! From phase2p@stsci.edu Wed Mar 8 09:40:22 1995 ! From miley@stsci.edu Wed Mar 8 09:39:58 1995 ! ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! Id: 6107 ! ! For help call your Program Coordinator: Max Mutchler ! Phone: 410 338-1321 , E-mail: mutchler@stsci.edu Proposal_Information Title: Dynamics and Ages of Nuclear Stellar Disks in Virgo E/S0 Galaxies Proposal_Category: GO Scientific_Category: Galaxies & Clusters Cycle: 5 Investigators PI_name: Walter Jaffe PI_Institution: Leiden Observatory, The Netherlands CoI_Name: Holland Ford CoI_Institution: John Hopkins University, USA Contact: N CoI_Name: Robert O'Connell CoI_Institution: University of Virginia, USA Contact: N CoI_Name: Frank van den Bosch CoI_Institution: Leiden Observatory, The Netherlands Contact: Y CoI_Name: Laura Ferrarese CoI_Institution: Johns Hopkins University, USA Contact: N Abstract: In our previous HST WFPC1 photometric study of a complete sample of ellpitical galaxies in the Virgo cluster, we discovered that the nuclei of ellipticals fainter than M_B = - 19.5 contain small, thin, bright stellar disks with radii less than 100 pc and heights less than 10 pc. Here we propose new observations of two of these disky ellipticals (NGC 4342, and NGC 4570), with the object of estimating the galaxy central masses, and measuring the age of the disks. With the FOS G570H spectroscopy we will measure the kinematics and line strengths of the disks at 20 pc resolution. With the WFPC2 we will take images at three wavelengths (U, V, I) to investigate population differences between the disks and the host galaxies. The rotation curves of the dynamically cold disks will yield accurate, unambiguous estimates (or limits) of the central masses, allowing us to determine if average cluster ellipticals host massive black holes. The population analysis and kinematics will help determine whether the fainter galaxies are the basic ``bricks" from which more luminous galaxies are formed, or are themselves composite systems. Questions Observing_Description: MULTI COLOR PHOTOMETRY WITH THE WFPC2: We will take three broad band images of both NGC 4342 and NGC 4570, using the PC1 camera with the F336W, F555W and F814W filters. These correspond to the U, V, and I colors of the Johnson Cousins system. From our HST (WFPC1) observations with the F555W filter we know the surface brightness (in the V-band) of these galaxies to high accuracy, and found the nuclei to be very bright due to the contribution of the nuclear disks (mu_V = 13.4, and 13.82 magn. arcsec^-2 in the centers of NGC 4342, and NGC 4570 resp.) We are repeating the F555W exposures here because the older WFPC1 observations would have to be deconvolved to compare them to the new WFPC2 U and I band images, leading to an unacceptable loss of accuracy. FOS SPECTROSCOPY OF THE NUCLEAR DISKS: We wil take spectra of the central regions of NGC 4342. Similar spectroscopy will be performed for NGC 4570 in a cycle 4 carryover proposal from cycle 1. We will use the G570H grating on the FOS red arm, covering a wavelength region that includes the Mg-b triplet near 5182 angstrom. We will use the 0.3'' aperture to obtain 7 spectra of NGC 4342; 5 along the major axis (offset = -0.5'', -0.25', 0.0'', +0.25'', and +0.5'') and two offset +/- 0.25'' along the minor axis. EXPOSURE TIMES FOR THE WFPC2 IMAGES: Using the known magnitudes, and aiming at a signal-to-noise of 100 at the center (this gives S/N approx. 30 at 1'' along the major axis), the exposure times can be calculated using formula 6.1 in the WFPC2 Instrument Handbook. In the V and I bands the necessary exposure times are roughly 200 sec. The F336W exposures are approximately 100 times longer than for the other two filters because of a combined effect of lower efficiency of the instrument and the fact that ellipticals are approximately 3 magnitudes fainter in U than in V. This would require extreme integration times, so we will settle for a S/N of 50 in the center of the U-band images. At 1'' along the major axis the signal-to-noise ratio is then approx. 