! File: 4591C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:18:55:51 coverpage: title_1: BORON IN LI- AND BE- DEFICIENT F STARS, A KEY title_2: DISCRIMINATOR OF STELLAR EVOLUTION SCENARIOS sci_cat: COOL STARS sci_subcat: STELLAR ATMOSPHERES proposal_for: GO pi_fname: ANN pi_mi: M. pi_lname: BOESGAARD pi_inst: 3150 pi_country: USA hours_pri: 5.42 num_pri: 8 hrs: Y funds_length: 12 off_fname: DAVID off_mi: A. off_lname: SHIRLEY off_title: SR V-P FOR RESEARCH off_inst: 3150 off_addr_1: SPONSORED PROGRAMS AND CONTRACTS OFFICE off_addr_2: 118 BARBARA BUILDING II, THE PENNSYLVANIA STATE UNIVERSITY off_city: UNIVERSITY PARK off_state: PA off_zip: 16802 off_country: USA off_phone: 814-865-1372 ! end of coverpage abstract: line_1: The surprising discovery that F stars in a narrow Teff range of line_2: only a few hundred degrees can be severely depleted in their surface line_3: Li abundance (a Li "dip") signals a fundamental failure of standard line_4: stellar evolution theory. Numerous physical mechanisms have been line_5: proposed to explain this dip, including microscopic diffusion, mass line_6: loss, meridional circulation, and rotationally-induced mixing driven line_7: by angular momentum loss. Identifying which of these (if any) might line_8: really be at work is not only of vital interest to stellar evolution line_9: theory, but also to cosmology. (For example, diffusion may lower age line_10: estimates for globular clusters, and rotationally-induced mixing line_11: suggests that the standard model of big bang nucleosynthesis may be line_12: incomplete.) B thus joins Li and Be as a crucial probe of stellar line_13: structure and discriminator of viable physical mechanisms, as the line_14: most powerful constraints are obtained when all three elements are line_15: considered simultaneously. B will be observed in eight stars, both line_16: solar metallicity and old disk (since depletion is metallicity line_17: dependent), four that are extremely deficient in Li and Be, three line_18: that are moderately so, and one that is Li- and Be- normal. We have line_19: extensive observational and theoretical experience using Li and Be line_20: (and have CYCLE2 time to use B) as probes of stellar structure. ! ! end of abstract general_form_proposers: lname: BOESGAARD fname: ANN title: PI mi: M. inst: 3150 country: USA ! lname: LAMBERT fname: DAVID mi: L. inst: UNIVERSITY OF TEXAS country: USA ! lname: DELIYANNIS fname: CONSTANTINE mi: P. inst: UNIVERSITY OF HAWAII country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: INTRODUCTION. line_2: With HST and GHRS, Boron joins Li and Be as a probe of stellar structure line_3: and evolution. Indeed, it is when all three elements are considered line_4: simultaneously that the most powerful constraints on stellar models are line_5: realized. This proposal is concerned with the depletion of B in stars of line_6: the Li-dip that are greatly depleted in Li and Be. The proposal is a line_7: development of our successful analyses of B in halo and disk stars. We also line_8: have had extensive observational and theoretical experience using Li and Be line_9: (and have CYCLE2 time to use B) as probes of stellar structure and evolution. line_11: THE LI-DIP. line_12: In increasing order of stability, Li, Be, and B are all destroyed line_13: by (p,alpha) reactions at a few million degrees in stellar interiors. line_14: Boesgaard and Tripicco (1986 ApJ 302 L49) discovered that in a narrow line_15: Teff region of a few hundred degrees, F stars are able to severely deplete line_16: their surface Li abundance. This startling discovery of a Li-dip blatantly line_17: contradicted the predictions of standard stellar evolution theory : in standard line_18: