! File: 4550C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:17:15:58 coverpage: title_1: CONSTRAINTS ON MASSIVE STAR EVOLUTION FROM CARBON AND OXYGEN title_2: ABUNDANCES IN LMC WC STARS. CYC3HIGH sci_cat: HOT STARS sci_subcat: MASSIVE STARS proposal_for: GO pi_fname: JOHN pi_mi: D pi_lname: HILLIER pi_inst: UNIVERSITAT MUENCHEN pi_country: GERMANY hours_pri: 13.28 num_pri: 4 fos: Y funds_amount: 141013 funds_length: 24 funds_date: SEP-93 off_fname: ROLF-PETER off_lname: KUDRITZKI off_title: DIRECTOR off_inst: INSTITUT F ASTRONOMY U ASTROPHYSIK DER UNIVERSITAET MUENCHEN off_addr_1: SCHEINERSTRASSE 1 off_addr_2: 8000 MUENCHEN 80 off_city: MUNICH off_country: GERMANY off_phone: +49-89-9220940 ! end of coverpage abstract: line_1: High signal-to-noise UV FOS spectra of a sample of WC-type Wolf-Rayet stars line_2: in the LMC will be obtained to determine C/He and O/C abundance ratios. line_3: These abundance ratios will provide urgently required constraints on the line_4: He-burning stage of the evolution of massive stars. The surface C/He and line_5: O/C abundance ratios in WC stars are influenced by mass loss, convection line_6: and overshooting, and the (uncertain) 12C(ALPHA,GAMMA)16O reaction rate. line_7: The spectra will be analyzed using sophisticated non-LTE radiative transfer line_8: codes which allow for spherical extension and stellar winds, and which line_9: incorporate the latest atomic data. Our quantitative analysis will also line_10: allow a determination of fundamental stellar parameters (eg Rstar, Teff), line_11: abundances of species such as Fe and Si, and accurate mass loss rates. line_12: These, and the C and O abundance determinations, will allow much tighter line_13: constraints to be placed on the evolution of massive stars. line_14: Starburst galaxies are currently an active area of research. Massive stars, line_15: including W-R stars, are seen to be playing a key role in the dynamics and line_16: evolution of these systems. It is imperative that we understand the line_17: evolution and properties of massive stars in the galaxy and LMC (where they line_18: are amenable to detailed spectroscopic studies) if we are to make reliable line_19: inferences concerning star formation rates, nucleosynthesis yields, line_20: and initial mass functions etc in starburst systems. ! ! end of abstract general_form_proposers: lname: HILLIER fname: JOHN title: PI mi: D inst: UNIVERSITAT MUENCHEN country: GERMANY esa: Y ! lname: HAMANN fname: WOLF-RAINER inst: UNIVERSITAT KIEL country: GERMANY esa: Y ! lname: WESSOLOWSKI fname: ULF inst: UNIVERSITAT KIEL country: GERMANY esa: Y ! lname: BUTLER fname: KEITH inst: UNIVERSITAT MUENCHEN country: GERMANY esa: Y ! lname: KUDRITZKI fname: ROLF mi: P inst: UNIVERSITAT MUENCHEN country: GERMANY esa: Y ! lname: LENNON fname: DANIEL mi: J inst: UNIVERSITAT MUENCHEN country: GERMANY esa: Y ! lname: VOELS fname: STEPHEN mi: A inst: UNIVERSITAT MUENCHEN country: GERMANY esa: Y ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: Justification not required for phase 2. ! question: 3 section: 1 line_1: Using FOS we will observe 4 WC4 stars in the LMC. Three sets of spectra, line_2: covering the wavelength ranges 1150-1606A (grating G130H), 1573-2330A line_3: (G190H), and 2222-3301A (G270H), will be obtained for each star. For line_4: HD32402, we will aim for a continuum S to N ratio in excess of 70:1, while line_5: for the other 3 stars we will aim for a S/N ratio of 40:1. The blue line_6: digicon will be used for all 3 regions. Although the red digicon could line_7: be used