! $Id: 5492,v 20.1 1995/07/12 18:33:00 pepsa Exp $ coverpage: title_1: DETECTION OF THE INTERGALACTIC MEDIUM USING GUNN-PETERSON HEII304A title_2: ABSORPTION IN QSOS, AND FAR UV SPECTRA (CYCLE 4, HIGH, GO-5492) sci_cat: QUASARS & AGN sci_subcat: QUASAR ABSORPTION proposal_for: GO pi_fname: DAVID pi_mi: R. pi_lname: TYTLER pi_inst: 1560 pi_country: USA hours_pri: 23.40 num_pri: 2 fos: Y funds_amount: 95000 funds_length: 24 ! end of coverpage abstract: line_1: FOS ultraviolet spectra will be obtained of two high zem QSOs which line_2: we have recently detected at 1400A with the FOC. One is the only QSO line_3: known which has sufficient ultraviolet flux for FOS spectra at line_4: wavelengths below HeII 304. The detection of Gunn-Peterson absorption line_5: by the Helium II Lyman-Alpha line at 304A, one of the most exciting line_6: prospects of the HST, will provide the first direct detection of the line_7: diffuse intergalactic medium (IGM). The absence of Gunn-Peterson H I line_8: 1215 absorption shows that the IGM is hot and/or of very low density, line_9: thus He I 584 is not seen. He II 304--the most promising line--should line_10: be observable from three sources: the diffuse IGM, the discrete line_11: Lyman-Alpha clouds, and the much rarer metal line absorption systems. line_12: The Gunn-Peterson continuum optical depth is not well constrained by line_13: models (range 0.3-3000). The mere detection of this one QSO below 304A line_14: would rule out many models, limiting the IGM density, temperature, and line_15: ionization mechanisms. The total absence of flux from several targets line_16: would rule out other models. The second QSO is the second brightest line_17: object known to have flux near 300A. Its redshift is too low to show line_18: HeII 304, but it is the only QSO which we know which is bright enough line_19: to check the exciting claim by Reimers etal that absorption systems line_20: show enhanced O/C abundances. ! ! end of abstract general_form_proposers: lname: TYTLER fname: DAVID title: PI mi: R inst: 1560 - UNIVERSITY OF CALIFORNIA, SAN DIEGO country: USA esa: N ! lname: FAN fname: XIAOMING inst: 1560 - UNIVERSITY OF CALIFORNIA, SAN DIEGO country: USA esa: N ! lname: COTTRELL fname: LANCE inst: 1560 - UNIVERSITY OF CALIFORNIA, SAN DIEGO country: USA esa: N ! lname: LANZETTA fname: KENNETH mi: M inst: 1560 - UNIVERSITY OF CALIFORNIA, SAN DIEGO country: USA esa: N ! lname: MCMAHON fname: RICHARD mi: G inst: UNIVERSITY OF CAMBRIDGE country: UNITED KINGDOM esa: Y ! lname: HAZARD fname: CYRIL inst: UNIVERSITY OF PITTSBURGH country: USA esa: N ! ! end of general_form_proposers block general_form_text: ! question: 3 section: 1 line_1: 1. SCIENCE GOALS: line_2: We have two main goals: line_3: 1. We will observe Q1935-6914 with FOS G130H(Blue) to get a spectrum line_4: of the rest frame wavelengths below 304A. The QSO is at emission line_5: redshift 3.152, so we are interested in observed wavelengths below line_6: (1+3.152)*304=1262A. We expect to see strong continuum absorption due line_7: to He~II in the intergalactic medium, known as Gunn-Peterson line_8: absorption. We are interested in all wavelengths below 1262. line_9: 2. We will obtain spectra of a second target, Q1334-0033, with line_10: FOS G130H, G190H and G270H. The G130H spectrum is a intended to line_11: give the continuum level and any strong lines or Lyman limits line_12: (SNR=5 at 1370A). The G190H and G270H spectra will have line_13: SNR=25 and 30/diode, sufficient for the detection of far UV absorption line_14: lines in intervening absorption systems. The goal is to check the line_15: claim by Reimers etal that