#1
|
|||
|
|||
Daily 3595
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3595 PERIOD COVERED: DOYs 110-111 OBSERVATIONS SCHEDULED NIC3 9999 The COSMOS 2-Degree ACS Survey NICMOS Parallels The COSMOS 2-Degree ACS Survey NICMOS Parallels. This program is a companion to program 9822. NIC/NIC3 9865 The NICMOS Parallel Observing Program We propose to continue managing the NICMOS pure parallel program. Based on our experience, we are well prepared to make optimal use of the parallel opportunities. The improved sensitivity and efficiency of our observations will substantially increase the number of line-emitting galaxies detected. As our previous work has demonstrated, the most frequently detected line is Halpha at 0.7z1.9, which provides an excellent measure of current star formation rate. We will also detect star-forming and active galaxies in other redshift ranges using other emission lines. The grism observations will produce by far the best available Halpha luminosity functions over the crucial--but poorly observed--redshift range where galaxies appear to have assembled most of their stellar mass. This key process of galaxy evolution needs to be studied with IR data; we found that observations at shorter wavelengths appear to have missed a large fraction of the star-formation in galaxies, due to dust reddening. We will also obtain deep F110W and F160W images, to examine the space densities and morphologies of faint red galaxies. In addition to carrying out the public parallels, we will make the fully reduced and calibrated images and spectra available on-line, with some ground-based data for the deepest parallel fields included. NIC2 9845 NICMOS Confirmation of a Young Planetary-Mass Companion We have recently discovered a strong candidate for a planetary-mass {~10 Mjup} companion to a young Sun-like star, based on near-IR imaging and spectroscopy with the Keck and Subaru adaptive optics {AO} systems. While the ground-based data strongly suggest that the candidate has a very low effective temperature, and hence a very low mass, they are not definitive. We propose to obtain NICMOS coronagraphy to measure the companion's 1.9um water-band absorption. This feature is a distinct signature of very cool objects and is unobservable from the ground. The combined ground-based and space-based data set will determine whether the companion has a very low temperature, and hence if it is the lowest mass companion found to date by direct imaging. ACS/WFC/WFPC2 9822 The COSMOS 2-Degree ACS Survey We will undertake a 2 square degree imaging survey {Cosmic Evolution Survey -- COSMOS} with ACS in the I {F814W} band of the VIMOS equatorial field. This wide field survey is essential to understand the interplay between Large Scale Structure {LSS} evolution and the formation of galaxies, dark matter and AGNs and is the one region of parameter space completely unexplored at present by HST. The equatorial field was selected for its accessibility to all ground-based telescopes and low IR background and because it will eventually contain ~100, 000 galaxy spectra from the VLT-VIMOS instrument. The imaging will detect over 2 million objects with I 27 mag {AB, 10 sigma}, over 35, 000 Lyman Break Galaxies {LBGs} and extremely red galaxies out to z ~ 5. COSMOS is the only HST project specifically designed to probe the formation and evolution of structures ranging from galaxies up to Coma-size clusters in the epoch of peak galaxy, AGN, star and cluster formation {z ~0.5 to 3}. The size of the largest structures necessitate the 2 degree field. Our team is committed to the assembly of several public ancillary datasets including the optical spectra, deep XMM and VLA imaging, ground-based optical/IR imaging, UV imaging from GALEX and IR data from SIRTF. Combining the full-spectrum multiwavelength imaging and spectroscopic coverage with ACS sub-kpc resolution, COSMOS will be Hubble's ultimate legacy for understanding the evolution of both the visible and dark universe. ACS/WFC 9811 Establishing the Metallicity Distribution in Normal Giant Ellipticals NGC 3377 and 3379, the Leo Group ellipticals at d=11 Mpc, are the nearest E galaxies commonly regarded to be structurally"normal", and as such, they are keystone objects for understanding the evolution and early star formation history of large ellipticals. The ACS/WFC camera now gives us the ability to obtain the metallicity distribution function {MDF} of their stellar population by direct resolution and photometry of their halo stars. To do this, we will follow the same highly successful techniques we have previously used for NGC 5128 with WFPC2 {V, I} imaging: the {V-I} colors of the brightest red-giant stars are highly sensitive to metallicity, and their locations in the color-magnitude diagram can be used for direct construction of the MDF. This will be a major step forward to understanding the formation history of these cosmologically dominant galaxies. ACS/WFC 9788 A Narrow-band Snapshot Survey of Nearby Galaxies We propose to use ACS/WFC to conduct the first comprehensive HST narrow-band {H-alpha + [N II]} imaging survey of the central regions of nearby bulge-dominated