Proposal_Information Title: FOS SPECTROPOLARIMETRY OF OVV QUASARS Proposal_Category: GTO/FOS Scientific_Category: QUASARS Cycle: 5 Investigators PI_name: Dr. J.R.P. Angel PI_Institution: Steward Observatory CoI_Name: Dr. Paul Smith CoI_Institution: Steward Observatory Contact: Y CoI_Name: Dr. Richard Allen CoI_Institution: Steward Observatory Contact: N CoI_Name: Dr. Edward Beaver CoI_Institution: UC, San Diego Contact: N CoI_Name: Dr. E. Margaret Burbidge CoI_Institution: UC, San Diego Contact: N CoI_Name: Dr. Bruce Margon CoI_Institution: University of Washington Contact: N CoI_Name: Dr. Holland Ford CoI_Institution: Johns Hopkins University Contact: N CoI_Name: Dr. Frank Bartko CoI_Institution: Martin Marietta Corporation Contact: N CoI_Name: Dr. Arthur Davidsen CoI_Institution: Johns Hopkins University Contact: N CoI_Name: Dr. Richard Harms CoI_Institution: Applied Research Corporation Contact: N CoI_Name: Dr. Ralph Bohlin CoI_Institution: Space Telescope Science Institute Contact: N Abstract: ! Free format text (please update) Several Optically Violent Variable (OVV) quasars show strong wavelength-dependent linear polarization at optical and near-IR wavelengths. The wavelength dependence is in the sense that the polarization increases with wavelength. This behavior, which is quite different from that exhibited by the other type of synchrotron-dominated AGN, the BL Lac objects, has been explained by the presence of a blue, low-polarization continuum component that dilutes the synchrotron polarization of the OVV. It has been proposed that this unpolarized continuum component is "normal" quasar light and that these objects would be low- polarization, optically selected quasars if we were not located in the line-of-sight of the relativistically-beamed synchrotron jet. This program is designed to extend the study of the polarization properties of OVV quasars into the ultraviolet. Two of the brighter OVVs, 3C345 and 3C454.3, will be observed with the polarimeter of the FOS in order to measure the dilution caused by the blue continuum component in the UV. An attempt will be made to acquire simultaneous (or near-simultaneous) ground-based optical polarimetry of these variable objects to complement the UV measurements and characterize the wavelength-dependent polarization observed at longer wavelengths. In order to facilitate these ground-based observations, we request that the HST observations be made around new moon if possible (any time during the 2 weeks following a third quarter moon will allow accurate optical polarimetry of the targets). In addition, optical measurements can only be made when the targets are reasonably placed in the night sky. Therefore, please do not schedule the 3C345 observations between September 15 and February 1. Do not schedule the 3C454.3 observations between December 15 and June 1. Questions ! Free format text (please update) Observing_Description: We propose to obtain UV spectropolarimetry of two OVV quasars using the FOS. Observations will be made using the BLUE Digicon of the FOS, 1.0 aperture, and G190H, G270H, and G400H gratings. Polarimetry using G400H will be taken so that there is some spectral overlap between the HST observations and planned near-simultaneous optical polarimetry. As stated in the Abstract, we request that the HST observations be scheduled between third and first quarter moon. Optical, ground-based polarimetric signal-to- noise ratio is largely determined by the sky background. Therefore, avoiding a bright moon is essential for accurate optical polarimetry and will greatly increase the scientific yield of the invested HST time. Since both quasars are highly variable, an ACQ/PEAK will be used to acquire the targets. Because of the variable nature of these objects, all polarimetry must be acquired during 1 visit to each target. Short spectroscopic exposures of the targets using G570H will be made during the acquisition orbits in order to fully use the available