! File: 2943C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:23:50:26 coverpage: title_1: INTERNAL VELOCITY DISTRIBUTION IN GLOBULAR CLUSTERS title_2: PART ONE sci_cat: STELLAR POPULATIONS proposal_for: GTO/AST longterm: 5 cont_id: 1007 pi_fname: WILLIAM pi_mi: H. pi_lname: JEFFERYS pi_inst: TEXAS, UNIVERSITY OF pi_country: USA pi_phone: 512-471-4461 keywords_1: GLOBULAR CLUSTERS, PROPER MOTIONS, INTERNAL keywords_2: VELOCITIES hours_pri: 19.01 num_pri: 22 wf_pc: X pi_position: PROFESSOR ! end of coverpage abstract: line_1: The goal of this project is to study the internal velocity dispersion for six line_2: globular clusters with a range of characteristics. We expect to determine the line_3: virial mass for each cluster and a kinematic distance (statistical parallax) line_4: where radial velocity observations exist. The radial and azimuthal components line_5: of the velocity distribution will be analyzed to determine the degree of line_6: anisotropy in the velocities as a function of distance from the cluster center line_7: for three of the clusters. In addition, the degree to which equipartition of line_8: energy exists among the various mass groupings will be studied from the bright line_9: giants down to one-half solar mass in three of the clusters. line_10: The observations are designed to yield an accuracy of +/- 1 km/sec in the line_11: derived cluster velocity dispersion at each location in the cluster for the line_12: nearer clusters and +/- 2 km/sec for the more distant clusters. ! ! end of abstract general_form_proposers: lname: JEFFERYS fname: WILLIAM mi: H. inst: TEXAS, UNIVERSITY OF country: USA ! lname: BENEDICT fname: GEORGE mi: F. inst: TEXAS, UNIVERSITY OF country: USA ! lname: DUNCOMBE fname: RAYNOR mi: L. inst: TEXAS, UNIVERSITY OF country: USA ! lname: FRANZ fname: OTTO mi: G. inst: LOWELL OBSERVATORY country: USA ! lname: FREDRICK fname: LAURENCE mi: W. inst: VIRGINIA, UNIVERSITY OF country: USA ! lname: HEMENWAY fname: PAUL mi: D. inst: TEXAS, UNIVERSITY OF country: USA ! lname: SHELUS fname: PETER mi: J. inst: TEXAS, UNIVERSITY OF country: USA ! lname: VAN ALTENA fname: WILLIAM mi: F. inst: YALE UNIVERSITY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The observations for each cluster are divided into four separate regions line_2: with different exposure levels. Spatially, the regions selected are the line_3: central core, a region east of the center at 10 core radii, and two regions line_4: east and west of the center at 20 core radii. Observations at 10 and 20 core line_5: radii will be used to study the run of isotropy in the velocities. Due to the line_6: low density of stars far from the center, it is necessary to have two regions line_7: at 20 core radii. Each "exposure" consists of 5 separate exposures offset from line_8: each other by small amounts on the order of an arcsec. The purpose of these line_9: offsets is to average out the pixel to pixel variations in the CCD detectors. line_10: In addition, the first three of these exposures are taken with the V filter and line_11: the last two with the R filter. This group of exposures is defined by sequence line_12: PC5. Due to image crowding in the center, only a short 25 second exposure is line_13: taken, while at the other positions both a short 100 second and a long 1000 line_14: second exposure is taken. This range of exposures allows us to reach from the line_15: horizontal branch to the main sequence with a positional accuracy of 0.001 line_16: arcsec. These exposures will be repeated after five