for region 2 (G190H), we feel that its rapid response variation line_8: near 1600A would adversely affect our ability to reliably combine this line_9: spectrum with that extending from 1150 to 1606A. The region from 1500-1700A line_10: is particularly important as it contains the CIV 1550 resonance doublet, line_11: and HeII 1640 whose formation is somewhat different from other HeII line_12: emission lines. We chose the blue detector for G270H because of detector line_13: stability (ie. one detector used continuously for all exposures), because line_14: of the slight increase in wavelength range allowing greater overlap with line_15: ground based observations, and because of overall system efficiency. line_17: As recommended by the TAC, observations of a further 3WC stars, and one WO line_18: star will be requested in a subsequent cycle. The selected stars have been line_19: the subject of an extensive optical observational study by Torres et al line_20: (1986), and show no evidence for binarity. They represent a complete sample line_21: of the known single WC/WO stars in the LMC. The v magnitudes (corrected for line_22: emission lines) range from 14th to 16.5th magnitude (Vacca and line_23: Torres-Dodgen 1990). ! question: 4 section: 1 line_1: The UV spectrum is essential for our analysis as it provides crucial line_2: information not available in the optical spectral region. The rich line_3: emission-line spectrum means that there are few (relatively) blend line_4: free lines ideally suited to abundance analyses. Many of these (eg CIV line_5: 1550) lie in the UV. Lines in the optical region are formed by line_6: recombination. However, the UV contains many lines formed by line_7: collisional processes. These lines provide additional diagnostics on line_8: the wind structure. Lines due to Fe (principally FeV and FeVI) are line_9: only observable in the UV. The targets are not suitable for IUE line_10: observations given our requirements of signal to noise, resolution, line_11: and problems with crowding in our target fields. line_13: The proposers have had extensive experience in modelling W-R and O line_14: stars. Some ground-based data are already available for the present line_15: stars, and further high signal-to-noise ground observations will be line_16: obtained for the project. A parallel study to determine O and C line_17: abundances in galactic WC stars is in progress by Hillier and line_18: Bohannan. In addition, Koesterke et al (1992) have established a line_19: coarse grid of WC models that can be used to provide initial estimates line_20: of the stellar parameters. They are using this grid to determine C/He line_21: abundances and stellar parameters for a sample of galactic WC stars. ! question: 4 section: 2 line_1: All four stars have been observed with the IUE SWP camera at low line_2: dispersion, and hence from the IUE continuum fluxes we have been able to line_3: estimate required exposure times. In addittion, all 4 stars have flux line_4: calibrated optical spectra, which, in conjunction with the IUE spectra, line_5: allows acquizition fluxes to be estimated. line_7: For 2 stars we require a signal-to-noise ratio of 40:1 per resolution line_8: element (diode) which was calculated on the basis of continuum fluxes at line_9: 1285A, 1690A, and 2200A). A signal-to-noise ratio of 40 to 1 will allow us line_10: to obtain high quality profiles, to detect blends and weak absorption line_11: features, and allow good continuum placement. The latter is essential for line_12: accurate profiles, and if we are to