! File: 2185C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:02:50:55 coverpage: title_1: ASTROMETRY VERIFICATIONS AND TESTS; AST-OV-20 proposal_for: OV/AST pi_title: PROF. pi_fname: WILLIAM pi_mi: H. pi_lname: JEFFREYS pi_inst: UNIVERSITY OF TEXAS pi_country: USA pi_phone: (512) 471-4461 hours_pri: 0.50 num_pri: 21 fgs: X ! end of coverpage abstract: line_1: The goal of this test is to 1) verify that each FGS filter wheel position as line_2: commanded actually results from the command. This is required for any line_3: observations requiring a filter other than the "clear" filter. 2) verify that line_4: the FGSs will be able to observe stars of different magnitudes by using line_5: different integration sample times. The test will be coordinated with P-E. line_6: Successful conclusion of this test is required for astrometry on objects line_7: fainter than the Guide Star limit. 3) determine if objects fainter than the line_8: nominal 17.0 magnitude limit can be observed with the FGSs. The nominal limit line_9: may be used as a guide line, but the magnitudes may be uncertain by a magnitude. line_10: 4) verify that each FGS is capable of performing a Transfer Function Scan and line_11: determine an empirical "S" curve. This test is to be coordinated with P-E. line_12: 5) verify the ability of the FGSs to obtain astrometric data on a 17th line_13: magnitude star which will allow its relative position to be determined to line_14: 0.002" in one minute. 6)determine the effects of varying FGE NFES Slope in line_15: transiting from coarse track to fine lock, on the statistical nature of the line_16: astrometric data, and on the parameters which allow acquisition of astrometric line_17: targets with different characteristics. Priorities for FGS Bays 3,1,2 are line_18: 1,1,1. These tests should be performed contiguously with the PE test "First line_19: Order Plate Scale and FGS/FGS/FGS Alignment. ! ! end of abstract general_form_proposers: lname: TEAM fname: ASTROMETRY SCIENCE inst: UNIVERSITY OF TEXAS country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: Justifications for each subsection of this test follow: line_2: 1) When commanding the Filter Wheel of an FGS, the observer must know which line_3: filter goes with which position, and know that the filter wheel will go to line_4: the commanded position. line_5: 2) The astrometric instrument must be able to take astrometric data on stars at line_6: least as faint as 17th magnitude. The operation will require setting the line_7: integration exponent to a value other than the default (0). Optimum line_8: operation at a given magnitude will require a knowledge of the behavior of line_9: the FGSs with different integration sample times. line_10: 3) Verify the actual faint limit for astrometry with each FGS unit. line_11: 4) Engineering verification of transfer function scan astrometry is required line_12: before Science Verification. line_13: 5) The position of a 17th magnitude star with respect to other stars in the line_14: FGS/FOV to 0.002" is a CEI specification for Astrometry. This test line_15: determines how long a measurement is required to obtain what accuracy on a line_16: 17th magnitude star for each FGS. line_17: 6) Operation of the FGSs for astrometry requires parameters to be set in line_18: the FGE. These parameters are uplinked and will vary from default values line_19: used for "regular" guiding, and may vary for special guiding problems, as line_20: well as astrometric use. We wish to vary the uplink parameter K1 (the NFES line_21: Slope of the linear portion of the "S" curve). The optimum value for this line_22: slope will depend on the height of the "S" curve, which, in turn, depends on line_23: the optical