HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3133<br /><br />PERIOD COVERED: DOY 158-160: 0000Z [UTC] 06/07/02 - 0000Z [UTC] 06/09/02<br /><br />OBSERVATIONS SCHEDULED AND ACCOMPLISHED:<br /><br />9353<br /><br />Direct imaging of the progenitors of massive, core-collapse supernovae<br /><br />Modern supernovae searches in the nearby Universe are discovering vast numbers<br />of SNe which have massive star progenitors {Types II, Ib and Ic}. The extensive<br />HST {and ground-based} image archives of galaxies within ~20 Mpc enables their<br />individual bright stellar content to be resolved. As massive, evolved stars are<br />the most luminous single objects in a galaxy, the progenitors of core-collapse<br />SNe should be directly detectable on pre-explosion images. Within the last year<br />we have set direct mass limits on the progenitors of two SNe Type II-P by<br />analyzing pre-explosion archive images and follow up HST exposures. We have now<br />identified six other recent, nearby SNe which have WFPC2 archive exposures of<br />the site taken before explosion. Additionally, our Cycle 10 SNAP program will<br />double the WFPC2 image archive of nearby galaxies which significantly increases<br />the chances of having multi-colour photometry of pre-explosion sites for future<br />SNe. In this Cycle, we request time on two fronts. Firstly we require imaging of<br />the six SNe with existing pre-explosion data in order to perform exact<br />astrometry of the SNe positions to around 0.05''. Secondly, as a follow on from<br />our two successful Cycle 10 programs, we request ToO status for any nearby<br />core-collapse SN which explodes during Cycle 11 and which has pre-explosion HST<br />images. The goal of this proposal is to directly identify the progenitor stars<br />of core-collapse SNe.<br /><br />ACS 9027<br /><br />ACS SBC Geometric Distortion Calibration<br /><br />This activity will obtain a series of images to evaluate the geometric<br />distortion over the field of view of the ACS SBC channel, after its image<br />quality has been optimized with the corrector mechanism. Images will be obtained<br />in filter F125LP, with a pattern of POS-TARG offsets in each axis. These data<br />will be complemented by the images of the same field obtained in proposal 9024,<br />"ACS SBC Flat Field Strability", which utilizes a similar image offsetting<br />technique at larger spatial scales. The observations may be scheduled<br />back-to-back with those from proposal 9024. NGC 6681 {18.7 h, -32 deg} will be<br />the target, as this star field has been used extensively by the STIS program for<br />UV PSF measurement and photometry<br /><br />ACS 9476<br /><br />Galaxy Evolution in the Richest Clusters at z=0.8: the EDisCS Cluster Sample<br /><br />The study of distant cluster galaxies requires two key ingredients: {1} deep<br />high-resolution imaging, to constrain galaxy structure; and {2} 8m-class<br />spectroscopy, to measure stellar content, star-formation rates, dynamics, and<br />cluster membership. We will reach both conditions with the addition of HST/ACS<br />imaging to our suite of VLT {36 nights} and NTT {20 nights} observations of 10<br />confirmed clusters at z~0.8, drawn from the ESO Distant Cluster Survey {EDisCS}.<br />The proposed HST/ACS data will complement our existing optical/IR imaging and<br />spectroscopy with quantitative measures of cluster galaxy morphologies {i.e.<br />sizes and shapes, bulge-disk decompositions, asymmetry parameters}, and with<br />measurements of cluster masses via weak lensing. Major advantages unique to the<br />EDisCS project include: {i} uniform selection of clusters; {ii} large enough<br />sample sizes to characterize the substantial cluster-to-cluster variation in<br />galaxy populations; {iii} large quantities of high quality data from 8m<br />telescopes; {iv} uniform measurements of morphologies, spectroscopic and<br />photometric redshifts, SEDs, star-formation/AGN activities, and internal<br />kinematics; {v} optical selection of clusters to complement the X-ray selection<br />of almost all high-z clusters in the ACS GTO programs; {vi} forefront numerical<br />simulations designed specifically to allow physical interpretation of observed<br />differences between the high-z and local clusters.