observe the broad dielectronic features line_13: predicted by our models. The need for high resolution and high S/N in line_14: studying W-R spectra has previously been stressed, for example, by Bappu line_15: (1973). line_17: For the brightest WC star (HD32402) we have opted for a S/N of 70:1 per line_18: resolution element. This enhanced S/N will serve 2 purposes. It will allow line_19: us to obtain useful data down to 1160A, where the detector/system response line_20: has fallen by more than a factor of 7 from 1285A. In this region CIII 1176, line_21: and additional FeVI lines are to be found. Secondly, the higher S/N will line_22: allow this spectrum to be used as a 'template' to assist in the continuum line_23: definition, reddening determinations, and modelling of the other WC stars. ! question: 5 section: 1 line_1: NO GAP justification: The UV spectra of early type stars is known to vary line_2: with time. In order to obtain completely consistent UV spectra line_3: over our spectral range, we require that the spectra for our 3 wavelength line_4: ranges be obtained as close together as possible. The order does not matter line_5: hence we have not used the SEQ requirement. ! question: 6 section: 1 line_1: No special calibrations etc required. ! question: 7 section: 1 line_1: Data Reduction: line_3: As of 1-Sep-1993 the PI will be commencing an associate professor position at line_4: the university of Pittsburgh. Some workstations are available, on a limited line_5: basis, for reduction however the PI intends to invest in a high powered line_6: workstation for both reduction and model development. We have requested ST line_7: funds, and intend to purchase the workstation on a 50% cost sharing basis with line_8: the University of Pittsburgh. In order to partially verify the reduction line_9: procedures, data reduction will be performed independently in both Munich and line_10: in Pittsburgh. line_12: The institute in Munich has a cluster of 12 DEC VAXStations (3 x 3200, 2 x line_13: 3100, 7 x 2000, 21 VUPS total, several with 8-bit color display) plus a cluster line_14: of DEC Decstations (2 x 5000, 1 x VT1300,all with 8-bit color display) on which line_15: all major astronomical software environments (IDL, IRAF, IRAF/STSDAS and MIDAS) line_16: are installed. Data calibration and reduction will be performed using the line_17: latest software and calibration databases available locally or at the nearby line_18: ST-ECF in Garching. Note that personnel have already gained experience with FOS line_19: data reduction as a result of a Cycle 1 allocation of time and are familiar line_20: with the procedures and software. ! question: 7 section: 2 line_1: The analysis will be carried out by performing spectral synthesis line_2: using state of the art non-LTE wind codes. Two independent codes are line_3: available, allowing important consistency checks. These codes have line_4: been developed by the PI (eg Hillier 1989, 1990), and by Hamann, line_5: Schmutz and collaborators in Kiel (eg Hamman and Wessolowski 1990). line_6: All codes are continually undergoing improvements and revisions as line_7: assumptions are relaxed, and as the latest atomic data are line_8: incorporated. They have been used with great success in investigating line_9: the structure of W-R stars (Hillier 1987,1988,1989, Schmutz et al line_10: 1989). In addition we will have access to the extensive set of non-LTE line_11: codes developed by Kudritzki and collaborators (eg Gabler et al 1989) line_12: which have been used with great success modelling O