! $Id: 5421,v 4.1 1994/07/27 17:46:02 pepsa Exp $ coverpage: title_1: ABUNDANCES OF VERY HEAVY ELEMENTS IN THE EARLY GALAXY: title_2: CYCLE4 MEDIUM sci_cat: COOL STARS sci_subcat: CHEMICAL ABUNDANCES proposal_for: GO pi_fname: JOHN pi_mi: J. pi_lname: COWAN pi_inst: UNIVERSITY OF OKLAHOMA pi_country: USA pi_phone: 405-325-3961 hours_pri: 13.40 num_pri: 1 hrs: Y off_fname: CHERYL off_lname: PATTON off_title: SPONS. PROG. COORD. off_inst: 3065 off_addr_1: OFFICE OF RESEARCH ADMINISTRATION off_addr_2: 1000 ASP AVENUE, ROOM 314 off_addr_3: UNIVERSITY OF OKLAHOMA off_city: NORMAN off_state: OK off_zip: 730190430 off_country: USA off_phone: 405-325-4757 ! end of coverpage abstract: line_1: We propose to search for spectral lines indicating the presence line_2: of the very heavy elements platinum, iridium, bismuth and osmium line_3: in the very old, metal-poor halo giant HD 122563, line_4: and to determine the relative abundances line_5: of these elements. These elements, synthesized in stellar line_6: interiors by r(apid) and s(low) neutron line_7: capture processes, have never before been detected in metal-poor line_8: stars because their only strong lines lie in the ultraviolet line_9: spectral region. The abundances of these r- and s-process line_10: nucleosynthesis products in halo stars will serve to provide line_11: important constraints both on the early history and chemical line_12: evolution of the Galaxy and, indirectly, on the age of the line_13: Galaxy and the universe. ! ! end of abstract general_form_proposers: lname: COWAN fname: JOHN mi: J. inst: UNIVERSITY OF OKLAHOMA country: USA ! lname: SNEDEN fname: CHRISTOPHER inst: UNIVERSITY OF TEXAS country: USA ! lname: TRURAN fname: JAMES mi: W. inst: UNIVERSITY OF CHICAGO country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will measure the abundances of the heavy r-process elements line_2: Os,Ir, Pt and the s-process element Bi in extreme Population II line_3: stars in an attempt to understand more about the early history line_4: of the Galaxy. Specifically, we will obtain spectra for all line_5: four of these elements, which have spectral lines in the line_6: ultraviolet, with wavelengths near 3000 A. We have chosen a very line_7: metal-poor halo giant for observations with the HST: HD 122563. line_8: This star is the brightest very metal-poor ([Fe/H] = -2.7) star line_9: in the sky, and has been analyzed repeatedly with visual line_10: wavelength spectra (see Sneden and Parthasarathy 1983, Ap. J., line_11: 257, 757). It is the halo star with the most completely determined line_12: heavy element abundance distribution. It has (roughly) a solar line_13: content relative to Fe of the lighter neutron capture element line_14: group Sr-Y-Zr, but severe-to-moderate deficiencies in the heavier line_15: Ba-...-Dy group. Additionally, the s-process elements such as line_16: Ba are much more depleted than are the r-process elements line_17: such as Eu. ! question: 3 section: 2 line_1: Finally, abundances will be derived by syntheses of the spectra line_2: obtained with the HST. The model atmospheres employed for the line_3: stars will be those adopted by Gratton and Sneden (1991a). line_4: Particular attention will be paid to the abundances of ordinary line_5: metals (e. g. Fe, Ni, Ti) determined from the new uv spectra. line_6: These abundances must agree, within observation and analysis errors, line_7: to the abundances derived from the (easily analyzed) visual line_8: wavelength spectra already on hand. Then the abundances determined line_9: from the analysis of the Pt, Ir, Os and Bi features will be line_10: compared to the abundances of the ordinary metals to ascertain line_11: the degree of enrichment of the exotic very heavy elements. line_13: We already have predicted the approximate expected strengths for line_14: the Os I, Ir I, Pt I and Bi I lines. Adopting a) model atmosphere line_15: parameters from Gilroy et al. (1988), b) recent published line_16: oscillator strengths for the lines, and c) predicted abundance line_17: ratios for these elements with respect to Ba and Eu from r-process line_18: synthesis calculations or from the