! File: 4283C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:20:16:25 coverpage: title_1: MASS RATIO DETERMINATION FOR DOUBLES WITH SUBSTELLAR MASS MEMBERS title_2: CYCLE 3 - MEDIUM sci_cat: COOL STARS proposal_for: GO/AST longterm: 3 pi_title: DR. pi_fname: LAURENCE pi_mi: G. pi_lname: TAFF pi_inst: STSCI pi_country: USA pi_phone: 410-338-4799 keywords_1: STELLAR MASSES, LOW MASS STARS keywords_2: DOUBLE STARS hours_pri: 10.00 num_pri: 3 fgs: Y pi_position: INSTR SCIENTIST ! end of coverpage abstract: line_1: Stellar masses which lie at or just below the stellar/ line_2: sub-stellar boundary are difficult to determine with certainty. line_3: Only binary stars with low luminosity members provide masses. line_4: In the best studied cases a significant source of line_5: uncertainty in the estimated masses is the blending of line_6: the light on the photographic plates used to record line_7: the stars' positions. The blending must be modelled in line_8: order to determine the locus of the center of mass. The line_9: position of the center of mass determines the mass ratio. line_10: Without knowing this, or the fraction of the total mass of line_11: the pair present in each component of the system, the line_12: uncertainty resulting from blending provides a point of line_13: attack for those who question the reality of ~ 0.05 solar line_14: mass estimates and thus not clearly sub-stellar or "brown line_15: dwarfs". We plan to resolve the pairs, measure orbital line_16: motion for mass ratio and determine individual masses line_17: with the help of orbital parameters which are well determined line_18: from ground-based work. ! ! end of abstract general_form_proposers: lname: TAFF fname: LAURENCE title: DR. mi: G. inst: STSCI country: USA ! lname: HERSHEY fname: JOHN title: DR. mi: L. inst: COMPUTER SCIENCE CORP AT STSCI country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: Several stellar masses which lie at or just below the line_2: stellar/sub- stellar mass boundary (at approximately 0.08 line_3: solar masses) have been determined from orbits of red dwarf line_4: binaries. [Knowledge of masses at the "brown dwarf" boundary line_5: is important in many areas such as stellar evolution, line_6: galactic age and evolution, the tail of the stellar mass line_7: function, the total mass of clusters (and the Galaxy) and line_8: so on (see Stevenson, Ann Rev A & Ap 29, 163, 1991)]. In line_9: each case a significant source of uncertainty in the mass est- line_10: imation is the blending of the light from the double star on line_11: photographic plates. The blending must be modelled in order line_12: to determine the locus of the center of mass in the plate reference line_13: frame. The position of the center of mass determines the mass line_14: ratio, which is the fraction of the total mass of the line_15: pair present in each component of the system. This line_16: uncertainty, resulting from blending induced by atmospheric line_17: seeing, has given an opening to those who would question line_18: whether or not some of these stars with masses determined to line_19: be 0.06 solar masses may, in fact, be as large as 0.08 and line_20: thus not clearly sub-stellar or "brown dwarfs". ! question: 2 section: 2 line_1: Speckle interferometry cannot provide the mass ratio and line_2: individual masses of these close pairs because it cannot line_3: provide the star positions in a reference frame of line_4: background stars. While speckle interferometry, and other line_5: forms of ground-based interferometry used on bright stars line_6: can resolve most of these systems, only position angle and line_7: distance are furnished. The absolute motion of the center of line_8: mass is not fixed because no other (i.e., reference) stars line_9: are observed when performing speckle work. Thus, the HST is line_10: not needed to observe these systems to compute the RELATIVE line_11: orbit; rather the HST is critical for computing the ABSOLUTE line_12: orbit. The HST Fine Guidance Sensors are uniquely capable line_13: of resolving these close, faint stars AND measuring line_14: background stars to provide a reference frame in which to line_15: determine the locus of the center of mass of the pairs. line_16: The HIPPARCOS mission is too short in duration and unlikely to line_17: detect them as doubles. ! question: 2 section: 3 line_1: The measurement of a mass ratio can be done with little HST line_2: Fine Guidance Sensor spacecraft time since it is only line_3: necessary to observe the pair in a few orientations during line_4: their orbits thereby separating the curvilinear orbital line_5: motion from the linear proper motion (and small linear line_6: motions of the reference frame resulting from those stars line_7: own motions and parallaxes; this is essentially a form of line_8: systematic error which is taken out by the self- calibrating line_9: nature of the observations). If the measurements are line_10: performed at the same (or nearly the same parallax factor), line_11: the ground based parallax error in the program star is elimina- line_12: ted and the full HST FGS precision is available for the mass line_13: ratio determination. (To bring the parallax beyond the line_14: ground-based level would require more observing on HST line_15: than requested here and is neither necessary nor needed for line_16: this work.) The time of year for observing is determined by line_17: the spacecraft roll which orients the FGS field of view for line_18: the best reference frame. ! question: 2 section: 4 line_1: To resolve the doubles we would observe them using the line_2: FGS TRANSfer Mode. For the reference stars the FGS line_3: POSitional mode would be used. All of this would be line_4: performed during the same visit (i.e., HST pointing). Any line_5: zero point differential between two modes will drop out in line_6: the series of observations (again this is a form of line_7: systematic error which disappears because of the line_8: self-calibrating nature of these proposed observations). ! question: 2 section: 5 line_1: There are three doubles which have good parallaxes, orbital line_2: coverage, and rather good mass determination at the slightly line_3: sub-stellar level but for which blending is the weakest line_4: link in mass determination (Ianna et al., 1988 AJ 95, 1228) line_5: They are L722-22, Ross 614, and Wolf 424. They would need to line_6: be observed a few times throughout ~ half their orbits. The line_7: FGSs should be able to provide the resolution, line_8: sensitivity AND reference frame unavailable on the line_9: ground to instruments which can resolve the pair, and to line_10: successfully eliminate the questions which have been raised line_11: about the uncertainty of the mass determinations. ! question: 3 section: 1 line_1: Observe the target double star in POS and TRANS mode. Observe line_2: a field of reference stars in POS mode , return to the double line_3: and observe in TRANS and POS mode; all in Fine Lock guidance. ! question: 3 section: 2 line_1: POSitional Mode FGS Observations to establish a reference line_2: reference frame for each scientific target plus the line_3: TRANSfer Mode observations of the scientific targets. Primary line_4: objective is measuring long-term orbital motion. In Cycle 4 line_5: and 5 with full years available, more time contraints for line_6: parallax factors will be introduced. ! question: 4 section: 1 line_1: Speckle interferometry cannot provide the mass ratio and line_2: individual masses of these close pairs because it cannot line_3: provide the star positions in a reference frame of line_4: background stars. While speckle interferometry, and other line_5: forms of ground-based interferometry used on bright stars line_6: can resolve most of these systems, only position angle and line_7: distance are furnished. The absolute motion of the center of line_8: mass is not fixed because no other (i.e., reference) stars line_9: are observed when performing speckle work. Thus, the HST is line_10: not needed to observe these systems to compute the RELATIVE line_11: orbit; rather the HST is critical for computing the ABSOLUTE line_12: orbit. The HST Fine Guidance Sensors are uniquely capable line_13: of resolving these close, faint stars AND measuring line_14: background stars to provide a reference frame in which to line_15: determine the locus of the center of mass of the pairs. line_16: The HIPPARCOS mission is too short and unlikely to detect line_17: them as doubles. ! question: 5 section: 1 line_1: More seasonal time contraints will be brought in after Cycle line_2: 3 when a full year of parallax factors will be available. For line_3: for cycle 3 it is important to get first epoch observations line_4: of the slow orbital motion which is not seasonally dependent. ! question: 7 section: 1 line_1: Data reduction will be performed using software tools line_2: at STScI written by the Instrument Scientist's group. line_3: The investigators will write programs to provide the line_4: parallactic and orbital computations to fit the observed line_5: stellar positions. ! !end of general form text general_form_address: lname: TAFF fname: LAURENCE mi: G. title: DR. category: PI addr_1: STSCI city: BALTIMORE state: MD zip: 21218 country: USA phone: (410)338-4767 ! lname: HERSHEY fname: JOHN mi: L. title: DR. inst: COMPUTER SCIENCE CORP. ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: L722-22 descr_1: A,141 pos_1: RA= 3.8640416D +/-0.00139D, pos_2: DEC=-16.1307D +/-0.00139D equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 1983.80 ra_pm_val: 0.045526 ra_pm_unct: 0.000694 dec_pm_val: -0.5950 dec_pm_unct: 0.0100 an_prlx_val: 0.1890 an_prlx_unct: 0.0050 comment_1: SCIENTIFIC TARGET fluxnum_1: 1 fluxval_1: V=12.62 +/- 0.5 ! targnum: 2 name_1: L722-22-0002-REF descr_1: J,701 pos_1: RA= 3.8676667D +/-0.00139D, pos_2: DEC=-16.1415272D +/-0.00139D equinox: 2000 pm_or_par: N comment_1: CLOSE REF STAR fluxnum_1: 1 fluxval_1: V=14.82 +/- 0.5 ! targnum: 3 name_1: L722-22-0003-REF descr_1: J,701 pos_1: RA= 3.8372500D +/-0.00139D, pos_2: DEC=-16.1202507D +/-0.00139D equinox: 2000 pm_or_par: N comment_1: CLOSE REF STAR fluxnum_1: 1 