! File: 4509C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:15:28:33 coverpage: title_1: A SPECTROSCOPIC MAP OF THE CORE OF ETA CARINAE - CYC3MEDIUM sci_cat: HOT STARS sci_subcat: MASSIVE STARS proposal_for: GO pi_title: PROF. pi_fname: KRIS pi_lname: DAVIDSON pi_inst: UNIVERSITY OF MINNESOTA pi_country: U.S.A. pi_phone: 612-624-5711 hours_pri: 0.48 num_pri: 11 fos: Y funds_amount: 63351 funds_length: 12 funds_date: JAN-94 off_fname: RICK off_lname: DUNN off_title: ASSISTANT DIRECTOR off_inst: 2710 off_addr_1: OFFICE OF RESEARCH AND TECHNOLOGY TRANSFER off_addr_2: ADMINISTRATIVE SERVICES CENTER, UNIV. OF MINNESOTA off_addr_3: 1919 UNIVERSITY AVE. off_city: ST. PAUL off_state: MN off_zip: 55455 off_country: U.S.A. off_phone: 612-624-8526 ! end of coverpage abstract: line_1: FOS/RD observations of the core of Eta Carinae at wavelengths 5000--8000 A are line_2: needed to supplement and complete the UV-visual FOS/BL spectra made in 1991. line_3: Eta Car, the very massive, most extreme LBV, has surprising sub-arcsec line_4: structure near its central star. Spectroscopy of this physically mysterious line_5: structure is needed before we can be sure of the nature of Eta Car, line_6: and only the HST/FOS can provide the necessary spatial resolution. line_7: FOS/BL data covering wavelengths 1200--5500 A were obtained in Cycle 1. line_8: Longer wavelengths are needed for many important emission lines and also to line_9: make connection with the speckle images observed around 8000 A. Moreover, line_10: the high FOS/RD count rates for this object will allow far more spatial line_11: information to be obtained than was practical with the FOS/BL detector. line_12: We propose to obtain short-exposure (but high S/N) data on a grid of positions line_13: about 1 arcsec across. For technical reasons related to the high count rates, line_14: Cycle 3 is probably the last realistic opportunity to obtain these data. ! ! end of abstract general_form_proposers: lname: DAVIDSON fname: KRIS title: PI inst: UNIVERSITY OF MINNESOTA country: USA ! lname: HUMPHREYS fname: ROBERTA mi: M. inst: UNIVERSITY OF MINNESOTA country: USA ! lname: ROSA fname: MICHAEL inst: EUROPEAN SOUTHERN OBSERVATORY country: GERMANY esa: Y ! lname: WALBORN fname: NOLAN mi: R. inst: STSCI country: USA ! lname: EBBETS fname: DENNIS inst: BALL AEROSPACE country: USA ! lname: WEIGELT fname: GERD inst: MAX-PLANCK-INSTITUT FUR RADIOASTRONOMIE country: GERMANY esa: Y ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: With the FOS/RD detector, which we require in order to reach line_2: wavelengths beyond 5500 A, only the smallest FOS aperture (0.1" line_3: square) is safe to use on the core of Eta Carinae; Eta is too line_4: bright for the other apertures. Fortunately we do not need line_5: absolute flux calibrations, so the 0.1" aperture is OK. This line_6: small aperture will give the best available combination of spatial line_7: and spectral resolution, regardless of HST's optical defect. line_8: (After COSTAR is installed, the core of Eta Car will be too bright line_9: for FOS/RD even with the 0.1" aperture.) Therefore we use FOS/RD line_10: with a 0.1" square aperture for all parts of this program. line_11: ---- The first step is a multi-stage peakup acquisition. The line_12: core of Eta Carinae is slightly diffuse and has several components line_13: in emission-line light, all within a size of the order of 0.3". line_14: The small aperture size