years to obtain the proper line_17: motions. line_18: The sequence PC10 is used to spatially calibrate the detector system both line_19: before and after the observations. The sequence consists of ten exposures line_20: randomly placed over the 32 x 32 subgrid of the CCD. It is hoped to use these line_21: observations to further increase the accuracy of the relative positions of the line_22: stars through a bootstrap calibration developed procedure suggested by line_23: Eichhorn. ! question: 3 section: 2 line_1: Due to time limitations, three of the clustes are to be observed only in line_2: their centers. The outer regions are included in the observing logsheets as line_3: priority 3 objects. The total observing time listed on the cover sheet assumes line_4: that priority 3 objects will not be observed and that filter changes can be line_5: made during the 60 second read out of the CCD. line_7: Cycle 1 18.22 hours line_8: Cycle 2 0.45 hours line_9: Cycle 3 0.00 hours line_10: Cycle 4 0.00 hours line_11: Cycle 5 0.00 hours ! question: 4 section: 1 line_1: Ground based observations of the proper motions are limited by the first line_2: epoch plates, which usually have a very bright limiting magnitude. In line_3: addition, the poor seeing makes it impossible to observe near the center of the line_4: cluster and limits the positional accuracy to a value some 15 times poorer than line_5: is possible with the PC. Since the difference in the positional accuracy line_6: translates directly into a difference in the epoch difference, we would have to line_7: wait at least 65 years for the second epoch on the ground. ! question: 5 section: 1 line_1: The only special scheduling requirements are to maintain the same roll line_2: angle for all of the exposures in one sequence. This is necessary if we are to line_3: have the same stars on all exposures. ! question: 6 section: 1 line_1: Sequence PC10 is used to obtain observations of the central region of NGC line_2: 6656 before and after the observations, which will hopefully be completed line_3: during the first year of operations. The ten offset exposures will be used to line_4: obtain a bootstrap calibration of the spatial characteristics of the PC, and to line_5: study the changes in the system over the observational period. ! question: 7 section: 1 line_1: The data reduction will be done with the Astrometric Data Reduction line_2: Software developed by the Astrometry Team on computational facilities already line_3: available at the home institutions of the Team members. ! question: 10 section: 1 line_1: Computational facilities and the ADRS software package. ! question: 13 section: 1 line_1: Planetary Camera exposures will be taken of six of the globular clusters line_2: (NGC 104, NGC 1851, NGC 6205, NGC 6656, NGC 6752, NGC 7078, NGC 7099) to line_3: determine their internal motions from the horizontal branch to the main line_4: sequence. These motions will also be used to study the degree of relaxation line_5: and isotropy in stars of differing masses. In addition, exposures will be line_6: taken of Pal 1 to determine its membership and tangential velocity in the line_7: galactic frame of reference. ! !end of general form text general_form_address: lname: JEFFERYS fname: WILLIAM mi: H. category: PI inst: UNIVERSITY OF TEXAS addr_1: ASTRONOMY DEPARTMENT city: AUSTIN state: TX zip: 78712 country: USA phone: (212) 471-4461 ! lname: VAN ALTENA fname: WILLIAM mi: F. category: CON inst: YALE UNIVERSITY addr_1: 260 WHITNEY AVENUE city: NEW HAVEN state: CT zip: 