! File: 1188C.PROP ! Database: PEPDB ! Date: 16-FEB-1994:05:14:48 coverpage: title_1: UV SPECTROSCOPY OF THE COMPONENTS OF R136 -- CYCLE 0 sci_cat: STELLAR ASTROPHYSICS proposal_for: GTO/HRS pi_title: DR. pi_fname: DENNIS pi_mi: C. pi_lname: EBBETS pi_inst: BALL AEROSPACE CORPORATION pi_country: USA pi_phone: (303) 939-5964 keywords_1: SUPERGIANT STAR, WOLF-RAYET STAR, MASS LOSS, LMC 30 keywords_2: DORADUS hours_pri: 7.80 num_pri: 9 realtime: X pi_position: PRIN MEM TECH STAFF ! end of coverpage abstract: line_1: R136 is the bright central object of the 30 Doradus nebula in the LMC. It line_2: contains an unusually tight grouping of very massive and luminous O and line_3: Wolf-Rayet type stars. The brightest recognizeable component, called R136A1, line_4: may be an unresolved group of several stars, or may be a single object line_5: with a mass of order 800 Mo. Detailed studies of the individual components line_6: have been hampered by a lack of sufficient spatial resolution. The High line_7: Resolution Spectrograph will be used to obtain detailed ultraviolet spatial and line_8: spectral information about the five or so brightest discrete components. The line_9: goal of the program is to study the spectral morphology, stellar wind line_10: characteristics, ultraviolet luminosities and ultimately the masses included line_11: in this unusual and interesting object. line_13: redlined for phase 2, 7/19/88, dce line_14: updated for cycle 1 phase 2 9/21/89 line_15: revised lines 1-7 for cycle zero 11/15/90 ! ! end of abstract general_form_proposers: lname: SAVAGE fname: BLAIR mi: D. inst: WISCONSIN, UNIVERSITY OF country: USA ! lname: EBBETS fname: DENNIS mi: C. inst: BALL AEROSPACE CORPORATION country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: There are three sets of observations in this program. The first consists of line_2: multiple observations of R136a1, obtained with grating configuration G140L, line_3: spaced over the 2 1/2 years of the GTO period. The purpose is to investigate line_4: the possibility of spectrum variablity with very high quality data. The second line_5: set consists of spectra of the other compnents of R136. We plan to observe line_6: R136a2, R136b, and R136c, also with G140L. Time is also allocated for an line_7: observation of the "fuzz", which shows an O type optical spectrum. The line_8: objective is to study in detail the spectra of each discrete component, using line_9: the spatial resolution povided by the HRS small science aperture. The third line_10: set of observations will study the profiles of selected stellar and line_11: interstellar lines in the brightest component, R136a1, using the HRS medium line_12: resolution grating G160M. The prominent stellar wind lines of OV, CIV, HeII and line_13: NIV will be observed, along with photospheric FeV, interstellar SiIV, and other line_14: interstellar components in the spectral regions observed. line_16: Cycle 0: Exposures 1-7 1.09 hours priority=2 line_17: Cycle 1: Exposures 12-22, 26-30 2.39 hours priority=2 line_18: Cycle 2: Exposures 32.5-40 2.83 hours priority=1,2 line_19: Cycle 3: Exposures 41-45, 23-25, line_20: 45.5-53 1.49 hours priority=2,3 line_21: Total = 7.80 hours ! question: 4 section: 1 line_1: R136 has been studied extensively from the ground with imagery and line_2: spectroscopy. Over a dozen observations have been made with the IUE. Much has line_3: been learned from these studies, but all have been ultimately limited by the line_4: finite spatial resolution allowed by the atmosphere and the instruments. ST line_5: will produce images (not part of this proposal) with much finer spatial line_6: resolution, and will provide vastly superior data related to the number, line_7: distribution and nature of the components. The HRS will have the spatial line_8: resolution, sensitivity and spectral resolving power to provide high quality line_9: ultraviolet spectra of each component. ! question: 5 section: 1 line_1: R136 is a very crowded field. Successful completion of this program requires line_2: that the component being observed be precisely centered in the 0.25 arc sec line_3: aperture. We request real time target acquisition capability, to ensure that line_4: the centering is adequate, and to make adjustments to the pointing if line_5: necessary. The basic capablility for acquiring targets in complex fields should line_6: have been developed during SV, using R136 as a verification target. line_7: See SV tests HRS-04 "HRS Spiral Search Pattern" line_8: and HRS-06 "Mode I Target Acquisition With HRS Maps. ! question: 7 section: 1 line_1: The spectra will be calibrated and reduced using standard