! Proposal 5909, submission 1 ! PI: Neal Jackson ! Received Fri Mar 10 06:38:16 EST 1995 ! From: pi21@stsci.edu ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5909,v 2.1 1995/03/10 19:03:29 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: Marc Bremmer ! Phone: 410 338-4458 , E-mail: bremmer@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Date generated: Sat Dec 17 10:07:11 EST 1994 ! Proposal_Information ! Section 4 Title: Complete Ionization Mapping of Cygnus A Proposal_Category: GO Scientific_Category: AGN Cycle: 5 Investigators PI_name: Neal Jackson PI_Institution: NRAL Jodrell Bank CoI_Name: Clive Tadhunter CoI_Institution: Sheffield University Contact: N ! Y or N (designate at most one contact) CoI_Name: Martin Shaw CoI_Institution: Sheffield University Contact: N ! Y or N (designate at most one contact) CoI_Name: George Miley CoI_Institution: Leiden Observatory Contact: N ! Y or N (designate at most one contact) CoI_Name: William Sparks CoI_Institution: STScI Contact: N ! Y or N (designate at most one contact) CoI_Name: Duccio Macchetto CoI_Institution: STScI Contact: N ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We propose the most detailed imaging study yet undertaken of a wide range of lines in the prototypical radio galaxy Cygnus A. Lines of ionization states from OI to OIII will be investigated and correlated in detail with each other and with the radio structure. The data will allow us to investigate the physical mechanisms operating in each separate part of the source and hence to disentangle the influences of nuclear photoionization and shocks induced by the passage of the radio jet. The data will also allow us to clarify the current confusion regarding the possible nitrogen overabundance. Since all the phenomena occur within a radius of 0.5" this is not possible from the ground: we know from previous investigations that clumping takes place on scales (0.1--0.2 arcsecond) that are only accessible to the HST. Our ultimate goal will be to determine what parts of the extended line and continuum emission have their origins in photoionization by a hidden nucleus (quantifying the degree of anisotropy with which this nucleus emits) and what parts are shock excited (determining with unprecedented clarity the physical conditions in the shocks). Questions ! Free format text (please update) Observing_Description: We calculate the expected flux in the weakest line, OI. The magnitude of the continuum in V in the central 4" (roughly the extent of the emission lines) is about 16.3. In the ramp filter (assuming a bandwidth of 80Angstrom , cf figure 3.3 of the WFPC2 Handbook and an efficiency 30\ less than that of the 673N filter) we will obtain about 100 continuum counts per second within this area (using equation 6.1. of the WFPC2 Handbook). The equivalent width of the line is about 50Angstrom , hence we will obtain 60 line counts per second. We expect the bulk of the line counts to be distributed within regions totalling a few square arcseconds, so the ``astrophysically interesting'' pixels will contain about 0.3 continuum and 0.2 line counts per second. The corresponding continuum image to be subtracted will have a bandwidth about 10 times bigger and therefore about 3 counts per second. Integration times of 30 minutes in the line filter will therefore give S:N in the line per pixel of 360/SQRT((540+360) = 12 per pixel. 2 orbits are therefore necessary for a good (S:N 20) image of OI and 1 orbit will be used for the other, stronger lines. Real_Time_Justification: The authors are engaged in a programme of study of Cygnus A with ground based telescopes. CNT and MS have extensive new spectroscopic data taken with the William Herschel Telescope which is just published or in press. NJ and CNT have new blue spectropolarimetric data to constrain the nature of Cygnus A's blue extended continuum emission which was taken last month an is now being analysed. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number:1 Target_Name:3C405 Alternate_Names:CYGNUS-A Description:GALAXY Position:RA=19H 59M 28.34S +/- 0.01S, DEC=40D 44' 2.2" +/- 0.1" Equinox:J2000 RV_or_Z:Z=0.057 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux:V=16.3,B-V=0.7 ! 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 On_Hold_Comments: Visit_Comments: Exposure_Number:10 ! Section 6.5 Target_Name:3C405 Config:WFPC2 Opmode:IMAGE Aperture:LRF Sp_Element:LRF Wavelength:3937 Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:2300S Special_Requirements: Comments: Exposure_Number:13 ! Section 6.5 Target_Name:3C405 Config:WFPC2 Opmode:IMAGE Aperture:LRF Sp_Element:LRF Wavelength:3937 Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:1100S Special_Requirements: Comments: Exposure_Number:40 ! Section 6.5 Target_Name:3C405 Config:WFPC2 Opmode:IMAGE Aperture:LRF Sp_Element:LRF Wavelength:3937 Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:1200S Special_Requirements: Comments: Exposure_Number:42 ! Section 6.5 Target_Name:3C405 Config:WFPC2 Opmode:IMAGE Aperture:LRF Sp_Element:LRF Wavelength:3937 Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:1000S Special_Requirements: Comments: Exposure_Number:43 ! Section 6.5 Target_Name:3C405 Config:WFPC2 Opmode:IMAGE Aperture:PC1 Sp_Element:F814W Wavelength: Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:1000S Special_Requirements: Comments: Exposure_Number:50 ! Section 6.5 Target_Name:3C405 Config:WFPC2 Opmode:IMAGE Aperture:LRF Sp_Element:LRF Wavelength:6657 Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:2500S Special_Requirements: Comments: Exposure_Number:53 ! Section 6.5 Target_Name:3C405 Config:WFPC2 Opmode:IMAGE Aperture:LRF Sp_Element:LRF Wavelength:6657 Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:1000S Special_Requirements: Comments: Exposure_Number:70 ! Section 6.5 Target_Name:3C405 Config:WFPC2 Opmode:IMAGE Aperture:PC1 Sp_Element:F336W Wavelength: Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:1000S Special_Requirements: Comments: Exposure_Number:77 ! Section 6.5 Target_Name:3C405 Config:WFPC2 Opmode:IMAGE Aperture:PC1 Sp_Element:F336W Wavelength: Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:1100S Special_Requirements: Comments: Exposure_Number:80 ! Section 6.5 Target_Name:3C405 Config:WFPC2 Opmode:IMAGE Aperture:LRF Sp_Element:LRF Wavelength:6934 Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:1100S Special_Requirements: Comments: Visits ! Section 6 Visit_Number: 2 Visit_Requirements: ! Section 7.1 On_Hold_Comments: Visit_Comments: Exposure_Number:90 ! Section 6.5 Target_Name:3C405 Config:WFPC2 Opmode:IMAGE Aperture:LRF Sp_Element:LRF Wavelength:5290 Optional_Parameters:CR-SPLIT=NO Number_of_Iterations:1 Time_Per_Exposure:400S Special_Requirements: Comments: Exposure_Number:91 ! Section 6.5 Target_Name:3C405 Config:WFPC2 Opmode:IMAGE Aperture:LRF Sp_Element:LRF Wavelength:5290 Optional_Parameters:CR-SPLIT=NO Number_of_Iterations:1 Time_Per_Exposure:400S Special_Requirements: Comments: Exposure_Number:92 ! Section 6.5 Target_Name:3C405 Config:WFPC2 Opmode:IMAGE Aperture:LRF Sp_Element:LRF Wavelength:5290 Optional_Parameters:CR-SPLIT=NO Number_of_Iterations:1 Time_Per_Exposure:500S Special_Requirements: Comments: Exposure_Number:95 ! Section 6.5 Target_Name:3C405 Config:WFPC2 Opmode:IMAGE Aperture:LRF Sp_Element:LRF Wavelength:6934 Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:400S Special_Requirements: 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 ! PI Address from Phase I is: ! ! Lower Withington, Macclesfield, ! 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