of the Cepheid

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 11567

Boron Abundances in Rapidly Rotating Early-B Stars

Models of rotation in early-B stars predict that rotationally driven mixing should deplete surface boron abundances during the main-sequence lifetime of many stars However, recent work has shown that many boron depleted stars are intrinsically slow rotators for which models predict no depletion should have occurred, while observations of nitrogen in some more rapidly rotating stars show less mixing than the models predict Boron can provide unique information on the earliest stages of mixing in B stars, but previous surveys have been biased towards narrow- lined stars because of the difficulty in measuring boron abundances in rapidly rotating stars The two targets observed as part of our Cycle 13 SNAP program 10175, just before STIS failed, demonstrate that it is possible to make useful boron abundance measurements for early-B stars with Vsin(i) above 100 km/s We propose to extend that survey to a large enough sample of stars to allow statistically significant tests of models of rotational mixing in early-B stars

STIS/CCD 11852

STIS CCD Spectroscopic Flats C17

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

WFC3/IR/S/C 11929

IR Dark Current Monitor

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

WFC3/UVIS 11911

UVIS L-Flats and Geometric Distortion

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 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

ACS/WFC 11995

CCD Daily Monitor (Part 2)

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

12259 - GSAcq(2,3,3) at 119/10:11:22z was successful REAcqs(2,3,3) scheduled at 119/11:36:48z, 1312z, 1451z, 1633z, and 1815z all failed

Observations affected: WFC3 111-130, proposal ID#11911

12263 - GSAcq(1,2,1) results in fine lock backup (2,0,2) using FGS-2 @ 120/0323z

Observations Possibly affected: COS 34-38 Proposal ID#11687, ACS 115-116 Proposal ID#11995, STIS 47 Proposal ID#11845

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

                  SCHEDULED SUCCESSFUL

FGS GSAcq 07 07 FGS REAcq 11 06 OBAD with Maneuver 05 05

SIGNIFICANT EVENTS: (None)

============================================================================== TOPIC: Daily Report #5087

http://groups google com/group/sci astro hubble/t/15fcdcabcf4e7945?hl=en

== 1 of 1 == Date: Mon, May 3 2010 7:29Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5087

PERIOD COVERED: 5am April 30 - 5am May 03, 2010 (DOY 120/09:00z-123/09:00z)

OBSERVATIONS SCHEDULED

WFC3/UV/IR 12021

An Irradiated Disk in an Ultraluminous X-Ray Source

Whether ultraluminous X-ray sources (ULXs) contain stellar-mass or intermediate-mass black holes (IMBHs) is an important, but as yet unresolved, astrophysical question We have discovered variable optical emission from the ULX NGC 5408 X-1 that we interpret as reprocessed emission in an irradiated disk We propose simultaneous observations with Chandra and HST to test this interpretation and place constraints on the geometry of the accretion disk The observations should provide a means to discriminate between stellar-mass versus intermediate-mass black holes

ACS/WFC 11995

CCD Daily Monitor (Part 2)

WFC3/IR/S/C 11929

IR Dark Current Monitor

WFC3/UVIS/IR 11909

UVIS Hot Pixel Anneal

WFC3/UVIS 11908

Cycle 17: UVIS Bowtie Monitor

Ground testing revealed an intermittent hysteresis type effect in the UVIS detector (both CCDs) at the level of ~1%, lasting hours to days Initially found via an unexpected bowtie-shaped feature in flatfield ratios, subsequent lab tests on similar e2v devices have since shown that it is also present as simply an overall offset across the entire CCD, i e , a QE offset without any discernable pattern These lab tests have further revealed that overexposing the detector to count levels several times full well fills the traps and effectively neutralizes the bowtie Each visit in this proposal acquires a set of three 3x3 binned internal flatfields: the first unsaturated image will be used to detect any bowtie, the second, highly exposed image will neutralize the bowtie if it is present, and the final image will allow for verification that the bowtie is gone

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

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/NUV 11896

NUV Spectroscopic Sensitivity Monitoring

The purpose of this proposal is to monitor sensitivity of each NUV grating mode to detect any changes due to contamination or other causes