models, Li is preserved in the outermost several % of the mass (after the line_19: ZAMS), yet the surface convection zone occupies 0.1% of the mass or less. line_20: Hence, there is no way to affect the surface Li abundance in these models line_21: (e.g. as might be the case in lower mass stars, where Li burning occurs at line_22: the base of the convection zone). To make matters worse, there is an line_23: accompanying Be-dip, but not in the Hyades (Boesgaard and Budge 1989 ApJ 338 ! question: 2 section: 2 line_1: 875); deficiency of Be must develop more slowly than the corresponding line_2: Li one. Be-deficient F stars are known (Boesgaard 1976 ApJ 210 466). line_3: To explain the Li dip, proposed physical mechanisms (beyond the line_4: standard model) have proliferated in recent years. These include mass loss line_5: (Schramm et al. 1990 ApJL 359 L55), microscopic diffusion (Michaud line_6: 1986 ApJ 302 650), meridional circulation (Charbonneau and Michaud 1988 line_7: ApJ 334 746), overshoot, turbulent diffusion (Vauclair 1988 ApJ 335 971), line_8: and rotationally-induced mixing related to the onset of instabilities that line_9: cause angular momentum transport (Pinsonneault et al. 1990 ApJS 74 501, line_10: "Yale" models). It is not yet clear which of these (if any) is correct. line_11: While each of the above mechanisms can allegedly form a Li dip, line_12: each mechanism leaves different Be and B abundance signatures. We line_13: propose to add B to Li and Be observations as a powerful tool to uncover line_14: and decipher the signature of the responsible mechanism(s). As an example line_15: of the power of using more than one element at a time, consider 110 Her, line_16: which is definitively depleted in Be by a factor of 5-10, and in Li by a factor line_17: of 100-200, yet still retains a detectable abundance of Li (Boesgaard and line_18: Lavery 1986 ApJ 309 762). Since Be survives to about twice the ZAMS line_19: depth as does Li, this remarkable pattern of having depleted surface Be line_20: without having also depleted all the surface Li requires specific line_21: circumstances, which severely constrain or eliminate most of the proposed line_22: mechanisms (Deliyannis and Pinsonneault 1992 in IAU Colloquium #137, line_23: ed. W.W. Weiss, ASP Conference Series, in press). For example, mass ! question: 2 section: 3 line_1: loss is argued against because it wipes out surface Li before surface Be is line_2: affected ; mechanisms requiring rapid mixing are similarly argued against. line_3: Proposed diffusion scenarios are also argued against because, in one case, line_4: Li and Be deplete comparably, and in another case the Be abundance increases line_5: even as Li decreases. However, the Yale rotational models (which yield slow line_6: mixing) agree both qualitatively and quantitatively with 110 Her. line_7: Still more stringent constraints are required, and adding B will line_8: multiply our power to discriminate between stellar evolutionary scenarios. line_9: Our previous observations suggest that B is underabundant in Procyon by a line_10: factor of 3 relative to the two Li- and Be- normal dwarfs Theta UMa and line_11: Iota Peg. This mild deficiency and the ordering Li>Be>B of the line_12: deficiencies are both consistent with destruction, perhaps aided by mixing, line_13: but not with pure diffusion. In the case of diffusion, studies of other line_14: elements have shown none of the anomalies predicted (Boesgaard and Lavery line_15: 1986 ApJ 309 762). Further discriminatory constraints, and determining line_16: the details of how mixing occurs (if this is the correct scenario) will require line_17: solid observations of B. line_18: First, we propose to complete