characteristics of each axis of each FGS "as-built," and on the ! question: 2 section: 2 line_1: line_2: object being observed. An extended object will reduce tha amplitude of the line_3: "S" curve, as will another star of whatever magnitude in the 5" square line_4: aperture, as will stray light or background nebulosity. Therefore, the line_5: effects of changing the slope must be determined for each FGS axis. In some line_6: cases, using an incorrect value may reduce efficiency. In others, it may line_7: make the difference between obtaining and not obtaining an observation. ! question: 3 section: 1 line_1: A) Acquire Guide Stars in FGS 1 and 3. line_2: 1) VERIFY FILTER WHEEL line_3: a) Set filter position 1 of FGS 2. Acquire a 10th magnitude star with known line_4: spectral type with FGS 2. Obtain 1 minute of data including PMT counts on line_5: the star with FGS 2. line_6: b) Repeat (a) for filter position 2 of FGS 2. line_7: c) Repeat (a) for filter position 3 of FGS 2. line_8: d) Repeat (a) for filter position 4 of FGS 2. line_9: 2) VERIFY INTEGRATION TIMES line_10: a) Obtain and measure an 11th magnitude star with i=0 and 1, in FGS 2. line_11: b) Obtain and measure a 13th magnitude star with i=1 and 3, in FGS 2. line_12: c) Obtain and measure a 15th magnitude star with i=3 and 7, in FGS 2. line_13: 3) VERIFY MAGNITUDE LIMITS line_14: a) Acquire 17th magnitude star in FGS 2 and take data for 1 min. line_15: b) Attempt to acquire 17.5 magnitude star in FGS 2. line_16: If successful, take data for 1.5 minute. line_17: c) If successful, attempt to acquire 18.0 magnitude star in FGS 2. line_18: If successful, take data for 2 minutes. line_19: 4) VERIFY TRANSFER FUNCTION SCAN line_20: a) Drive FGS 2 to expected location of test star. line_21: b) Go into Coarse Track (CT) and determine position of optical centroid. line_22: c) Back off at a 45D angle from CT position by (0.50 + 0.25) scan length. line_23: d) Ramp up to the scan rate (0.005 arcsec/sec, TBR). ! question: 3 section: 2 line_1: e) Scan across the star at 45D, taking data. line_2: f) Ramp down to zero rate. line_3: 5) TEST ASTROMETRIC ACCURACY ON A 17TH MAGNITUDE STAR IN 1 MIN line_4: a) Set on a 17th magnitude star with FGS 2 as Astrometer. line_5: b) Obtain FGS data for 5 minutes line_6: 6) VERIFY ASTROMETRY WITH DIFFERENT UPLINK PARAMETERS line_7: b) Set the K1 for FGS 2 at the default. line_8: c) Acquire Reference Star 1 in FGS 2 as Astrometer. line_9: d) Take astrometric data for 1 minute. line_10: e) Reset the K1 for FGS 2 at about .8 of the default. line_11: e) Move astrometer 10 arcsec away from the target by moving the astrometer star line_12: selectors. line_13: f) Reacquire Reference Star 1 if possible and take data for 1 minute. line_14: g) Repeat e and f at about 1.5 of the default. line_16: B) Repeat A with FGS 3 as Astrometer. line_18: C) Repeat with FGS 1 as Astrometer. line_20: N.B. FGS numbers refer to BAY numbers. ! question: 4 section: 1 line_1: 1) VERIFY FILTER WHEEL OPERATION line_2: The star will need ground-based magnitudes and multicolor photometry line_3: sufficient to distinguish the various filters. line_4: 2) VERIFY INTEGRATION TIMES, line_5: 3) VERIFY MAGNITUDE LIMITS, line_6: 4) VERIFY TRANSFER, FUNCTION SCAN, line_7: 5) TEST THE ASTROMETRIC 17TH MAGNITUDE STAR IN 1 MIN., line_8: 6) VERIFY ASTROMETRY WITH DIFFERENT UPLINK PARAMETERS. (Positions to line_9: 0.5 arcsec and magnitudes to 0.3 magnitudes will be provided from the line_10: ground.) ! question: 5 section: 0 line_1: (item 1 re RT branching deleted in 6/16/88 redline) line_3: 2) 32 Kbit link. line_4: 3) The successful conclusion of subsection 1) of this test is necessary for line_5: subsection 3) , subsection 5) , and any observations of stars