! File: 2938C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:23:30:37 coverpage: title_1: UNSEEN AND PLANETARY COMPANIONS (BARNARD'S STAR) sci_cat: STELLAR ASTROPHYSICS proposal_for: GTO/AST longterm: 3 cont_id: 1005 pi_title: DR. pi_fname: WILLIAM pi_mi: H. pi_lname: JEFFERYS pi_inst: UNIVERSITY OF TEXAS AT AUSTIN pi_country: USA pi_phone: (512) 471-1455 keywords_1: UNSEEN COMPANIONS, PLANETRAY COMPANIONS, BLACK DWARFS hours_pri: 12.00 num_pri: 1 fgs: Y pi_position: PROFESSOR ! end of coverpage abstract: line_1: With these HST observations we are line_2: initiating a systematic search for variable proper line_3: motion objects trying to discover low mass objects in line_4: orbit around red dwarfs. Using well established astrometric line_5: techniques we will secure relative positional measurements line_6: for selected objects over very long intervals of time looking line_7: for systematic perturbations to rectilinear motion. Within the line_8: Astrometric Data Reduction System (SDAS), such perturbations will line_9: be extracted and reduced further to provide the relevant mass and line_10: orbital parameters of the composents. The HST is an instrument, line_11: the engineering specifications of which, open up the opportunity line_12: to extend this astrometric discipline far beyond the present line_13: bounds of ground-based and other observations. ! ! end of abstract general_form_proposers: lname: JEFFERYS fname: WILLIAM title: DR. mi: H. inst: UNIVERSITY OF TEXAS country: USA ! lname: BENEDICT fname: GEORGE title: DR. mi: F. inst: UNIVERSITY OF TEXAS country: USA ! lname: DUNCOMBE fname: RAYNOR title: DR. mi: L. inst: UNIVERSITY OF TEXAS country: USA ! lname: HEMENWAY fname: PAUL title: DR. mi: D. inst: UNIVERSITY OF TEXAS country: USA ! lname: SHELUS fname: PETER title: DR. mi: S. inst: UNIVERSITY OF TEXAS country: USA ! lname: FRANZ fname: OTTO title: DR. mi: G. inst: LOWELL OBSERVATORY country: USA ! lname: FREDRICK fname: LAURENCE title: DR. mi: W. inst: UNIVERSITY OF VIRGINIA country: USA ! lname: VAN ALTENA fname: WILLIAM title: DR. mi: F. inst: YALE UNIVERSITY country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: Similar to Bessell's study of Sirius and Procyon, which led to the line_2: discovery of previously unseen stellar companions, observatories line_3: having access to long focus astrometric instruments have line_4: established very-long-term systematic searches for variable proper line_5: motion objects as a part of their standard parallax programs. line_6: These efforts have been rewarded by the discovery of objects of line_7: extreme astrophysical interest. The objects which have aroused line_8: the greatest excitement are those of very low mass in orbit around line_9: late spectral type stars. On an ordinary mass-luminosity diagram line_10: many of these objects lie below the lower mass limit presently line_11: hypothesized for actual stellar objects. If such objects are line_12: found in orbit about other stars and yet have masses so small line_13: that they cannot physically be stars, can they be planetary type line_14: objects? With the HST, an instrument having the engineering line_15: specifications that it does, there opens up a magnificent line_16: opportunity to continue a vital astrometric discipline in ways line_17: not previously possible. With the use of the Fine Guidance line_18: Sensors (FGS) we are planning a series of observations to line_19: establish a two-pronged effort for seeking deviations of motion line_20: from that which is rectilinear. ! question: 2 section: 2 line_1: The first of these concerns objects which are at or near the line_2: limits of ground-based techniques; with these we would wish to line_3: firmly