8239( 9) - 05/08/00 11:37 - [ 1] PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID: 8239 Version: 9 Check-in Date: 08-May-2000 11:36:09 1.Proposal Title: Imaging the NLR in a complete sample of z<0.5 radio-quiet PG quasars ------------------------------------------------------------------------------------ 2. Proposal For 3. Cycle GO 8 ------------------------------------------------------------------------------------ 4. Investigators Contact? PI: Heino Falcke Max-Planck-Institut Fur Radioastronomie CoI: Prof. Andrew Wilson Astronomy Dept., University of Maryland N CoI: Prof. Beverley J. Wills University of Texas, Austin N ------------------------------------------------------------------------------------ 5. Abstract Quasar activity is an important and little understood phase in the evolution of galaxies, where a central engine leaves its visible imprints in the galaxy through strong ionization and heating of the ISM. But, what is the structure of these hot emission line regions in quasars? Do quasars have ionization cones due to obscuring tori, as in Seyferts? Is this emission line region different in radio-loud and radio -quiet quasars, and possibly affected by radio jets shaping the ISM, or is there a contribution from star formation? How is the emission- line region affected by different host galaxies? To answer these questions one needs the high resolution of HST. Surprisingly, however, a thorough study of quasar emission- line regions has not yet been made with HST. Here we propose to use the Linear Ramp Filters (LRF) and now available dithering techniques to survey a complete sample of the seven brightest radio-quiet z<0.5 PG quasars and image their narrow line regions (NLRs) with H ST. A similar survey of Seyfert galaxies we have conducted with the LRFs has revealed spectacular jet- and bowshock-like structures, and ionization cones. Since the NLR will be affected by the host galaxy type, energy input from the central engine, the presence or absence of a nuclear torus, different types of jets, star formation, or tidal interactions, the program will help us to investigate a number of key elements of AGN physics. ------------------------------------------------------------------------------------ 8239( 9) - 05/08/00 11:37 - [ 2] Observations Description ------------------------ sectionSample selection and observations subsectionSample selection For our survey we have used the PG quasar sample which is one of the best studied quasar samples available. For all sources, high quality ground based spectroscopy, multi-color photometry, VLA observations, IR and X-ray observations are available. From this sample, we have selected all radio-quiet quasars (using the combined radio- to-optical ratio and spectral index criterion defined in Falcke et al. 1996a) with redshift z<0.5 and OIII Lambda5007 emission lines fluxes >6cdot10^-14 erg/sec/cm^2. Most of the objects in our sample have either extended optical or radio emisson (important because of the close association between radio and optical in Seyferts) as seen from ground based telescopes. subsectionFeasibility of imaging extended structures The ground based resolution of 1 -- 2arcsec would correspond to 5-10 kpc in quasars, which is not good enough to see any details. We can, however, naively assume tha t the sizes of the NLR structures are luminosity-dependent, similar to what has been found for the BLR of Seyferts and quasars from reverberation mapping (e.g. Kaspi 1997): the distance from the nucleus, r_gas, at which gas has an ionization parameter U, is r_gas \propto (Q/U)^0.5 for a given gas density, where Q is the number of ionizing photons emitted by the nucleus. The observed line flux, F, should scale as Q/D^2, where D is the distance to the galaxy. Thus the angular size of the emission-line region is Theta = r_gas/D \propto (F/U)^0.5. Since the line fluxes of quasars are one order of magnitude fainter than those of Seyferts, the angular sizes of the gas would be 3 times smaller for a given value of U. This is too small to detect detailed structures in ground based observations but it should be possible to resolve the structures with HST. This is of course an overly simplistic estimate, since it assumes a constant ionization parameter and gas density, and hence can o nl y serve as a basic illustration