our investigation of Procyon (Be- line_19: poor by a factor of 45 or more). This will include an examination of the line_20: 11B/10B isotope ratio at 2090A, which will provide further information line_21: about the possible destruction mechanisms at work, since the two isotopes line_22: burn at slightly different temperatures. Next, since, as Procyon suggests, line_23: the most Be-deficient stars are the ones most likely to be deficient in B, we ! question: 2 section: 4 line_1: propose to look at Sigma Boo and Theta Cyg, which are both also severely line_2: Be-deficient. At what level of Be-deficiency does B deficiency begin? In line_3: analogy with 110 Her, the strongest contraints would be obtained if stars with line_4: barely detectable Be already showed a B deficiency (but the constraints will line_5: still be quite strong even if such stars do NOT show a B deficiency). We line_6: propose to investigate this question by including HR 244 (Figure 1) and HR 6541, line_7: for which our recent CFHT spectra show barely detectable Be lines. (Note that line_8: in 110 Her, which is "moderately" depleted in Be, B will be observed as part line_9: of our CYCLE2 GO3614.) Light element depletion is predicted (and also observed) line_10: to be a strong function of metallicity (e.g. Deliyannis, Demarque, and Kawaler line_11: 1990 ApJS 73 21; Deliyannis and Pinsonneault 1990 ApJL 367 L67); observations line_12: of B in old disk stars will therefore provide additional important constraints. line_13: We thus include the somewhat metal-deficient star 62 UMa, which shows no (CFHT) line_14: Be line (see Figure 1), and Sigma Peg, which shows a barely detectable Be line. line_15: Finally, we include the Li- and Be- normal star HR 235 as a standard. We stress line_16: that we have excellent CCD spectra of all these stars in the Be region (e.g. line_17: Figure 1), as well as high resolution and high S/N spectra of the Li region. line_19: BORON AND HST. line_20: In F dwarfs B is detectable via the B I resonance lines at 2496.8 and line_21: 2089.6A. (The other lines of these multiplets are blended.) The 2496.8A line_22: line provides reliable results for F dwarfs - see Figure 2 for ECH-B and line_23: G270M observations of Procyon and Theta Uma. Johansson et al. ! question: 2 section: 5 line_1: (preprint) find the two lines to have the same gf-value with 2089.6A having line_2: an isotope shift of 25mA which is measureable with ECH-B. Synthetic line_3: spectra with the best available line lists suggest the 2089.6A line is line_4: unblended; the line appears in the solar spectrum for example. line_5: We propose to observe the following sharp-lined stars : line_6: 1. Procyon with ECH-B at 2497 and 2090A, Sigma Boo and 62 UMa with line_7: G270M at 2497A, and Theta Cyg with ECH-B at 2497A, for B in stars with line_8: only upper limits to Be (and thus extremely deficient Be). line_9: 2. HR 244, HR 6541, and Sigma Peg with G270M at 2497A, for B in line_10: stars with barely detected (and significantly deficient) Be. line_11: 3. HR 235 with G270M at 2497A, for B in a Li- and Be- normal line_12: star, as a standard. ! question: 3 section: 1 line_1: The proposed observations use B in F stars as a probe of stellar structure. line_2: 1. Procyon will be observed at 2497A with ECH-B to determine a reliable line_3: B depletion factor. line_4: 2. Six Be-poor stars (with different degrees of Be depletion, both with solar line_5: metallicity and slightly metal-poor) and one Be-normal star will be observed line_6: at 2497A with either ECH-B or G270M to get a S/N = 60-100. ! question: 4 section: 1 line_1: Boron is a trace element with no detectable transitions in the visible or line_2: infrared spectra of main sequence