confirm or reject the actual existence of perturbations and line_4: allow for a smooth transition between ground- and space-based line_5: observations of this type. The second would be an effort to line_6: search for objects which are now beyond ground-based technologies. line_7: Requested dates of observation fpr Barnard's Star are: line_8: 09/06/93, 09/21/93, 10/06/93, line_9: 03/06/94, 03/21/94, 04/05/94, 06/14/94, 06/29/94, line_10: 09/09/94, 09/21/94, 10/06/94, line_11: 03/06/95, 03/21/95, 04/05/95, 06/14/95, 06/29/95 line_12: 09/09/95, 09/21/95, 10/06/95, ! question: 3 section: 1 line_1: These position mode observations are to be made within line_2: +/- 5 days of the listed dates. Observations are planned line_3: at times of both maximum and minimum parallax factors. line_4: At maximum parallax factor observations will be most sensitive line_5: to parallax; at minimum parallax factor observations will line_6: be most sensitive to proper motion. line_7: Observation sequence: line_8: Acquire guide stars in the FGS units selected got guiding. line_9: Measure target, then referenec stars, then target. line_10: Use FGS unit designated as Astrometry Prime. ! question: 4 section: 1 line_1: Ground-based parallaxes in the very best of circumstances are line_2: limited to 0.002 seconds of arc, which are some 4 times poorer than line_3: that projected for HST observations. Of much more importance is line_4: the fact that this four-fold increase from the best of the line_5: ground-based accuracies will enhance the chances fror detecting line_6: orbital perturbations undetectable from the ground. ! question: 5 section: 1 line_1: All observations must be made within +/- 5 days of listed line_2: dates. ! question: 6 section: 1 line_1: All of the FGS observations shoueld be uninterrupted to line_2: minimize effects of thermal drifts. ! question: 7 section: 1 line_1: Data reduction will be performed using the ADRS within the SDAS line_2: system at STScI with other reductions being performed in Austin. line_3: All data will be put into the ADRS format for analysis using the line_4: GAUSS module. All results, together with best-level estimates of line_5: their errors and their covariances will be made available, as line_6: needed. ! question: 8 section: 1 line_1: N/A ! question: 9 section: 1 line_1: N/A ! question: 10 section: 1 line_1: ADRS will be available in Austin. ! !end of general form text general_form_address: lname: JEFFERYS category: PI ! lname: JEFFERYS fname: WILLIAM mi: H. title: DR. category: PI inst: UNIVERSITY OF TEXAS addr_1: DEPARTMENT OF ASTRONOMY city: AUSTIN state: TX zip: 78712 country: USA phone: (512)471-1455 telex: TEXASTRO ! lname: SHELUS fname: PETER mi: J. title: DR. category: CON inst: UNIVERSITY OF TEXAS addr_1: DEPARTMENT OF ASTRONOMY city: AUSTIN state: TX zip: 78712 country: USA phone: (512)471-3339 ! ! end of general_form_address records fixed_targets: targnum: 29 name_1: BARNARDS-STAR descr_1: HIGHEST PROPER MOTION STAR pos_1: RA = 17H 55M 20.94S +/- 2", pos_2: DEC = +4D 39' 21.40" +/- 2" equinox: 1950.0 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1985.50 ra_pm_val: -0.050000 ra_pm_unct: 0.000667 dec_pm_val: 10.3100 dec_pm_unct: 0.0100 an_prlx_val: 0.5520 an_prlx_unct: 0.0050 fluxnum_1: 1 fluxval_1: V = 9.54 +/- 0.02 ! targnum: 30 name_1: BARNARD-75-REF descr_1: REFERENCE STAR FOR BARNARDS STAR pos_1: RA = 269.436264D +/- 0.0003D, pos_2: DEC = +4.690059D +/- 0.0003D equinox: 2000.0 fluxnum_1: 1 fluxval_1: V = 16.84 +/- 0.6 ! targnum: 31 name_1: BARNARD-76-REF descr_1: REFERENCE STAR FOR BARNARDS STAR pos_1: RA = 269.47687D +/- 0.0003D, pos_2: DEC = +4.680570D +/- 0.0003D equinox: 2000.0 fluxnum_1: 1 fluxval_1: V = 13.26 +/- 0.6 ! targnum: 32 