HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3143<br /><br />PERIOD COVERED: DOY 172-174<br /><br />OBSERVATIONS SCHEDULED [see HSTARS below for possible observation problems]<br /><br />ACS/CAL 9558<br /><br />ACS weekly Test<br /><br />This program consists of basic tests to monitor, the read noise, the development<br />of hot pixels and test for any source of noise in ACS CCD detectors. This<br />programme will be executed once a day for the entire lifetime of ACS.<br /><br />ACS/HRC/WFC 9292<br /><br />The Nature of Galaxies at z > 4<br /><br />The Advanced Camera for Surveys [HRC and WFC] was used to further look into<br />recent discoveries of a number of galaxies and quasars at redshifts greater than<br />5 that has identified the z>5-6 epoch as key to understanding the earliest<br />formation phases for galaxies. However, establishing the characteristics and<br />properties of these earliest galaxies is proving to be a particularly difficult.<br />They are faint, with I{AB} magnitudes around 26-27. Thus, substantial<br />investments of time are needed to obtain high S/N images, while ground-based<br />spectroscopy, even with 8-10 m class telescopes, has provided little more than<br />redshifts. Establishing the physical properties of these galaxies will be a<br />challenge for the foreseeable future. However, there is a subset of this high<br />redshift population that is amenable to more detailed study. These are sources<br />that have been strongly lensed by low redshift clusters.<br /><br />ACS/WFC 9584<br /><br />ACS Default {Archival} Pure Parallel Program II.<br /><br />The Advanced Camera for Surveys [WFC] was used to test ACS pure parallels.<br /><br />ACS/WFC 9575<br /><br />Default {Archival} Pure Parallel Program.<br /><br />The Advanced Camera for Surveys [WFC] was used to test ACS pure parallels in<br />POMS.<br /><br />ACS/WFC/HRC 9075<br /><br />Cosmological Parameters from Type Ia Supernovae at High Redshift.<br /><br />The Advanced Camera for Surveys [WFC and HRC] was used to obtain a Hubble<br />diagram of Type Ia supernovae {SNe Ia} that will be of long lasting value as a<br />record of the expansion history of the universe.<br /><br />FGS/1 9034<br /><br />The Masses and Luminosities of Population II Stars.<br /><br />Fine Guidance Sensor 11R was used to observe the mass-luminosity relation {MLR}<br />of Population II stars of which very little is currently known. With the advent<br />of the Hipparcos Catalogue, improved distances to many spectroscopic binaries<br />known to be Pop II systems are now available. After surveying the literature and<br />making reasonable estimates of the secondary masses, we find 13 systems whose<br />minimum separation should be larger than the resolution limit of FGS #1.<br /><br />GTO/ACS 9290<br /><br />The Nature of Galaxies at z > 4.<br /><br />The Morphological, Photometric, and Spectroscopic Properties of Intermediate<br />Redshift Cluster.New and fundamental constraints on the evolutionary state of<br />high redshift clusters will be made by obtaining deep, multiband images {SDSS g,<br />r, i, z} over the central 1.5 Mpc regions of seven distant clusters in the range<br />0.76 < z < 1.27. In addition, slitless spectroscopy, using the WFC GRISM, will<br />be performed over the central 750 kpc region of each system galaxy.<br /><br />NICMOS 9269<br /><br />NICMOS Parallel Thermal Background<br /><br />NICMOS Camera 3 pure parallel exposures in the F222M filter will be obtained for<br />the entire duration of SMOV to establish the stability of the HST+NCS+Instrument<br />thermal emission.<br /><br />NICMOS 8790<br /><br />NICMOS Post-SAA calibration - CR Persistence Part 1.<br /><br />A new procedure proposed to alleviate the CR-persistence problem of NICMOS. Dark<br />frames will be obtained immediately upon exiting the SAA contour 23, and every<br />time a NICMOS exposure is scheduled within 50 minutes of coming out of the SAA.<br />The darks will be obtained in parallel in all three NICMOS Cameras. The POST-SAA<br />darks will be non-standard reference files available to users with a USEAFTER<br />date/time mark.