of the general behaviour. Wills et al. (1993) for example, using more sophisticated models to fit their FOS spectra of quasars, find that the NLR of quasars should be several kpc large and hence easily resolvable with HST. And indeed some quasars from our sample, which have already been imaged from the ground, do show extended OIII emission outside a radius of 2^ . Moreover, the extended emission-line structure of a number of radio loud quasars (also from the PG sample) has been successfuly imaged with the LRFs in an HST snapshot survey of 3C sources. subsectionChoice of filters We now propose to observe all seven quasars in our sample in the OIII line and an adjacent continuum, as well as a nearby star for PSF subtraction. The availability of Linear Ramp Filters, the refurbished WFPC2, and the advances in dithering data reduction software make this imaging project now possible. The results of our Seyfert galaxy observations have already demo ns trated that one can expect reliable and exiting results with this approach. The OIII Lambda5007 line was chosen because it traces the high- excitation gas, and in contrast to HAlpha or HBeta has no broad component, which otherwise would lead to a very strong, most likely saturated, point source in the center. In our sample the OIII Lambda5007 line is also redshifted into a regime where the WFPC2 is most sensitive, whereas HAlpha is in some cases already shifted into a relatively inefficient wavelength regime of the WFPC2. O II on the other hand would still be too far in the blue regime and also requires more integration time for the same S/N. We will observe each target in such a way as to cover the OIIILambda5007 line with the appropriate LRF. We shall also observe each quasar in an off-band continuum filter. Since in quasars the continuum is dominated by a strong point source, using a broad filter provides no additional benefits since the central pixel will saturate withi n ten to twenty seconds of observing time. Moreover, using the isophotes measured by Bahcall et al. (1997), which are around 25 mag arcsec^-2 in broad-band HST images of quasar host galaxies, we find that the contribution of the host galaxy continuum will be negligible in our narrow filter even in long exposures so that the EW of the extended nebulae will be very high. Hence, the only region of interest for continuum subtraction will be very close to the nucleus where we can get a SNR of >100 within a minute of integration even in a narrow-band filter. From our experience with Seyfert galaxies we found that narrow-band filter continuum subtraction provided superior results when compared to results obtained with broad-band filters. Broad-band imaging of quasar host galaxies can therefore not be achieved within this program and is left to other projects, some of which include sources proposed here. subsectionEstimate of integration times We have collected the nuclear (~1-2'') e mi ssion-line fluxes, which have an average value of 1* 10^- 13 erg cm^-2 s^-1 for OIII, from the study of Boroson & Green (1992). For a fiducial redshift of 0.3 the OIII line is shifted into the range around ~6500 Angstrom where the WFPC2 is most sensitive. From Stockton & MacKenty (1987) we find that the extended flux is roughly one tenth of the total flux at a radius of 2^ from the nucleus. The average flux of our sample is 10^-13 erg/sec/cm^2 and hence the surface brightness at 2^ for the extended flux is sim0.25\cdot10^- 14 erg/sec/cm^2/arcsecond. Using the WFPC2 exposure time calculator, we find that we can reach a S/N of 10 within 3200 sec. To avoid saturation and blooming of the central pixel this exposure, however, has to be split into a set of four to eight exposures of 400-800 sec length for our sources. The drawback is a slightly reduced S/N but on the other hand this will allow us to achieve effective CR rejection and dithering. For the contiuum observations a q uasar of 15.5 mag will give a S/N of 100 in the F588N filter within 60 sec, reaching 10-20\ of saturation. The line and the continuum images for each object should of course be taken on the same positions of the (WF or PC) chips. subsectionDithering As mentioned above, the large number of splits we have to do can be turned to our advantage by performing sub-pixel offsets to obtain a dithered image. Substantial