15. The central S/N of 100 is chosen since we plan to do accurate surface photometry. With all exposures being CR split, none of the exposures will encounter saturation. We do not know before hand whether the estimate of the U-V color of approx. 3 magn is correct. This value corresponds to K0 Giants, which normally make up the major light contribution in elliptical. If, however, the stellar disk contains young stars the U-V color can be orders of magnitude lower. In that case the total exposure will be saturated. Therefore, the long U integrations are split in a couple of subexposures of which at least two are relatively short, in case the nuclear disk is young. THE TARGET ACQUISITION WITH THE FOS: Since the nucleus of NGC 4342 is bright (SURF(V) = 13.4) and stronly peaked (almost point-source like) we can easily do a ACQ/PEAK on the nucleus of NGC 4342 itself. The aperture to be used for our observations is the 0.3. The standard acquisition procedure is to use four ACQ/PEAK stages, starting with a 1x3 dwell pattern of the 4.3 aperture, followed by dwells using the 1.0, 0.3 and 0.3 apertures, respectively. Since the first twelf minutes of the first FOS orbit will be used to acquire a guide star, only the first two stages will fit in the first orbit of the visit. Only the third stage will fit in the second orbit, and the fourth and final stage will take up most of the third orbit. This is then an extremely inefficient procedure that leaves much unused target visibility at the end of the first and second orbit. We have therefore devised an alternative scheme based on five stages that can be executed entirely in only two orbits and yields the same pointing accuracy (0.037'') as the default four-stage peak-up. It uses a 2x7 dwell of the 4.3 aperture, a 7x2 dwell of the 1.0 aperture, a 3x3 dwell of the 0.5 aperture, a 3x3 dwell of the 0.3 aperture, and finally, a 5x5 dwell of the 0.3 aperture. For each stage the parameters SCAN-STEP-X and SCAN-STEP-Y are chosen such that apertures at different dwell positions overlap slightly, and in addition cover entirely the aperture chosen in the previous stage. The first three stages fill the first orbit of the visit, the final two stages fill the second orbit of the visit. The exposure times used are clearly longer than required according to Table 2.1.6 in the FOS instrument handbook, but since this is an extended source instead of a point source, as assumed for the values in the table, we simply follow the save approach. Furthermore, the exposure times are negligible compared to the individual overhead times. EXPOSURE TIMES FOR THE FOS SPECTRA: Since our goal is getting an understanding of the dynamics of the nuclear, stellar disks embedded in ellipticals, we are not only interested in deriving the rotation velocity (ie. the first order moment of the line profiles), but also interested in deriving velocity dispersion and if possible even higher order moments, that might allow us to attempt bulge/disk decomposition of the line profiles. We therefore aim for a S/N per diode of 60 at the center (SURF(V) = 13.4), S/N = 60 at +/- 0.25'' along the major axis (SURF(V) = 14.15), S/N = 35 at +/- 0.5'' along the major axis (SURF(V) = 14.97), and SN = 30 at +/-0.25'' along the minor axis (SURF(V) = 15.1). The S/N decreases outside for two reasons: Since the surface brightness (accurately known from WFPC cycle 1 data) stronly decreases outside, the outer points would require too long integrations, and secondly, the most interesting points, when studying the