<br /><br />STIS 9618<br /><br />STIS MAMA Dispersion Solutions<br /><br />Obtain wavecals just deep enough to constrain wavelength and spatial distortion<br />maps without overusing the calibration lamp. For the first time on orbit, data<br />will be obtained at all available central wavelengths. This information will<br />help constrain global models of STIS optical performance being developed at ECF<br />and STScI. During the observations, MSM monthly offsets will be set to zero to<br />complement observations over the past couple of cycles, which occurred at extreme<br />monthly offsets. The echelle observations at zero offset will yield dispersion<br />solutions that are directly applicable to all echelle science data obtained<br />after monthly offsets are disabled.<br /><br />STIS 9435<br /><br />Systematic Search for Rotation at the Base of Outflows from T Tauri Stars<br /><br />We wish to search for rotation signatures in the initial portion {first 100 AU}<br />of a sample of outflows emanating from T Tauri stars {TTSs}. This project<br />originates from our detection of systematic transverse radial velocity shifts in<br />STIS spectra of the DG Tau jet {Bacciotti et al., 2002}. The shifts, observed in<br />a region where the flow is already collimated, but has not yet manifestly<br />interacted with its environment, are consistent with the predictions of magneto-<br />centrifugal launching models, and may constitute the first observed indication<br />for rotation in the initial portion of a jet flow. Rotation is a fundamental<br />ingredient in star formation theories, thus we propose to confirm the above<br />result by carrying out a systematic survey in similar flows. We plan to take for<br />each jet a STIS spectrum in the 6300 -- 6800 Angstrom range, with the slit<br />perpendicular to the flow direction and at a distance of about 0.''3 from the<br />source {i.e., in our targets, 40 -- 70 AU along the jet depending on inclination<br />angle}. Since the flows are resolved transversely with HST, the proposed slit<br />orientation allows for the direct detection of systematic velocity shifts. Where<br />found, we will check for consistency between the sense of rotation observed and<br />that of the underlying disk through CO interferometric measurements. As a<br />by-product, estimates of the excitation conditions across the flow {including<br />ionization fraction} and of the mass outflow rates will be derived.<br /><br />STIS/CCD 9187<br /><br />A Lyman Limit Snapshot Survey: The Search for Candidate D/H Absorbers.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to measure D/H in gas<br />clouds seen against background QSOs. This provides a unique and fundamental<br />cosmological probe of the baryonic density parameter. To date, most of the QSO<br />absorption line D/H constraints have been derived at high redshift. In this<br />proposal the proposers investigate a lower redshift range, because there are two<br />potentially crucial advantages to be gained by carrying out D/H measurements at<br />intermediate redshift. First, the background of HI forest lines is lower and<br />contamination of the DI feature is significantly reduced. Second, a far larger<br />sample of very bright QSOs exists.<br /><br />STIS/CCD 8904<br /><br />Bias Monitor-Part 2.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to monitor the bias in<br />the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4 in order<br />to build up high-S/N superbiases and track the evolution of hot columns.<br /><br />STIS/CCD 9066<br /><br />Closing in on the Hydrogen Reionization Edge of the Universe.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used in parallel constrain<br />the Hydrogen reionization edge in emission that marks the transition from a<br />neutral to a fully ionized IGM at a predicted redshifts.<br /><br />STIS/CCD 9186<br /><br />D/H in Lyman Limit Absorbers with Simple Velocity Structure.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to observe the deuterium<br />abundance in QSO absorbers that provides a direct measurement of the baryonic<br />density of the Universe. This proposal will obtain new high resolution data of<br />two carefully selected, intermediate redshift absorption systems.<br /><br />STIS/CCD 8902<br /><br />Dark Monitor-Part 2.