7856( 4) - 04/03/98 17:19 - [ 1] PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID: 7856 Version: 4 Check-in Date: 03-Apr-1998 17:17:50 1.Proposal Title: Jets, cones and the alignment effect in high-z radio galaxies ------------------------------------------------------------------------------------ 2. Proposal For 3. Cycle GO 7 ------------------------------------------------------------------------------------ 4. Investigators Contact? PI: CLIVE TADHUNTER UNIVERSITY OF SHEFFIELD CoI: Montse Villar-Martin University of Sheffield N CoI: Neil Clark Space Telescope Science Institute N CoI: Dave Axon Space Telescope Science Institute N ------------------------------------------------------------------------------------ 5. Abstract Two distinct physical mechanisms --- anisotropic quasar illumination and jet-cloud interactions --- are required to explain the general properties of high-z (z > 0.5) radio galaxies. Although the detection of scattered quasar features in many powerful radio galaxies demonstrates the importance of quasar illumination, the highly collimated structures visible in recent HST images are inconsistent with illumination of the ISM by the broad radiation cones predicted by the unified schemes for powerful radio sources. We argue that the failure to detect the broad cones may be due in part to an observational selection effect: that the existing OIILambda3727 images are biased towards the high surface brightness shocked structures along the radio axis. Since the gas in the radiation cones will be highly ionized, the cones will be difficult to detect in the existing OIILambda3727 images, but readily detectable in OIIILambda5007 images. We predict that the high-z radio galaxies will have a markedly different appearance in OIIILambda5007 than in the existing OIILambda3727 images, and we propose to make a sensitive search for the OIII cones in three high redshift radio galaxies using NICMOS on the HST. The detection of the broad cones outside the main aligned structures would lead to a reconciliation of the jet-cloud interaction and quasar illumination models, whereas the failure to detect the broad cones in OIII would imply that the gas structures are intrinsically aligned along the radio axes of the high redshift sources. ------------------------------------------------------------------------------------ 7856( 4) - 04/03/98 17:19 - [ 2] Observations Description ------------------------ The three targets which we have selected for this project --- 3C368 (z=1.135), 3C324 (z=1.202) and 3C266 (z=1.270) --- have all been extensively observed by the HST in the rest-frame UV (including filters covering OIILambda3727). All show highly collimated UV structures which are closely aligned to within sim10^degrees of the inner radio axis (Best et al. 1996). The aligned structures have radial extents of 2 -- 4 arcseconds. We require observations of three objects to guard against the possibility that the central illuminating quasar is unusually weak in any single source we might choose. We can make robust predictions of the expected OIII surface brightnesses of individual extended emission line regions (EELR), based on extrapolations of the properties of the EELR of low redshift radio galaxies. Note that, in contrast to the high-z radio galaxies, the EELR around most low-z radio galaxies show a broad distribution and their properties are entirely consistent with broad cone quasar illumination. It is only in a minority of cases at low redshifts that there is evidence for strong jet-cloud interactions. The redshift dependence of the OIII surface brightness of the EELR is given by the following equation: begindisplaymath SB_OIII(z) \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ \\\\propto C_f(z) Q_I(z) R(z) (1 + z)^-4 enddisplaymath where C_f(z) is the mean covering factor of individual emission line clouds/clumps as a function of redshift (z), Q_I(z) is the variation in mean quasar ionizing luminosity as a function if redshift, R(z) is the variation in the OIIILambda5007/HBeta ratio as a function of redshift, and (1 + z)^-4 is the standard cosmological dimming in the surface brightness (H_0 = 50 km s^-1 Mpc^-1 and q_0 = 0.0 assumed throughout). We now consider how the various factors in the equation are likely to change: beginenumerate item Covering factor (C(z)) We expect there to be more warm clouds/clumps present in the cones of the high redshift radio sources than in