visibility time during these orbits. Real_Time_Justification: We do not require REAL-TIME observations. However, obtaining ground-based optical observations that would complement the HST UV data could be made if the HST measurements were scheduled when the moon is not too bright (+/- 1 week of the date of a new moon). Because the targets are variable, we intend to acquire near-simultaneous optical observations. These optical observations can be made only if the targets are reasonably placed in the night sky. The period between September 15 and February 1 should be avoided when scheduling the 3C345 HST observation. Likewise, please avoid December 15 to June 1 when scheduling 3C454.3. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Ground-based optical polarimetry will be obtained simultaneously (hopefully within a day) with the HST polarimetry. If possible, schedule the HST observations within 1 week of a new moon (see above). In addition, it is necessary for the targets to be in the night sky so that ground-based measurements can be made. Therefore please avoid September 15 to February 1 when scheduling 3C345 and avoid December 15 to June 1 when scheduling 3C454.3. Fixed_Targets Target_Number: 1 Target_Name: 3C345 Alternate_Names: 4C39.48,NRAO513 Description: GALAXY, Quasar Position: RA = 16H 42M 58.78S +/- 0.05S, DEC = 39D 48' 37.0" +/- 0.4", PLATE-ID = 00CL Equinox: J2000 RV_or_Z: Z = 0.595 Flux: V = 16.0 +/- 1.3, B-V = 0.3, E(B-V) = 0.00 Comments: Variable quasar (OVV) Target_Number: 2 Target_Name: 3C454.3 Alternate_Names: 4C15.76,PKS2251+158 Description: GALAXY, Quasar Position: RA = 22H 53M 57.77S +/- 0.05S, DEC = 16D 08' 53.3" +/- 0.4", PLATE-ID = 00GO Equinox: J2000 RV_or_Z: Z = 0.859 Flux: V = 16.5 +/- 1.0, B-V = 0.47, E(B-V) = 0.065 Comments: Variable quasar (OVV) Visits Visit_Number: 01 Visit_Requirements: PERIOD 29.530589D AND ZERO-PHASE 14-MAY-95:20:48 Visit_Comments: Please schedule the HST observation within 1 week of New Moon as a bright sky greatly compromises the planned optical ground based observations. ZERO-PHASE above represents full moon. Also, in order for ground based observations to be possible, the HST observation for 3C345 should be made before 15-SEP-95 or BETWEEN 1-FEB-96 AND 15-SEP-96 (i.e., ground-based observations are NOT possible between 15-SEP and 1-FEB). Optimal time for ground-based observations is MAY-JUN. The time critical specical requirements were not used because a visit cannot have both time and phase critical special requirements. Time criticality will be implmented manually by the program coordinator (Tony Roman). Exposure_Number: 100 Target_Name: 3C345 Config: FOS/BL Opmode: ACQ/PEAK Aperture: 4.3 Sp_Element: MIRROR Optional_Parameters: SCAN-STEP-Y=1.23, SEARCH-SIZE-X=1, SEARCH-SIZE-Y=3 Number_of_Iterations: 1 Time_Per_Exposure: 2.0S Special_Requirements: ONBOARD ACQ FOR 101 Exposure_Number: 101 Target_Name: 3C345 Config: FOS/BL Opmode: ACQ/PEAK Aperture: 1.0 Sp_Element: MIRROR Optional_Parameters: SCAN-STEP-X=0.61, SCAN-STEP-Y=0.61, SEARCH-SIZE-X=6, SEARCH-SIZE-Y=2 Number_of_Iterations: 1 Time_Per_Exposure: 2.0S Special_Requirements: ONBOARD ACQ FOR 102 Exposure_Number: 102 Target_Name: 3C345 Config: FOS/BL Opmode: ACQ/PEAK Aperture: 0.3 Sp_Element: MIRROR Optional_Parameters: SCAN-STEP-X=0.17, SCAN-STEP-Y=0.17, SEARCH-SIZE-X=5, SEARCH-SIZE-Y=5 Number_of_Iterations: 1 Time_Per_Exposure: 2.2S Special_Requirements: ONBOARD ACQ FOR 103-110 Exposure_Number: 103 Target_Name: 3C345 Config: FOS/BL Opmode: ACCUM Aperture: 1.0 Sp_Element: G570H Wavelength: 5690 Number_of_Iterations: 1 Time_Per_Exposure: 450S Special_Requirements: PHASE .27 TO .73 Comments: Phase represents new moon +/- ~7 days Exposure_Number: 104 Target_Name: 3C345 Config: FOS/BL Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: 1959 Optional_Parameters: POLSCAN=8B Number_of_Iterations: 1 Time_Per_Exposure: 1860S Exposure_Number: 105 Target_Name: 3C345 Config: FOS/BL Opmode: ACCUM Aperture: 