! Proposal 5923, submission 2 ! PI: Axon David ! Received Fri Aug 4 20:09:33 EDT 1995 ! From: axon@stsci.edu ! Anything after a "!" is ignored, and may be deleted ! ! All keywords with multiple entries are comma delimited except the ! Visit_Requirements and Special_Requirements keywords which can be ! delimited with carriage returns or semi-colons, but not commas ! ! For help call your Program Coordinator: Ray Lucas ! Phone: 410 338-4716 , E-mail: lucas@stsci.edu Proposal_Information ! Section 4 Title: The Structure of The Emission Line Regions of Compact Steep Spectrum Radio Sources. Proposal_Category: GO Scientific_Category: AGN Cycle: 5 Investigators PI_name: David J. Axon PI_Institution: Space Telescope Science Institute CoI_Name: Andrew Robinson CoI_Institution: Institute of Astronomy, Cambridge University Contact: ! Y or N (designate at most one contact) CoI_Name: Ralph Spencer CoI_Institution: Nuffield Radio Astronomy Laboratories Contact: ! Y or N (designate at most one contact) CoI_Name: Hardip Sanghera CoI_Institution: Netherlands Foundation for Research in Astronomy Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) Extended emission line regions (EELR) aligned with the radio structure have been found in AGN of all radio powers and redshifts. This alignment implies that the nuclear radiation is collimated. Generally the EELR of Seyfert galaxies stretch many Kpc beyond their radio structure and their ionization structure is dominated by the form of the nuclear radiation. In contrast the EELR in powerful radio sources are co-spatial with the radio structure. There, interactions with the radio ejecta are an important source of excitation. This contribution severly limits our ability to use the EELR as an aspect independent method of determining the role of beaming at high luminosity. The Compact Steep Spectrum sources have quasi-linear radio structure confined to small angular (<= 0.2 -1.5 '') and spatial scales (<= 10 Kpc). We believe that anisotropic radiation will excite EELR beyond the CSS radio emission, providing a high radio luminosity sample in which these effects are decoupled. This will allow a direct study of beaming in gas which is not interacting with the radio ejecta for a sample of sources with a wind range of intrinsic powers. In contrast on scales Co-spatial with the radio structure we expect to see the strong interactions manifested as NLR. We have already developed a true dynamical model for the formation of the NLR in Seyferts which explains both their velocity field and morphology. Resolving the emission structure of CSS and comparing this with the radio structure is essential in extending this modeling to the regime of more powerful ionizing radiation field and very large shock velocities. In principal finding and measuring displacemnts between the gas and radio emission in this region gives cooling times and hence shock velocities. Here we propose WFPC/2 emission line imagery of the CSS in CIV or OIII5007 to establish their emission line structure and its relationship to the radio structure. Questions ! Free format text (please update) Observing_Description: We propose a program of narrow band imaging of CSS with the WFPC2 to allow us to establish the emmision line structure of the sources. We have chosen a representative sub-sample of objects which stradle a wide a range of redshift/radio power as possible from those studied previously with MERLIN. These include both QSO's and radio galaxies. Our observing stratergy will be to make two exposures per source using available ramp filters to isolate either CIV at intermediate z and OIII5007 in the low z subsets and and the continuum emission. We have calculated the exposure times from the ground based spectroscopy using a toy model in which the gas is confined to a cylinder aligned with the radio axis, and whose length corresponds to the size of the observed region, typically 2-5 arcseconds. We have designed our programme so as to reach a limiting surface brightness of 10^(-15) erg cm^ -2 s^-1 per pixel. Even if we then fail to detect ENLR the NLR structure will still be well measured. As it stands the programme is a large one, and we regard this as the optimuum sample. Some part of the programme can however be accomplished with a smaller allocation at the cost of z range. Follow on spectroscopy will be deffered until HST longslit capabilities are restored with STIS. Real_Time_Justification: None The data will be reduced using the standard FOS pipeline processing and standard packages such as IRAF/STSDAS. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: 3C48 Alternate_Names: Description: Galaxy, Radio Galaxy Position: RA=01H 37M 41.30S +/- 0.05S, DEC=33D 09' 35.39" +/- 0.05" ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=16.2+/- 0.1 ! Include at least V and B-V Comments: Target_Number: 2 Target_Name: 3C303.1 Alternate_Names: Description: Galaxy, Radio Galaxy Position: RA=14H 43M 14.44S +/- 0.05S, DEC=77D 07' 22.6" +/- 0.05" ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=19.0+/- 0.5 ! Include at least V and B-V Comments: Target_Number: 3 Target_Name: 3C277.1 Alternate_Names: Description: Galaxy, Radio Galaxy Position: RA=12H 52M 26.38S +/- 0.05S, DEC=56D 34' 19.41" +/- 0.05" ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=17.2+/- 0.5 ! Include at least V and B-V Comments: Target_Number: 4 Target_Name: 3C147 Alternate_Names: Description: Galaxy, Radio Galaxy Position: RA=05H 42M 36.12S +/- 0.05S, DEC=49D 51' 07.178" +/- 0.05" ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=16.9+/- 0.5 ! Include at least V and B-V Comments: Target_Number: 5 Target_Name: 4C12.50 Alternate_Names: Description: Galaxy, Radio Galaxy Position: RA=13H 47M 33.36S +/- 0.05S, DEC=12D 17' 24.2" +/- 0.05" ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=17.2+/- 0.5 ! Include at least V and B-V Comments: Target_Number: 6 Target_Name: 3C268.3 Alternate_Names: Description: Galaxy, Radio Galaxy Position: RA=12H 06M 24.71S +/- 0.05S, DEC=64D 14' 40.94" +/- 0.05" ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=17.2+/- 0.5 ! Include at least V and B-V Comments: Target_Number: 7 Target_Name: 3C454.1 Alternate_Names: Description: Galaxy, Radio Galaxy Position: RA=22H 50M 32.59S +/- 0.05S, DEC=71D 29' 19.06" +/- 0.05" ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=17.8+/- 0.5 ! Include at least V and B-V Comments: ! This is a template for a single visit containing a single exposure ! Repeat exposure and visit blocks as needed Visits ! Section 6 Visit_Number: 1 Visit_Requirements: ! Section 7.1 ! Uncomment or copy visit level special requirements needed ! Most of these requirements (including ORIENT) will limit scheduling ! PCS MODE [Fine | Gyro] ! GUIDing TOLerance ! ORIENTation TO ! ORIENTation TO FROM ! ORIENTation TO FROM NOMINAL ! SAME ORIENTation AS ! CVZ ! PARallel ! AFTER [BY [TO ]] ! AFTER ! BEFORE ! BETWEEN AND ! GROUP WITHIN