! File: 2862C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:19:05:12 coverpage: title_1: LINKING HIPPARCOS TO THE EXTRAGALACTIC REFERENCE FRAME title_2: PART 5 OF 6, NEWC, CYCLE 2,CONTINUATION OF 2565-HIGH sci_cat: COOL STARS sci_subcat: ASTROMETRY proposal_for: GO cont_id: 2565 pi_title: DR pi_fname: PAUL pi_mi: D pi_lname: HEMENWAY pi_inst: UNIVERSITY OF TEXAS AT AUSTIN pi_country: USA pi_phone: (512)471-3431 keywords_1: REFERENCE FRAMES, HIPPARCOS, QUASARS hours_pri: 80.00 num_pri: 175 fgs: Y funds_amount: 292590 funds_length: 36 pi_position: RSSCI ! end of coverpage abstract: line_1: Determination of a non-rotating Reference Frame is crucial line_2: to progress in many areas, including: Galactic motions, line_3: local (Oort's A and B) and global (R0) parameters derived line_4: from them, solar system motion discrepancies (Planet X); line_5: and in conjunction with the VLBI radio reference frame, line_6: the registration of radio and optical images at an accuracy line_7: well below the resolution limit of HST images (0.06 arcsec). line_8: The goal of the Program is to tie the HIPPARCOS and Extra- line_9: galactic Reference Frames together at the 0.0005 arcsec and line_10: 0.0005 arcsec/year level. The HST data will allow a deter- line_11: mination of the brightness distribution in the stellar and line_12: extragalactic objects observed and time dependent changes line_13: therein at the 0.001 arcsec/year level. line_14: The Program requires targets distributed over the whole sky line_15: to define a rigid Reference Frame. GTO observations will line_16: provide initial first epoch data and preliminary proper motions. line_17: The observations will consist of relative positions of Extra- line_18: galactic objects (EGOs) and HIPPARCOS stars, measured with the line_19: FGSs. ! ! end of abstract general_form_proposers: lname: HEMENWAY fname: PAUL title: DR mi: D inst: UNIVERSITY OF TEXAS AT AUSTIN country: USA ! lname: ARGUE fname: NOEL title: DR inst: THE OBSERVATORIES country: ENGLAND ! lname: DUNCOMBE fname: RAYNOR title: DR mi: L inst: UNIVERSITY OF TEXAS AT AUSTIN country: USA ! lname: HUGHES fname: JAMES title: DR inst: U.S. NAVAL OBSERVATORY country: USA ! lname: JAUNCEY fname: DAVID title: DR inst: C.S.I.R.O. country: AUSTRALIA ! lname: JOHNSTON fname: KENNETH title: DR inst: U.S. NAVAL RESEARCH LAB country: USA ! lname: KOVALEVSKY fname: JEAN title: DR inst: C.E.R.G.A. country: FRANCE ! lname: LESTRADE fname: JEAN title: DR inst: BUREAU DE LONGITUDE country: FRANCE ! lname: PERRYMAN fname: MICHAEL title: DR inst: E.S.T.E.C. country: HOLLAND ! lname: PRESTON fname: ROBERT title: DR inst: JET PROPULSION LAB country: USA ! lname: TURON fname: CATHERINE title: DR inst: OBSERVATOIRE DE MEUDON country: FRANCE ! lname: DEVEGT fname: CHRISTIAN title: DR inst: HAMBURGER STERNWARTE country: FGR ! lname: WALTER fname: HANS title: DR inst: ANSTRONOMISCHE RECHENINSTITUT country: FGR ! lname: WHITE fname: GRAEME title: DR inst: C.S.I.R.O. country: AUSTRALIA ! lname: KRISTIAN fname: JEROME title: DR inst: CALTECH country: USA ! lname: TAPLEY fname: BYRON title: PROF. inst: UNIV OF TEXAS AT AUSTIN country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: The astronomical uses of an accurate coordinate reference frame line_2: are manifest. The reference frame provides the kinematic basis line_3: for all dynamical studies of celestial objects. The HIPPARCOS line_4: satellite will determine positions, proper motions, and line_5: parallaxes for about 100000 stars evenly distributed over the line_6: sky (Kovalevsky, _Space Science Rev._, 39,41,1984). A residual line_7: time dependent rotation of the reference frame would introduce line_8: a systematic effect in the system of proper motions that biases line_9: all the astronomical uses that can be made of the system in line_10: kinematical and dynamical studies of the Galaxy. (Galactic line_11: differential rotation and its variation with distance, asymmetry line_12: of motions with respect to the galactic plane, kinematics of line_13: halo stars and other stellar populations, group motions, and line_14: determining the birth places of stars, are a few examples of line_15: galactic studies which are adversely affected by a residual line_16: rotation of the reference frame.) This proposal is to reduce line_17: this undesirable bias by determining the rotation of the line_18: HIPPARCOS frame with respect to extragalactic objects. The line_19: method is to measure the proper motion of some stars in the line_20: HIPPARCOS system with respect to extragalactic objects (EGOs) line_21: using the Hubble Space Telescope (HST). ! question: 2 section: 2 line_1: HST can provide the information needed to link the HIPPARCOS line_2: proper motion system to the fixed reference system defined by line_3: the EGOs. The object of the overall program is to obtain the line_4: observations necessary to determine this link to an accuracy line_5: of the order of the systematic regional errors that may exist line_6: in the final HIPPARCOS catalogue. line_8: The nominal HIPPARCOS accuracy for stars brighter than 10.5 is line_9: expected to be 0.002 arcsec in position and parallax, and 0.002 line_10: arcsec/year in proper motion. HIPPARCOS will observe objects line_11: between 10.5 and 12 magnitude with reduced accuracy. The basic line_12: HIPPARCOS data will be accurate large angle separations of stars line_13: (chords on the celestial sphere). The system solution will line_14: yield a "solid body" celestial coordinate system an order of line_15: magnitude more accurate systematically than the individual line_16: random errors of the individual stars. Caused by unknown line_17: systematic biases of instrumental origin, they have not been line_18: properly assessed, but they should not exceed 0.1 milliarcsec line_19: in position, or 0.1 milliarcsec/year in proper motion. ! question: 2 section: 3 line_1: However, the nature of the HIPPARCOS reference system is such line_2: that it has a double indeterminacy: an arbitrary "solid body" line_3: rotation proportional to time in its proper motion system, line_4: and an arbitrary solid body rotational offset from any line_5: "standard" (e.g. inertial or quasi-inertial) coordinate line_6: system, in position. line_8: R. L. Duncombe and P. D. Hemenway plan to use about 40 hours line_9: of GTO time to observe HIPPARCOS stars near extragalactic line_10: objects. The stars have been screened from about 300 stars line_11: by a large program of speckle interferometry specifically for line_12: this purpose. (C.f. Hemenway, et al., 1985 ESA special line_13: Publication SP-234, p.281; Argue, et al., _Mon. Not. RAS_, line_14: 206,669, and 216,447.) Drs. Franz and McAlister have done line_15: the northern hemisphere speckle observations (private line_16: communcation to PDH). ! question: 2 section: 4 line_1: Simulations by Froeschle and Kovalevsky (_Astron. Astrophys._, line_2: 116, 89, 1982) show that for observations evenly distribued line_3: over the sky, the elements of the rotation matrix would be line_4: obtained with an accuracy of 0.003 arcsec/year rms for 40 line_5: pairs and 0.0023 arcsec/year for 70 pairs. We have identified line_6: 175 stars around 91 EGOs that are observable astrometrically line_7: with HST. This distribution should allow the determination of line_8: the rotation matrix to an accuracy of the order of 0.0016 line_9: arcsec/year. However, these figures represent measurements line_10: over the lifetime of the HIPPARCOS mission, 2.5 years and the line_11: subsequent accuracy for the tie to EGOs at the end of the line_12: mission. A longer time base will reduce the error propor- line_13: tionally to the time base for the next several years after the line_14: HIPPARCOS mission is completed. The determination of the line_15: components of the rotation matrices depends critically on line_16: the distribution being uniform over the sphere. A loss of the line_17: sources south of -30 degrees declination increases the rms of line_18: the solution by a factor of 1.4, for example. Therefore, the line_19: first priority is to make sure that the EGOs that are observed line_20: are well distributed over the celestial sphere. ! question: 2 section: 5 line_1: Although this result is very accurate, it does not reach the line_2: expected accuracy of the HIPPARCOS system by a factor of 2 line_3: or 3. By reobserving all the HIPPARCOS star-EGO pairs over line_4: the course of the HST lifetime, the error of the