! File: 5198C.PROP ! Database: PEPDB ! Date: 24-FEB-1994:00:41:34 coverpage: title_1: THE EVOLUTION OF BORON : IMPLICATIONS FOR GALACTIC EVOLUTION title_2: AND COSMOLOGY: PART 2 sci_cat: COOL STARS sci_subcat: EVOLUTION/COSMOLOGY proposal_for: GO cont_id: 4510 pi_title: DR. pi_fname: DOUGLAS pi_mi: K. pi_lname: DUNCAN pi_inst: 1710 pi_country: USA pi_phone: 312-702-8207 hours_pri: 22.83 num_pri: 9 hrs: Y funds_amount: 208338 funds_length: 18 funds_date: JUL-93 pi_position: ASSOC. PROFESSOR off_fname: JOYCE off_lname: FREEDMAN off_title: ASSOC. VP. RESEARCH off_inst: 1710 off_addr_1: 970 E. 58TH ST. off_city: CHICAGO off_state: IL off_zip: 60637 off_country: USA off_phone: 312-702-8604 ! end of coverpage abstract: line_1: We propose to observe boron in late type stars of metallicities ranging line_2: from disk to extreme halo and combine this data with our ground-based line_3: measurements of Be and Li. The evolution of Li, Be, and B has now been line_4: shown to be a powerful descriminant between different models of the chemical line_5: and dynamical evolution of the galaxy, and must be added to the evolution of line_6: \[Fe/H\] and \[O/H\] as the critical test of such models. Light element line_7: production depends on the intensity and shape of the cosmic ray spectrum, which line_8: in turn depends on the supernova rate and thus the star formation rate. It also line_9: depends on the rise of the (progenitor) CNO abundances, and the decline of line_10: the gas mass fraction, which is affected by rates of infall of fresh line_11: (unprocessed) material and outflow, e.g. by supernova heating. By concentrating line_12: on stars at the transition from old disk to halo and in the halo population line_13: we can learn the most about the importance of each of these critcal properties line_14: of the early galaxy. Already the first 3 HST observations of B in halo stars line_15: CANNOT be matched by existing models of galactic chemical evolution (4). line_16: -- In addition, the search for primordial B and Be in the most metal-poor line_17: stars is the key for discriminating between standard and inhomogeneous big line_18: bang nucleosynthesis models. Some recent evidence hints at inconsistancy line_19: in the standard model, and accurate observations of B and Be are critical line_20: to test and constrain the various inhomogeneous models. ! ! end of abstract general_form_proposers: lname: DUNCAN fname: DOUGLAS title: PI mi: K. inst: 1710 country: USA ! lname: BOESGAARD fname: ANN mi: M. inst: UNIVERSITY OF HAWAII/PENN STATE UNIVERSITY country: USA ! lname: DELIYANNIS fname: CONSTANTINE mi: P. inst: 2190 country: USA ! lname: HOBBS fname: LEWIS mi: M. inst: 1716 country: USA ! lname: KING fname: JEREMY mi: R. inst: 2190 country: USA ! lname: RYAN fname: SEAN mi: G. inst: 3550 country: USA/AUSTRALIA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: ! question: 3 section: 1 line_1: A single GHRS observation will be made of each star, using the G270M grating line_2: centered at 2500A, the wavelength of the B resonance lines. The same line_3: techniques (FP-SPLIT, the best vignetting corrections, etc.) used for achieving line_4: the highest S/N on weak features which were successfully used to observe the line_5: first three halo stars (Duncan, Lambert, and Lemke, CYCLE 1) will be used. line_6: The new SSA ACQ/PEAKUP capability is requested for better efficiency. ! question: 4 section: 1 line_1: The only boron lines suitable for late-type stars are in the UV (2500A) line_2: and cannot be observed from the ground, or with enough resolution with IUE. ! question: 4 section: 2 line_1: [The PI is former GHRS Instrument Scientist.] Count rates are scaled from: line_2: Count rates observed (by PI) in HD 140283, a halo star of similar spectral line_3: type, observed with exactly the same GHRS setup. Allowance was made for the line_4: dependence of the UV flux on the slightly different effective temperatures line_5: of our stars. ! question: 5 section: 1 line_1: none. ! question: 6 section: 1 line_1: An extra comparison or standard star is being requested to aid in the model line_2: atmosphere analysis. We have deliberately left 2.17 hours for this, so the line_3: RPSS RESOURCE ESTIMATE submitted is LOW. We will request this extra target line_4: on a separate "STScI Change Request Form." ! question: 7 section: 1 line_1: Duncan has extensive STSDAS/IRAF experience, and the ability to reduce the line_2: data at U.Chicago. Also, he has already done successful specrtum synthesis line_3: work, using the latest synthesis program and atmospheres of Kurucz (1991, line_4: private communication), essential