! File: 5231C.PROP ! Database: PEPDB ! Date: 24-FEB-1994:02:14:10 coverpage: title_1: KP1635 ADDITION sci_cat: QUASARS & AGN proposal_for: GTO/HSP longterm: 3 cont_id: 1096 pi_fname: ROBERT pi_mi: C. pi_lname: BLESS pi_inst: WISCONSIN, UNIVERSITY OF pi_country: USA pi_phone: 608-262-1715 keywords_1: GRAVITATIONAL LENSES; BLACK HOLES; HUBBLE CONSTANT hours_pri: 8.38 num_pri: 7 ! end of coverpage abstract: line_1: Photometric and polarimetric observations will be line_2: made of systems whose properties are ascribed to the line_3: effect of a gravitational lens. The similarity of line_4: the images in the previously unobserved UV region of line_5: the spectrum, both photometrically and line_6: polarimetrically, is necessary for these objects to line_7: be gravitational lens systems; any differences found line_8: will be carefully studied to determine what line_9: constraints they put on the system. Systems whose line_10: properties appear consistent with a point mass line_11: deflector (i.e., a black hole) will be monitored to line_12: determine whether photometric or polarimetric line_13: variablity exists in the images. The distance to the line_14: deflecting mass in this case can be related to the line_15: path length difference between the two image paths line_16: from the imaged quasar to the observer. The path line_17: length difference can be derived directly from the line_18: time difference between the same variation occurring line_19: in each image. The parallaxes of objects at E+3 Mpc line_20: distances are of obvious importance to a wide ! ! end of abstract general_form_proposers: lname: VAN CITTERS fname: G. mi: W. inst: NATIONAL SCIENCE FOUNDATION 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 ! 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 ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The operational method of determing delta t would be line_2: to: -determine if the quasar image more distant line_3: from the deflecting mass varies photometrically or line_4: polarimetrically; -if so, detect some characteistic line_5: signature in the variation; (Timescales on the order line_6: of weeks are the optimum ones sought for the purpose line_7: of this program.) -monitor the other image until the line_8: variation with this characteristic signature is line_9: detected; then -observe the second image well enough line_10: to identify the variation as identical to the one line_11: previously observed in the first image. Cycle 1 line_12: (SV/GTO) observations: Exposures (line numbers) line_13: 45.9 - 61.1 and, Exposures (line numbers) 61.9 - line_14: 67.25 Cycle 2 (SV/GTO) observation: Exposures (line line_15: numbers) Note:STScI had to divide this program 71.9 line_16: - 82.2 into two programs, 1096 and 1391. ! question: 4 section: 1 line_1: Justification of necessity of ST observations: (1) line_2: Observations in the UV, accessible only to ST, will line_3: effectively double the frequency range over which line_4: the similarity of the images broad-band spectral and line_5: polarimetric properities can be examined. (2) The line_6: reliable identification of individual variations line_7: requires accurate photometry or polarimetry. The line_8: images are faint enough that the increased signal to line_9: noise avilable with ST/HSP over ground-based line_10: photmetry (polarimetry) may make the difference line_11: between identifying an individual variation and line_12: remaining uncertain to whether a variation seen in line_13: one image is really identical to that observed in line_14: the other. ! question: 7 section: 1 line_1: Description of plans for data reduction and analysis line_2: Standard data reduction procedures will be applied line_3: to both the photometric and polarimetric data. line_4: Measurements of any photmetric quantity or line_5: normalized Stokes parameter will be compared to the line_6: same quantity measured at a different time, i.e., line_7: relative and not absolute measurements will be made. line_8: Analysis will concentrate on the detection of line_9: characteristic signatures in any variablity line_10: detected. The derivation of the parallax of the line_11: deflecting mass from an observed time delay is out line_12: lined in Sec. 2. above. ! question: 12 section: 1 line_1: The gravitational lens program is directly related line_2: to the third scientific objective of HSP listed in line_3: the CEI specifications: "Measurement of the time line_4: scales of fastest variablity of ... Quasi-Stellar line_5: Objects (QSO's) to determine their characteristic line_6: dimensions", and also the fifth scientific line_7: objective, "Determination of the wavelength and time line_8: dependence of polarization in ... QSO's active line_9: galactic nuclei, etc.". ! question: 13 section: 1 line_1: Photometric and polarimetric observations