Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 4591c Report Date: 09-May-96:19:43 Version: ********** Check-in Date: ********** 1.Proposal Title: BORON IN LI- AND BE- DEFICIENT F STARS, A KEY DISCRIMINATOR OF STELLAR EVOLUTION SCENARIOS ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID COOL STARS GO Sub Category STELLAR ATMOSPHERES ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone Ann M. Boesgaard 3150 USA ------------------------------------------------------------------------------------ 7. Abstract The surprising discovery that F stars in a narrow Teff range of only a few hundred degrees can be severely depleted in their surface Li abundance (a Li "dip") signals a fundamental failure of standard stellar evolution theory. Numerous physical mechanisms have been proposed to explain this dip, including microscopic diffusion, mass loss, meridional circulation, and rotationally-induced mixing driven by angular momentum loss. Identifying which of these (if any) might really be at work is not only of vital interest to stellar evolution theory, but also to cosmology. (For example, diffusion may lower age estimates for globular clusters, and rotationally- induced mixing suggests that the standard model of big bang nucleosynthesis may be incomplete.) B thus joins Li and Be as a crucial probe of stellar structure and discriminator of viable physical mechanisms, as the most powerful constraints are obtained when all three elements are considered simultaneously. B will be observed in eight stars, both solar metallicity and old disk (since depletion is metallicity dependent), four that are extremely deficient in Li and Be, three that are moderately so, and one that is Li- and Be- normal. We have extensive observational and theoretical experience using Li and Be (and have CYCLE2 time to use B) as probes of stellar structure. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 5.42 par: 0 10. Num targs pri: 8 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: HRS ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 4591c PI: Ann M. Boesgaard Proposal Title: BORON IN LI- AND BE- DEFICIENT F STARS, A KEY DISCRIMINATOR OF STELLAR EVOLUTION SCENARIOS ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Pi Ann M. Boesgaard 3150 USA David L. Lambert UNIVERSITY OF TEXAS USA Constantine P. Deliyannis UNIVERSITY OF HAWAII USA Page 3 ------------------------------------------------------------------------------------ 2. Scientific Justification. INTRODUCTION. With HST and GHRS, Boron joins Li and Be as a probe of stellar structure and evolution. Indeed, it is when all three elements are considered simultaneously that the most powerful constraints on stellar models are realized. This proposal is concerned with the depletion of B in stars of the Li-dip that are greatly depleted in Li and Be. The proposal is a development of our successful analyses of B in halo and disk stars. We also have had extensive observational and theoretical experience using Li and Be (and have CYCLE2 time to use B) as probes of stellar structure and evolution. THE LI-DIP. In increasing order of stability, Li, Be, and B are all destroyed by (p,alpha) reactions at a few million degrees in stellar interiors. Boesgaard and Tripicco (1986 ApJ 302 L49) discovered that in a narrow Teff region of a few hundred degrees, F stars are able to severely deplete their surface Li abundance. This startling discovery of a Li-dip blatantly contradicted the predictions of standard stellar evolution theory : in standard models, Li is preserved in the outermost several % of the mass (after the ZAMS), yet the surface convection zone occupies 0.1% of the mass or less. Hence, there is no way to affect the surface Li abundance in these models (e.g. as might be the case in lower mass stars, where Li burning occurs at the base of the convection zone). To make matters