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

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)

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

FGS 11789

An Astrometric Calibration of Population II Distance Indicators

In 2002, HST produced a highly precise parallax for RR Lyrae That measurement resulted in an absolute magnitude, M(V)= 0 61+/-0 11, a useful result, judged by the over ten refereed citations each year since It is, however, unsatisfactory to have the direct, parallax-based, distance scale of Population II variables based on a single star We propose, therefore, to obtain the parallaxes of four additional RR Lyrae stars and two Population II Cepheids, or W Vir stars The Population II Cepheids lie with the RR Lyrae stars on a common K-band Period-Luminosity relation Using these parallaxes to inform that relationship, we anticipate a zero point error of 0 04 magnitude This result should greatly strengthen confidence in the Population II distance scale and increase our understanding of RR Lyrae star and Pop II Cepheid astrophysics

STIS/CCD/MA1 11737

The Distance Dependence of the Interstellar N/O Abundance Ratio: A Gould Belt Influence?

The degree of elemental abundance homogeneity in the interstellar medium is a function of the enrichment and mixing processes that govern galactic chemical evolution Observations of young stars and the interstellar gas within ~500 pc of the Sun have revealed a local ISM that is so well-mixed it is having an impact on ideas regarding the formation of extrasolar planets However, the situation just beyond the local ISM is not so clear Sensitive UV absorption line measurements have recently revealed a pattern of inhomogeneities in the interstellar O, N, and Kr gas-phase abundances at distances of ~500 pc and beyond that appear nucleosynthetic in origin rather than due to dust depletion In particular, based on a sample of 13 sightlines, Knauth et al (2006) have found that the nearby stars (d < 500 pc) exhibit a mean interstellar N/O abundance ratio that is significantly higher (0 18 dex) than that toward the more distant stars Interestingly, all of their sightlines lie in the sky vicinity of the Gould Belt of OB associations, molecular clouds, and diffuse gas encircling the Sun at a distance of ~400 pc Is it possible that mixing processes have not yet smoothed out the recent ISM enrichment by massive stars in the young Belt region? By measuring the interstellar N/O ratios in a strategic new sample of sightlines with STIS, we propose to test the apparent N/O homogeneity inside the Gould Belt and determine if the apparent decline in the N/O ratio with distance is robust and associated with the Belt region

WFC3/UV/IR 11709

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

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

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

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

COS/FUV 11687

SNAPing Coronal Iron

WFC3/UVIS 11675

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

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

WFC3/UV/IR 11664

The WFC3 Galactic Bulge Treasury Program: Populations, Formation History, and Planets

Exploiting the full power of the Wide Field Camera 3 (WFC3), we propose deep panchromatic imaging of four fields in the Galactic bulge These data will enable a sensitive dissection of its stellar populations, using a new set of reddening-free photometric indices we have constructed from broad-band filters across UV, optical, and near-IR wavelengths These indices will provide accurate temperatures and metallicities for hundreds of thousands of individual bulge stars Proper motions of these stars derived from multi-epoch observations will allow separation of pure bulge samples from foreground disk contamination Our catalogs of proper motions and panchromatic photometry will support a wide range of bulge studies

Using these photometric and astrometric tools, we will reconstruct the detailed star-formation history as a function of position within the bulge, and thus differentiate between rapid- and extended-formation scenarios We will also measure the dependence of the stellar mass function on metallicity, revealing how the characteristic mass of star formation varies with chemistry Our sample of bulge stars with accurate metallicities will include 12 candidate hosts of extrasolar planets Planet frequency is correlated with metallicity in the solar neighborhood; our measurements will extend this knowledge to a remote environment with a very distinct chemistry

Our proposal also includes observations of six well-studied globular and open star clusters; these observations will serve to calibrate our photometric indices, provide empirical population templates, and transform the theoretical isochrone libraries into the WFC3 filter system Besides enabling our own program, these products will provide powerful new tools for a host of other stellar-population investigations with HST/WFC3 We will deliver all of the products from this Treasury Program to the community in a timely fashion

