! $Id: 5676,v 8.1 1994/07/27 20:17:59 pepsa Exp $ coverpage: title_1: UV SPECTROSCOPY AND IMAGING IN THE CRAB NEBULA - CARRYOVER sci_cat: INTERSTELLAR MEDIUM sci_subcat: SN & SNR proposal_for: GO/CAR cont_id: 4356 pi_title: PROF. pi_fname: KRIS pi_lname: DAVIDSON pi_inst: UNIVERSITY OF MINNESOTA pi_country: USA pi_phone: 612-624-5711 hours_pri: 5.58 num_pri: 8 fos: Y funds_amount: 131756 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, UNIVERSITY OF MINNESOTA off_addr_3: 1919 UNIVERSITY AVE. off_city: ST. PAUL off_state: MN off_zip: 55455 off_country: USA off_phone: 612-624-8526 ! end of coverpage abstract: line_1: The Crab Nebula is the most observable SNR that is composed mainly of line_2: processed ejecta rather than swept-up interstellar matter. This makes line_3: it one of the most critical of all astronomical objects for SN and line_4: nucleosynthesis theory. However, despite its fame, the Crab is NOT line_5: understood and does not yet give much support to stellar evolution and line_6: nucleosynthesis theory. A shortage of nitrogen is particularly line_7: troubling, among other unresolved puzzles. Meanwhile, line_8: chemical abundance variations and correlations with bipolar structure line_9: have recently become interesting with reference to other objects line_10: (e.g. SN1987A). ...These problems absolutely require UV observations line_11: of the Crab which can be done only with HST. UV spectra with FOS are line_12: most obviously needed, mainly to obtain C, N, Mg, and Si abundances. line_13: UV images with FOC are also highly desirable, in case there are line_14: surprises such as (e.g.) carbon-rich UV-bright condensations. No such line_15: data will have been obtained yet by the end of HST Cycle 2 -- not even line_16: a brief reconnaissance. Here we propose a suitable program of exploratory line_17: FOC and especially FOS observations. These observations are line_18: appropriate for Cycle 3 (i.e., before COSTAR) because their spatial line_19: resolution is limited by S/N, not by telescope optics. ! ! end of abstract general_form_proposers: lname: DAVIDSON fname: KRIS title: PI inst: UNIVERSITY OF MINNESOTA country: USA ! lname: UOMOTO fname: ALAN mi: K inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: MACALPINE fname: GORDON mi: M inst: UNIVERSITY OF MICHIGAN country: USA ! lname: BLAIR fname: WILLIAM mi: P inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: HENRY fname: RICHARD mi: BC inst: UNIVERSITY OF OKLAHOMA country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We propose FOS spectroscopy of 4 selected target condensations in line_2: the Crab Nebula, using the largest ordinary FOS aperture (1" sq) line_3: and the FOS/BL detector. We concentrate on the spectral range line_4: 1230--2000 A where the most important emission lines are, mainly line_5: using grating G160L but also using G130H and G190H for the brightest line_6: target. Spectral range 2000--3300 A is given less emphasis, using line_7: G270H. Longer wavelengths are also sampled with short exposure line_8: times using grating G400H, in order to normalize fluxes measured line_9: in ground-based data (not yet obtained). Exposure times range line_10: from 3 minutes (G400H only) to