stars. It is essential to measure the B line_3: abundance and not rely on inferences from Be. line_5: IUE lacks the spectral resolution and the S/N to detect the B I lines. This line_6: is well seen by the fact after more than a decade of IUE activity the only line_7: papers on the B I line are two providing dull upper limits to the B abundance line_8: in metal-poor stars. Our GHRS observations show that the real B abundance in line_9: such stars is 1.0 dex or more below the not very convincing IUE upper limits. line_10: Lack of IUE activity on B is not due to oversight or benign neglect by line_11: observers. line_13: Boron abundances for A to B stars (Teff = 10,000 to 20,000 K) were derived line_14: by Boesgaard and Heacox (1978, ApJ 226 888) from Copernicus spectra of the B II line_15: 1362A resonance line. (Their mean B abundance is in good agreement with our line_16: values for Theta Uma and Iota Peg from the B I line.) While the B II line line_17: should be exploited with HST, it will not provide the information sought under line_18: this proposal because (i) The Be-deficient stars of the Li-gap are too cool to line_19: emit photospheric radiation at 1362A and B is predominantly neutral, and line_20: (ii) the B II line has a very small isotopic shift and does not permit a line_21: measurement of the 11B/10B ratio. line_23: In short, our proposal can only be done with HST and the GHRS. ! question: 4 section: 2 line_1: In determining the B abundance four options are available: ECH-B or G270M at line_2: 2497A, and ECH-B or G200M at 2090A. For the typical F dwarf the relative count line_3: rates per pixel of the four options are line_4: ECH-B at 2497A = 1.0 ECH-B at 2090A = 1.1 line_5: G270M at 2497A = 13.0 G200M at 2090A = 2.4 line_7: In estimating the count rates, we have taken fluxes from the IUE Spectral line_8: Atlas for aprogram star or estimated the flux from a star of the same spectral line_9: type taking account of the differences in the V magnitudes. The recipe was line_10: checked against our GTO observations of Procyon, Theta Uma, and Iota Peg. line_12: Our experience with spectra at 2497A shows that a S/N = 60-100 is needed. line_13: While ECH-B is always desired, G270M (or G200M) is useful (Figure 2). ! question: 5 section: 1 line_1: NONE. ! question: 6 section: 1 line_1: None. ! question: 7 section: 1 line_1: We have previously pioneered B detections both in Pop I stars line_2: (eg Boesgaard and Heacox 1978 ApJ 226 888) and in Pop II stars from HST (below). line_3: In Austin, we have exercised all the tools needed to extract B abundances line_4: from the spectra. Our GTO spectra of three halo dwarfs have been reduced, line_5: analyzed, and interpreted - see Duncan, Lambert, and Lemke (1992, ApJ, in line_6: press). A paper is in preparation on B in the F dwarfs Theta Uma, Iota Peg, line_7: and Procyon. The new spectra can therefore be reduced in a timely fashion. line_8: A line list for the new 2090A region is available. The PI with D Lambert line_9: will assume responsibility for the analysis. line_10: Interpretation of the B abundances will be done primarily by C Deliyannis line_11: with the support of the PI and CoI. Deliyannis has extensive experience in the line_12: modelling of the structure of F dwarfs. line_13: We are completely ready to analyze and interpret the data. ! question: 8 section: 1 line_1: None. ! question: 9 section: 1 line_1: line_2: Lambert is PI on all these GTO proposals and a Co-I on the GO proposals: line_4: GTO1064 Boron in Main Sequence Stars, related line_5: GTO1065 Isotopic Abundances of Carbon and Oxygen and Fractionation of line_6: Interstellar Carbon Monoxide, not related line_7: GTO1066 Carbon Chemistry in Interstellar Diffuse