is unconventional for the coarse stages line_15: of the peakup; but existing PC and FOC images, and a successful line_16: Cycle 1 peakup on the same target, indicate that our planned line_17: acquisition will indeed locate the peak or "centroid" of light. line_18: This peakup position will then be used as a convenient reference line_19: position for offsetting to other nearby target positions, all line_20: within 1". line_21: ---- Following the peakup acquisition, we observe a selected line_23: set of target locations, with separations of the order of 0.15" ! question: 3 section: 2 line_1: and acquired by offsets from the reference position. These line_2: targets will not be cleanly resolved from each other, given line_3: the HST's p.s.f. However, we will use specialized computer line_4: analyses of the entire set in order to disentangle the line_5: spectral components later (primary star, ejected knots, etc). line_6: An individual exposure time of only 2 minutes will give high line_7: S/N ratios for each of these bright target locations. We line_8: will use grating G570H for every target; gratings G400H and line_9: G780H will also be used for as many of the targets as possible. line_10: (G400H is a late addition to the program, intended to partially line_11: compensate for a recently-discovered ST pointing error in the line_12: cycle 1 FOS/BL observations.) ! question: 4 section: 1 line_1: Spatial resolution is the advantage of ST for this project. line_2: The "components" of Eta Carinae (primary star, blobs of ejecta, line_3: conceivably fainter companion stars) are separated by only line_4: 0.1 to 0.2". Ground-based speckle techniques can provide images line_5: but not detailed spectroscopic information on each component. line_6: -- Ironically, this project is possible only because of the ST's line_7: optical defect, even though high spatial resolution is a goal. line_8: If the HST's primary mirror were optically correct, then the line_9: FOS/RD count rates for our targets would be too high. line_10: --- Regarding COUNT RATES and exposure times: line_11: Cycle 1 FOS/BL observations of the peakup location showed line_12: that the 5000 A continuum flux through the 0.3" aperture line_13: (i.e., including the effect of aperture throughput) was line_14: about 6e-13 erg cm-2 s-1 A-1. The flux through the 0.1" line_15: aperture should be smaller by a factor of roughly 0.3 (a line_16: compromise between the point-source and extended-source line_17: cases). The expected count rate with grating G570H is then line_18: of the order of 400 counts/s per diode at 5000 A. The count line_19: rate would be less than 200 at long wavelengths, and more line_20: than 1000 in the peaks of several emission lines. A 2-minute line_21: exposure would therefore give a range of 15000--150000 counts line_22: per diode at the peakup target location, except in the very line_23: bright H-alpha emission line. ! question: 4 section: 2 line_1: --- The brightest emission in this object is the H-alpha line. line_2: The cycle 1 FOS/BL observations showed a maximum flux of about line_3: 6e-12 erg cm-2 s-1 A-1 getting through the 0.3" aperture at the line_4: peak of H-beta (H-alpha is not accessible with FOS/BL). The line_5: line width implicit here is largely instrumental (2 or 3 diodes). line_6: According to ground-based observations as well as theoretical line_7: considerations, the H-alpha emission is roughly 8 times as line_8: bright as H-beta, i.e. its peak would have been 5e-11 erg cm-2 line_9: s-1 A-1 through the 0.3" FOS aperture, or 1.5e-11 through the line_10: 0.1" aperture that we plan to use with FOS/RD. This gives a line_11: peak count rate of about 13000 or 22000 counts/s per diode, line_12: using grating G570H or G780H respectively. Count rates line_13: like this would occur in only 2 or 3 diodes, the apparent line_14: line width. line_15: --- The continuum and peak count rates discussed above refer line_16: to the peak-up target location; the outlying targets should line_17: be fainter by factors of about 3. line_18: --- Since it is difficult to describe our target brightnesses line_19: in terms of point sources, in the exposure log we have chosen line_20: to specify equivalent surface brightnesses instead, including line_21: blurring by the p.s.f. When estimating count rates from these line_22: numbers, use the aperture area (= 0.01 square arcsec) in place line_23: of the "throughput" (e.g. "7 percent") used for point sources. ! question: 5 section: 1 line_1: We do not have any special scheduling or calibration line_2: requests. The 0.1" FOS apertures are seldom used and line_3: may be uncalibrated, but we do not need absolute fluxes. line_4: The instrument orientation angle is not critical for line_5: our program. ! question: 6 section: 1 line_1: No special calibrations are needed (see question 5 above). ! question: 7 section: 1 line_1: Initial reduction of the FOS data should be more or less routine, line_2: except that the various targets must be treated very uniformly. line_3: Rosa and Davidson will share the initial data reduction. line_4: --- Then, however, subsquent analyses of the overall set of data line_5: will be very NON-routine and will require far more effort than line_6: normal for this amount of ST time. Davidson has already taken line_7: some exploratory steps in connection with earlier project line_8: GO 2338, and will be developing some of the necessary programs line_9: during summer 1993. The basic problem is that 2 to 5 line_10: different spectra will be mixed together in each of the line_11: target locations, with different mixing ratios of course. line_12: At present we expect to attempt two different approaches. line_13: In the first, we use only general ideas about characteristics line_14: of the different intrinsic spectra: "Given N observed spectra, line_15: each of which is a different mixture of M intrinsic spectra line_16: where M < N, what can we figure out about the intrinsic line_17: spectra?" Unique solutions cannot be found but additional line_18: astrophysical knowledge, e.g. of the differences between line_19: continuum and emission-line spectra, can help. In the second, line_20: potentially superior approach, we construct models of the line_21: FOS response as a function of position, consistent with the line_22: existing images (Ebbets' and Weigelt's ST images, Weigelt's line_23: speckle data) and with the ST's spatial p.s.f. convolved ! question: 7 section: 2 line_1: with the 0.1" FOS aperture. In the simplest form of this line_2: approach we model the object as 3 or 4 point sources; in line_3: an ultimate form this approach would be almost like image line_4: deconvolution of a whole "spectral map". Davidson, possibly line_5: assisted by a student and/or Rosa, will undertake these line_6: tasks. line_7: --- As noted above, Ebbets and especially Weigelt will provide line_8: high-resolution images needed for the analyses. Humphreys and line_9: Walborn will interpret the intrinsic spectrum of the primary line_10: star (and also secondary stars, if any are found to be line_11: present). Davidson and Rosa will interpret emission lines. line_12: It is possible that R. Kudritzki and K. Simon in Munich, line_13: who were CoIs on the related FOS/BL project GO 2338, will line_14: collaborate also on the final results, e.g. through stellar line_15: atmosphere modeling. line_16: --- Ultimately, the best possible separation of component line_17: spectra is so difficult that it will probably not be completed line_18: within a year of the observations. Of course we expect to line_19: publish interim results before that is finally done. ! question: 8 section: 1 line_1: No pertinent additional comments or requirements that we line_2: can think of. As noted above, HST imaging results from line_3: some other projects will probably be used for the data line_4: analysis; some of these images are generally available and line_5: CoIs on this proposal are obtaining the others. A "special line_6: catalog" of acquisition/guide stars for this field, ZZZQ, line_7: was prepared by KD several years ago using the Minnesota line_8: APS machine. ! question: 9 section: 1 line_1: --GO 2338, "Spectroscopy of ...Eta Carinae point sources" (Davidson line_2: was PI); very directly related to this project, because it was line_3: a predecessor using FOS/BL rather than FOS/RD. Because of line_4: the difficulty of the analysis, and lately because of discovery line_5: of an ST offsetting error, the results have not yet been published line_6: even though the spectral data are pretty good. line_7: --GTO 1186, "Imaging...Eta Car" and other GTO projects of Dennis line_8: Ebbets: some of the images will be used in connection with this line_9: project. Otherwise, Ebbets' Eta Car projects have been concerned line_10: mostly with the diffuse ejecta several arcsec from the core of line_11: Eta, rather than with this core itself. Some preliminary results line_12: have appeared in poster papers at several meetings, e.g. ASP line_13: at Madison, WI in summer 1992. line_14: --GO 3815, "UV Obs...Hubble-Sandage Variables" (Humphreys is line_15: PI): Not directly related, although the H-S variables are line_16: generically related to Eta Carinae. GO 3815 observations have not line_17: all been done yet, no publications yet. Several of us are line_18: involved with GO 3815. line_19: --GO 2416, "...super metal poor galaxies" (RJ Dufour was PI, line_20: KD was a CoI): not related to this project. line_21: --Rosa has been involved with number of other GTO projects. ! question: 10 section: 1 line_1: Computer infrastructure at Minnesota and ESO will be used for most line_2: of the data reduction and analysis; KD will be preparing some line_3: of the required special computer programs during spring and summer line_4: 1993. Supporting ground-based speckle data is provided by line_5: Weigelt's group, using ESO telescopes. A special catalog of line_6: guide stars, to replace the GSC in the crowded field of Eta Car, line_7: has been produced by KD using the Automated Plate Scanner at line_8: the University of Minnesota with various special plates. line_9: It is hoped that a student at Minnesota will assist with the line_10: the FOS-"spectral map" analysis. ! !end of general form text general_form_address: lname: DAVIDSON fname: KRIS