disk {S0 to Sbc} galaxies. This survey will cover, at high angular resolution extending over a large field, an unprecedented number of galaxies representing many different environments. It will have important applications for many astrophysical problems of current interest, and it will be an invaluable addition to the HST legacy. The observations will be conducted in snapshot mode, drawing targets from a complete sample of 145 galaxies selected from the Palomar spectroscopic survey of nearby galaxies. Our group will use the data for two primary applications. First, we will search for nuclear emission-line disks suitable for future kinematic measurements with STIS, in order to better constrain the recently discovered relations between black hole mass and bulge properties. Preliminary imaging of the type proposed here must be done, sooner or later, if we are to make progress in this exciting new field. Second, we will investigate a number of issues related to extragalactic star formation. Specifically, we will systematically characterize the properties of H II regions and super star clusters on all galactic scales, from circumnuclear regions to the large-scale disk. ACS/HRC 9747 An Imaging Survey of the Statistical Frequency of Binaries Among Exceptionally-Young Dynamical Families in the Main Asteroid Belt We propose an ambitious SNAPSHOT program to determine the frequency of binaries among two very young asteroid families in the Main Belt, with potentially profound implications. These families {of C- and S-type} have recently been discovered {Nesvorny et al. 2002, Nature 417, 720}, through dynamical modeling, to have been formed at 5.8 MY and 8.3 MY ago in catastrophic impact events. This is the first time such precise and young ages have been assigned to a family. Main-belt binaries are almost certainly produced by collisions, and we would expect a young family to have a significantly higher frequency of binaries than the background, because they may not yet have been destroyed by impact or longer-term gravitational instabilities. In fact, one of the prime observables from such an event should be the propensity for satellites. This is the best way that new numerical models for binary production by collisions {motivated largely by our ground-based discoveries of satellites among larger asteroids}, can be validated and calibrated. We will also measure two control clusters, one being an "old" family, and the other a collection of background asteroids that do not have a family association, and further compare with our determined value for the frequency of large main-belt binaries {2%}. We request visits to 180 targets, using ACS/HRC. ACS 9294 Observations of the Host Galaxy of 3C 273 The highly luminous flat-spectrum QSO 3C 273 {z=0.158, V=12.8, M_V~-26.4} will be imaged with the WFC in the [O III]5007 and H-alpha emission lines with the narrow-band filters FR601N and FR782N, respectively. Off-band images in F475W and F850LP will also be acquired to accurately subtract the underlying galaxy continuum. Combined with the broad-band HRC coronagraphic images from the ERO program 8992, these new images will offer the most complete and detailed view yet of the host galaxy and environment of this QSO. NIC1/NIC2/NIC3 8792 NICMOS Post-SAA calibration - CR Persistence Part 3 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. The keyword 'USEAFTER=date/time' will also be added to the header of each POST-SAA DARK frame. The keyword must be populated with the time, in addition to the date, because HST crosses the SAA ~8 times per day so each POST-SAA DARK will need to have the appropriate time specified, for users to identify the ones they need. Both the raw and processed images will be archived as POST-SAA DARKSs. Generally we expect that all NICMOS science/calibration observations started within 50 minutes of leaving an SAA will need such maps to remove the CR persistence from the science images. Each observation will need its own CRMAP, as different SAA passages leave different imprints on the NICMOS detectors. WFPC2 10070 WFPC2 CYCLE 12 Supplemental Darks Part 2/3 This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. WFPC2 10068 WFPC2 CYCLE 12 Standard Darks This dark calibration program obtains dark frames every week in order to provide data for the ongoing calibration of the CCD dark current rate, and to monitor and characterize the evolution of hot pixels. Over an extended period these data will also provide a monitor of radiation damage to the CCDs. ACS/HRC/WFC 10060 CCD Daily Monitor 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. STIS/MA1 10034 Cycle 12 MAMA Dark Monitor This test performs the routine monitoring of the MAMA detector dark noise. This proposal will provide the primary means of checking on health of the MAMA detectors systems through frequent monitoring of the background count rate. The purpose is to look for evidence of change in dark indicative of detector problem developing. STIS/CCD 10022 STIS CCD Hot Pixel Annealing Cycle 12 The effectiveness of the CCD hot pixel annealing process is assessed by measuring the dark current behavior before and after annealing and by searching for any window contamination effects. In addition CTE performance is examined by looking for traps in a low signal level flat. Follows on from proposal 9612. STIS/CCD 10020 CCD Bias Monitor - Part 2 Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4, to build up high-S/N superbiases and track the evolution of hot columns. STIS/CCD 10018 CCD Dark Monitor-Part 2 Monitor the darks for the STIS CCD. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9386: GS Acquisition (2,3,2) @ 110/12:17:47Z failed to RGA control due to SRLE on FGS 2. Primary Search Radius = 30.0 arcsec. Prior FHST Roll Delay Update (U2,3RD) showed attitude errors: V1 = 20.913, V2 = -89.066, V3 = 15.6714 arcsec. Successful executed ARU/PRT @ 110/13:19:48Z to save subsequent GS Reacquisition @ 110/13:54:58Z (OR 17128 with COP 3.06). Under investigation. HSTAR 9387: OTA SE review of PTAS TC run for M_SA103O SMS, determined the GS Reacquisition (2,1,2) @ 105/01:04:57Z required two attempts on FGS 1 due to SSLEX during the first attempt. Under investigation. HSTAR 9398: Based on PCS SE input and review of PTAS TC run log for M_SA103O SMS, OTA SE confirms the GS Acquisition (1,2,1) @ 106/17:16:23Z achieved FL-DV on both FGSs @ 106/17:20:22Z, but then went to SSM control @ ~106/17:22:22Z. The LOL Recovery was successful and no further LOL was seen during the guiding period on these stars. Under investigation. COMPLETED OPS REQs: 17128-0 - ARU/PRT @ 110/1320z 17126-3 - Eclipse Management, GMT 110 @ 110/1843z 17127-1 - Continuation of FSW 2.5B On-Orbit Verification @ 110/1851z 17129-1 - ACS FSW CS4.0 Installation @ 111/2046z 17130-0 -Genslew for proposal 9906 - slot 13 @ 111/2308z 17131-0 -Genslew for proposal 9906 - slot 14 @ 111/2310z 17132-0 -Genslew for proposal 9906 - slot 1 @ 111/2313z 17133-0 - Genslew for proposal 9906 - slot 2 @ 111/2316z 17134-0 - Genslew for proposal 9906 - slot 3 @ 112/0708z OPS NOTES EXECUTED: 1223-0 - Delivery of ACS FSW CS4.0 Loads @ 110/2100z 1220-0 - Adjust Recharge Ratio Limits for High Sun DOY 2004/110-119 @ 110/2208z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 13 13 110/1217z (HSTAR # 9386) FGS REacq 19 19 110/1043z FHST Update 29 29 LOSS of LOCK SIGNIFICANT EVENTS: Day 110 Continued FSW 2.5b on-orbit verification (OR 17127-1 with attached script). FHST 1 was placed in Rate Control under FGS guiding from ~ 110/14:21Z - 14:35Z. FHSTs 1, 2, and 3 were placed in simultaneous Rate Control under FGS guiding from ~ 110/14:35Z - 14:50Z. FHST 3 was placed in Rate Control under RGA control from ~ 110/14:50Z - 15:05Z. FHST 2 was place in Rate Control under RGA control following the 110/17:00Z FM Update from ~ 110/18:38Z - 18:51Z. Solar Eclipse 110/13:47Z - 14:05Z and 110/15:36Z - 15:46Z (OR 17126-3 with attached ROP PS-02A and MEGG timeline). Temporarily disable the Rate of Charge and SA old Protection safemode tests. CCS timer was modified to prevent software logic from operating as if a CSS failure occurred due to the eclipse. With Trickle Charge verified, reset the safemode tests and CSS timer to their nominal state @ 110/18:44Z. Preliminary results from limited real-time data appear to indicate Trickle Charge was reached during both eclipse periods. Successfully executed ARU/PRT @ 110/13:19:48Z to save subsequent GS Reacquisition @ 110/13:54:58Z (OR 17128 with COP 3.06). See HSTAR 9386. ACS FSW CS4.0 EEPROM installation and verification 111/10:12Z - 20:38Z (OR 17129-1 with attached script). This FSW change will improve the ability of the ACS to position its Filter Wheel more reliably. The FSW will be loaded into EEPROM while the ACS remains in Operate Mode. ACS will remain under ACS FSW CS3.0CF control until ACS transition to Anneal Mode @ ~116/09:00Z and then back to Operate Mode @ ~116/22:00Z, at which time the new FSW CS4.0 will be loaded into EDAC memory and initiated. Day 111 Successfully completed ACS FSW 4.0 uplink (segments 1 – 199) to EEPROM memory @ 111/20:46Z [OR 17129-1 with attached ACS FSW Version 4.0 Install Procedure (EEPROM)]. No errors or problems were encountered during the loading process. The new image now resides in the ACS EEPROM. Post-install memory dump was completed and transferred to the Payload FSW Team. No discrepancies or differences were found with the newly loaded ACS FSW CS4.0 image. When ACS emerges from its monthly anneal cycles ~116/22:00Z, the new FSW will be activated. ACS EEPROM dump was executed @097/22:00Z (OR 17120). ACS EEPROM dump CSIJ04097215708.EFS was collected and transferred to the FSW Team; analysis completed and contents were verified to match ground image. |
Thread Tools | |
Display Modes | |
|
|
Similar Threads | ||||
Thread | Thread Starter | Forum | Replies | Last Post |
Monitoring NASA Daily ISS Report | JimO | Space Station | 2 | June 1st 04 10:33 PM |
JimO Speaks on 'Daily Planet' re Hubble | JimO | Policy | 0 | February 11th 04 11:53 PM |
Spirit's daily activities schedule? | Matti Anttila | Policy | 0 | January 15th 04 09:39 AM |
best site for daily schedule of rover activity? | bob | History | 2 | January 5th 04 01:16 PM |
Investor's Business Daily: Rethinking NASA | dougk | Policy | 1 | August 28th 03 12:07 AM |