almost an hour each. line_11: ... In increasing order of difficulty, our goals are (1) to line_12: measure the CIV 1548, HeII 1640, and CIII 1908 emission lines line_13: to estimate the carbon abundance; (2) to detect NIII 1750 in line_14: order to make nitrogen estimates far more secure; and (3) to line_15: detect other lines of NIV, SiIII, SiIV, etc., all in the same line_16: wavelength range. In the lower-priority 2000-3300 A range we line_17: hope to discover whether MgII 2798 and/or other lines are present. line_18: ... The target condensations are diffuse, with typical diameters line_19: of roughly 2". Our target selection criteria are (1) each line_20: target condensation is among the 40 brightest local peaks line_21: in the Crab Nebula in [OIII] light; (2) each target is a line_22: relatively well-defined conensation, or a sector of a narrow line_23: filament; and (3) we sample the morphologically different ! question: 3 section: 2 line_1: parts of the SNR as widely as possible with this small a line_2: number of targets. line_3: ... Acquisitions will be by offset from reference stars. line_4: We have measured positions of the targets and offset stars line_5: using high-quality ground-based CCD images; pointing line_6: accuracies of 0.1" or even 0.2" are acceptable and we have line_7: measured the required offsets to slightly better than 0.1" line_8: (rms dev). We have taken the small expansionary motion of line_9: the SNR into account in the planned offsets. line_10: ... Originally we hoped to use the FOS/RD detector in line_11: addition to FOS/BL, to provide better efficiency at most line_12: wavelengths. However, FOS/BL is definitely needed for line_13: the shortest-wavelength lines and there is not enough line_14: available time to make side-switches practical. line_15: ...... Our Phase I proposal also included UV imaging with line_16: the FOC. However, we and the TAC agree that spectroscopy line_17: has a higher priority, and with the limited amount of line_18: time that has been allotted we have deleted the FOC images. line_19: (One reason is that the FOS is better-suited than the FOC line_20: for observations of a low-surface-brightness extended object line_21: like the Crab.) line_22: ...... Altogether, this project should be viewed as a line_23: reconnaissance rather than a full detailed study. ! question: 4 section: 1 line_1: HST is needed because these are UV observations of faint, line_2: small objects. line_3: ... A major effort was made to observe the Crab Nebula with line_4: IUE, with marginal results reported by Davidson et al. (1982) line_5: Ap.J. 253, 696. The IUE was capable of measuring just the line_6: three brightest UV lines (CIV 1548, HeII 1640, CIII 1908) line_7: integrated over the brightest large amorphous region in the line_8: Crab. The story for ASTRO (HUT and UIT) is similar, with line_9: even less spatial resolution for the spectroscopy. With HST line_10: we can observe particular condensations (this is important line_11: for theoretical modeling), the sensitivity is adequate to line_12: observe additional locations in the SNR (morphological line_13: variations are known to exist there), and we hope to detect line_14: important fainter