individual line_5: motions is reduced proportionally to the time, and the overall line_6: solution should reach the 0.0008 arcsec/year level. If, in line_7: addition, about 15 radio stars are observed by VLBI giving a line_8: precision of proper motion of about 0.002 arcsec/year, then line_9: the expected global accuracy will become: line_10: a) 0.0025 arcsec/year if this proposal is not accepted, line_11: b) 0.0016 arcsec/yr if the GTO plus this proposal is accepted, line_12: c) 0.0012 arcsec/year if the full combined list is observed, and line_13: d) 0.0005 arcsec/yr if all observations of all types over the line_14: HST lifetime are observed. line_16: Some points which need stressing: line_17: a) Two HST time scales are important, one common to the line_18: HIPPARCOS epoch should start AS SOON AS POSSIBLE AFTER LAUNCH line_19: to reach the full potential of the tie between the VLBI frame line_20: and the HIPPARCOS frame, which requires observations of the line_21: same objects at the same epochs. The early epoch observations line_22: will also give the longest time base for the proper motion line_23: determinations, ! question: 2 section: 6 line_1: b) HIPPARCOS can only observe down to 12th magnitude with line_2: reduced accuracy. It cannot observe the Exragalactic objects line_3: directly, line_5: c) The program and object selection have been the subjects of line_6: intensive efforts by many people over the last few years, line_7: including the Working Group on Radio/Optical Identifications line_8: of IAU Commission 24, Subgroup 2130 of the HIPPARCOS Input line_9: Catalogue Consortium, a working group of one of the HIPPARCOS line_10: reduction consortia (F.A.S.T.), the speckle observers headed line_11: by Franz and McAlister in the north and Argue and Morgan in line_12: the south, and the southern hemisphere radio observers headed line_13: by Jauncey and White, who have identified the southern sources line_14: in this proposal through a major effort in the last two years, line_16: d) Jauncey, White, and Preston are working to make all the line_17: radio sources in this proposal part of the VLBI reference line_18: frame, including establishing the Australian VLBI capability, ! question: 2 section: 7 line_1: e) A set of 414 candidate stars near EGOs was included in the line_2: HIPPARCOS Input Catalogue in 1982 to make sure that the stars line_3: would be observed by HIPPARCOS. The speckle programs comprised line_4: these stars and the stars near the southern EGOs subsequently line_5: indentified by Jauncey and White. line_7: The objectives of this program are: line_8: 1) Provide an accurate tie of the HIPPARCOS Coordinate line_9: Reference System (positions and proper motions) to the best line_10: available extragalactic (e.g. VLBI) system, at the epoch of line_11: HIPPARCOS, line_13: 2) Tie the HIPPARCOS Reference System of proper motions to a line_14: (non-rotating) extragalactic system of optical objects, line_16: 3) Thereby establishing the connection between the Radio and line_17: Optical reference frames to the millarcsecond level (allowing line_18: the registration of HST images to radio images (VLA, VLBI, line_19: VLBA) to an accuracy well below the reolution limit of HST), line_20: anywhere in the sky, ! question: 2 section: 8 line_1: 4) Obtain single-epoch information on the brightness distri- line_2: bution of EGOs and stars, and line_4: 5) Obtain time dependent studies of the resolved and unresolved line_5: structure of (4) at the 0.001 arcsec/year level of accuracy. line_7: We have a brief statement from the HIPPARCOS Science Team line_8: supporting the importance of this work to the HIPPARCOS project, line_9: and its usefulness for both HIPPARCOS and HST astrometric data. line_10: The stement is included as an appendix to the proposal. ! question: 2 section: 9 line_1: APPENDIX: line_2: The following statement was communicated at the end of line_3: December, 1985: line_5: The eleven members of the HIPPARCOS Science Team, the scientific line_6: representatives who advise ESA directly on the scientific line_7: conduct, planning and organisation of the HIPPARCOS project, line_8: have expressed their full support for this collaborative line_9: programme. For the reasons set out in