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Daily 3622
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3622 PERIOD COVERED: DOY 148 OBSERVATIONS SCHEDULED ACS 10058 Improved wavelength calibration for the WFC G800L grism ACS G800L observations of an emission line star {the WC Wolf-Rayet star WR96} and a compact planetary nebula {LMC-SMP81} will be obtained to provide improved coverage of the field variation of the dispersion solution for the WFC and G800L grism. A direct image and a corresponding grism image will be taken at many different positions across the WFC field. By fitting the emission lines, the field dependence of the wavelength zero point and dispersion will be measured. The WR star was already used in Cycle 11 calibrations and these observations provide improved spatial coverage to map the variation of the dispersion with position. The observations of the fainter planetary nebula provide an independent wavelength calibration for a few points over the field. ACS/HRC 9851 Host Galaxies of Reverberation-Mapped AGNs We propose to obtain unsaturated ACS high-resolution images of all reverberation-mapped active galactic nuclei in order to remove the point-like nuclear light from each image, thus yielding a "nucleus-free" image of the host galaxy. This will allow investigation of host-galaxy properties: our particular interest is determination of the host-galaxy starlight contribution to the reverberation mapping observations, which is necessary for accurate determination of the relationship between the AGN continuum flux and the size of the broad Balmer-line emitting region of AGNs. Because this relationship is used to estimate black-hole masses of large samples of distant AGNs, correct determination of the slope of this relationship is critically important. 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. ACS/HRC/WFC 9781 Galaxy Evolution in Action : The Detailed Morphology of Post-Starburst Galaxy If galaxies evolve morphologically, then some should be in transition between late and early types. One proposed evolutionary mechanism is a galaxy-galaxy merger, but evolved merger products are difficult to find. Fortunately, spectroscopic surveys have now uncovered large numbers of E+A galaxies, a class of objects whose post-starburst spectra, current lack of HI gas, and pressure-supported kinematics suggest that they are the missing panel that connects the "Toomre sequence" of merging spirals with normal ellipticals and S0s. Our first HST observations of five of these galaxies are intriguing. We find a considerable range of tidally disturbed morphologies, an "E+A" fundamental plane, significant differences among the color gradients within 1 kpc {~0.8''}, and populations of bright, blue globular clusters. These initial results are difficult to interpret, however, because they are drawn from a small sample of galaxies whose very blue overall colors may have selected a particular evolutionary path of E+As. Here we propose for ACS imaging of the remaining 15 E+As from the Las Campanas Redshift Survey to probe the full range of E+A properties. The proposed observations will allow us to 1} determine what fraction of the interactions that lead to E+As destroy all disk-like structures {and therefore necessarily lead to elliptical formation}, 2} measure the inner color gradients and constrain the spatial distribution of stars produced as gas sinks to the center during a merger, and 3} determine whether these interactions produce globular clusters in the required numbers to account for the increased specific frequency of clusters in early-type 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/WFC 9892 H-alpha Snapshots of Nearby Galaxies observed in F300W: Quantifying Star Formation in a Dusty Universe Previous studies of nearby galaxies show large discrepancies between different star formation {SF} indicators on large {100 pc, or even global} scales: the strikingly complex interplay of young stars, dust and ionized gas are the primary cause of this variance. The few galaxies in the HST Archive with both WFPC2 H-alpha and mid-UV {F255W or F300W} imaging show this complex geometry extending down to 10 pc scales. We propose a SNAPshot survey in the ACS/WFC H-alpha filter of 48 galaxies of all Hubble types, that are nearby but beyond the Local Group, and that were previously imaged with WFPC2 in the mid-UV and in F814W. We aim to provide a benchmark for understanding the SF processes in both normal and star-bursting galaxies, at spatial resolutions unattainable from the ground for a large and varied galaxy sample. These data can be applied to a wide range of astrophysical problems and will, therefore, be made public immediately. Our science goals are to: {1} spatially resolve the dust clouds and filaments which strongly affect mid-UV and H-alpha derived SF rates, {2} test how the large-scale correlation between H-alpha and mid-UV flux breaks down on pc scales, and {3} model the propagation of star formation by comparing the SF over time scales of ~100 Myr {via mid-UV} and ~5 Myr {via H-alpha}. This will {4} significantly improve our insight into, and calibration of SF in UV-bright galaxies at high z, and into the cosmic SF history. ACS/WFC/WFPC2 9774 Young Massive Clusters in Spiral Galaxies and the Connection with Open Clusters We propose to carry out a census of star clusters in the disks of the nearby spiral galaxies NGC 45, NGC 1313, NGC 4395, NGC 5236 and NGC 7793. Using ACS, we will identify much fainter and older star clusters than possible in previous ground-based surveys, or even in HST imaging of more distant galaxies. For the first time, we will