! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5850,v 2.1 1995/01/26 21:45:11 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: Peg Stanley ! Phone: 410 338-4536 , E-mail: pstanley@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: dopita-106.prop ! Date generated: Fri Dec 16 15:38:12 EST 1994 ! Proposal_Information ! Section 4 Title: A Definitive Test for the Excitation Mechanism of LINERs Proposal_Category: GO Scientific_Category: AGN Cycle: 5 Investigators PI_name: Michael A. Dopita PI_Institution: Mt. Stromlo and Siding Spring Observatories CoI_Name: Anuradha Koratkar CoI_Institution: Space Telescope Science Institute Contact: Y ! Y or N (designate at most one contact) CoI_Name: Geoffrey V. Bicknell CoI_Institution: Mt. Stromlo and Siding Spring Observatories Contact: ! Y or N (designate at most one contact) CoI_Name: Ralph S. Sutherland CoI_Institution: JILA, University of Colorado Contact: ! Y or N (designate at most one contact) CoI_Name: John F. Hawley CoI_Institution: Virginia Institute for Theoretical Astronomy, U. of Virginia Contact: ! Y or N (designate at most one contact) CoI_Name: Elaine Sadler CoI_Institution: Dept. of Physics, U. of Sydney Contact: ! Y or N (designate at most one contact) CoI_Name: Mark Allen CoI_Institution: Mt. Stromlo and Siding Spring Observatories Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We propose to undertake a definitive test which will determine whether LINERs are photoionised or shock ionised, by obtaining a single FOS spectrum of the bright, nearby and unreddened accretion disk of M87 from 1150 - 6800 Angstrom. At visible wavelengths, the emission-line diagnostics which might distinguish between excitation mechanisms are ambiguous. However, models generated using our shock and photoionisation code MAPPINGS II, shows that a comparison between the optical and the UV line intensities produces an unambiguous diagnostic. The shock produces a strong UV emission line spectrum, and the photoionisation mechanism does not. If LINER nuclei turn out to be shock excited, we will be able to compare the results with the predictions of the magnetic instability model of Balbus and Hawley (1991) which provides both a means of angular momentum transport in accretion disks, and of shock generation in the outer atmospheric layers of such disks. This would provide a powerful new insight into the accretion process of AGN, and open up the way for a quantitative understanding of the LINER phenomenon. Questions ! Free format text (please update) Observing_Description: In Cycle 5 we propose to obtain a complete, high quality spectrum of a single region of the M87 accretion disk at a radial distance of 0.5 arc sec. from the nucleus, using the 0.86 as circular aperture of FOS. We would obtain FOS/BL spectrophotometry in the range 1150-4500Angstrom using the G130H, G190H gratings and Prism , and FOS/RD spectrophotometry in the range 2221-6740Angstrom using G270H , G400H, and G570 gratings. Tho optical spectra are necessary to properly normalise the UV spectra to the optical. We aim to achieve a sensitivity which is sufficient to detect lines as faint as 5% of H-beta throughout the UV and optical spectrum. The FOS/BL Prism observation is needed to ensure reliable calibration between the FOS/BL and the FOS/RD observations. Real_Time_Justification: For the FOS spectrophotometry to be used as input to modelling codes, all the observations on the blue side, and all the observations on the red side need to be obtained contiguously, and without interruption. The proposed observation is entirely self-contained. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: NGC4486 Alternate_Names: M87 Description: Galaxy, Elliptical, Liner Position: RA=12H 30M 49.4286S +/- 0.3S, DEC=+12D 23' 27.985" +/- 0.3", PLATE-ID=00IY Equinox: J2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=16.7 E(B-V)= 0.01 Comments: Target_Number: 2 Target_Name: NGC4486-OFFSET Alternate_Names: M87-OFFSET Description: Galaxy, Elliptical, Liner Position: R=0.6", PA=201D, FROM 1, PLATE-ID=00IY Equinox: J2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=16.25 E(B-V)= 0.01 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 ! 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