intervening Lyman limit systems (with line_16: optical depth below 1) have very high ionization, with enhanced O/C. line_18: 2. OBSERVATION OF Q1935-6914: line_20: We have discovered that Q1935-6914, with zem=3.152 & V about 18, line_21: has sufficient redshift and flux for the detection of HeII 304A. From line_22: our Cycle 3 FOC UV image, we find its flux at 1400A is about line_23: 1.92x10(-16) ergs/cm^2/s/A. To measure the Gunn-Peterson optical depth, ! question: 3 section: 2 line_1: we need spectra at wavelengths less than 304(1+zem)=1262A. line_2: Either G130H or G160L cover this wavelength, but we MUST use G130H line_3: because we need the 1A resolution to limit the amount of spectrum line_4: which is destroyed by geo-coronal Ly-alpha and OI~1304 emission. line_5: (The FWHM=7A resolution of G160L leaves too little continuum which line_6: is free of emission line flux.) The G130H also gives more cts/Angstrom, line_7: but this is offset by 4 times the dark per Ang. line_9: We will use the 1.0 aperture. The G130H(Blue) has line_10: efficiency at 1260A, E = 0.00325, and the throughput of 1.0" aperture line_11: is 0.91. With the above target flux, the signal at 1260A is line_12: N(obj)=1.63x10(-3) cts/s/diode. We obtain S/N = 1.74*10(-2)*sqrt(T). line_13: With T=56080 seconds exposure time we would obtain S/N=4.12, and worse line_14: farther into the UV. Since the mean dark in blue detector of line_15: 0.0077cts/s/d is 4.2 times our 1260A signal, we examined the use of line_16: REJLIM, but in a preprint Tytler and Davis show that REJLIM gives line_17: only a 10% - 22% gain, which we consider is not worth the risk of line_18: getting no data (if a noisy diode is not switched off) and line_19: complications to the schedule etc. ! question: 3 section: 3 line_1: 2.3 ACQUISITIONS for Q1935-6914: line_2: We need to be carefull of the acquisition of this object, because line_3: the exposure time is so long. Although we do have an accurate FOC UV line_4: flux (one epoch - 1993 only), we are also unsure of the magnitude in line_5: the optical (poor quality measurements of around V=17.3 and 18.8) line_6: so we use ACQ/PEAK, not BINARY. line_8: We use the fainter magnitude of 18.8 for ACQ/PEAK exposure times. line_10: 2.4 ACQUISITIONS for all spectra line_12: We acquire into the 4.3, then 1.0 then 0.5 exactly copying the example line_13: on p.64 of the FOS Instrument Manual, version 4.0. Then we add a line_14: acq into the slit, to improve the centering of the object in the line_15: wavelength direction. This acq has steps of 0.057 arcsec, and should line_16: center to 0.03 arcsec, which is 0.4 pixels. Then we observe with the line_17: 1.0 aperture. We considered using the 0.5, but there are no advantages. line_18: The sky is negligible, the wavlength zero point depends on the line_19: acquisition and not on the slit, and the resolution does not depend line_20: on the slit. ! question: 3 section: 4 line_1: line_2: 2.2 USE OF RAPID for all spectra line_4: We request RAPID mode because we want to receive a spectrum every 40 line_5: sec (1345 in all for Q1935-6914). The SNR is set by the dark, line_6: which varies by a factor of two around the orbit, so we will weight line_7: each spectrum by SNR, which varies with wavelength, line_8: before we sum the spectra. This is not essential, but it will line_9: boost the final SNR, so it should be done if there will be no line_10: impact on scheduling or other problems. ! question: 3 section: 5 line_1: line_3: -------------------------------------------------------------------- line_6: 3. OBSERVATION OF Q1334-0033 line_8: Our FOC image showed that Q1334-0033, zem=2.782 \& V=17.4, has flux at line_9: 1400A of about 4.0x10(-16) ergs/cm^2/s/A. The expected line_10: HeII 304A emission line is at about 1150A, which HST can not reach, line_11: so it is not suitable for measuring GP absorption tau(304). line_12: Instead we will observe it to detect far-UV narrow absorption lines. line_13: We assume an approximately flat spectrum across the wavelengths of line_14: interest. We will get spectra with G130H(blue), G190H(red) and line_15: G270H(red) to cover all HST UV wavelength region. line_17: We should obtain SNR=5, 25, 30/diode at wavelengths line_18: 1370, 1900, and 2700A respectively. In following we assume an line_19: approximately flat spectrum across the wavelengths of interests, and line_20: we give estimates of exposure time (in hours) to get these SNR. ! question: 3 section: 6 line_1: Grating Dark Wave E(L) T(L) N(L) N(sky) S/N Time(h) line_2: ------------------------------------------------------------------------ line_3: G130H/Blue 0.008 1370 0.005 0.910 0.00568 4.84(-8) 5 2.73 line_5: G190H/Red 0.01 1900 0.026 0.92 0.0530 0.00223 25 4.03 line_7: G270H/Red 0.01 2700 0.064 0.93 0.273 0.093 30 1.26 line_8: (we request slightly different exposure times on the logsheet.) line_9: Above for 1.0 arcsec aperture. ! question: 3 section: 7 line_1: 3.1 ACQUISITION of Q1334-0033 line_2: We know the FOC UV flux form this object, but we are uncertain line_3: of the visible flux, so we use ACQ/PEAK instead of binary. line_4: The acquisition steps are identical to those for the first object. line_5: First we acq into the red side and take one G270H and one G190H line_6: spectrum. Then we change to the blue camera for the G130H. ! question: 3 section: 8 line_1: line_2: 3.2 ITEMS TO CHECK?? for Q1334-0033 line_4: We request a whole new acquisition after 102.5 after swap from RED to line_5: BLUE, which we believe is necessary because the total spacecraft time line_6: exceeds 6 hours. Is this correct? ! question: 4 section: 1 line_1: ! question: 5 section: 1 line_1: SPECIAL REQUIREMENTS ! question: 6 section: 1 line_1: ! ! ! ! ! question: 8 section: 1 line_1: No addition requests. ! question: 9 section: 1 line_1: 9. Have you (or your collaborators) received any previous HST observing line_2: time or archival data? If so: line_4: a. List HST program numbers and titles, and present authors involved line_5: in each line_7: 2593 White dwarf stars: PI Shipman (include Tytler) line_8: 3801 and continuations 4107, 4969. QSO Suitable for the Observation of line_9: HeII 304: PI Tytler (includes Lanzetta, Turnshek). line_10: 4324 Damped Lyman Alpha Systems in IUE Spectra: PI Lanzetta (includes line_11: Wolfe, Turnshek). line_12: 4396 and continuations 4952, 4953. QSO Absorption System Snap Shot line_13: Survey: PI Tytler (includes Bowen, Fan, Lanzetta) line_15: b. Specify which of the above programs are related to this proposal and line_16: summarize the scientific relationship, completion status, and main line_17: results from each. line_19: Programs 3801, 4107 & 4969 have yielded about 80 images of QSO fields, line_20: in which we discovered two QSO targets suitable for further observation line_21: in this proposal. line_23: No data have been obtained from program 4324. ! question: 9 section: 2 line_1: c. List publications resulting from the above data (Format: Title, line_2: Authors,Journal, Volume, Page, and Year.) line_4: Optical HST GASP Positions and Finding Charts for Bright Quasars from line_5: the HST FOS 'QSO Absorption System Snap Shot Survey', Bowen, Osmer, line_6: Tytler, Cottrell, Fan, Lanzetta, submitted to AJ, 1993. ! question: 10 section: 1 line_1: 