<br /><br />ACS 9395<br /><br />Is Bulge Formation Still Going-On? An ACS Survey of Pseudo-Bulges<br /><br />Pseudo-bulges, i.e., bulges with an exponential light profile, have been<br />unveiled in the centers of many intermediate-type disks. Their structural<br />similarity with the disks provides support to theoretical scenarios in which<br />bulges may form due to secular evolution processes within the host disks. If at<br />play, these processes would likely be active throughout a large fraction of<br />cosmic history down to our days: `young' bulges should exist. Our previous HST<br />WFPC2 and NICMOS survey of ~100 spirals has provided V-H colors for 11 Sb-Sc<br />pseudo-bulges, and these could be interpreted as suggestive of relatively young<br />stellar ages. Furthermore, dense nuclei have been discovered in these<br />pseudo-bulges, and their V-H colors may imply stellar masses sufficiently large<br />to activate the formation of the pseudo- bulge by means of dynamical dissolution<br />of progenitor bars. However, the V-H color, on its own, is fully degenerate<br />towards stellar ages, metallicities and masses, as well as dust content. We<br />therefore propose to use ACS to observe the 11 pseudo-bulges of our combined<br />WFPC2 and NICMOS sample in the F330W, F435W, and F814W filters. Extending the<br />wavelength baseline to the bluer passbands is essential to break the<br />mass-age-metallicity-dust degeneracy, and will provide far more accurate<br />estimates for the stellar population properties of the pseudo-bulges and their<br />nuclei. Proving the existence of `young' bulges in the local Universe would have<br />a big impact in our understanding of the formation of the Hubble sequence.<br /><br />ACS 9024<br /><br />SBC flat field uniformity<br /><br />The stability and uniformity of the low-frequency flat fields {L-flat} of all<br />ACS detectors will be assessed by using multiple pointing observations of the<br />globular cluster NGC6681 - thus imaging moderately dense stellar fields. By<br />placing the same star over different portions of the detectors and measuring<br />relative changes in its brightness it will be possible to determine local<br />variations in the response of the detectors. Based on previous experience with<br />STIS, it is deemed that a total of nine different pointings will suffice to<br />provide adequate characterization of the flat field stability in any given band.<br />For each filter to be tested, the baseline consists of 9 pointings with steps of<br />~20% of the FOV in a diagonal cross pattern. During SMOV, the complement of<br />filters to be tested is limited to the following: for the SBC, F125LP and<br />F150LP. In order to provide complementary data for the geometric distortion<br />programmes {9027 and 9028}, and also to check that the distortion is not<br />chromatic, three additional exposures will be taken with F125LP with a very<br />small {~10 pixel} offset from the centre {see proposals 9027 and 9028}.<br />Execution of this programme must await completion of programme 9011 {ACS to FGS<br />alignment} and the ensuing PDB update.<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 9473<br /><br />Masses and IMF Variations in Super Star Clusters<br /><br />We are proposing to obtain high spatial resolution images of a set of super star<br />clusters for which we have been granted observing time to measure velocity<br />dispersions via high- resolution ground-based optical echelle and K-band<br />spectroscopy. The images will allow us to fit the light profiles and measure the<br />radii of the clusters, and when combined with the velocity dispersions, will<br />enable us to estimate the cluster masses. By comparing the mass-to-light ratios<br />with those predicted from spectral synthesis models, we will investigate<br />possible variations in the slope and lower mass cut-offs of the initial mass<br />functions in these clusters. Correlations of the variations of these parameters<br />with cluster environment may provide insight into the formation mechanisms for<br />super star clusters. By comparing the light profiles obtained in a blue and red<br />filter, we will also search for evidence of mass segregation in the clusters.<br />Since these clusters are too young to have experienced dynamical mass<br />segregation, differences in the light profiles of the clusters in the two<br />filters could be due to processes that differentiate between high and low mass<br />stars during the birth of the clusters and would provide further constraints on<br />theoretical models of cluster formation. Since these clusters are far too<br />compact to be resolved by any ground-based observations, the ACS/HRC on board<br />HST is the only instrument capable of carrying out these observations.<br /><br />ACS/HRC 9020<br /><br />Preliminary ACS Sensitivity.<br /><br />The Advanced Camera for Surveys [HrC] was used to observe a spectrophotometric<br />standard star through each filter of each camera to assess the sensitivity of<br />the instrument. The star is placed at the center of the aperture, and two images<br />are taken through each filter.<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 8947<br /><br />Weekly Test.<br /><br />The Advanced Camera for Surveys [WFC and HRC] was used to perform basic tests to<br />monitor, the read noise, the development of hot pixels and test for any source<br />of noise in ACS CCD detectors. This program will be executed at least once a day<br />for the entire lifetime of ACS.<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 />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 8986<br /><br />NICMOS Photometry Test<br /><br />This proposal contains the necessary exposures to re-calibrate NICMOS.