HUBBLE SPACE TELESCOPE DAILY REPORT # 3179 PERIOD COVERED: DOY 226 OBSERVATIONS SCHEDULED (see HSTARS below for possible observation problems) STIS 8653 Collimation and Physical Conditions Within the HH 30 Protostellar Jet We propose to observe the protostellar jet HH 30 through a wide slit with STIS in order to determine the distance from the star that the jet becomes collimated, and to diagnose the density, temperature, shock structure, and ionization within the collimation region. The proposed observations will provide an image of the jet in each emission line across the entire optical spectrum with minimal contamination from the reflection nebula near the star, a marked improvement over existing narrowband images that cover only a few lines which emit over a limited range of densities and ionization states. Ratios of the new emission-line images will probe the physical conditions in the jet with HST spatial resolution and make it possible to observe the shape and location of any shocks in the flow, resolve the cooling layers behind these shocks, and trace the recombination of any ionized gas that emerges from the base of the jet. The proximity and brightness of HH 30 together with its favorable inclination angle make this an ideal object to study jet collimation. The new STIS spectra are precisely what are needed to test MHD models of jet collimation from accretion disks. Understanding how jets originate, become collimated, and form shocks has profound implications for the distribution of magnetic fields and angular momentum within accretion disks, which in turn control how stars and planets form. 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. STIS/MA1/MA2 8920 Cycle 10 MAMA Dark Measurements. The Space Telescope Imaging Spectrograph (MA1 and MA2) was used to perform the routine monitoring of the MAMA detector dark noise, and is the primary means of checking on health of the MAMA detectors systems through frequent monitoring of the background count rate. 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 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. NICMOS 9325 Photometric Stability This NICMOS post-SMOV3b early calibration proposal carries out photometric monitoring observations after SMOV3b, nominally spanning the approximate time frame April-August 2002. FGS 9347 FGS Astrometry of the Extrasolar Planet of Epsilon Eridani We propose observations with HST/FGS in Position Mode to determine the astrometric elements {perturbation orbit semimajor axis and inclination} of the candidate extra-solar planet around the K2 V star Epsilon Eridani that has been detected by Doppler spectroscopy. These observations will also permit us to determine the actual mass of the planet by providing the sin{i} factor which can not be determined with the radial velocity method. High precision radial velocity {RV} measurements spanning the years 1980.8--2000.0 for the nearby {3.22 pc} star Epsilon Eri show convincing variations with a period of ~ 7 yrs. These data represent a combination of six independent data sets taken with four different telescopes. A least squares orbital solution using robust estimation yields orbital parameters of period, P = 6.9 yrs, velocity K- amplitude = 19 m/s, eccentricity e = 0.6, projected companion mass M_B sin{i} = 0.83 M_Jupiter. An estimate of the inclination yields a perturbation semi-major axis, Alpha = 0arcs0022, easily within the reach of HST/FGS astrometry. SNAP 9356 SNAPSHOT survey of the Planetary Nebulae population of the Galactic Bulge The spectacular structures seen in HST images of planetary nebulae {PNe} are generally accepted as originating from hydrodynamical interactions between stellar winds: the interacting-stellar wind model {ISW}. Traditionally, the shaping is thought to occur after the star becomes hot enough to ionize the PN. But recent HST images indicate that the shaping may occur earlier, and the newer GISW model puts the shaping during the pre-planetary nebula evolution. The relative importance of both models is not known: GISW shaping will account for some fraction of PNe, but estimates range from 15--100 during the PN phase, especially for the youngest PNe. We here propose an HST SNAPshot survey of compact PNe in the Galactic Bulge, to test these predictions. The Bulge provides the only PNe population for which progenitor masses are known and nebular ages can be measured. In support of these HST measurements we have already measured velocity fields and emission line fluxes. The survey will give an unbiassed sampling of morphologies, and allow evolutionary sequences to be determined to test the ISW versus the GISW model. By-products of the survey will be the determination of nebular masses, diameters and filling factors. We will also obtain the White Dwarf mass distribution in the Bulge, and the initial-final mass function for low-mass stars. NICMOS 9366 H_2 Imaging of Proto-Planetary Nebulae: Probing the Dynamics and Morphology H_2 emission provides an excellent probe of the physical conditions in planetary nebulae {PNs} and also in proto- planetary nebulae {PPNs}, objects in transition between the asymptotic giant branch {AGB} and PN phases. It is thought that the shaping of the PN occurs when a fast wind interacts with the remnant of the AGB progenitor during the PPN phase. The study of shock-excited H_2 in PPNs will allow us to study this process. We request HST/NICMOS H_2 and complementary K and H broad-band images of 13 PPNs with a range of spectral types of the central star. We presently have very high- resolution {~100, 000} H_2 spectra for 7 of these, which we will use with the high-resolution images to study the velocity structure of the fast wind. We will also explore the relationship between the presence of H_2 and a bipolar shape for the nebula, as has been found in PNs. However, the role of