HUBBLE SPACE TELESCOPE<br /><br /><br />DAILY REPORT # 3369<br /><br /><br />PERIOD COVERED: DOY 142<br /><br /><br />OBSERVATIONS SCHEDULED<br /><br /><br />WF/PC-2 9173<br /><br /><br />The Pattern of Heavy Element Abundances in a Damped LyAlpha Galaxy.<br /><br /><br />The WF/PC-2 was used to observe the quasar PKS 1127-143. X-ray absorption<br />associated with an intervening 21-cm and damped LyAlpha$ absorber at z=0.312 in<br />its spectrum has been detected with Chandra. The advantage of the X- ray<br />measurement is that the derived metallicity is insensitive to ionization,<br />inclusion of an atom in a molecule, or depletion onto grains. The X-ray<br />absorption is mostly due to oxygen, and the abundance agrees with the oxygen<br />abundance of 16-40 lines in a galaxy at the redshift of the absorber. The STIS<br />spectrum will allow measurement of Zn II, an undepleted iron peak element.<br />Comparison of the oxygen group measured in the X-rays with the iron peak nuclei<br />measured will reveal whether the absorber has a Pop II, halo-type abundance<br />pattern or a Pop I, disk-like abundance pattern.<br /><br /><br />ACS/WFC 9351<br /><br /><br />Determining Hubble's Constant from Observations of Cepheids in the Host Galaxy<br />of SN Ia 1994ae<br /><br /><br />We propose to determine the luminosity of the type Ia supernova {SN Ia} 1994ae<br />by observing Cepheids in the host spiral galaxy NGC 3370. Modern CCD photometry<br />has yielded an extremely tight Hubble diagram for SNe Ia with a precisely<br />determined intercept {i.e., Delta H_0/H_0} 1 measurement of the true Hubble<br />constant is still limited by the calibration. The HST calibration of all but a<br />few SNe Ia observed to date is significantly compromised by the systematics of<br />photographic photometry and host galaxy extinction, as well as by the<br />photometric uncertainties associated with WFPC2. In contrast, SN 1994ae is one<br />of the very best-observed SNe Ia with CCD photometry. The exquisite B, V, R, and<br />I light curves are well-sampled beginning 10 days before maximum brightness, and<br />they indicate little reddening. From our supernova photometry and the current<br />provisional SN Ia calibration we would find a distance of 30 +/- 2.1 Mpc, well<br />within the range where ACS can accurately observe Cepheid light curves and<br />distinguish Cepheids from nonvariable stars.<br /><br /><br />NICMOS/STIS CCD 9405<br /><br /><br />The Origin of Gamma-Ray Bursts<br /><br /><br />The rapid and accurate localization of gamma-ray bursts {GRBs} promised by a<br />working HETE-2 during the coming year may well revolutionize our ability to<br />study these enigmatic, highly luminous transients. We propose a program of HST<br />and Chandra observations to capitalize on this extraordinary opportunity. We<br />will perform some of the most stringent tests yet of the standard model, in<br />which GRBs represent collimated relativistic outflows from collapsing massive<br />stars. NICMOS imaging and STIS CCD spectroscopy will detect broad atomic<br />features of supernovae underlying GRB optical transients, at luminosities more<br />than three times fainter than SN 1998bw. UV, optical, and X-ray spectroscopy<br />will be used to study the local ISM around the GRB. Chandra spectroscopy will<br />investigate whether the GRB X-ray lines are from metals freshly ripped from the<br />stellar core by the GRB. HST and CTIO infra-red imaging of the GRBs and their<br />hosts will be used to determine whether `dark' bursts are the product of<br />unusually strong local extinction; imaging studies may for the first time locate<br />the hosts of `short' GRBs. Our early polarimetry and late-time broadband imaging<br />will further test physical models of the relativistic blast wave that produces<br />the bright GRB afterglow, and will provide unique insight into the influence of<br />the GRB environment on the afterglow.<br /><br /><br />ACS/WFPC2 9481<br /><br /><br />Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS Survey<br />Fields<br /><br /><br />In anticipation of the allocation of ACS high-latitude imaging survey{s}, we<br />request a modification of the default pure parallel program for those WFPC2<br />parallels that fall within the ACS survey field. Rather than duplicate the red<br />bands which will be done much better with ACS, we propose to observe in the<br />near-ultraviolet F300W filter. These data will enable study of the rest-frame<br />ultraviolet morphology of galaxies at 0<z<1. We will determine the morphological<br />k-correction, and the location of star formation within galaxies, using a sample<br />that is likely to be nearly complete with multi-wavelength photometry and<br />spectroscopic redshifts. The results can be used to interpret observations of<br />higher redshift galaxies by ACS.