the proposal, the line_10: HIPPARCOS Science Team has confirmed the importance of the line_11: propsed observations for the interpretation and exploitation line_12: of both HIPPARCOS and Space Telescope astrometric data. line_14: Professor Adrian Blaauw, chairman of the ESA HIPPARCOS proposal line_15: selection committee; and Professor Walter Fricke*, chairman of line_16: the HIPPARCOS Input Catalogue Consortium steering committee, line_17: have also given their support to the present proposal. line_19: *Deceased 28 March 1988. ! question: 3 section: 1 line_1: The basic datum required is the relative separation line_2: angle of an EGO and a HIPPARCOS star. One would hope to rely on line_3: the knowledge of the FGS calibrations to simply measure one line_4: object and then the other. However, because of thermal and line_5: mechanical instabilities during "exposures", initially we will line_6: follow the GTO observing strategy of measuring two objects line_7: several times with some intermediate background stars as a line_8: stability check. Should the FGS measurements prove to be as line_9: stable as expected, then the number of check stars and the line_10: frequency of measurement may be reduced by a large factor (up line_11: to about 5). Since a single measurement of a single pair is line_12: expected to average about 20 minutes, overall slewing time is line_13: expected to be a major factor in actual time consumption. line_14: Based on OV/SV/GTO observations, we will learn how to optimize line_15: the use of HST for the objectives of this program. ! question: 3 section: 2 line_1: For EGOs brighter than 17.0, the observations will consist of line_2: obtaining FGS reading on: 1) the EGO, 2) the HIPPARCOS star, line_3: and 3-5) 3 background stars (when available) in the pickle. line_4: The following sequence will be observed: 1,3-5,2,1,2,5-3,1. line_5: When a star is brighter than V=9.0, the neutral density filter line_6: will be inserted. Whenever possible, another HIPPARCOS star line_7: will be included as one of the "background" stars. ! question: 4 section: 1 line_1: Simulations have shown that the expected regional systematic line_2: effects within the HIPPARCOS catalogue should be ~0.0001 arcsec. line_3: The expected individual HIPPARCOS position and motion errors line_4: are expected to be 0.002 arcsec and 0.002 arcsec/year. In line_5: tying the HIPPARCOS Reference Frame to EGOs, the error of the line_6: frame will depend on the errors of observations of the line_7: individual objects used. Two methods of high accuracy line_8: observations have been proposed. First is the VLBI observation line_9: of radio stars in HIPPARCOS directly with respect to EGOs. line_10: VLBI sensitivity limits the stars to a few RS CVn stars, with line_11: an accuracy of 0.002 arcsec. Some of these stars show radio- line_12: optical offsets at the 0.002 arcsec level. ! question: 4 section: 2 line_1: The second method is the one proposed here. The FGS measure- line_2: ments have an accuracy commensurate with both HIPPARCOS and line_3: radio measurements, again 0.002 arcsec. Other proposed line_4: methods rely on photographic astrometry of thousands of stars, line_5: galaxies, and QSOs, with measuring accuracies in the 0.1 to line_6: 0.01 arcsec range. These methods suffer from large systematic line_7: effects. No information about the optical structure of the line_8: EGOs or the stars can be obtained at teh 0.04 to 0.002 arcsec line_9: level. Such information is obtained as a matter of course line_10: during HST observations. line_12: The proposed HST observations are the only optical means which line_13: can approach the expected accuracy of the individual HIPPARCOS line_14: star measurements, and these observations are REQUIRED, to line_15: achieve a reduction to a non-rotating coordinate frame at the line_16: level of the internal systematic accuracy of HIPPARCOS. ! question: 5 section: 1 line_1: The FGS observations are expected to take 51.2 sec/setting= line_2: (1/40 sec/sample)*(32 samples/integration)*(2^6 integrations/ line_3: setting) seconds/setting for the 11 settings/"observation" line_4: described in (3) above, due to the need to average over the line_5: "thermal hunt" cycle of the FGSs. The