! File: 4318C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:21:39:35 coverpage: title_1: THE INTERSTELLAR ABUNDANCE OF GERMANIUM AND KRYPTON title_2: CYC3SUPP sci_cat: INTERSTELLAR MEDIUM sci_subcat: ABSORPTION LINES proposal_for: GO pi_fname: JASON pi_mi: A. pi_lname: CARDELLI pi_inst: UNIVERSITY OF WISCONSIN pi_country: USA hours_pri: 3.05 num_pri: 2 hrs: Y funds_length: 24 off_fname: ROBERT off_mi: W. off_lname: ERICKSON off_title: ADMINISTRATOR off_inst: 3884 off_addr_1: 750 UNIVERSITY AVENUE off_city: MADISON off_state: WI off_zip: 53706 off_country: USA off_phone: 608-262-3822 ! end of coverpage abstract: line_1: Elemental abundances and the enrichment of interstellar gas are a line_2: strong function of the processes associated with the broad spectrum line_3: of stellar evolution. Stellar evolution theory predicts that line_4: specific elements can have dramatically different nucleosynthetic line_5: histories and so studying the gas phase abundances of such elements line_6: in both the Milky Way and other galaxies provides important line_7: information on both stellar and subsequently galactic evolution. We line_8: propose to study the abundances of the heavy elements Ge (Z = 32) line_9: and Kr (Z = 36) toward six stars representing three distinctly line_10: different galactic directions. These elements represent a) the line_11: heaviest elements studied in the ISM to date and b) nucleosynthetic line_12: origins uniquely different from any element yet studied in the ISM. line_13: Greater than 95% of the 'cosmic' abundance of Ge and Kr derive line_14: from a combination of the s- and r-process. Compare this with line_15: Zn (Z=30), traditionally the heaviest element studied in the ISM, line_16: for which greater than 88% of the cosmic abundance derives from line_17: 'Fe-peak' nucleosynthesis. ! ! end of abstract general_form_proposers: lname: CARDELLI fname: JASON title: PI mi: A. inst: UNIVERSITY OF WISCONSIN country: USA ! lname: MEYER fname: DAVID mi: M. inst: NORTHWESTERN UNIVERSITY country: USA esa: N ! lname: SAVAGE fname: BLAIR mi: D. inst: UNIVERSITY OF WISCONSIN country: USA esa: N ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The goals of this proposal are to obtain high signal-to-noise data line_2: of the region centered around 1240 A for the purpose of determining line_3: accurate IS abundances for the heavy elements Kr and Ge toward 2 stars. line_4: The single GHRS setup fo reach stars using grating G160M, a 4 sample line_5: per diode substep (STEP-PATT = 5), and FP-SPLIT=STD. We expect to line_6: achieve S/N values of about 660 PER SUBSTEP (sample). Because of the line_7: large total counts desired, we have broken each exposure into multiples line_8: avoid overlfowing the onboard accumulator limits of 65,500 cts (note line_9: that the acutual number of readouts is the product of no. expsoures line_10: x no. fp-split = 16 (a readout is done after each of the four line_11: fp-splits)). This will give us approximately 28000 cts per substep line_12: (accum. bin), well below the roll-over value. ! !end of general form text general_form_address: lname: CARDELLI fname: JASON mi: A. category: PI inst: University of Wisconsin addr_1: DEPARTMENT OF ASTRONOMY addr_2: 475 N. CHARTER STREET city: MADISON state: WI zip: 53706 country: USA phone: 608-262-7921 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: KAPPA-ORI name_2: HD38771 descr_1: B0.5 IA STAR pos_1: RA = 05H 45M 23.01S +/- 0.03S, pos_2: DEC = -09D 41' 9.45" +/- 0.5", equinox: 1950 pm_or_par: Y ra_pm_val: -0.003000 ra_pm_unct: 0.001000 dec_pm_val: -0.0050 dec_pm_unct: 0.0010 fluxnum_1: 1 fluxval_1: V=2.06, TYPE=B0.5 IA, fluxval_2: E(B-V)=0.07 ! targnum: 2 name_1: EPSILON-PER name_2: HD24760 descr_1: B0.5 V STAR pos_1: RA = 03H 54M 29.43S +/- 0.03S, pos_2: DEC = +39D 52' 2.54" +/- 0.5", equinox: 1950 pm_or_par: Y ra_pm_val: 0.017000 ra_pm_unct: 0.001000 dec_pm_val: -0.0240 dec_pm_unct: 0.0010 fluxnum_1: 1 fluxval_1: V=2.86, TYPE=B0.5 V, fluxval_2: E(B-V)=0.11 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: KAPPA-ORI config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=3, param_2: BRIGHT=RETURN, req_1: ONBOARD ACQ FOR 2; req_2: CYCLE 3 / 1-3 comment_1: STEP-TIME=0.2S ! linenum: 2.000 targname: KAPPA-ORI config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 20.4S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 3 comment_1: STEP-TIME=0.2S ! linenum: 3.000 targname: KAPPA-ORI config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1239 num_exp: 4 time_per_exp: 7.254M s_to_n: 660 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD, ! linenum: 4.000 targname: EPSILON-PER config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=3, param_2: BRIGHT=RETURN, req_1: ONBOARD ACQ FOR 5; req_2: CYCLE 3 / 4-6 comment_1: STEP-TIME=0.2S ! linenum: 5.000 targname: EPSILON-PER config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 20.4S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 6 comment_1: STEP-TIME=0.2S ! linenum: 6.000 targname: EPSILON-PER config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1239 num_exp: 4 time_per_exp: 9.067M s_to_n: 660 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD, ! ! end of exposure logsheet ! No scan data records found