! $Id: 5323,v 6.1 1994/07/27 16:35:40 pepsa Exp $ coverpage: title_1: ATMOSPHERIC DYNAMICS AND MASS LOSS IN title_2: GAPPERS, CLUMPERS, AND HYBRIDS CYC4 - MEDIUM sci_cat: COOL STARS sci_subcat: ATMOSPHERES & WINDS proposal_for: GO pi_fname: THOMAS pi_mi: R. pi_lname: AYRES pi_inst: 1762 pi_country: USA pi_phone: 303-492-4051 keywords_1: STAR, G III-I, K III-I, CORONA, WIND hours_pri: 10.48 num_pri: 3 hrs: Y funds_amount: 59202 funds_length: 12 funds_date: MAR-94 pi_position: RESEARCH PROFESSOR off_fname: LAURENCE off_mi: D. off_lname: NELSON off_title: DIRECTOR off_inst: 1760 off_addr_1: OFFICE OF CONTRACTS AND GRANTS off_addr_2: CAMPUS BOX 19 off_city: BOULDER off_state: CO off_zip: 80309 off_country: USA off_phone: 303-492-2695 ! end of coverpage abstract: line_1: The giant branch evolution of moderate-mass stars provides a vital test of line_2: our understanding of magnetic dynamo action, coronal energization, and winds. line_3: The blatant``X-ray deficiency'' of the Hertzsprung-gap giants appears to line_4: be genuine, while that of many ``hybrid-chromosphere'' supergiants appears line_5: to be due to absorption by a previously unrecognized warm or hot component of line_6: their winds; not apparent in the Mg II circumstellar features but quite line_7: evident in the H I Lyman-alpha profile (of at least one case). There also line_8: is new evidence for a warm wind on the G0 secondary of Capella -- a ``gap'' line_9: star. The mass-loss rate is low, but dynamically quite significant in line_10: braking the fast stellar rotation. Outflows of some kind probably exist on line_11: post-helium-flash Clump giants, as well, although ``antiwinds'' are the line_12: hallmark of the archetype, Beta Ceti. I propose to clarify the subcoronal line_13: properties of the Hertzsprung-gap, active Clump, and Hybrid stars through a line_14: spectral dissection of one representative of each class. My strategy is to line_15: use the HST/GHRS to record key FUV emissions -- spanning the broad line_16: temperature range 10,000-250,000 K -- with high S/N to measure line widths, line_17: profile asymmetries, circumstellar absorptions, systematic Doppler shifts, line_18: and density-sensitive line ratios. Such diagnostics will be used to constrain line_19: existing physical models, and develop new ones. The HST spectra will strongly line_20: complement ongoing X-ray work with ROSAT and recent EUVE spectroscopy. ! ! end of abstract general_form_proposers: lname: AYRES fname: THOMAS title: DR. inst: COLORADO, UNIVERSITY OF country: USA esa: N ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The observational objective is to acquire selected important spectral line_2: diagnostics of the dynamical and structural properties of the sub- line_3: coronal layers and winds of three pivotal giants either in or near the line_4: Hertzsprung gap, or in the post-helium-flash Clump. As a side benefit, line_5: the chromospheric H I & Mg II emissions contain ISM components that line_6: probe local sightlines. line_7: The observation plan, in order of priority, is as follows: line_8: ========================================================================== line_9: setting/aper wavelengths purpose line_10: -------------------------------------------------------------------------- line_11: (1) G160M/LSA 1205-1240 moderate S/N profiles of key emission-measure line_12: (1') -- /SSA -- species O V] 1218 (250,000 K) and N V 1238 line_13: (200,000 K); high S/N profiles of strong chromo- line_14: spheric feature H I 1215 (<20,000 K) and Si III line_15: 1206 (30,000 K). Use short exposure with SSA line_16: to suppress geocoronal H I in extreme core of line_17: stellar H I emission profile; use