procedures either in line_2: RSDP, or the IDT facilities. The time series on R136a1 will be carefully line_3: examined for variability, particularly in the CIV and HeII stellar wind lines. line_4: The spectra of all components will be studied in terms of gross spectral line_5: morphologhy, for the purposes of classification. Stellar wind diagnostics such line_6: as terminal velocities and mass loss rates will be derived from comparison of line_7: line profiles with model predictions and experience with similar stars. The line_8: ultraviolet spectral energy distributions will be studied by correcting for now line_9: known effects of galactic and LMC extinction. Profiles, equivalent widths and line_10: velocity components of interstellar lines will be derived from the medium line_11: resoultion observations. ! question: 8 section: 1 line_1: The ability to acquire point source targets in complex fields, including the line_2: use of HRS field maps, must have been verified and perfected before these line_3: observations can proceed. Similarly, the ability to execute small offset line_4: maneuvers to sequentially observe a number of close targets must have been line_5: verified. ! question: 9 section: 1 line_1: Both Ebbets and Savage are involved in several GTO programs. ! question: 10 section: 1 line_1: Data reduction and analysis facilities, part time research assistant, line_2: manuscript preparation, publication costs, travel expenses. ! question: 12 section: 1 line_1: The observations of R136a1 should be scheduled at three widely spaced line_2: intervals. line_5: SV Prerequisites line_6: HRS 05.3 Mode II Target Acquisition - offet or functional equivalent line_7: HRS 06 Mode I Target Acquisition with HRS Maps line_8: HRS 08 HRS Low Resolution Calibration ! question: 13 section: 1 line_1: The High Resolution Spectrograph will be used to observe the UV spectrum of line_2: the bright components of R136. The brightest member, R136a1 will be observed 4 line_3: times to search for variability over a 2 1/2 period. All other componets wil be line_4: observed once. Several prominent stellar wind lines, and a few important line_5: interstellar regions will be observed with the medium resolution R=20000 line_6: grating. ! !end of general form text general_form_address: lname: SAVAGE fname: BLAIR mi: D. category: CON inst: UNIVERSITY OF WISCONSIN addr_1: DEPARTMENT OF ASTRONOMY addr_2: 475 N. CHARTER ST. city: MADISON state: WI zip: 53706 country: USA phone: (608) 262-4909 ! lname: EBBETS fname: DENNIS mi: C. title: DR. category: PI inst: BALL AEROSPACE SYSTEMS GROUP addr_1: GHRS PROJECT AR-1 addr_2: P.O. BOX 1062 city: BOULDER state: CO zip: 80306 country: USA phone: (303) 939-5964 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: R136A1 name_2: HD38268 descr_1: BRIGHTEST COMPONENT OF R136 pos_1: RA = 5H 38M 42.50S +/- 0.1S, pos_2: DEC = -69D 06' 02.8" +/- 1" equinox: 2000 pm_or_par: NO acqpr_1: COMP comment_1: POSITION FROM PC IMAGE MEASURED comment_2: BY ARCHIE BETWEEN A1 AND A2 comment_3: UV CONTINUUM FLUXES ESTIMATED FROM comment_4: IUE OBSERVATIONS OF TOTAL FLUX AND comment_5: RATIOS OF COMPONENT BRIGHTNESSES IN comment_6: VISIBLE LIGHT. comment_7: GS PLATE ID = 06B0 fluxnum_1: 1 fluxval_1: V = 10.1 fluxnum_2: 2 fluxval_2: F-CONT(1500) = 6.2 E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: R136A1 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1325S fluxnum_1: 1 priority: 2 param_1: SEARCH-SIZE=5 req_1: INT ACQ FOR 2-7; req_3: CYCLE 0 / 1-7; req_4: SEQ 1-7 NO GAP; comment_2: EARLY ACQ FOR 12,32.5,41; ! linenum: 2.000 targname: R136A1 config: HRS opmode: IMAGE aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 96.8S fluxnum_1: 1 priority: 2 ! linenum: 3.000 targname: R136A1 config: HRS opmode: IMAGE aperture: 2.0 sp_element: MIRROR-N1 num_exp: 1 time_per_exp: 484S fluxnum_1: 1 priority: 2 ! linenum: 4.000 targname: R136A1 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1200 num_exp: 2 time_per_exp: 10M s_to_n: 50 fluxnum_1: 2 priority: 2 param_1: STEP-PATT=2, param_2: FP-SPLIT=STD, ! linenum: 5.000 targname: R136A1 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1450 num_exp: 1 time_per_exp: 10M s_to_n: 50 fluxnum_1: 2 priority: 2 param_1: STEP-PATT=2, param_2: FP-SPLIT=STD, ! linenum: 6.000 targname: R136A1 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1700 num_exp: 2 time_per_exp: 8M s_to_n: 50 fluxnum_1: 2 priority: 2 param_1: STEP-PATT=2, param_2: FP-SPLIT=STD, ! linenum: 7.000 targname: R136A1 config: HRS opmode: IMAGE aperture: 2.0 sp_element: MIRROR-N1 num_exp: 1 time_per_exp: 484S fluxnum_1: 1 priority: 2 ! ! end of exposure logsheet ! No scan data records found