! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6702,v 7.1 1996/05/02 17:49:32 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6702,v 7.1 1996/05/02 17:49:32 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: Landis ! Phone: 410-338-4560 , E-mail: landis@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-0799.kay.prop ! Date generated: Fri Dec 22 16:04:39 EST 1995 ! Proposal_Information ! Section 4 Title: Multicolor Imaging Polarimetry of Obscured Seyfert 2 Nuclei Proposal_Category: GO Scientific_Category: AGN Cycle: 6 Investigators PI_name: Dr. Laura Kay PI_Institution: Barnard College, Columbia University CoI_Name: Dr. Ross Cohen CoI_Institution: University of California, San Diego Contact: ! Y or N (designate at most one contact) CoI_Name: Dr. Robert Antonucci CoI_Institution: University of California, Santa Barbara Contact: ! Y or N (designate at most one contact) CoI_Name: Todd Hurt CoI_Institution: University of California, Santa Barbara Contact: ! Y or N (designate at most one contact) CoI_Name: Dr. Julian Krolik CoI_Institution: Johns Hopkins University Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) The polarized flux spectra of at least 10 Seyfert 2 galaxies look like the flux spectra of Seyfert 1 nuclei, and the polarization position angles are generally perpendicular to the radio structure. This and other evidence suggests that all Seyfert 2s may have obscured Seyfert 1 nuclei visible only in reflected light. Off-nuclear dust clouds have been observed in some Seyfert 2s that reflect and bluen the nuclear light. Previously we have obtained FOS spectropolarimetry measurements on eight Seyfert 2 galaxies. Here we are proposing to use the FOC to conduct imaging polarimetry in two UV colors for 3 of these Seyferts to look for off-nuclear scattering mirrors and to resolve spatially the nuclear (electron scattering) mirrors. Polarimetric imaging provides a robust way to look for reflected radiation from hidden nuclei. Optical imaging polarimetry observations have been difficult from the ground because of the need for high spatial resolution and because of the dilution of this reflected light by starlight. The UV images will exclude almost all of the cool starlight that typically dilutes polarization, and comparisons of the images at the two wavelengths should allow us to distinguish between dust or electron scattering as the polarigenic mechanisms. We can then determine the geometry of the scattering regions and the physical nature of the scatterers. The electron scattering region size scale is a key model constraint. Questions ! Free format text (please update) Observing_Description: For each object we would like a series of FOC/96 polarization images using F275W and F342W, taking exposures in each color with POL0, POL60, and POL120. Our goal is to observe in the UV to resolve scattering mirrors near the nucleus and to reduce the dilution of the polarization by cool starlight. By measuring the polarized flux in 2 colors, we can calculate the polarized flux spectral index and distinguish between a dust scattered and an electron scattered AGN. We chose the FOC over WFPC--2 because FOC has higher angular resolution and is faster below 4500Angstroms ("Call for Proposals", p33). The FOC F320W filter has a poor PSF, and the F220W filter is not advantageous because the POL60 filter does not transmit below 1800Angstroms and drops to 65% transmittance at 2200Angstroms. Field of view was chosen to be the largest possible consistent with the required dynamic range. For Mark3 with the F275W filter we use the 512 * 512 zoomed format (7" * 14"). For Mark3 with the F342W filter and for Mark477 we use the 512 * 512 format (7" * 7"). Exposure times are 6 orbits for F275W and 3 orbits for F342W for Mark 477. The visibility period for these targets is 52 and 57 min. We will acquire guide stars and take a single polarization filter image with F275W during the first orbit, allowing for 7 min imaging overhead. The result is 37--42 min available for the first orbit, and 39--44 min for the subsequent orbits. The slightly lower exposure time in POL0 can be compensated by a slight scaling in the reductions. Mrk 3 fits into the 3 visits CVZ category, and thus we require only 3 orbits for F275W and 1 for F342W for the 3 POL filters. Images of Mrk 3, Mrk 463, and NGC 1068 suggest mirror sizes ~0.6 sq. arcsec, so we adapt that for the present objects, and plan to bin the polarization in 0.1" square bins, or larger in regions of low signal-to-noise. The fluxes are known from our FOS data and from archival images. If the polarized flux is measured to a 10% accuracy, we can fix the spectral index to an error of order 1, which will allow us to distinguish between dust (up to nu^3) and electron (nu^-1) scattering. Real_Time_Justification: Mrk 3 fits into the 3 visit CVZ category. This is our most highly polarized object; if it cannot be scheduled into the CVZ we would like to observe it as with the others for 9 orbits. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number:1 Target_Name:MARK3 Alternate_Names:UGC3426 Description:GALAXY,Seyfert,NLR Position:RA=06H 15M 36.27S +/-1", DEC=71D 02' 15.3" +/- 1", PLATE-ID=00M8 Equinox:2000 RV_or_Z:Z=0.0137 Flux:V=13.34,B-V=1.15 Comments: Target_Number:2 Target_Name:MARK477 Alternate_Names:IZW92,VV74 Description:GALAXY,Seyfert,NLR Position:RA=14H 40M 38.09S +/-1", DEC=53D 30' 16.0" +/- 1", PLATE-ID=01AL Equinox:2000 RV_or_Z:Z=0.0382 Flux:V=15.03,B-V=1.02 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:CVZ ! 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