rotation curve to look for evidence of say a massive black hole, are the inner points. We therefore feel that this strategy is appropriate for our scientifc aims. From the S/N ratios mentioned above the integration times are calculated using formula 1 in Table 1.2.1 in the FOS instrument handbook. The wavelength taken in these calculations is that of the redshifted Mg-b triplet. THE WAVELENGHT CALIBRATION: After each FOS orbit we will take a wavelength calibration frame. The main cause for shifts in wavelenght along the diodes is changing the wheel with gratings. This will not happen during our FOS visit. However, there is another source of changes, namely the Earth magnetic field which acts on the electron beam in both the spatial and the dispersion direction, causing errors up to approximately 15 to 20 km per sec. Since we want high accuracy in the rotation velocities to be derived, we should therefore take these calibration frames in order to keep track of possible shifts in between two exposures. They can be taken during occulatation so that no valuable exposure time is lost. Real_Time_Justification: Calibration_Justification: We will obtain wavelnght calibration spectra at the end of each orbit of the FOS visit. As explained above this is essential for an accurate determination of velocities. Since expected velocities for different models often only mildly vary, high accuracy is of vital importance. These calibration exposures do not waste any visibility time, since the wavelength calibration exposures can be done during occultation. Additional_Comments: ABSOLUTELY NO CHANGES OR MODIFICATIONS, NOT EVEN MINOR ONES, SHOULD BE MADE TO THIS PROGRAM WITHOUT CONSULTING THE PI OR THE CONTACT FIRST. Fixed_Targets Target_Number: 11 Target_Name: NGC4570 Alternate_Names: Description: GALAXY, ELLIPTICAL, NUCLEUS Position: RA = 12H 36M 53.340S +/- 0.003S, DEC = +7D 14' 46.18" +/- 0.05" Equinox: J2000.0 RV_or_Z: V = +1730 Flux: V = 10.75 +/- 0.06, B-V = 0.95 +/- 0.06, SURF(V) = 13.82 +/- 0.02 Comments: The WFPC2 images of NGC 4570 Fluxes as follows: V is total V magn SURF(V) = central surface brightness Target_Number: 21 Target_Name: NGC4342 Alternate_Names: IC3256 Description: GALAXY, ELLIPTICAL, NUCLEUS Position: RA = 12H 23M 39.003S +/- 0.003S, DEC = +7D 3' 13.52" +/- 0.05" Equinox: J2000.0 RV_or_Z: V = +714 Flux: V = 12.56 +/- 0.1, B-V = 0.98 +/- 0.07, SURF(V) = 13.40 +/- 0.02 Comments: The WFPC2 images of NGC 4342 Fluxes as follows: V is total V magn SURF(V) = central surface brightness Target_Number: 100 Target_Name: NGC4342-NUC Alternate_Names: IC3256 Description: GALAXY, ELLIPTICAL, NUCLEUS Position: RA = 12H 23M 39.003S +/- 0.003S, DEC = +7D 3' 13.52" +/- 0.05" Equinox: J2000.0 RV_or_Z: V = +714 Flux: V = 12.56 +/- 0.1, B-V = 0.98 +/- 0.07, SURF(V) = 13.40 +/- 0.02 Comments: the center of NGC 4342 SURF(V) = surface brightness at r = 0.0 Target_Number: 101 Target_Name: NGC4342-MAJ1A Alternate_Names: IC3256 Description: GALAXY, ELLIPTICAL, NUCLEUS Position: RA-OFF = +0.0036S +/- 0.005S, DEC-OFF = -0.2440" +/- 0.05", FROM 100 Equinox: J2000.0 RV_or_Z: V = +714 Flux: V = 12.56 +/- 0.1, B-V = 0.98 +/- 0.07, SURF(V) = 14.10 +/- 0.02 Comments: +0.25'' offset along major axis SURF(V) = surface brightness at r = 0.25'' Target_Number: 102 Target_Name: NGC4342-MAJ1B Alternate_Names: IC3256 Description: GALAXY, ELLIPTICAL, NUCLEUS Position: RA-OFF = -0.0036S +/- 0.005S, DEC-OFF = +0.2440" +/- 0.05", FROM 100 Equinox: J2000.0 RV_or_Z: V = +714 Flux: V = 12.56 +/- 0.1, B-V = 0.98 +/- 0.07, SURF(V) = 14.10 +/- 0.02 Comments: -0.25'' offset along major axis SURF(V) = surface brightness at r = 0.25'' Target_Number: 111 Target_Name: NGC4342-MAJ2A Alternate_Names: IC3256 Description: GALAXY, ELLIPTICAL, NUCLEUS Position: RA-OFF = +0.0073S +/- 0.005S, DEC-OFF = -0.4880" +/- 0.05", FROM 100 Equinox: J2000.0 RV_or_Z: V = +714 Flux: V = 12.56 +/- 0.1, B-V = 0.98 +/- 0.07, SURF(V) = 14.97 +/- 0.04 Comments: +0.50'' offset along major axis SURF(V) = surface brightness at r = 0.5'' Target_Number: 112 Target_Name: NGC4342-MAJ2B Alternate_Names: IC3256 Description: GALAXY, ELLIPTICAL, NUCLEUS Position: RA-OFF = -0.0073S +/- 0.005S, DEC-OFF = +0.4880" +/- 0.05", FROM 100 Equinox: J2000.0 RV_or_Z: V = +714 Flux: V = 12.56 +/- 0.1, B-V = 0.98 +/- 0.07, SURF(V) = 14.97 +/- 0.04 Comments: -0.50'' offset along major axis SURF(V) = surface brightness at r = 0.5'' Target_Number: 121 Target_Name: NGC4342-MIN1A Alternate_Names: IC3256 Description: GALAXY, ELLIPTICAL, NUCLEUS Position: RA-OFF = +0.0163S +/- 0.005S, DEC-OFF = -0.0545" +/- 0.05", FROM 100 Equinox: J2000.0 RV_or_Z: V = +714 Flux: V = 12.56 +/- 0.1, B-V = 0.98 +/- 0.07, SURF(V) = 14.65 +/- 0.04 Comments: +0.25'' offset along minor axis SURF(V) = surface brightness at r = 0.25'' (minor) Target_Number: 122 Target_Name: NGC4342-MIN1B Alternate_Names: IC3256 Description: GALAXY, ELLIPTICAL, NUCLEUS Position: RA-OFF = -0.0163S +/- 0.005S, DEC-OFF = +0.0545" +/- 0.05", FROM 100 Equinox: J2000.0 RV_or_Z: V = +714 Flux: V = 12.56 +/- 0.1, B-V = 0.98 +/- 0.07, SURF(V) = 14.65 +/- 0.04 Comments: -0.25'' offset along minor axis SURF(V) = surface brightness at r = 0.25'' (minor) Visits Visit_Number: 1 Visit_Requirements: On_Hold_Comments: Visit_Comments: In this visit the WFPC2 images of NGC 4570 will be taken. Total of 3 orbits. Exposure_Number: 100 Target_Name: NGC4570 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F336W Optional_Parameters: ATD-GAIN = 7 CR-SPLIT = 0.272727 CR-TOLERANCE = 0.05 Number_of_Iterations: 1 Time_Per_Exposure: 2200S Special_Requirements: END ORBIT Comments: The U-Band image of NGC 4570 This exposure will fill entire orbit 1 Exposure_Number: 101 Target_Name: NGC4570 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F336W Optional_Parameters: ATD-GAIN = 7 CR-SPLIT = 0.48 CR-TOLERANCE = 0.05 Number_of_Iterations: 1 Time_Per_Exposure: 2500S Special_Requirements: POS TARG 0.5, 0.5 END ORBIT Comments: The U-Band image of NGC 4570 This exposure will fill entire orbit 2 Offset 11 pixels in x and y direction Exposure_Number: 102 Target_Name: NGC4570 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F336W Optional_Parameters: ATD-GAIN = 7 CR-SPLIT = NO Number_of_Iterations: 1 Time_Per_Exposure: 400S Special_Requirements: POS TARG -0.5, -0.5 Comments: The U-Band image of NGC 4570 This exposure will partly fill orbit 3 Offset 11 pixels in x and y direction Exposure_Number: 110 Target_Name: NGC4570 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F555W Optional_Parameters: ATD-GAIN = 7 CR-SPLIT = NO Number_of_Iterations: 1 Time_Per_Exposure: 200S Special_Requirements: Comments: The V-Band image of NGC 4570 This exposure will fill partly orbit 3 Exposure_Number: 111 Target_Name: NGC4570 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F555W Optional_Parameters: ATD-GAIN = 7 CR-SPLIT = NO Number_of_Iterations: 1 Time_Per_Exposure: 200S Special_Requirements: POS TARG 0.5, 0.5 Comments: The V-Band image of NGC 4570 This exposure will fill partly orbit 3 Exposure_Number: 120 Target_Name: NGC4570 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F814W Optional_Parameters: ATD-GAIN = 7 CR-SPLIT = NO Number_of_Iterations: 1 Time_Per_Exposure: 260S Special_Requirements: Comments: The I-Band image of NGC 4570 This exposure will fill partly orbit 3 Exposure_Number: 121 Target_Name: NGC4570 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F814W Optional_Parameters: ATD-GAIN = 7 CR-SPLIT = NO Number_of_Iterations: 1 Time_Per_Exposure: 200S Special_Requirements: POS TARG 0.5, 0.5 END ORBIT Comments: The I-Band image of NGC 4570 This exposure