HUBBLE SPACE TELESCOPE<br /><br />DAILY REPORT # 3125<br /><br />PERIOD COVERED: 0000Z {UTC} 05/27/02 - 0000Z {UTC} 05/28/02<br /><br />OBSERVATIONS SCHEDULED AND ACCOMPLISHED:<br /><br />STIS/CCD 8572<br /><br />Identifying Normal Galaxies at 1.3 < z < 2.5.<br /><br />The Space Telescope Imaging Spectrograph {CCD} was used to perform studies of<br />faint, distant galaxies. It is now possible to observe hundreds of galaxies out<br />to z=1 and in the range 3 < z < 4.5, yet the redshift range 1 < z <3 remains<br />largely unexplored.<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.<br />Dark frames will be obtained immediately upon exiting the SAA contour 23, and<br />every time a NICMOS exposure is scheduled within 50 minutes of coming out of the<br />SAA. The darks will be obtained in parallel in all three NICMOS Cameras. The<br />POST-SAA darks will be non-standard reference files available to users with a<br />USEAFTER date/time mark.<br /><br />STIS/CCD 8902<br /><br />Dark Monitor-Part 2.<br /><br />STIS/CCD 8904<br /><br />Bias Monitor-Part 2.<br /><br />2x2 bin settings at gain=1, and 1x1 at gain = 4 in order to build up high-S/N<br />superbiases and track the evolution of hot columns.<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 />WF/PC-2 8941<br /><br />Cycle 10 UV Earthflats.<br /><br />The WF/PC-2 was used to monitor flat field stability by obtaining sequences of<br />earth streak flats to improve the quality of pipeline flat fields for the WFPC2<br />UV filter set.<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 />STIS/CCD/MA1 9182<br /><br />The Thermal Glow of Gamma Ray Pulsar.<br /><br />The Space Telescope Imaging Spectrograph {CCD and MA1} was used to perform time-<br />and energy- resolved UV observations of two young Gamma-ray pulsars. The<br />targets, the Vela and Geminga pulsars, are the brightest neutron stars spanning<br />the critical 10^4-10^6y age range, where the thermal surface emission is<br />detectable. The UV light curves obtained will provide phase-resolved colors that<br />will isolate this thermal emission and test the equation of state and<br />fundamental interactions of matter at supernuclear densities. In addition,<br />combining the UV results with IR/optical and X-ray data, the proposers will map<br />spectral variations in the non-thermal pulsations and probe the acceleration<br />physics of these GeV gamma-ray machines.<br /><br />WF/PC-2 9258<br /><br />Observatory Focus Monitor.<br /><br />The WF/PC-2 was used to more accurately define the HST focus. The HST focus<br />drifts slowly and shows evidence of undergoing slips of a few microns at random<br />times. The rate of the WF/PC-2 monitoring program is insufficient to track<br />and/or understand OTA behavior in order to request timely and appropriate<br />Secondary Mirror corrections.<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 />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 />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 />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 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/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 9586<br /><br />ACS Polarization Calibration<br /><br />This proposal aims to calibrate the polarization modes most heavily used in<br />Cycle 11. We need L-flat observations, observations of a polarized star and an<br />unpolarized star, and an observation of an extended polarized source.<br /><br />WFPC2 9634<br /><br />POMS Test Proposal: WFII targeted parallel archive proposal<br /><br />The parallel opportunities available with WFPC2 in the neighborhood of bright<br />galaxies are treated in a slightly different way from the normal pure parallels.<br />Local Group galaxies offer the opportunity for a closer look at young stellar<br />populations. Narrow-band images in F656N can be used both to identify young<br />stars via their emission lines, and to map the gas distribution in star-forming<br />regions. Thus, the filter F656N is added to the four standard filters. Near more<br />distant galaxies, up to about 10 Mpc, we can map the population of globular<br />clusters; for this purpose, F300W is less useful, and only F450W, F606W, and<br />F814W will be used.<br /><br />FLIGHT OPERATIONS SUMMARY:<br /><br />HSTARs:<br />8664 - C-String CoredataServer ISP @147/0241z<br />8665 - ispnul problem @148/0150z<br /><br />COMPLETED OPS REQs: None<br /><br />OPS NOTES EXECUTED: None<br /><br /> SCHEDULED SUCCESSFUL FAILURE TIMES<br />FGS GSacq 6 6<br />FGS REacq 10 10<br />FHST Update 18 18<br />LOSS of LOCK None<br /><br />Operations Notes: None<br /><br />SIGNIFICANT EVENTS:<br /><br />Continuation of Servicing Mission Orbital Verification and the gradual<br />resumption of normal science observations and calibrations.