category: PI inst: University of Minnesota addr_1: ASTRONOMY DEPT., UNIV. OF MINNESOTA addr_2: 116 CHURCH ST. S.E. city: MINNEAPOLIS state: MN zip: 55455 country: USA phone: 612-624-5711 ! ! end of general_form_address records fixed_targets: targnum: 10 name_1: HD93308-PKUP-OFFSET name_2: ETA-CAR-PKUP-OFFSET descr_1: A,148,159,926 pos_1: RA = 10H 45M 3.62S +/- 0.05S, pos_2: DEC = -59D 41' 3.9" +/- 0.4", pos_3: PLATE-ID = ZZZQ equinox: 2000 comment_1: SPECIAL CAT ZZZQ IS ESSENTIAL. comment_2: FLUXES PER SQ ARCSEC ARE DEFINED comment_3: HERE AS IF THIS WERE A DIFFUSE comment_4: OBJECT 0.4" ACROSS, INCLUDING comment_5: EFFECT OF PSF. SIMPLY MULTIPLY comment_6: SURF() VALUE BY FOS APERTURE AREA comment_7: USING 100-PERCENT THROUGHPUT. comment_8: H-ALPHA (6563) IS DEFINITELY comment_9: THE BRIGHTEST EMISSION LINE HERE. fluxnum_1: 1 fluxval_1: SURF(4000) = 10 +/- 5 E-12 fluxnum_2: 2 fluxval_2: SURF(5500) = 10 +/- 5 E-12 fluxnum_3: 3 fluxval_3: SURF(7000) = 10 +/- 5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(6563) = 2 +/- 1 E-9 fluxnum_5: 4 fluxval_5: W-LINE(6563) = 12 +/- 3 ! targnum: 110 name_1: HD93308-012E012S name_2: ETA-CAR-012E012S descr_1: A,148,159,926 pos_1: R = 0.177", pos_2: PA = 135D, pos_3: FROM 10 equinox: 2000 comment_1: SEE COMMENTS FOR TARGNUM 10. fluxnum_1: 1 fluxval_1: SURF(4000) = 10 +/- 5 E-12 fluxnum_2: 2 fluxval_2: SURF(5500) = 10 +/- 5 E-12 fluxnum_3: 3 fluxval_3: SURF(7000) = 10 +/- 5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(6563) = 2 +/- 1 E-9 fluxnum_5: 4 fluxval_5: W-LINE(6563) = 12 +/- 3 ! targnum: 120 name_1: HD93308-025E025S name_2: ETA-CAR-025E025S descr_1: A,148,159,926 pos_1: R = 0.354", pos_2: PA = 135D, pos_3: FROM 10 equinox: 2000 comment_1: SEE COMMENTS FOR TARGNUM 10. fluxnum_1: 1 fluxval_1: SURF(4000) = 10 +/- 5 E-12 fluxnum_2: 2 fluxval_2: SURF(5500) = 10 +/- 5 E-12 fluxnum_3: 3 fluxval_3: SURF(7000) = 10 +/- 5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(6563) = 2 +/- 1 E-9 fluxnum_5: 4 fluxval_5: W-LINE(6563) = 12 +/- 3 ! targnum: 130 name_1: HD93308-037E037S name_2: ETA-CAR-037E037S descr_1: A,148,159,926 pos_1: R = 0.530", pos_2: PA = 135D, pos_3: FROM 10 equinox: 2000 comment_1: SEE COMMENTS FOR TARGNUM 10. fluxnum_1: 1 fluxval_1: SURF(4000) = 10 +/- 5 E-12 fluxnum_2: 2 fluxval_2: SURF(5500) = 10 +/- 5 E-12 fluxnum_3: 3 fluxval_3: SURF(7000) = 10 +/- 5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(6563) = 2 +/- 1 E-9 fluxnum_5: 4 fluxval_5: W-LINE(6563) = 12 +/- 3 ! targnum: 210 name_1: HD93308-012W012N name_2: ETA-CAR-012W012N descr_1: A,148,159,926 pos_1: R = 0.177", pos_2: PA = 315D, pos_3: FROM 10 equinox: 2000 comment_1: SEE COMMENTS FOR TARGNUM 10. fluxnum_1: 1 fluxval_1: SURF(4000) = 10 +/- 5 E-12 fluxnum_2: 2 fluxval_2: SURF(5500) = 10 +/- 5 E-12 fluxnum_3: 3 fluxval_3: SURF(7000) = 10 +/- 5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(6563) = 2 +/- 1 E-9 fluxnum_5: 4 fluxval_5: W-LINE(6563) = 12 +/- 3 ! targnum: 220 name_1: HD93308-025W025N name_2: ETA-CAR-025W025N descr_1: A,148,159,926 pos_1: R = 0.354", pos_2: PA = 315D, pos_3: FROM 10 equinox: 2000 comment_1: SEE COMMENTS FOR TARGNUM 10. fluxnum_1: 1 fluxval_1: SURF(4000) = 10 +/- 5 E-12 fluxnum_2: 2 fluxval_2: SURF(5500) = 10 +/- 5 E-12 fluxnum_3: 3 fluxval_3: SURF(7000) = 10 +/- 5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(6563) = 2 +/- 1 E-9 fluxnum_5: 4 fluxval_5: W-LINE(6563) = 12 +/- 3 ! targnum: 230 name_1: HD93308-037W037N name_2: ETA-CAR-037W037N descr_1: A,148,159,926 pos_1: R = 0.530", pos_2: PA = 315D, pos_3: FROM 10 equinox: 2000 comment_1: SEE COMMENTS FOR TARGNUM 10. fluxnum_1: 1 fluxval_1: SURF(4000) = 10 +/- 5 E-12 fluxnum_2: 2 fluxval_2: SURF(5500) = 10 +/- 5 E-12 fluxnum_3: 3 fluxval_3: SURF(7000) = 10 +/- 5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(6563) = 2 +/- 1 E-9 fluxnum_5: 4 fluxval_5: W-LINE(6563) = 12 +/- 3 ! targnum: 310 name_1: HD93308-000E025N name_2: ETA-CAR-000E025N descr_1: A,148,159,926 pos_1: R = 0.250", pos_2: PA = 0D, pos_3: FROM 10 equinox: 2000 comment_1: SEE COMMENTS FOR TARGNUM 10. fluxnum_1: 1 fluxval_1: SURF(4000) = 10 +/- 5 E-12 fluxnum_2: 2 fluxval_2: SURF(5500) = 10 +/- 5 E-12 fluxnum_3: 3 fluxval_3: SURF(7000) = 10 +/- 5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(6563) = 2 +/- 1 E-9 fluxnum_5: 4 fluxval_5: W-LINE(6563) = 12 +/- 3 ! targnum: 320 name_1: HD93308-025E025N name_2: ETA-CAR-025E025N descr_1: A,148,159,926 pos_1: R = 0.354", pos_2: PA = 45D, pos_3: FROM 10 equinox: 2000 comment_1: SEE COMMENTS FOR TARGNUM 10. fluxnum_1: 1 fluxval_1: SURF(4000) = 10 +/- 5 E-12 fluxnum_2: 2 fluxval_2: SURF(5500) = 10 +/- 5 E-12 fluxnum_3: 3 fluxval_3: SURF(7000) = 10 +/- 5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(6563) = 2 +/- 1 E-9 fluxnum_5: 4 fluxval_5: W-LINE(6563) = 12 +/- 3 ! targnum: 410 name_1: HD93308-025W000S name_2: ETA-CAR-025W000S descr_1: A,148,159,926 pos_1: R = 0.250", pos_2: PA = 270D, pos_3: FROM 10 equinox: 2000 comment_1: SEE COMMENTS FOR TARGNUM 10. fluxnum_1: 1 fluxval_1: SURF(4000) = 10 +/- 5 E-12 fluxnum_2: 2 fluxval_2: SURF(5500) = 10 +/- 5 E-12 fluxnum_3: 3 fluxval_3: SURF(7000) = 10 +/- 5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(6563) = 2 +/- 1 E-9 fluxnum_5: 4 fluxval_5: W-LINE(6563) = 12 +/- 3 ! targnum: 420 name_1: HD93308-025W025S name_2: ETA-CAR-025W025S descr_1: A,148,159,926 pos_1: R = 0.354", pos_2: PA = 225D, pos_3: FROM 10 equinox: 2000 comment_1: SEE COMMENTS FOR TARGNUM 10. fluxnum_1: 1 fluxval_1: SURF(4000) = 10 +/- 5 E-12 fluxnum_2: 2 fluxval_2: SURF(5500) = 10 +/- 5 E-12 fluxnum_3: 3 fluxval_3: SURF(7000) = 10 +/- 5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(6563) = 2 +/- 1 E-9 fluxnum_5: 4 fluxval_5: W-LINE(6563) = 12 +/- 3 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 11.000 targname: HD93308-PKUP-OFFSET config: FOS/RD opmode: ACQ/PEAK aperture: 0.1-PAIR-B sp_element: G570H wavelength: 4600-4820 num_exp: 1 time_per_exp: 6S s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE-X=5 param_2: SCAN-STEP-X=0.72 param_3: SEARCH-SIZE-Y=5 param_4: SCAN-STEP-Y=0.72 req_1: CYCLE 3 / 11-150; req_2: ONBOARD ACQ FOR 12; comment_1: TOO BRIGHT FOR LARGER APERTURE. comment_2: PEAKUP OBJECTIVE IS CENTROID comment_3: OF SMALL EXTENDED SOURCE. comment_4: ONLY 4600-4820A ENABLED, TO comment_5: EXCLUDE BRIGHT EMIS LINES ! linenum: 12.000 targname: HD93308-PKUP-OFFSET config: FOS/RD opmode: ACQ/PEAK aperture: 0.1-PAIR-B sp_element: G570H wavelength: 4600-4820 num_exp: 1 time_per_exp: 8S s_to_n: 40 fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE-X=4 param_2: SCAN-STEP-X=0.28 param_3: SEARCH-SIZE-Y=4 param_4: SCAN-STEP-Y=0.28 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 13; comment_1: SEE COMMENTS LINE 11. ! linenum: 13.000 targname: HD93308-PKUP-OFFSET config: FOS/RD opmode: ACQ/PEAK aperture: 0.1-PAIR-B sp_element: G570H wavelength: 4600-4820 num_exp: 1 time_per_exp: 32S s_to_n: 100 fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE-X=6 param_2: SCAN-STEP-X=0.065 param_3: SEARCH-SIZE-Y=6 param_4: SCAN-STEP-Y=0.065 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 100-150; comment_1: SEE COMMENTS LINE 11. comment_2: 6 X 6 FINAL PEAKUP MAP comment_3: WILL BE USED TO HELP comment_4: ANALYZE DATA. ! linenum: 51.000 sequence_1: DEFINE sequence_2: THREEGR targname: # config: FOS/RD opmode: RAPID aperture: 0.1-PAIR-B sp_element: G570H num_exp: 1 time_per_exp: 128S s_to_n: 60 fluxnum_1: 2 priority: 1 param_1: READ-TIME=3.2, param_2: STEP-TIME=0.1, param_3: STEP-PATT=SINGLE req_1: GROUP 51-53 NO GAP comment_1: FORCE TAPE RECORDER TO 32K BIT. comment_2: S/N REFERS TO 1/4 DIODE. comment_3: USE RAPID MODE BECAUSE comment_4: H-ALPHA IS VERY BRIGHT, comment_5: SEE FLUXNUM 4. ! linenum: 52.000 sequence_1: DEFINE sequence_2: THREEGR targname: # config: FOS/RD opmode: RAPID aperture: 0.1-PAIR-B sp_element: G780H num_exp: 1 time_per_exp: 140.8S s_to_n: 45 fluxnum_1: 3 priority: 1 param_1: READ-TIME=3.2, param_2: STEP-TIME=0.1, param_3: STEP-PATT=SINGLE comment_1: FORCE TAPE RECORDER TO 32K BIT. comment_2: SEE COMMENTS LINE 51. ! linenum: 53.000 sequence_1: DEFINE sequence_2: THREEGR targname: # config: FOS/RD opmode: ACCUM aperture: 0.1-PAIR-B sp_element: G400H wavelength: 3240-4787 num_exp: 1 time_per_exp: 80S s_to_n: 55 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=SINGLE comment_1: S/N FOR 1/4 DIODE. ! linenum: 61.000 sequence_1: DEFINE sequence_2: TWOGR targname: # config: FOS/RD opmode: RAPID aperture: 0.1-PAIR-B sp_element: G570H num_exp: 1 time_per_exp: 128S s_to_n: 60 fluxnum_1: 2 priority: 1 param_1: READ-TIME=3.2, param_2: STEP-TIME=0.1, param_3: STEP-PATT=SINGLE req_1: GROUP 61-62 NO GAP comment_1: FORCE TAPE RECORDER TO 32K BIT. comment_2: SEE COMMENTS LINE 51. ! linenum: 62.000 sequence_1: DEFINE sequence_2: TWOGR targname: # config: FOS/RD opmode: RAPID aperture: 0.1-PAIR-B sp_element: G780H num_exp: 1 time_per_exp: 140.8S s_to_n: 45 fluxnum_1: 3 priority: 1 param_1: READ-TIME=3.2, param_2: STEP-TIME=0.1, param_3: STEP-PATT=SINGLE comment_1: FORCE TAPE RECORDER TO 32K BIT. comment_2: SEE COMMENTS LINE 51. ! linenum: 71.000 sequence_1: DEFINE sequence_2: ONEGR targname: # config: FOS/RD opmode: RAPID aperture: 0.1-PAIR-B sp_element: G570H num_exp: 1 time_per_exp: 128S s_to_n: 60 fluxnum_1: 2 priority: 1 param_1: READ-TIME=3.2, param_2: STEP-PATT=SINGLE comment_1: FORCE TAPE RECORDER TO 32K BIT. comment_2: SEE COMMENTS LINE 51. ! linenum: 100.000 sequence_1: USE sequence_2: TWOGR targname: HD93308-PKUP-OFFSET req_1: GROUP 100-150 NO GAP ! linenum: 105.000 sequence_1: USE sequence_2: THREEGR targname: HD93308-012E012S ! linenum: 110.000 sequence_1: USE sequence_2: THREEGR targname: HD93308-012W012N ! linenum: 115.000 sequence_1: USE sequence_2: TWOGR targname: HD93308-025W025N ! linenum: 120.000 sequence_1: USE sequence_2: ONEGR targname: HD93308-037W037N ! linenum: 125.000 sequence_1: USE sequence_2: TWOGR targname: HD93308-025E025S ! linenum: 130.000 sequence_1: USE sequence_2: ONEGR targname: HD93308-037E037S ! linenum: 135.000 sequence_1: USE sequence_2: TWOGR targname: HD93308-025W000S ! linenum: 140.000 sequence_1: USE sequence_2: ONEGR targname: HD93308-025W025S ! linenum: 145.000 sequence_1: USE sequence_2: TWOGR targname: HD93308-000E025N ! linenum: 150.000 sequence_1: USE sequence_2: ONEGR targname: HD93308-025E025N ! ! end of exposure logsheet ! No scan data records found