solar system r-process fractions, line_19: we predict that the Pt I lines will have equivalent widths of line_20: about 20 mA, or log (W/lambda) ~ -5.2 . The Ir I, Os I and Bi I line_21: equivalent widths should be about 10 mA, or log (W/lambda) ~ -5.5 . line_22: Therefore the lines of these 4 elements should be easily seen line_23: with the high resolutions to be employed here. ! question: 4 section: 1 line_1: We wish to use the High Resolution Spectrograph to obtain very high line_2: resolution spectra of Pt, Ir, Os and Bi. Only low excitation line_3: transitions of the neutral species of each element have detection line_4: possibilities, for the singly ionized transitions are either line_5: extremely weak or are located too far in the ultraviolet. None line_6: of the neutral species under study here have strong lines line_7: redward of 3064A and thus they are totally inaccessible from line_8: ground-based observations. We have limited our transition search line_9: to wavelengths between 2700 A and 3100 A, for our K-giant stars line_10: simply do not have enough flux in the farther UV to permit HST line_11: high resolution observations. We have chosen the following line_12: regions for our integrations: 1) 3059A (Os I), 3065A (Pt I), line_13: 3025A (Bi I); 2) 2925A (Ir I), 2930A (Pt I), 2898A (Bi I); and line_14: 3) 2998A (Pt I), 3025A (Bi I). line_16: We will use the SSA, grating 270M, and 4 substeps per diode line_17: to achieve an ultimate resolution of 50,000 while capturing line_18: about 45A of spectrum per integration. The resolution requirement line_19: is due to the crowded spectral region near 3000 A in these stars, line_20: and the spectral coverage requirement, aside from increasing the line_21: number of candidate lines available per integration, will aid line_22: considerably in the setting of continua for our spectrum syntheses. ! question: 5 section: 1 line_1: NONE ! question: 6 section: 1 line_1: NONE ! ! question: 8 section: 1 line_1: NONE ! question: 9 section: 1 line_1: #3880, (Cycle 3) "CIRCUMSTELLAR AND INTERSTELLAR ABSORPTION LINES IN line_2: PLANETARY NEBULAE CENTRAL STARS", H. Dinerstein, L. Danly, S. Heap, line_3: C. Sneden. This project is unrelated to the present proposal. line_4: The data are still being gathered for this project. ! question: 10 section: 1 line_1: We will provide graduate students to assist in data reduction; line_2: some financial support is requested for these students. We will line_3: provide some computer services for initial data analysis. line_4: Funds are requested to purchase a small workstation to enable us to line_5: process the data at a faster rate and to do analyses not possible line_6: on the heavily subscribed department computers. We will also line_7: provide secretarial support for preparing manuscripts for line_8: publication and any graphics support required. ! !end of general form text general_form_address: lname: COWAN fname: JOHN mi: J. category: PI inst: UNIVERSITY OF OKLAHOMA addr_1: DEPARTMENT OF PHYSICS AND ASTRONOMY addr_2: 440 WEST BROOKS city: NORMAN state: OK zip: 73019 country: USA phone: 405-325-3961 telex: COWAN@PHAST.NHN.UOKNOR.EDU ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD122563 name_2: HR5270 descr_1: A,185,140 pos_1: RA = 14H 0M 4.55S +/- 0.01S, pos_2: DEC = +09D 55' 38.80" +/- 0.15" equinox: 1950 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_val: -0.013400 dec_pm_val: -0.0660 rv_or_z: V = -24.7 comment_1: THE CONTINUUM FLUX ESTIMATE AT comment_2: 2650A IS A LOWER LIMIT TO THIS comment_3: STAR'S FLUX PUBLISHED BY GUSTAFSSON comment_4: ET AL. (1980, A&A, 89, 255); THE comment_5: FLUX AT 3000A IS AN INTERPOLATION comment_6: BETWEEN THE 2650A FLUX AND THE "U" comment_7: BANDPASS FLUX. fluxnum_1: 1 fluxval_1: V = 6.20 fluxnum_2: 2 fluxval_2: B-V = +0.90 fluxnum_3: 3 fluxval_3: U-B = +0.38 fluxnum_4: 4 fluxval_4: F-CONT(2650) = 5 E-13 fluxnum_5: 5 fluxval_5: F-CONT(3000) = 1.5 E-12 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HD122563 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 4.5S fluxnum_1: 1 fluxnum_2: 4 fluxnum_3: 5 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 4; ONBOARD