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to monitor the darks.<br /><br />STIS/CCD 8895<br /><br />Far-UV Spectroscopy Of The Disk Around HD 100546.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to perform a one-orbit<br />program to do long-slit spectroscopy of HD 100546. Lyman-alpha has been seen in<br />emission in IUE/SWP spectra. This spectra would map the spatial extent of<br />Lyman-alpha emission and give the spatial orientation of the disk {i.e. which<br />side is the approaching side}. The proposal completed with no reported problems.<br /><br />STIS/CCD 9131<br /><br />Imaging the Host Galaxies of High Redshift Type Ia Supernovae.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to complete the snapshot<br />survey of distant galaxies of known redshift which hosted supernovae {SNe} of<br />Type Ia found via the Supernova Cosmology Project {SCP}.<br /><br />STIS/CCD 9148<br /><br />Light Echos and the Nature of Type Ia Supernovae.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to take STIS snapshot<br />images of a subset of 43 well observed Type Ia supernovae {SNIa}, most of which<br />have been discovered in late type galaxies over the last 40 years to make a<br />systematic search for light echos around SN Ia. STIS will also observe a sample<br />of 10 SN II and SN Ib/c, which are believed to be the result of massive star<br />core collapse and, therefore, to be thin-disk population objects, in order to<br />make an empirical calibration of the accuracy of our method for determining<br />scale heights. The SN Ia sample will provide a direct as well as accurate<br />estimate of the scale height of SN Ia which is an important clue to the<br />progenitors of these events.<br /><br />STIS/CCD 9088<br /><br />Next Generation Spectral Library of Stars.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to produce a "Next<br />Generation'' Spectral Library of 600 stars for use in modeling the integrated<br />light of galaxies and clusters by using the low dispersion UV and optical<br />gratings of STIS. The library will be roughly equally divided among four<br />metallicities, very low {Fe/H < -1.5}, low {-1.5 < Fe/H < -0.5}, near-solar<br />{-0.5 < Fe/H < 0.1}, and super-solar {Fe/H > 0.1}, well-sampling the entire<br />HR-diagram in each bin. Such a library will surpass all extant compilations and<br />have lasting archival value, well into the Next Generation Space Telescope era.<br /><br />STIS/CCD 9317<br /><br />Pure Parallel Imaging Program: Cycle 10.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to perform the default<br />archival pure parallel program for STIS during cycle 10.<br /><br />STIS/MA1/MA2 8920<br /><br />Cycle 10 MAMA Dark Measurements.<br /><br />The Space Telescope Imaging Spectrograph [MA1 and MA2] was used to perform the<br />routine monitoring of the MAMA detector dark noise, and is the primary means of<br />checking on health of the MAMA detectors systems through frequent monitoring of<br />the background count rate.<br /><br />WF/PC-2 9104<br /><br />A Study of Proplyds and a Protostellar Condensation at the Center of M20.<br /><br />The WF/PC-2 was used to observe the Trifid nebula {M20} that is a well-known<br />prominent optical HII region trisected by bands of obscuring dust lanes and<br />excited by an O7.5 star HD 164492A. Our recent study of near-IR ground-based<br />observations of this region at J, H, K and L show all seven components of HD<br />164492 {A to G} identified optically. Our sub-arcsecond radio continuum VLA and<br />ground- based observations of M20 also show free-free emission from three<br />stellar sources {B, C and D} and a bright rim outlining a protostellar<br />condensation {TC1} lying close to the O7V star {HD 164492A} at the center of the<br />nebula. Based on a number of strong arguments, these stars have disks associated<br />with them and their envelopes are photoionized externally by the UV radiation<br />from the hot central star, HD 164492A. These proposed WFPC2 observations are<br />intended to search for neutral protoplanetary disks ``proplyds'', to study the<br />optically bright rim of ionized gas associated with TC1 for signs of star<br />formation, and to make a detailed subarcsecond determination of extinction<br />toward the dust lanes of M20 using HAlpha and 6cm data.