! File: 2338C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:05:06:27 coverpage: title_1: SPECTROSCOPY OF THE SPECKLE-RESOLVED ETA CARINAE POINT SOURCES sci_cat: STELLAR ASTROPHYSICS sci_subcat: MASSIVE STARS proposal_for: GO pi_title: DR. pi_fname: KRIS pi_lname: DAVIDSON pi_inst: MINNESOTA, UNIVERSITY OF pi_country: USA pi_phone: 612-624-5711 keywords_1: EARLY TYPE STARS, ATMOSPHERES, UV SPECTROSCOPY, keywords_2: STELLAR EVOLUTION, NUCLEOSYNTHESIS, ABUNDANCES, LBVS, LUMINOUS STARS, MASSIVE ST hours_pri: 6.00 num_pri: 1 fos: X funds_amount: 53000 funds_length: 12 funds_date: AUG-91 off_fname: MERLIN off_lname: GARLID off_title: ASSIST. DIRECTOR off_inst: UNIVERSITY OF MINNESOTA off_addr_1: ORTTA, 1919 UNIV. AVE off_addr_2: 5TH FLOOR off_addr_3: (OFC OF RES & TECH TRANSFER ADMIN) off_city: ST. PAUL off_state: MN off_zip: 55104 off_country: USA ! end of coverpage abstract: line_1: Eta carinae is thought to be the most extreme known Luminous Blue Variable line_2: (LBV), marking the unstable upper boundary of the HR Diagram. It is crucial line_3: for theories of the LBV outburst phenomenon, only recently beginning to be line_4: developed. Recently the "central object" in Eta Carinae has been found by line_5: speckle techniques to be multiple. Combined with the presence of circumstellar line_6: emission and scattering, this multiplicity means that high spatial resolution line_7: is needed in order to obtain spectral data specifically on the primary line_8: component, the very massive LBV star. The fainter components are also important line_9: -- if they are stars, then this is a unique chance to study a truly coeval line_10: system of very massive stars of known age (known because the LBV is present), line_11: and if they are nebular objects, then we need spectra in order to understand line_12: why they are so unexpectedly bright. For these reasons we propose to us the line_13: FOS to obtain spectra of the primary star and of its companion objects. The line_14: stellar spectra will be used for a quantitative analysis by NLTE methods, line_15: aiming for estimates of Teff, g, chemical composition, mass, mass-loss rate, line_16: wind velocity field, and luminosity. ! ! end of abstract general_form_proposers: lname: DAVIDSON fname: KRIS title: P.I. inst: MINNESOTA, UNIVERSITY OF country: USA ! lname: WEIGELT fname: G. inst: MAX-PLANCK-INSTITUT F. RADIOASTRONOMIE country: FRG esa: X ! lname: ROSA fname: MICHAEL inst: EUROPEAN SOUTHERN OBSERVATORY country: FRG esa: X ! lname: WOLF fname: B. inst: HEIDELBERG STATE OBSERVATORY country: FRG esa: X ! lname: HUMPHREYS fname: R. mi: M. inst: MINNESOTA, UNIVERSITY OF country: USA ! lname: KUDRITZKI fname: ROLF-PETER inst: MUNICH UNIVERSITY country: FRG esa: X ! lname: WALBORN fname: NOLAN mi: R. inst: STSCI country: USA ! lname: SIMON fname: KLAUS mi: P. inst: MUNICH UNIVERSITY country: FRG esa: X ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: (The following text has been revised, April 1991, to describe the post- line_2: reassessment modified observing plan. In the original version planned line_3: in 1988-89, each of the 4 known components in Eta Car was to be observed line_4: individually with the tiny 0.1" FOS aperture. However, the components line_5: cannot be fully separated in this way with the ST's imperfect p.s.f.; line_6: hence the following revised plan, which seeks mainly to distinguish line_7: between the primary component and its fainter companions.) line_8: The 4 speckle-resolved