lines, especially NIII 1750. line_15: ... We will supplement the HST/FOS observations with line_16: specific ground-based spectroscopy of exactly the same line_17: targets at longer wavelengths. We hope to obtain these line_18: ground-based data in late 1993. line_19: ... Example of expected count rates and exposure time: line_20: Based on available IUE and ground-based data, combined line_21: with ionization models, we expect the CIII 1908 emission line_22: line to produce a flux of the order of 1.e-15 erg cm-2 s-1 line_23: through the 1" square FOS aperture at one of our targets. ! question: 4 section: 2 line_1: With the efficiencies listed in the FOS handbook this will line_2: give somewhat less than 200 counts per hour with G160L. line_3: NIII 1750 is "expected" to be several times fainter. Therefore line_4: exposure times approaching an hour are needed for this part of line_5: the spectrum (even though one motivation for the project is the line_6: hope that some regions will be brighter than expected in some line_7: UV emission lines). ! question: 5 section: 1 line_1: We have no special scheduling requests. There is no need line_2: for any particular orientation of the FOS aperture. There line_3: is no need for the targets to be observed all on the same line_4: day or even the same month. ! question: 6 section: 1 line_1: No special calibration requirements are needed. ! ! question: 8 section: 1 line_1: During January 1993 we have measured the precise target offsets line_2: and other acquisition data, using several different CCD images line_3: and plates obtained in 1986-1991. line_4: --- Precisely-positioned violet-to-red spectrophotometry of line_5: our FOS targets will be obtained with the McGraw-Hill 2.4-m line_6: telescope and (we hope) with one or more larger telescopes line_7: also. ! question: 9 section: 1 line_1: --GO 2338, "Spectroscopy of...Eta Carinae", Davidson is PI; not line_2: related to this project. line_3: --GO 2416, "Imagery and spectroscopy of super metal poor galaxies", line_4: Davidson was a CoI. Not related. line_5: --GO 3815, "UV observations of Hubble-Sandage variables...", line_6: Davidson is a CoI. Not related. line_7: --GTO 1062, "A Search for Extra-Solar Planets", Uomoto is a CoI. line_8: Not related. line_9: --Uomoto and Davidson are also assisting some GTO programs, but line_10: not as CoIs. line_11: --Data from these programs: FOS data were obtained in GO 2338, line_12: but are not ready for publication yet because of the complexity line_13: of the data. GO 2416 observations began in August 1992 and are line_14: still in progress; no publications yet. GTO 1062 is a "cycle 9" line_15: project, no data yet. ! question: 10 section: 1 line_1: Most importantly, the McGraw-Hill 2.4-m telescope will be used line_2: for ground-based spectrophotometry of our FOS targets. line_3: The usual computer infrastructure is provided by each of our line_4: institutions. Students at several of our institutions will line_5: probably be involved in the data reduction and analysis and line_6: in the ground-based observations. The APS at the University line_7: of Minnesota was already used several years ago to assess line_8: reliability of the GSC acquisition and