worse, there is an accompanying Be-dip, but not in the Hyades (Boesgaard and Budge 1989 ApJ 338 875); deficiency of Be must develop more slowly than the corresponding Li one. Be-deficient F stars are known (Boesgaard 1976 ApJ 210 466). To explain the Li dip, proposed physical mechanisms (beyond the standard model) have proliferated in recent years. These include mass loss (Schramm et al. 1990 ApJL 359 L55), microscopic diffusion (Michaud 1986 ApJ 302 650), meridional circulation (Charbonneau and Michaud 1988 ApJ 334 746), overshoot, turbulent diffusion (Vauclair 1988 ApJ 335 971), and rotationally-induced mixing related to the onset of instabilities that cause angular momentum transport (Pinsonneault et al. 1990 ApJS 74 501, "Yale" models). It is not yet clear which of these (if any) is correct. While each of the above mechanisms can allegedly form a Li dip, each mechanism leaves different Be and B abundance signatures. We propose to add B to Li and Be observations as a powerful tool to uncover and decipher the signature of the responsible mechanism(s). As an example of the power of using more than one element at a time, consider 110 Her, which is definitively depleted in Be by a factor of 5-10, and in Li by a factor of 100-200, yet still retains a detectable abundance of Li (Boesgaard and Lavery 1986 ApJ 309 762). Since Be survives to about twice the ZAMS depth as does Li, this remarkable pattern of having depleted surface Be without having also depleted all the surface Li requires specific circumstances, which severely constrain or eliminate most of the proposed mechanisms (Deliyannis and Pinsonneault 1992 in IAU Colloquium #137, ed. W.W. Weiss, ASP Conference Series, in press). For example, mass loss is argued against because it wipes out surface Li before surface Be is affected ; mechanisms requiring rapid mixing are similarly argued against. Proposed diffusion scenarios are also argued against because, in one case, Li and Be deplete comparably, and in another case the Be abundance increases even as Li decreases. However, the Yale rotational models (which yield slow mixing) agree both qualitatively and quantitatively with 110 Her. Still more stringent constraints are required, and adding B will multiply our power to discriminate between stellar evolutionary scenarios. Our previous observations suggest that B is underabundant in Procyon by a factor of 3 relative to the two Li- and Be- normal dwarfs Theta UMa and Iota Peg. This mild deficiency and the ordering Li>Be>B of the deficiencies are both consistent with destruction, perhaps aided by mixing, but not with pure diffusion. In the case of diffusion, studies of other elements have shown none of the anomalies predicted (Boesgaard and Lavery 1986 ApJ 309 762). Further discriminatory constraints, and determining the details of how mixing occurs (if this is the correct scenario) will require solid observations of B. First, we propose to complete our investigation of Procyon (Be - poor by a factor of 45 or more). This will include an examination of the 11B/10B isotope ratio at 2090A, which will provide further information about the possible destruction mechanisms at work, since the two isotopes burn at slightly different temperatures. Next, since, as Procyon suggests, the most Be-deficient stars are the ones most likely to be deficient in B, we propose to look at Sigma Boo and Theta Cyg, which are both also severely Be-deficient. At what level of Be-deficiency does B deficiency begin? In analogy with 110 Her, the strongest contraints would be obtained if stars with barely detectable Be already showed a B deficiency (but the constraints will still be quite strong even if such stars do NOT show a B deficiency). We propose to investigate this question by including HR 244 (Figure 1) and HR 6541, for which our recent CFHT spectra show barely detectable Be lines. (Note that