their low redshift couterparts (see scientific justification). Consequently, we are more likely to pick up clouds/clumps with large C_f, and we expect the maximum covering factor of individual clouds/clumps to increase with redshift. However, in the calculation below we make the conservative assumption that the covering factor of the warm clouds is the same at high and low redshift (i.e. C_f(z=0.07) = C_f(z = 1.0)). item Quasar ionizing luminosity (Q_I(z)) There is now considerable evidence that the quasar ionizing luminosity will increase with radio power. This evidence comprises direct correlations between optical, X-ray and radio luminosities of quasars (Browne & Murphy 1987), correlations between emission line luminosity and radio luminosity (e.g. Baum & Heckman 1989, Rawlings & Saunders 1991, Tadhunter et al. 1997) and correlations between far-IR luminosity and radio luminosity (Heckman et al. 1994). For objects selected from a flux limited sample such as 3C there will be a strong correlation between redshift and radio power. Thus, we expect the illuminating quasars in the z ~ 1 radio galaxies to be considerably more luminous than in their low redshift counterparts. The factor by which the quasars in z ~ 1 radio galaxies will be more luminous than the quasars in z ~ 0.07 radio galaxies is between Q_I(1)/Q_I(0.07) = 15 --- from the correlations based on a heterogeneous collection of quasars in Browne & Murphy (1986) --- and Q_I(1)/Q_I(0.07) = 70 --- based on the correlations between far-IR luminosity, emission line luminosity and radio power. item Ionization. Because the quasar ionizing luminosity increases with redshift, and the extended nebulosities around low redshift radio galaxies are already highly ionized (with OIIILambda5007/HBeta ~ 10), we expect the clouds in the ionization cones of high-z radio galaxies to be highly ionized (OII(3727)/OIII(5007) < 0.1; OIII(5007)/HBeta > 10). We will assume OIII/HBeta = 10, but this is likely to be conservative. endenumerate The EELR associated with the broad cones of radio galaxies in the redshift range 0.05 < z < 0.1 have typical OIII surface brightenesses of 5times10^-16 < SB_OIII < 1times10^-15 erg cm^-2 s^-1 sq.arcsec.^-1, for EELR well away from the radio axis (data from Tadhunter 1987). Following the assumptions outlined above, we estimate that the OIII surface brightnesses of the emission line regions in the broad cones of the high-z radio galaxies will be in the range 5 times10^- 16 < SB_OIII < 5 * 10^- 15 erg cm^-2 s^-1 sq.arcsec.^-1, depending on the exact factor by which the illuminating quasars at z ~ 1 a brighter than those at z = 0.075. Note that the estimated surface brightnesses of OIII in the high redshift objects are at least as large as those measured in the low redshift objects. This is because the increase in quasar ionizing luminosity with redshift more than compensates for the (1 + z)^-4 cosmological dimming. For the F110M filter, which has a bandwidth of 0.2 Mum, the predicted surface brightness translates into an effective flux density over the bandwidth of 10^-6 < SB_OIII < 10^-5 Jy sq.arcsec^- 1. Using the sensitivity figures given in the NICMOS manual for F110M and Camera 1, we estimate that we will detect ~ 8000 - 80,000 photons from the source per sq.arcsec in 10,000s. If the individual emitting filaments cover a surface area of 0.5 sq.arcsec., using the latest information on the NICMOS detectors and filter sensitivities we estimate that they will be detected at signal to noise level of S/N ~4 -- 40 in 10,000s (4 orbits), depending on the exact factor by which quasars are more luminous at z ~ 1 than they are at z ~ 0.075. This assumes that we make one major readout in MULTIACCUM mode per orbit (4 in total per object), but we have not taken into account any reduction in the effective readout noise due to combining the separate MULTIACCUM reads associated with a particular exposure. We will also take images in the medium-band F165M filter which avoids strong emission lines. These images will be used to distinguish between stellar continuum and emission line features, and produce continuum-free emission line maps. Based on previous ground-based photometry, we estimate that the typical mean H- band surface brightness within the central few arcseconds of these sources is 20.4 mag sq.arcsec.