stars. line_14: The code developed by the PI allows for the full non-LTE treatment of line_15: H, HeI, CII-CIV, NIII-NV, and OIII-OVI. Recently Becker and Butler line_16: (1992) have developed an extensive FeV model atom. The model atom will line_17: soon be incorporated into the code, and will be a first step in line_18: allowing the full treatment of non-LTE line blanketing. ! question: 8 section: 1 line_1: Revised target positions, obtained with GASP, are now supplied with the line_2: Phase 2 proposal. ! question: 9 section: 1 line_1: GO No. 2233/4110 THE PHYSICS OF MASSIVE O-STARS IN DIFFERENT PARENT line_2: GALAXIES line_4: GTO No. 1215 ULTRAVIOLET SPECTRAL ATLAS OF O-STARS IN THE MILKY WAY line_5: AND MAGELLANIC CLOUDS line_7: The present proposal is related to these in so far as they are all line_8: concerned with the general topic of the physics and nature of hot line_9: massive stars in other galaxies. ! question: 9 section: 2 line_1: Stellar parameters and abundances (including iron) have so far been line_2: obtained for 3 very massive early O-type stars in the LMC. In line_3: addition, estimates have been made of the mass-loss rates, terminal line_4: velocities and hence the stellar masses and distances. The 15 other line_5: targets from this project are due to be observed before the end of line_6: this year. ! question: 9 section: 3 line_1: First Results from the GHRS: Spectroscopic determination of stellar line_2: parameters of an O3f star, Melnick 42, in the Large Magellanic Cloud, line_3: Heap, S.R., Altner, B., Ebbets, D., Hubeny, I., Hutchings, J.S., line_4: Kudritzki, R.P. Voels, S.A., Haser, S., Pauldrach, A., Puls, J., line_5: Butler, K., 1991., Ap. J. Let., 377, L29. line_7: Kudritzki, R.P., Becker, S.R., Butler, K., Gabler, R., Haser, S., Husfeld, D., line_8: Lennon, D.J., Pauldrach, A., Puls, J., Voels, S. 1992b, 'Hot Stars and line_9: the Hubble Space Telescope', in 'Science with the Hubble Space Telescope', line_10: ESO, in press. ! question: 10 section: 1 line_1: University of Pittsburgh: line_3: As noted in Section 6, the university has agreed to provide 50% funding of a line_4: high powered work station for reduction (some work stations are already line_5: available for this) and extensive model development. In addition, the PI will line_6: have access to the Pittsburgh Supercomputer center for more extensive model line_7: calculations. line_9: Munich University: line_11: Data reduction and analysis facilities and personal are described under Section line_12: 6. There are no problems with the funding of the necessary computer line_13: calculations required for this project, either at Kiel, or Munich. line_15: Funds for travel, preparation of observations, reduction, etc will also be line_16: available. ! !end of general form text general_form_address: lname: HILLIER fname: JOHN mi: D category: PI inst: Universitat Muenchen addr_1: SCHEINERSTRASSE 1 addr_2: 8000 MUENCHEN 80 city: MUENCHEN/MUNICH country: GERMANY phone: +49-89-9220940 to_date: 31-AUG-92 ! lname: HILLIER fname: JOHN mi: D category: PI inst: UNIVERSITY OF PITTSBURGH addr_1: DEPARTMENT OF PHYSICS AND ASTRONOMY addr_2: 3941 O'HARA STRREET addr_3: 100 ALLEN HALL city: PITTSBURGH, PA 15260 country: USA phone: 412-624-9000 from_date: 01-SEP-93 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD32402 name_2: WS6 name_3: BR10 descr_1: B,102; descr_2: HOST=LMC descr_3: TYPE=WC4 pos_1: PLATE-ID=05ZW, pos_2: RA = 04H 57M 24.191S +/- 0.50", pos_3: DEC = -68D 23' 57.23" +/- 0.50" equinox: 2000 rv_or_z: V= +280 acqpr_1: COMP comment_1: V=14.01 +/- 0.1 comment_2: E(B-V)=0.06 fluxnum_1: 001 fluxval_1: V=13.30 +/- 0.1, TYPE=WC4 fluxnum_2: 002 fluxval_2: B-V=-0.19 +/- 0.05 fluxnum_3: 003 fluxval_3: E(B-V)=0.07 +/- 0.03 fluxnum_4: 004 fluxval_4: F-CONT(5560)=9.0 +/- 0.5 E-15 fluxnum_5: 005 fluxval_5: F-CONT(2225)=1.7 +/- 0.2 E-13 fluxnum_6: 006 fluxval_6: F-CONT(1690)=4.5 +/- 0.1 E-13 fluxnum_7: 007 fluxval_7: F-CONT(1285)=1.0 +/- 0.1 E-12 ! targnum: 11 name_1: HD37026 name_2: WS31 name_3: BR43 descr_1: B,102; descr_2: HOST=LMC descr_3: TYPE=WC4 pos_1: PLATE-ID=05ZW, pos_2: RA = 05H 30M 12.216S +/- 0.50", pos_3: DEC = -67D 26' 08.49" +/- 0.50" equinox: 2000 rv_or_z: V= +280 comment_1: V=14.46 +/- 0.1 comment_2: E(B-V)=0.05 fluxnum_1: 001 fluxval_1: V=13.60 +/- 0.1, TYPE=WC4 fluxnum_2: 002 fluxval_2: B-V=-0.31 +/- 0.05 fluxnum_3: 003 fluxval_3: E(B-V)=0.06 +/- 0.02 fluxnum_4: 004 fluxval_4: F-CONT(5560)=7.0 +/- 0.5 E-15 fluxnum_5: 005 fluxval_5: F-CONT(2225)=6.9 +/- 0.5 E-14 fluxnum_6: 006 fluxval_6: F-CONT(1690)=1.8 +/- 0.2 E-13 fluxnum_7: 007 fluxval_7: F-CONT(1285)=4.6 +/- 0.5 E-13 ! targnum: 21 name_1: HD37680 name_2: WS35 name_3: BR50 descr_1: B,102; descr_2: HOST=LMC descr_3: TYPE=WC4 pos_1: PLATE-ID=05ZW, pos_2: RA = 05H 34M 19.387S +/- 0.50", pos_3: DEC = -69D 45' 10.08" +/- 0.50" equinox: 2000 rv_or_z: V= +280 comment_1: V=14.27 comment_2: E(B-V)=0.01 fluxnum_1: 001 fluxval_1: V=13.35 +/- 0.1, TYPE=WC4 fluxnum_2: 002 fluxval_2: B-V=-0.20 +/- 0.05 fluxnum_3: 003 fluxval_3: E(B-V)=0.01 +/- 0.03 fluxnum_4: 004 fluxval_4: F-CONT(5560)=8.0 +/- 0.5 E-15 fluxnum_5: 005 fluxval_5: F-CONT(2225)=9.2 +/- 0.5 E-14 fluxnum_6: 006 fluxval_6: F-CONT(1690)=1.7 +/- 0.2 E-13 fluxnum_7: 007 fluxval_7: F-CONT(1285)=4.5 +/- 0.1 E-13 ! targnum: 31 name_1: HD32257 name_2: WS4 name_3: BR8 descr_1: B,102; descr_2: HOST=LMC descr_3: TYPE=WC4 pos_1: PLATE-ID=05ZW, pos_2: RA = 04H 56M 02.952S +/- 0.50", pos_3: DEC = -69D 27' 21.59" +/- 0.50" equinox: 2000 rv_or_z: V= +280 comment_1: V=15.12 +/- 0.1 comment_2: E(B-V)=0.06 fluxnum_1: 001 fluxval_1: V=14.27 +/- 0.1, TYPE=WC4 fluxnum_2: 002 fluxval_2: B-V=-0.20 +/- 0.05 fluxnum_3: 003 fluxval_3: E(B-V)=0.07 +/- 0.03 fluxnum_4: 004 fluxval_4: F-CONT(5560)=3.5 +/- 0.2 E-15 fluxnum_5: 005 fluxval_5: F-CONT(2225)=3.2 +/- 0.2 E-14 fluxnum_6: 006 fluxval_6: F-CONT(1690)=7.8 +/- 0.2 E-14 fluxnum_7: 007 fluxval_7: F-CONT(1285)=2.2 +/- 0.1 E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 11.000 targname: HD32402 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.66S fluxnum_1: 4 priority: 1 param_1: FAINT=940.0, param_2: BRIGHT=33000.0 req_1: CYCLE 3/11.00-15.00; req_2: GROUP 11.00-15.00 NO GAP; req_3: ONBOARD ACQ FOR 12.00; ! linenum: 12.000 targname: HD32402 config: FOS/BL opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 1.2S fluxnum_1: 4 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 13.00; req_2: SPATIAL SCAN; ! linenum: 13.000 targname: HD32402 config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G130H num_exp: 1 time_per_exp: 2350S s_to_n: 70 fluxnum_1: 5 priority: 1 ! linenum: 14.000 targname: HD32402 config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G190H num_exp: 1 time_per_exp: 980S s_to_n: 70 fluxnum_1: 6 priority: 1 ! linenum: 15.000 targname: HD32402 config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G270H num_exp: 1 time_per_exp: 365S s_to_n: 70 fluxnum_1: 7 priority: 1 ! linenum: 21.000 targname: HD37026 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.66S fluxnum_1: 4 priority: 2 param_1: FAINT=660.0, param_2: BRIGHT=33000.0 req_1: CYCLE 3/21.00-25.00; req_2: GROUP 21.00-25.00 NO