<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 9328<br /><br />Comprehensive STIS Spectroscopy of the Supernova Remnant 1987A's Formation<br /><br />The visible consequences of the hard shock of the impact of SN 1987A's ejecta<br />upon the inner circumstellar ring are apparent and developing rapidly. Over the<br />past year, this phenomenon has made a transition, from emission originating in<br />just a few "hot spots" at restricted locations in position angle {PA} around the<br />ER, to a collision producing optical emission over a nearly continuous<br />distribution {with few breaks larger than 45 degrees in PA} and indications of<br />low-level emission arising from nearly all PAs. We propose a modest but<br />effective program to trace superbly the development of the entire interaction<br />region by drawing on capabilities of STIS which are well-matched to the task,<br />and on the strength of comparison with existing STIS data.<br /><br />STIS 9619<br /><br />Echelle Blaze Shift vs. MSM Monthly Offset<br /><br />In the near future, monthly MSM offsets will probably be disabled for STIS<br />echelle gratings, alleviating to some extent calibration problems associated<br />with the monthly offsets. The data from this program will be used to improve<br />empirical and optical models relating wavelength and blaze function shifts.<br />These models will in turn be used to improve the calibration of archival echelle<br />data obtained while monthly MSM offsets were enabled. The flux standard HZ43<br />will be observed with the E230H echelle grating at a central wavelength of 2513<br />Angstroms. Five exposures will be obtained, each with a different monthly offset<br />applied to the Mode Select Mechanism {MSM}.<br /><br />STIS 8643<br /><br />Ultraviolet Properties of the Metal Rich M87 Globular Cluster System<br /><br />We propose to use STIS imaging to obtain far-ultraviolet photometry of the metal<br />rich globular cluster system of the elliptical galaxy M87. This system<br />represents a key link between the well understood populations of the clusters<br />and the hot stars in elliptical galaxies, where our physical insight is<br />presently limited. Our goal is to establish the relationship between cluster<br />metal abundance and the production of UV-bright populations of stars on the<br />``extreme horizontal branch'' at T{eff} > 16000K. These stars are the source of<br />the surprising ``ultraviolet-upturn'' phenomenon in elliptical galaxies. Our<br />observations will fill a major gap in the present coverage of cluster metal<br />abundances. This would be an important step in understanding the dependence of<br />the upturn on its parent stellar population. A basic motivation is the<br />expectation that the UV-upturn could be the most sensitive probe of the ages and<br />abundances of elliptical galaxy populations. We plan to observe 3 fields in M87,<br />which will provide a sample of ~ 30--50 UV-detected objects in the brightest 3<br />magnitudes of its cluster luminosity function. The program is technically<br />challenging but appears feasible. Relatively long integrations are needed, under<br />conditions of minimum dayglow emission from Earth's atmosphere.<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 8908<br /><br />CCD Imaging Flats C10.<br /><br />The Space Telescope Imaging Spectrograph [CCD] was used to investigate<br />flat-field stability over a monthly period.<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 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 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/CCD/MA1 9067<br /><br />UV Detectability of Bright Quasars in the Sloan Fields.<br /><br />The Space Telescope Imaging Spectrograph [CCD and MA1] was used to take MAMA<br />spectra of approximately 30 new, bright, high-redshift quasars in each of the<br />next three cycles.<br /><br />WF/PC-2 9043<br /><br />Cepheid Distances to Early-type Galaxies.<br /><br />The WF/PC-2 was used to continue observations in the HST Key Project on the<br />Extragalactic Distance Scale and the HST project on the "Calibration of Nearby<br />Type Ia Supernovae'' that have greatly improved our knowledge of the Hubble<br />Constant by providing a solid zero point for the Tully- Fisher {TF} relation and<br />Type Ia Supernovae {SNIa}. However, severe inconsistencies remain for distance<br />estimators to early-type galaxies such as surface brightness fluctuations {SBF},<br />the planetary nebula luminosity function {PNLF}, the fundamental plane {FP}, and<br />the globular cluster luminosity function {GCLF}. As a result, the distance to<br />the Virgo cluster core remains uncertain by as much as 20 determination is<br />directly affected by a lingering 0.1 mag {5 uncertainty in the photometric<br />calibration of the WFPC2. Resolving these issues is essential not only to firm<br />up the extragalactic distance scale, but also to understand the mass and<br />velocity structure of the local universe. SBF in particular is emerging as the<br />method of choice for mapping local velocity fields to 10, 000 kms because it<br />offers an order of magnitude less Malmquist bias than TF, and SNIa are too rare<br />to study large scale flows effectively. This project will tighten the<br />photometric calibration of the WFPC2, and provide a solid Cepheid calibration<br />for SBF and PNLF.