! 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 <angle>
! ORIENTation <angle1> TO <angle2>
! ORIENTation <angle1> TO <angle2> FROM <visit>
! ORIENTation <angle1> TO <angle2> FROM NOMINAL
! SAME ORIENTation AS <visit>
! CVZ
! PARallel
! AFTER <visit> [BY <time1> [TO <time2>]]
! AFTER <date>
! BEFORE <date>
! BETWEEN <date1> AND <date2>
! GROUP <visit-list> WITHIN <time>
! PERIOD <time> AND ZERO-PHASE <date>
! SEQ <visit-list> WITHIN <time>
! ON HOLD [FOR <visit>]
On_Hold_Comments:
Visit_Comments:
Exposure_Number: 1 ! Section 6.5
Target_Name: 3C460.0
Config: WFPC2
Opmode: IMAGE
Aperture: PC1
Sp_Element: F547M
Wavelength:
Optional_Parameters: CR-SPLIT=0.5
CR-TOLERANCE=0.0
Number_of_Iterations: 1
Time_Per_Exposure: 600S
Special_Requirements: POS TARG 0.0, 0.0
MAX DUR 2000S ! Section 7.2
MIN DUR 300S
EXPAND
! Uncomment or copy exposure level special requirements needed
Exposure_Number: 2 ! Section 6.5
Target_Name: 3C460.0
Config: WFPC2
Opmode: IMAGE
Aperture: PC1
Sp_Element: F300W
Wavelength:
Optional_Parameters: CR-SPLIT=0.5
CR-TOLERANCE=0.0
Number_of_Iterations: 1
Time_Per_Exposure: 1200S
Special_Requirements: POS TARG 0.0, 0.0
MAX DUR 2000S ! Section 7.2
MIN DUR 600S
EXPAND
END ORBIT
Exposure_Number: 3 ! Section 6.5
Target_Name: 3C460.0
Config: WFPC2
Opmode: IMAGE
Aperture: LRF
Sp_Element: LRF
Wavelength: 6348.8
Optional_Parameters: CR-SPLIT=0.5
CR-TOLERANCE=0.0
Number_of_Iterations: 1
Time_Per_Exposure: 2400S
Special_Requirements: POS TARG 0.0, 0.0
MAX DUR 3000S ! Section 7.2
MIN DUR 1200S
EXPAND
END ORBIT
Visit_Number: 2
Visit_Requirements: PCS MODE Fine
On_Hold_Comments:
Visit_Comments:
Exposure_Number: 1 ! Section 6.5
Target_Name: 3C330.0
Config: WFPC2
Opmode: IMAGE
Aperture: PC1
Sp_Element: F675W
Wavelength:
Optional_Parameters: CR-SPLIT=0.5
CR-TOLERANCE=0.0
Number_of_Iterations: 1
Time_Per_Exposure: 600S
Special_Requirements: POS TARG 0.0, 0.0
MAX DUR 2000S
MIN DUR 300S
EXPAND
Exposure_Number: 2 ! Section 6.5
Target_Name: 3C330.0
Config: WFPC2
Opmode: IMAGE
Aperture: PC1
Sp_Element: F380W
Wavelength:
Optional_Parameters: CR-SPLIT=0.5
CR-TOLERANCE=0.0
Number_of_Iterations: 1
Time_Per_Exposure: 1200S
Special_Requirements: POS TARG 0.0, 0.0
MAX DUR 2000S
MIN DUR 600S
EXPAND
END ORBIT
Exposure_Number: 3 ! Section 6.5
Target_Name: 3C330.0
Config: WFPC2
Opmode: IMAGE
Aperture: LRF
Sp_Element: LRF
Wavelength: 7761
Optional_Parameters: CR-SPLIT=0.5
CR-TOLERANCE=0.0
Number_of_Iterations: 1
Time_Per_Exposure: 2400S
Special_Requirements: POS TARG 0.0, 0.0
MAX DUR 3000S
MIN DUR 1200S
EXPAND
END ORBIT
Visit_Number: 3
Visit_Requirements: PCS MODE Fine
ORIENT 261D TO 301D
On_Hold_Comments:
Visit_Comments: ORIENT 81D TO 121D ALSO ACCEPTABLE.
Exposure_Number: 1 ! Section 6.5
Target_Name: 3C79.0
Config: WFPC2
Opmode: IMAGE
Aperture: PC1
Sp_Element: F547M
Wavelength:
Optional_Parameters: CR-SPLIT=0.5
CR-TOLERANCE=0.0
Number_of_Iterations: 1
Time_Per_Exposure: 600S
Special_Requirements: POS TARG 0.0, 0.0
MAX DUR 2000S
MIN DUR 300S
EXPAND
Exposure_Number: 2 ! Section 6.5
Target_Name: 3C79.0
Config: WFPC2
Opmode: IMAGE
Aperture: PC1
Sp_Element: F300W
Wavelength:
Optional_Parameters: CR-SPLIT=0.5
CR-TOLERANCE=0.0
Number_of_Iterations: 1
Time_Per_Exposure: 1200S
Special_Requirements: POS TARG 0.0, 0.0
MAX DUR 2000S
MIN DUR 600S
EXPAND
END ORBIT
Exposure_Number: 3 ! Section 6.5
Target_Name: 3C79.0
Config: WFPC2
Opmode: IMAGE
Aperture: LRF
Sp_Element: LRF
Wavelength: 6290
Optional_Parameters: CR-SPLIT=0.5
CR-TOLERANCE=0.0
Number_of_Iterations: 1
Time_Per_Exposure: 2400S
Special_Requirements: POS TARG 0.0, 0.0
MAX DUR 3000S
MIN DUR 900S
EXPAND
END ORBIT
Comments:
Data_Distribution ! Defaults indicated; change if desired
Medium: 8MM ! 8MM or 6250BPI or 1600BPI
Blocking_Factor: 10 ! 10 or 1
! Only astronomers with very old 9-
! track tape drives should consider
! a blocking factor of 1
Ship_To: PI_Address ! STSCI or PI_Address or <free-text>
! PI Address from Phase I is:
!
! 813 Santa Barbara St., Pasadena
! , CA 91101
!
!
Ship_Via: UPS ! UPS (2-day) or OVERNIGHT
! Overnight shipping done at PI expense
Recipient_Email: ! Needed if Ship_To: is not PI_Address
! <free-text>
! Let us know what you think of this template and software!
! Please send a list of your likes and dislikes to your Program Coordinator