GAP; req_3: ONBOARD ACQ FOR 22.00; ! linenum: 22.000 targname: HD37026 config: FOS/BL opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 0.90S fluxnum_1: 4 priority: 2 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 23.00; req_2: SPATIAL SCAN; ! linenum: 23.000 targname: HD37026 config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G130H num_exp: 1 time_per_exp: 1740S s_to_n: 40 fluxnum_1: 5 priority: 2 ! linenum: 24.000 targname: HD37026 config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G190H num_exp: 1 time_per_exp: 825S s_to_n: 40 fluxnum_1: 6 priority: 2 ! linenum: 25.000 targname: HD37026 config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G270H num_exp: 1 time_per_exp: 300S s_to_n: 40 fluxnum_1: 7 priority: 2 ! linenum: 31.000 targname: HD37680 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.66S fluxnum_1: 4 priority: 2 param_1: FAINT=940.0, param_2: BRIGHT=33000.0 req_1: CYCLE 3/31.00-35.00; req_2: GROUP 31.00-35.00 NO GAP; req_3: ONBOARD ACQ FOR 32.00; ! linenum: 32.000 targname: HD37680 config: FOS/BL opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 0.93S fluxnum_1: 4 priority: 2 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 33.00; req_2: SPATIAL SCAN; ! linenum: 33.000 targname: HD37680 config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G130H num_exp: 1 time_per_exp: 1800S s_to_n: 40 fluxnum_1: 5 priority: 2 ! linenum: 34.000 targname: HD37680 config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G190H num_exp: 1 time_per_exp: 840S s_to_n: 40 fluxnum_1: 6 priority: 2 ! linenum: 35.000 targname: HD37680 config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G270H num_exp: 1 time_per_exp: 220S s_to_n: 40 fluxnum_1: 7 priority: 2 ! linenum: 41.000 targname: HD32257 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.11S fluxnum_1: 4 priority: 2 param_1: FAINT=660.0, param_2: BRIGHT=33000.0 req_1: CYCLE 3/41.00-45.00; req_2: GROUP 41.00-45.00 NO GAP; req_3: ONBOARD ACQ FOR 42.00; ! linenum: 42.000 targname: HD32257 config: FOS/BL opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 2.23S fluxnum_1: 4 priority: 2 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 43.00; req_2: SPATIAL SCAN; ! linenum: 43.000 targname: HD32257 config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G130H num_exp: 1 time_per_exp: 3100S s_to_n: 37 fluxnum_1: 5 priority: 2 ! linenum: 44.000 targname: HD32257 config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G190H num_exp: 1 time_per_exp: 1920S s_to_n: 40 fluxnum_1: 6 priority: 2 ! linenum: 45.000 targname: HD32257 config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G270H num_exp: 1 time_per_exp: 660S s_to_n: 40 fluxnum_1: 7 priority: 2 ! ! end of exposure logsheet scan_data: line_list: 12.00 fgs_scan: cont_dwell: D dwell_pnts: 7 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 0.4000 sides_angle: 0.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 0.2 wid_offset: ! line_list: 22.00 fgs_scan: cont_dwell: D dwell_pnts: 7 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 0.4000 sides_angle: 0.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 0.2 wid_offset: ! line_list: 32.00 fgs_scan: cont_dwell: D dwell_pnts: 7 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 0.4000 sides_angle: 0.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 0.2 wid_offset: ! line_list: 42.00 fgs_scan: cont_dwell: D dwell_pnts: 7 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 0.4000 sides_angle: 0.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 0.2 wid_offset: ! ! end of scan data