<br /><br /><br />ACS 9482<br /><br /><br />ACS Pure Parallel Lyman-Alpha Emission Survey {APPLES}<br /><br /><br />Ly-alpha line emission is an efficient tool for identifying young galaxies at<br />high redshift, because it is strong in galaxies with young stars and little or<br />no dust --- properties expected in galaxies undergoing their first burst of<br />star- formation. Slitless spectroscopy with the ACS Wide-Field Camera and G800L<br />grism allows an unmatched search efficiency for such objects over the<br />uninterrupted range 4 <~ z <~ 7. We propose the ACS Pure Parallel Ly-alpha<br />Emission Survey {``APPLES''}, to exploit this unique HST capability and so<br />obtain the largest and most uniform sample of high redshift Ly-alpha emitters<br />yet. Parallel observations will allow this survey to be conducted with minimal<br />impact on HST resources, and we will place reduced images and extracted spectra<br />in the public domain within three months of observation. We aim to find ~ 1000<br />Ly-alpha emitters, 5 times the biggest current sample of Ly-alpha emitters. This<br />unprecedented sample will provide robust statistics on the populations and<br />evolution of Ly-alpha emitters between redshifts 4--7; a robust measurement of<br />the reionization redshift completely independent of the Gunn-Peterson trough;<br />spatial clustering information for Ly-alpha emitters which would let us probe<br />their bias function and hence halo mass as a function of redshift; many galaxies<br />at redshift exceeding 6; and lower redshift serendipitous discoveries.<br /><br /><br />ACS 9583<br /><br /><br />The Great Observatories Origins Deep Survey: Imaging with ACS<br /><br /><br />We propose a Treasury program of ACS imaging as part of the Great Observatories<br />Origins Deep Survey {GOODS}, covering 320{square}', or 32* the area of the two<br />original WFPC2 HDFs, to within 0.5--0.8 mag of their depth in four ACS bands,<br />BViz. The two GOODS fields, the Hubble Deep Field North and Chandra Deep Field<br />South, are the premier deep survey areas from X-- ray to radio wavelengths. ACS<br />data will provide unique angular resolution, sensitivity, and wavelength<br />coverage to close the gap between the deepest Chandra and SIRTF observations.<br />Supported by extensive imaging and spectroscopy from the VLT, Keck, Subaru,<br />NOAO, Gemini, VLA, JCMT, and other facilities, the combined GOODS data set will<br />make it possible to map the evolution of the Hubble sequence with redshift,<br />reconstruct the history of galaxy mass assembly, star formation and nuclear<br />activity from the epoch of reionization to the present, trace the growth of<br />density perturbations via cosmic shear, and, with properly phased z--band<br />observations, detect ~ 12 Type Ia supernovae at 1.2<z<1.8 to test the cosmic<br />acceleration and the presence of dark energy. All HST, SIRTF, Chandra, and<br />supporting GOODS data are non-- proprietary, with science--quality images and<br />catalogs released on a timescale of months. This will constitute the deepest,<br />largest, and most uniform panchromatic data set ever assembled to study the<br />distant universe.<br /><br /><br />WFPC2 9594<br /><br /><br />WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt2/3<br /><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 /><br />STIS 9606<br /><br /><br />CCD Dark Monitor-Part 2<br /><br /><br />Monitor the darks for the STIS CCD.<br /><br /><br />STIS 9608<br /><br /><br />CCD Bias Monitor - Part 2<br /><br /><br />Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1<br />at gain = 4, to build up high-S/N superbiases and track the evolution of hot<br />columns.<br /><br /><br />ACS 9674<br /><br /><br />CCD Daily Monitor<br /><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 /><br />STIS 9708<br /><br /><br />STIS Pure Parallel Imaging Program: Cycle 11<br /><br /><br />This is the default archival pure parallel program for STIS during cycle 11.<br /><br /><br />WFPC2 9709<br /><br /><br />POMS Test Proposal: WFII parallel archive proposal<br /><br /><br />This is the generic target version of the WFPC2 Archival Pure Parallel program.<br />The program will be used to take parallel images of random areas of the sky,<br />following the recommendations of the 2002 Parallels Working Group.<br /><br /><br />WFPC2 9710<br /><br /><br />POMS Test Proposal: WFII backup parallel archive proposal<br /><br /><br />This is a POMS test proposal designed to simulate scientific plans.<br /><br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br /><br />Significant Spacecraft Anomalies: [The following are preliminary reports of<br />potential non-nominal performance that will be investigated.] None<br /><br /><br />COMPLETED OPS REQs: None<br /><br /><br />OPS NOTES EXECUTED: None<br /><br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 5 5 <br />FGS REacq 10 10<br />FHST Update 10 10<br />LOSS of LOCK<br /><br /><br />SIGNIFICANT EVENTS:<br />HST FSW 2.3c Ops Acceptance Test for RAM installation, back out, and EEPROM<br />installation scheduled 143/10:00Z - 144/01:00Z with GDOC, HITT, SE, and VEST<br />using CCS "B" and "C" Strings with CCS Release 4.0.2.2 and PRD O06100R1T.<br />The purpose of this testing is to verify installation and back out procedures<br />for the RAM version of FSW 2.2c and EEPROM installation procedure in an<br />operational scenario.