^-1. Using the sensitivity figures for the F165M filter given in the NICMOS manual we estimate that, at this surface brightness level, we will achieve a S/N of ~ 8 for a 0.1 sq.arcsec. extraction aperture in a 2400s exposure. This will be more than adequate to map the distribution of starlight in the host galaxies. Note that the starlight will only be a significant source of noise in our F110M images in the central cores of the galaxies (< 1 arcsec. radius); at larger radii the background, readout noise and dark current will dominate. With 10,000s (~4 orbits) integration per object in F110M, and 2400s (~1 orbit) total integration per object in F165M , we will require 15 orbits to complete observations of 3 sources. Real Time Justification ----------------------- Calibration Justification ------------------------- Additional Comments ------------------- ------------------------------------------------------------------------------------ 7856( 4) - 04/03/98 17:19 - [ 3] Data Distribution Media: DAT Blocking Factor: 10 Ship To: PI_Address Ship Via: Email: ------------------------------------------------------------------------------------ 7856( 4) - 04/03/98 17:19 - [ 4] TARGET LIST a) Fixed Targets ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial | Flux data No | Name | Description | Position |Eqnx | Vel. | ------------------------------------------------------------------------------------------------------------------------------------ 1 3C368 GALAXY,RADIO GALAXY RA=18H 5M 6.41S +/- J2000 J = 18.06+/-0.16 0.02S,DEC=11D 1' 33.0" +/- 0.2" F-CONT(11000)=2.0+/-0.2e-17 Comments: The object is too faint to be visible in DSS images. The above position is the accurate position of the radio core derived from the latest VLA radio maps of the source (Best et al. 1997). This position has been cross-checked with positions from the Texas radio catalogue, and with the position for the same source in the NICMOS exposure catalogue. All the positions agree to within ~1 acrcec (both coordinate).The major uncertainty in the position is the offset between the radio and GSS astrometric reference frames (<0.5 arcseconds in most cases).N.B. The GSS Plate-ID is given as 08ZO in the fits header of the DSS image retrieved from STScI, but the programme won't accept this on processing, so I have deleted the Plate-ID (it is not relevant anyway given that the object is not visible in the DSS image). 2 3C324 GALAXY,RADIO GALAXY RA=15H 49M 48.81S +/- J2000 H = 18.07+/-0.17 0.02S,DEC=21D 25' 38.0" +/- 0.2" F-CONT(16000)=7.0+/-1.0e-18 Comments: The object is too faint to be visible in DSS images. The above position is the accurate position of the radio core derived from the latest radio maps of the source. The major uncertainty in the position is the offset between the radio and GSS astrometric reference frames (<0.5 arcseconds in most cases).N.B. The GSS Plate-ID is given as A0Z8 in the fits header of the DSS image retrieved from STScI, but the programme won't accept this on processing, so I have deleted the Plate-ID (it is not relevant anyway given that the object is not visible in the DSS image). 3 3C266 GALAXY,RADIO GALAXY RA=11H 45M 43.35S +/- J2000 K = 17.88+/-0.09 0.02S,DEC=49D 46' 7.8" +/- F-CONT(22000)=3.3+/-0.5e-18 0.2",PLATE-ID=024C Comments: The object is too faint to be visible in DSS images. The above position is the accurate position of the radio core derived from the latest radio maps of the source. The major uncertainty in the position is the offset between the radio and GSS astrometric reference frames (<0.5 arcseconds in most cases). 7856( 4) - 04/03/98 17:19 - [ 5] Visit: 01 Visit Priority: Visit Requirements: On Hold Comments: Additional Comments: There is one exposure for each orbit ([OIII] emission lines). The object will be moved by a small amount (1.505 arcsec/ 35 pixels N,S,E,W relative to the centre) between orbits in order to be certain of avoiding regions of reduced sensitivity and to improve sky subtraction/flat fielding. No ORIENT is specified (for the parallel observations) since the parallel observations with NIC2 are not of a specific target but of the general field (for the archive). Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 1 3C368 NIC1 MULTIAC NIC1 F110M SAMP-SEQ=SPARS256,NSAMP=12 1 DEF POS TARG -1.505,0.0 PAR 2 CUM WITH 1 ------------------------------------------------------------------------------------------------------------------------------------ 2 ANY NIC2 MULTIAC NIC2 F110W NSAMP=12,SAMP-SEQ=SPARS256 1 DEF CUM ------------------------------------------------------------------------------------------------------------------------------------ 3 3C368 NIC1 MULTIAC NIC1 F110M SAMP-SEQ=SPARS256,NSAMP=13 1 DEF POS TARG 1.505,0.0 PAR 4 CUM WITH 3 ------------------------------------------------------------------------------------------------------------------------------------ 4 ANY NIC2 MULTIAC NIC2 F110W NSAMP=12,SAMP-SEQ=SPARS256 1 DEF CUM ------------------------------------------------------------------------------------------------------------------------------------ 5 3C368 NIC1 MULTIAC NIC1 F110M SAMP-SEQ=SPARS256,NSAMP=13 1 DEF POS TARG 0.0,1.505 PAR 6 CUM WITH 5 ------------------------------------------------------------------------------------------------------------------------------------ 6 ANY NIC2 MULTIAC NIC2 F110W NSAMP=12,SAMP-SEQ=SPARS256 1 DEF CUM ------------------------------------------------------------------------------------------------------------------------------------ 7 3C368 NIC1 MULTIAC NIC1 F110M SAMP-SEQ=SPARS256,NSAMP=13 1 DEF POS TARG 0.0,-1.505 PAR 8 CUM WITH 7 ------------------------------------------------------------------------------------------------------------------------------------ 8 ANY NIC2 MULTIAC NIC2 F160W NSAMP=12,SAMP-SEQ=SPARS256 1 DEF CUM ------------------------------------------------------------------------------------------------------------------------------------ 9 3C368 NIC1 MULTIAC NIC1 F110M SAMP-SEQ=SPARS256,NSAMP=13 1 DEF PAR 10 WITH 9 CUM ------------------------------------------------------------------------------------------------------------------------------------ 10 ANY NIC2 MULTIAC NIC2 F160W NSAMP=12,SAMP-SEQ=SPARS256 1 DEF CUM ------------------------------------------------------------------------------------------------------------------------------------ 7856( 4) - 04/03/98 17:19 - [ 6] Visit: 02 Visit Priority: Visit Requirements: On Hold Comments: Additional Comments: There is one primary exposure for each of the first four orbits ([OIII] images), but there are two primary exposures in the last orbit (for the continuum). The object will be moved by a small amount (1.505 arcsec/ 35 pixels N,S,E,W relative to the centre) between orbits in order to be certain of avoiding regions of reduced sensitivity and to improve sky subtraction/flat fielding. No ORIENT is specified (for the parallel observations) since the parallel observations with NIC2 are not of a specific target but of the general field (for the archive). Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 1 3C324 NIC1 MULTIAC NIC1 F110M SAMP-SEQ=SPARS256,NSAMP=12 1 DEF POS TARG -1.505,0.0 PAR 2 CUM WITH 1 ------------------------------------------------------------------------------------------------------------------------------------ 2 ANY NIC2 MULTIAC NIC2 F110W NSAMP=12,SAMP-SEQ=SPARS256 1 DEF CUM ------------------------------------------------------------------------------------------------------------------------------------ 3 3C324 NIC1 MULTIAC NIC1 F110M SAMP-SEQ=SPARS256,NSAMP=13 1 DEF POS TARG 1.505,0.0 PAR 4 CUM WITH 3 ------------------------------------------------------------------------------------------------------------------------------------ 4 ANY NIC2 MULTIAC NIC2 F110W NSAMP=12,SAMP-SEQ=SPARS256 1 DEF CUM ------------------------------------------------------------------------------------------------------------------------------------ 5 3C324 NIC1 MULTIAC NIC1 F110M SAMP-SEQ=SPARS256,NSAMP=13 1 DEF POS TARG 0.0,1.505 PAR 6 CUM WITH 5 ------------------------------------------------------------------------------------------------------------------------------------ 6 ANY NIC2 MULTIAC NIC2 F110W NSAMP=12,SAMP-SEQ=SPARS256 1 DEF CUM ------------------------------------------------------------------------------------------------------------------------------------ 7 3C324 NIC1 MULTIAC NIC1 F110M SAMP-SEQ=SPARS256,NSAMP=13 1 DEF POS TARG 0.0,-1.505 PAR 8 CUM WITH 7 ------------------------------------------------------------------------------------------------------------------------------------ 8 ANY NIC2 MULTIAC NIC2 F160W NSAMP=12,SAMP-SEQ=SPARS256 1 DEF CUM ------------------------------------------------------------------------------------------------------------------------------------ 9 3C324 NIC1 MULTIAC NIC1 F165M SAMP-SEQ=SPARS256,NSAMP=7 1 DEF POS TARG -1.505,0.0 CUM ------------------------------------------------------------------------------------------------------------------------------------ 