fainter than line_6: the guide star limit. line_7: 4) Use astrophysically single stars for subsection 3). The results of line_8: subsection 2) are required to properly interpret the results line_9: of subsection 3. FGS observations of any object the magnitude of which line_10: is 16.5 or fainter will require a knowledge of the results of this test. line_11: 5) The successful conclusion of subsection 4) is required for the line_12: observations to be performed in AST-OV -8c, AST-SV-3c, and AST-SV-5. It is line_13: also required for any Transfer Function Scans or Moving Target Astrometer line_14: Ephermeris Track observations to be performed. line_15: 6) This test should be performed contiguously with, but separately from the PE line_16: test "First Order Plate Scale and FGS/FGS/FGS alignment. ! question: 5 section: 2 line_1: 1) The plan is to use stars already calibrated for spectral characteristics. line_2: Specific ground-based observations prior to this test may be required. line_3: Use 32 Kbit/sec FN format. Data must include all FGS data for the entire line_4: observations, not just when "data valid flag" is up. The important line_5: information is the detailed transition from coarse track to fine lock. ! question: 7 section: 1 line_1: 1) The data will be reduced using the ADRS software to determine the observed line_2: flux density as a function of filter position. The observed flux density line_3: will then be used in combination with the known spectral characteristics of line_4: the star plus the measured transmission characteristics of the various line_5: filters to determine empirically which filter is in which filter wheel line_6: position in each FGS. This table of filter vs. filter wheel position will be line_7: inserted into the Project Data Base. line_8: 2) ADRS within SDAS will be used to determine centroid and statistical line_9: information from the data, to determine the significance of changing the line_10: threshhold value of the FGSs. line_11: 3) ADRS in SDAS will be used to analyze the data. However, the nature of the line_12: test is such that an "on-off" answer essentially characterizes the nature of line_13: the test, and will be available from real-time or quick-look data. This test line_14: may be performed using P-E specified software to look at the incoming data. line_15: (TBR). line_16: 4) ADRS within SDAS will be used to derive the observed transfer function line_17: and determine whether the scans were conducted correctly. line_18: 5) ADRS within SDAS will be used to derive centroid and statistical line_19: information for various subsets of the FGS data, and determine the length of line_20: time necessary to derive positional accuracy of 0.002" accuracy on a 17th line_21: magnitude star. line_22: 6) ADRS within SDAS will be used to determine centroid and statistical line_23: information from the data, to determine the significance of changing the ! question: 7 section: 2 line_1: line_2: NFES Slope for the FGSs. ! question: 10 section: 1 line_1: 1), 2), 3), 5) ADRS will be available in Austin for data reduction. Some line_2: personnel will be available to aid in the OV data reduction. Some PDS line_3: OV support for Guide Stars is being provided. line_4: 4) ADRS will be available in Austin. Double star transfer function analysis line_5: software will also be available at the Lowell Observatory (Franz). ! !end of general form text general_form_address: lname: JEFFERYS fname: W. mi: H. category: PI inst: UNIVERSITY OF TEXAS ! lname: SHELUS fname: PETER category: CON inst: UNIVERSITY OF TEXAS addr_1: RLM 15.308 city: AUSTIN state: TX zip: 78712 country: USA phone: (512) 471-3339 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: UPGREN-62 descr_1: STAR IN NGC188 pos_1: RA= 00H 37M 11.07S +/- 2.0S, pos_2: DEC= +85D 04' 19.0" +/- 2.