HUBBLE SPACE TELESCOPE DAILY REPORT # 3174 PERIOD COVERED: DOY 219 OBSERVATIONS SCHEDULED (see HSTARS below for possible observation problems) NICMOS 8790 NICMOS Post-SAA calibration - CR Persistence Part 1. A new procedure proposed to alleviate the CR-persistence problem of NICMOS. Dark frames will be obtained immediately upon exiting the SAA contour 23, and every time a NICMOS exposure is scheduled within 50 minutes of coming out of the SAA. The darks will be obtained in parallel in all three NICMOS Cameras. The POST-SAA darks will be non-standard reference files available to users with a USEAFTER date/time mark. STIS/CCD 8902 Dark Monitor-Part 2. The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks. STIS/CCD 8904 Bias Monitor-Part 2. The Space Telescope Imaging Spectrograph (CCD) was used to monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4 in order to build up high-S/N superbiases and track the evolution of hot columns. WFPC2 8934 WFPC2 Decontaminations and Associated Observations Pt. 3/3 photometric stability check, focus monitor, pre- and post-decon internals {bias, intflats, kspots, & darks}, UV throughput check, VISFLAT sweep, and internal UV flat check. WFPC2 8938 WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3. This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. STIS/CCD 9066 Closing in on the Hydrogen Reionization Edge of the Universe. The Space Telescope Imaging Spectrograph (CCD) was used in parallel constrain the Hydrogen reionization edge in emission that marks the transition from a neutral to a fully ionized IGM at a predicted redshifts. STIS/CCD/MA1 9137 Quasar Absorbers and Large Scale Structure. The Space Telescope Imaging Spectrograph (CCD and MA1) was used to perform spectroscopy of 15 bright quasars in a 22 square degree region that has well-sampled galaxy redshifts. STIS/CCD 9317 Pure Parallel Imaging Program: Cycle 10. The Space Telescope Imaging Spectrograph (CCD) was used to perform the default archival pure parallel program for STIS during cycle 10. GO 9387 The Natural Occulting Disk and Host Galaxy of the Red BAL Quasar FIRST J1556+3517 We propose an innovative imaging observation of the host galaxy of the red, broad absorption line {BAL} quasar FIRST J1556+3517. This object is already noteworthy as being the first radio-loud BAL quasar, and moreover a member of the very rare class of ``Fe-LoBAL'' quasars. FIRST J1556+3517 also has the unique property {out of some 60+ BALQSOs} of having unpolarized BAL troughs wider than the bandpass of the linear ramp filter of ACS. This unpolarized trough light most likely arises from stars comprising the host galaxy of FIRST J1556+3517. In this special quasar exists a natural occulting disk -- the BAL outflow -- and the opportunity to image a quasar host galaxy at high redshift without the complications of separating out the quasar. Red low-ionization BAL quasars like FIRST J1556+3517 have been hypothesized to be young merger products with high accretion rates and active star formation, perhaps representing a key evolutionary state in the lifetime of massive galaxies. FGS/1 9407 Astrometry of a Star Hosting an Extrasolar Planet: The Mass of Upsilon Andromedae. Fine Guidance Sensor #1 was used to determine the astrometric elements {perturbation orbit semimajor axis and inclination} produced by the outermost extra-solar planet orbiting the F8V star Upsilon Andromedae. These observations will permit us to determine the actual mass of the planet by providing the presently unknown sin i factor intrinsic to the radial velocity method which discovered this object. An inclination, i = 30degrees, within the range of one very low precision determination using reanalyzed HIPPARCOS intermediate data products, would produce the observed radial velocity amplitude, K = 66 ms with a companion mass of ~8 M_Jupiter. Such a mass would induce in Upsilon Andromedae a perturbation semi-major axis, Alpha = 0arcs0012. The proposed observations will yield a planetary mass, rather than, as previous investigations have done, only suggest a planetary mass companion. SNAP/STIS 9434 A SNAPSHOT Survey of the Hot Interstellar Medium We propose to obtain SNAPSHOT STIS echelle observations of key tracers of hot interstellar gas {CIV, NV and SiIV} for selected FUSE Team OVI survey targets with known UV fluxes. By taking advantage of the SNAPSHOT observing mode we will efficiently obtain a large number of spectra suitable for the study of the highly ionized hot component of the interstellar medium {ISM}. Our goals are to explore the physical conditions in and distribution of such gas, as well as to explore the nature of the interfaces between the hot ISM and the other interstellar gas phases. Using inter--comparisons of the various ionic ratios for CIV, NV, OVI and SiIV, we will be able to discriminate between the various models for the production of the highly ionized gas in the Galactic ISM. The survey will also enable detailed studies of regions already known to contain hot gas through X-ray emission measurements {e.g., SNRs and radio loops}. The proposed SNAPSHOT observations will extend our previous Cycle 9 survey {which was compromised by the STIS side 1 failure}, and should roughly double the number of stars for which high quality STIS observations of the important hot gas tracers are available, enabling us to derive a truly global view of the hot ISM. ACS 9460 Irradiated Jets and Proto-Planetary Disks in the Outer Orion Nebula We propose to acquire high resolution ACS H-alpha , [N II] , and [O III] images in four outlying portions of the Orion Nebula that will sample the type of environment in which most members of the Trapezium cluster stars are located. We seek to understand the properties of outflows and protoplanetary disks `proplyds' located more than 4' {0.5 pc} from the core of the Orion Nebula as a function of the radiation field intensity. Two of our target fields contain recently identified externally irradiated jets that suffer large C-shaped bends. The Orion jets are ionized by external UV radiation. Thus, the structures of the