1.0 Sp_Element: G270H Wavelength: 2750 Optional_Parameters: POLSCAN=8B Number_of_Iterations: 1 Time_Per_Exposure: 1860S Exposure_Number: 106 Target_Name: 3C345 Config: FOS/BL Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: 1959 Optional_Parameters: POLSCAN=8B Number_of_Iterations: 1 Time_Per_Exposure: 1860S Exposure_Number: 107 Target_Name: 3C345 Config: FOS/BL Opmode: ACCUM Aperture: 1.0 Sp_Element: G400H Wavelength: 4008 Optional_Parameters: POLSCAN=8A Number_of_Iterations: 1 Time_Per_Exposure: 1860S Exposure_Number: 108 Target_Name: 3C345 Config: FOS/BL Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: 1959 Optional_Parameters: POLSCAN=8B Number_of_Iterations: 1 Time_Per_Exposure: 1860S Exposure_Number: 109 Target_Name: 3C345 Config: FOS/BL Opmode: ACCUM Aperture: 1.0 Sp_Element: G270H Wavelength: 2750 Optional_Parameters: POLSCAN=8B Number_of_Iterations: 1 Time_Per_Exposure: 1860S Exposure_Number: 110 Target_Name: 3C345 Config: FOS/BL Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: 1959 Optional_Parameters: POLSCAN=8B Number_of_Iterations: 1 Time_Per_Exposure: 1860S Visit_Number: 02 Visit_Requirements: PERIOD 29.530589D AND ZERO-PHASE 14-MAY-95:20:48 Visit_Comments: Please schedule the HST observation within 1 week of New Moon as a bright sky greatly compromises the planned optical ground based observations. ZERO-PHASE above represents full moon. Also, in order for ground based observations to be possible, the HST observation for 3C454.3 should be made before BETWEEN 1-JUN-95 AND 15-DEC-95 or BETWEEN 1-JUN-96 AND 15-DEC-96 (i.e., ground-based observations are NOT possible between 15-DEC and 1-JUN). Optimal time for ground-based observations is SEP-OCT. The time critical specical requirements were not used because a visit cannot have both time and phase critical special requirements. Time criticality will be implmented manually by the program coordinator (Tony Roman). Exposure_Number: 200 Target_Name: 3C454.3 Config: FOS/BL Opmode: ACQ/PEAK Aperture: 4.3 Sp_Element: MIRROR Optional_Parameters: SCAN-STEP-Y=1.23, SEARCH-SIZE-X=1, SEARCH-SIZE-Y=3 Number_of_Iterations: 1 Time_Per_Exposure: 2.0S Special_Requirements: ONBOARD ACQ FOR 201 Exposure_Number: 201 Target_Name: 3C454.3 Config: FOS/BL Opmode: ACQ/PEAK Aperture: 1.0 Sp_Element: MIRROR Optional_Parameters: SCAN-STEP-X=0.61, SCAN-STEP-Y=0.61, SEARCH-SIZE-X=6, SEARCH-SIZE-Y=2 Number_of_Iterations: 1 Time_Per_Exposure: 2.0S Special_Requirements: ONBOARD ACQ FOR 202 Exposure_Number: 202 Target_Name: 3C454.3 Config: FOS/BL Opmode: ACQ/PEAK Aperture: 0.3 Sp_Element: MIRROR Optional_Parameters: SCAN-STEP-X=0.17, SCAN-STEP-Y=0.17, SEARCH-SIZE-X=5, SEARCH-SIZE-Y=5 Number_of_Iterations: 1 Time_Per_Exposure: 2.2S Special_Requirements: ONBOARD ACQ FOR 203-207 Exposure_Number: 203 Target_Name: 3C454.3 Config: FOS/BL Opmode: ACCUM Aperture: 1.0 Sp_Element: G570H Wavelength: 5690 Number_of_Iterations: 1 Time_Per_Exposure: 380S Special_Requirements: PHASE .27 TO .73 Comments: Phase represents new moon +/- ~7 days Exposure_Number: 204 Target_Name: 3C454.3 Config: FOS/BL Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: 1959 Optional_Parameters: POLSCAN=4B Number_of_Iterations: 1 Time_Per_Exposure: 2020S Exposure_Number: 205 Target_Name: 3C454.3 Config: FOS/BL Opmode: ACCUM Aperture: 1.0 Sp_Element: G270H Wavelength: 2750 Optional_Parameters: POLSCAN=4B Number_of_Iterations: 1 Time_Per_Exposure: 2020S Exposure_Number: 206 Target_Name: 3C454.3 Config: FOS/BL Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: 1959 Optional_Parameters: POLSCAN=4B Number_of_Iterations: 1 Time_Per_Exposure: 2020S Exposure_Number: 207 Target_Name: 3C454.3 Config: FOS/BL Opmode: ACCUM Aperture: 1.0 Sp_Element: G400H Wavelength: 4008 Optional_Parameters: POLSCAN=4A Number_of_Iterations: 1 Time_Per_Exposure: 2020S Data_Distribution Medium: 8MM ! 8MM or 6250BPI or 1600BPI Blocking_Factor: 10 ! 10 or 1 Ship_To: PI_Address ! 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