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V=9.80 +/- 0.05 fluxnum_2: 2 fluxval_2: B=11.33 +/-0.07 ! targnum: 2 name_1: UPGREN-69 descr_1: ^ pos_1: RA= 00H 37M 51.90S +/- 0.5S, pos_2: DEC= +84D 57' 47.8" +/- 0.5" equinox: ^ fluxnum_1: 1 fluxval_1: V=9.58 +/- 0.05 fluxnum_2: 2 fluxval_2: B=10.08 +/- 0.07 ! targnum: 3 name_1: UPGREN-112 descr_1: STAR IN NGC 188 pos_1: RA= 00H 40M 58.18S +/- 2S, pos_2: DEC= +85D 03' 31.1" +/- 2" equinox: 1950 fluxnum_1: 1 fluxval_1: V= 10.84 +/- 0.05 fluxnum_2: 2 fluxval_2: B= 12.12 +/- 0.05 ! targnum: 4 name_1: UPGREN-111 descr_1: ^ pos_1: RA= 00H 40M 46.26S +/- 2S, pos_2: DEC= +85D 01' 41.5" +/- 2" equinox: ^ fluxnum_1: 1 fluxval_1: V= 12.41 +/- 0.05 fluxnum_2: 2 fluxval_2: B= 13.75 +/- 0.05 ! targnum: 5 name_1: UPGREN-108 descr_1: ^ pos_1: RA= 00H 40M 39.36S +/- 2S, pos_2: DEC= +85D 02' 12.6" +/- 2" equinox: ^ fluxnum_1: 1 fluxval_1: V= 15.03 +/- 0.05 fluxnum_2: 2 fluxval_2: B= 15.72 +/- 0.05 ! targnum: 6 name_1: SANDAGE-I117 descr_1: NGC188 STAR pos_1: RA= 00H 40M 52.61S +/- 2S, pos_2: DEC= +84D 58' 18.5" +/- 2" equinox: ^ fluxnum_1: 1 fluxval_1: V= 17.40 +/- 0.05 fluxnum_2: 2 fluxval_2: B= 18.32 +/- 0.05 ! targnum: 7 name_1: SANDAGE-I118 descr_1: NGC188 STAR pos_1: RA= 00H 41M 13.76S +/- 2S, pos_2: DEC= +84D 58' 30.8" +/- 2" equinox: ^ fluxnum_1: 1 fluxval_1: V= 17.02 +/- 0.05 fluxnum_2: 2 fluxval_2: B= 18.08 +/- 0.05 ! targnum: 8 name_1: SANDAGE-I166 descr_1: NGC 188 STAR pos_1: RA= 00H 43M 38.61S +/- 2S, pos_2: DEC= +84D 58' 19.6" +/- 2", equinox: ^ comment_1: TARGETS 6,7, AND 8 MUST BE OBSERVED comment_3: WITH ONE POINTING/FGS MEASUREMENT fluxnum_1: 1 fluxval_1: V= 18.03 +/- 0.05 fluxnum_2: 2 fluxval_2: B= 19.29 +/- 0.05 ! targnum: 9 name_1: UPGREN-138 descr_1: NGC188 STAR pos_1: RA= 00H 41M 56.73S +/- 2S, pos_2: DEC= 84D 59' 06.2" +/- 2", equinox: 1950 fluxnum_1: 1 fluxval_1: V=14.28 +/- 0.05 fluxnum_2: 2 fluxval_2: B=15.16 +/- 0.05 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: AST-FIL targname: UPGREN-62 config: FGS opmode: POS aperture: # sp_element: F583W num_exp: 1 time_per_exp: 1M fluxnum_1: 1 priority: 1 param_1: FES-TIME=0.025, param_2: DATA-RATE=32, req_1: SAME ORIENT FOR 2-4 AS 1; ! linenum: 2.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F5ND num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ req_1: SAME POS FOR 2-4 AS 1; req_2: SEQ 1-4 NO GAP; ! linenum: 3.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F650W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 4.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F550W num_exp: ^ time_per_exp: ^ fluxnum_1: ^ priority: ^ param_1: ^ ! linenum: 11.000 sequence_1: DEFINE sequence_2: INT-TIM targname: UPGREN-112 config: FGS opmode: POS aperture: # sp_element: F550W num_exp: 1 time_per_exp: 1M fluxnum_1: 1 priority: 1 param_1: FES-TIME=0.025, param_2: DATA-RATE=32, req_1: SAME POS FOR 12-16 AS 11; ! linenum: 12.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ fluxnum_1: 1 priority: ^ param_1: FES-TIME=0.05, param_2: DATA-RATE=32, req_1: SAME ORIENT FOR 12-16 AS 11; ! linenum: 13.000 sequence_1: ^ targname: UPGREN-111 config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ fluxnum_1: 1 priority: ^ param_1: ^ req_1: SEQ 11-16 NO GAP; ! linenum: 14.