fluxval_1: V=14.10 +/- 0.5 ! targnum: 4 name_1: L722-22-0004-REF descr_1: J,701 pos_1: RA= 3.8755834D +/-0.00139D, pos_2: DEC=-16.1578331D +/-0.00139D, equinox: 2000 pm_or_par: N comment_1: CLOSE REF STAR fluxnum_1: 1 fluxval_1: V=17.39 +/- 0.5 ! targnum: 5 name_1: L722-22-0005-REF descr_1: J,701 pos_1: RA= 3.8445001D +/-0.00139D, pos_2: DEC=-16.1630001D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=17.18 +/- 0.5 ! targnum: 6 name_1: L722-22-0006-REF descr_1: J,701 pos_1: RA= 3.8183751D +/-0.00139D, pos_2: DEC=-16.1315002D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=16.92 +/- 0.5 ! targnum: 7 name_1: L722-22-0007-REF descr_1: J,701 pos_1: RA= 3.9148333D +/-0.00139D, pos_2: DEC=-16.1189995D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=16.32 +/- 0.5 ! targnum: 8 name_1: L722-22-0008-REF descr_1: J,701 pos_1: RA= 3.9035001D +/-0.00139D, pos_2: DEC=-16.0891666D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=13.38 +/- 0.5 ! targnum: 9 name_1: L722-22-0009-REF descr_1: J,701 pos_1: RA= 3.9003334D +/-0.00139D, pos_2: DEC=-16.0824184D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=16.38 +/- 0.5 ! targnum: 10 name_1: L722-22-0010-REF descr_1: J,701 pos_1: RA= 3.8077500D +/-0.00139D, pos_2: DEC=-16.1048336D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=16.61 +/- 0.5 ! targnum: 11 name_1: L722-22-0011-REF descr_1: J,701 pos_1: RA= 3.9244583D +/-0.00139D, pos_2: DEC=-16.1021671D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=17.04 +/- 0.5 ! targnum: 12 name_1: L722-22-0012-REF descr_1: J,701 pos_1: RA= 3.8366251D +/-0.00139D, pos_2: DEC=-16.1974716D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=16.97 +/- 0.5 ! targnum: 13 name_1: L722-22-0013-REF descr_1: J,701 pos_1: RA= 3.9290416D +/-0.00139D, pos_2: DEC=-16.1772499D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=16.03 +/- 0.5 ! targnum: 14 name_1: L722-22-0014-REF descr_1: J,701 pos_1: RA= 3.9423335D +/-0.00139D, pos_2: DEC=-16.1177216D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=16.25 +/- 0.5 ! targnum: 15 name_1: L722-22-0015-REF descr_1: J,701 pos_1: RA= 3.8855834D +/-0.00139D, pos_2: DEC=-16.0588055D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=14.42 +/- 0.5 ! targnum: 16 name_1: L722-22-0016-REF descr_1: J,701 pos_1: RA= 3.8137918D +/-0.00139D, pos_2: DEC=-16.0721684D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=17.35 +/- 0.5 ! targnum: 17 name_1: L722-22-0017-REF descr_1: J,701 pos_1: RA= 3.8807917D +/-0.00139D, pos_2: DEC=-16.2142239D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=16.76 +/- 0.5 ! targnum: 18 name_1: L722-22-0018-REF descr_1: J,701 pos_1: RA= 3.9070833D +/-0.00139D, pos_2: DEC=-16.2063904D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=16.14 +/- 0.5 ! targnum: 19 name_1: L722-22-0019-REF descr_1: J,701 pos_1: RA= 3.9416666D +/-0.00139D, pos_2: DEC=-16.1818047D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=15.64 +/- 0.5 ! targnum: 20 name_1: L722-22-0020-REF descr_1: J,701 pos_1: RA= 3.9169166D +/-0.00139D, pos_2: DEC=-16.2089443D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=16.59 +/- 0.5 ! targnum: 21 name_1: L722-22-0021-REF descr_1: J,701 pos_1: RA= 3.9404166D +/-0.00139D, pos_2: DEC=-16.0681953D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=16.46 +/- 0.5 ! targnum: 22 name_1: L722-22-0022-REF descr_1: J,701 pos_1: RA= 3.8378334D +/-0.00139D, pos_2: DEC=-16.0369167D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=15.69 +/- 0.5 ! targnum: 23 name_1: L722-22-0023-REF descr_1: J,701 pos_1: RA= 3.8140833D +/-0.00139D, pos_2: DEC=-16.0466385D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=14.02 +/- 0.5 ! targnum: 24 name_1: L722-22-0024-REF descr_1: J,701 pos_1: RA= 3.9720416D +/-0.00139D, pos_2: DEC=-16.1341381D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=16.52 +/- 0.5 ! targnum: 25 name_1: L722-22-0025-REF descr_1: J,701 pos_1: RA= 3.9215417D +/-0.00139D, pos_2: DEC=-16.0458603D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=16.38 +/- 0.5 ! targnum: 26 name_1: L722-22-0026-REF descr_1: J,701 pos_1: RA= 3.8276668D +/-0.00139D, pos_2: DEC=-16.2296124D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=14.61 +/- 0.5 ! targnum: 27 name_1: L722-22-0027-REF descr_1: J,701 pos_1: RA= 3.7597084D +/-0.00139D, pos_2: DEC=-16.1507492D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=16.48 +/- 0.5 ! targnum: 28 name_1: L722-22-0028-REF descr_1: J,701 pos_1: RA= 3.8177083D +/-0.00139D, pos_2: DEC=-16.0374165D +/-0.00139D, equinox: 2000 pm_or_par: N fluxnum_1: 1 fluxval_1: V=16.24 +/- 0.5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22 config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 50S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: DATA-RATE=32 req_1: SEQ 1-7 NON-INT; req_2: GUID TOL 0.007"/1 - 34; req_3: GROUP 1-34 NO GAP; req_4: CYCLE 3 / 1-38; ! linenum: 2.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22 config: FGS opmode: TRANS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 225S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: DATA-RATE=32 param_2: STEP-SIZE=1.0 param_3: SCANS=8 ! linenum: 3.