! File: 3210C.PROP ! Database: PEPDB ! Date: 18-FEB-1994:22:03:16 coverpage: title_1: R136 G160M CYCLE 2 sci_cat: INTERSTELLAR MEDIUM proposal_for: GTO/HRS cont_id: 1188 pi_title: DR. pi_fname: DENNIS pi_mi: C. pi_lname: EBBETS pi_inst: BALL AEROSPACE SYSTEMS pi_country: USA pi_phone: (303) 939-5964 keywords_1: ABSORPTION LINE SYSTEM, IGM hours_pri: 2.84 num_pri: 1 hrs: Y time_crit: Y pi_position: PRIN MEM TECH STAFF ! end of coverpage abstract: line_1: This is a new proposal submitted in March, 1992 to define line_2: GHRS medium resolution spectra (G160M) of R136 for the purpose line_3: of observing interstellar N V absrption lines in the LMC and line_4: the MW halo. It is based on exposure lines extracted from the line_5: previous cycle 2 proposal, modified now to account for the loss line_6: of all side 1 capabilities, and the denial of augmentation time. line_7: The observation contains an onboard acquisition, several image line_8: mode maps, a wavecal with SC2 and LSA spectra at a central line_9: wavelength of 1250. The orientation of the HST is specified to line_10: cause the brightest components to align with the long axis of the line_11: science diodes, minimizing the spatial smearing of the data. line_12: REVISION HISTORY: 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 line_16: Revised for cycle 1 exposures February 09, 1991 line_17: Revised for cycles 2-5 May 22, 1991 line_18: Revised for cycle 2 only March 4, 1992 line_19: This proposal uses baseline GTO time only. ! ! 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: Cycle 2 baseline time: line_2: R136A LSA G160M 1250 S/N=45 line_3: step-patt=2 2 samples per diode width line_4: comb=four (def), fp-split=std (4) line_5: 12 subexposures, 5.33 minutes each line_6: should get 2000 cts/diode in each bin in continuum line_7: orient to align brightest components with diodes line_8: derive spatial distribution of stars from N2 images line_9: construct PSF from FOC image of single star line_10: deconvolve to enhance spectral resolution line_11: Onboard Acq should use standard search with faint limit line_12: Return to brightest point is not required. ! question: 4 section: 1 line_1: R136 is the brightest object in the LMC. The interstelar line_2: spectrum provides information about the entire line of sight, line_3: including our Milky Way galaxy and halo, the LMC halo and line_4: general interstellar environment, the 30 Doradus region, and line_5: the environment in the immediate vicinity of the R136 line_6: cluster. Nitrogen V is a good tracer of very hot gas, but line_7: its resonance lines are only accessible in the UV near 1240. line_8: These GHRS medium resolution spectra will be of higher line_9: spectral resolution and signal to noise ratio that was line_10: possible with IUE, or the existing ow resolution GHRS spectra line_11: obtained in cycle 0. ! question: 5 section: 1 line_1: Basic requirement was to get roughly 2000 cts/diode in each line_2: of two spectral bins. This S/N will show good detail in ISM line_3: absorption lines, and should allow at least some enhancement line_4: using deconvolution. The LSA is used because the count rate line_5: with the SSA would be too low to get decent S/N without a line_6: very long exposure. The flux at 1250 was derived from the line_7: cycle 0 G140L LSA exposure. The G160M sensitivity was derived line_8: from the inflight SV calibration. Sixty four minutes of total line_9: exposure time is required. This is broken into 5 minute sub- line_10: exposures to minimize magnetic and thermal drifts. The N2 line_11: maps are included to verify proper centering in the LSA, and line_12: allow construction of a line spread function by combining the line_13: observed spatial distribution and relative brightnesses of line_14: components of R136 with the FOC UV PSF of a single star. An line_15: onboard acq with a double locate is expected to be successful line_16: based on the observed initial pointing accuracy and N2 count line_17: rate from the cycle 0 observations. ! question: 6 section: 1 line_1: R136 is a tight cluster with nearly 60 stars visible in the line_2: LSA. The 6 brightest components contribute over 53% of the line_3: total light. They are arranged in such a way that 5 of them line_4: can be made to lie parallel to the long dimension of the line_5: science diodes with a judicious orientation of the aperture. line_6: I estimate that a line running 45 - 225 degrees measured