10. Resources to be supplied by your institution(s) in support of this line_2: project (e.g. data-analysis capabilities, research assistance, line_3: students, funds). line_5: UCSD has one of the largest groups in the world working on QSOs and line_6: especially absorption lines: 5 faculty, 2 research scientists, 2 line_7: postdocs, 7 graduate students and 3 undergraduates. We are also the line_8: home institution for the FOS. The PI (faculty), CO-I (postdoc) and line_9: one graduate student will be involved with this proposal. We have 1 line_10: Sun sparcstation-1, and 1 sun-360 and one Sun IPX which could be used line_11: for this proposal. We also have 3 Sun SLC work stations which lack line_12: imaging capability. We have a large amount of relevant software. We line_13: have regular access to Lick, and hopefully the Keck observatory, where line_14: we will obtain observations of the QSO targets. We receive partial line_15: funding (air ticket only) from the university for observing trips at line_16: Lick. Money is available to support special (minority) undergraduates. line_18: McMahon has access to the AAT which will be used to obtain optical line_19: spectra of the southern target. ! !end of general form text general_form_address: lname: Tytler fname: David mi: R category: PI inst: 1560 - University of California, San Diego addr_1: CASS, 0111 addr_2: UNIVERSITY OF CALIFORNIA AT SAN DIEGO city: La Jolla state: CA zip: 92093 country: USA phone: (619) 534-7670 ! ! end of general_form_address records fixed_targets: targnum: 101 name_1: QSO-194025-690756 name_2: QSO-1935-6914 name_3: QSO1935-692 descr_1: E,313,314, descr_2: H,515,519 pos_1: PLATE-ID=01CB, pos_2: RA = 19H 40M 25.56S +/- 0.1S, pos_3: DEC = -69D 07' 56.5" +/- 1.0" equinox: J2000 pos_epoch_bj: J pos_epoch_yr: 2000.00 rv_or_z: ZEM= 3.152 comment_1: Q1935-6914, G130H, SNR= 4.1 1260A, comment_3: OBSERVATION OF HEII GUNN-PETERSON, comment_4: OUR MOST IMPORTANT OBSERVATION --- comment_5: PLEASE SCHEDULE EARLY IN CYCLE 4 -- fluxnum_1: 1 fluxval_1: V = 18.8 +/- 0.5 fluxnum_2: 2 fluxval_2: F(1400)=1.92+/- 0.57 E-16 ! targnum: 102 name_1: QSO-133647-004858 name_2: QSO-1334-0033 name_3: QSO1334-005-UM590 descr_1: E,313, descr_2: H,515,519 pos_1: PLATE-ID=02OA, pos_2: RA = 13H 36M 47.13S +/- 0.1S, pos_3: DEC = -00D 48' 57.78" +/- 1.0" equinox: J2000 pos_epoch_bj: J pos_epoch_yr: 2000.00 rv_or_z: ZEM= 2.783 comment_1: GO REF. Q1334-0033 comment_2: FOR FAR-UV ABSORPTION LINES fluxnum_1: 1 fluxval_1: V = 17.4 +/- 0.5 fluxnum_2: 2 fluxval_2: F(1400)=4.0 +/- 0.3 E-16 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 101.100 targname: QSO-194025-690756 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 40S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-Y=1.204, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, req_1: CYCLE 4; req_2: GROUP 101.1-101.65 WITHIN 30D; req_3: ONBOARD ACQ FOR 101.2; comment_1: ACQ/PEAK COPIED FROM FOS comment_2: HANDBK.V4.0,P.67, LINE 13.0-13.2, comment_3: OBSERVATION OF HEII GUNN-PETERSON, comment_4: OUR MOST IMPORTANT OBSERVATION comment_5: PLEASE SCHEDULE EARLY IN CYCLE 4 ! linenum: 101.200 targname: QSO-194025-690756 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 40S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-X=0.602, param_2: SCAN-STEP-Y=0.602, param_3: SEARCH-SIZE-X=6, param_4: SEARCH-SIZE-Y=2, req_1: CYCLE 4; req_2: ONBOARD ACQUISITION FOR 101.3; ! linenum: 101.300 targname: QSO-194025-690756 config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 60S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE-X=3, param_2: SEARCH-SIZE-Y=3, param_3: SCAN-STEP-X=0.3, param_4: SCAN-STEP-Y=0.3, req_1: CYCLE 4; req_2: ONBOARD ACQUISITION FOR 101.4; ! linenum: 101.400 targname: QSO-194025-690756 config: FOS/BL opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 130S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE-X=9, param_2: SEARCH-SIZE-Y=1, param_3: SCAN-STEP-X=0.057, req_1: CYCLE 4; req_2: ONBOARD ACQUISITION FOR 101.5; comment_1: TO IMPROVE WAVELENGTH ACCURACY ! linenum: 101.500 targname: QSO-194025-690756 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H num_exp: 1 time_per_exp: 26880S priority: 1 param_1: READ-TIME=40 req_1: CYCLE 4; comment_1: GR=G130H, TO GET S/N=4.12 AT 1260A. comment_2: OBSERVATION OF HEII GUNN-PETERSON comment_3: OUR MOST IMPORTANT OBSERVATION - comment_4: PLEASE SCHEDULE EARLY IN CYCLE 4 ! linenum: 101.610 targname: QSO-194025-690756 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 40S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-Y=1.204, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 101.62 comment_1: OBSERVATION OF HEII GUNN-PETERSON, comment_2: OUR MOST IMPORTANT OBSERVATION comment_3: PLEASE SCHEDULE EARLY IN CYCLE 4 ! linenum: 101.620 targname: QSO-194025-690756 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 40S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-X=0.602, param_2: SCAN-STEP-Y=0.602, param_3: SEARCH-SIZE-X=6, param_4: SEARCH-SIZE-Y=2, req_1: CYCLE 4; req_2: ONBOARD ACQUISITION FOR 101.63 ! linenum: 101.630 targname: QSO-194025-690756 config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 60S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE-X=3, param_2: SEARCH-SIZE-Y=3, param_3: SCAN-STEP-X=0.3, param_4: SCAN-STEP-Y=0.3, req_1: CYCLE 4; req_2: ONBOARD ACQUISITION FOR 101.64 ! linenum: 101.640 targname: QSO-194025-690756 config: FOS/BL opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 130S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE-X=9, param_2: SEARCH-SIZE-Y=1, param_3: SCAN-STEP-X=0.057, req_1: CYCLE 4; req_2: ONBOARD ACQUISITION FOR 101.65 comment_1: TO IMPROVE WAVELENGTH ACCURACY ! linenum: 101.650 targname: QSO-194025-690756 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H num_exp: 1 time_per_exp: 26880S priority: 1 param_1: READ-TIME=40 req_1: CYCLE 4; comment_1: GR=G130H, TO GET S/N=4.12 AT 1260A. comment_2: OBSERVATION OF HEII GUNN-PETERSON comment_3: OUR MOST IMPORTANT OBSERVATION - comment_4: PLEASE SCHEDULE EARLY IN CYCLE 4 ! linenum: 102.100 targname: QSO-133647-004858 config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 2 param_1: SCAN-STEP-Y=1.204, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, req_1: CYCLE 4; req_2: GROUP 102.1-102.6 NO GAP; req_3: ONBOARD ACQUISITION FOR 102.2; ! linenum: 102.200 targname: QSO-133647-004858 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 2 param_1: SCAN-STEP-X=0.602, param_2: SCAN-STEP-Y=0.602, param_3: SEARCH-SIZE-X=6, param_4: SEARCH-SIZE-Y=2, req_1: CYCLE 4; req_2: ONBOARD ACQUISITION FOR 102.3; ! linenum: 102.300 targname: QSO-133647-004858 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 18S priority: 2 param_1: SEARCH-SIZE-X=5 param_2: SEARCH-SIZE-Y=5 param_3: SCAN-STEP-X=.172 param_4: SCAN-STEP-Y=.172 req_1: CYCLE 4; req_2: ONBOARD ACQUISITION FOR 102.4; ! linenum: 102.400 targname: QSO-133647-004858 config: FOS/RD opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 30S priority: 2 param_1: SEARCH-SIZE-X=9 param_2: SEARCH-SIZE-Y=1 param_3: SCAN-STEP-X=.057 param_4: SCAN-STEP-Y=.057 req_1: CYCLE 4; req_2: ONBOARD ACQUISITION FOR 102.5; comment_1: TO IMPROVE WAVELENGTH ACCURACY ! linenum: 102.500 targname: QSO-133647-004858 config: FOS/RD opmode: RAPID aperture: 1.0 