Date: October 7th 2010

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Daily Report #5195 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/3710cabb280227b9?hl=en
Daily Report #5196 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/d89676afcd654e5d?hl=en

============================================================================== TOPIC: Daily Report #5195

http://groups google com/group/sci astro hubble/t/3710cabb280227b9?hl=en

== 1 of 1 == Date: Tues, Oct 5 2010 1:03Ã‚Â pm From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5195

PERIOD COVERED: 8:00pm October 4 - 7:59pm October 5, 2010 (DOY 277/00:00z-277/23:59z)

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

12448 - SDF fails to properly output science data following software change starting at 277/0143z

Observations possibly affected: WFC3 26-17, Proposal ID#12307; WFC3 8, Proposal ID#11929; WFC3 19-20, 22-24, 30-34 Proposal ID#12215; WFC3 21, Proposal ID#12215; WFC3 9-11, 13-18 Proposal ID#12348; WFC3 4-7 Proposal ID#11905; WFC3 28-29, 32 Proposal ID#11700; WFC 1-6 Proposal ID#11582; WFC 1, 8-14 Proposal ID#11996; WFC 15-18 Proposal ID#12209; COS 30-35 Proposal ID#11741; STIS 3-4 Proposal ID#11845; STIS 5-7 Proposal ID#11847; STIS 1-2 Proposal ID#11849

12450 - GSAcq(1,2,1) at 277/18:04z results in fine lock back (1,0,1), stop flag on FGS-1 at 277/1807z

Observations possibly affected: WFC3 26-27, Proposal ID#12307

COMPLETED OPS REQUEST: 18933-1 Inhibit NSSC-1 ATP pointer@277/19:08z

COMPLETED OPS NOTES: (None)

                    Scheduled   Successful

FGS GSAcq 8 8 FGS REAcq 8 8 OBAD with Maneuver 8 8

SIGNIFICANT EVENTS:

FLASH SIC&DH ATP pointer halted

In response to the failure of the SDF to properly output science data at 277/19:10 the NSSC-1 ATP was inhibited and SDF input enabled via Ops Request 18933 This will facilitate the recovery of the remaining science data in the SIs and interception of the reprocessed SMS

OBSERVATIONS SCHEDULED:

COS/FUV 11895

FUV Detector Dark Monitor

Monitor the FUV detector dark rate by taking long science exposures without illuminating the detector The detector dark rate and spatial distribution of counts will be compared to pre-launch and SMOV data in order to verify the nominal operation of the detector Variations of count rate as a function of orbital position will be analyzed to find dependence of dark rate on proximity to the SAA Dependence of dark rate as function of time will also be tracked

COS/FUV 12169

The Frequency and Chemical Composition of Planetary Debris Discs around Young White Dwarfs

Throughout the past few years, it has become increasingly clear that the most plausible scenario to explain the metal-pollution observed in ~20% of all cool white dwarfs is accretion from rocky debris material - suggesting that these white dwarfs may have had, or may still have terrestial planets as well This hypothesis is corroborated through the infrared detection of circumstellar dust around the most heavily polluted white dwarfs Traditionally, the detection of metal pollution is done in the optical using the Ca H/K lines, leading to a strong bias against hot/young white dwarfs Hence, most of our knowledge about the late evolution of planetary systems is based on white dwarfs with cooling ages >0 5Gyr We propose an HST/COS ultraviolet spectroscopic snapshot survey to carry out the first systematic investigation of the fraction of metal-pollution among young (20-100Myr) white dwarfs, probing the correlation with white dwarf (and hence progenitor) mass, and determining the Si/H, C/H, and potentially N/H and O/H abundance ratios of their circumstellar debris material

COS/FUV 12212

What are the Locations and Kinematics of Mass Outflows in AGN?

Mass outflows of ionized gas in AGN, first revealed through blueshifted UV and X-ray absorption lines, are likely important feedback mechanisms for the enrichment of the IGM, self-regulation of black-hole growth, and formation of structure in the early Universe To understand the origin, dynamics, and impact of the outflowing absorbers on their surroundings, we need to know their locations (radial positions and polar angles with respect to the AGN rotation axes) and kinematics (radial and transverse velocities) We will use COS high-resolution spectra of 11 Seyfert 1 galaxies to derive velocity-dependent covering factors, ionic column densities, number densities (via metastable lines or variability), and ionization parameters (via photoionization models) of the UV absorbers, and thereby determine their radial locations as we have done for NGC 4151 We will use absorption variability over time scales of up to ~20 years, to determine transverse velocities and detect changes in radial velocities We will use STIS G430M long-slit spectra and WFC3 [OIII] images to resolve the kinematics of the narrow-line region (NLR) and determine the inclinations of the AGN, to investigate the connection between nuclear absorption and NLR emission outflows and their dependence on polar angle