guide stars in the line_9: field of the Crab Nebula. ! !end of general form text general_form_address: lname: DAVIDSON fname: KRIS category: PI inst: University of Minnesota addr_1: UNIVERSITY OF MINNESOTA addr_2: ASTRONOMY DEPT. addr_3: 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: WM09-053427+220047-STAR-OFFSET name_2: CRAB-NEB-STAR-071X-008Y-OFFSET descr_1: A,140 pos_1: RA = 5H 34M 27.20S +/- 0.04S, pos_2: DEC = +22D 0' 47.7" +/- 0.3", pos_3: PLATE-ID=000M equinox: J2000 comment_1: WM REF STARS--WYCKOFF AND MURRAY comment_2: 1977, MNRAS 180, 717. SP TYPES ARE comment_3: UNKNOWN, COLORS ONLY EDUC GUESSES. comment_4: LOCAL X,Y COORDS (ARCSEC, EQ 2000) comment_5: ARE GIVEN IN NAME_2. comment_6: -- RE. PLATE-ID: OUR COORDS WERE comment_7: NOT MEASURED WITH GSSS, BUT ARE comment_8: CONSISTENT WITH GSC PLATE 000M, AND comment_9: NOT WITH PLATE 0075 WHICH comment_10: DISAGREES BY 2". fluxnum_1: 1 fluxval_1: V = 14.5 +/- 0.2 fluxnum_2: 2 fluxval_2: B-V = 1.1 +/- 0.3 ! targnum: 11 name_1: NGC1952-053429+220037 name_2: CRAB-NEB-KNOT-043X-018Y name_3: CRAB-NEB-BF1 descr_1: G,506,925,927 pos_1: R = 29.43", pos_2: PA = 109.9D, pos_3: FROM 10, equinox: J2000 comment_1: CONDENSATION IN BRIGHTEST FILAMENT comment_2: OF CRAB NEB. FLUXES ARE GUESSES comment_3: BASED ON CCD IMS AND IUE, DEFINED comment_4: SO THAT FOS APERTURE THROUGHPUT IS comment_5: INCLUDED. W-LINE = 1.0 IS NOMINAL comment_6: VALUE, REAL LWIDTHS ARE UNKNOWN, comment_7: PRODUCT (SURF-LINE * W-LINE) IS OK. fluxnum_1: 1 fluxval_1: SURF(V) = 20.0 +/- 1.0 fluxnum_2: 2 fluxval_2: SURF-LINE(1548) = 16 +/- 7 E-16 fluxnum_3: 2 fluxval_3: W-LINE(1548) = 1.0 +/- 0.5 fluxnum_4: 3 fluxval_4: SURF-LINE(1908) = 16 +/- 7 E-16 fluxnum_5: 3 fluxval_5: W-LINE(1908) = 1.0 +/- 0.5 fluxnum_6: 4 fluxval_6: SURF-LINE(2798) = 4 +/- 4 E-16 fluxnum_7: 4 fluxval_7: W-LINE(2798) = 1.0 +/- 0.5 fluxnum_8: 5 fluxval_8: SURF-LINE(3727) = 160 +/- 70 E-16 fluxnum_9: 5 fluxval_9: W-LINE(3727) = 1.0 +/- 0.5 fluxnum_10: 6 fluxval_10: SIZE = 2 +/- 1 ! targnum: 30 name_1: WM17-053433+220229-STAR-OFFSET name_2: CRAB-NEB-STAR+017X+094Y-OFFSET descr_1: A,140 pos_1: RA = 5H 34M 33.54S +/- 0.04S, pos_2: DEC = +22D 2' 29.7" +/- 0.3", pos_3: PLATE-ID=000M equinox: J2000 comment_1: SEE COMMENTS FOR TARGET 10 fluxnum_1: 1 fluxval_1: V = 15.25 +/- 0.2 fluxnum_2: 2 fluxval_2: B-V = 0.8 +/- 0.3 ! targnum: 31 name_1: NGC1952-053433+220202 name_2: CRAB-NEB-KNOT+013X+067Y name_3: CRAB-NEB-N2 descr_1: G,506,925,927 pos_1: R = 27.41", pos_2: PA = 189.53D, pos_3: FROM 30, equinox: J2000 comment_1: EAST SIDE NORTHERN LOOP, CRAB NEB. comment_2: SEE TARGET 11 COMMENTS. fluxnum_1: 1 fluxval_1: SURF(V) = 20.0 +/- 1.0 fluxnum_2: 2 fluxval_2: SURF-LINE(1548) = 8 +/- 4 E-16 fluxnum_3: 2 fluxval_3: W-LINE(1548) = 1.0 +/- 0.5 fluxnum_4: 3 fluxval_4: SURF-LINE(1908) = 8 +/- 4 E-16 fluxnum_5: 3 fluxval_5: W-LINE(1908) = 1.0 +/- 0.5 fluxnum_6: 4 fluxval_6: SURF-LINE(2798) = 2 +/- 2 E-16 fluxnum_7: 4 fluxval_7: W-LINE(2798) = 1.0 +/- 0.5 fluxnum_8: 5 fluxval_8: SURF-LINE(3727) = 80 +/- 30 E-16 fluxnum_9: 5 fluxval_9: W-LINE(3727) = 1.0 +/- 0.5 ! targnum: 40 name_1: WM21-053436+220037-STAR-OFFSET name_2: CRAB-NEB-STAR+048X-019Y-OFFSET descr_1: A,140 pos_1: RA = 5H 34M 35.71S +/- 0.04S, pos_2: DEC = +22D 0' 37.3" +/- 0.3", pos_3: PLATE-ID=000M equinox: J2000 comment_1: SEE COMMENTS FOR TARGET 10 fluxnum_1: 1 fluxval_1: V = 15.5 +/- 0.2 fluxnum_2: 2 fluxval_2: B-V = 1.1 +/- 0.3 ! targnum: 41 name_1: NGC1952-053434+220051 name_2: CRAB-NEB-KNOT+025X-005Y name_3: CRAB-NEB-E2 descr_1: G,506,925,927 pos_1: R = 26.27", pos_2: PA = 302.6D, pos_3: FROM 40, equinox: J2000 comment_1: IN FILAMENT E OF PULSAR, CRAB NEB. comment_2: SEE TARGET 11 COMMENTS. fluxnum_1: 1 fluxval_1: SURF(V) = 20.0 +/- 1.0 fluxnum_2: 2 fluxval_2: SURF-LINE(1548) = 7 +/- 4 E-16 fluxnum_3: 2 fluxval_3: W-LINE(1548) = 1.0 +/- 0.5 fluxnum_4: 3 fluxval_4: SURF-LINE(1908) = 7 +/- 4 E-16 fluxnum_5: 3 fluxval_5: W-LINE(1908) = 1.0 +/- 0.5 fluxnum_6: 4 fluxval_6: SURF-LINE(2798) = 2 +/- 2 E-16 fluxnum_7: 4 fluxval_7: W-LINE(2798) = 1.0 +/- 0.5 fluxnum_8: 5 fluxval_8: SURF-LINE(3727) = 70 +/- 30 E-16 fluxnum_9: 5 fluxval_9: W-LINE(3727) = 1.0 +/- 0.5 ! targnum: 50 name_1: WM18-053433+215951-STAR-OFFSET name_2: CRAB-NEB-STAR+011X-064Y-OFFSET descr_1: A,140 pos_1: RA = 5H 34M 33.07S +/- 0.04S, pos_2: DEC = +21D 59' 51.7" +/- 0.3", pos_3: PLATE-ID=000M equinox: J2000 acqpr_1: BKG comment_1: SEE COMMENTS FOR TARGET 10 comment_2: THIS IS OUR FAINTEST ACQ STAR comment_3: BUT HAS BRIGHTEST BACKGROUND fluxnum_1: 1 fluxval_1: V = 16.4 +/- 0.2 fluxnum_2: 2 fluxval_2: B-V = 1.3 +/- 0.2 fluxnum_3: 3 fluxval_3: SURF-BKG(V) = 20.1 +/- 0.2 ! targnum: 51 name_1: NGC1952-053434+215953 name_2: CRAB-NEB-KNOT+030X-063Y name_3: CRAB-NEB-S1 descr_1: G,506,925,927 pos_1: R = 19.67", pos_2: PA = 87.5D, pos_3: FROM 50, equinox: J2000 comment_1: IN BRT FIL S OF PULSAR, CRAB NEB. comment_2: SEE TARGET 11 COMMENTS. fluxnum_1: 1 fluxval_1: SURF(V) = 20.0 +/- 1.0 fluxnum_2: 2 fluxval_2: SURF-LINE(1548) = 9 +/- 4 E-16 fluxnum_3: 2 fluxval_3: W-LINE(1548) = 1.0 +/- 0.5 fluxnum_4: 3 fluxval_4: SURF-LINE(1908) = 9 +/- 4 E-16 fluxnum_5: 3 fluxval_5: W-LINE(1908) = 1.0 +/- 0.5 fluxnum_6: 4 fluxval_6: SURF-LINE(2798) = 2 +/- 2 E-16 fluxnum_7: 4 fluxval_7: W-LINE(2798) = 1.0 +/- 0.5 fluxnum_8: 5 fluxval_8: SURF-LINE(3727) = 90 +/- 40 E-16 fluxnum_9: 5 fluxval_9: W-LINE(3727) = 1.0 +/- 0.5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 10.100 sequence_1: DEFINE sequence_2: FOSEQ-1 targname: # config: FOS/BL opmode: ACCUM aperture: 1.0-PAIR sp_element: G130H num_exp: 1 time_per_exp: 55M s_to_n: 11 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=SINGLE req_1: CYCLE 4 / 10.1-10.4; ! req_1: CYCLE 3 / 10.1-10.4; req_2: GROUP 10.1-10.4 NO GAP comment_1: QUOTED S/N RATIO REFERS TO TOTAL comment_2: EMISSION LINE, MORE THAN ONE DIODE. comment_3: THIS SEQ FOR BRIGHTEST TARG ONLY. ! linenum: 10.200 sequence_1: DEFINE sequence_2: FOSEQ-1 targname: # config: FOS/BL opmode: ACCUM aperture: 1.0-PAIR sp_element: G190H num_exp: 1 time_per_exp: 55M s_to_n: 18 fluxnum_1: 3 priority: 1 param_1: STEP-PATT=SINGLE comment_1: SEE COMMENTS FOR LINE 10.1. ! linenum: 10.300 sequence_1: DEFINE sequence_2: FOSEQ-1 targname: # config: FOS/BL opmode: ACCUM aperture: 1.0-PAIR sp_element: G270H num_exp: 1 time_per_exp: 20M s_to_n: 10 fluxnum_1: 4 priority: 1 param_1: STEP-PATT=SINGLE comment_1: SEE COMMENTS FOR LINE 10.1. ! linenum: 10.400 sequence_1: DEFINE