! File: 4942C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:11:34:42 coverpage: title_1: ACTIVE GALACTIC NUCLEI - CYC2HIGH sci_cat: QUASARS & AGN proposal_for: GTO/HSP cont_id: 1099 pi_fname: ROBERT pi_mi: C. pi_lname: BLESS pi_inst: WISCONSIN, UNIVERSITY OF pi_country: USA pi_phone: (608)262-1715 keywords_1: QUASARS; BL LAC OBJECTS; ACTIVE GALACTIC NUCLEI hours_pri: 9.63 num_pri: 33 realtime: Y ! end of coverpage abstract: line_1: The discovery of QSO's and (other) active galactic line_2: nuclei have radically altered the classical view of line_3: galactic evolution as a slow process occuring over line_4: cosmological time-scales. From the growing body of line_5: observations there are many varied theories line_6: developing to explain these highly energetic line_7: phenomena. To be successful, a theory must explain line_8: the large amplitude, rapid variations in both flux line_9: and polarization that characterize these objects. line_10: Variability in all parts of the spectrum has been line_11: observed, in some cases on time scales as short as line_12: minutes, placing constraints on the volume over line_13: which the phenomenon occurs. Observations on even line_14: shorter time scales would significantly affect these line_15: constraints. This program will monitor the intensity line_16: and linear polarization of the radiation emitted by line_17: AGN's and relate the results to the structure of line_18: their nuclei and the nature of their central power line_19: source. Revision History: Prepared for future line_20: cycles submission--BJW 4/22/92; ! ! end of abstract general_form_proposers: lname: VAN CITTERS fname: G. mi: W. inst: NATIONAL SCIENCE FOUNDATION country: USA ! lname: BLESS fname: ROBERT mi: C. inst: WISCONSIN, UNIVERSITY OF country: USA ! lname: DOLAN fname: JOSEPH mi: F. inst: NASA, GODDARD SPACE FLIGHT CENTER country: USA ! lname: ELLIOT fname: JAMES mi: L. inst: MASSACHUSETTS INSTITUTE OF TECHNOLOGY country: USA ! lname: ROBINSON fname: EDWARD mi: L. inst: TEXAS, UNIVERSITY OF country: USA ! lname: WHITE fname: RICHARD mi: L. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The wavelength dependence of linear polarization, line_2: its associated position angle, and the intensity of line_3: the radiation emitted by active galactic nuclei will line_4: be monitored over several different timescales line_5: (seconds to months). Representatives of different line_6: members of several classes of AGN's will be line_7: monitored: BL Lac objects; quasars, including those line_8: which are X-ray sources, are radio loud, possess line_9: super-liminal expansion, etc.; Seyfert Galaxies; and line_10: AGN's possessing a jet morphology. The shortest line_11: timescales over which photometric or polarimetric line_12: fluctuations are observed to occur can be related to line_13: the maximum scales size of the emitting region. line_14: Cycle 0 (SV/GTO) observations: None ! question: 4 section: 1 line_1: (1) UV observations, accessible only to ST, are line_2: expected to reveal more information about the line_3: objects than observations in the visual region. The line_4: energy source is presumed to involve high energy line_5: phenomena; hence, the higher the energy of the line_6: photons one observes, the fewer intermediate steps line_7: are required between the energy source and the line_8: emission of the observed photon. Fewer intermediate line_9: steps imply that more direct inferences can be made line_10: about the energy source itself. (2) UV measurents line_11: of the wavelength dependence of polarization will line_12: effectively double the frequency interval over which line_13: we have polarimetric information. ! question: 7 section: 1 line_1: Intrinsic polarization can be distinguished from line_2: polarization impressed on a beam of radiation by its line_3: travel through the interstellar or intergalactic line_4: medium by means of its (a) temporal variability line_5: (interstellar and intergalactic polarization can line_6: vary only on timescales of millenia); (b) wavelength line_7: dependence (different from that impressed on the line_8: radiation by the ISM or the IGM); or (c) variation line_9: in magnitude or position angle vs. distance from the line_10: active central region of the object under study, if line_11: resolvable. The methods of distinguishing between line_12: various source mechanisms emitting the observed line_13: radiation once the intrinsic polarization is known line_14: are too detailed to