will fill orbit 3. Visits Visit_Number: 2 Visit_Requirements: On_Hold_Comments: Visit_Comments: In this visit the WFPC2 images of NGC 4342 will be taken. Total of 2 orbits. Exposure_Number: 200 Target_Name: NGC4342 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F336W Optional_Parameters: ATD-GAIN = 7 CR-SPLIT = 0.272727 CR-TOLERANCE = 0.05 Number_of_Iterations: 1 Time_Per_Exposure: 2200S Special_Requirements: END ORBIT Comments: The U-Band image of NGC 4343 This exposure fills orbit 4 Exposure_Number: 201 Target_Name: NGC4342 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F336W Optional_Parameters: ATD-GAIN = 7 CR-SPLIT = 0.3333 CR-TOLERANCE = 0.05 Number_of_Iterations: 1 Time_Per_Exposure: 1500S Special_Requirements: POS TARG 0.5, 0.5 Comments: The U-band exposure of NGC 4342. Exposure partly fill orbit 5. Offset 11 pixels in x and y direction Exposure_Number: 210 Target_Name: NGC4342 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F555W Optional_Parameters: ATD-GAIN = 7 CR-SPLIT = 0.5 CR-TOLERANCE = 0.05 Number_of_Iterations: 1 Time_Per_Exposure: 200S Special_Requirements: Comments: The V-band image of NGC 4342 Exposure partly fills orbit 5. Exposure_Number: 220 Target_Name: NGC4342 Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F814W Optional_Parameters: ATD-GAIN = 7 CR-SPLIT = 0.5 CR-TOLERANCE = 0.05 Number_of_Iterations: 1 Time_Per_Exposure: 200S Special_Requirements: Comments: The I-band image of NGC 4342 End of orbit 5. Final orbit of visit 1. Visits Visit_Number: 3 Visit_Requirements: On_Hold_Comments: Visit_Comments: In this visit the FOS spectra of NGC 4342 will be taken. Total of 5 orbits. Exposure_Number: 301 Target_Name: NGC4342 Config: FOS/RD Opmode: ACQ/PEAK Aperture: 4.3 Sp_Element: G570H Optional_Parameters: SCAN-STEP-X = 3.36, SCAN-STEP-Y = 0.8, SEARCH-SIZE-X = 2, SEARCH-SIZE-Y = 7, TYPE = UP Number_of_Iterations: 1 Time_Per_Exposure: 4S Special_Requirements: ONBOARD ACQ FOR 302 NO SPLIT Comments: Exp time yields >1000 counts at center This exposure partly fills orbit 6. Exposure_Number: 302 Target_Name: NGC4342 Config: FOS/RD Opmode: ACQ/PEAK Aperture: 1.0 Sp_Element: G570H Optional_Parameters: SCAN-STEP-X = 0.5229, SCAN-STEP-Y = 0.6495, SEARCH-SIZE-X = 7, SEARCH-SIZE-Y = 2, TYPE = UP Number_of_Iterations: 1 Time_Per_Exposure: 4S Special_Requirements: ONBOARD ACQ FOR 303 NO SPLIT Comments: Exp time yields >1000 counts at center This exposure partly fills up orbit 6. Exposure_Number: 303 Target_Name: NGC4342 Config: FOS/RD Opmode: ACQ/PEAK Aperture: 0.5 Sp_Element: G570H Optional_Parameters: SCAN-STEP-X = 0.2867, SCAN-STEP-Y = 0.2867, SEARCH-SIZE-X = 3, SEARCH-SIZE-Y = 3, TYPE = UP Number_of_Iterations: 1 Time_Per_Exposure: 4S Special_Requirements: ONBOARD ACQ FOR 304 NO SPLIT END ORBIT Comments: Exp time yields >1000 counts at center This exposure fills orbit 6. Exposure_Number: 304 Target_Name: NGC4342 Config: FOS/RD Opmode: ACQ/PEAK Aperture: 0.3 Sp_Element: G570H Optional_Parameters: SCAN-STEP-X = 0.1433, SCAN-STEP-Y = 0.1433 SEARCH-SIZE-X = 3, SEARCH-SIZE-Y = 3, TYPE = UP Number_of_Iterations: 1 Time_Per_Exposure: 4S Special_Requirements: ONBOARD ACQ FOR 305 NO SPLIT Comments: Exp time yields >1000 counts at center This exposure partly fills up orbit 7. Exposure_Number: 305 Target_Name: NGC4342 Config: FOS/RD Opmode: ACQ/PEAK Aperture: 0.3 Sp_Element: G570H Optional_Parameters: SCAN-STEP-X = 0.052, SCAN-STEP-Y = 0.052 SEARCH-SIZE-X = 5, SEARCH-SIZE-Y = 5, TYPE = UP Number_of_Iterations: 1 Time_Per_Exposure: 40S Special_Requirements: ONBOARD ACQ FOR 309-379 NO SPLIT Comments: Exp time yields approx. 