components of Eta Carinae are all within a 0.3" line_9: region. Their relative (offset) positions are known to a precision line_10: of about 0.03" from several independent and mutually consistent speckle line_11: observations during 1983--1989. The primary component A is probably line_12: the LBV star, while its companions BCD may be either stars or compact line_13: blobs of ejecta. Because all 3 objects BCD are to the northwest of A, line_14: we can separate the spectrum of object A from the combined spectrum line_15: of B+C+D with the 0.3" FOS aperture. Here is the procedure: line_16: (1) The first step is a fairly routine peak-up on the combined object line_17: A+B+C+D. This defines a reference location called PKUP, a sort of line_18: centroid of ABCD (peak of convolution with the effective p.s.f.). line_19: (2) Next, offset about 0.2" southeast from PKUP, to a location called line_20: SE. Simulations with a realistic p.s.f. have shown that this offset line_21: ----( question 3 continued in next section )---- ! question: 3 section: 2 line_1: from the peak-up location gives nearly the maximum ratio of line_2: (counts due to A)/(counts due to B+C+D), line_3: for a fairly wide range of brightness ratios A/(B+C+D). (The ratio of line_4: counts A/(B+C+D) is expected to be of the order of 5 at position SE.) line_5: Several FOS gratings are used to obtain a spectrum at position SE. line_6: (3) Similarly, an offset location NW, about 0.2" northwest of PKUP, line_7: gives the maximum ratio of counts (B+C+D)/A, probably about 3. line_8: (4) A few short exposures are also taken at a nearby offset location line_9: called NE, and at PKUP too, to roughly indicate the contributions of line_10: local diffuse emission-line gas to the spectra taken at SE and NW. line_11: ...When all these steps have been done, differences between the spectra line_12: obtained in steps 2 and 3 should reveal the qualitative difference line_13: between object A and the fainter components B+C+D. Detailed modeling line_14: of all the data with the known ST/FOS characteristics should enable us line_15: to quantitatively estimate the separate spectra A vs. B+C+D, well line_16: enough for good atmospheric analysis of star A and rougher analysis of line_17: objects B, C, and D. Obviously these data are also needed for planning line_18: any future detailed observations of A, B, C, D individually. line_19: ...We will use the blue digicon with 5 FOS gratings to cover wavelengths line_20: 1200--5300 A. S/N ratios of the order of 50 per sampling element line_21: (1/4 diode) are needed for the detailed analysis. ! question: 4 section: 1 line_1: (1) High spatial resolution is needed to resolve the multiple system line_2: of Eta Carinae. Ground-based speckle observations cannot provide good line_3: spectroscopic data on this object. Moreover, the small FOS apertures line_4: are better than larger ground-based apertures for minimizing spectral line_5: contamination by emission lines from surrounding circumstellar gas. line_6: (2) The UV part of the spectrum is indispensable for analysis of the line_7: photosphere and stellar wind of each star. If any of the components line_8: turn out to be nebular objects, then UV emission lines are critical -- line_9: especially since they would probably turn out to be nitrogen-rich. line_10: Existing UV data obtained with the IUE include everything within a 3" line_11: aperture, heavily contaminated by circumstellar diffuse material. line_12: (3) For the proposed