WFC3/UV 12324

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

============================================================================== TOPIC: Daily Report #5196

http://groups google com/group/sci astro hubble/t/d89676afcd654e5d?hl=en

== 1 of 1 == Date: Wed, Oct 6 2010 7:43Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5196

PERIOD COVERED: 8:00pm October 4 - 7:59pm October 5, 2010 (DOY 278/00:00z-278/23:59z)

FLIGHT OPERATIONS SUMMARY:

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

HSTARS:

12452 - GSAcq(1,2,1) at 278/14:55:23z Resulted in Fine Lock Back-up on FGS1

Observations possibly affected: WFC3 1 Proposal ID#12344; WFC3 2-3 Proposal ID#12345; STIS 1 Proposal ID#12212

HSTARS FOR DOY 263, 265, 266, AND 267

12453 - REAcq(2,1,1) at 263/18:48z required two attempts to achieve CT-DV

Observations possibly affected: COS 23-28 Proposal ID#11997; COS 29 Proposal ID#11894

12454 - REAcq(1,2,1) at 265/13:58z required two attempts for FL-DV on FGS2

Observations possibly affected: COS 64-66 Proposal ID#11598

12455 - REAcq(2,1,1) at 266/15:18z required two attempts to achieve CT-DV

Observations possibly affected: WFC3 86-91 Proposal ID#12256

12456 - REAcq(1,2,1) at 267/21:54z required multiple attempts for CT-DV on FGS1

Observations possibly affected: WFC3 116-117 Proposal ID#11591

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

                    Scheduled   Successful

FGS GSAcq 10 10 FGS REAcq 06 06 OBAD with Maneuver 08 08

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

ACS/WFC 12210

SLACS for the Masses: Extending Strong Lensing to Lower Masses and Smaller Radii

Strong gravitational lensing provides the most accurate possible measurement of mass in the central regions of early-type galaxies (ETGs) We propose to continue the highly productive Sloan Lens ACS (SLACS) Survey for strong gravitational lens galaxies by observing a substantial fraction of 135 new ETG gravitational-lens candidates with HST-ACS WFC F814W Snapshot imaging The proposed target sample has been selected from the seventh and final data release of the Sloan Digital Sky Survey, and is designed to complement the distribution of previously confirmed SLACS lenses in lens-galaxy mass and in the ratio of Einstein radius to optical half-light radius The observations we propose will lead to a combined SLACS sample covering nearly two decades in mass, with dense mapping of enclosed mass as a function of radius out to the half-light radius and beyond With this longer mass baseline, we will extend our lensing and dynamical analysis of the mass structure and scaling relations of ETGs to galaxies of significantly lower mass, and directly test for a transition in structural and dark-matter content trends at intermediate galaxy mass The broader mass coverage will also enable us to make a direct connection to the structure of well-studied nearby ETGs as deduced from dynamical modeling of their line-of-sight velocity distribution fields Finally, the combined sample will allow a more conclusive test of the current SLACS result that the intrinsic scatter in ETG mass-density structure is not significantly correlated with any other galaxy observables The final SLACS sample at the conclusion of this program will comprise approximately 130 lenses with known foreground and background redshifts, and is likely to be the largest confirmed sample of strong-lens galaxies for many years to come

COS/FUV 12212

What are the Locations and Kinematics of Mass Outflows in AGN?

COS/NUV/FUV/WFC3/UV 12248

How Dwarf Galaxies Got That Way: Mapping Multiphase Gaseous Halos and Galactic Winds Below L*

One of the most vexing problems in galaxy formation concerns how gas accretion and feedback influence the evolution of galaxies In high mass galaxies, numerical simulations predict the initial fuel is accreted through 'cold' streams, after which AGN suppress star formation to leave galaxies red and gas-poor In the shallow potential wells that host dwarf galaxies, gas accretion can be very efficient, and "superwinds" driven either by hot gas expelled by SNe or momentum imparted by SNe and hot-star radiation are regarded as the likely source(s) of feedback However, major doubts persist about the physics of gas accretion, and particularly about SN-driven feedback, including their scalings with halo mass and their influence on the evolution of the galaxies While "superwinds" are visible in X-rays near the point of their departure, they generally drop below detectable surface-brightness limits at ~ 10 kpc Cold clumps in winds can be detected as blue-shifted absorption against the galaxy's own starlight, but the radial extent of these winds are difficult to constrain, leaving their energy, momentum, and ultimate fate uncertain Wind prescriptions in hydrodynamical simulations are uncertain and at present are constrained only by indirect observations, e g by their influence on the stellar masses of galaxies and IGM metallicity All these doubts lead to one conclusion: we do not understand gas accretion and feedback because we generally do not observe the infall and winds directly, in the extended gaseous halos of galaxies, when it is happening To do this effectively, we must harness the power of absorption-line spectroscopy to measure the density, temperature, metallicity, and kinematics of small quantities of diffuse gas in galaxy halos The most important physical diagnostics lie in the FUV, so this is uniquely a problem for HST and COS We propose new COS G130M and G160M observations of 41 QSOs that probe the gaseous halos of 44 SDSS dwarf galaxies well inside their virial radii Using sensitive absorption-line measurements of the multiphase gas diagnostics Lya, CII/IV, Si II/III/IV, and other species, supplemented by optical data from SDSS and Keck, we will map the halos of galaxies with L = 0 02 - 0 3 L*, stellar masses M* = 10^(8-10) Msun, over impact parameter from 15 - 150 kpc These observations will directly constrain the content and kinematics of accreting and outflowing material, provide a concrete target for simulations to hit, and statistically test proposed galactic superwind models These observations will also inform the study of galaxies at high z, where the shallow halo potentials that host dwarf galaxies today were the norm These observations are low-risk and routine for COS, easily schedulable, and promise a major advance in our understanding of how dwarf galaxies came to be

