! File: 5017C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:15:30:39 coverpage: title_1: INTERNAL VELOCITY DISTRIBUTION IN GLOBULAR CLUSTERS title_2: PART THREE,CYCLE 3, HIGH 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_11: The observations are designed to yield an accuracy of +/- 1 km/sec in the line_12: derived cluster velocity dispersion at each location in the cluster for the line_13: 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 three separate regions line_2: with different exposure levels. Spatially, the regions selected are the line_3: central core, a region offset from the center 5 core radii, and a region line_4: offset from the center 10 core radii. Observations at 5 and 10 core line_5: radii will be used to study the run of isotropy in the velocities. line_6: Each "exposure" consists of 5 or 10 separate exposures offset from line_7: each other by small amounts on the order of an arcsec. The purpose of these line_8: offsets is to average out the pixel to pixel variations in the CCD detectors. line_9: In addition, the first three of these exposures are taken with the V filter and line_10: the last two with the R filter. The groups of exposures are defined by sequences line_11: PC5 and PC10. Due to image crowding in the center, only short 25 and 100 second line_12: exposures are taken, while at the other positions, a long 1000 second exposure line_13: is taken. This range of exposures allows us to reach from the line_14: horizontal branch to the main sequence with a positional accuracy of 0.001 line_15: arcsec. These exposures will be repeated after five years to obtain the proper line_16: motions. ! question: 3 section: 2 line_1: These three clusters are to be observed at their centers and at the two offset line_2: positions, at 5 and 10 core radii. Cycle 3 estimated observing time = line_3: Cycle 3: 16.47 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: 6752 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: NGC7078 name_2: M15 descr_1: C,201 pos_1: RA=21H 27M 33.35S +/- 0.1S, pos_2: DEC=+11D 56' 48.8" +/- 1" equinox: 1950 pm_or_par: N acqpr_1: EXT plate_req: N ! targnum: 2 name_1: NGC7078-R1 descr_1: ^ pos_1: RA=21H 27M 33.35S +/- 0.1S, pos_2: DEC=+11D 58' 48.8" +/- 1" equinox: ^ pm_or_par: ^ acqpr_1: ^ plate_req: ^ ! targnum: 3 name_1: NGC7078-R2 descr_1: ^ pos_1: RA=21H 27M 33.35S +/- 0.1S, pos_2: DEC=+11D 54' 48.8" +/- 1" equinox: ^ pm_or_par: ^ acqpr_1: ^ plate_req: ^ ! targnum: 4 name_1: NGC7099 name_2: M30 descr_1: C,201 pos_2: RA=21H 37M 31.64S +/- 0.1S, pos_3: DEC=-23D 24' 23.1" +/- 1" equinox: 1950 pm_or_par: N acqpr_1: EXT plate_req: N ! targnum: 5 name_1: NGC7099-R1 descr_1: ^ pos_2: RA=21H 37M 31.64S +/- 0.1S, pos_3: DEC=-23D 26' 38.1" +/- 1" equinox: ^ pm_or_par: ^ acqpr_1: ^ plate_req: ^ ! targnum: 6 name_1: NGC7099-R2 descr_1: ^ pos_2: RA=21H 37M 31.64S +/- 0.1S, pos_3: DEC=-23D 22' 08.1" +/- 1" equinox: ^ pm_or_par: ^ acqpr_1: ^ plate_req: ^ ! targnum: 7 name_1: NGC6205 name_2: M13 descr_1: C,201 pos_2: RA=16H 39M 54.19S +/- 0.1S, pos_3: DEC=+36D 33' 16.3" +/- 1" equinox: 1950 pm_or_par: N acqpr_1: EXT plate_req: N ! targnum: 8 name_1: NGC6205-R1 descr_1: ^ pos_2: RA=16H 39M 54.19S +/- 0.1S, pos_3: DEC=+36D 36' 58.3" +/- 1" equinox: ^ pm_or_par: ^ acqpr_1: ^ plate_req: ^ ! targnum: 9 name_1: NGC6205-R2 descr_1: ^ pos_2: RA=16H 39M 54.19S +/- 0.1S, pos_3: DEC=+36D 40' 40.3" +/- 1" 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: 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; req_2: SEQ 1-5 NO GAP; ! 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 2-5 AS 1; req_2: POS TARG +5.70,-14.30; ! linenum: 3.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: ^ num_exp: ^ time_per_exp: ^ priority: ^ param_1: ^ param_2: ^ req_1: POS TARG +14.30,-14.30; ! linenum: 4.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F785LP wavelength: 8958 num_exp: ^ time_per_exp: ^ priority: ^ param_1: ^ param_2: ^ req_1: POS TARG +14.30,-5.70; ! linenum: 5.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: ^ num_exp: ^ time_per_exp: ^ priority: ^ param_1: ^ param_2: ^ req_1: POS TARG +5.70,-5.70; ! linenum: 14.000 sequence_1: USE PC5 targname: NGC7078 time_per_exp: X1.0 priority: 1 req_1: CYCLE 3 / 14-22 comment_1: FIRST EPOCH EXPOSURES OF NGC7078 USING comment_2: PC + F555W AND PC + F785LP ! linenum: 15.000 sequence_1: USE PC5 targname: NGC7078-R1 time_per_exp: X10 priority: 2 ! linenum: 16.000 sequence_1: USE PC5 targname: NGC7078-R2 time_per_exp: X10 priority: 2 ! linenum: 17.000 sequence_1: USE PC5 targname: NGC7099 time_per_exp: X1.0 priority: 1 comment_1: FIRST EPOCH EXPOSURES OF NGC7099 USING comment_2: PC + F555W AND PC + F785LP ! linenum: 18.000 sequence_1: USE PC5 targname: NGC7099-R1 time_per_exp: X10 priority: 2 ! linenum: 19.000 sequence_1: USE PC5 targname: NGC7099-R2 time_per_exp: X10 priority: 2 ! linenum: 20.000 sequence_1: USE PC5 targname: NGC6205 time_per_exp: X1.0 priority: 1 comment_1: FIRST EPOCH EXPOSURES OF NGC6205 USING comment_2: PC + F555W AND PC + F785LP ! linenum: 21.000 sequence_1: USE PC5 targname: NGC6205-R1 time_per_exp: X10 priority: 2 ! linenum: 22.000 sequence_1: USE PC5 targname: NGC6205-R2 time_per_exp: X10 priority: 2 ! ! end of exposure logsheet ! No scan data records found