in 110 Her, which is "moderately" depleted in Be, B will be observed as part of our CYCLE2 GO3614.) Light element depletion is predicted (and also observed) to be a strong function of metallicity (e.g. Deliyannis, Demarque, and Kawaler 1990 ApJS 73 21; Deliyannis and Pinsonneault 1990 ApJL 367 L67); observations of B in old disk stars will therefore provide additional important constraints. We thus include the somewhat metal-deficient star 62 UMa, which shows no (CFHT) Be line (see Figure 1), and Sigma Peg, which shows a barely detectable Be line. Finally, we include the Li- and Be- normal star HR 235 as a standard. We stress that we have excellent CCD spectra of all these stars in the Be region (e.g. Figure 1), as well as high resolution and high S/N spectra of the Li region. BORON AND HST. In F dwarfs B is detectable via the B I resonance lines at 2496.8 and 2089.6A. (The other lines of these multiplets are blended.) The 2496.8A line provides reliable results for F dwarfs - see Figure 2 for ECH-B and G270M observations of Procyon and Theta Uma. Johansson et al. (preprint) find the two lines to have the same gf-value with 2089.6A having an isotope shift of 25mA which is measureable with ECH-B. Synthetic spectra with the best available line lists suggest the 2089.6A line is unblended; the line appears in the solar spectrum for example. We propose to observe the following sharp-lined stars : 1. Procyon with ECH-B at 2497 and 2090A, Sigma Boo and 62 UMa with G270M at 2497A, and Theta Cyg with ECH-B at 2497A, for B in stars with only upper limits to Be (and thus extremely deficient Be). 2. HR 244, HR 6541, and Sigma Peg with G270M at 2497A, for B in stars with barely detected (and significantly deficient) Be. 3. HR 235 with G270M at 2497A, for B in a Li- and Be- normal star, as a standard. Page 4 ------------------------------------------------------------------------------------ 3. Description of proposed observations. The proposed observations use B in F stars as a probe of stellar structure. 1. Procyon will be observed at 2497A with ECH-B to determine a reliable B depletion factor. 2. Six Be-poor stars (with different degrees of Be depletion, both with solar metallicity and slightly metal-poor) and one Be-normal star will be observed at 2497A with either ECH-B or G270M to get a S/N = 60-100. ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. Boron is a trace element with no detectable transitions in the visible or infrared spectra of main sequence stars. It is essential to measure the B abundance and not rely on inferences from Be. IUE lacks the spectral resolution and the S/N to detect the B I lines. This is well seen by the fact after more than a decade of IUE activity the only papers on the B I line are two providing dull upper limits to the B abundance in metal-poor stars. Our GHRS observations show that the real B abundance in such stars is 1.0 dex or more below the not very convincing IUE upper limits. Lack of IUE activity on B is not due to oversight or benign neglect by observers. Boron abundances for A to B stars (Teff = 10,000 to 20,000 K) were derived by Boesgaard and Heacox (1978, ApJ 226 888) from Copernicus spectra of the B II 1362A resonance line. (Their mean B abundance is in good agreement with our values for Theta Uma and Iota Peg from the B I line.) While the B II line should be exploited with HST, it will not provide the information sought under this proposal because (i) The Be-deficient stars of the Li-gap are too cool to emit photospheric radiation at 1362A and B is predominantly neutral, and (ii) the B II line has a very small isotopic shift and does not permit a measurement of the 11B/10B ratio. In short, our proposal can only be done with HST and the GHRS. In determining the B abundance four options are available: ECH-B or G270M at 2497A, and ECH-B or G200M at 2090A. For the typical F dwarf