<br /><br />WF/PC-2 9050<br /><br />Outflow Collimation in Bipolar Symbiotic Nebulae.<br /><br />The WF/PC-2 was used to observe flow collimation in evolved stars that is<br />neither expected nor understood. Classical theories of stellar evolution do not<br />predict and cannot explain this bipolarity. More exotic concepts {binary<br />interactions, spun-up atmospheres, poloidal or toroidal magnetized winds} have<br />been proposed, but observations are yet to verify or falsify any of their<br />predictions. This proposal will probe the near-nuclear morphology and kinematics<br />of four bright, low-extinction targets whose large-scale structure is highly<br />bipolar. The goal is to provide a detailed description of the circumnuclear<br />outflows, to uncover the physical structure and nature of the collimator, and to<br />evaluate the speculative collimation mechanisms. The bright nucleus has hampered<br />efforts to explore the nebular collimators that lie close to the star, so we'll<br />use STIS to disperse the nuclear light and, thus, to avoid its glare. A<br />secondary goal is to obtain second-epoch WFPC2 images of all targets.<br /><br />WF/PC-2 9318<br /><br />POMS Test Proposal: WFII Parallel Archive Proposal Continuation.<br /><br />The WF/PC-2 was used to perform the generic target version of the WFPC2 Archival<br />Pure Parallel program. The program was used to take parallel images of random<br />areas of the sky, following the recommendations of the Parallels Working Group.<br /><br />WFPC2 8938<br /><br />WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3.<br /><br />This dark calibration program obtains 3 dark frames every day to provide data<br />for monitoring and characterizing the evolution of hot pixels.<br /><br />FLIGHT OPERATIONS SUMMARY<br /><br />HSTARs:<br /><br />8709 - NBOOTSAA CCL skip FOM commanding @170/1929zDuring recovery of NICMOS<br /> from SUSPEND, the CCL NBOOTSAA skipped the FOM homing commands.<br /> SISE advised FC to continue with commanding and OPS Request#16791 was<br /> modified to omit last step [position FOM, since already in correct location]<br /> with STScI Commanding concurrence. Note from SI SE: This HSTAR does not<br /> point towards an anomaly. It simply tracks changes that should be made to<br /> a CCL used in the NICMOS recovery from suspend. Summary: a telemetry check<br /> in the CCL needs to be moved up to allow more samples [major frames] prior<br /> to homing the FOM. At its' current position, there is a possibility that<br /> the telemetry check may get inaccurate data. We are also talking about<br /> adding a check to the COP for the FOM temperatures prior to executing this CCL.<br /> Under investigation.<br /><br />8710 - NBOOTSAA CCL skip FOM commanding @170/1929z [********HSTAR 8710 Rejected*****]<br /><br />8711 - BAY 6 TEMP SENSOR [TB6AESB] OOL LIMITS @172/1446z. Between 2002/172/14:46:16Z<br /> and 2002/172/15:20:00Z mnemonic TB6AESB [bay 6 aft ES bulkhead] violated its<br /> upper red temperature OOL high= 20.4354 deg C intermittently, and can be seen<br /> in attachments. PRD LIMITS -50.0/20.0 deg C. Y/R High Limit is +20.0 deg C.<br /> TCS on call notified. Last reported ref. HSTAR #8451. Under<br /> investigation.<br /><br />8712 - Bay 5 forward bulkhead temperature out of limit @172/2244z.Bay 5 ES Forward<br /> Bulkhead temperature TB5ESB broke limit briefly from 22:43:46 to 22:43:58,<br /> again from 22:44:04 to 22:51:04, and from 22:51:16 to 22:51:34, each time with<br /> a maximum value of 25.1561 DegC, limit is 25.0 DegC. On call TCS engineer<br /> notified. Under investigation.<br /><br />COMPLETED OPS REQs: None<br /><br />OPS NOTES EXECUTED:<br />1006-3 - AXIAL link2 Temp Limit Change @172/1335z<br />1014-1 - Main Baffle 3 Limit Adjust Closed[EMNBF3T Lim Restored] @174/0100z<br />1008-0 - Raise Battery 3 Upper Temp limit Closed[Lim Restored to 3.0deg] @174/2049z<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 19 19<br />FGS REacq 28 28<br />FHST Update 40 40<br />LOSS of LOCK None<br /><br />SIGNIFICANT EVENTS:<br />Reconditioned ESTR @ 175/00:45Z [ROP RD-7A].