WFC3/UV/ACS/WFC 11636

First Resolved Imaging of Escaping Lyman Continuum

WFC3/UVIS 11628

Globular Cluster Candidates for Hosting a Central Black Hole

We are continuing our study of the dynamical properties of globular clusters and we propose to obtain surface brightness profiles for high concentration clusters Our results to date show that the distribution of central surface brightness slopes do not conform to standard models This has important implications for how they form and evolve, and suggest the possible presence of central intermediate-mass black holes From our previous archival proposals (AR-9542 and AR- 10315), we find that many high concentration globular clusters do not have flat cores or steep central cusps, instead they show weak cusps Numerical simulations suggest that clusters with weak cusps may harbor intermediate-mass black holes and we have one confirmation of this connection with omega Centauri This cluster shows a shallow cusp in its surface brightness profile, while kinematical measurements suggest the presence of a black hole in its center Our goal is to extend these studies to a sample containing 85% of the Galactic globular clusters with concentrations higher than 1 7 and look for objects departing from isothermal behavior The ACS globular cluster survey (GO-10775) provides enough objects to have an excellent coverage of a wide range of galactic clusters, but it contains only a couple of the ones with high concentration The proposed sample consists of clusters whose light profile can only be adequately measured from space-based imaging This would take us close to completeness for the high concentration cases and therefore provide a more complete list of candidates for containing a central black hole The dataset will also be combined with our existing kinematic measurements and enhanced with future kinematic studies to perform detailed dynamical modeling

STIS/CCD 11606

Dynamical Hypermassive Black Hole Masses

We will use STIS spectra to derive the masses of 5 hypermassive black holes (HMBHs) From the observed scaling relations defined by less massive spheroids, these objects are expected to reside at the nuclei of host galaxies with stellar velocity dispersions greater than 320 km/s These 5 targets have confirmed regular gas distributions on the scales of the black hole sphere of influence It is essential that the sphere of influence is resolved for accurate determinations of black hole mass (0 1") These scales cannot be effectively observed from the ground Only two HMBHs have had their masses modeled so far; it is impossible to draw any general conclusions about the connections between HMBH mass and their massive host galaxies With these 5 targets we will determine whether these HMBHs deviate from the scaling relations defined by less massive spheroids A larger sample will allow us to firmly anchor the high mass end of the correlation between black hole mass and stellar velocity dispersion, and other scaling relations Therefore we are also conducting a SNAPshot program with which we expect to detect a further 24 HMBH candidates for STIS observation in future cycles At the completion of this project we will have populated the high mass end of the scaling relations with the sample sizes enjoyed by less massive spheroids

ACS/WFC3 11604

The Nuclear Structure of OH Megamaser Galaxies

We propose a snapshot survey of a complete sample of 80 OH megamaser galaxies Each galaxy will be imaged with the ACS/WFC through F814W and a linear ramp filter (FR656N or FR716N or FR782N or FR853N) allowing us to study both the spheroid and the gas morphology in Halpha + [N II] We will use the 9% ramps FR647M (5370-7570 angstroms) centered at 7000 angstroms and FR914M (7570-10, 719 angstroms) 8000 angstroms for continuum subtraction for the high and low z objects respectively OH megamaser galaxies (OHMG) form an important class of ultraluminous IR-galaxies (ULIRGs) whose maser lines emit QSO-like luminosities ULIRGs in general are associated with recent mergers but it is often unclear whether their power output is dominated by starbursts or a hidden QSO because of the high absorbing columns which hide their nuclei even at X-ray wavelengths In contrast, OHMG exhibit strong evidence for the presence of an energetically important and recently triggered active nucleus In particular it is clear that much of the gas must have already collapsed to form a nuclear disk which may be the progenitor of a circum-nuclear torus, a key element of the unified scheme of AGN A great advantage of studying OHMG systems over the general ULIRG population, is that the circum-nuclear disks are effectively "fixed" at an inner, edge on, orientation, eliminating varying inclination as a nuisance parameter We will use the HST observations in conjunction with existing maser and spectroscopic data to construct a detailed picture of the circum-nuclear regions of a hitherto relatively neglected class of galaxy that may hold the key to understanding the relationship between galaxy mergers, nuclear star-formation, and the growth of massive black holes and the triggering of nuclear activity