sequence_2: FOSEQ-1 targname: # config: FOS/BL opmode: ACCUM aperture: 1.0-PAIR sp_element: G400H num_exp: 1 time_per_exp: 5M s_to_n: 38 fluxnum_1: 5 priority: 1 param_1: STEP-PATT=SINGLE comment_1: G400H USED FOR NORMALIZATION comment_2: OF GROUND-BASED DATA. comment_3: SEE COMMENTS FOR LINE 10.1. ! linenum: 11.100 sequence_1: DEFINE sequence_2: FOSEQ-2 targname: # config: FOS/BL opmode: ACCUM aperture: 1.0-PAIR sp_element: G160L num_exp: 1 time_per_exp: 60M s_to_n: 10 fluxnum_1: 2 priority: 2 param_1: STEP-PATT=SINGLE req_1: CYCLE 4 / 11.1-11.2; ! req_1: CYCLE 3 / 11.1-11.2; req_2: GROUP 11.1-11.2 NO GAP comment_1: QUOTED S/N RATIO REFERS TO TOTAL comment_2: EMISSION LINE, MORE THAN ONE DIODE. comment_3: TARGETS FOR THIS SEQ ALL HAVE comment_4: SIMILAR EXPECTED BRIGHTNESS. ! linenum: 11.200 sequence_1: DEFINE sequence_2: FOSEQ-2 targname: # config: FOS/BL opmode: ACCUM aperture: 1.0-PAIR sp_element: G400H num_exp: 1 time_per_exp: 5M s_to_n: 30 fluxnum_1: 5 priority: 2 param_1: STEP-PATT=SINGLE comment_1: G400H USED FOR NORMALIZATION comment_2: OF GROUND-BASED DATA. comment_3: SEE COMMENTS FOR LINE 11.1. ! linenum: 110.000 targname: WM09-053427+220047-STAR-OFFSET config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 31S ! original cy3 value was-- time_per_exp: 25S fluxnum_1: 1 priority: 1 req_1: CYCLE 4 / 110-111; ! req_1: CYCLE 3 / 110-111; req_2: ONBOARD ACQ FOR 111; req_3: SEQ 110-111 NO GAP comment_1: TARGNUM 10 comment_2: please check time_per_exp? ! linenum: 111.000 sequence_1: USE sequence_2: FOSEQ-1 targname: NGC1952-053429+220037 comment_1: TARGNUM 11 comment_2: SEE SEQ DEF FOR S/N ! linenum: 130.000 targname: WM17-053433+220229-STAR-OFFSET config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 35S ! original value was-- time_per_exp: 35S fluxnum_1: 1 priority: 2 req_1: CYCLE 4 / 130-131; ! req_1: CYCLE 3 / 130-131; req_2: ONBOARD ACQ FOR 131; req_3: SEQ 130-131 NO GAP comment_1: TARGNUM 30 comment_2: please check time_per_exp? ! linenum: 131.000 sequence_1: USE sequence_2: FOSEQ-2 targname: NGC1952-053433+220202 comment_1: TARGNUM 31 comment_2: SEE SEQ DEF FOR S/N; TARGNUMS comment_3: 31,41,51 HAVE SIMILAR FLUXES. ! linenum: 140.000 targname: WM21-053436+220037-STAR-OFFSET config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 76S ! original cy3 value was-- time_per_exp: 65S fluxnum_1: 1 priority: 2 req_1: CYCLE 4 / 140-141; ! req_1: CYCLE 3 / 140-141; req_2: ONBOARD ACQ FOR 141; req_3: SEQ 140-141 NO GAP comment_1: TARGNUM 40 comment_2: please check time_per_exp ? ! linenum: 141.000 sequence_1: USE sequence_2: FOSEQ-2 targname: NGC1952-053434+220051 comment_1: TARGNUM 41 comment_2: SEE LINE 131 COMMENT ! linenum: 150.000 targname: WM18-053433+215951-STAR-OFFSET config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 260S ! original cy3 value was-- time_per_exp: 3M fluxnum_1: 1 priority: 2 req_1: CYCLE 4 / 150-151; ! req_1: CYCLE 3 / 150-151; req_2: ONBOARD ACQ FOR 151; req_3: SEQ 150-151 NO GAP comment_1: TARGNUM 50 comment_2: please check time_per_exp? ! linenum: 151.000 sequence_1: USE sequence_2: FOSEQ-2 targname: NGC1952-053434+215953 comment_1: TARGNUM 51 comment_2: SEE LINE 121 COMMENT ! ! end of exposure logsheet ! No scan data records found