DAILY REPORT # 3312

PERIOD COVERED: DOY 63

OBSERVATIONS SCHEDULED

NICMOS 8791

NICMOS Post-SAA calibration - CR Persistence Part 2

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.

NICMOS 9360

Paschen-alpha Imaging of a SIRTF-Selected Nearby Galaxy Sample

We propose to carry out a NICMOS snapshot survey in the Paschen-alpha {PAlpha} emission line and H-band of the sample of galaxies being observed at 3.5 -- 160 microns as part of SIRTF Nearby Galaxies Survey {SINGS} and a related guaranteed time survey of starburst galaxies. The PAlpha images, accessible only from HST, will be combined with groundbased HAlpha imaging to measure the extinction in the star-forming centers of these galaxies, and obtain robust, extinction- corrected maps of the massive star formation rate {SFR}. The PAlpha data by themselves will provide reliable `extinction- free' SFRs, and a cross-calibration of the {dust--affected} HAlpha-- and UV--based SFRs. The PAlpha--based SFR measurements will extend the SFR-vs.-gas density law {Schmidt--law} to surface densities at least 30 times higher than what is accessible using HAlpha--based SFR measurements alone, bridging the gap between normal galaxies and IR--luminous starbursts. Furthermore, the combination of the HST PAlpha images with the SIRTF images and spectra, as well as ancillary ground--based UBVRIJHK images and GALEX UV images being obtained as part of the SINGS project, will provide a definitive study of the radiative transfer of starlight and dust heating in star--forming galaxies. The processed NICMOS images will be incorporated into the public SINGS Legacy Data Archive, to enable scores of follow-up studies by the astronomical community at large.

ACS/HRC 9379

Near Ultraviolet Imaging of Seyfert Galaxies: Understanding the Starburst-AGN Connection

We propose a near-UV snapshot survey of 101 Seyfert galaxies using ACS/HRC and the filter F330W, a configuration which is optimal to detect faint star forming regions around their nuclei. These images will complement optical and near-IR images available in the HST archive, thus providing a panchromatic atlas of the inner regions of active galaxies, which we will use to study the starburst-AGN connection. The main goals of this proposal are: {1} Determine the frequency of circumnuclear starbursts in Seyferts, down to levels which cannot be observed from the ground; {2} characterize the observational {fluxes, colors, structure, sizes} and intrinsic {luminosities, masses, ages, global star-formation rate} properties of these clusters; {3} derive the luminosity functions of young star clusters around the nucleus of Seyferts and compare these results with those from normal and starburst galaxies to determine their survival rate close to the AGN; {4} address questions about the relation between AGNs and starbursts, like the possible connection between the masses and luminosities of black holes and starbursts, and the implications for the evolution of the black holes and their host galaxy bulges. By adding UV images to the existing optical and near-IR ones, this project will create an extremely valuable database for astronomers with a broad range of scientific interests, from the properties of the AGN to the properties of their host galaxies.

ACS 9409

The Evolution of Globular Cluster Systems in Merger Remnants

Mergers seem to have played a major role in determining the shapes and dynamics of elliptical galaxies. A few galactic mergers still occur and offer valuable clues to past evolutionary processes. Globular clusters formed during mergers are crucial probes for age-dating such events, and help shed light on the process of cluster formation and evolution. With young globulars in ongoing mergers now well studied, we propose to make deep ACS observations of intermediate-age globular clusters in two bona fide ellipticals: NGC 1316 and 3610. These ellipticals have line-strength indices, UBV colors, and fine structure indicative of their being 2 -- 4 Gyr old merger remnants. Past HST+WFPC2 observations have shown that they also possess significant numbers of intermediate-age globulars as part of their bimodal cluster populations. We plan to use the new HST+ACS observations to {1} measure high-accuracy BVI colors for clusters up to ~ 2 -- 3 mag fainter than ever before, {2} use these colors to separate first- and second-generation clusters, and {3} determine the luminosity functions of the two kinds of clusters to 3 -- 4 mag past the peak for old globulars. Deep dithered BVI images form a crucial part of our observing strategy. This program should permit---for the first time---to directly detect the predicted evolution of the cluster luminosity function from a power law for young clusters to the Gaussian distribution typical of old globulars.