the relative count rates per pixel of the four options are ECH-B at 2497A = 1.0 ECH-B at 2090A = 1.1 G270M at 2497A = 13.0 G200M at 2090A = 2.4 In estimating the count rates, we have taken fluxes from the IUE Spectral Atlas for aprogram star or estimated the flux from a star of the same spectral type taking account of the differences in the V magnitudes. The recipe was checked against our GTO observations of Procyon, Theta Uma, and Iota Peg. Our experience with spectra at 2497A shows that a S/N = 60-100 is needed. While ECH-B is always desired, G270M (or G200M) is useful (Figure 2). ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. NONE. ------------------------------------------------------------------------------------ 6. Description of special calibration exposures. None. ------------------------------------------------------------------------------------ 7. Data reduction and analysis plans. We have previously pioneered B detections both in Pop I stars (eg Boesgaard and Heacox 1978 ApJ 226 888) and in Pop II stars from HST (below). In Austin, we have exercised all the tools needed to extract B abundances from the spectra. Our GTO spectra of three halo dwarfs have been reduced, analyzed, and interpreted - see Duncan, Lambert, and Lemke (1992, ApJ, in press). A paper is in preparation on B in the F dwarfs Theta Uma, Iota Peg, and Procyon. The new spectra can therefore be reduced in a timely fashion. A line list for the new 2090A region is available. The PI with D Lambert will assume responsibility for the analysis. Interpretation of the B abundances will be done primarily by C Deliyannis with the support of the PI and CoI. Deliyannis has extensive experience in the modelling of the structure of F dwarfs. We are completely ready to analyze and interpret the data. ------------------------------------------------------------------------------------ 8. Additional comments or special requests. None. Page 5 ------------------------------------------------------------------------------------ 9. Description of previous HST work. Lambert is PI on all these GTO proposals and a Co-I on the GO proposals: GTO1064 Boron in Main Sequence Stars, related GTO1065 Isotopic Abundances of Carbon and Oxygen and Fractionation of Interstellar Carbon Monoxide, not related GTO1066 Carbon Chemistry in Interstellar Diffuse Clouds, not related GTO1067 Old Novae and Cataclysmic Variables - DQ Her, not related GTO1068 Epsilon Aurigae- A Search for the Secondary, not related GO3824 A Search for Silicon and Carbon in GP Com, not related GO3479 Boron in Pop. II Dwarfs - Primeval or Spallated?, related Deliyannis is a Co-I on the following GO proposal: GO3614 Boron as a Probe of Stellar Structure and Mass Loss, related GTO observations of three halo dwarfs with [Fe/H] = -2.6 to -1.1 showed the B abundance to increase linearly with [Fe/H]. The B abundances with published Be abundances show that B/Be = 10 for the halo. This ratio is that predicted for Be and B production by spallation induced by cosmic rays. There is no evidence that either Be or B were produced in significant levels by the Big Bang, a prediction consistent with models of standard Big Bangs. No observations have yet been made under GO3479 which is intended to provide ECH-B spectra of two halo dwarfs. Boron has been shown to be depleted slightly in the very Be-por F star Procyon. The B abundance of two Be-normal F dwarfs is close to solar and the abundance seen previously in B and A type stars. 3614 : data not yet obtained. First Results from the GHRS: C I, S I, and CO toward Xi Persei and the Physical Conditions of the Diffuse Clouds. A M Smith, F C Bruhweiler, D L Lambert, B D Savage, J A Cardelli, D C Ebbets, C-H Lyu, & Y Sheffer, ApJ, 377, L61, 1991. Fractionation of CO in the Diffuse Clouds toward Zeta Oph, Y Sheffer, S R Federman, D L Lambert, & J A Cardelli, ApJ, in press, 1992. The Abundance of Boron in three Halo Stars, D K Duncan, D L Lambert, & M Lemke, ApJ, in press, 1992. ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). Adequate facilities for the reduction of the GHRS spectra and computation of synthetic spectra are available at Texas and Hawaii. Models of stellar interiors are readily calculated in Hawaii. ------------------------------------------------------------------------------------ 11. Address Information Name: ANN M. BOESGAARD Category: PI Institution: 3150 Address: PENN STATE UNIVERSITY 525 DAVEY LAB City: UNIVERSITY PARK State: PA Zip Code: 16802 Country: USA Telephone: 814-865-0418 Telex (or e-mail): ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 4591c [ 6] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial |Acqui|FLX| Flux data No | Name | Description | Position |Eqnx | Vel. |Prblm|REF| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 1 HD4813 PHI- A,134 RA = 0H 50M 7.5S +/- 0.1S, J2000 V = +8 1 V=5.19, TYPE=F7IV, B-V=0.50 CET HR235 DEC = -10D 38' 40" +/- 1.0" Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec) J 2000.00 -0.0156 +/- 0.0007 -0.2230 +/- 0.0020 0.0650 +/- 0.0100 ------------------------------------------------------------------------------------------------------------------------------------ 2 HD61421 A,134 RA = 7H 39M 18.1S +/- 0.01S, J2000 V = -3 1 V = 0.38, TYPE=F5IV, B-V = 0.42 PROCYON DEC = +5D 13' 30.1" +/- HR2943 0.02" Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec) B 2000.00 -0.0473 +/- 0.0003 -1.0290 +/- 0.0010 0.2920 +/- 0.0100 ------------------------------------------------------------------------------------------------------------------------------------ 3 HD128167 SIG A,134 RA = 14H 34M 40.8S +/- 0.1S, J2000 V = 0 1 V = 4.46, TYPE = F2V, B-V = 0.36 -BOO HR5447 DEC = +29D 44' 42.5" +/- 0.02" Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec) J 2000.00 0.0145 +/- 0.0005 0.1290 +/- 0.0010 0.0680 +/- 0.0100 ------------------------------------------------------------------------------------------------------------------------------------ 4 HD185395 THE A,134 RA = 19H 36M 26.5S +/- J2000 V = -28 1 V = 4.48, TYPE = F4V, B-V = 0.38 -CYG HR7469 0.01S, DEC = +50D 13' 15.8" +/- 0.02" Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec) J 2000.00 -0.0025 +/- 0.0010 0.2560 +/- 0.0010 0.0560 +/- 0.0100 ------------------------------------------------------------------------------------------------------------------------------------ 5 HD101606 62- A,134 RA = 11H 41M 34.3S +/- J2000 V = +32 1 V = 5.73, TYPE = F4V, B-V = 0.43 UMA HR4501 0.09S, DEC = +31D 44' 45.5" +/- 0.09" Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec) J 2000.00 -0.0274 +/- 0.0030 0.0190 +/- 0.0020 0.0260 +/- 0.0100 ------------------------------------------------------------------------------------------------------------------------------------ 6 HD5015 HR244 A,134 RA = 0H 53M 4.2S +/- 0.09S, J2000 V = +21 1 V = 4.82, TYPE = F8V, B-V = 0.53 DEC = +61D 7' 26.5" +/- 0.09" Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec) J 2000.00 -0.0098 +/- 0.0030 0.1780 +/- 0.0020 0.0660 +/- 0.0100 ------------------------------------------------------------------------------------------------------------------------------------ 7 HD159332 A,134 RA = 17H 33M 22.8S +/- J2000 V = -59 1 V = 5.64, TYPE = F6V, B-V = 0.48 HR6541 0.03S, DEC = +19D 15' 24.0" +/- .03" Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec) J 2000.00 -0.0022 +/- 0.0040 -0.0930 +/- 0.0040 0.0320 +/- 0.0100 ------------------------------------------------------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 4591c [ 7] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial |Acqui|FLX| Flux data No | Name | Description | Position |Eqnx | Vel. |Prblm|REF| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 8 HD216385 SIG A,134 RA = 22H 52M 24.1S +/- J2000 V = +12 