directly explore the connection between young "massive'' {or "super''} star clusters {YMCs} and lower-mass "open'' clusters in different star forming environments. We will test the universality of the luminosity- and mass functions of stellar clusters and establish whether the presence of YMCs is a result of a top-heavy cluster luminosity function, or follows from generally richer cluster systems. Our target galaxies span a range of morphological properties, surface brightness and star formation rate. Some of them are known from ground-based studies to host large numbers of YMCs while others have more modest cluster populations. However, previous ground-based data were restricted to luminous clusters younger than about 500 Myr. Here we will extend the search to clusters formed throughout the entire lifetime of each galaxy and reach clusters with properties typical of the Milky Way open clusters. This will allow us to close the gap between studies of extragalactic and Galactic disk clusters. 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. 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. STIS 9718 SMC Extinction Curve Towards a Quiescent Molecular Cloud The lack of 2175 A bump in the SMC extinction curve is interpreted as an absence of small carbon grains. ISO mid-IR observations support this interpretation by showing that PAH features are absent in the spectra of SMC and LMC massive star forming regions. However, the only ISO observation of an SMC quiescent molecular cloud shows all PAH features, indicating a PAH abundance relative to large dust grains similar to that of Milky Way clouds. We identified a reddened B2III star associated with this cloud. We propose to observe it with STIS to derive the xetinction curve of SMC dust away from HII regions. This observation will provide the first measure of the extinction properties of SMC dust away from star forming regions. It will allow us to disentangle the effects of metallicity and star formation on the SMC extinction curve and dust composition and to assess the relevance of the SMC bump-free extinction curve to low metallicity and/or starburst galaxies in general. STIS/CCD 10018 CCD Dark Monitor-Part 2 Monitor the darks for the STIS CCD. 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/MA1/MA2 9827 UV extinction by dust in unexplored LMC environments The ensemble of results from studies of the UV extinction in the Milky Way, Magellanic Clouds {MC}, M31 and M33, indicates a complex dependence of the dust properties with environment, where starburst activity and metallicity are relevant factors. Work in the LMC to date, based on IUE data, has several drawbacks: a} only supergiants could be used, b} they all have moderate extinction, c} the IUE S/N is limited, d} the large IUE slit may include light from other sources, such as scattered light from dust or faint companion stars, e} studies are confined to few {extreme} environments. We propose to obtain UV extinction curves more accurate than previous ones {from STIS spectra of main sequence stars with higher reddening}, sampling four environments in the LMC with different levels of star formation activity, including the general field, hitherto unexplored. The results will characterize the properties of dust in different conditions, at the LMC metallicity, which is useful to intepret integrated properties of distant galaxies, as well as GALEX upcoming UV surveys. A complementary study is under way with FUSE in the far-UV range. The combined results will provide insight on the properties of small grains. 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/ACS/WFC 9720 Age-dating Star Clusters in M101 M101 represents perhaps our best chance to study the stellar population of a luminous, late type spiral galaxy, due to both its proximity and its face-on orientation. For these reasons, 13 orbits of HST ACS observing time were allocated in Cycle 11 to obtain a 4x4 mosaic image of M101 in BVI . Unfortunately, a degeneracy between age and reddening exists when only these three bands are available. Hence, we propose to augment these observations by obtaining WFPC2 U band and ACS H alpha images. This will enable the accurate determination of ages for the young clusters, secure identifications of 75-100 old globular clusters, and allow a quantitative study of the HII region sizes and structures. Some of the specific questions we will address a How do the young clusters form and evolve? What fraction of the clusters dissolve and on what timescales? Do clusters evolve with a continuum of properties? Using WFPC2 and ACS in parallel, and making use of the fact that M101 is in the CVZ, allows us to greatly enhance the science return of previous HST observations for the cost of only 4 orbits. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) None SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 09 09 FGS REacq 06 06 FHST Update 17 17 LOSS of LOCK SIGNIFICANT EVENTS: Successfully completed third and final round of OBAD Data Collections, Sections N, O, P, I, and Q @ 148/03:15Z, adding four more scheduled OBAD/Rate Control combinations to the eleven collected over the past two days. (OR 17169 with attached script). Successfully executed the 4th FGS-2R TRTTT with macro kicking off at 148/18:02Z and 19:42Z, for the 1st and 2nd runs, respectively (OR 17170-2). OTA SE remained on console to monitor the successful GS Acquisition (1,3,1) @ 148/20:41Z. Due to TDRSS schedule, data were not available until SSR engineering data playback @ 148/21:50Z. Continuous MERGED data will be available 5/28/04 (am) for the analysis to begin. |
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