ACS 9463

Are OH/IR stars the youngest post-AGB stars? An ACS SNAPshot imaging survey

Essentially all well-characterized preplanetary nebulae {PPNs}-- objects in transition between the AGB and planetary nebula evolutionary phases - are bipolar, whereas the mass-loss envelopes of AGB stars are strikingly spherical. In order to understand the processes leading to bipolar mass-ejection, we need to know at what stage of stellar evolution does bipolarity in the mass-loss first manifest itself? We have recently hypothesized that most OH/IR stars {evolved mass- losing stars with OH maser emission} are very young PPNe. We propose an ACS/SNAPshot imaging survey of a large, morphologically unbiased sample of these objects, selected using their IRAS 12-to-25micron colors. Our ground-based imaging study of OH/IR stars has revealed a few compact bipolar objects, supporting our hypothesis. However since most objects remain unresolved, HST observations are needed to determine how and when the bipolar geometry asserts itself. Our complementary program of interferometric mapping of the OH maser emission in our sources is yielding kinematic information with spatial resolution comparable to that in the HST images. The HST/radio data will provide crucial input for theories of post-AGB stellar evolution. In addition, these data will also indicate whether the multiple concentric rings, ``searchlight beams'', and truncated equatorial disks recently discovered with HST in a few PPNs, are common or rare phenomena.

ACS 9468

ACS Grism Parallel Survey of Emission- line Galaxies at Redshift z pl 7

We propose an ACS grism parallel survey to search for emission-line galaxies toward 50 random lines of sight over the redshift interval 0 < z pl 7. We request ACS parallel observations of duration more than one orbit at high galactic latitude to identify ~ 300 HAlpha emission-line galaxies at 0.2 pl z pl 0.5, ~ 720 O IILambda3727 emission-line galaxies at 0.3 pl z pl 1.68, and pg 1000 Ly-alpha emission-line galaxies at 3 pl z pl 7 with total emission line flux f pg 2* 10^-17 ergs s^-1 cm^-2 over 578 arcmin^2. We will obtain direct images with the F814W and F606W filters and dispersed images with the WFC/G800L grism at each position. The direct images will serve to provide a zeroth order model both for wavelength calibration of the extracted 1D spectra and for determining extraction apertures of the corresponding dispersed images. The primary scientific objectives are as follows: {1} We will establish a uniform sample of HAlpha and O II emission-line galaxies at z<1.7 in order to obtain accurate measurements of co-moving star formation rate density versus redshift over this redshift range. {2} We will study the spatial and statistical distribution of star formation rate intensity in individual galaxies using the spatially resolved emission-line morphology in the grism images. And {3} we will study high-redshift universe using Ly-alpha emitting galaxies identified at z pl 7 in the survey. The data will be available to the community immediately as they are obtained.

STIS 9469

NGC 4303: A Seyfert 2 nucleus powered by stars?

NGC 4303 is to date the best example of the claimed starburst- AGN connection. HST images have unveiled the existence of an unresolved {size <= 4 pc} UV-optical-NIR bright core connected with a star-forming spiral {radius ~ 250 pc}. The STIS UV spectrum of the core shows prominently the characteristic broad absorption lines produced by the winds of massive young stars, and it is best fitted with the synthesised spectrum of a massive, young {<= 5 Myr} stellar cluster. Ground-based optical spectra of the nucleus containing the bright core, place it at the borderline of low-excitation Seyfert 2 and LINER nuclei. STIS 0.1^'' slit spectroscopy of the unresolved core is requested to obtain an unambiguous AGN classification of it, and to measure its enclosed mass, i.e. determine the presence and mass of the black-hole. In addition, the spectra will be combined with evolutionary spectral synthesis and photoionization models to quantify the relative AGN and stellar energy contributions. If the Seyfert classification is confirmed, NGC 4303 will be the first ever detected galaxy with a Seyfert nucleus where the ionizing and bolometric energy output of its core {size <= 4 pc} could be dominated by a massive stellar cluster of young stars, as implied by the STIS UV spectrum. NGC 4303 will also be one of the few Seyferts for which the mass enclosed within the inner few pc would have been determined independently from stellar and gas kinematics.