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ fluxnum_1: 1 priority: ^ param_1: FES-TIME=0.2, param_2: DATA-RATE=32, ! linenum: 15.000 sequence_1: ^ targname: UPGREN-108 config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ fluxnum_1: 1 priority: ^ param_1: ^ ! linenum: 16.000 sequence_1: DEFINE sequence_2: INT-TIM targname: UPGREN-108 config: FGS opmode: POS aperture: # sp_element: F550W num_exp: 1 time_per_exp: 1M fluxnum_1: 1 priority: 1 param_1: FES-TIME=1.6, param_2: DATA-RATE=32, ! linenum: 21.000 sequence_1: DEFINE sequence_2: MAG-LIM targname: SANDAGE-I118 config: FGS opmode: POS aperture: # sp_element: F583W num_exp: 1 time_per_exp: 1M fluxnum_1: 1 priority: 1 param_1: DATA-RATE=32, req_1: SAME POS FOR 22-23 AS 21; req_2: SAME ORIENT FOR 22-23 AS 21; req_3: SEQ 21-23 NO GAP; ! linenum: 22.000 sequence_1: ^ sequence_2: ^ targname: SANDAGE-I117 config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: 1.5M fluxnum_1: 1 priority: 1 param_1: ^ ! linenum: 23.000 sequence_1: ^ sequence_2: ^ targname: SANDAGE-I166 config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: 2M fluxnum_1: 1 priority: 1 param_1: ^ ! linenum: 31.000 sequence_1: DEFINE sequence_2: FGS-TFN targname: UPGREN-69 config: FGS opmode: TRANS aperture: # sp_element: F583W num_exp: 1 time_per_exp: 100S fluxnum_1: 1 priority: 1 param_1: STEP-SIZE=0.125, comment_1: USE DATA-RATE=32. ! linenum: 51.000 sequence_1: DEFINE sequence_2: STAR-17 targname: SANDAGE-I118 config: FGS opmode: POS aperture: # sp_element: F583W num_exp: 1 time_per_exp: 5M fluxnum_1: 1 priority: 1 param_1: DATA-RATE=32, ! linenum: 61.000 sequence_1: DEFINE sequence_2: SLOPE targname: UPGREN-138 config: FGS opmode: POS aperture: # sp_element: F550W num_exp: 1 time_per_exp: 1M fluxnum_1: 1 priority: 1 param_1: FES-TIME=0.025, param_3: DATA-RATE=32, param_4: COUNT=900, req_1: SEQ 61-63 NO GAP; req_2: SAME POS FOR 62-63 AS 61; req_3: SAME ORIENT FOR 62-63 AS 61; comment_1: MOVE ASTROMETER STAR SELECTORS TO comment_2: POSITION THE TARGET AT THE INITIAL comment_3: POSITION TO START COARSE TRACK, USING comment_4: COUNT PARAMETER TO FORCE ADJUSTMENT comment_5: OF K1X AND K1Y. ! linenum: 62.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ fluxnum_1: 1 priority: ^ param_2: DATA-RATE=32, param_3: FES-TIME=0.025, comment_1: MOVE ASTROMETER STAR SELECTORS TO comment_2: POSITION THE TARGET AT THE INITIAL comment_3: POSITION TO START COARSE TRACK. comment_4: USING GROUND SYSTEM GENERATED NOMINAL comment_5: K1 VALUES. ! linenum: 63.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ fluxnum_1: 1 priority: ^ param_2: DATA-RATE=32, param_3: FES-TIME=0.025, param_4: COUNT=5200, comment_1: MOVE ASTROMETER STAR SELECTORS TO comment_2: POSITION THE TARGET AT THE INITIAL comment_3: POSITION TO START COARSE TRACK, USING comment_4: COUNT PARAMETER TO FORCE ADJUSTMENT comment_5: OF K1X AND K1Y. ! linenum: 71.000 sequence_1: USE sequence_2: AST-FIL aperture: 1 req_1: SEQ 71-77; ! linenum: 72.000 sequence_1: USE sequence_2: INT-TIM aperture: 1 ! linenum: 73.000 sequence_1: USE sequence_2: MAG-LIM aperture: 1 ! linenum: 74.000 sequence_1: USE sequence_2: FGS-TFN aperture: 1 ! linenum: 76.000 sequence_1: USE sequence_2: STAR-17 aperture: 1 ! linenum: 77.000 sequence_1: USE sequence_2: SLOPE aperture: 1 ! linenum: 81.000 sequence_1: USE sequence_2: AST-FIL aperture: 2 req_1: SEQ 81-87; ! linenum: 82.000 sequence_1: USE sequence_2: INT-TIM aperture: 2 ! linenum: 83.000 sequence_1: USE sequence_2: MAG-LIM aperture: 2 ! linenum: 84.000 sequence_1: USE sequence_2: FGS-TFN aperture: 2 ! linenum: 86.000 sequence_1: USE sequence_2: STAR-17 aperture: 2 ! linenum: 87.000 sequence_1: USE sequence_2: SLOPE aperture: 2 ! linenum: 91.000 sequence_1: USE sequence_2: AST-FIL aperture: 3 req_1: SEQ 91-97; ! linenum: 92.000 sequence_1: USE sequence_2: INT-TIM aperture: 3 ! linenum: 93.000 sequence_1: USE sequence_2: MAG-LIM aperture: 3 ! linenum: 94.000 sequence_1: USE sequence_2: FGS-TFN aperture: 3 ! linenum: 96.000 sequence_1: USE sequence_2: STAR-17 aperture: 3 ! linenum: 97.000 sequence_1: USE sequence_2: SLOPE aperture: 3 ! ! end of exposure logsheet ! No scan data records found