! Proposal 6696, submission 1 ! PI: Robert Fosbury ! Received Thu Feb 15 03:26:04 EST 1996 ! From: rfosbury@eso.org ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6696,v 6.1 1996/06/12 21:00:11 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6696,v 6.1 1996/06/12 21:00:11 pepsa Exp $ ! ! Refer to the HST Phase II Proposal Instructions to fill this out ! ! 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: Bremmer ! Phone: 410-338-4458 , E-mail: bremmer@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-0785.fosbury.prop ! Date generated: Fri Dec 22 15:43:02 EST 1995 ! ! Completed by RAEF, 14 February 1996 Proposal_Information ! Section 4 Title: Studying the UV emission line spectrum of high z radio galaxies. Effects of geometry and dust. Proposal_Category: GO Scientific_Category: AGN Cycle: 6 Investigators PI_name: Robert Fosbury PI_Institution: Space Telecope European Coordinating Facility CoI_Name: Luc Binette CoI_Institution: Obstervatoire de Lyon Contact: ! Y or N (designate at most one contact) CoI_Name: Patrick Leahy CoI_Institution: Jodrell Bank Contact: ! Y or N (designate at most one contact) CoI_Name: Sperello di Serego Alighieri CoI_Institution: Observatorio Astrofisico di Arcetri Contact: ! Y or N (designate at most one contact) CoI_Name: Clive Tadhunter CoI_Institution: University of Sheffield Contact: ! Y or N (designate at most one contact) CoI_Name: Montserrat Villar-Marti n CoI_Institution: Space Telecope European Coordinating Facility Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) Powerful radio sources at all redshifts exhibit extended structures which are believed to be excited in some way by the active nucleus. This extranuclear activity, often seen on scales exceeding 100 kpc, emits both lines and continuum in the optical and ultraviolet bands. A clear understanding of the physical processes operating in these extended emission line regions (EELR) enables us to measure the properties (gas mass and density, kinematics, chemical composition etc.) of a host galaxy's environment from the present epoch out to redshifts of 3 or 4. This is a proposal to apply newly- developed ultraviolet emission line diagnostics to the EELR in two radio galaxies which show orientation-dependent asymmetries. Ratios of resonance to semi-forbidden lines are sensitive, in distinguishable ways, both to dust and to the viewing geometry of externally illuminated clouds. By distinguishing in this way between the material on the near and far side of the AGN, we can use other observed asymmetries, eg, radio jet sidedness, radio depolarization asymmetry and EELR and radio brightness asymmetry, to build a three dimensional picture of the source and so obtain a true picture of the interactions between the various components. Such improved physical understanding will greatly sharpen our ability to disentangle stellar and AGN-induced processes in the highest redshift radio galaxies. Questions ! Free format text (please update) Observing_Description: Our main goal is to distinguish spatially the nuclear region and the off-nuclear extended emission line regions having at the same time a reasonable spectral resolution. We have defined an strategy where FOS apertures will be used, positioned in several different locations on each object, on the extended emission line regions at both sides of the nucleus (existing ground base and HST images will help us to define the exact locations where we want to position the apertures). We have selected the grating G160L using the blue digicon. This covers the spectral range 1140- 2508 Angstrom to include the four UV lines Ly-Alpha, CIV1550, HeII1640 and CIII]1909 for both our targets.We will obtain short G650L observations at each position to cross calibrate with our groundbased spectra. To calculate a typical exposure time we have used a typical target which has a surface brightness in H-Beta for the EELR filaments of ~ 6 *10^-15 erg cm^-2 s^-1 sq.arcsec^-1. From the four lines of interest, photoionization models predict that CIII] is the faintest (observations for high z radio galaxies confirm this point except for an extreme case, see fig. 2). This line is not sensitive to perspective when little dust is involved, as we expect. Derived from our photoionization models appropriate for the conditions under study, we can assume that CIII]/H-Beta ~ 1, at both sides of the nucleus. Thus, CIII] surface brightness is ~ 6* 10^-15 erg cm^-2 s^-1 sq.arcsec^-1. The