deeper exp- line_18: osure through LSA to obtain moderate (>20:1 line_19: at peak) S/N profiles of fainter emissions. ! question: 3 section: 2 line_1: (2) G160M/LSA 1386-1420 high S/N profiles of Si IV 1393,1402; detections line_2: of density-sensitive O IV] 1401,04,07 multiplet line_4: (3) G160M/LSA 1538-1572 high S/N profiles of key emission-measure spec- line_5: ies C IV 1548,50 (100,000 K); detect possible line_6: warm wind absorption features. line_8: (4)ECH-B20/SSA 2791-2805 very high S/N profiles of key chromospheric line_9: emissions Mg II 2795,802. SSA for best resol- line_10: ution of LISM and/or circumstellar components. line_11: ------------------------------------------------------------------------- line_12: I intend to obtain sufficient S/N to record not only the line fluxes but line_13: also the profile shapes and any systematic Doppler shifts of the high- line_14: excitation species. The profile widths indicate the amplitudes of non- line_15: thermal Doppler motions in the 30,000-250,000 K layers of the transition line_16: zone, which play a crucial role in theories of the subcoronal energy line_17: balance. Any systematic line shifts could be related to large-scale bulk line_18: flows of material, like the redshifts (antiwinds) of Si IV-C IV tempera- line_19: ture gas routinely observed in coronal stars of all luminosity classes, line_20: and thought to be connected with the TZ downdrafts seen in coronal mag- line_21: netic loops on the Sun. Finally, the high resolution (20,000) and high line_22: S/N (>30) obtainable on the Si IV 1393 and C IV 1548 features might line_23: permit the detection of blue-shifted absorptions due to warm winds. ! question: 4 section: 1 line_1: line_2: The object of the program is to study the subcoronal properties of line_3: pivotal stars selected from X-ray/C IV correlation diagrams. The line_4: appropriate diagnostics (of 30,000-200,000 K gas) are high-excitation line_5: emissions of the FUV region: the dramatic differences between the line_6: various groups seen in their behavior of C IV vis-a-vis X-rays is not line_7: mirrored in the Ca II or H-alpha lines, for example. line_9: All three of the target stars have been studied extensively with the IUE line_10: in its low-resolution (5 A) mode. Thirty-one Comae has been attempted line_11: once, Beta Ceti twice, and Alpha TrA several times in the R=10,000 FUV line_12: echelle mode of IUE. However, the resulting spectra -- the deepest pos- line_13: sible with IUE -- are of marginal value (C IV faint; Lyman alpha severely line_14: contaminated by overexposed geocoronal emission; O IV] well below sensi- line_15: tivity threshholds). Indeed, the key O IV] features have been seen by line_16: IUE (faintly) in only two `normal' late-type stars: Alpha Aurigae Ab line_17: (G0 III) and Beta Draconis (G2 Ib), both of which are significantly line_18: brighter FUV sources than the three giants proposed here. (Incident- line_19: ally, Capella itself is not a suitable target for the present purpose line_20: because the FUV emissions from the two stars -- one an active Clump ! question: 4 section: 2 line_1: giant, the other a Hertzsprung-gap giant -- are blended at all orbital line_2: phases, and difficult to unambiguously separate.) line_4: By virtue of the RIASS program, the three targets have been studied in line_5: detail based on ROSAT survey material: 31 Com and Beta Cet were strong line_6: detections by the PSPC, both having sufficient counts for a crude det- line_7: ermination of the coronal temperature; and both class-III giants were line_8: seen by the WFC in its S2 filter. Indeed, I am PI of an EUVE spectro- line_9: scopy program to record both giants: observations of 31 Com already were line_10: obtained in February 1993. Alpha TrA was a relatively weak PSPC detect- line_11: ion in the RASS, but was the subject of a deep ROSAT pointing by R. Ros- line_12: ner and collaborators. Unfortunately, Alpha TrA is too absorbed in the line_13: 100-300 A region to provide a useable EUVE spectrum. line_15: My colleague J. Linsky (JILA) has obtained GHRS/GTO observations of line_16: selected FUV emissions, and the Mg II h & k lines, in Alpha TrA very line_17: recently. However, owing to lack of observing time, he dropped ob- line_18: servations of the 1205-1240 A region because -- at the time the Phase line_19: II plan was prepared -- Lyman-alpha was believed to be uninteresting. line_20: However, the very recent recognition of anomalous blueward absorption ! question: 4 section: 3 line_1: in IUE profiles of Lyman-alpha has elevated that interval to one of line_2: crucial importance. Thus I propose here to obtain a spectrum of the line_3: vital 1205-1240 A region, but will not duplicate the other FUV set- line_4: tings already acquired by Linsky. A brief exposure of Mg II h & k line_5: at echelle resolution is warranted, however, because the profiles are line_6: known to be variable. line_8: Thus, the proposed HST investigation builds upon a strong base of pre- line_9: vious and current work, which however has reached the limitations of line_10: the historical FUV instrumentation. Only the HST/GHRS can provide the line_11: new high S/N, high spectral resolution material required to make further line_12: progress in understanding the wide diversity in the coronal/subcoronal line_13: properties of stars in the moderate-mass sector of the giant branch. line_15: I obtained FUV emission fluxes for the three proposed targets from coadded line_16: IUE SWP-LO spectra, and additional values for H I Lyman-alpha from a recent line_17: survey of high-resolution profiles by myself and collaborators. I estimated line_18: line widths by reference to existing (weak) SWP-HI spectra of the the C IV line_19: emissions of the program stars. The table below provides a summary of the line_20: typical peak flux values, proposed exposure times, and expected S/N ratios. ! question: 4 section: 4 line_1: line_2: ===================================================================== line_3: prio.| exp. 1 & 1' | exp. 2 | exp. 3 | exp. 4 | line_4: --------------------------------------------------------------------- line_5: | Si III H I N V | Si IV O IV] | C IV | Mg II | line_6: | 1206 1215 1238 | 1393 1401 | 1548 | 2795 | line_7: ===================================================================== line_8: -- 31 Comae (G0 III) -- line_9: --------------------------------------------------------------------- line_10: Flux | 8: 60 3 | 7 0.5: | 16 | 90 | line_11: --------------------------------------------------------------------- line_12: texp | 65M LSA + 10M SSA | 70M LSA | 30M LSA | 25M SSA | line_13: --------------------------------------------------------------------- line_14: S/N | 30 40/ssb 20 | 40 10: | 35 | 50/ssb | line_15: ===================================================================== line_16: -- Beta Ceti (K0 III) -- line_17: --------------------------------------------------------------------- line_18: Flux | 15: 120 11 | 12 1: | 8 | 500 | line_19: --------------------------------------------------------------------- line_20: texp | 30M LSA + 5M SSA | 45M LSA | 40M LSA | 5M SSA | ! question: 4 section: 5 line_1: --------------------------------------------------------------------- line_2: S/N | 30 40/ssb 25 | 40 10: | 30 | 50/ssb | line_3: ===================================================================== line_4: -- Alpha Trianguli Australis (K2 II-III) -- line_5: --------------------------------------------------------------------- line_6: Flux | 8: 80 5 | -- | -- | 700 | line_7: --------------------------------------------------------------------- line_8: texp | 65M LSA + 10M SSA | -- | -- | 5M SSA | line_9: --------------------------------------------------------------------- line_10: S/N | 30 50/ssb 25 | -- | -- | 60/ssb | line_11: ===================================================================== line_12: Notes: Fluxes in units of 1E-13 ergs/cm^2/s/A at Earth at line peak; line_13: S/N is either per resolution element (i.e., 1 diode), after line_14: smoothing over substep pattern, or per substep bin (ssb). line_16: For a well-resolved line (FWHM >> 1 diode), the S/N of the integrated flux line_17: is about twice the peak S/N (per diode), thus a peak S/N of 10 ensures an line_18: accuracy in the line flux of about 5%. For the density-sensitive O IV] line_19: lines, a 5% uncertainty in the flux ratio translates into a (very small) line_20: 15% uncertainty in the electron density over the range log N= 8.5-10.5 ! question: 4 section: 6 line_1: where the O IV] diagnostic is useful (and where the densities of the sub- line_2: coronal layers of evolved stars are thought to lie). In addition, a peak line_3: S/N of 10 or more will yield an accuracy in the emission centroid of about line_4: a tenth of a diode or better, or about 1.5 km/s for G160M. This is compar- line_5: able to the precision of the GHRS wavelength scales that can be achieved line_6: for a well-centered image in the LSA, with an accompanying lamp spectrum. ! question: 5 section: 1 line_1: Assurance of the precision of the wavelength scales of the medium-resolution line_2: and high-resolution spectra is essential to the scientific objectives of our line_3: program. Thus we propose to obtain wavelength calibrations for the G160M and line_4: ECH-B20 settings. The lamp exposures should be of order 60S or longer, to line_5: obtain the requisite accuracy in the assigned wavelength scales. ! question: 6 section: 1 line_1: OSF Line Number(s) Instrument Mode Special Calibration Requirement(s) line_2: ___________________ __________ _______ __________________________________ line_4: 1.0 -- 3.3 GHRS ACCUM Lamp exposures to ensure precis- line_5: ion of wavelength scales for line_6: G160M & ECH-B20 spectra. Should line_7: achieve S/N= 10, or better, in line_8: moderate-strength Pt II emissions ! ! ! question: 9 section: 1 line_1: P2485: ``Sleuthing the Dynamo: Cycle 1 Observations'' line_2: [peripherly related to present project] line_4: P3908: ``Sleuthing the Dynamo: Cycle 2 Observations'' line_5: [peripherly related to present project] line_7: P4492: ``The Distant Future of Solar Activity: Cycle 3 Observations'' line_8: [peripherly related to present project] line_10: P2485: all five targets observed fall `92; P3908: four of five line_11: targets observed fall `92. Spectra currently are being reduced line_12: and analyzed. P2485 targets were weaker than expected at C IV line_13: 1549; but P3908 targets were brighter, and one of the Pleiades G line_14: stars flared during one of the three orbits of observation with line_15: the FOS. The main results of the program will be presented at line_16: the summer `93 meeting of the AAS in Berkeley, and at the 8th line_17: Cambridge Workshop in the fall. line_19: P4492: No observations to date. ! question: 9 section: 2 line_1: ``GHRS observations of the local interstellar medium and the deuterium/hydrogen line_2: ratio along the line of sight towards Capella,'' Linsky, J. L., Brown, A., line_3: Gayley, K. G., Diplas, A., Savage, B. D., Ayres, T. R., Landsman, W., Shore, line_4: S., & Heap, S. R., Astrophysical Journal, 402, 694, (1993). line_6: ``The hydrogen Lyman alpha emission of Capella'', Ayres, T. R., Brown, A., line_7: Gayley, K. G., & Linsky, J. L., Astrophysical Journal, 402, 710, (1993). line_9: ``IUE far-ultraviolet spectra of Capella and Gamma Draconis for comparison to line_10: HST/GHRS GTO observations'', Ayres, T. R., in The First Year of HST Observat- line_11: ions, ed. A. L. Kinney and J. C. Blades (Baltimore: Space Telescope Science line_12: Institute), p. 216 (1991). line_14: ``A Remarkable FUV Flare on the Pleiades G Dwarf HZ 314'', Ayres,T., Basri, G., line_15: Simon, T., Stauffer, J., Stern, R., Antiochos, S., Bookbinder, J., Brown, A., line_16: Doschek, G., Linsky, J., Ramsey, L., & Walter, F., in Bull. Am. Astron. Soc. line_17: (in press, 1993). ! question: 10 section: 1 line_1: At the University of Colorado a version of the reduction software writ- line_2: ten by the GHRS team is available on a variety of platforms; as is line_3: IRAF/SDAS. We expect to conduct theoretical studies of the UV and line_4: X-ray emissions from stellar atmospheres using fast numerical simulat- line_5: ion codes recently implemented on high-performance workstations. line_6: These codes were developed originally for use with IUE and ROSAT/WFC line_7: data, and modified more recently for EUVE spectroscopy. Their appli- line_8: cation to the HST data is straightforward. There are a number of un- line_9: dergraduate and graduate students working on HST data, who potentially line_10: could contribute significantly to (and benefit intellectually from) line_11: the Sleuthing continuation. The University provides substantial help line_12: in the form of matching funds for hardware purchases and FTE funding line_13: for some of the computer system support staff and other essential line_14: administrative positions. ! !end of general form text general_form_address: lname: AYRES fname: THOMAS mi: R. category: PI inst: 1762 addr_1: CNTR. ASTROPHYS. & SPACE ASTRON. addr_2: CAMPUS BOX 389 (CASA) city: BOULDER state: CO zip: 80309 country: USA phone: 303-492-4051 telex: (SPAN) HYADES::AYRES ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD111812 name_2: 31-COM descr_1: A, 138, 901, 905 pos_1: RA = 12H 51M 41.84S +/- 0.03S, pos_2: DEC = +27D 32' 26.3" +/- 0.1" equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: -0.001000 dec_pm_val: -0.0130 an_prlx_val: 0.0110 an_prlx_unct: 0.0070 rv_or_z: V=-1 fluxnum_1: 1 fluxval_1: V = 4.94 +/- 0.10, TYPE = G0III fluxnum_2: 2 fluxval_2: B-V = +0.67 +/- 0.01 fluxnum_3: 3 fluxval_3: F-LINE(1215)= 60 +/- 10 E-13 fluxnum_4: 4 fluxval_4: W-LINE(1215)= 3 +/- 1 fluxnum_5: 5 fluxval_5: F-LINE(2795)= 90 +/- 10 E-13 fluxnum_6: 6 fluxval_6: W-LINE(2795)= 3 +/- 1 fluxnum_7: 7 fluxval_7: F-LINE(1393)= 7 +/- 1 E-13 fluxnum_8: 8 fluxval_8: W-LINE(1393)= 1 +/- 0.3 fluxnum_9: 9 fluxval_9: F-LINE(1548)= 16 +/- 3 E-13 fluxnum_10: 10 fluxval_10: W-LINE(1548)= 1 +/- 0.3 ! targnum: 2 name_1: HD4128 name_2: BETA-CET descr_1: A, 140, 901, 905 pos_1: RA = 0H 43M 35.30S +/- 0.03S, pos_2: DEC = -17D 59' 12.0" +/- 0.1" equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.016300 dec_pm_val: 0.0360 an_prlx_val: 0.0610 an_prlx_unct: 0.0070 rv_or_z: V=+13 fluxnum_1: 1 fluxval_1: V = 2.04 +/- 0.10, TYPE = K0III fluxnum_2: 2 fluxval_2: B-V = +1.02 +/- 0.01 fluxnum_3: 3 fluxval_3: F-LINE(1215)= 120 +/- 20 E-13 fluxnum_4: 4 fluxval_4: W-LINE(1215)= 2 +/- 1 fluxnum_5: 5 fluxval_5: F-LINE(2795)= 500 +/- 100 E-13 fluxnum_6: 6 fluxval_6: W-LINE(2795)= 2 +/- 1 fluxnum_7: 7 fluxval_7: F-LINE(1393)= 12 +/- 3 E-13 fluxnum_8: 8 fluxval_8: W-LINE(1393)= 1 +/- 0.3 fluxnum_9: 9 fluxval_9: F-LINE(1548)= 8 +/- 2 