WFC3/IR 12286

Hubble Infrared Pure Parallel Imaging Extragalactic Survey (HIPPIES)

WFC3 has demonstrated its unprecedented power in probing the early universe Here we propose to continue our pure parallel program with this instrument to search for LBGs at z~6--8 Our program, dubbed as the Hubble Infrared Pure Parallel Imaging Extragalactic Survey ("HIPPIES"), will carry on the HST pure parallel legacy in the new decade We request 205 orbits in Cycle-18, which will spread over ~ 50 high Galactic latitude visits (|b|>20deg) that last for 3 orbits and longer, resulting a total survey area of ~230 square arcmin Combining the WFC3 pure parallel observations in Cycle-17, HIPPIES will complement other existing and forthcoming WFC3 surveys, and will make unique contributions to the study in the new redshift frontier because of the randomness of the survey fields To make full use of the parallel opportunities, HIPPIES will also take ACS parallels to study LBGs at z~5--6 Being a pure parallel program, HIPPIES will only make very limited demand on the scarce HST resources, but will have potentially large scientific returns As in previous cycle, we waive all proprietary data rights, and will make the enhanced data products public in a timely manner

(1) The WFC3 part of HIPPIES aims at the most luminous LBG population at z~8 and z~7 As its survey fields are random and completely uncorrelated, the number counts of the bright LBGs from HIPPIES will be least affected by the "cosmic variance", and hence we will be able to obtain the best constraint on the bright-end of the LBG luminosity function at z~8 and 7 Comparing the result from HIPPIES to the hydrodynamic simulations will test the input physics and provide insight into the nature of the early galaxies (2) The z~7--8 candidates from HIPPIES, 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 (3) The ACS part of HIPPIES will produce a significant number of candidate LBGs at z~5 and z~6 per ACS field Combining with the existing, suitable ACS fields in the HST archive, we will be able to utilize the random nature of the survey to quantify the cosmic variance and to measure the galaxy bias at z~5--6, and therefore the galaxy halo masses at these redshifts (4) 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

WFC3/UV 12215

Searching for the Missing Low-Mass Companions of Massive Stars

Recent results on binary companions of massive O stars appear to indicate that the distribution of secondary masses is truncated at low masses It thus mimics the distribution of companions of G dwarfs and also the Initial Mass Function (IMF), except that it is shifted upward by a factor of 20 in mass These results, if correct, provide a distribution of mass ratios that hints at a strong constraint on the star-formation process However, this intriguing result is derived from a complex simulation of data which suffer from observational incompleteness at the low-mass end

We propose a snapshot survey to test this result in a very direct way HST WFC3 images of a sample of the nearest Cepheids (which were formerly B stars of ~5 Msun) will search for low-mass companions down to M dwarfs We will confirm any companions as young stars, and thus true physical companions, through follow-up Chandra X-ray images Our survey will show clearly whether the companion mass distribution is truncated at low masses, but at a mass much higher than that of the IMF or G dwarfs

WFC3/UV 12344

Cycle 18: 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/UV 12345

UVIS Long Darks Test

Darks during SMOV showed a systematically lower global dark rate as well as lower scatter when compared to the Cycle 17 darks Those two sets of exposures differ in exposure time - 1800 sec during SMOV and 900 sec during Cycle 17 Hypothetically, the effect could be caused by short-duration stray light, say ~500-sec in duration During the latter part of Cycle 17, operation of WFC3 was changed to additionally block the light path to the detector with the CSM This program acquires a small number of darks at the longer SMOV exposure times (1800 sec) in order to check whether the effect repeats in the new operating mode

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

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