1 V = 5.16, TYPE = F7IV, B-V = 0.48 -PEG HR8697 0.03S, DEC = +9D 50' 8.4" +/- 0.03" Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec) J 2000.00 0.0353 +/- 0.0010 0.0490 +/- 0.0100 0.0430 +/- 0.0100 ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 4591c [ 8] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 1 HD4813 HRS ACQ 2.0 MIRROR-A2 BRIGHT=RETURN 1 3.6S 25 1 1 CYCLE 3 / 1.0-1.2 0.4S ONBOARD ACQ FOR 1.1 Comments: STEP-TIME=0.4S ------------------------------------------------------------------------------------------------------------------------------------ 1.1 HD4813 HRS ACQ/ 0.25 MIRROR-A2 SEARCH-SIZE=5 1 75S 25 1 1 CYCLE 3 PEAKUP 3.0S ONBOARD ACQ FOR 1.2 Comments: STEP-TIME=3.0S ------------------------------------------------------------------------------------------------------------------------------------ 1.2 HD4813 HRS ACCUM 0.25 G270M 2497 STEP-PATT=5 1 30.0M 80 1 1 CYCLE 3 FP-SPLIT=STD 30.0M ------------------------------------------------------------------------------------------------------------------------------------ 2 HD61421 HRS ACQ 2.0 MIRROR-A2 BRIGHT=RETURN 1 3.6S 25 1 1 CYCLE 3 / 2.0-2.2 0.4S ONBOARD ACQ FOR 2.1 Comments: STEP-TIME=0.4S ------------------------------------------------------------------------------------------------------------------------------------ 2.1 HD61421 HRS ACQ/ 0.25 MIRROR-A2 SEARCH-SIZE=5 1 50S 25 1 1 CYCLE 3 PEAKUP 2.0S ONBOARD ACQ FOR 2.2 Comments: STEP-TIME=2.0S ------------------------------------------------------------------------------------------------------------------------------------ 2.2 HD61421 HRS ACCUM 0.25 ECH-B 2497 STEP-PATT=7 2 20.0M 80 1 1 CYCLE 3 FP-SPLIT=STD 40.0M ------------------------------------------------------------------------------------------------------------------------------------ 3 HD128167 HRS ACQ 2.0 MIRROR-A2 BRIGHT=RETURN 1 3.6S 25 1 1 CYCLE 3 / 3.0-3.1 0.4S ONBOARD ACQ FOR 3.1 Comments: STEP-TIME=0.4S ------------------------------------------------------------------------------------------------------------------------------------ 3.1 HD128167 HRS ACQ/ 0.25 MIRROR-A2 SEARCH-SIZE=5 1 50S 25 1 1 CYCLE 3 PEAKUP 2.0S ONBOARD ACQ FOR 3.2 Comments: STEP-TIME=2.0S ------------------------------------------------------------------------------------------------------------------------------------ 3.2 HD128167 HRS ACCUM 0.25 G270M 2497 STEP-PATT=5 1 25.0M 80 1 1 CYCLE 3 FP-SPLIT=STD 25.0M ------------------------------------------------------------------------------------------------------------------------------------ 4 HD185395 HRS ACQ 2.0 MIRROR-A2 BRIGHT=RETURN 1 3.6S 25 1 1 CYCLE 3 / 4.0-4.1 0.4S ONBOARD ACQ FOR 4.1 Comments: STEP-TIME=0.4S ------------------------------------------------------------------------------------------------------------------------------------ 4.1 HD185395 HRS ACQ/ 0.25 MIRROR-A2 SEARCH-SIZE=5 1 50S 25 1 1 CYCLE 3 PEAKUP 2.0S ONBOARD ACQ FOR 4.2 Comments: STEP-TIME=2.0S ------------------------------------------------------------------------------------------------------------------------------------ 4.2 HD185395 HRS ACCUM 0.25 ECH-B 2497 STEP-PATT=7 3 27.0M 80 1 1 CYCLE 3 FP-SPLIT=STD 81.0M ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 4591c [ 9] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 5 HD101606 HRS ACQ 2.0 MIRROR-A2 BRIGHT=RETURN 1 3.6S 25 1 1 CYCLE 3 / 5.0-5.2 0.4S ONBOARD ACQ FOR 5.1 Comments: STEP-TIME=0.4S ------------------------------------------------------------------------------------------------------------------------------------ 5.1 HD101606 HRS ACQ/ 0.25 MIRROR-A2 SEARCH-SIZE=5 1 75S 25 1 1 CYCLE 3 PEAKUP 3.0S ONBOARD ACQ FOR 5.2 Comments: STEP-TIME=3.0S ------------------------------------------------------------------------------------------------------------------------------------ 5.2 HD101606 HRS ACCUM 0.25 G270M 2497 STEP-PATT=5 2 23.0M 80 1 1 