! Proposal 6436, submission 1 ! PI: Dan Maoz ! Received Tue Feb 6 13:32:47 EST 1996 ! From: dani@wise.tau.ac.il ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6436,v 6.1 1997/03/18 19:16:18 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6436,v 6.1 1997/03/18 19:16:18 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: Bremmer ! Phone: 410-338-4458 , E-mail: bremmer@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-0124.maoz.prop ! Date generated: Fri Dec 22 15:31:49 EST 1995 ! Proposal_Information ! Section 4 Title: High-Resolution Narrow-Band Imaging of LINERs, in Search of Their Central Engines Proposal_Category: GO Scientific_Category: AGN Cycle: 6 Investigators PI_name: Dan Maoz PI_Institution: Tel-Aviv University CoI_Name: Michael Eracleous CoI_Institution: University of California, Berkeley Contact: ! Y or N (designate at most one contact) CoI_Name: Richard Pogge CoI_Institution: Ohio State University Contact: ! Y or N (designate at most one contact) CoI_Name: Luis Ho CoI_Institution: Center for Astrophysics Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) More than 30% of all galaxies contain LINER nuclei, which may be the weakest but most common manifestation of quasar activity. The nature of LINERs has, however, remained controversial. We propose narrow-band [OIII]5007 and Halpha+[NII] imaging of the nuclei of five LINER galaxies. These galaxies are representative of two types of LINERs that have been discovered by previous HST UV observations: UV bright, possessing a compact nuclear UV continuum source, and UV dark. We will use the images to test models for the central engines of LINERs, and to see whether the difference between UV-bright and UV-dark LINERs is the result of obscuration, episodic activity of the central UV source, or the absence of an AGN-like ionizing continuum source. Comparison of the results to similar data for Seyfert nuclei will test the idea that there is continuity between the properties of LINERs and more luminous AGNs. Although this is a self-contained project with its own objectives, the results will contribute to a large, on-going program of UV spectroscopy ( HST/FOS, approved Cycle 5), IR spectroscopy ( ISO, approved), radio mapping ( VLA, approved) and X-ray imaging spectroscopy ( ROSAT and ASCA archival data). The multiwavelength database from this program will allow a unique, comprehensive study of a well-defined sample of LINERs. Questions ! Free format text (please update) Observing_Description: In Table 1 (below) we list our proposed targets along with their heliocentric radial velocities. Data for a sixth target, NGC 404, will be obtained from the HST archive when they become public. The targets represent the two classes of LINERs identified in previous HST UV observations, and were selected on the basis of their bright, high-contrast HAlpha lines (determined from spectra and narrow-band images obtained from the ground). All of these objects are also targets of our multiwavelength program. To achieve our scientific objectives, we need to detect the line-emitting regions against a bright stellar continuum. This requires a signal-to-noise ratio (S/N) of ~10 per pixel. Since all of our targets are nearby and relatively bright, we will be able to obtain narrow-band Halpha/[NII] and [OIII] images, and corresponding off-band, continuum images for each target with WFPC2 within a few (2-4) spacecraft orbits (see below). The faintest of these objects, NGC 3718, is an exception because an [OIII] image of it would require a prohibitively long exposure time. We therefore propose to obtained only an Halpha [NII] (and corresponding off-band image) for NGC 3718. The [OIII] gap prediction of the duty cycle hypothesis will therefore not be tested in this single object. We emphasize that the proposed targets are the brightest and highest emission-line contrast objects observed by the HST in the UV -- no alternative targets exist. The redshifts of our proposed targets place the emission lines within the bandpasses of available narrow-band filters, so we will not need to resort to ramp filters. We will use the F502N filter to cover the region around the [OIII] line, and either the F656N or the F658N filter to cover the Halpha/[NII] complex (depending on the redshift). The off-band filters were chosen after considering both the bandpasses of available filters, as well as their throughputs, in order to make efficient use of spacecraft time without compromising our scientific objectives. Accordingly we have selected filters F547M and F791W as off-band filters for [OIII] and Halpha/[NII], respectively. Although the bandpasses of these filters are broad, (500 and 1,000 Angstrom, respectively), they are located close to the desired emission lines and cover very flat regions of the stellar continuum. The