<br /><br />WF/PC-2 9157<br /><br />Fundamental Properties Of L-Type Dwarfs In Binaries.<br /><br />The WF/PC-2 was used to characterize the physical properties of eight L-dwarfs<br />in four binary systems. The goal is to obtain astrometric, photometric and<br />spectroscopic measurements of each component that will yield basic information<br />on atmospheric and dynamical properties.<br /><br />WF/PC-2 9345<br /><br />Fundamental Properties of L-type Dwarfs in Binaries.<br /><br />The WF/PC-2 was used to characterize the physical properties of eight L-dwarfs<br />in four binary systems. The goal is to obtain astrometric, photometric and<br />spectroscopic measurements of each component that will yield basic information<br />on their atmospheric and dynamical properties.<br /><br />WF/PC-2 9180<br /><br />Gamma-ray Burst Progenitors: Probing Their Environment.<br /><br />The WF/PC-2 was used to perform a target of opportunity observation of gamma ray<br />burster [GRB], GRB-011121. GRB astronomy is a field maturing at a phenomenal<br />rate. Three important new observational and theoretical discoveries, formulated<br />over the last twelve months, allow the proposer to address new, and in many<br />cases, more sophisticated questions than could have been posed previously. These<br />developments: the discovery of X-ray lines in GRB 991216; the observation that<br />N_H as deduced from X-ray afterglow are one to two orders of magnitude larger<br />than the dust extinction inferred from optical afterglow; and the growing<br />realization that the afterglow emission may exhibit features of dust echoes,<br />appear to offer unexpected and new diagnostics that will directly inform us<br />about the progenitor, the circum-progenitor material and the immediate<br />interstellar environs.<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 9319<br /><br />POMS Test Proposal: WFII Backup Parallel Archive Proposal II.<br /><br />The WF/PC-2 was used to execute a POMS test proposal, designed to simulate<br />future scientific plans.<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. FLIGHT OPERATIONS<br />SUMMARY:<br /><br />HSTARs: [for further details see ]http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf]<br />8682 GRG2_3GT out of limits @ 158/10:56:27z<br />8683 GRG2_4GT out of limits @ 158/13:26:00z<br />8684 C string FOF queue buffer overflow errors @ 158/18:46:00z<br /><br />8685 Gyro 3 Motor Current OOL 158/22:44:33 GRG2_3MC [RGA 2-3 Motor current]<br /> flagged out of limits yellow high at EV=232.4mA. At 22:44:39 it flagged out<br /> red high at EV= 330.4mA. At 22:45:51 it flagged out yellow high EV= 252mA and<br /> went back inbounds at 158/22:46:03. The yellow limits L=195 H=220. The red limits<br /> L=70 H=270. During the time of the OOL we were not guiding, we were in orbit day and<br /> we were not in a SAA. The following Reacqs using gyro 3 were successful. Motor<br /> safemode test count reached 1795 which is equivalent to 45 seconds of a 90 second timer.<br /> PCS SE, MOSES, and NASA on call were contacted. Under investigation.<br /><br />8686 GSACQ[1,3,3] Fine Lock backup on FGS 3, scan step limit on FGS 1 @ 160/05:08:20z<br />8687 486 status buffer message D08, SYSTEM_MOMENTUM_LIMIT_EXCEEDED @ 160/160/23:44:37z<br />8688 Core Data Server /CCS Process /Ccl Isp alarm @ 160/03:03:00z<br /><br />COMPLETED OPS REQs:<br />16786-2 NICMOS EEPROM Dump @ 158/1316z<br /><br />OPS NOTES EXECUTED:<br />0900-1 Command Problem<br />0900-1 Command Problem<br />1012-0 Change Limits MAMA1Threshold Voltage<br />1013-0 Gyro 3 and 4 Temperature Adjust<br />0996-1 Raise Battery Temperature Upper limits to 2 deg<br />1012-1 Change Limits MAMA1Threshold Voltage<br />0916-0 Tabulation of Slew Attitude Error [Miss-distance]<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 28 28<br />FGS REacq 26 26<br />FHST Update 52 52<br />LOSS of LOCK None<br /><br />COMMENTS:<br />1. TTR #'s have been replaced by CDS #'s and DR #'s. Generic problems have CDS #'s.<br /> Any problem may have a unique DR #. A given occurrence of a generic problem will<br /> have a CDS #, but may or may not have a DR # assigned by CSC.<br />2. Loads for SA161M02_F1 are approved and available on CCS-C & CCS-B.<br />3. ESB code d08 is "System momentum exceeded limit" [Ref: HSTAR # 8687]<br />4. No new OOL values for gyro 3 current have been observed since HSTAR # 8685.<br /><br />Continuation of Servicing Mission Orbital Verification and the gradual<br />resumption of normal science observations and calibrations.