NLTE analyses, a sufficiently high spectral line_13: resolution and S/N ratio are necessary. line_14: ...These requirements are met only by the ST/FOS. Spectroscopic line_15: observations have been and are being pursued essentially to the line_16: limits attainable from the ground or with IUE. ! question: 5 section: 1 line_1: UV example, grating G190H with the blue detector: Primary object "A" line_2: is expected to have a flux somewhat less than 1.E-12 erg cm-2 s-1 A-1 line_3: in the 1600--2000 A wavelength region. Using estimates of 0.012 for line_4: for the basic instrument efficiency and 0.1 for the 0.3" aperture's line_5: throughput, and another factor of 0.6 to correct for the necessary line_6: 0.15" off-centering, we estimate roughly 4 counts/s per diode in this line_7: wavlength range. Thus a half-hour exposure gives roughly 7000 counts line_8: per diode and a S/N of the order of 40 for a 1/4-diode resolution line_9: element, except that contamination by the companion objects BCD is line_10: likely to reduce the effective S/N. The count rates are considerably line_11: higher for the longer-wavelength gratings, and lower for G130H. line_12: (S/N's listed in our observing plan may be optimistic.) Numbers for line_13: the combined fainter objects B+C+D are comparable to those for object A line_14: alone. In most cases we have aimed for S/Ns of 40 or more, to allow line_15: disentangling the different linear combinations of A and B+C+D as well line_16: as adequate spectral analysis later. line_17: ... We are very conscious of the need to carefully avoid excessive line_18: count rates with the FOS. Our flux estimates are based on photometry line_19: and spectrophotometry cited, e.g., in Ap.J.305, 867, supplemented by line_20: measurements of CCD images to determine how much of the light comes line_21: from the central core. (The possible count-rate danger is one reason line_22: why we are not using the red digicon; the other reason of course is line_23: the time needed to switch between BL and RD.) ! question: 6 section: 1 line_1: No special scheduling requests. ! question: 7 section: 1 line_1: (This is the original answer to this question, 1988:) line_2: The data will be reduced both at the Munich Observatory and also, line_3: in parallel, at Minnesota. Two software specialists at the Munich line_4: institute are funded by the German research ministry as part of a major line_5: soft- and hardware network dedicated to projects in space astronomy. line_6: This will be used by Kudritzki's group to reduce the data. At Minnesota line_7: the IRAF/SDAS software package will be used with a SUN computer system. line_8: Initial classification estimates will be made by Walborn and Humphreys. line_9: More detailed analysis by modeling, at Munich, will follow. Effective line_10: temperature, gravity, and helium abundance can be determined from line_11: photospheric spectra by fitting observed profiles of H, HeI, HeII line_12: lines with very detailed NLTE multi-level calculations. The UV part line_13: of the spectrum is more important than the visual for abundance line_14: analyses of O-type stars. The P-Cygni wind profiles will be fitted line_15: by detailed radiative transfer calculations, supplemented by hydrodynamic line_16: factors, to derive wind velocities and mass-loss rates. Analyses will line_17: be done differentially, relative to galactic O-stars, in order to line_18: minimize systematic uncertainties caused by deficiencies in the codes