sp_element: G270H num_exp: 1 time_per_exp: 4240S priority: 2 param_1: READ-TIME=40 req_1: CYCLE 4; comment_1: GR=G270H, SNR=30/DIODE AT 2700A ! linenum: 102.550 targname: WAVE config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H num_exp: 1 time_per_exp: DEF priority: 2 req_1: CYCLE 4; REQ_2: SEQ 102.5-102.55 NO GAP; ! linenum: 102.560 targname: WAVE config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: DEF priority: 2 req_1: CYCLE 4; REQ_2: SEQ 102.56-102.6 NO GAP; ! linenum: 102.600 targname: QSO-133647-004858 config: FOS/RD opmode: RAPID aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 15200S fluxnum_1: 1 priority: 2 param_1: READ-TIME=40 req_1: CYCLE 4; comment_1: GR=G190H, SNR=25 / DIODE AT 1900A ! linenum: 103.100 targname: QSO-133647-004858 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 20S fluxnum_1: 1 priority: 3 param_1: SCAN-STEP-Y=1.204, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, req_1: CYCLE 4; req_2: GROUP 103.1-103.5 NO GAP; req_3: ONBOARD ACQUISITION FOR 103.2; ! linenum: 103.200 targname: QSO-133647-004858 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 20S fluxnum_1: 1 priority: 3 param_1: SCAN-STEP-X=0.602, param_2: SCAN-STEP-Y=0.602, param_3: SEARCH-SIZE-X=6, param_4: SEARCH-SIZE-Y=2, req_1: CYCLE 4; req_2: ONBOARD ACQUISITION FOR 103.3; ! linenum: 103.300 targname: QSO-133647-004858 config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 30S priority: 3 param_1: SEARCH-SIZE-X=3 param_2: SEARCH-SIZE-Y=3 param_3: SCAN-STEP-X=.3 param_4: SCAN-STEP-Y=.3 req_1: CYCLE 4; req_2: ONBOARD ACQUISITION FOR 103.4; ! linenum: 103.400 targname: QSO-133647-004858 config: FOS/BL opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 50S fluxnum_1: 1 priority: 3 param_1: SEARCH-SIZE-X=9 param_2: SEARCH-SIZE-Y=1 param_3: SCAN-STEP-X=.057 param_4: SCAN-STEP-Y=.057 req_1: CYCLE 4; req_2: ONBOARD ACQUISITION FOR 103.5; comment_1: TO IMPROVE WAVELENGTH ACCURACY ! linenum: 103.500 targname: QSO-133647-004858 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H num_exp: 1 time_per_exp: 9920S priority: 3 param_1: READ-TIME=40 req_1: CYCLE 4; comment_1: GR=G130H, SNR=5/DIODE AT 1370A. ! linenum: 203.100 targname: QSO-133647-004858 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 20S fluxnum_1: 1 priority: 3 param_1: SCAN-STEP-Y=1.204, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, req_1: CYCLE 4; req_2: GROUP 203.1-203.5 NO GAP; req_3: ONBOARD ACQUISITION FOR 203.2; linenum: 203.200 targname: QSO-133647-004858 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 20S fluxnum_1: 1 priority: 3 param_1: SCAN-STEP-X=0.602, param_2: SCAN-STEP-Y=0.602, param_3: SEARCH-SIZE-X=6, param_4: SEARCH-SIZE-Y=2, req_1: CYCLE 4; req_2: ONBOARD ACQUISITION FOR 203.3; ! linenum: 203.300 targname: QSO-133647-004858 config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 30S priority: 3 param_1: SEARCH-SIZE-X=3 param_2: SEARCH-SIZE-Y=3 param_3: SCAN-STEP-X=.3 param_4: SCAN-STEP-Y=.3 req_1: CYCLE 4; req_2: ONBOARD ACQUISITION FOR 203.4; ! linenum: 203.400 targname: QSO-133647-004858 config: FOS/BL opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 50S fluxnum_1: 1 priority: 3 param_1: SEARCH-SIZE-X=9 param_2: SEARCH-SIZE-Y=1 param_3: SCAN-STEP-X=.057 param_4: SCAN-STEP-Y=.057 req_1: CYCLE 4; req_2: ONBOARD ACQUISITION FOR 203.5; comment_1: TO IMPROVE WAVELENGTH ACCURACY ! linenum: 203.500 targname: QSO-133647-004858 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H num_exp: 1 time_per_exp: 9920S priority: 3 param_1: READ-TIME=40 req_1: CYCLE 4; comment_1: GR=G130H, SNR=5/DIODE AT 1370A. ! ! end of exposure logsheet ! No scan data records found