E-13 fluxnum_10: 10 fluxval_10: W-LINE(1548)= 1 +/- 0.3 ! targnum: 3 name_1: HD150798 name_2: ALPHA-TRA descr_1: A, 140, 901, 905 pos_1: RA = 16H 48M 39.89S +/- 0.03S, pos_2: DEC = -69D 1' 39.5" +/- 0.1" equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.005200 dec_pm_val: -0.0340 an_prlx_val: 0.0310 an_prlx_unct: 0.0070 rv_or_z: V=-3 fluxnum_1: 1 fluxval_1: V = 1.92 +/- 0.10, TYPE = K2II fluxnum_2: 2 fluxval_2: B-V = +1.44 +/- 0.01 fluxnum_3: 3 fluxval_3: F-LINE(1215)= 80 +/- 10 E-13 fluxnum_4: 4 fluxval_4: W-LINE(1215)= 3 +/- 1 fluxnum_5: 5 fluxval_5: F-LINE(2795)= 700 +/- 100 E-13 fluxnum_6: 6 fluxval_6: W-LINE(2795)= 3 +/- 1 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 2.000 sequence_1: DEFINE sequence_2: MAG targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B20 wavelength: 2798 num_exp: 1 time_per_exp: 32S s_to_n: 30 s_to_n_time: 30S priority: 1 param_1: STEP-PATT=3 param_2: DOPPLER=OFF req_1: CALIB FOR 2.1; req_2: SEQ 2-2.1 NO GAP ! linenum: 2.100 sequence_1: DEFINE sequence_2: MAG targname: # config: ^ opmode: ^ aperture: 0.25 sp_element: ^ wavelength: ^ num_exp: 1 time_per_exp: 326.4S s_to_n: # s_to_n_time: # fluxnum_1: 5 fluxnum_2: 6 priority: ^ param_1: STEP-PATT=7 param_2: FP-SPLIT=STD param_3: DOPPLER=ON ! linenum: 2.500 sequence_1: DEFINE sequence_2: MAG1 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B20 wavelength: 2798 num_exp: 1 time_per_exp: 32S s_to_n: 30 s_to_n_time: 30S priority: 1 param_1: STEP-PATT=3 param_2: DOPPLER=OFF req_1: CALIB FOR 2.6; req_2: SEQ 2.5-2.6 NO GAP ! linenum: 2.600 sequence_1: DEFINE sequence_2: MAG1 targname: # config: ^ opmode: ^ aperture: 0.25 sp_element: ^ wavelength: ^ num_exp: 1 time_per_exp: 1305.6S s_to_n: # s_to_n_time: # fluxnum_1: 5 fluxnum_2: 6 priority: ^ param_1: STEP-PATT=7 param_2: FP-SPLIT=STD param_3: DOPPLER=ON ! linenum: 3.000 sequence_1: DEFINE sequence_2: LYA1 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1223 num_exp: 1 time_per_exp: 64S s_to_n: 30 s_to_n_time: 30S priority: 1 param_1: STEP-PATT=3 param_2: DOPPLER=OFF req_1: CALIB FOR 3.1; req_2: SEQ 3-3.1 NO GAP ! linenum: 3.100 sequence_1: DEFINE sequence_2: LYA1 targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1223 num_exp: 1 time_per_exp: 326.4S s_to_n: # s_to_n_time: # fluxnum_1: 3 fluxnum_2: 4 priority: 3 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD param_3: DOPPLER=ON ! linenum: 3.500 sequence_1: DEFINE sequence_2: LYA11 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1223 num_exp: 1 time_per_exp: 64S s_to_n: 30 s_to_n_time: 30S priority: 1 param_1: STEP-PATT=3 param_2: DOPPLER=OFF req_1: CALIB FOR 3.6; req_2: SEQ 3.5-3.6 NO GAP ! linenum: 3.600 sequence_1: DEFINE sequence_2: LYA11 targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1223 num_exp: 1 time_per_exp: 652.8S s_to_n: # s_to_n_time: # fluxnum_1: 3 fluxnum_2: 4 priority: 3 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD param_3: DOPPLER=ON ! linenum: 3.800 sequence_1: DEFINE sequence_2: LYA2 targname: # config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1223 num_exp: # time_per_exp: 1523.2S s_to_n: # s_to_n_time: # fluxnum_1: 3 fluxnum_2: 4 priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD param_3: DOPPLER=ON ! linenum: 4.000 sequence_1: DEFINE sequence_2: SILI targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1403 num_exp: 1 time_per_exp: 64S s_to_n: 30 s_to_n_time: 30S priority: 1 param_1: STEP-PATT=3 param_2: DOPPLER=OFF req_1: CALIB FOR 4.1; req_2: SEQ 4-4.1 NO GAP ! linenum: 4.100 sequence_1: DEFINE sequence_2: SILI targname: # config: ^ opmode: ^ aperture: 2.0 sp_element: ^ wavelength: ^ num_exp: # time_per_exp: 1305.6S s_to_n: # s_to_n_time: # fluxnum_1: 7 fluxnum_2: 8 