10000 counts at center This exposure fills up orbit 7. Since this is the critical peak-up stage the exposure time is longer as for the others. Exposure_Number: 309 Target_Name: WAVE Config: FOS/RD Opmode: ACCUM Aperture: 0.3 Sp_Element: G570H Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: DEF Special_Requirements: NO SPLIT END ORBIT Comments: This is a wave-cal exposure which can be done during occulatation. Exposure_Number: 310 Target_Name: NGC4342-NUC Config: FOS/RD Opmode: ACCUM Aperture: 0.3 Sp_Element: G570H Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 1000S Special_Requirements: NO SPLIT Comments: Aperture at nucleus of NGC 4342 This exposure partly fills orbit 8. Exposure_Number: 320 Target_Name: NGC4342-MAJ1A Config: FOS/RD Opmode: ACCUM Aperture: 0.3 Sp_Element: G570H Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 1200S Special_Requirements: NO SPLIT Comments: Aperture at offset +0.25'' along major axis. This exposure fills orbit 8. Exposure_Number: 329 Target_Name: WAVE Config: FOS/RD Opmode: ACCUM Aperture: 0.3 Sp_Element: G570H Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: DEF Special_Requirements: NO SPLIT END ORBIT Comments: This is a wave-cal exposure which can be done during occulatation. Exposure_Number: 330 Target_Name: NGC4342-MAJ1B Config: FOS/RD Opmode: ACCUM Aperture: 0.3 Sp_Element: G570H Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 1200S Special_Requirements: NO SPLIT Comments: Aperture at offset -0.25'' along major axis. This exposure partly fills orbit 9. Exposure_Number: 340 Target_Name: NGC4342-MAJ2A Config: FOS/RD Opmode: ACCUM Aperture: 0.3 Sp_Element: G570H Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 900S Special_Requirements: NO SPLIT Comments: Aperture at offset +0.5'' along major axis. This exposure fills orbit 9. Exposure_Number: 349 Target_Name: WAVE Config: FOS/RD Opmode: ACCUM Aperture: 0.3 Sp_Element: G570H Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: DEF Special_Requirements: NO SPLIT END ORBIT Comments: This is a wave-cal exposure which can be done during occulatation. Exposure_Number: 350 Target_Name: NGC4342-MAJ2B Config: FOS/RD Opmode: ACCUM Aperture: 0.3 Sp_Element: G570H Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 900S Special_Requirements: NO SPLIT Comments: Aperture at offset -0.5'' along major axis. Exposure partly fills orbit 10. Exposure_Number: 360 Target_Name: NGC4342-MIN1A Config: FOS/RD Opmode: ACCUM Aperture: 0.3 Sp_Element: G570H Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 500S Special_Requirements: NO SPLIT Comments: Aperture at offset +0.25'' along minor axis. Exposure partly fills orbit 10. Exposure_Number: 370 Target_Name: NGC4342-MIN1B Config: FOS/RD Opmode: ACCUM Aperture: 0.3 Sp_Element: G570H Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 500S Special_Requirements: NO SPLIT Comments: Aperture at offset -0.25'' along minor axis. Exposure fills orbit 10. Exposure_Number: 379 Target_Name: WAVE Config: FOS/RD Opmode: ACCUM Aperture: 0.3 Sp_Element: G570H Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: DEF Special_Requirements: NO SPLIT END ORBIT Comments: This is a wave-cal exposure which can be done during occulatation. Data_Distribution Medium: 8MM Blocking_Factor: 10 Ship_To: PI_Address ! P.O. Box 9513, 2300 RA Leiden, ! The Netherlands ! Ship_Via: UPS __Diagnostic-Sum-Section__ Software-Version (Controller= 2.1) Preprocessor (Errors= 0 Fatal-Errors= 0 ) Validation (Errors= 0 Fatal-Errors= 0 ) Transformation (Errors= 0 Fatal-Errors= 0 ) CASM (Errors= 0 Fatal-Errors= 0 ) __User-Comments__ Dear PC We are submitting this proposal from sol at STScI because, despite the best efforts of 4 astronomers and a system programmer, we were unable to get the RPS2 servers to function here in Leiden. The processing crashed on obscure error like "exit impossible; resize children failed". Advice from MAx proved to no avail. We hope this works better in Cycle 6. Cheers from your ever hopeful PI Walter Jaffe