CYCLE 3 FP-SPLIT=STD 46.0M ------------------------------------------------------------------------------------------------------------------------------------ 6 HD5015 HRS ACQ 2.0 MIRROR-A2 BRIGHT=RETURN 1 3.6S 25 1 1 CYCLE 3 / 6.0-6.2 0.4S ONBOARD ACQ FOR 6.1 Comments: STEP-TIME=0.4S ------------------------------------------------------------------------------------------------------------------------------------ 6.1 HD5015 HRS ACQ/ 0.25 MIRROR-A2 SEARCH-SIZE=5 1 50S 25 1 1 CYCLE 3 PEAKUP 2.0S ONBOARD ACQ FOR 6.2 Comments: STEP-TIME=2.0S ------------------------------------------------------------------------------------------------------------------------------------ 6.2 HD5015 HRS ACCUM 0.25 G270M 2497 STEP-PATT=5 1 30.0M 80 1 1 CYCLE 3 FP-SPLIT=STD 30.0M ------------------------------------------------------------------------------------------------------------------------------------ 7 HD159332 HRS ACQ 2.0 MIRROR-A2 BRIGHT=RETURN 1 3.6S 25 1 1 CYCLE 3 / 7.0-7.2 0.4S ONBOARD ACQ FOR 7.1 Comments: STEP-TIME=0.4S ------------------------------------------------------------------------------------------------------------------------------------ 7.1 HD159332 HRS ACQ/ 0.25 MIRROR-A2 SEARCH-SIZE=5 1 75S 25 1 1 CYCLE 3 PEAKUP 3.0S ONBOARD ACQ FOR 7.2 Comments: STEP-TIME=3.0S ------------------------------------------------------------------------------------------------------------------------------------ 7.2 HD159332 HRS ACCUM 0.25 G270M 2497 STEP-PATT=5 2 23.0M 80 1 1 CYCLE 3 FP-SPLIT=STD 46.0M ------------------------------------------------------------------------------------------------------------------------------------ 8 HD216385 HRS ACQ 2.0 MIRROR-A2 BRIGHT=RETURN 1 3.6S 25 1 1 CYCLE 3 / 8.0-8.2 0.4S ONBOARD ACQ FOR 8.1 Comments: STEP-TIME=0.4S ------------------------------------------------------------------------------------------------------------------------------------ 8.1 HD216385 HRS ACQ/ 0.25 MIRROR-A2 SEARCH-SIZE=5 1 75S 25 1 1 CYCLE 3 PEAKUP 3.0S ONBOARD ACQ FOR 8.2 Comments: STEP-TIME=3.0S ------------------------------------------------------------------------------------------------------------------------------------ 8.2 HD216385 HRS ACCUM 0.25 G270M 2497 STEP-PATT=5 1 30.0M 80 1 1 CYCLE 3 FP-SPLIT=STD 30.0M ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 4591c [ 10] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations HRS ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACQ ACQ/PEAKUP ACCUM ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters BRIGHT=RETURN SEARCH-SIZE=5 STEP-PATT=5 FP-SPLIT=STD STEP-PATT=7 ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 5.42 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category COOL STARS ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category STELLAR ATMOSPHERES ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements CYCLE 3 / 1.0-1.2; ONBOARD ACQ FOR 1.1 CYCLE 3; ONBOARD ACQ FOR 1.2 CYCLE 3 CYCLE 3 / 2.0-2.2; ONBOARD ACQ FOR 2.1 ONBOARD ACQ FOR 2.2 CYCLE 3 / 3.0-3.1; ONBOARD ACQ FOR 3.1 ONBOARD ACQ FOR 3.2 CYCLE 3 / 4.0-4.1; ONBOARD ACQ FOR 4.1 ONBOARD ACQ FOR 4.2 CYCLE 3 / 5.0-5.2; ONBOARD ACQ FOR 5.1 ONBOARD ACQ FOR 5.2 CYCLE 3 / 6.0-6.2; ONBOARD ACQ FOR 6.1 ONBOARD ACQ FOR 6.2 CYCLE 3 / 7.0-7.2; ONBOARD ACQ FOR 7.1 ONBOARD ACQ FOR 7.2 CYCLE 3 / 8.0-8.2; ONBOARD ACQ FOR 8.1 ONBOARD ACQ FOR 8.2 ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements MIRROR-A2 G270M ECH-B ------------------------------------------------------------------------------------------------------------------------------------ Target Names HD4813 PHI-CET HR235 HD61421 PROCYON HR2943 HD128167 SIG-BOO HR5447 HD185395 THE-CYG HR7469 HD101606 62-UMA HR4501 HD5015 HR244 HD159332 HR6541 HD216385 SIG-PEG HR8697 ------------------------------------------------------------------------------------------------------------------------------------