! File: 1052C.PROP ! Database: PEPDB ! Date: 15-FEB-1994:23:51:57 coverpage: title_1: GLOBULAR CLUSTER CORE STRUCTURE AND DYNAMICS (FOS 36) -- CYCLE 0 sci_cat: STELLAR POPULATIONS proposal_for: GTO/FOS pi_fname: RALPH pi_lname: BOHLIN pi_inst: SPACE TELESCOPE SCIENCE INSTITUTE pi_country: USA pi_phone: (301) 338-4804 keywords_1: GLOBULAR CLUSTER hours_pri: 6.58 num_pri: 24 wf_pc: X fos: X ! end of coverpage abstract: line_1: Obtain data on the stellar populations in the central cores of globular line_2: clusters. Clusters with and without central unresolved cusps, and with and line_3: without central X-ray sources will be observed. Spectra will be obtained at line_4: the center of the UV brightness, and at a distance within about one core line_5: radius. We might expect these spectra to differ; massive objects formed in line_6: collisions may produce unexpected spectral features, as well as relatively line_7: intense UV radiation in the central core. ! ! end of abstract general_form_proposers: lname: BEAVER fname: EDWARD inst: UC, SAN DIEGO country: USA ! lname: BURBIDGE fname: E. MARGARET inst: UC, SAN DIEGO country: USA ! lname: MARGON fname: BRUCE inst: WASHINGTON, UNIVERSITY OF country: USA ! lname: SPITZER JR. fname: LYMAN inst: PRINCETON UNIVERSITY country: USA ! lname: ANGEL fname: J. ROGER mi: P. inst: ARIZONA, UNIVERSITY OF country: USA ! lname: BARTKO fname: FRANK inst: APPLIED RESEARCH CORPORATION country: USA ! lname: DAVIDSEN fname: ARTHUR mi: F. inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: HARMS fname: RICHARD mi: J. inst: APPLIED RESEARCH CORPORATION country: USA ! lname: BOHLIN fname: RALPH inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: FORD fname: HOLLAND mi: C. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Since the globular clusters are faint, use the low dispersion G160L and line_2: the Prism on the Blueside. Use the lower 0.3" aperture. 20s DARK exposures line_3: are especially useful for these faint targets; take DARKS before and after each line_4: exposure. The PC images are essential for target acquisition for the spectra. line_5: Offset the PC pointing to place the center of the G.C. (quoted coordinates) line_6: 10" off the pyramid along the centerline of the best CCD chip. We require two line_7: months between delivery of the PC images and the final specification of the FOS line_8: pointings. FOS target acquisition in mode III assumes that the PC is line_9: calibrated for astrometry to 0.03". line_11: PC filters are F230W, F336W, and F547M. line_12: Cycle 0 Exp: 10, 16 line_13: Cycle 1 Exp: 10.9-12 line_14: Cycle 2 Exp: 13-15, 16.9-28 ! question: 5 section: 2 line_1: The SV prerequisite programs for all FOS line_2: observations in this program are: line_3: Prop ID 2195 FOS Target Acquisition Tests line_4: - All observations line_5: Prop ID 1317 Int./Ext. Wavelength Offsets line_6: - 1st target line_7: Prop ID 1318 Spectral Flat Fields line_8: - 1st target line_9: Prop ID 1320 Absolute Spectrophotometry line_10: - 1st visit of bright targets line_11: All WF/PC imaging with a center wavelength line_12: blueward of 5000 Angstroms requires UV flood ! question: 6 section: 1 line_1: DARK may or may not be necessary, but if incidents ever occur that raise the line_2: dark level, we will have no ex-post facto way of validating any continuum line_3: spectrum without a DARK measure at the time of each observation. ! question: 12 section: 1 line_1: This program does not become a viable scientific investigation until 5 of the 6 line_2: globular clusters have been observed by both the WFPC and FOS. No data should line_3: be made public sooner than 1 year after that time. ! question: 13 section: 1 line_1: Use FOS spectra to investigate the structure and dynamics of the cores of line_2: globular clusters. Spectra on and just off the core will be obtained for line_3: clusters with and without cusps and with and without central x-ray sources. ! !end of general form text general_form_address: lname: BOHLIN fname: RALPH category: PI inst: SPACE TELESCOPE SCIENCE INSTITUTE addr_1: HOMEWOOD CAMPUS city: BALTIMORE state: MD zip: 21218 country: USA phone: (301) 338-4804 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC1851 descr_1: GLOBULAR CLUSTER WITH CORE RADIUS=5.9" pos_1: RA=5H 12M 28.03S +/- 0.7", pos_2: DEC=-40D 06' 11.4" +/- 0.7" equinox: 1950 fluxnum_1: 1 fluxval_1: F(1500)=2.5 E-15 fluxnum_2: 2 fluxval_2: SURF(V)=14.7 ! targnum: 5 name_1: NGC6205 name_2: M13 descr_1: G.C. WITH CORE=46" pos_1: RA=16H 39M 53.28S +/- 1", pos_2: DEC=+36D 33' 11.5" +/- 1" equinox: 1950 fluxnum_1: 1 fluxval_1: SURF(V)=16.7 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE PC1 targname: # config: PC opmode: IMAGE aperture: ALL sp_element: F230W num_exp: 1 time_per_exp: 250S priority: # param_1: CR-SPLIT=0.1, param_2: PRE-FLASH=YES ! linenum: 2.000 sequence_1: DEFINE PC2 targname: # config: PC opmode: IMAGE aperture: ALL sp_element: F336W num_exp: 1 time_per_exp: 130S priority: # param_1: CR-SPLIT=0.1, param_2: PRE-FLASH=YES req_1: GROUP 2-3 WITHIN 15D; ! linenum: 3.000 sequence_1: ^ targname: # config: ^ opmode: ^ aperture: ^ sp_element: F547M num_exp: ^ time_per_exp: 100S priority: # param_1: ^ comment_1: THE PC ACQUISITION ASSUMES AN comment_2: ASTROMETRIC CALIBRATION OF comment_3: THE PC WITH 0".03 ACCURACY. ! linenum: 10.000 sequence_1: USE PC2 targname: NGC1851 priority: 1 req_2: GUID TOL 0.020"; req_3: CYCLE 0 ! linenum: 16.000 sequence_1: USE PC2 targname: NGC6205 priority: 2 req_2: GUID TOL 0.020"; req_3: CYCLE 0 ! linenum: 17.000 sequence_1: USE PC1 targname: NGC1851 priority: 1 req_2: GUID TOL 0.020"; req_3: CYCLE 0 ! linenum: 18.000 sequence_1: USE PC1 targname: NGC6205 priority: 2 req_2: GUID TOL 0.020"; req_3: CYCLE 0 ! ! end of exposure logsheet ! No scan data records found