Clouds, not related line_8: GTO1067 Old Novae and Cataclysmic Variables - DQ Her, not related line_9: GTO1068 Epsilon Aurigae- A Search for the Secondary, not related line_10: GO3824 A Search for Silicon and Carbon in GP Com, not related line_11: GO3479 Boron in Pop. II Dwarfs - Primeval or Spallated?, related line_13: Deliyannis is a Co-I on the following GO proposal: line_15: GO3614 Boron as a Probe of Stellar Structure and Mass Loss, related line_18: GTO observations of three halo dwarfs with [Fe/H] = -2.6 to -1.1 showed the B line_19: abundance to increase linearly with [Fe/H]. The B abundances with published Be line_20: abundances show that B/Be = 10 for the halo. This ratio is that predicted for line_21: Be and B production by spallation induced by cosmic rays. There is no evidence line_22: that either Be or B were produced in significant levels by the Big Bang, a line_23: prediction consistent with models of standard Big Bangs. No observations have ! question: 9 section: 2 line_1: yet been made under GO3479 which is intended to provide ECH-B spectra of two line_2: halo dwarfs. line_4: Boron has been shown to be depleted slightly in the very Be-por F star line_5: Procyon. The B abundance of two Be-normal F dwarfs is close to solar and the line_6: abundance seen previously in B and A type stars. line_8: 3614 : data not yet obtained. line_11: First Results from the GHRS: C I, S I, and CO toward Xi Persei and the line_12: Physical Conditions of the Diffuse Clouds. A M Smith, F C Bruhweiler, line_13: D L Lambert, B D Savage, J A Cardelli, D C Ebbets, C-H Lyu, & Y Sheffer, line_14: ApJ, 377, L61, 1991. line_16: Fractionation of CO in the Diffuse Clouds toward Zeta Oph, Y Sheffer, line_17: S R Federman, D L Lambert, & J A Cardelli, ApJ, in press, 1992. line_19: The Abundance of Boron in three Halo Stars, D K Duncan, D L Lambert, line_20: & M Lemke, ApJ, in press, 1992. ! question: 10 section: 1 line_1: line_2: Adequate facilities for the reduction of the GHRS spectra and computation of line_3: synthetic spectra are available at Texas and Hawaii. Models of stellar line_4: interiors are readily calculated in Hawaii. ! !end of general form text general_form_address: lname: BOESGAARD fname: ANN mi: M. category: PI inst: 3150 addr_1: PENN STATE UNIVERSITY addr_2: 525 DAVEY LAB city: UNIVERSITY PARK state: PA zip: 16802 country: USA phone: 814-865-0418 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD4813 name_2: PHI-CET name_3: HR235 descr_1: A,134 pos_1: RA = 0H 50M 7.5S +/- 0.1S, pos_2: DEC = -10D 38' 40" +/- 1.0" equinox: J2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: -0.015600 ra_pm_unct: 0.000700 dec_pm_val: -0.2230 dec_pm_unct: 0.0020 an_prlx_val: 0.0650 an_prlx_unct: 0.0100 rv_or_z: V = +8 fluxnum_1: 1 fluxval_1: V=5.19, TYPE=F7IV, B-V=0.50 ! targnum: 2 name_1: HD61421 name_2: PROCYON name_3: HR2943 descr_1: A,134 pos_1: RA = 7H 39M 18.1S +/- 0.01S, pos_2: DEC = +5D 13' 30.1" +/- 0.02" equinox: J2000 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 2000.00 ra_pm_val: -0.047300 ra_pm_unct: 0.000300 dec_pm_val: -1.0290 dec_pm_unct: 0.0010 an_prlx_val: 0.2920 an_prlx_unct: 0.0100 rv_or_z: V = -3 fluxnum_1: 1 fluxval_1: V = 0.38, TYPE=F5IV, B-V = 0.42 ! targnum: 3 name_1: HD128167 name_2: SIG-BOO name_3: HR5447 descr_1: A,134 pos_1: RA = 14H 34M 40.8S +/- 0.1S, pos_2: DEC = +29D 44' 42.5" +/- 0.02" equinox: J2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.014500 ra_pm_unct: 0.000500 dec_pm_val: 0.1290 dec_pm_unct: 0.0010 an_prlx_val: 0.0680 an_prlx_unct: 0.0100 rv_or_z: V = 0 fluxnum_1: 1 fluxval_1: V = 4.46, TYPE = F2V, B-V = 0.36 ! targnum: 4 name_1: HD185395 name_2: THE-CYG name_3: HR7469 descr_1: A,134 pos_1: RA = 19H 36M 26.5S +/- 0.01S, pos_2: DEC = +50D 13' 15.8" +/- 0.02" equinox: J2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: -0.002500 ra_pm_unct: 0.001000 dec_pm_val: 0.2560 dec_pm_unct: 0.0010 an_prlx_val: 0.0560 an_prlx_unct: 0.0100 rv_or_z: V = -28 fluxnum_1: 1 fluxval_1: V = 4.48, TYPE = F4V, B-V = 0.38 ! targnum: 5 name_1: HD101606 name_2: 62-UMA name_3: HR4501 descr_1: A,134 pos_1: RA = 11H 41M 34.3S +/- 0.09S, pos_2: DEC = +31D 44' 45.5" +/- 0.09" equinox: J2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: -0.027400 ra_pm_unct: 0.003000 dec_pm_val: 0.0190 dec_pm_unct: 0.0020 an_prlx_val: 0.0260 an_prlx_unct: 0.0100 rv_or_z: V = +32 fluxnum_1: 1 fluxval_1: V = 5.73, TYPE = F4V, B-V = 0.43 ! targnum: 6 name_1: HD5015 name_2: HR244 descr_1: A,134 pos_1: RA = 0H 53M 4.2S +/- 0.09S, pos_2: DEC = +61D 7' 26.5" +/- 0.09" equinox: J2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: -0.009800 ra_pm_unct: 0.003000 dec_pm_val: 0.1780 dec_pm_unct: 0.0020 an_prlx_val: 0.0660 an_prlx_unct: 0.0100 rv_or_z: V = +21 fluxnum_1: 1 fluxval_1: V = 4.82, TYPE = F8V, B-V = 0.53 ! targnum: 7 name_1: HD159332 name_2: HR6541 descr_1: A,134 pos_1: RA = 17H 33M 22.8S +/- 0.03S, pos_2: DEC = +19D 15' 24.0" +/- .03" equinox: J2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: -0.002200 ra_pm_unct: 0.004000 dec_pm_val: -0.0930 dec_pm_unct: 0.0040 an_prlx_val: 0.0320 an_prlx_unct: 0.0100 rv_or_z: V = -59 fluxnum_1: 1 fluxval_1: V = 5.64, TYPE = F6V, B-V = 0.48 ! targnum: 8 name_1: HD216385 name_2: SIG-PEG name_3: HR8697 descr_1: A,134 pos_1: RA = 22H 52M 24.1S +/- 0.03S, pos_2: DEC = +9D 50' 8.4" +/- 0.03" equinox: J2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.035300 ra_pm_unct: 0.001000 dec_pm_val: 0.0490 dec_pm_unct: 0.0100 an_prlx_val: 0.0430 an_prlx_unct: 0.0100 rv_or_z: V = +12 fluxnum_1: 1 fluxval_1: V = 5.16, TYPE = F7IV, B-V = 0.48 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HD4813 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 3.6S s_to_n: 25 s_to_n_time: 0.4S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3 / 1.0-1.2; req_2: ONBOARD ACQ FOR 1.1 comment_1: STEP-TIME=0.4S ! linenum: 1.100 targname: HD4813 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 75S s_to_n: 25 s_to_n_time: 3.0S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=5 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 1.2 comment_1: STEP-TIME=3.0S ! linenum: 1.200 targname: HD4813 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2497 num_exp: 1 time_per_exp: 30.0M s_to_n: 80 s_to_n_time: 30.0M fluxnum_1: 1 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD req_1: CYCLE 3 ! linenum: 2.000 targname: HD61421 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 3.6S s_to_n: 25 s_to_n_time: 0.4S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3 / 2.0-2.2; req_2: ONBOARD ACQ FOR 2.1 comment_1: STEP-TIME=0.4S ! linenum: 2.100 targname: HD61421 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: CYCLE 3; req_2: ONBOARD ACQ FOR 2.2 comment_1: STEP-TIME=2.0S ! linenum: 2.200 targname: HD61421 config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-B wavelength: 2497 num_exp: 2 time_per_exp: 20.0M s_to_n: 80 s_to_n_time: 40.0M fluxnum_1: 1 priority: 1 param_1: STEP-PATT=7, param_2: FP-SPLIT=STD req_1: CYCLE 3 ! linenum: 3.000 targname: HD128167 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 3.6S s_to_n: 25 s_to_n_time: 0.4S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3 / 3.0-3.1; req_2: ONBOARD ACQ FOR 3.1 comment_1: STEP-TIME=0.4S ! linenum: 3.100 targname: HD128167 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: CYCLE 3; req_2: ONBOARD ACQ FOR 3.2 comment_1: STEP-TIME=2.0S ! linenum: 3.200 targname: HD128167 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2497 