progress in data reduction techniques for dithered images and CR rejection has been made during the work on the HST deep field (Fruchter 1996). The recent versions of the ``drizzling'' software make it possible to produce a final image with much higher resolution and still achieve effective CR rejection. The higher resolution will also substantially improve fitting and subtraction of the PSF, which is usually undersampled on the WFC. Hence, the planned sequence will consist of four or eight (depening on the source) sets of exposures at four positions, offset by 5.5 pi xe ls with respect to each other. Each set will consist of one or two LRF exposures and a subsequent off-band image at the same location. subsectionPSF Subtraction Another, very specific problem of quasar emission-line imaging with LRFs is the PSF subtraction. Clearly, the relatively bright central point source in quasars requires a very accurate PSF subtraction, especially if one tries to image complicated emission-line regions where also ``spider-arms'' of the PSF have to be subtracted well. However, due to the design of the LRFs and their position- dependent transmission characteristic the PSF will vary from exposure to exposure. Because of the small number of LRF images so far taken and the large number of available wavelengths it is unlikely to find matching PSFs in the archive (they are not available in the PSF library at all). The LRF PSFs have also not been investigated well enough that one could blindly use theoretically constructed 2 -dimensional PSFs. In one of our pr ev ious LRF observations we tried to subtract the PSF from the nucleus of a Seyfert galaxy (Falcke et al. 1998) by simply constructing a PSF from field stars in our exposures. Because of the above mentioned problems, however, this method will not achieve the level of accuracy needed for quasar emission-line imaging. Hence, PSF subtraction will become an important part of our data reduction efforts. Therefore we want to use the remaining time of our second orbit for each quasar to observe a nearby field star at the same position and with the same LRF setting as the previous on-band exposures. This means we will be able to construct a high-quality PSF for each quasar and as a by- product we will be able to disucss the LRF PSF behaviour in greater detail. subsectionNumber of orbits The overhead for one set of on/off-band images is 2 min for initial filter change and positioning, 2 min read out for the exposure, 1 min for off-band filter change, and 1 min readout to give a total ov er head of 6min plus integration times of 800 and 60 sec. For a set of four dithered on/off observations this gives a total of 81 minutes. Acquisition and reacquisition (two orbits) consume another 15mins to give 96 mins. For two average 55 mins orbit this leaves another 14 minutes for PSF observations: each exposure will take 2mins for integration and read out and 1 min for a small angle maneuvre for a total of 12 mins, plus an initial filter change and motion of 3mins (assuming that we find a nearby star so that reacquisition is not necessary). For the brighter quasars where we have to take more sub-images we will have to reduce our integration time slightly, but in summary we can conclude that we can fit our observations well within two orbits for each source, requiring a total of 14 orbits to observe the whole sample. Real Time Justification ----------------------- All galaxies have been observed with the VLA in snapshot modes and spectroscopic information is available. Further, high-dynamic range VLA observations will be made with the VLA at 8 GHz to be compared with the HST maps. Most of our sources are part of the HST sample by Wills et al. (1995) and have FOS spectra available. Others will be included in a STIS proposal. In another collaboration we have also proposed to image the NLR of nearby radio galaxies and quasars as a follow-up to the 3C snap-shot survey. This will allow a direct comparison of our radio-quiet sample with radio-loud AGN. Calibration Justification ------------------------- Additional Comments ------------------- ------------------------------------------------------------------------------------ 8239( 9) - 05/08/00 11:37 - [ 3] Data Distribution Paper Products: YES Media: DAT Blocking Factor: 10 Ship To: PI_Address