ACS 9475

ACS coronagraphic survey for debris disks around nearby stars

We propose a comprehensive imaging survey of nearby stars that will realize the full potential of the ACS coronagraph to map debris disks, the extrasolar analogs of our Kuiper Belt. Most debris disks are detected only by excess thermal emission at far-infrared wavelengths. Because they have a factor of 100 less dust cross section than the young debris disks around HR 4796A and beta Pic, they are undectable by present techniques. In simulations of disk detectability, Kalas and Jewitt {1996} determined that detecting the scattered light from the disk requires at least two orders of magnitude of supression of the central PSF than is attainable from the ground. The ACS coronagraph finally provides this increase in sensitivity, surpassing the WFPC2 sensitivity to faint nebulosity near bright stars by at least three orders of magnitude. Mapping the debris around stars is particularly important for the indirect detection of planet-mass objects. Dynamical models have shown that unseen perturbers dynamically modify the radial, azimuthal and vertical structure of debris disks. These data will provide the critical high-resolution mapping of debris disks.

ACS/WFPC2 9481

Pure Parallel Near-UV Observations with WFPC2 within High-Latitude ACS Survey Fields

In anticipation of the allocation of ACS high-latitude imaging survey{s}, we request a modification of the default pure parallel program for those WFPC2 parallels that fall within the ACS survey field. Rather than duplicate the red bands which will be done much better with ACS, we propose to observe in the near-ultraviolet F300W filter. These data will enable study of the rest-frame ultraviolet morphology of galaxies at 0<z<1. We will determine the morphological k-correction, and the location of star formation within galaxies, using a sample that is likely to be nearly complete with multi-wavelength photometry and spectroscopic redshifts. The results can be used to interpret observations of higher redshift galaxies by ACS.

NICMOS 9484

The NICMOS Parallel Observing Program

We propose to manage the default set of pure parallels with NICMOS. Our experience with both our GO NICMOS parallel program and the public parallel NICMOS programs in cycle 7 prepared us to make optimal use of the parallel opportunities. The NICMOS G141 grism remains the most powerful survey tool for HAlpha emission-line galaxies at cosmologically interesting redshifts. It is particularly well suited to addressing two key uncertainties regarding the global history of star formation: the peak rate of star formation in the relatively unexplored but critical 1<= z <= 2 epoch, and the amount of star formation missing from UV continuum-based estimates due to high extinction. Our proposed deep G141 exposures will increase the sample of known HAlpha emission- line objects at z ~ 1.3 by roughly an order of magnitude. We will also obtain a mix of F110W and F160W images along random sight-lines to examine the space density and morphologies of the reddest galaxies. The nature of the extremely red galaxies remains unclear and our program of imaging and grism spectroscopy provides unique information regarding both the incidence of obscured star bursts and the build up of stellar mass at intermediate redshifts. In addition to carrying out the parallel program we will populate a public database with calibrated spectra and images, and provide limited ground- based optical and near-IR data for the deepest parallel fields.

STIS 9506

A SNAPSHOT SURVEY OF HIGH COLUMN DENSITY, LOW-Z LyAlpha ABSORBERS

in the UV to discover new high-column density {N_H >= 10^15 cm^-2} LyAlpha absorbers in the local Universe {z <= 0.45}. Many more of these high column density systems are needed because: {1} They contribute most of the baryons to the local IGM; {2} They include systems for which valuable metallicity and D/H measurements can be made with the Cosmic Origins Spectrograph {COS}; {3} They include many of the ``warm-hot'' absorbers, thought to be a large baryon reservoir in the local Universe; and {4} They are most likely to be ``associated'' with galaxy halos. Because of their low-z, many of these absorbers can be located relative to galaxies of known redshifts, allowing an immediate scientific return from these snapshots. Perhaps the most important, lasting results of this survey require higher resolution reobservations with COS by our GTO team. Using these snapshots to select the best targets, we will obtain COS R~22, 000 spectra to determine the D/H and metallicity of absorbers in galaxy halos, groups, and voids. We will use pairs and ``constellations'' of AGN to determine absorber sizes, shapes, and covering factors. Candidate ``warm-hot'' absorbers will be reobserved with COS to determine their numbers accurately and to assess their metallicity, sizes, and relationships to galaxies and galaxy groups.

