! This version incorporates changes from FOS/RD to FOS/BL with associated ! changes in times of ACQ/BINARY exposures. - RAL 2 August, 1995 ! Proposal 5928, submission 2 ! PI: Dr. Dean C. Hines ! Received Thu Jun 29 17:36:03 EDT 1995 ! From: dhines@pan.as.utexas.edu ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5928,v 4.1 1995/08/02 17:15:40 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 10:43:59 EST 1994 ! Proposal_Information ! Section 4 Title: Hidden QSOs in ``Warm'' Infrared Ultraluminous Galactic Nuclei Proposal_Category: GO Scientific_Category: AGN Cycle: 5 Investigators PI_name: Dr. Dean C. Hines PI_Institution: Steward Observatory CoI_Name: Dr. Beverley Wills CoI_Institution: University of Texas Contact: N ! Y or N (designate at most one contact) CoI_Name: Dr. Robert Goodrich CoI_Institution: StScI Contact: N ! Y or N (designate at most one contact) CoI_Name: Dr. Paul Smith CoI_Institution: Steward Observatory Contact: N ! Y or N (designate at most one contact) CoI_Name: Dr. Richard Allen CoI_Institution: Steward Observatory Contact: N ! Y or N (designate at most one contact) CoI_Name: Dr. Michael Sitko CoI_Institution: University of Cincinnati Contact: N ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) Our ground-based optical spectropolarimetry shows that nearly half of our sample of ``warm'' IR-Ultraluminous AGNs (L_IR >= 10^11.5 Lsun) exhibit high and wavelength dependent polarization (up to p = 25%). In several we observe typical QSO broad emission line spectra in polarized light suggesting an inner structure similar to the axisymmetric geometry proposed for lower luminosity AGNs such as NGC 1068. Our ground based spectropolarimetry also suggests a strong connection between the IR-Ultraluminous AGNs and the rare Broad Absorption Line (BAL) QSOs; the BALQSOs and the IR-Ultraluminous AGNs would appear as normal UV-excess QSOs if viewed along a different line of sight. UV-spectropolarimetry, which can only be accomplished with the HST FOS, combined with our ground-based optical spectropolarimetry will allow us to distinguish between electron scattering, dust scattering and dichroic absorption. In addition, the wide wavelength coverage will allow us to compare the polarization properties of the continuum, and emission-line and absorption-line features of different ionizations, and thus constraining the geometries of these regions. Questions ! Free format text (please update) Observing_Description: We propose to obtain UV spectropolarimetry of 2 highly polarized IR-Ultraluminous AGNs using the HST FOS. One is very highly polarized and probably highly obscured, while the other is confirmed BALQSOs. We have chosen the G270H grating for the polarization observations because it offers the best throughput. We also include G190H to examine the detailed emission/absorption profile of CIV in IRAS 07598+6508, and we include G190H observations to look for possible CIV and SiIV Broad Absorption Lines in IRAS 14026+4341 in total light. The expected UV polarizations for IRAS 07598+6508 and IRAS 14026+4341 are 4% and 12% respectively. Accurate polarimetry requires p/dp >= 5 in each resolution element, where dp = sqrt(2/Ct) with (C) being the expected counts per second per diode, and (t) the total integration time. We estimate C using the prescriptions outlined in the FOS Users Manual (Version 5.0) assuming F \propto nu^-2 in Table 1.2.2 and scaling by the object's V magnitude, or (when available) by estimating the count rate from highly smoothed IUE spectra. The steep powerlaw is justified by the reddened spectrum observed for these objects. We have selected bin sizes large enough to maximize the signal-to-noise, but small enough that the emission and absorption line polarization can be accurately determined. To obtain the polarization, at least 4 separate exposures with the waveplate at different position angles are required. The total number of orbits required for each object was estimated from the total integration time plus the overhead times needed to acquire the object, and to obtain 4 exposures per polarization observation. The overhead times for POLSCAN-4B were provided by USB and add about 6 minutes to the nominal overhead for ACCUM. For example, we estimate the count rate for the MgII broad absorption trough in IRAS 07598+6508 to be 0.5 c/s using the G270H filter and assuming a polarization at least 4%. The absorption feature is 12,000 km s-1 wide so 10 pixel bins allows approximately 5 resolution elements across the feature. The required exposure time to achieve p/dp >= 5 is 1.8 hours. For 3 orbits, the overhead times are 30 min, 27 min, and 14 min for guide star, acquisition and POLSCAN+ACCUM respectively for a total 71 minutes. The total spacecraft time is thus 179 minutes. Each orbit lasts approximately 60 minutes, so 3 orbits are needed to accomplish this observation. Observations of polarized and null standards during Cycle 4 have been planned by the FOS/Spectropolarimetry team (R.A. & P.S.). These time estimates are accurately reflected in the RPS2 output. 2 August, 1995 NOTE: Due to problems with the calibration of FOS/RD polarimetry, we have now switched to FOS/BL, with concurrent changes in the ACQ/BINARY exposure times. The new FOS/BL ACQ/BINARY exposure times we are using are ones which were recommended by the FOS Instrument Scientist. Real_Time_Justification: We do not require REAL-TIME observations. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Ground-based optical spectropolarimetry of all our targets has been previously obtained (resolution 300 -- 750 kms). Additional higher resolution optical spectropolarimetry of IRAS 07598+6508 and IRAS 14026+4341 are planned for the Spring and Summer 1995 seasons using facilities at McDonald and Steward Observatories. Fixed_Targets Target_Number: 1 Target_Name: IR1334+24 Alternate_Names: PSC 13349+2438 Description: GALAXY, QSO, Ultraluminous IR Gal, Nucleus, BLR Position: RA = 13H 37M 18.718S +/- 0.05S, DEC = 24D 23' 02.95" +/- 0.4", PLATE-ID = 01GF Equinox: J2000 RV_or_Z: Z = 0.1078 Flux: V = 14.7 +/- 0.5, F(3100) = 5 E-15, F(2700) = 4 E-15, F(1900) = 2 E-15, E(B-V) = 0.0 Comments: Fluxes based on low S/N IUE spectrophotometry Target_Number: 2 Target_Name: IR1402+43 Alternate_Names: PSC 14026+4341 Description: GALAXY, QSO, Ultraluminous IR Gal, Nucleus, BLR Position: RA = 14H 04M 38.860S +/- 0.05S, DEC = 43D 27' 07.0" +/- 0.4", PLATE-ID = 00XZ Equinox: J2000 RV_or_Z: Z = 0.323 Flux: V = 15.7 +/- 0.5, B-V = 0.2, F(3200) = 3 E-15 Comments: Flux density based on ground-based spectrophotometry Visits ! Section 6 Visit_Number: 01 Visit_Requirements: ! 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