num_exp: 1 time_per_exp: 25.0M s_to_n: 80 s_to_n_time: 25.0M fluxnum_1: 1 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD req_1: CYCLE 3 ! linenum: 4.000 targname: HD185395 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 3.6S s_to_n: 25 s_to_n_time: 0.4S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3 / 4.0-4.1; req_2: ONBOARD ACQ FOR 4.1 comment_1: STEP-TIME=0.4S ! linenum: 4.100 targname: HD185395 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: CYCLE 3; req_2: ONBOARD ACQ FOR 4.2 comment_1: STEP-TIME=2.0S ! linenum: 4.200 targname: HD185395 config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-B wavelength: 2497 num_exp: 3 time_per_exp: 27.0M s_to_n: 80 s_to_n_time: 81.0M fluxnum_1: 1 priority: 1 param_1: STEP-PATT=7, param_2: FP-SPLIT=STD req_1: CYCLE 3 ! linenum: 5.000 targname: HD101606 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 3.6S s_to_n: 25 s_to_n_time: 0.4S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3 / 5.0-5.2; req_2: ONBOARD ACQ FOR 5.1 comment_1: STEP-TIME=0.4S ! linenum: 5.100 targname: HD101606 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 75S s_to_n: 25 s_to_n_time: 3.0S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=5 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 5.2 comment_1: STEP-TIME=3.0S ! linenum: 5.200 targname: HD101606 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2497 num_exp: 2 time_per_exp: 23.0M s_to_n: 80 s_to_n_time: 46.0M fluxnum_1: 1 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD req_1: CYCLE 3 ! linenum: 6.000 targname: HD5015 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 3.6S s_to_n: 25 s_to_n_time: 0.4S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3 / 6.0-6.2; req_2: ONBOARD ACQ FOR 6.1 comment_1: STEP-TIME=0.4S ! linenum: 6.100 targname: HD5015 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: CYCLE 3; req_2: ONBOARD ACQ FOR 6.2 comment_1: STEP-TIME=2.0S ! linenum: 6.200 targname: HD5015 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2497 num_exp: 1 time_per_exp: 30.0M s_to_n: 80 s_to_n_time: 30.0M fluxnum_1: 1 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD req_1: CYCLE 3 ! linenum: 7.000 targname: HD159332 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 3.6S s_to_n: 25 s_to_n_time: 0.4S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3 / 7.0-7.2; req_2: ONBOARD ACQ FOR 7.1 comment_1: STEP-TIME=0.4S ! linenum: 7.100 targname: HD159332 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 75S s_to_n: 25 s_to_n_time: 3.0S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=5 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 7.2 comment_1: STEP-TIME=3.0S ! linenum: 7.200 targname: HD159332 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2497 num_exp: 2 time_per_exp: 23.0M s_to_n: 80 s_to_n_time: 46.0M fluxnum_1: 1 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD req_1: CYCLE 3 ! linenum: 8.000 targname: HD216385 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 3.6S s_to_n: 25 s_to_n_time: 0.4S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3 / 8.0-8.2; req_2: ONBOARD ACQ FOR 8.1 comment_1: STEP-TIME=0.4S ! linenum: 8.100 targname: HD216385 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 75S s_to_n: 25 s_to_n_time: 3.0S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=5 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 8.2 comment_1: STEP-TIME=3.0S ! linenum: 8.200 targname: HD216385 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2497 num_exp: 1 time_per_exp: 30.0M s_to_n: 80 s_to_n_time: 30.0M fluxnum_1: 1 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD req_1: CYCLE 3 ! ! end of exposure logsheet ! 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