the equatorial torus is expected to be different in these two cases, and in the PPNs it is expected to collimate the wind rather than shield the molecules. Thus the H_2 in the PPNs is expected at the ends of the lobes rather than in the torus. Radiatively-excited H_2 emission appears to be common in PPNs with central stars of B spectral types; this appears to be a transitional stage in the evolution of the H_2 in the nebula which these images will help us to better understand. ACS 9480 Cosmic Shear With ACS Pure Parallels Small distortions in the shapes of background galaxies by foreground mass provide a powerful method of directly measuring the amount and distribution of dark matter. Several groups have recently detected this weak lensing by large-scale structure, also called cosmic shear. The high resolution and sensitivity of HST/ACS provide a unique opportunity to measure cosmic shear accurately on small scales. Using 260 parallel orbits in Sloan textiti {F775W} we will measure for the first time: beginlistosetlength sep0cm setlengthemsep0cm setlength opsep0cm em the cosmic shear variance on scales <0.7 arcmin, em the skewness of the shear distribution, and em the magnification effect. endlist Our measurements will determine the amplitude of the mass power spectrum sigma_8Omega_m^0.5, with signal-to-noise {s/n} ~ 20, and the mass density Omega_m with s/n=4. They will be done at small angular scales where non-linear effects dominate the power spectrum, providing a test of the gravitational instability paradigm for structure formation. Measurements on these scales are not possible from the ground, because of the systematic effects induced by PSF smearing from seeing. Having many independent lines of sight reduces the uncertainty due to cosmic variance, making parallel observations ideal. 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. GO 9508 A binary system in the Kuiper Belt: 1998_WW31 1998_WW31 is the first Kuiper Belt Object, outside the pair Pluto/Charon, to be discovered as a binary object. Though only preliminary results are available from two orbits of HST DDT observation when this proposal is submitted, the pair exhibits a very high eccentricity {larger than 0.5} and a period of 570 days. The purpose of this proposal is to complete the monitoring of the pair on a full orbit, up to February 2003. Monitoring will then have to cease {Sun too close}. The binarity of an asteroid allows the determination of the total mass of the system and provides important information on the past Kuiper Belt environment {formation/collisions/capture processes}. If size can be obtained from albedo determination, the mass will give the density, a key parameter for any study of the origin and evolution of the Kuiper Belt. Hubble's unparalleled resolution provides the unique way to acquire observations of the pair good enough to access the physical characteristics of this system with a high degree of confidence, as the high eccentricity of the orbit keeps the two components less than 1 arc-second apart for most of the orbit. The observations would be made public immediately to allow the continuation of the education program offering to follow the pair on a regular basis to illustrate the prediction/verification iterative process of science and the direct use of simple laws for the determination of key parameters. 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. CAL/WF2 9597 Intflat Sweep, Visflat Sweep, and Filter Anomaly Check No abstract available. ACS 9650 CCD Hot Pixel Annealing Hot pixel annealing will be performed once every 4 weeks. The CCD TECs will be turned off and heaters will be activated to bring the WFC detector temperature to about +10C. The HRC temperature will reach about 30C.This state will be held for approximately 24 hours, after which the heaters are turned off, the TECs turned on, and the CCDs returned to normal operating condition. To assess the effectiveness of this procedure, a bias and two dark images will be taken before and after the annealing procedure for both WFC and HRC. 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: 8762 - G String not processing TDM DAT file @226/18:40z. While attempting to process the Daily Clock Correlation on the G string I received the following error message. An error occurred in attempting to use the ground station mailbox file. A ground station delay of zero has been selected by default. If you wish to reenter a ground station delay file name or mnemonic, enter command 'GOTO CHOOSE' to return to first menu page. You may also enter a nonzero ground delay on display DGSL when it appears. RUN TIME MESSAGE:ERROR READING GROUND SATION MAILBOX FILE; ERROR NUMBER: -1 this error message is saying that the TDM.DAT file has not been updating for the last 24hrs. Last update was on day 225 at 21:09. We have been in OPS MODE on G string since last week. Steve Bradenburg was able to verify that ODMs were being processed by the FEP. Under investigation. COMPLETED OPS REQs: None OPS NOTES EXECUTED: 1027-2 - Reset MCE1 Limits @227/1800z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 7 7 FGS REacq 9 9 FHST Update 13 13 LOSS of LOCK Operations Notes: Tested ability to switch to a 'Serial Conversion Device Mode' on a IP String (B) from 226/2130-2310z SIGNIFICANT EVENTS: FOT relocated to B23 Backup MOR day and evening shifts to accommodate AT&T work on OC3 redundant circuit and mux at the STScI. WSC Software Delivery 02002 to WSGT 227/07:20Z - 13:00Z. No User services available during the following timeframes: SGLT-4 (TDW 227/07:20Z - 11:20Z and SGLT-6 (TDZ 275) 227/07:20Z - 13:20Z. HST On-Orbit Checkout of real-time WSC interface scheduled daily 224 - 231 with GDOC, STOCC Ops (SIMOR), HITT, and CCS using CCS "G" String with CCS Release 4.0.1 and PRD O06100Q1. 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.