target flows can be directly determined from images without recourse to non-linear shock models. High resolution images of their shocks will be used to distinguish between several possible models of jet deflection and to directly compare with 3D numerical models of jets in side- winds. Two other fields contain large proplyd candidates and large numbers of young stars formed from the Orion molecular ridge. These young stars are in less irradiated environments than the well studied proplyds in the nebular core. We will search for new proplyds surrounding these stars to see if the lower radiation field implies a better chance of disk survival. These observations will serve to constrain the properties of protoplanetary disks in lower radiation environments than those in the nebular core. ACS 9472 A Snapshot Survey for Gravitational Lenses among z >= 4.0 Quasars Over the last few years, the Sloan Digital Sky Survey has revolutionized the study of high-redshift quasars by discovering over 200 objects with redshift greater than 4.0, more than doubling the number known in this redshift interval. The sample includes eight of the ten highest redshift quasars known. We propose a snapshot imaging survey of a well-defined sample of 250 z > 4.0 quasars in order to find objects which are gravitationally lensed. Lensing models including magnification bias predict that at least 4% of quasars in a flux-limited sample at z > 4 will be multiply lensed. Therefore this survey should find of order 10 lensed quasars at high redshift; only one gravitationally lensed quasar is currently known at z > 4. This survey will provide by far the best sample to date of high-redshift gravitational lenses. The observed fraction of lenses can put strong constraints on cosmological models, in particular on the cosmological constant Lambda. In addition, magnification bias can significantly bias estimates of the luminosity function of quasars and the evolution thereof; this work will constrain how important an effect this is, and thereby give us a better understanding of the evolution of quasars and black holes at early epochs, as well as constrain models for black hole formation. NICMOS 9484 The NICMOS Parallel Observing Program We propose to manage the default set of pure parallels with NICMOS. Our experience with both our GO NICMOS parallel program and the public parallel NICMOS programs in cycle 7 prepared us to make optimal use of the parallel opportunities. The NICMOS G141 grism remains the most powerful survey tool for HAlpha emission-line galaxies at cosmologically interesting redshifts. It is particularly well suited to addressing two key uncertainties regarding the global history of star formation: the peak rate of star formation in the relatively unexplored but critical 1<= z <= 2 epoch, and the amount of star formation missing from UV continuum-based estimates due to high extinction. Our proposed deep G141 exposures will increase the sample of known HAlpha emission- line objects at z ~ 1.3 by roughly an order of magnitude. We will also obtain a mix of F110W and F160W images along random sight-lines to examine the space density and morphologies of the reddest galaxies. The nature of the extremely red galaxies remains unclear and our program of imaging and grism spectroscopy provides unique information regarding both the incidence of obscured star bursts and the build up of stellar mass at intermediate redshifts. In addition to carrying out the parallel program we will populate a public database with calibrated spectra and images, and provide limited ground- based optical and near-IR data for the deepest parallel fields. ACS/CAL 9558 ACS weekly Test This program consists of basic tests to monitor, the read noise, the development of hot pixels and test for any source of noise in ACS CCD detectors. This programme will be executed once a day for the entire lifetime of ACS. WFPC2 9676 POMS Test Proposal: WFII parallel archive proposal This is the generic target version of the WFPC2 Archival Pure Parallel program. The program will be used to take parallel images of random areas of the sky, following the recommendations of the 2002 Parallels Working Group. FLIGHT OPERATIONS SUMMARY: HSTARS (For details see http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf) HSTARS: None COMPLETED OPS REQs: None OPS NOTES EXECUTED: None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 6 6 FGS REacq 10 10 FHST Update 14 14 LOSS of LOCK Operations Notes: None SIGNIFICANT EVENTS: Performed DSMC Interface Test using CCS "G" String with CCS Release 4.0.1 (IP Mode). Test was eventually successful, after a full day of troubleshooting with WSC test, GSFC NOM, STOCC Control, STOCCOPS, Sys Admin, IP NOC, SOC, CCS, I&C, and HITT problem was isolated and fixed. Determined that in order for GCMRs to be transmitted successfully in IP Mode, the HST Packet Filters must be configured to pass sequence errors. CCS dose not increment the Sequence Counter in acknowledgement messages back to the DSMC, thus the Packet Filters drop these acknowledgement blocks instead of sending blocks to the DSMC and GCMRs fail. Modified Packet Filter to pass sequence errors, GCMRs worked nominally. See GSCA 534. WSC Software Delivery 02002 220/18:00Z - 221/00:00Z. No User services available during the following timeframes: SGLT-2 (TDRS 171) 220/18:00Z - 22:00Z and SGLT-3 (TDRS Spare) 220/18:00Z - 221/00:00Z. HST CCS 4.0.1 Operational Readiness for Source/Destination Code test scheduled 220/12:00Z - 16:00Z with GDOC, SOC, HITT, and CCS using CCS "B" String with CCS Release 4.0.1 and PRD D06100R2. HST "B" String Command Timing test scheduled 220/17:00Z - 22:00Z with GDOC, SOC, HITT, and CCS using CCS "B" String with Release 4.0.1 and PRD D06100R2. HST On-Orbit Checkout of real-time WSC interface scheduled daily 217 - 224 with GDOC, STOCC Ops (SIMOR), HITT, and CCS using CCS "G" String with CCS Release 4.0.1 and PRD D06100R2. The purpose of this testing is to verify CCS Release 4.0.1 (IP) capability to interface through the IP Packet Filters to WSC for real-time telemetry and commands.