merit exposition here, but line_15: typical methods of analysis are outlined in the line_16: following references: - Aligned grains causing line_17: optical polarization in Type I Seyferts: Martin et line_18: al., 1982. - Shot-like flaring of independent line_19: sources of randomly oriented strong optical line_20: polarization in BL Lac objects: Moore et al., 1982. ! question: 12 section: 1 line_1: Observing the polarization of active extragalactic line_2: objects is Scientific Objective 5 of the HSP CEI line_3: specifications: "Determination of the wavelength and line_4: time dependence of polarization in . . . , QSO's, line_5: active galactic nuclei, etc." ! question: 13 section: 1 line_1: The intensity and linear polarization of the line_2: radiation emitted by a representative sample of line_3: active galactic nuclei (including BL Lac objects, line_4: quasars and Seyfert galaxies) will be monitored on line_5: timescales ranging from seconds to months. The line_6: results will be used to determine the structure of line_7: the nuclei of active extragalactic objects and the line_8: nature of their central power source. ! !end of general form text general_form_address: lname: BLESS fname: ROBERT mi: C. category: PI inst: UNIVERSITY OF WISCONSIN addr_1: UNIVERSITY OF WISCONSIN addr_2: SPACE ASTRONOMY LAB. city: MADISON state: WI zip: 53706 country: USA ! lname: DOLAN fname: JOSEPH mi: F. category: CON inst: NASA, GODDARD SPACE FLIGHT CENTER addr_1: CODE 681 city: GREENBELT state: MD zip: 20771 country: USA phone: (301)286-5920 telex: 89675 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: BL-LAC descr_1: ACTIVE GALACTIC NUCLEUS pos_1: RA = 22H 02M 43.27S +/- 0.1S, pos_2: DEC = +42D 16' 40.3"+/-1" equinox: 2000 comment_1: POSREF = DOLAN fluxnum_1: 1 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 0.700 sequence_1: DEFINE sequence_2: ACQP targname: # config: HSP/POL opmode: ACQ num_exp: 1 time_per_exp: 40S s_to_n: 15 s_to_n_time: 0.05S fluxnum_1: 1 priority: # ! linenum: 1.000 sequence_1: DEFINE sequence_2: POL targname: # config: HSP/POL opmode: SINGLE aperture: POL0 sp_element: # num_exp: 1 time_per_exp: 180S s_to_n: 100 fluxnum_1: 1 priority: # req_1: SEQ 1-4 NON-INT; req_2: CYCLE 3 /1.000-43.2; ! linenum: 2.000 sequence_1: ^ targname: # config: ^ opmode: ^ aperture: POL90 sp_element: # num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: # ! linenum: 3.000 sequence_1: ^ targname: # config: ^ opmode: ^ aperture: POL45 sp_element: # num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: # ! linenum: 4.000 sequence_1: ^ targname: # config: ^ opmode: ^ aperture: POL135 sp_element: # num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: # ! linenum: 35.900 sequence_1: USE ACQP targname: BL-LAC priority: 2 req_1: ONBOARD ACQ FOR 38.000-39.000; req_2: SEQ 35.900-39.000 NO GAP; req_3: CYCLE 3 / 35.900-43.2000; req_4: PCS MODE FINE / 35.900-43.2000; ! linenum: 38.000 sequence_1: USE POL targname: BL-LAC sp_element: F277M priority: 2 ! linenum: 39.000 sequence_1: USE POL targname: BL-LAC sp_element: F277M priority: 2 ! linenum: 40.050 sequence_1: USE ACQP targname: BL-LAC priority: 2 req_1: ONBOARD ACQ FOR 40.100-40.200; req_2: SEQ 40.050-40.200 NO GAP; req_3: AFTER 35.900 BY 2D +/- 0.1D; ! linenum: 40.100 sequence_1: USE POL targname: BL-LAC sp_element: F277M priority: 2 ! linenum: 40.200 sequence_1: USE POL targname: BL-LAC sp_element: F277M priority: 2 ! linenum: 41.050 sequence_1: USE ACQP targname: ^ priority: 2 req_1: ONBOARD ACQ FOR 41.100-41.200; req_2: AFTER 40.050 BY 2D +/- 0.1D; req_4: SEQ 41.050-41.200 NO GAP; ! linenum: 41.100 sequence_1: USE POL targname: BL-LAC sp_element: F277M priority: 2 ! linenum: 41.200 sequence_1: USE POL targname: BL-LAC sp_element: F277M priority: 2 ! linenum: 42.050 sequence_1: USE ACQP targname: BL-LAC priority: 2 req_1: ONBOARD ACQ FOR 42.100-42.200; req_2: AFTER 41.050 BY 2D +/- 0.1D; req_4: SEQ 42.050-42.200 NO GAP; ! linenum: 42.100 sequence_1: USE POL targname: BL-LAC sp_element: F277M priority: 2 ! linenum: 42.200 sequence_1: USE POL targname: BL-LAC sp_element: F277M priority: 2 ! linenum: 43.050 sequence_1: USE ACQP targname: BL-LAC priority: 2 req_1: ONBOARD ACQ FOR 43.100-43.200; req_2: AFTER 42.050 BY 2D +/- 0.1D; req_4: SEQ 43.050-43.200 NO GAP; ! linenum: 43.100 sequence_1: USE POL targname: BL-LAC sp_element: F277M priority: 2 ! linenum: 43.200 sequence_1: USE POL targname: BL-LAC sp_element: F277M priority: 2 ! ! end of exposure logsheet ! No scan data records found