overhead per observation line_6: is expected to be twice the "time on target". Thus we have line_7: allotted 20 minutes for a single "average" observation with the line_8: FGSs. ! question: 5 section: 2 line_1: At an average of 3 single epoch observations/hour of HST time, line_2: with 40 hours allotted of GTO time and 8 hours GO time/year line_3: for 10 years, one arrives at 360 single-epoch observations to line_4: cover the 165 pairs. We expect to obtain 160 single epoch line_5: separations, 120 one-year proper motions, and a distribution line_6: of 2-5 year proper motions. Operational experience in the first line_7: year should substantially increase the efficiency of the line_8: observational procedures, so we should increase the number of line_9: observations we can obtain during the program, for the same line_10: number of requested hours. The program proposed here is the line_11: minimum acceptable program to reach an acceptable accuracy line_12: in the Extragalactic Link. The ideal goal is to obtain 10 line_13: year positions and proper motions for all 165 pairs, yielding line_14: a system solution in the submilliarcsecond range. The 20 line_15: hours for the first GO year will provide 30 single epochs. ! question: 6 section: 1 line_1: Because of power constraints, off-nominal roll will be available line_2: only under restricted conditions. Therefore, in order to line_3: maintain the maximum scheduling flexibility, the time of year line_4: has been selected to make the orientation of the astrometer line_5: FGS line_6: conform to the position angle of the EGO-HIPPARCOS star pair line_7: for the nominal roll on that date. In order to remove the line_8: effect of the HIPPARCOS star parallax in the determination of line_9: the proper motion, the observations of a given HIPPARCOS star line_10: EGO pair must be made at intervals of one year exactly, within line_11: a few days. line_14: Each observation consists of separate settings of the FGSs. line_15: The thermal/mechanical stability line_16: of the OTA/FGS is expected to hold only over about 10 minutes. line_17: We have included check star measurements in the observation line_18: plan. However, each entire observation sequence must be line_19: performed contiguously to allow accurate determination of the line_20: target relative positions. ! question: 8 section: 1 line_1: AT THE TIME OF THIS SUBMISSION, THE RESOURCE ESTIMATOR IS line_2: OVERESTIMATING THE FGS OVERHEAD. WE HAVE BEEN TOLD TO line_3: USE THE RESOURCE ESTIMATOR NUMBER, BUT THAT THE ACTUAL TIME line_4: CHARGED WILL BE REDUCED TO REFLECT A BETTER ESTIMATE OF THE line_5: TRUE OVERHEAD WHEN IT BECOMES AVAILABLE. The RESOURCE line_6: ESTIMATOR is currently giving 4.2 min between each FGS line_7: setting, while it takes less than a minute in reality. line_8: (1/26/93--PDH). ! question: 8 section: 2 line_1: This proposal is inteded to extend observations of the GTO line_2: sources over a longer time base to improve the accuracy of line_3: the proper motions and obtain more temporal structure data. line_4: The distribution of labor will be as follows: line_6: Cycle 1: Identification of Reference Stars - Hemenway line_7: Measurement of Positions of Targets, Reference Stars line_8: - Hemenway, UT Staff line_9: - Argue line_10: - Jauncey and White line_11: - deVegt line_13: Observations: Obtain HST data - All line_14: (Some at STScI, some at ECF) line_16: Reduction: Reduce HST data to positional differences and line_17: brightness distribution - All line_19: Incorporation of Stars in HIPPARCOS - Turon ! question: 8 section: 3 line_1: Reduction of HIPPARCOS Coordinates to Radio Frame line_2: - Kovalevsky line_3: - Preston line_4: - Lestrade line_5: - Johnston line_7: Reduction of HIPPARCOS Proper Motion System to EGO System line_8: - Johnston line_9: - Jauncey line_10: - deVegt line_11: - Preston line_12: - Hemenway line_13: - Perryman ! !end of general form text general_form_address: lname: HEMENWAY fname: PAUL mi: D title: DR. category: PI inst: UNIVERSITY OF TEXAS AT AUSTIN addr_1: DEPARTMENT OF ASTRONOMY addr_2: UNIVERSITY OF TEXAS AT AUSTIN city: AUSTIN state: TX zip: 78712 country: USA phone: (512)471-3431 ! ! end of general_form_address records fixed_targets: targnum: 221 