10 3C324 NIC1 MULTIAC NIC1 F165M SAMP-SEQ=SPARS256,NSAMP=7 1 DEF POS TARG 1.505,0.0 CUM ------------------------------------------------------------------------------------------------------------------------------------ 7856( 4) - 04/03/98 17:19 - [ 7] Visit: 03 Visit Priority: Visit Requirements: On Hold Comments: Additional Comments: There is one primary exposure for each orbit ([OIII] emission line). The object will be moved by a small amount (1.505 arcsec/ 35 pixels N,S,E,W relative to the centre) between orbits in order to be certain of avoiding regions of reduced sensitivity and to improve sky subtraction/flat fielding. No ORIENT is specified (for the parallel observations) since the parallel observations with NIC2 are not of a specific target but of the general field (for the archive). Exposures ------------------------------------------------------------------------------------------------------------------------------------ Exposure| Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | Special Number | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 1 3C266 NIC1 MULTIAC NIC1 F110M SAMP-SEQ=SPARS256,NSAMP=13 1 DEF POS TARG -1.505,0.0 PAR 2 CUM WITH 1 ------------------------------------------------------------------------------------------------------------------------------------ 2 ANY NIC2 MULTIAC NIC2 F110W NSAMP=13,SAMP-SEQ=SPARS256 1 DEF CUM ------------------------------------------------------------------------------------------------------------------------------------ 3 3C266 NIC1 MULTIAC NIC1 F110M SAMP-SEQ=SPARS256,NSAMP=13 1 DEF POS TARG 1.505,0.0 PAR 4 CUM WITH 3 ------------------------------------------------------------------------------------------------------------------------------------ 4 ANY NIC2 MULTIAC NIC2 F110W NSAMP=13,SAMP-SEQ=SPARS256 1 DEF CUM ------------------------------------------------------------------------------------------------------------------------------------ 5 3C266 NIC1 MULTIAC NIC1 F110M SAMP-SEQ=SPARS256,NSAMP=13 1 DEF POS TARG 0.0,1.505 PAR 6 CUM WITH 5 ------------------------------------------------------------------------------------------------------------------------------------ 6 ANY NIC2 MULTIAC NIC2 F110W NSAMP=13,SAMP-SEQ=SPARS256 1 DEF CUM ------------------------------------------------------------------------------------------------------------------------------------ 7 3C266 NIC1 MULTIAC NIC1 F110M SAMP-SEQ=SPARS256,NSAMP=13 1 DEF POS TARG 0.0,-1.505 PAR 8 CUM WITH 7 ------------------------------------------------------------------------------------------------------------------------------------ 8 ANY NIC2 MULTIAC NIC2 F160W NSAMP=13,SAMP-SEQ=SPARS256 1 DEF CUM ------------------------------------------------------------------------------------------------------------------------------------ 9 3C266 NIC1 MULTIAC NIC1 F110M SAMP-SEQ=SPARS256,NSAMP=13 1 DEF POS TARG -1.505,0.0 PAR CUM 10 WITH 9 ------------------------------------------------------------------------------------------------------------------------------------ 10 ANY NIC2 MULTIAC NIC2 F160W NSAMP=13,SAMP-SEQ=SPARS256 1 DEF CUM ------------------------------------------------------------------------------------------------------------------------------------ 7856( 4) - 04/03/98 17:19 - [ 8] Summary Form for Proposal 7856 Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations NIC1 NIC2 ------------------------------------------------------------------------------------------------------------------------------------ Opmodes MULTIACCUM ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters SAMP-SEQ=SPARS256 NSAMP=12 NSAMP=13 NSAMP=7 ------------------------------------------------------------------------------------------------------------------------------------ Proposal Category GO ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements POS TARG -1.505,0.0 PAR 2 WITH 1 POS TARG 1.505,0.0 PAR 4 WITH 3 POS TARG 0.0,1.505 PAR 6 WITH 5 POS TARG 0.0,-1.505 PAR 8 WITH 7 PAR 10 WITH 9 POS TARG -1.505,0.0 POS TARG 1.505,0.0 POS TARG -1.505,0.0 PAR 10 WITH 9 ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements F110M F110W F160W F165M ------------------------------------------------------------------------------------------------------------------------------------ Target Names 3C368 ANY 3C324 3C266 ------------------------------------------------------------------------------------------------------------------------------------