ACQ FOR 2.0 comment_1: STEP_TIME=0.5S; EXPECT 15000 comment_2: COUNTS IN STEP-TIME TARGET IS comment_3: METAL-POOR, SO UV MAGS ARE comment_4: SLIGHTLY UNCERTAIN ! linenum: 2.000 targname: HD122563 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 25S fluxnum_1: 1 fluxnum_2: 4 fluxnum_3: 5 priority: 1 param_1: SEARCH-SIZE=5 req_1: CYCLE 4; ONBOARD ACQ/PEAKUP FOR 3.0 comment_1: STEP-TIME=1.0S ! linenum: 3.000 targname: HD122563 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 3060 num_exp: 8 time_per_exp: 1200S s_to_n: 70 s_to_n_time: 2400S fluxnum_1: 1 fluxnum_2: 4 fluxnum_3: 5 priority: 1 param_1: STEP-PATT=3 param_2: FP-SPLIT=STD param_3: STEP-TIME=0.2 param_4: COMB=FOUR req_1: CYCLE 4; comment_1: TOTAL EXPOSURE=9600S--BREAK UP TO comment_2: AVOID DRIFT DUE TO GIMP; S/N IS PER comment_3: SUBSTEP; WANT HIGH S/N IN EACH comment_4: SUBSTEP FOR DECONVOLUTION. ! linenum: 4.000 targname: HD122563 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 4.5S fluxnum_1: 1 fluxnum_2: 4 fluxnum_3: 5 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 4; ONBOARD ACQ FOR 5.0 comment_1: STEP_TIME=0.5S; EXPECT 15000 comment_2: COUNTS IN STEP-TIME TARGET IS comment_3: METAL-POOR, SO UV MAGS ARE comment_4: SLIGHTLY UNCERTAIN ! linenum: 5.000 targname: HD122563 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 25S fluxnum_1: 1 fluxnum_2: 4 fluxnum_3: 5 priority: 1 param_1: SEARCH-SIZE=5 req_1: CYCLE 4; ONBOARD ACQ/PEAKUP FOR 6.0 comment_1: STEP-TIME=1.0S ! linenum: 6.000 targname: HD122563 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2915 num_exp: 8 time_per_exp: 1200S s_to_n: 70 s_to_n_time: 2400S fluxnum_1: 1 fluxnum_2: 4 fluxnum_3: 5 priority: 1 param_1: STEP-PATT=3 param_2: FP-SPLIT=STD param_3: STEP-TIME=0.2 param_4: COMB=FOUR req_1: CYCLE 4; comment_1: TOTAL EXPOSURE=9600S--BREAK UP TO comment_2: AVOID DRIFT DUE TO GIMP; S/N IS PER comment_3: SUBSTEP; WANT HIGH S/N IN EACH comment_4: SUBSTEP FOR DECONVOLUTION. ! linenum: 7.000 targname: HD122563 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 4.5S fluxnum_1: 1 fluxnum_2: 4 fluxnum_3: 5 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 4; ONBOARD ACQ FOR 8.0 comment_1: STEP_TIME=0.5S; EXPECT 15000 comment_2: COUNTS IN STEP-TIME TARGET IS comment_3: METAL-POOR, SO UV MAGS ARE comment_4: SLIGHTLY UNCERTAIN ! linenum: 8.000 targname: HD122563 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 25S fluxnum_1: 1 fluxnum_2: 4 fluxnum_3: 5 priority: 1 param_1: SEARCH-SIZE=5 req_1: CYCLE 4; ONBOARD ACQ/PEAKUP FOR 9.0 comment_1: STEP-TIME=1.0S ! linenum: 9.000 targname: HD122563 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 3010 num_exp: 8 time_per_exp: 1200S s_to_n: 70 s_to_n_time: 2400S fluxnum_1: 1 fluxnum_2: 4 fluxnum_3: 5 priority: 1 param_1: STEP-PATT=3 param_2: FP-SPLIT=STD param_3: STEP-TIME=0.2 param_4: COMB=FOUR req_1: CYCLE 4; comment_1: TOTAL EXPOSURE=9600S--BREAK UP TO comment_2: AVOID DRIFT DUE TO GIMP; S/N IS PER comment_3: SUBSTEP; WANT HIGH S/N IN EACH comment_4: SUBSTEP FOR DECONVOLUTION. ! linenum: 10.000 targname: HD122563 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 4.5S fluxnum_1: 1 fluxnum_2: 4 fluxnum_3: 5 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 4; ONBOARD ACQ FOR 11.0 comment_1: STEP_TIME=0.5S; EXPECT 15000 comment_2: COUNTS IN STEP-TIME TARGET IS comment_3: METAL-POOR, SO UV MAGS ARE comment_4: SLIGHTLY UNCERTAIN ! linenum: 11.000 targname: HD122563 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 25S fluxnum_1: 1 fluxnum_2: 4 fluxnum_3: 5 priority: 1 param_1: SEARCH-SIZE=5 req_1: CYCLE 4; ONBOARD ACQ/PEAKUP FOR 12.0 comment_1: STEP-TIME=1.0S ! linenum: 12.000 targname: HD122563 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2833 num_exp: 6 time_per_exp: 1200S s_to_n: 60 s_to_n_time: 1800S fluxnum_1: 1 fluxnum_2: 4 fluxnum_3: 5 priority: 1 param_1: STEP-PATT=3 param_2: FP-SPLIT=STD param_3: STEP-TIME=0.2 param_4: COMB=FOUR req_1: CYCLE 4; comment_1: TOTAL EXPOSURE=7200S--BREAK UP TO comment_2: AVOID DRIFT DUE TO GIMP; S/N IS PER comment_3: SUBSTEP; WANT HIGH S/N IN EACH comment_4: SUBSTEP FOR DECONVOLUTION. ! ! end of exposure logsheet ! No scan data records found