Ship Via: Email: ------------------------------------------------------------------------------------ 8239( 9) - 05/08/00 11:37 - [ 4] TARGET LIST Fixed Targets ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial | Flux data No | Name | Description | Position |Eqnx | Vel. | ------------------------------------------------------------------------------------------------------------------------------------ 1 PG0026+129 GALAXY, QSO RA=00H 29M 13.71S +/- 0.2", J2000 V = 15.3 DEC=13D 16' 3.83" +/- 0.2", B-V = 0.3 PLATE-ID=028X 2 PG0026+129- CALIBRATION, Point RA=00H 29M 9.55S +/- 0.2", J2000 V = 11.38 CALIB Spread Function DEC=13D 15' 17.16" +/- 0.2", PLATE-ID=028X 3 PG0052+251 GALAXY, QSO RA=00H 54M 52.13S +/- 0.2", J2000 V = 15.4 DEC=25D 25' 39.33" +/- 0.2", B-V = 0.3 PLATE-ID=02BD 4 PG0052+251- CALIBRATION, Point RA=00H 55M 8.68S +/- 0.2", J2000 V = 13.51 CALIB Spread Function DEC=25D 21' 43.28" +/- 0.2", PLATE-ID=02BD 5 PG0157+001 GALAXY, QSO RA=01H 59M 50.21S +/- 0.2", J2000 V = 15.7 DEC=00D 23' 41.55" +/- 0.2", B-V = 0.3 PLATE-ID=0086 6 PG0157+001- CALIBRATION, Point RA=01H 59M 41.41S +/- 0.2", J2000 V = 14.23 CALIB Spread Function DEC=00D 19' 36.0" +/- 0.2", PLATE-ID=0086 7 PG0953+414 GALAXY, QSO RA=09H 56M 52.35S +/- 0.2", J2000 V = 15.3 DEC=41D 15' 22.53" +/- 0.2", B-V = -0.3 PLATE-ID=00XW 8 PG0953+414- CALIBRATION, Point RA=09H 56M 57.15S +/- 0.2", J2000 V = 13.61 CALIB Spread Function DEC=41D 16' 50.15" +/- 0.2", PLATE-ID=00XW 9 PG1012+008 GALAXY, QSO RA=10H 14M 54.89S +/- 0.2", J2000 V = 15.8 DEC=00D 33' 36.82" +/- 0.2", B-V = 0 PLATE-ID=023E 10 PG1012+008- CALIBRATION, Point RA=10H 14M 58.10S +/- 0.2", J2000 V = 14.06 CALIB Spread Function DEC=00D 32' 5.44" +/- 0.2", PLATE-ID=023E 11 PG1049-005 GALAXY, QSO RA=10H 51M 51.46S +/- 0.2", DEC= J2000 V = 15.95 -00D 51' 18.16" +/- 0.2", PLATE- B-V = 0 ID=00H0 12 PG1049-005- CALIBRATION, Point RA=10H 52M 4.74S +/- 0.2", DEC=- J2000 V = 13.61 CALIB Spread Function 00D 52' 33.09" +/- 0.2", PLATE- ID=00H0 13 PG1307+085 GALAXY, QSO RA=13H 9M 47.03S +/- 0.2", J2000 V = 15.28 DEC=08D 19' 49.62" +/- 0.2", B-V = 0.3 PLATE-ID=00IZ 14 PG1307+085- CALIBRATION, Point RA=13H 9M 35.60S +/- 0.2", J2000 V = 13.18 CALIB Spread Function DEC=08D 19' 22.22" +/- 0.2", PLATE-ID=00IZ 8239( 9) - 05/08/00 11:37 - [ 5] Visit: 01 Visit Priority: Visit Requirements: DROP TO GYRO IF NECESSARY On Hold Comments: Additional Comments: Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 10 PG0026+129 WFPC2 IMAGE LRF LRF 5718 CR-SPLIT=0.5 4 600 S MIN DUR 85% MAX DUR 115% ------------------------------------------------------------------------------------------------------------------------------------ 30 PG0026+129 WFPC2 IMAGE PC1-FIX F588N CR-SPLIT=0.5 1 240 S SAME POS AS 10 ------------------------------------------------------------------------------------------------------------------------------------ 40 PG0026+129- WFPC2 IMAGE LRF LRF 5718 CR-SPLIT=0.5 1 12 S CALIB ------------------------------------------------------------------------------------------------------------------------------------ 8239( 9) - 05/08/00 11:37 - [ 6] Visit: 02 Visit Priority: Visit Requirements: DROP TO GYRO IF NECESSARY On Hold Comments: Additional Comments: Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 10 PG0052+251 WFPC2 IMAGE LRF LRF 5783 DITHER-TYPE=BOX,CR-SPLIT=NO 1 300 S ------------------------------------------------------------------------------------------------------------------------------------ 15 PG0052+251 WFPC2 IMAGE LRF LRF 5783 CR-SPLIT=0.5 1 360 S POS TARG -0.725,-0.725 MAX DUR 150% MIN DUR 50% ------------------------------------------------------------------------------------------------------------------------------------ 30 PG0052+251 WFPC2 IMAGE WF3-FIX F588N CR-SPLIT=NO,DITHER-TYPE=BOX 1 60 S NO SPLIT SAME POS AS 10 ------------------------------------------------------------------------------------------------------------------------------------ 40 PG0052+251- WFPC2 IMAGE LRF LRF 5783 CR-SPLIT=NO,DITHER-TYPE=BOX 1 35 S NO SPLIT CALIB ------------------------------------------------------------------------------------------------------------------------------------ 8239( 9) - 05/08/00 11:37 - [ 7] Visit: 03 Visit Priority: Visit Requirements: DROP TO GYRO IF NECESSARY On Hold Comments: Additional