name_1: NEWEGOC-45NEWHIP-45 descr_1: E pos_1: RA = 166.11375D +/- .0008D, pos_2: DEC = 38.2086111D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=13.5 +/- 1 ! targnum: 222 name_1: NEWHIP-45-REF descr_1: A pos_1: RA = 166.130375D +/- .0008D, pos_2: DEC = 38.2413611D +/- .0008D, equinox: 2000 pm_or_par: Y ra_pm_val: -0.005432 dec_pm_val: -0.0030 fluxnum_1: 1 fluxval_1: V=6.04 +/- 1 ! targnum: 223 name_1: 220-REF descr_1: J,701 pos_1: RA = 166.21337D +/- .0008D, pos_2: DEC = 38.28591D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=14.54 +/- 1 ! targnum: 224 name_1: 221-REF descr_1: J,701 pos_1: RA = 166.15892D +/- .0008D, pos_2: DEC = 38.26493D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=15.26 +/- 1 ! targnum: 225 name_1: 222-REF descr_1: J,701 pos_1: RA = 166.18343D +/- .0008D, pos_2: DEC = 38.24675D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=7.1 +/- 1 ! targnum: 421 name_1: NEWEGOC-47NEWHIP-47 descr_1: E pos_1: RA = 166.11375D +/- .0008D, pos_2: DEC = 38.2086111D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=13.5 +/- 1 ! targnum: 422 name_1: NEWHIP-47-REF descr_1: A pos_1: RA = 166.384083D +/- .0008D, pos_2: DEC = 38.2758333D +/- .0008D, equinox: 2000 pm_or_par: Y ra_pm_val: -0.027005 dec_pm_val: 0.0520 fluxnum_1: 1 fluxval_1: V=8.79 +/- 1 ! targnum: 423 name_1: 420-REF descr_1: J,701 pos_1: RA = 166.38806D +/- .0008D, pos_2: DEC = 38.29825D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=12.89 +/- 1 ! targnum: 424 name_1: 421-REF descr_1: J,701 pos_1: RA = 166.21337D +/- .0008D, pos_2: DEC = 38.28591D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=14.54 +/- 1 ! targnum: 425 name_1: 422-REF descr_1: J,701 pos_1: RA = 166.18343D +/- .0008D, pos_2: DEC = 38.24675D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=7.1 +/- 1 ! targnum: 521 name_1: NEWEGOC-48NEWHIP-48 descr_1: E pos_1: RA = 166.11375D +/- .0008D, pos_2: DEC = 38.2086111D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=13.5 +/- 1 ! targnum: 522 name_1: NEWHIP-48-REF descr_1: A pos_1: RA = 166.183083D +/- .0008D, pos_2: DEC = 38.2466389D +/- .0008D, equinox: 2000 pm_or_par: Y ra_pm_val: -0.005772 dec_pm_val: -0.0120 fluxnum_1: 1 fluxval_1: V=7.55 +/- 1 ! targnum: 523 name_1: 520-REF descr_1: J,701 pos_1: RA = 166.17921D +/- .0008D, pos_2: DEC = 38.22103D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=15.31 +/- 1 ! targnum: 524 name_1: 521-REF descr_1: J,701 pos_1: RA = 166.21337D +/- .0008D, pos_2: DEC = 38.28591D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=14.54 +/- 1 ! targnum: 525 name_1: 522-REF descr_1: J,701 pos_1: RA = 166.15892D +/- .0008D, pos_2: DEC = 38.26493D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=15.26 +/- 1 ! targnum: 621 name_1: NEWEGOC-50NEWHIP-50 descr_1: E pos_1: RA = 229.4242236D +/- .0008D, pos_2: DEC = -24.37207592D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=15 +/- 1 ! targnum: 622 name_1: NEWHIP-50-REF descr_1: A pos_1: RA = 229.438125D +/- .0008D, pos_2: DEC = -24.428639D +/- .0008D, equinox: 2000 pm_or_par: Y ra_pm_val: -0.003588 dec_pm_val: -0.0580 fluxnum_1: 1 fluxval_1: V=9.08 +/- 1 ! targnum: 623 name_1: 620-REF descr_1: J,701 pos_1: RA = 229.49139D +/- .0008D, pos_2: DEC = -24.45816D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=12.92 +/- 1 ! targnum: 624 name_1: 621-REF descr_1: J,701 pos_1: RA = 229.45978D +/- .0008D, pos_2: DEC = -24.38389D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=13.76 +/- 1 ! targnum: 625 name_1: 622-REF descr_1: J,701 pos_1: RA = 229.46983D +/- .0008D, pos_2: DEC = -24.42986D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=13.53 +/- 1 ! targnum: 721 name_1: NEWEGOC-52NEWHIP-52 descr_1: E pos_1: RA = 253.4675693D +/- .0008D, pos_2: DEC = 39.76016882D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=13.8 +/- 1 ! targnum: 722 name_1: NEWHIP-52-REF descr_1: A pos_1: RA = 253.247458D +/- .0008D, pos_2: DEC = 39.6055278D +/- .0008D, equinox: 2000 pm_or_par: Y ra_pm_val: -0.007442 dec_pm_val: -0.0220 fluxnum_1: 1 fluxval_1: V=9.89 +/- 1 ! targnum: 723 name_1: 720-REF descr_1: J,701 pos_1: RA = 253.32033D +/- .0008D, pos_2: DEC = 39.70772D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=13.53 +/- 1 ! targnum: 724 name_1: 721-REF descr_1: J,701 pos_1: RA = 