line_7: north through east will give the best alignment. When this is line_8: added to the 45 degree GHRS orientation to U3, it gives the line_9: specified 90 degrees orientation requested. An orientation of line_10: 270 would be fine also. The tolerance +/- 10 degrees was line_11: calculated to place the most distant component R136A6 no more line_12: than 1/2 science diode width from the optimum alignment. This line_13: special orientation will minimize the broadening of the line_14: spectrum due to the spatial distribution of the stars, and line_15: provide the best possible spectral resolving power while line_16: still allowing use of the LSA, and its much more favorable line_17: count rate and exposure time. ! question: 7 section: 1 line_1: The spectra will be calibrated and reduced using IDT facility line_2: at GSFC, University of Wisconsin and Ball Aerospace. An exact line_3: wavelength calibration will be derived from the SC2 wavecal. line_4: The 12 subexposures will be aligned and combined to minimize line_5: smearing from thermal or magnetic drifts. The spectra will be line_6: corrected for scattered light and rectified to a flat line_7: continuum. We will derive a line spread function for this line_8: observation, and attempt to enhance the resolution using line_9: block-iterative, Lucy and Jansson deconvolution algorithms. line_10: Features visible in the raw data, and for which the three line_11: techniques agree will be regarded as confident detections. line_12: All interstellar lines in the recorded region will line_13: be identified, analyzed for velocity components and structure, line_14: equivalent widths and profiles. ! question: 8 section: 1 line_1: This proposal reflects GHRS team Baseline GTO observing time line_2: for cycle 2 only. ! question: 9 section: 1 line_1: Ebbets and Savage developed, executed and helped analyze line_2: virtually all of the GHRS proposals for the Science Verific- line_3: cation, Science Assessment and Early Release Observations. line_4: R136 was also observed in cycle 0 in proposal 1188. Early line_5: results were presented at the Atlanta AAS meeting, and in an line_6: upcoming Ap.J. Letter. ! question: 10 section: 1 line_1: Computer facilities, research assistants, travel ! !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: R136A name_2: HD38268 descr_1: G,515,517,H,503,515,517 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: G140L OBSERVATIONS IN CYCLE 0. comment_5: GS PLATE ID = 06B0 fluxnum_1: 1 fluxval_1: V = 10.1 fluxnum_2: 2 fluxval_2: F-CONT(1250) = 8.0 E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 10.000 targname: R136A config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 5.0S s_to_n: 50 fluxnum_1: 1 priority: 1 param_1: FAINT=8000, param_2: BRIGHT=65535, param_3: SEARCH-SIZE=5, req_1: ONBOARD ACQ FOR 20-80; req_2: CYCLE 2 /10-80; req_3: SEQ 10-80; req_4: ORIENT 90D +/- 10D / 10-80; comment_1: ORIENTATION OF 270 +/- 10D comment_2: WOULD ALSO BE ACCEPTABLE comment_3: STEP-TIME = 0.2 SECONDS ! linenum: 20.000 targname: R136A config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 20.4S s_to_n: 50 fluxnum_1: 1 priority: 1 comment_1: STEP-TIME = .2 SECOND ! linenum: 30.000 targname: R136A config: HRS opmode: IMAGE aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 96.8S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: NX=22, param_2: NY=22, ! linenum: 40.000 targname: R136A config: HRS opmode: IMAGE aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 242S s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: NX=22, param_2: NY=22, param_3: DELTA-X=2, param_4: DELTA-Y=2 ! linenum: 50.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1250 num_exp: 1 time_per_exp: 64.0S s_to_n: 25 priority: 1 param_1: STEP-PATT=2, req_1: CALIB FOR 60; req_2: SEQ 50-70 NO GAP; ! linenum: 60.000 targname: R136A config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1250 num_exp: 3 time_per_exp: 1280.0S s_to_n: 45 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=2, param_2: FP-SPLIT=STD, ! linenum: 70.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1250 num_exp: 1 time_per_exp: 64.0S s_to_n: 25 priority: 1 param_1: STEP-PATT=2, req_1: CALIB FOR 60; ! linenum: 80.000 targname: R136A config: HRS opmode: IMAGE aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 96.8S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: NX=22, param_2: NY=22, ! ! end of exposure logsheet ! No scan data records found