WFPC2 9594

WFPC2 CYCLE 11 SUPPLEMENTAL DARKS pt2/3

This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels

CAL/WF2 9597

Intflat Sweep, Visflat Sweep, and Filter Anomaly Check

No abstract available.

WFPC2 9599

WFPC2 Cycle 11 UV Earth Flats

Monitor flat field stability. This proposal obtains sequences of earth streak flats to improve the quality of pipeline flat fields for the WFPC2 UV filter set. These Earth flats will complement the UV earth flat data obtained during cycles 8-10.

STIS 9605

CCD Dark Monitor-Part 1

Monitor the darks for the STIS CCD

STIS 9607

CCD Bias Monitor - Part 1

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 9615

Cycle 11 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 9633

STIS parallel archive proposal - Nearby Galaxies - Imaging and Spectroscopy

Using parallel opportunities with STIS which were not allocated by the TAC, we propose to obtain deep STIS imagery with both the Clear {50CCD} and Long-Pass {F28X50LP} filters in order to make color-magnitude diagrams and luminosity functions for nearby galaxies. For local group galaxies, we also include G750L slitless spectroscopy to search for e.g., Carbon stars, late M giants and S-type stars. This survey will be useful to study the star formation histories, chemical evolution, and distances to these galaxies. These data will be placed immediately into the Hubble Data Archive.

ACS 9657

ACS Internal Flat Field Stability

The flat field stability and characterization obtained during the ground calibration and SMOV phases will be tested and verified through a sub-sample of the filter set. Only internal exposures with the calibration lamps will be required.

ACS 9658

ACS Earth Flats

This program will obtain sequences of flat field images by observing the bright Earth. Several UV filters from the interim calibration program {9564} require additional exposures to obtain the required illumination. A few UV filters from this program will be repeated to monitor for changes in the flat fields and to verify the interim results. Since no streaks are observed in the UV, the wavelength coverage is extended to longer wavelengths in order to explore the severity of streaks in the flats from clouds in the FOV. We have added exposures for the HRC in the visible filters to verify the results derived from the L-flat campaign and to explore the severity of streaks. We have also added exposures on WFC using the minimum exposure time and using filters which will not saturate the brightest WFC pixel by more than 10 times the full well.

ACS 9673

CCD Daily Monitor

for any source of noise in ACS CCD detectors. This programme will be executed once a day for the entire lifetime of ACS

WFPC2 9676

POMS Test Proposal: WFII parallel archive proposal

This is the generic target version of the WFPC2 Archival Pure Parallel program. The program will be used to take parallel images of random areas of the sky, following the recommendations of the 2002 Parallels Working Group.

NICMOS 9702

NICMOS Parallel Thermal Background

NICMOS Camera 2 pure parallel exposures in the F222M and F237M filters to establish the stability of the HST+NCS+Instrument thermal emission. This data will be compared against the already available Camera 3 measurements in F222M which show an increased thermal background.

STIS 9706

STIS Pure Parallel Imaging Program: Cycle 10

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) None

COMPLETED OPS REQs: None

OPS NOTES EXECUTED:1081-0 Adjust Software Main Bus Current, Red Limit @064/1643z

                           SCHEDULED     SUCCESSFUL    FAILURE TIMES
FGS GSacq               13                       13            
FGS REacq               5                          5
FHST Update             25                    25
LOSS of LOCK

SIGNIFICANT EVENTS:

On-Line Data Archive test 3/4/2003. The Online Data Archive test was completed successfully. The test was executed in the OPS account to ensure required data was available. All objectives were met and all requests performed as expected. No TSARs or CRs were written.

CCS 4.0.2 Source/Destination Codes test performed 3/4/2003. The test was successful. All destination codes were verified along with the source ID in both GSTDN and JSC single stage modes.

Engineering Data Products Test for CCS 4.0.1. Historical requests were submitted on G- string (CCS 4.0.2). Plots and reports were generated for a 24-hour time span and compared against plots and reports generated on A-string (CCS 4.0.1) for the same time period. The comparison revealed no significant differences for either the plots or the reports.

News from Commercial Space Watch