Comments: Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 10 PG0157+001 WFPC2 IMAGE LRF LRF 5828 DITHER-TYPE=BOX,CR-SPLIT=NO 1 300 S ------------------------------------------------------------------------------------------------------------------------------------ 15 PG0157+001 WFPC2 IMAGE LRF LRF 5828 CR-SPLIT=0.5 1 360 S POS TARG -0.725,-0.725 MAX DUR 150% MIN DUR 50% ------------------------------------------------------------------------------------------------------------------------------------ 30 PG0157+001 WFPC2 IMAGE WF3-FIX F588N CR-SPLIT=NO,DITHER-TYPE=BOX 1 60 S NO SPLIT SAME POS AS 10 ------------------------------------------------------------------------------------------------------------------------------------ 40 PG0157+001- WFPC2 IMAGE LRF LRF 5828 CR-SPLIT=NO,DITHER-TYPE=BOX 1 45 S NO SPLIT CALIB ------------------------------------------------------------------------------------------------------------------------------------ 8239( 9) - 05/08/00 11:37 - [ 8] Visit: 04 Visit Priority: Visit Requirements: DROP TO GYRO IF NECESSARY On Hold Comments: Additional Comments: Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 10 PG0953+414 WFPC2 IMAGE LRF LRF 6204 DITHER-TYPE=BOX,CR-SPLIT=NO 1 200 S ------------------------------------------------------------------------------------------------------------------------------------ 15 PG0953+414 WFPC2 IMAGE LRF LRF 6204 CR-SPLIT=0.5 1 300 S POS TARG -0.725,-0.725 MAX DUR 150% MIN DUR 50% ------------------------------------------------------------------------------------------------------------------------------------ 17 PG0953+414 WFPC2 IMAGE LRF LRF 6204 CR-SPLIT=0.5 1 300 S POS TARG -0.775,-0.775 MAX DUR 150% MIN DUR 50% ------------------------------------------------------------------------------------------------------------------------------------ 30 PG0953+414 WFPC2 IMAGE WF2-FIX F631N CR-SPLIT=NO,DITHER-TYPE=BOX 1 60 S NO SPLIT SAME POS AS 10 ------------------------------------------------------------------------------------------------------------------------------------ 40 PG0953+414- WFPC2 IMAGE LRF LRF 6204 CR-SPLIT=NO,DITHER-TYPE=BOX 1 55 S NO SPLIT CALIB ------------------------------------------------------------------------------------------------------------------------------------ 8239( 9) - 05/08/00 11:37 - [ 9] Visit: 05 Visit Priority: Visit Requirements: DROP TO GYRO IF NECESSARY On Hold Comments: Additional Comments: Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 10 PG1012+008 WFPC2 IMAGE LRF LRF 5933 DITHER-TYPE=BOX,CR-SPLIT=NO 1 400 S ------------------------------------------------------------------------------------------------------------------------------------ 15 PG1012+008 WFPC2 IMAGE LRF LRF 5933 CR-SPLIT=0.5 1 200 S POS TARG -0.725,-0.725 MAX DUR 150% MIN DUR 50% ------------------------------------------------------------------------------------------------------------------------------------ 30 PG1012+008 WFPC2 IMAGE WF4-FIX F631N CR-SPLIT=NO,DITHER-TYPE=BOX 1 60 S NO SPLIT SAME POS AS 10 ------------------------------------------------------------------------------------------------------------------------------------ 40 PG1012+008- WFPC2 IMAGE LRF LRF 5933 CR-SPLIT=NO,DITHER-TYPE=BOX 1 60 S NO SPLIT CALIB ------------------------------------------------------------------------------------------------------------------------------------ 8239( 9) - 05/08/00 11:37 - [ 10] Visit: 06 Visit Priority: Visit Requirements: DROP TO GYRO IF NECESSARY On Hold Comments: Additional Comments: Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 10 PG1049-005 WFPC2 IMAGE LRF LRF 6794 DITHER-TYPE=BOX,CR-SPLIT=NO 1 260 S ------------------------------------------------------------------------------------------------------------------------------------ 15 PG1049-005 WFPC2 IMAGE LRF LRF 6794 CR-SPLIT=0.5 1 400 S POS TARG -0.725,-0.725 MAX DUR 150% MIN DUR 50% ------------------------------------------------------------------------------------------------------------------------------------ 17 PG1049-005 WFPC2 IMAGE LRF LRF 6794 CR-SPLIT=0.5 1 280 S POS TARG -0.775,-0.775 MAX DUR 150% MIN DUR 50% ------------------------------------------------------------------------------------------------------------------------------------ 30 PG1049-005 WFPC2 IMAGE WF2-FIX F673N CR-SPLIT=NO,DITHER-TYPE=BOX 