! NOTE: THIS VERSION MODIFIED AFTER PMDB PROPOSAL PREP SO THAT THE ORIENT ! ANGLE AND COMMENT WOULD REFLECT WHAT WAS ACTUALLY IMPLEMENTED IN THE ! PMDB. - RAL - 5 JULY, 1995 ! Proposal 5930, submission 1 ! PI: Dr. Patrick McCarthy ! Received Wed Mar 15 18:43:47 EST 1995 ! From: odea@stsci.edu ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5930,v 6.1 1995/07/05 14:11:44 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: Ray Lucas ! Phone: 410 338-4716 , E-mail: lucas@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Date generated: Sat Dec 17 10:46:07 EST 1994 ! Proposal_Information ! Section 4 Title: WFPC2 Imaging of Intermediate Redshift Radio Galaxies Proposal_Category: GO Scientific_Category: AGN Cycle: 5 Investigators PI_name: Dr. Patrick McCarthy PI_Institution: Observatories of the Carnegie Institution CoI_Name: Dr. Stefi Baum CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Dr. William Sparks CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Dr. George Miley CoI_Institution: Sterrewatch, Leiden University Contact: ! Y or N (designate at most one contact) CoI_Name: Dr. Daniel Golombek CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Dr. John Birretta CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Dr. Duccio Macchetto CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We propose to image three radio galaxies with redshifts between 0.2 and 0.5. All of these showed significant structure on sub-arc second scales in our SNAPSHOT images from cycle 4. These galaxies appear to be intermediate redshift analogues to the high redshift radio galaxies and exhibit the alignment effect. This short program will provide insights into the physical processes that are produce the extended continuum and emission-line regions in powerful radio sources. Questions ! Free format text (please update) Observing_Description: We intend to observe each object in OIII for a single orbit and to use a second orbit for each target to observe through two continuum filters. We have chose the two continuum filters to provide line-free continuum ( or as much so as possible) in the optical near OIII and in the rest frame ultraviolet and we intend to scale our integrations times by the throughput of the telescope/filter assembly to provide roughly equal sensitivity in the optical and uv (rest frame) images. All observations will be cr-split. In a single orbit, we will thus obtain optical integrations of roughly 8 minutes total duration and uv integrations of roughly 24 minutes total duration. Our existing WFPC2 snapshot continuum images (see Figure 1.), which are of duration roughly 3 minutes total show interesting features, but also pass light from emission lines at the redshifts of our objects. With the new continuum images we request here, we will obtain line- free continuum images in two colours with a signal to noise better than that of our snapshot observations. The rest frame optical observations will allow us to subtract the continuum from our line images, the rest frame uv images will allow us to study the alignment effect in these low redshift sources at the same rest wavelengths at which the alignment affect is seen in the high redshift radio galaxies, and the two colours will allow us to pinpoint blue regions (e.g., synchrotron jets and hotspots, scattering cones, star formation). We have ground-based OIII5007 images of all three galaxies and so have a reliable measure of the total fluxes and surface brightnesses at 1^'' resolution (McCarthy et al. 1994, in press). We estimate that in 1 orbit, we can obtain a signal to noise of roughly 3-5 for the line emission, under the conservative assumption that the line emission seen in the ground based images is evenly spread over the 1'' ground based beam (see sample calculation below). These observations will be crucial for studying gas/jet interactions, for distinguishing continuum and gas features and for studying their relationship to one another (e.g., both shocked gas and uv synchrotron might be expected to arise in similar sites). Sample Line Calculation > From ground based images in OIII5007, we know that the line flux of 3C460 is 3* 10^-15 erg/sec/cm^2 and that that emission is spread over a region roughly 1'' x 4'' in size. For the WF we therefore expect a flux of roughly 7.5 * 10^-18 per pixel (making the conservative estimate that the flux is evenly spread over that region). Using the information provided in the WFPC2 handbook, we find that in a typical single orbit integration time of 2400 seconds, we will achieve a signal to noise of roughly 3 per pixel, allowing for quantization and shot noise. However, the typical signal to noise should be quite a bit higher, as we expect the line emitting regions to show significant structure on the scale of the HST beam. NOTE: On advice of WFPC2 IS John Biretta ( one of our co-Is ) we have changed Exp Log line 3 in Visits 1 and 2 to LRF. Likewise, on the same basis, we have changed Exp Log line 3 in visit 3 to LRF in combination with an absolute ORIENT range. A value 180 degrees off this ORIENT range is acceptable also if necessary for scheduling purposes. Real_Time_Justification: At present we extensive supporting observations in hand. These consist of the SNAPSHOT images shown above, as well as ground-base photometry, long-slit spectra, narrow-band images and VLA observations. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: 3C460.0 Alternate_Names: Description: GALAXY; RADIO GALAXY; Position: RA=23H 18M 59.75S +/- 0.1S, ! Most common specification format is DEC=+23D 30M 20.4S +/- 1" , ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: B1950 RV_or_Z: Z=0.268 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=18.8 ! Include at least V and B-V Comments: B-V=0.5 +/- 0.2 Target_Number: 2 Target_Name: 3C330.0 Alternate_Names: Description: GALAXY; RADIO GALAXY; HIGH Z GAL; Position: RA=16H 09M 13.90S +/- 0.1S, ! Most common specification format is DEC=+66D 04M 22.8S +/- 1" , ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: B1950 RV_or_Z: Z=0.550 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=20.33 ! Include at least V and B-V Comments: B-V=0.5 +/- 0.2 Target_Number: 3 Target_Name: 3C79.0 Alternate_Names: Description: GALAXY; RADIO GALAXY; Position: RA=03H 07M 11.48S +/- 0.1S, ! Most common specification format is DEC=+16D 54M 36.9S +/- 1", ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: B1950 RV_or_Z: Z=0.2559 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=18.5 ! Include at least V and B-V Comments: B-V=0.5 +/- 0.2 ! 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: PCS MODE Fine ! 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