ACS/WFC3 11599

Distances of Planetary Nebulae from SNAPshots of Resolved Companions

Reliable distances to individual planetary nebulae (PNe) in the Milky Way are needed to advance our understanding of their spatial distribution, birthrates, influence on galactic chemistry, and the luminosities and evolutionary states of their central stars (CSPN) Few PNe have good distances, however One of the best ways to remedy this problem is to find resolved physical companions to the CSPN and measure their distances by photometric main-sequence fitting We have previously used HST to identify and measure probable companions to 10 CSPN, based on angular separations and statistical arguments only We now propose to use HST to re-observe 48 PNe from that program for which additional companions are possibly present We then can use the added criterion of common proper motion to confirm our original candidate companions and identify new ones in cases that could not confidently be studied before We will image the region around each CSPN in the V and I bands, and in some cases in the B band Field stars that appear close to the CSPN by chance will be revealed by their relative proper motion during the 13+ years since our original survey, leaving only genuine physical companions in our improved and enlarged sample This study will increase the number of Galactic PNe with reliable distances by 50 percent and improve the distances to PNe with previously known companions

WFC3/UVIS 11594

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

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

ACS/WFC/WFC3/UV 11578

The Extremely Metal-Poor BCD Galaxy DDO 68: a Young Galaxy in the Local Universe ?

STIS/CCD 11567

Boron Abundances in Rapidly Rotating Early-B Stars

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

NIC3/WFC3/IR 11149

Characterizing the Stellar Populations in Lyman-Alpha Emitters and Lyman Break Galaxies at 5 7

The epoch of reionization marks a major phase transition of the Universe, during which the intergalactic space became transparent to UV photons Determining when this occurred and the physical processes involved represents the latest frontier in observational cosmology Over the last few years, searches have intensified to identify the population of high-redshift (z>6) galaxies that might be responsible for this process, but the progress is hampered partly by the difficulty of obtaining physical information (stellar mass, age, star formation rate/history) for individual sources This is because the number of z>6 galaxies that have both secure spectroscopic redshifts and high-quality infrared photometry (especially with Spitzer/IRAC) is still fairly small Considering that only several photometric points are available per source, and that many model SEDs are highly degenerate, it is crucial to obtain as many observational constraints as possible for each source to ensure the validity of SED modeling To better understand the physical properties of high-redshift galaxies, we propose here to conduct HST/NICMOS (72 orbits) and Spitzer/IRAC (102 hours) imaging of spectroscopically confirmed, bright (z<26 mag (AB)) Ly-alpha emitters (LAEs) and Lyman-break galaxies (LBGs) at 5 76 as suggested recently? (2) Is Ly-alpha emission systematically suppressed at z>6 with respect to continuum emission? (i e , are we reaching the epoch of incomplete reionization?), and (3) Do we see any sign of abnormally young stellar population in any of the z>6 galaxies?

WFC3/ACS/IR 11142

Revealing the Physical Nature of Infrared Luminous Galaxies at 0 3

We aim to determine physical properties of IR luminous galaxies at 0 3 0 8mJy and their mid-IR spectra have already provided the majority targets with spectroscopic redshifts (0 31 ULIRGs, as in the local Universe, (2) study the co-evolution of star formation and blackhole accretion by investigating the relations between the fraction of starburst/AGN measured from mid-IR spectra vs HST morphologies, L(bol) and z, and (3) obtain the current best estimates of the far-IR emission, thus L(bol) for this sample, and establish if the relative contribution of mid-to-far IR dust emission is correlated with morphology (resolved vs unresolved)

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 25 25 FGS REAcq 22 22 OBAD with Maneuver 22 22

SIGNIFICANT EVENTS: (None)

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