line_19: or the atomic parameters. If any of the objects are found to be nebular, line_20: or have overlying nebular lines, Davidson and Rosa will attempt line_21: interpretation of these. Details cannot be stated in advance because line_22: we do not know whether we'll find shock- or photoionization heating, etc. ! question: 8 section: 1 line_1: Basic relative positions of the 4 components are already known from line_2: several independent and mutually consistent sets of ground-based line_3: speckle data. Additional data on separations of the 4 components line_4: may be provided by some short-exposure PC images planned as part of line_5: a GTO program by D. Ebbets, in which Davidson and Walborn are line_6: assisting. Davidson has done a considerable amount of ground-based line_7: astrometric work on the position of the core of Eta Car and also to line_8: provide a "special catalog" for ST acquisition in this crowded region. ! question: 9 section: 1 line_1: See question 8 above. Originally it was hoped that short-exposure line_2: FOC images made in program 1255 GTO/FOC-86G would also be available, line_3: (Weigelt is involved there), but Eta Car was removed from the list line_4: of highest-priority targets for that program. ! question: 10 section: 1 line_1: (This is the original, 1988 answer to this question:) line_2: Munich: Drs. K. Butler & S. Becker will assist in NLTE line_3: theory and atomic physics. A. Pauldrach and J. Puls will line_4: contribute to stellar wind hydrodynamics and diagnostics. line_5: NLTE model atmosphere, line formation, and stellar wind line_6: codes are implemented on a CDC Cyber 185 and a Cray 1 line_7: directly linked to the Institute. Funding of the calculations line_8: that are done in Munich will cause no problems. line_9: Minnesota: The Graduate School of the University contributed line_10: $12000 toward the cost of the SUN purchased by Davidson, line_11: Humphreys, and others. Additional equipment and software line_12: is continually being added in the usual modern fashion. ! !end of general form text general_form_address: lname: DAVIDSON fname: KRIS title: DR. category: PI inst: UNIVERSITY OF MINNESOTA addr_1: 116 CHURCH ST. S.E. city: MINNEAPOLIS state: MN zip: 55455 country: USA ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD93308-PKUP-OFFSET name_2: ETA-CAR-PKUP-OFFSET descr_1: STAR; LBV; MULTIPLE STAR pos_1: RA = 10H 45M 03.62S +/- 0.04S , pos_2: DEC = -59D 41' 03.90" +/- 0.30", pos_3: PLATE-ID = ZZZQ equinox: 2000 pos_epoch_bj: J pos_epoch_yr: 1989.00 comment_1: PEAKUP REF POSITION FOR TARGETS comment_2: 2-4. ETA CAR HAS FOUR KNOWN comment_3: COMPONENTS ABCD, SEPARATIONS comment_4: 0.1 TO 0.3 ARCSEC. TARGET 1 IS comment_5: A PEAKUP CENTROID LOCATION comment_6: WITHIN ABCD. FLUXES QUOTED FOR comment_7: TARGET 1 REPRESENT ROUGH TOTAL comment_8: OF ALL 4 COMPONENTS. PLATE-ID comment_9: REFERS TO A SPECIAL CATALOG. fluxnum_1: 1 fluxval_1: V = 7.6 +/- 0.3 fluxnum_2: 2 fluxval_2: B-V = 0.7 +/- 0.2 fluxnum_3: 3 fluxval_3: F-CONT(4800) = 3.0 +/-.6 E-12 fluxnum_4: 4 fluxval_4: F-CONT(2000) = 2.5 +/-.6 E-12 fluxnum_5: 5 fluxval_5: F-CONT(1400) = 2.0 +/-.6 E-12 fluxnum_6: 6 fluxval_6: E(B-V) = 0.9 +/- 0.2 ! targnum: 2 name_1: HD93308-SE name_2: ETA-CAR-SE descr_1: STAR; MASSIVE LBV; HIGH LUMINOSITY STAR pos_1: R = 0.179", pos_2: PA = 142D, pos_3: FROM 1 equinox: 2000 pos_epoch_bj: J pos_epoch_yr: 1989.00 comment_1: TARGET 2 REPRESENTS PRIMARY comment_2: COMPONENT A. MORE PRECISELY, comment_3: THIS IS OFFSET