! File: 2634C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:09:43:23 coverpage: title_1: B AND BE AS PROBES OF COSMIC RAY SPALLATION AND STELLAR STRUCTURE sci_cat: STELLAR ASTROPHYSICS sci_subcat: STELLAR ATMOSPHERES proposal_for: GO pi_title: DR. pi_fname: DOUGLAS pi_mi: K. pi_lname: DUNCAN pi_inst: STSCI pi_country: USA pi_phone: 301-338-4935 keywords_1: DWARF, POPULATION II, COSMIC RAYS, HALO, STELLAR keywords_2: STRUCTURE, OPEN CLUSTER hours_pri: 4.20 num_pri: 5 hrs: Y funds_amount: 52498 funds_length: 12 funds_date: OCT-90 pi_position: HRS INSTR. SCIENTIST off_fname: PETER off_lname: STOCKMAN off_title: DIRECTOR off_inst: SPACE TELESCOPE SCIENCE INSTITUTE off_addr_1: 3700 SAN MARTIN DRIVE off_city: BALTIMORE off_state: MD off_zip: 21218 off_country: USA off_phone: 301-338-4935 ! end of coverpage abstract: line_1: I. We propose to observe Boron and Beryllium in one intermediate metallicity line_2: halo stars ([Fe/H]~-1.5) which appears to have formed at the time when the line_3: galaxy was just beginning to syntheize those two light elements through the line_4: spallation reactions of cosmic rays on C,N,O nuclei in the interstellar medium. line_5: The B and Be abundances and their ratio yield knowledge of the energetic line_6: particle flux at this epoch and on the time of formation of the halo, in the line_7: same way that the current interstellar medium light element abundances are used line_8: to constrain theories of present cosmic rays. line_9: II. We propose to observe B in two stars in the "Li gap," the mysterious line_10: narrow temperature range in F stars in which Li is depleted by more than an line_11: order of magnitude compared to stars just a few 100 K hotter or cooler. line_12: Knowledge of whether B is depleted in the same star should help decide whether line_13: turbulent diffusion, gravitational settling, or some other as yet unknown line_14: mixing process is responsible for the gap. ! ! end of abstract general_form_proposers: lname: SODERBLOM fname: DAVID title: DR. mi: R. inst: STSCI country: USA ! lname: DUNCAN fname: DOUGLAS title: P.I. mi: K. inst: STSCI country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Observations will be standard ACCUM mode GHRS spectra, line_2: using G270, SSA and ECH-B, LSA settings. Resolution line_3: will be about .03-.1 angstrom, S/N 45, adequate for spectum line_4: synthesis work. To assure adequate S/N, FP/SPLIT will line_5: be used. ! question: 4 section: 0 line_1: The B I line at 2498 ang. is not observable from the ground. line_2: The Be II line at 3130 ang. is only very marginally line_3: observable. A 5300 sec. exposure on a 4-m. telescope allowed line_4: an abundance measurement with error of 250 per cent. Since line_5: the present purpose is to derive the Be/B ratio as a test of line_6: cosmic ray models of the early galaxy, we need a much better line_7: measurement. That is why an HST spectrum is needed for the line_8: two halo stars. ! question: 5 section: 0 line_1: All long wavelength, low-res. IUE exposures ever taken line_2: of very metal poor and intermediate metal-poor stars were line_3: examined, as well as ones of a number of solar-metallicity line_4: stars. A grid was constructed of flux at 2500 ang. and line_5: 3130 ang. as a function of stellar temperature and metallicity, line_6: for stars with U mag. = 0. For each star, interpolation was line_7: made according to temp. and metal abundance, and fluxes line_8: scaled according to U magnitude. line_9: This computation, has now been updated mid-April, 1991 line_10: with the newest sensitivity curves and should be quite good. line_11: The S/N reached will only line_12: be 40-50, rather than 70, but should still be adequate. ! question: 6 section: 1 line_1: None. ! question: 7 section: 0 line_1: Initial reduction will be done at STScI by Duncan and line_2: Soderblom, using STSDAS, of course. line_3: Dave Lambert, an Observatory Scientist and GTO, has line_4: invited us to combine our observations with simlar line_5: ones he is doing with his GTO time, and to do the line_6: analysis together. All three of us have experience line_7: with spectrum synthesis. This work could be done line_8: either at the Univ. of Texas or at STScI. line_10: The eventual interpretation of the abundances in terms line_11: of theoretical models (e.g. gravitational settling) is line_12: more