253.44106D +/- .0008D, pos_2: DEC = 39.7359D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=12.43 +/- 1 ! targnum: 725 name_1: 722-REF descr_1: J,701 pos_1: RA = 253.28449D +/- .0008D, pos_2: DEC = 39.63098D +/- .0008D, equinox: 2000 fluxnum_1: 1 fluxval_1: V=14.08 +/- 1 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 22.001 targname: NEWEGOC-45NEWHIP-45 config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 51.2S fluxnum_1: 1 priority: 1 param_1: DATA-RATE = 32 req_2: SEQ 22.001-22.011 NO GAP; req_3: SAME POS FOR 22.002-22.011 AS 22.001; req_4: CYCLE 2 / 22.001-22.011; req_5: COND IF POS MODE ASTROMETRY OPERATIONAL req_6: / 22.001-72.011; req_7: ORIENT 233.49D +/- .3D; req_8: POS TARG +127.1,-67.074; comment_1: NEAR JD2449024.48 V1 AXIS AND comment_2: ORIENTATION SPECIFIED TO PUT comment_3: REFERENCE STARS IN PICKLE. JDTOBS IS comment_4: THE JULIAN DATE THAT THIS ORIENTATION comment_5: IS AT NOMINAL ROLL. 180D OPTION IS NOT ! linenum: 22.002 targname: 220-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 22.003 targname: 221-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 22.004 targname: 222-REF config: ^ opmode: ^ aperture: ^ sp_element: F5ND num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 22.005 targname: NEWHIP-45-REF config: ^ opmode: ^ aperture: ^ sp_element: F5ND num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 22.006 targname: NEWEGOC-45NEWHIP-45 config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 22.007 targname: NEWHIP-45-REF config: FGS opmode: POS aperture: 3 sp_element: F5ND num_exp: 1 time_per_exp: 51.2S fluxnum_1: 1 priority: 1 param_1: DATA-RATE = 32 ! linenum: 22.008 targname: 222-REF config: ^ opmode: ^ aperture: ^ sp_element: F5ND num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 22.009 targname: 221-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 22.010 targname: 220-REF config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 51.2S fluxnum_1: 1 priority: 1 param_1: DATA-RATE = 32 ! linenum: 22.011 targname: NEWEGOC-45NEWHIP-45 config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 42.001 targname: NEWEGOC-47NEWHIP-47 config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 51.2S fluxnum_1: 1 priority: 1 param_1: DATA-RATE = 32 req_2: SEQ 42.001-42.011 NO GAP; req_3: SAME POS FOR 42.002-42.011 AS 42.001; req_4: CYCLE 2 / 42.001-42.011; req_5: ORIENT 253.73D +/- .3D; req_6: POS TARG +425.641,-132.683; comment_1: NEAR JD2449010.74 V1 AXIS AND comment_2: ORIENTATION SPECIFIED TO PUT comment_3: REFERENCE STARS IN PICKLE. JDTOBS IS comment_4: THE JULIAN DATE THAT THIS ORIENTATION comment_5: IS AT NOMINAL ROLL. 180D OPTION IS NOT ! linenum: 42.002 targname: 420-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 42.003 targname: 421-REF config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 51.2S fluxnum_1: 1 priority: 1 param_1: DATA-RATE = 32 ! linenum: 42.004 targname: 422-REF config: ^ opmode: ^ aperture: ^ sp_element: F5ND num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 42.005 targname: NEWHIP-47-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 42.006 targname: NEWEGOC-47NEWHIP-47 config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 42.007 targname: NEWHIP-47-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 42.008 targname: 422-REF config: ^ opmode: ^ aperture: ^ sp_element: F5ND num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 42.009 targname: 421-REF config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 51.2S fluxnum_1: 1 priority: 1 param_1: DATA-RATE = 32 ! linenum: 42.010 targname: 420-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 42.011 targname: NEWEGOC-47NEWHIP-47 config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 52.001 targname: NEWEGOC-48NEWHIP-48 config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 51.2S fluxnum_1: 1 priority: 1 param_1: DATA-RATE = 32 req_2: SEQ 52.001-52.011 NO GAP; req_3: SAME POS FOR 52.002-52.011 AS 52.001; req_4: CYCLE 2 / 52.001-52.011; req_5: ORIENT 223.16D +/- .3D; req_6: POS TARG +3.406,-10.551; comment_1: NEAR JD2449030.13 V1 AXIS AND comment_2: ORIENTATION SPECIFIED TO PUT comment_3: REFERENCE STARS IN PICKLE. JDTOBS IS comment_4: THE JULIAN DATE THAT THIS ORIENTATION comment_5: IS AT