name_1: BARNARD-77-REF descr_1: REFERENCE STAR FOR BARNARDS STAR pos_1: RA = 269.478272D +/- 0.0003D, pos_2: DEC = +4.677535D +/- 0.0003D equinox: 2000.0 fluxnum_1: 1 fluxval_1: V = 16.84 +/- 0.6 ! targnum: 33 name_1: BARNARD-81-REF descr_1: REFERENCE STAR FOR BARNARDS STAR pos_1: RA = 269.437087D +/- 0.0003D, pos_2: DEC = +4.679343D +/- 0.0003D equinox: 2000.0 fluxnum_1: 1 fluxval_1: V = 15.5 +/- 0.6 ! targnum: 34 name_1: BARNARD-90-REF descr_1: REFERENCE STAR FOR BARNARDS STAR pos_1: RA = 269.42924D +/- 0.0003D, pos_2: DEC = +4.666314D +/- 0.0003D equinox: 2000.0 fluxnum_1: 1 fluxval_1: V = 15.5 +/- 0.6 ! targnum: 35 name_1: BARNARD-91-REF descr_1: REFERENCE STAR FOR BARNARDS STAR pos_1: RA = 269.456590D +/- 0.0003D, pos_2: DEC = +4.706910D +/- 0.0003D equinox: 2000.0 fluxnum_1: 1 fluxval_1: V = 14.52 +/- 0.6 ! targnum: 36 name_1: BARNARD-93-REF descr_1: REFERENCE STAR FOR BARNARDS STAR pos_1: RA = 269.457916D +/- 0.0003D, pos_2: DEC = +4.674444D +/- 0.0003D equinox: 2000.0 fluxnum_1: 1 fluxval_1: V = 16.54 +/- 0.6 ! targnum: 37 name_1: BARNARD-94-REF descr_1: REFERENCE STAR FOR BARNARDS STAR pos_1: RA = 269.466480D +/- 0.0003D, pos_2: DEC = +4.705630D +/- 0.0003D equinox: 2000.0 fluxnum_1: 1 fluxval_1: V = 11.18 +/- 0.6 ! targnum: 38 name_1: BARNARD-110-REF descr_1: REFERENCE STAR FOR BARNARDS STAR pos_1: RA = 269.427218D +/- 0.0003D, pos_2: DEC = +4.646727D +/- 0.0003D equinox: 2000.0 fluxnum_1: 1 fluxval_1: V = 15.64 +/- 0.6 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 20.000 sequence_1: DEFINE sequence_2: SEQ21 targname: BARNARDS-STAR config: FGS opmode: POS aperture: PRIME sp_element: F583W num_exp: 1 time_per_exp: 52S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: DATA-RATE=32 req_1: SEQ 20-22 NON-INT; req_2: GUID TOL 0.007"; req_3: GROUP-FGS 20-22 WITHIN 30M; comment_1: AVOID TERMINATOR CROSSING comment_2: IF THE VISIBILITY PERIOD IS LESS THAN comment_3: 30M, PLEASE CONTACT PETE SHELUS. IF comment_4: IT IS MORE THAN 30M, THEN GROUP-FGS comment_5: CAN BE TAILORED TO FIT. ! linenum: 21.000 sequence_1: DEFINE sequence_2: SEQ21 targname: BARNARD-75-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ req_1: DO FOR TARG 30-38; comment_1: OBSERVE ONLY THOSE REFERENCE STARS comment_2: WITHIN THE ASTROMETRY PICKLE ! linenum: 22.000 sequence_1: DEFINE sequence_2: SEQ21 targname: BARNARDS-STAR config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 23.000 sequence_1: USE SEQ21 req_1: AT 06-SEP-93 +/- 5D; req_2: REPEAT 23 EVERY 15D +/- 1D FOR 2 MORE req_3: TIMES; req_4: CYCLE 3; comment_1: MAXIMUM NEGATIVE PARALLAX FACTOR ! linenum: 24.000 sequence_1: USE SEQ21 req_1: AT 06-MAR-94 +/- 5D; req_2: REPEAT 24 EVERY 15D +/- 1D FOR 2 MORE req_3: TIMES; req_4: CYCLE 3; comment_1: MAXIMUM POSITIVE PARALLAX FACTOR ! linenum: 25.000 sequence_1: USE SEQ21 req_1: AT 14-JUN-94 +/- 5D; req_2: REPEAT 25 EVERY 15D +/- 1D FOR 1 MORE req_3: TIMES; req_4: CYCLE 3; comment_1: ZERO PARALLAX FACTOR ! linenum: 26.000 sequence_1: USE SEQ21 req_1: AT 06-SEP-94 +/- 5D; req_2: REPEAT 26 EVERY 15D +/- 1D FOR 2 MORE req_3: TIMES; req_4: CYCLE 3; comment_1: MAXIMUM NEGATIVE PARALLAX FACTOR ! linenum: 27.000 sequence_1: USE SEQ21 req_1: AT 06-MAR-95 +/- 5D; req_2: REPEAT 27 EVERY 15D +/- 1D FOR 2 MORE req_3: TIMES; req_4: CYCLE 3; comment_1: MAXIMUM POSITIVE PARALLAX FACTOR ! linenum: 28.000 sequence_1: USE SEQ21 req_1: AT 14-JUN-95 +/- 5D; req_2: REPEAT 28 EVERY 15D +/- 1D FOR 1 MORE req_3: TIMES; req_4: CYCLE 3; comment_1: ZERO PARALLAX FACTOR ! linenum: 29.000 sequence_1: USE SEQ21 req_1: AT 06-SEP-95 +/- 5D; req_2: REPEAT 29 EVERY 15D +/- 1D FOR 2 MORE req_3: TIMES; req_4: CYCLE 3; comment_1: MAXIMUM NEGATIVE PARALLAX FACTOR ! ! end of exposure logsheet ! No scan data records found