will be line_2: made of gravitational lens systems whose properties line_3: suggest that a black hole may be the deflecting line_4: mass. If the lensed quasar is variable, a line_5: characteristic signature in the variation will be line_6: sought and the delayed image monitored to determine line_7: the path length difference between images by a line_8: "time-of-flight" measurement. The parallax of the line_9: deflecting mass may then be determined. ! !end of general form text general_form_address: lname: BLESS fname: ROBERT mi: C. category: PI inst: UNIVERSITY OF WISCONSIN addr_1: SPACE ASTRONOMY LAB. addr_2: 1150 UNIVERSITY AVE. city: MADISON state: WI zip: 53706 country: USA phone: 608-262-1715 ! lname: DOLAN fname: JOSEPH mi: F. category: CON inst: NASA GODDARD SFC addr_1: CODE 681 city: GREENBELT state: MD zip: 20771 country: USA phone: 301-286-5920 ! ! end of general_form_address records fixed_targets: targnum: 10 name_1: KP1635+267A descr_1: GRAVITATIONALLY LENSED QUASAR pos_1: RA = 16H 34M 59.1S +/- 0.1S, pos_2: DEC = +26D 42' 04" +/- 1" equinox: 1950 comment_1: POSREF = AP.J.,V221,PP473,1978 fluxnum_1: 1 fluxval_1: V=18.5 ! targnum: 11 name_1: KP1635+267B descr_1: ^ pos_1: RA-OFF= -0.047S +/- 0.01S, pos_2: DEC-OFF= +3.72" +/- 0.1", pos_3: FROM 10 equinox: ^ comment_1: POSREF = DOLAN fluxnum_1: 1 fluxval_1: V=20.0 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 0.500 sequence_1: DEFINE sequence_2: ACQP targname: # config: HSP/POL opmode: ACQ num_exp: 1 time_per_exp: 1M s_to_n: # fluxnum_1: 1 priority: # ! linenum: 5.000 sequence_1: DEFINE sequence_2: POL targname: # config: HSP/POL opmode: STAR-SKY aperture: POL0 sp_element: # num_exp: 1 time_per_exp: 200S s_to_n: 100 fluxnum_1: 1 priority: # param_1: # req_1: SEQ 5-7 NON-INT; ! linenum: 7.000 sequence_1: ^ targname: # config: ^ opmode: ^ aperture: POL90 sp_element: # num_exp: ^ time_per_exp: 200S s_to_n: 100 fluxnum_1: 1 priority: # param_1: # ! linenum: 9.000 sequence_1: ^ targname: # config: ^ opmode: ^ aperture: POL45 sp_element: # num_exp: ^ time_per_exp: 200S s_to_n: 100 fluxnum_1: 1 priority: # param_1: # req_1: SEQ 9-11 NON-INT; ! linenum: 11.000 sequence_1: DEFINE sequence_2: POL targname: # config: HSP/POL opmode: STAR-SKY aperture: POL135 sp_element: # num_exp: 1 time_per_exp: 200S s_to_n: 100 fluxnum_1: 1 priority: # param_1: # ! linenum: 45.900 sequence_1: USE ACQP targname: KP1635+267A time_per_exp: X3 s_to_n: 10 s_to_n_time: 0.9S priority: 2 req_1: ONBOARD ACQ FOR 49.000-49.109; req_2: CYCLE 3 / 45.900-49.109; req_3: PCS MODE FINE / 45.900-49.109; ! linenum: 49.000 sequence_1: USE sequence_2: POL targname: KP1635+267A sp_element: F277M priority: 2 param_1: SPOILER-ANGLE=340.5, param_2: SPOILER-SPREAD=10, param_3: SKY-SAMPLE=0.3, req_1: SEQ 45.9-49.109 NO GAP; ! linenum: 49.001 sequence_1: USE sequence_2: POL targname: KP1635+267A sp_element: F277M priority: 2 param_1: SPOILER-ANGLE=340.5, param_2: SPOILER-SPREAD=10, param_3: SKY-SAMPLE=0.3, ! linenum: 49.002 sequence_1: USE sequence_2: POL targname: KP1635+267A sp_element: F277M priority: 2 param_1: SPOILER-ANGLE=340.5, param_2: SPOILER-SPREAD=10, param_3: SKY-SAMPLE=0.3, ! linenum: 49.003 sequence_1: USE sequence_2: POL targname: KP1635+267A sp_element: F277M priority: 2 param_1: SPOILER-ANGLE=340.5, param_2: SPOILER-SPREAD=10, param_3: SKY-SAMPLE=0.3, ! linenum: 49.004 sequence_1: USE sequence_2: POL targname: KP1635+267A sp_element: F277M priority: 2 param_1: SPOILER-ANGLE=340.5, param_2: SPOILER-SPREAD=10, param_3: SKY-SAMPLE=0.3, ! linenum: 49.100 sequence_1: USE sequence_2: POL targname: KP1635+267B sp_element: F277M priority: 2 param_1: SKY-SAMPLE=0.3, ! linenum: 49.101 sequence_1: USE sequence_2: POL targname: KP1635+267B sp_element: F277M priority: 2 param_1: SKY-SAMPLE=0.3, ! linenum: 49.102 sequence_1: USE sequence_2: POL targname: KP1635+267B sp_element: F277M priority: 2 param_1: SKY-SAMPLE=0.3, ! linenum: 49.103 sequence_1: USE sequence_2: POL targname: KP1635+267B sp_element: F277M priority: 2 param_1: SKY-SAMPLE=0.3, ! linenum: 49.104 sequence_1: USE sequence_2: POL targname: KP1635+267B sp_element: F277M priority: 2 param_1: SKY-SAMPLE=0.3, ! linenum: 49.105 sequence_1: USE sequence_2: POL targname: KP1635+267B sp_element: F277M priority: 2 param_1: SKY-SAMPLE=0.3, ! linenum: 49.106 sequence_1: USE sequence_2: POL targname: KP1635+267B sp_element: F277M priority: 2 param_1: SKY-SAMPLE=0.3, ! linenum: 49.107 sequence_1: USE sequence_2: POL targname: KP1635+267B sp_element: F277M priority: 2 param_1: SKY-SAMPLE=0.3, ! linenum: 49.108 sequence_1: USE sequence_2: POL targname: KP1635+267B sp_element: F277M priority: 2 param_1: SKY-SAMPLE=0.3, ! linenum: 49.109 sequence_1: USE sequence_2: POL targname: KP1635+267B sp_element: F277M priority: 2 param_1: SKY-SAMPLE=0.3, ! ! end of exposure logsheet ! No scan data records found