inverse sensitivity of G160L at 1900 Angstrom is 9.453e-15 erg cm^-2 Angstrom ^-1 count^ -1, and using ACCUM, we have ~ 0.11 counts s^-1 diode^-1. We want a S/N of about 20 per line and this requires for each EELR position about 1-2 orbits of exposure for each blue spectrum. In addition, we need an extra orbit for each object to obtain short optical exposutes. With TA overheads, we can obtain good coverage for two targets: PKS2152-69 and PKS0349-27. We have abundant information on PKS2152-69, including HST UV polarimetry and ROSAT data, which help in the planning and interpretation. Both PKS0349-27 and PKS2152-69 have optical spectroscopy which is very useful to constrain the input parameters of our models. They will also be useful to compare the spatial distribution of the UV and optical lines. To study the UV rest frame at earlier epochs, we are applying for groundbased observations at La Silla Observatory, Chile, (3.6 and/or NTT), in order to obtain Ly-Alpha narrow band images and long slit UV (rest frame) spectra for high z radio galaxies. Additional_Comments: A public F606W PC snapshot image of PKS2152-69 has been used to plan the spectroscopy of this object. For PKS0349-27, we have used narrow-band imaging from ESO. The use of NO SPLIT and SEQ <> NON-INT for some exposures is to avoid a known RPS2 bug. Fixed_Targets ! Section 5.1 Target_Number:1 Target_Name:PKS2152-69-NUC Alternate_Names:GSC0932700131 Description:GALAXY,ELLIPTICAL,RADIO GALAXY Position:RA=21H 57M 06.02S +/- 0.06S, DEC=-69D 41' 23.3" +/-0.3", PLATE-ID=017B Equinox:J2000 RV_or_Z:Z=0.028 Flux:V=16.4+/-0.5, ! estimate of point source SURF-BKG(V)=17.4+/-0.5, ! underlying galaxy F-CONT(1450)=1+/-0.5E-15 ! From IUE Comments:PC image available in F606W, nucleus strongly peaked but saturated. Used for offset measurements. Target_Number:2 Target_Name:PKS2152-69-HEAD Alternate_Names: Description:GALAXY,ELLIPTICAL,RADIO GALAXY Position: RA-OFF=+1.286S +/- 0.02S ,DEC-OFF=+6.36" +/- 0.1" ,FROM 1 Equinox:J2000 RV_or_Z:Z=0.028 Flux:F-LINE(1216)=3 +/- 1 E-14, ! from IUE F-LINE(5007)=1 +/- 0.2 E-14 ! from GB spectroscopy Comments:Head of jet-cloud interaction Target_Number:3 Target_Name:PKS2152-69-TAIL Alternate_Names: Description:GALAXY,ELLIPTICAL,RADIO GALAXY Position: RA-OFF=+1.404S +/- 0.02S ,DEC-OFF=+7.17" +/- 0.1" ,FROM 1 Equinox:J2000 RV_or_Z:Z=0.028 Flux:F-LINE(1216)=3 +/- 1 E-14, ! from IUE F-LINE(5007)=1 +/- 0.2 E-14 ! from GB spectroscopy Comments:Tail of jet-cloud interaction Target_Number:4 Target_Name:PKS2152-69-BOW Alternate_Names: Description:GALAXY,ELLIPTICAL,RADIO GALAXY Position: RA-OFF=+0.471S +/- 0.02S ,DEC-OFF=+1.51" +/- 0.1" ,FROM 1 Equinox:J2000 RV_or_Z:Z=0.028 Flux:F-LINE(5007)=1 +/- 0.5 E-14 ! from GB spectroscopy (approx) Comments:Bow shock seen in PC image Target_Number:10 Target_Name:PKS0349-27-NUC Alternate_Names:GSC0645400099 Description:GALAXY,ELLIPTICAL,RADIO GALAXY Position:RA=03H 51M 35.82S +/- 0.07S, DEC=-27D 44' 33.9" +/- 1.0", PLATE-ID=015O Equinox:J2000 RV_or_Z:Z=0.066 Flux:V=16.0,B-V=1.0 ! Galaxy ,F-LINE(5007)= 9 +/- 2 E-15 ! from GB spectroscopy Comments:Nucleus may not be very peaked Target_Number:11 Target_Name:PKS0349-27-JETNE Alternate_Names: Description:GALAXY,ELLIPTICAL,RADIO GALAXY Position: XI-OFF=+3.99" +/- 0.2" ,ETA-OFF=+3.56" +/- 0.2" ,FROM 10 Equinox:J2000 RV_or_Z:Z=0.066 Flux:F-LINE(5007)=6 +/- 2 E-15 ! from GB spectroscopy Comments: Target_Number:12 Target_Name:PKS0349-27-JETSW Alternate_Names: Description:GALAXY,ELLIPTICAL,RADIO GALAXY Position: XI-OFF=-0.74" +/- 0.2" ,ETA-OFF=-1.26" +/- 0.2" ,FROM 10 Equinox:J2000 RV_or_Z:Z=0.066 Flux:F-LINE(5007)=3 +/- 1 E-15 ! from GB spectroscopy Comments: Target_Number:13 Target_Name:PKS0349-27-EAST Alternate_Names: Description:GALAXY,ELLIPTICAL,RADIO GALAXY Position: XI-OFF=+11.58" +/- 0.2" ,ETA-OFF=+2.31" +/- 0.2" ,FROM 10 Equinox:J2000 RV_or_Z:Z=0.066 Flux:F-LINE(5007)=2 +/- 0.5 E-15 ! from GB spectroscopy Comments: Target_Number:14 Target_Name:PKS0349-27-WEST Alternate_Names: Description:GALAXY,ELLIPTICAL,RADIO GALAXY Position: XI-OFF=-11.45" +/- 0.2" ,ETA-OFF=-0.54" +/- 0.2" ,FROM 10 Equinox:J2000 RV_or_Z:Z=0.066 Flux:F-LINE(5007)=6 +/- 2 E-15 ! from GB spectroscopy ! 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 ! DROP TO GYRO IF NECESSARY [NO REACQuisition] ! ORIENTation TO ! ORIENTation TO FROM ! ORIENTation TO FROM NOMINAL ! SAME ORIENTation AS ! CVZ ! PARallel ! SCHEDulability ! AFTER [BY [TO ]] ! AFTER ! BEFORE ! BETWEEN AND ! GROUP WITHIN