priority: ^ param_1: STEP-PATT=5 param_2: FP-SPLIT=STD param_3: DOPPLER=ON ! linenum: 5.000 sequence_1: DEFINE sequence_2: CARB targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1555 num_exp: 1 time_per_exp: 64S s_to_n: 30 s_to_n_time: 30S priority: 2 param_1: STEP-PATT=3 param_2: DOPPLER=OFF req_1: CALIB FOR 5.1; req_2: SEQ 5-5.1 NO GAP ! linenum: 5.100 sequence_1: DEFINE sequence_2: CARB targname: # config: ^ opmode: ^ aperture: 2.0 sp_element: ^ wavelength: ^ num_exp: 1 time_per_exp: 1305.6S s_to_n: # s_to_n_time: # fluxnum_1: 9 fluxnum_2: 10 priority: ^ param_1: STEP-PATT=5 param_2: FP-SPLIT=STD param_3: DOPPLER=ON ! linenum: 10.000 targname: HD111812 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 45S s_to_n: 70 s_to_n_time: 6S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: SEARCH-SIZE=3, param_2: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 10.1; req_2: CYCLE 4 / 10-10.7; req_3: SEQ 10-10.7 NO GAP; comment_1: STEP TIME = 5 SEC ! linenum: 10.100 targname: ^ config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 125S s_to_n: 70 s_to_n_time: 6S fluxnum_1: 1 fluxnum_2: 2 param_1: SEARCH-SIZE=5, priority: 1 req_1: ONBOARD ACQ FOR 10.2-10.7 comment_1: STEP-TIME=5 SEC ! linenum: 10.200 sequence_1: USE sequence_2: MAG1 targname: ^ s_to_n: 50 s_to_n_time: 25M ! linenum: 10.300 sequence_1: USE sequence_2: LYA11 targname: ^ s_to_n: 40 s_to_n_time: 70M ! linenum: 10.500 sequence_1: USE sequence_2: LYA2 targname: ^ num_exp: 2 s_to_n: 40 s_to_n_time: 70M ! linenum: 10.600 sequence_1: USE sequence_2: SILI targname: ^ num_exp: 3 s_to_n: 40 s_to_n_time: 70M ! linenum: 10.700 sequence_1: USE sequence_2: CARB targname: HD111812 s_to_n: 30 s_to_n_time: 30M ! linenum: 11.000 targname: HD4128 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 22.5S s_to_n: 70 s_to_n_time: 2.5S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: SEARCH-SIZE=3, param_2: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 11.1; req_2: CYCLE 4 / 11-11.7; req_3: SEQ 11-11.7 NO GAP; comment_1: STEP TIME = 2.5 SEC ! linenum: 11.100 targname: ^ config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 62.5S s_to_n: 70 s_to_n_time: 2.5S fluxnum_1: 1 fluxnum_2: 2 param_1: SEARCH-SIZE=5, priority: 1 req_1: ONBOARD ACQ FOR 11.2-11.7 comment_1: STEP-TIME=2.5 SEC ! linenum: 11.200 sequence_1: USE sequence_2: MAG targname: ^ s_to_n: 50 s_to_n_time: 5M ! linenum: 11.300 sequence_1: USE sequence_2: LYA1 targname: ^ s_to_n: 40 s_to_n_time: 35M ! linenum: 11.500 sequence_1: USE sequence_2: LYA2 targname: ^ num_exp: 1 s_to_n: 40 s_to_n_time: 35M ! linenum: 11.600 sequence_1: USE sequence_2: SILI targname: ^ num_exp: 2 s_to_n: 40 s_to_n_time: 45M ! linenum: 11.700 sequence_1: USE sequence_2: CARB targname: ^ s_to_n: 30 s_to_n_time: 40M ! linenum: 12.000 targname: HD150798 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 90S s_to_n: 70 s_to_n_time: 12.5S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: SEARCH-SIZE=3, param_2: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 12.1; req_2: CYCLE 4 / 12-12.5; req_3: SEQ 12-12.5 NO GAP; comment_1: STEP TIME = 10 SEC ! linenum: 12.100 targname: ^ config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 250S s_to_n: 70 s_to_n_time: 12.5S fluxnum_1: 1 fluxnum_2: 2 param_1: SEARCH-SIZE=5, priority: 1 req_1: ONBOARD ACQ FOR 12.2-12.5 comment_1: STEP-TIME=10 SEC ! linenum: 12.200 sequence_1: USE sequence_2: MAG targname: HD150798 s_to_n: 50 s_to_n_time: 5M ! linenum: 12.300 sequence_1: USE sequence_2: LYA11 targname: ^ s_to_n: 40 s_to_n_time: 70M ! linenum: 12.500 sequence_1: USE sequence_2: LYA2 targname: ^ num_exp: 2 s_to_n: 40 s_to_n_time: 70M ! ! end of exposure logsheet ! No scan data records found