1 60 S NO SPLIT SAME POS AS 10 ------------------------------------------------------------------------------------------------------------------------------------ 40 PG1049-005- WFPC2 IMAGE LRF LRF 6794 CR-SPLIT=NO,DITHER-TYPE=BOX 1 45 S NO SPLIT CALIB ------------------------------------------------------------------------------------------------------------------------------------ 8239( 9) - 05/08/00 11:37 - [ 11] Visit: 07 Visit Priority: Visit Requirements: DROP TO GYRO IF NECESSARY On Hold Comments: Additional Comments: Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 10 PG1307+085 WFPC2 IMAGE LRF LRF 5783 DITHER-TYPE=BOX,CR-SPLIT=NO 1 300 S GS ACQ SCENARIO SINGLE ------------------------------------------------------------------------------------------------------------------------------------ 15 PG1307+085 WFPC2 IMAGE LRF LRF 5783 CR-SPLIT=0.5 1 360 S POS TARG -0.725,-0.725 MAX DUR 150% MIN DUR 50% ------------------------------------------------------------------------------------------------------------------------------------ 30 PG1307+085 WFPC2 IMAGE WF3-FIX F588N CR-SPLIT=NO,DITHER-TYPE=BOX 1 60 S NO SPLIT SAME POS AS 10 ------------------------------------------------------------------------------------------------------------------------------------ 40 PG1307+085- WFPC2 IMAGE LRF LRF 5783 CR-SPLIT=NO,DITHER-TYPE=BOX 1 35 S NO SPLIT CALIB ------------------------------------------------------------------------------------------------------------------------------------ 8239( 9) - 05/08/00 11:37 - [ 12] Visit: 15 Visit Priority: Visit Requirements: DROP TO GYRO IF NECESSARY On Hold Comments: Additional Comments: Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 10 PG1012+008 WFPC2 IMAGE LRF LRF 5933 DITHER-TYPE=BOX,CR-SPLIT=NO 1 400 S ------------------------------------------------------------------------------------------------------------------------------------ 15 PG1012+008 WFPC2 IMAGE LRF LRF 5933 CR-SPLIT=0.5 1 200 S POS TARG -0.725,-0.725 MAX DUR 150% MIN DUR 50% ------------------------------------------------------------------------------------------------------------------------------------ 30 PG1012+008 WFPC2 IMAGE WF4-FIX F631N CR-SPLIT=NO,DITHER-TYPE=BOX 1 60 S NO SPLIT SAME POS AS 10 ------------------------------------------------------------------------------------------------------------------------------------ 40 PG1012+008- WFPC2 IMAGE LRF LRF 5933 CR-SPLIT=NO,DITHER-TYPE=BOX 1 60 S NO SPLIT CALIB ------------------------------------------------------------------------------------------------------------------------------------ 8239( 9) - 05/08/00 11:37 - [ 13] Summary Form for Proposal 8239 Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Apertures LRF PC1-FIX WF3-FIX WF2-FIX WF4-FIX ------------------------------------------------------------------------------------------------------------------------------------ Configurations WFPC2 ------------------------------------------------------------------------------------------------------------------------------------ Opmodes IMAGE ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters CR-SPLIT=0.5 CR-SPLIT=NO DITHER-TYPE=BOX ------------------------------------------------------------------------------------------------------------------------------------ Proposal Category GO ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements DROP TO GYRO IF NECESSARY MIN DUR 85% MAX DUR 115% SAME POS AS 10 POS TARG -0.725,-0.725 MAX DUR 150% MIN DUR 50% NO SPLIT SAME POS AS 10 NO SPLIT POS TARG -0.775,-0.775 MAX DUR 150% MIN DUR 50% GS ACQ SCENARIO SINGLE ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements LRF F588N F631N F673N ------------------------------------------------------------------------------------------------------------------------------------ Target Names PG0026+129 PG0026+129-CALIB PG0052+251 PG0052+251-CALIB PG0157+001 PG0157+001-CALIB PG0953+414 PG0953+414-CALIB PG1012+008 PG1012+008-CALIB PG1049-005 PG1049-005-CALIB PG1307+085 PG1307+085-CALIB ------------------------------------------------------------------------------------------------------------------------------------ Wavelengths 5718 5783 5828 6204 5933 6794 ------------------------------------------------------------------------------------------------------------------------------------