06511 country: USA phone: (203) 436-8318 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC6752 descr_1: C,201 pos_1: RA= 19H 10M 52.47S +/- 0.08S, pos_2: DEC= -59D 59' 04.2" +/- 0.5" equinox: 2000 pm_or_par: N acqpr_1: EXT plate_req: N ! targnum: 2 name_1: NGC6752-R1 descr_1: ^ pos_1: RA= 19H 11M 05.41S +/- 0.08S, pos_2: DEC= -59D 56' 27.4" +/- 0.5" equinox: ^ pm_or_par: ^ acqpr_1: ^ plate_req: ^ ! targnum: 3 name_1: NGC6752-R2 descr_1: ^ pos_1: RA= 19H 10M 57.85S +/- 0.08S, pos_2: DEC= -59D 53' 11.0" +/- 0.5" equinox: ^ pm_or_par: ^ acqpr_1: ^ plate_req: ^ ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: PC10 targname: # config: PC opmode: IMAGE aperture: PCALL-FIX sp_element: F555W wavelength: 5479 num_exp: 1 time_per_exp: 100S priority: # param_1: CR-SPLIT=NO, PRE-FLASH=YES param_2: CLOCKS=YES req_1: POS TARG +10.00,-10.00 / 1-10; req_2: SEQ 1-10 NO GAP; comment_1: POS TARG OFFSETS ARE BASED ON comment_2: CYCLE 2 COORD SYSTEM comment_3: (I.E. PCALL-FIX TOGETHER WITH comment_4: POS TARG +10.0,-10.0 EQUALS APEX) ! linenum: 2.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: ^ num_exp: ^ time_per_exp: ^ priority: ^ param_1: ^ param_2: ^ req_1: SAME ORIENT FOR 2-10 AS 1; req_2: SPATIAL SCAN ! linenum: 6.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F785LP wavelength: 8958 num_exp: ^ time_per_exp: ^ priority: ^ param_1: ^ param_2: ^ req_1: SPATIAL SCAN ! linenum: 10.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: ^ num_exp: ^ time_per_exp: ^ priority: ^ param_1: ^ param_2: ^ ! linenum: 11.000 sequence_1: DEFINE sequence_2: PC5 targname: # config: PC opmode: IMAGE aperture: PCALL-FIX sp_element: F555W wavelength: 5479 num_exp: 1 time_per_exp: 100S priority: # param_1: CR-SPLIT=NO, PRE-FLASH=YES param_2: CLOCKS=YES req_1: POS TARG +10.00,-10.00 / 11-14; req_2: SEQ 11-14 NO GAP; ! linenum: 12.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: ^ num_exp: ^ time_per_exp: ^ priority: ^ param_1: ^ param_2: ^ req_1: SAME ORIENT FOR 12-14 AS 11; req_2: SPATIAL SCAN ! linenum: 14.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F785LP wavelength: 8958 num_exp: ^ time_per_exp: ^ priority: ^ param_1: ^ param_2: ^ req_1: SPATIAL SCAN ! linenum: 16.000 sequence_1: USE PC10 targname: NGC6752 time_per_exp: X1.0 priority: 1 req_1: CYCLE 1 / 16-19 comment_1: ASTROMETRIC CALIBRATION OF PC + F555W comment_2: AND F785LP ! linenum: 17.000 sequence_1: USE PC5 targname: NGC6752 time_per_exp: X0.26 priority: 1 ! linenum: 18.000 sequence_1: USE PC5 targname: NGC6752-R1 time_per_exp: X10 priority: 2 ! linenum: 19.000 sequence_1: USE PC5 targname: NGC6752-R2 time_per_exp: X10 priority: 2 ! ! end of exposure logsheet scan_data: line_list: 2.0 fgs_scan: cont_dwell: D dwell_pnts: 2 dwell_secs: 0.00 scan_width: 8.6000 scan_length: 8.6000 sides_angle: 270.0000 number_lines: 2 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 4.3 wid_offset: 4.3 ! line_list: 6.0 fgs_scan: cont_dwell: D dwell_pnts: 2 dwell_secs: 0.00 scan_width: 4.3000 scan_length: 4.3000 sides_angle: 270.0000 number_lines: 2 scan_rate: 0.0000 first_line_pa: 45.0000 scan_frame: S/C len_offset: 2.15 wid_offset: 2.15 ! line_list: 12.0 fgs_scan: cont_dwell: D dwell_pnts: 2 dwell_secs: 0.00 scan_width: 8.6000 scan_length: 8.6000 sides_angle: 270.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 0.00 wid_offset: 4.30 ! line_list: 14.0 fgs_scan: cont_dwell: D dwell_pnts: 2 dwell_secs: 0.00 scan_width: 8.6000 scan_length: 8.6000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 0.00 wid_offset: 4.30 ! ! end of scan data