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22 config: FGS opmode: TRANS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 225S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: DATA-RATE=32 param_2: STEP-SIZE=1.0 param_3: SCANS=8 ! linenum: 4.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0002-REF config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 50S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: DATA-RATE=32 ! linenum: 5.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0003-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 6.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0004-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 7.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22 config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 8.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22 config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: DATA-RATE=32 req_1: GROUP-FGS 8-32 WITHIN 20M; req_2: GROUP 8-34 NON-INT; comment_1: PLEASE MAXIMIZE THE GROUP <--> comment_2: WITHIN TIME, WITHOUT DROPPING comment_3: LINES 33 AND 34 AT END ! linenum: 9.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0005-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 10.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0006-REF config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 50S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: DATA-RATE=32 ! linenum: 11.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0007-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 12.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0008-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 13.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0009-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 14.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0010-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 15.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0011-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 16.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0012-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 17.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0013-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 18.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0014-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 19.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0015-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 20.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0016-REF config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 50S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: DATA-RATE=32 ! linenum: 21.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0017-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 22.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0018-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 23.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0019-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 24.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0020-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 25.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0021-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 26.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0022-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 27.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0023-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 28.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0024-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 29.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0025-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 30.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0026-REF config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 50S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: DATA-RATE=32 ! linenum: 31.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0027-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 32.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22-0028-REF config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 33.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22 config: FGS opmode: TRANS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 283S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: DATA-RATE=32 param_2: STEP-SIZE=1.0 param_3: SCANS=10 ! linenum: 34.000 sequence_1: DEFINE sequence_2: LSEQ01 targname: L722-22 config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 50S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: DATA-RATE=32 ! linenum: 35.000 sequence_1: USE LSEQ01 req_1: AT 9-JUL-93 +/- 50D; comment_1: PAR. FAC. ~+0.7 TO 0.4 ! linenum: 36.000 sequence_1: USE LSEQ01 req_1: AT 9-JUL-93 +/- 50D; comment_1: PAR. FAC. ~+0.7 TO 0.4 ! linenum: 37.000 sequence_1: USE LSEQ01 req_1: AT 11-NOV-93 +/- 20D; comment_1: PAR. FAC. ~-.5 TO -.85 ! linenum: 38.000 sequence_1: USE LSEQ01 req_1: AT 11-NOV-93 +/- 20D; comment_1: PAR. FAC. ~-.5 TO -.85 ! ! end of exposure logsheet ! No scan data records found