for determining accurate B abundances. line_5: From the analysis of 3 metal-poor stars in Cycle 0, a good line-list and line_6: suitable programs are ready and waiting to be applied to the new stars. line_7: HOWEVER, the more metal-rich stars are more difficult to analyze, having line_8: many, many more lines. We will add one standard star, of very well known line_9: composition, to help make an empirical comparison. Considerable time will line_10: be required to make a careful anaysis of the data, even though we have line_11: the facilities. ! question: 8 section: 1 line_1: none. ! question: 9 section: 1 line_1: 2251. Hobbs, PI. "The Properties of Single Interstellar Clouds: line_2: Modified Cycle 1 Observations". UNRELATED to this (boron) proposal. line_3: 2634. Duncan, PI. "Boron and Be as probes of Cosmic Ray Spallation..." line_4: RELATED: The analysis techniques are exactly the same as needed here. line_5: 2691. Duncan, PI. "Precision Prallaxes of Cepheids...using WF/PC." line_6: UNRELATED to this (boron) proposal. line_7: 3472. Hobbs, PI. "The Properties of Single Interstellar Clouds: line_8: Cycle 2". UNRELATED to this (boron) proposal. line_9: 3482. Vidal-Madjar, PI ; Hobbs, Co-I. "The Nature of the Infalling line_10: Material on the Star Beta Pictoris." UNRELATED to this (boron) proposal. line_11: 3614. Duncan, PI ; Deliyannis, Co-I. "Boron as a Probe of Stellar line_12: Structure and Mass Loss." RELATED: The analysis techniques are exactly the line_13: same as needed for the current proposal. The science is different. line_14: 3993. Hobbs, PI. "The Properties of Single Interstellar Clouds: line_15: Cycle 1, Side 2 Observations". UNRELATED to this (boron) proposal. ! question: 9 section: 2 line_1: 2251. First data just received July 1992. 2634. All spectra obtained. line_2: Data reduced; B detected, spectrum synthesis done. Results in ApJ (below), line_3: much quoted. 2691. Data not yet obtained. 3472. Data not yet obtained. line_4: 3482. Data not yet obtained. 3614. First data obtained this week. line_5: 3993. First data received in April 1992, currently being analyzed. ! question: 9 section: 3 line_1: "The Abundance of Boron in Three Halo Stars", Duncan, Lambert, and Lemke, line_2: Ap. J. 401, 584, Dec. 20, 1992. ! question: 10 section: 1 line_1: Normal office and secretarial support is provided to the PI and Co-Is line_2: by their institutions. Sun workstation powerful enough to handle data line_3: reduction and the running of theoretical stellar interiors models to track line_4: Boron mixing is provided through this grant. Support for hooking up line_5: computer equipment is provided by the institutions. ! !end of general form text general_form_address: lname: DUNCAN fname: DOUGLAS mi: K. category: PI inst: 1710 addr_1: Dept.of Astron. and Astrophys. addr_2: 5640 S. Ellis Ave. city: Chicago state: IL zip: 60637 country: USA phone: 312-702-0560 ! ! end of general_form_address records fixed_targets: targnum: 9 name_1: HD124897 name_2: (ARCTURUS) descr_1: A,140 pos_1: RA=14H 15M 39.677S +/- 0.1S, pos_2: DEC=+19D 10' 56.7" +/- 1.0" equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: -0.077100 ra_pm_unct: 0.003000 dec_pm_val: -1.9980 dec_pm_unct: 0.0030 an_prlx_unct: 0.0100 fluxnum_1: 1 fluxval_1: V=-0.04,B-V=1.23,TYPE=K1III ! targnum: 10 name_1: HD103095 descr_1: A,137,911 pos_1: RA=11H 52M 58.767S +/- 0.1S, pos_2: DEC=+37D 43' 07.35" +/- 1.0" equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: -0.077100 ra_pm_unct: 0.005000 dec_pm_val: -5.8130 dec_pm_unct: 0.0050 an_prlx_val: 0.0100 an_prlx_unct: 0.0100 fluxnum_1: 1 fluxval_1: V=6.45,B-V=0.75,TYPE=SDG ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 9.000 targname: HD124897 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 1.8S s_to_n: 25 s_to_n_time: .2S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3 / 9.0-9.3; req_2: ONBOARD ACQ FOR 9.1 comment_1: STEP-TIME=0.2S ! linenum: 9.100 targname: HD124897 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 50S s_to_n: 25 s_to_n_time: 2.0S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=5 req_1: ONBOARD ACQ FOR 9.2-9.3 comment_1: STEP-TIME=2.0S ! linenum: 9.200 targname: HD124897 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2498 num_exp: 7 time_per_exp: 440S s_to_n: 90 s_to_n_time: 24M fluxnum_1: 1 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD ! linenum: 9.300 targname: HD124897 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 3130 num_exp: 1 time_per_exp: 390S s_to_n: 150 s_to_n_time: 5M fluxnum_1: 1 priority: 1 param_1: STEP-PATT=7, param_2: FP-SPLIT=STD ! ! end of exposure logsheet ! No scan data records found