NOMINAL ROLL. 180D OPTION IS NOT ! linenum: 52.002 targname: 520-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 52.003 targname: 521-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 52.004 targname: 522-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 52.005 targname: NEWHIP-48-REF config: ^ opmode: ^ aperture: ^ sp_element: F5ND num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 52.006 targname: NEWEGOC-48NEWHIP-48 config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 52.007 targname: NEWHIP-48-REF config: ^ opmode: ^ aperture: ^ sp_element: F5ND num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 52.008 targname: 522-REF config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 51.2S fluxnum_1: 1 priority: 1 param_1: DATA-RATE = 32 ! linenum: 52.009 targname: 521-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 52.010 targname: 520-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 52.011 targname: NEWEGOC-48NEWHIP-48 config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 51.2S fluxnum_1: 1 priority: 1 param_1: DATA-RATE = 32 ! linenum: 62.001 targname: NEWEGOC-50NEWHIP-50 config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 51.2S fluxnum_1: 1 priority: 1 param_1: DATA-RATE = 32 req_2: SEQ 62.001-62.011 NO GAP; req_3: SAME POS FOR 62.002-62.011 AS 62.001; req_4: CYCLE 2 / 62.001-62.011; req_5: ORIENT 349.33D +/- .3D; req_6: POS TARG +223.825,-88.169; comment_1: NEAR JD2449118.44 V1 AXIS AND comment_2: ORIENTATION SPECIFIED TO PUT comment_3: REFERENCE STARS IN PICKLE. JDTOBS IS comment_4: THE JULIAN DATE THAT THIS ORIENTATION comment_5: IS AT NOMINAL ROLL. 180D OPTION IS NOT ! linenum: 62.002 targname: 620-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 62.003 targname: 621-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 62.004 targname: 622-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 62.005 targname: NEWHIP-50-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 62.006 targname: NEWEGOC-50NEWHIP-50 config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 62.007 targname: NEWHIP-50-REF config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 51.2S fluxnum_1: 1 priority: 1 param_1: DATA-RATE = 32 ! linenum: 62.008 targname: 622-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 62.009 targname: 621-REF config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 51.2S fluxnum_1: 1 priority: 1 param_1: DATA-RATE = 32 ! linenum: 62.010 targname: 620-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 62.011 targname: NEWEGOC-50NEWHIP-50 config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 72.001 targname: NEWEGOC-52NEWHIP-52 config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 51.2S fluxnum_1: 1 priority: 1 param_1: DATA-RATE = 32 req_2: SEQ 72.001-72.011 NO GAP; req_3: SAME POS FOR 72.002-72.011 AS 72.001; req_4: CYCLE 2 / 72.001-72.011; req_5: ORIENT 226.6D +/- .3D; req_6: POS TARG -427.591,-128.818; comment_1: NEAR JD2449100.64 V1 AXIS AND comment_2: ORIENTATION SPECIFIED TO PUT comment_3: REFERENCE STARS IN PICKLE. JDTOBS IS comment_4: THE JULIAN DATE THAT THIS ORIENTATION comment_5: IS AT NOMINAL ROLL. 180D OPTION IS NOT ! linenum: 72.002 targname: 720-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 72.003 targname: 721-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 72.004 targname: 722-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 72.005 targname: NEWHIP-52-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 72.006 targname: NEWEGOC-52NEWHIP-52 config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 51.2S fluxnum_1: 1 priority: 1 param_1: DATA-RATE = 32 ! linenum: 72.007 targname: NEWHIP-52-REF config: FGS opmode: POS aperture: 3 sp_element: F583W num_exp: 1 time_per_exp: 51.2S fluxnum_1: 1 priority: 1 param_1: DATA-RATE = 32 ! linenum: 72.008 targname: 722-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 72.009 targname: 721-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 72.010 targname: 720-REF config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 72.011 targname: NEWEGOC-52NEWHIP-52 config: ^ opmode: ^ aperture: ^ sp_element: F583W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! ! end of exposure logsheet ! No scan data records found