use of two broad bands will also improve the accuracy of the determination of the continuum underlying the emission lines. We have used a range of galaxy spectra from Ho et al. (1993) to estimate the uncertainty in the continuum level when using the broad-band filters, and find that it is less than 1%. Finally we note that these same broad-band filters have been used successfully by several GO and GTO narrow-line imaging programs of AGNs. To estimate the exposure times needed to achieve the desired S/N, we used our ground-based nuclear spectra and emission-line images of the target galaxies. Expected count rates were computed from the spectra using the SYNPHOT and XCAL software packages (Bushouse 1993; Horne 1990). The ground-based images were used to estimate the sizes and surface brightnesses of the line-emitting regions. The exposure times required to achieve S/N~ 10 per pixel are included in Table 1. These estimates show that we can achieve a S/N of 10-12 in 2 spacecraft orbits for the brighter targets, and within 4 orbits for the fainter ones. The number of orbits required for each object was computed using the available worksheets and taking into account overheads for detector readout and housekeeping tasks. If a bright point source is present, the flux in the central few pixels could exceed the mean flux per pixel by as much as a factor of 10. Hence we will divide each exposure into several sub-exposures to avoid saturation. This procedure will also facilitate elimination of cosmic rays from the images. The results of this study will contribute to a larger, on- going program to compile a multiwavelength database on a well -defined sample of LINERs. Ultraviolet spectra of four of the UV-bright LINERs (NGC 404, NGC 4569, NGC 4579, NGC 5055) have been or are being obtained with the FOS in Cycles 4 & 5. Infrared spectra of these four UV-bright LINERs and two of the UV-dark ones (NGC 4192 and NGC 3718) will be obtained during 1996 by the ISO satellite. We have an approved program to map all 25 LINERs in the HST sample with the VLA at 3.5 cm and 6 cm. We already have high spectral-resolution optical data on all the targets from Lick and Palomar Observatories, and X-ray data for several objects are available in the ROSAT and ASCA archives. As explained above, we have obtained and analyzed ground-based narrow-band images of all the targets in order to guide our target selection and reliably estimate exposure times. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: NGC3718 Alternate_Names: Description: GALAXY,SPIRAL Position: RA=11H32M35.05S +/- 0.01S,DEC=+53D 04' 05.2" +/- 0.10" ! Most common specification format is ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: J2000 RV_or_Z: V = +1247 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: SURF(V)=20.0+/-1.0 F-LINE(6563)=9.5+/-2 E-14 ! Include at least V and B-V Comments: Target_Number: 2 Target_Name: NGC4192 Alternate_Names: Description: GALAXY,SPIRAL Position: RA=12H13M48.2S +/- 0.01S,DEC=+14D54'01.0" +/- 0.10" ! Most common specification format is ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: J2000 RV_or_Z: V = -142 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: SURF(V)=20.0+/-1.0 F-LINE(6563)=9.6+/-2 E-14 ! Include at least V and B-V Comments: Target_Number: 3 Target_Name: NGC4569 Alternate_Names: Description: GALAXY,SPIRAL Position: RA=12H36M49.7S +/- 0.01S,DEC=+13D09'46.0" +/- 0.10" ! Most common specification format is ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: J2000 RV_or_Z: V = -235 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: SURF(V)=20.0+/-1.0 F-LINE(6563)=4.4+/-0.4 E-13 ! Include at least V and B-V Comments: Target_Number: 4 Target_Name: NGC4579 Alternate_Names: Description: GALAXY,SPIRAL Position: RA=12H37M43.5S +/- 0.01S,DEC=+11D49'05.0" +/- 0.10" ! Most common specification format is ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: J2000 RV_or_Z: V = +1519 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: SURF(V)=20.0+/-1.0 F-LINE(6563)=1.3+/-2 E-13 ! Include at least V and B-V Comments: Target_Number: 5 Target_Name: NGC5005 Alternate_Names: Description: GALAXY,SPIRAL Position: RA=13H 10M 56.26S +/- 0.01S,DEC=+37D 03' 32.8" +/- 0.10" ! Most common specification format is ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: J2000 RV_or_Z: V = +946 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: SURF(V)=20.0+/-1.0 F-LINE(6563)=9.5+/-2 E-14 ! Include at least V and B-V Comments: Solar_System_Targets ! Section 5.2 Generic_Targets ! Section 5.3 Scan_Data ! Appendix B ! This is a template for a single visit containing a single exposure ! Repeat exposure and visit blocks as needed Visits ! Section 6 Visit_Number: 01 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 ! 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