involved. Two groups, Michaud et al in Canada, and line_13: Vauclair et al in France perform such calculations. The line_14: calculations for B and Be in this temperature range have line_15: not yet been done, though with current interest they may line_16: be expected. One of us (DD) has an invitation to work line_17: with the French group on this problem. ! question: 10 section: 0 line_1: Normal access to STScI facilities. Only 7 spectra will be line_2: produced. Reduction will be under STSDAS. ! !end of general form text general_form_address: lname: DUNCAN fname: DOUGLAS mi: K. title: DR. category: PI inst: SPACE TELESCOPE SCIENCE INSTITUTE addr_1: 3700 SAN MARTIN DRIVE city: BALTIMORE state: MD zip: 21218 country: USA ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD84937 descr_1: STAR; SUBDWARF pos_1: RA = 09H 46M 12.283S +/- 0.06S, pos_2: DEC = +13D 59' 10.3" +/- 1.0" equinox: J1950 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 1959.23 ra_pm_val: 0.024067 ra_pm_unct: 0.001000 dec_pm_val: -0.7690 dec_pm_unct: 0.0150 an_prlx_val: 0.1000 an_prlx_unct: 0.0500 fluxnum_1: 1 fluxval_1: V = 8.32 fluxnum_2: 2 fluxval_2: B-V = 0.37 +/- 0.02,U-B = -0.20 +/- 0.03 fluxnum_3: 3 fluxval_3: F(3130) = 1.3 +/- 0.3 E-12 fluxnum_4: 4 fluxval_4: F(2500) = 0.86 +/- 0.1 E-12 ! targnum: 2 name_1: VB13 descr_1: STAR; OPEN CLUSTER pos_1: RA = 4H 10M 42.22S +/- 0.06S, pos_2: DEC = 18D 25' 24.2" +/- 1.0" equinox: J2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 1983.00 ra_pm_val: 0.007867 ra_pm_unct: 0.000667 dec_pm_val: -0.0350 dec_pm_unct: 0.0080 an_prlx_val: 0.1000 an_prlx_unct: 0.0500 fluxnum_1: 1 fluxval_1: V = 6.62 fluxnum_2: 2 fluxval_2: B-V = 0.43 +/- 0.01,U-B = -0.01 +/- 0.02 fluxnum_3: 3 fluxval_3: F(3130) = 4.8 +/- 0.8 E-12 fluxnum_4: 4 fluxval_4: F(2500) = 0.79 +/- 0.25 E-12 ! targnum: 3 name_1: VB14 descr_1: STAR; OPEN CLUSTER pos_1: RA = 4H 11M 20.08S +/- 0.06S, pos_2: DEC = 5D 31' 22.9" +/- 1.0" equinox: J2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 1982.90 ra_pm_val: 0.008933 ra_pm_unct: 0.000667 dec_pm_val: 0.0090 dec_pm_unct: 0.0100 an_prlx_val: 0.1000 an_prlx_unct: 0.0500 fluxnum_1: 1 fluxval_1: V = 5.72 fluxnum_2: 2 fluxval_2: B-V = 0.36 +/- 0.01,U-B = 0.00 +/- 0.02 fluxnum_3: 3 fluxval_3: F(3130) = 1.2 +/- 0.3 E-11 fluxnum_4: 4 fluxval_4: F(2500) = 2.2 +/- 0.6 E-12 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HD84937 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 2.5S fluxnum_1: 3 fluxnum_2: 4 priority: 1 param_1: SEARCH-SIZE=5 param_2: FAINT=5000 req_1: ONBOARD ACQ FOR 2; req_2: CYCLE 1 / 1-10 ! linenum: 2.000 targname: HD84937 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 3130 num_exp: 2 time_per_exp: 2160S s_to_n: 40 s_to_n_time: 4000S fluxnum_1: 3 priority: 1 param_1: FP-SPLIT=STD param_2: STEP-PATT=7 ! linenum: 3.000 targname: HD84937 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 9.2S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 4 ! linenum: 4.000 targname: HD84937 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2498 num_exp: 2 time_per_exp: 2000S s_to_n: 60 s_to_n_time: 4000S fluxnum_1: 4 priority: 1 param_1: FP-SPLIT=STD param_2: STEP-PATT=5 ! linenum: 5.000 targname: VB13 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 9S fluxnum_1: 3 fluxnum_2: 4 priority: 1 param_1: SEARCH-SIZE=3 param_2: FAINT=500 req_1: ONBOARD ACQ FOR 6 ! linenum: 6.000 targname: VB13 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 46S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 7 ! linenum: 7.000 targname: VB13 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2498 num_exp: 1 time_per_exp: 2300S s_to_n: 50 s_to_n_time: 2300S fluxnum_1: 3 fluxnum_2: 4 priority: 1 param_1: FP-SPLIT=STD param_2: STEP-PATT=5 ! linenum: 8.000 targname: VB14 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 3.6S fluxnum_1: 3 fluxnum_2: 4 priority: 1 param_1: SEARCH-SIZE=3 param_2: FAINT=500 req_1: ONBOARD ACQ FOR 9 ! linenum: 9.000 targname: VB14 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 18.4S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 10 ! linenum: 10.000 targname: VB14 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2498 num_exp: 1 time_per_exp: 1080S s_to_n: 50 s_to_n_time: 1080S fluxnum_1: 3 fluxnum_2: 4 priority: 1 param_1: FP-SPLIT=STD param_2: STEP-PATT=5 ! ! end of exposure logsheet ! No scan data records found