WHERE MAX RESPONSE comment_4: RATIO A/(B+C+D) IS EXPECTED comment_5: USING 0.3" FOS APER. QUOTED FLUX comment_6: IS ROUGHLY BRTNESS OF A, DIVIDED comment_7: BY 1.5 TO CORRECT FOR NECESSARY comment_8: 0.15" OFF-CENTER POINTING. FE II comment_9: EMIS ENHANCES FLUX AROUND 2600 A. fluxnum_1: 1 fluxval_1: V = 8.8 +/- 0.4 fluxnum_2: 2 fluxval_2: B-V = 0.8 +/- 0.2 fluxnum_3: 3 fluxval_3: F-CONT(4800) = 1.0 +/-.5 E-12 fluxnum_4: 4 fluxval_4: F-CONT(4200) = 0.9 +/-.5 E-12 fluxnum_5: 5 fluxval_5: F(2600) = 1.3 +/-2.0 E-12 fluxnum_6: 6 fluxval_6: F-CONT(2000) = 0.7 +/-.5 E-12 fluxnum_7: 7 fluxval_7: F-CONT(1400) = 0.6 +/-.5 E-12 ! targnum: 3 name_1: HD93308-NW name_2: ETA-CAR-NW descr_1: STAR; HIGH LUMINOSITY MULTIPLE OBJECT pos_1: R = 0.240" , pos_2: PA = 322D , pos_3: FROM 1 equinox: 2000 pos_epoch_bj: J pos_epoch_yr: 1989.00 comment_1: TARGET 3 REPRESENTS COMPONENTS comment_2: BCD. MORE PRECISELY, THIS IS comment_3: OFFSET WHERE MAXIMAL RESPONSE comment_4: RATIO (B+C+D)/A IS EXPECTED comment_5: USING THE 0.3" FOS APERTURE. comment_6: QUOTED FLUX IS VERY ROUGH AND comment_7: REPRESENTS SUM B+C+D, DIVIDED BY comment_8: 2 TO CORRECT FOR NECESSARY OFF- comment_9: CENTER POINTING. OBJECTS BCD comment_10: MAY BE COMPACT BLOBS, NOT STARS. fluxnum_1: 1 fluxval_1: V = 9.7 +/- 0.6 fluxnum_2: 2 fluxval_2: B-V = 0.6 +/- 0.2 fluxnum_3: 3 fluxval_3: F-CONT(4800) = 5.0 +/- 1.5 E-13 fluxnum_4: 4 fluxval_4: F-CONT(4200) = 5.0 +/- 1.5 E-13 fluxnum_5: 5 fluxval_5: F(2600) = 7.0 +/- 2.0 E-13 fluxnum_6: 6 fluxval_6: F-CONT(2000) = 5.0 +/- 1.5 E-13 fluxnum_7: 7 fluxval_7: F-CONT(1400) = 5.0 +/- 1.5 E-13 ! targnum: 4 name_1: HD93308-NE name_2: ETA-CAR-NE descr_1: STAR; HII REGION; GASEOUS BACKGROUND pos_1: R = 0.36" , pos_2: PA = 45D , pos_3: FROM 1 equinox: 2000 pos_epoch_bj: J pos_epoch_yr: 1989.00 comment_1: TARGET 4 REPRESENTS LOCAL comment_2: DIFFUSE BACKGROUND, FOR MODELING comment_3: SPECTRA TAKEN ON MAIN TARGETS 2 comment_4: AND 3. TARGETS 2-3-4 FORM APPROX comment_5: EQUILATERAL TRIANGLE, MARGINALLY comment_6: RESOLVED WITH 0.3" FOS APERTURE. comment_7: QUOTED FLUX FOR TARGET 4 IS comment_8: MERELY A PLAUSIBLE GUESS. fluxnum_1: 1 fluxval_1: V = 10.7 +/- 1.0 fluxnum_2: 2 fluxval_2: B-V = 0.6 +/- 0.3 fluxnum_3: 3 fluxval_3: F(4800) = 2.0 +/- 1.0 E-13 fluxnum_4: 4 fluxval_4: F(4200) = 2.0 +/- 1.0 E-13 fluxnum_5: 5 fluxval_5: F(2600) = 2.0 +/- 1.0 E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 30.000 targname: HD93308-PKUP-OFFSET config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G570H wavelength: 4600-4820 num_exp: 1 time_per_exp: 0.7S s_to_n: 60 fluxnum_1: 2 priority: 1 param_1: SEARCH-SIZE=6, param_2: SCAN-STEP=0.7 req_1: ONBOARD ACQ FOR 40;CYCLE 1; comment_1: ONLY 4600-4820 RANGE ENABLED comment_2: TO EXCLUDE H-BETA. comment_3: S-TO-N RATIOS ASSUME SMALLEST comment_4: PLAUSIBLE FLUX, BECAUSE THE TRUE comment_5: BRIGHTNESS OF THE CORE OF comment_6: ETA CAR IS VERY UNCERTAIN. ! linenum: 40.000 targname: HD93308-PKUP-OFFSET config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: G570H wavelength: 4600-4820 num_exp: 1 time_per_exp: 1S s_to_n: 60 fluxnum_1: 2 priority: 1 param_1: SEARCH-SIZE=5, param_2: SCAN-STEP=0.24 req_1: ONBOARD ACQ FOR 50;CYCLE 1; comment_1: ONLY 4600-4820 RANGE ENABLED comment_2: TO EXCLUDE H-BETA. ! linenum: 50.000 targname: HD93308-PKUP-OFFSET config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: G570H wavelength: 4600-4820 num_exp: 1 time_per_exp: 2S s_to_n: 60 fluxnum_1: 2 priority: 1 param_1: SEARCH-SIZE=6, param_2: SCAN-STEP=0.075 req_1: ONBOARD ACQ FOR 60;CYCLE 1; comment_1: ONLY 4600-4820 RANGE ENABLED comment_2: TO EXCLUDE H-BETA. comment_3: 6 X 6 MAP FROM THIS STAGE OF comment_4: PEAKUP MAY BE USEFUL FOR comment_5: MODELING THE SPECTRAL DATA. ! linenum: 60.000 targname: HD93308-PKUP-OFFSET config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: G570H wavelength: 4600-4820 num_exp: 1 time_per_exp: 6S s_to_n: 100 fluxnum_1: 2 priority: 1 param_1: SEARCH-SIZE=4, param_2: SCAN-STEP=0.033 req_1: ONBOARD ACQ FOR 210-530;CYCLE 1; comment_1: ONLY 4600-4820 RANGE ENABLED TO comment_2: EXCLUDE H-BETA. ! linenum: 110.000 sequence_1: DEFINE sequence_2: MAINOBS targname: # config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G570H wavelength: 4610-5150 num_exp: 1 time_per_exp: 500 S s_to_n: 60 fluxnum_1: 3 priority: # comment_1: S/N RATIOS QUOTED FOR ALL SCIENCE comment_2: EXPOSURES REFER TO A 1/4-DIODE comment_3: RESOLUTION ELEMENT. THESE S/N comment_4: RATIOS ARE PROBABLY OPTIMISTIC comment_5: BECAUSE THERE IS CONTAMINATION BY comment_6: THE COMPANION OBJECTS. ! linenum: 120.000 sequence_1: DEFINE sequence_2: MAINOBS targname: # config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G400H wavelength: 3250-4800 num_exp: 1 time_per_exp: 700 S s_to_n: 70 fluxnum_1: 4 priority: # ! linenum: 130.000 sequence_1: DEFINE sequence_2: MAINOBS targname: # config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G270H wavelength: 2240-3290 num_exp: 1 time_per_exp: 500 S s_to_n: 70 fluxnum_1: 5 priority: # ! linenum: 140.000 sequence_1: DEFINE sequence_2: MAINOBS targname: # config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G190H wavelength: 1590-2300 num_exp: 1 time_per_exp: 1800 S s_to_n: 50 fluxnum_1: 6 priority: # ! linenum: 150.000 sequence_1: DEFINE sequence_2: MAINOBS targname: # config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G130H wavelength: 1220-1600 num_exp: 1 time_per_exp: 2400 S s_to_n: 25 fluxnum_1: 7 priority: # ! linenum: 210.000 sequence_1: USE sequence_2: MAINOBS targname: HD93308-SE priority: 2 req_1: CYCLE 1; ! linenum: 310.000 sequence_1: USE sequence_2: MAINOBS targname: HD93308-NW priority: 3 req_1: CYCLE 1; ! linenum: 410.000 targname: HD93308-NE config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G570H wavelength: 4610-5150 num_exp: 1 time_per_exp: 500 S s_to_n: 40 fluxnum_1: 3 priority: 4 req_1: CYCLE 1; ! linenum: 420.000 targname: HD93308-NE config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G400H wavelength: 3250-4810 num_exp: 1 time_per_exp: 500 S s_to_n: 40 fluxnum_1: 4 priority: 4 req_1: CYCLE 1; ! linenum: 430.000 targname: HD93308-NE config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G270H wavelength: 2240-3290 num_exp: 1 time_per_exp: 500 S s_to_n: 40 fluxnum_1: 5 priority: 4 req_1: CYCLE 1; ! linenum: 510.000 targname: HD93308-PKUP-OFFSET config: FOS/BL opmode: ACCUM aperture: 0.5 sp_element: G570H wavelength: 4610-5150 num_exp: 1 time_per_exp: 120 S s_to_n: 100 fluxnum_1: 3 priority: 5 req_1: CYCLE 1; ! linenum: 520.000 targname: HD93308-PKUP-OFFSET config: FOS/BL opmode: ACCUM aperture: 0.5 sp_element: G400H wavelength: 3250-4810 num_exp: 1 time_per_exp: 120 S s_to_n: 100 fluxnum_1: 4 priority: 5 req_1: CYCLE 1; ! linenum: 530.000 targname: HD93308-PKUP-OFFSET config: FOS/BL opmode: ACCUM aperture: 0.5 sp_element: G270H wavelength: 2240-3290 num_exp: 1 time_per_exp: 120 S s_to_n: 100 fluxnum_1: 5 priority: 5 req_1: CYCLE 1; ! ! end of exposure logsheet ! No scan data records found