! File: 4276C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:19:59:16 coverpage: title_1: THE ABUNDANCE AND EVOLUTION OF CARBON IN THE SPIRAL GALAXY NGC 2403: title_2: CYCLE3 MEDIUM sci_cat: GALAXIES & CLUSTERS sci_subcat: GAS & DUST proposal_for: GO pi_fname: DONALD pi_mi: R. pi_lname: GARNETT pi_inst: UNIVERSITY OF MINNESOTA pi_country: USA hours_pri: 10.55 num_pri: 6 fos: Y funds_length: 12 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: ADMISTRATIVE SERVICES CENTER off_addr_3: 1919 UNIVERSITY AVENUE off_city: ST. PAUL off_state: MN off_zip: 55104 off_country: USA off_phone: (612) 624-5826 ! end of coverpage abstract: line_1: We propose to observe UV emission lines of carbon from H II regions in line_2: the spiral galaxy NGC 2403. These measurements, combined with line_3: corresponding optical spectra, will be used to derive carbon abundances line_4: and C/O ratios across the disk of NGC 2403. Our measurements will line_5: provide the first good sample of data on carbon abundances across a line_6: spiral galaxy. We will use the derived abundances to study the time line_7: evolution of C/O across the galaxy and compare the results with those line_8: obtained from observations of stars in our own Galaxy as well as line_9: theoretical predictions for the behavior of C/O in spirals. In line_10: particular, we will make detailed comparisons between the behavior of line_11: C, N, He, and O in the outer parts of NGC 2403 with that observed in line_12: irregular galaxies of similar abundances; such comparison will tell us line_13: if the evolution of the outer disks of spirals has proceeded in line_14: similar fashion as for the irregulars. In addition, we will compare line_15: the gradients for C and N across the disk to obtain an improved line_16: estimate of the fraction of N produced by primary nucleosynthesis. ! ! end of abstract general_form_proposers: lname: GARNETT fname: DONALD title: PI mi: R. inst: UNIVERSITY OF MINNESOTA country: USA ! lname: DUFOUR fname: REGINALD mi: J. inst: RICE UNIVERSITY country: USA ! lname: PEIMBERT fname: MANUEL inst: INSTITUTO DE ASTRONOMIA country: MEXICO ! lname: SHIELDS fname: GREGORY mi: A. inst: UNIVERSITY OF TEXAS country: USA ! lname: SKILLMAN fname: EVAN mi: D. inst: UNIVERSITY OF MINNESOTA country: USA ! lname: TERLEVICH fname: ELENA inst: ROYAL GREENWICH OBSERVATORY country: UNITED KINGDOM esa: Y ! lname: TERLEVICH fname: ROBERTO mi: J. inst: ROYAL GREENWICH OBSERVATORY country: UNITED KINGDOM esa: Y ! lname: TORRES-PEIMBERT fname: SILVIA inst: INSTITUTO DE ASTRONOMIA country: MEXICO ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: ! question: 3 section: 1 line_1: We will be using the FOS with the red detector, grating G190H, and the 1" line_2: circular aperture to observe the C III] feature at 1908 A at approximately line_3: 4 A spectral resolution. In general, we wish to obtain a S/N ratio of 10 or line_4: better in the C III] feature in order to derive C abundances with the required line_5: precision. However, nebular electron temperatures fall steeply with increasing line_6: oxygen abundance, and consequently, so do the UV emission line strengths. Thus, line_7: for the more metal-rich H II regions prohibitively long exposures are needed line_8: to obtain the desired S/N. As a compromise we have settled on exposure times line_9: long enough to reach a S/N in excess of 5 for the C III] line, except for VS line_10: 44 and VS 9, where we predict we can reach S/N of 10 in short integrations. line_11: Since we will be determining the C/H abundance ratio by relating the flux line_12: of C III] to that of H-beta, we need to ensure that we have the proper line_13: photometric scaling of the UV spectrum to the optical spectrum (there are no line_14: emission lines in the UV we can use to determine such scaling). Therefore, line_15: we will obtain short exposures at the same position for each object using line_16: the same detector and aperture, but with grating G570H. This setup includes line_17: H-beta, H-alpha, and [O III] 5007 A at approximately 10 A resolution. These line_18: spectra will provide the correct photometric scaling of the UV C III] lines line_19: relative to H-beta and [O III] in the optical. We will also use these spectra line_20: to determine the amount of interstellar extinction. With exposures of order line_21: only 5 minutes, we estimate that we can obtain S/N > 50 for H-beta, H-alpha, line_22: and [O III] 5007, based on the fluxes listed in the exposure logs. ! question: 4 section: 1 line_1: We require HST observations for this project because carbon abundances for H II line_2: regions cannot be reliably measured from the ground. The dominant ionization line_3: stage of C in H II regions is C++, for which the only strong emission lines are line_4: the collisionally-excited C III] 1907-9A lines. These lines have been detected line_5: in a few H II regions with IUE, with large uncertainties in many cases because line_6: of IUE's low sensitivity. The high dynamic range of the FOS detector allows an line_7: improvement of 10-100 over that possible with the IUE. Coupled with the 35-fold line_8: increase in light gathering power, we will be able to measure C line strengths line_9: in H II regions previously unattainable. We have reached the limits of what can line_10: be done with IUE on extragalactic H II regions; nevertheless, the knowledge line_11: gained from these observations provide firm groundwork for this proposal. line_12: We already have high quality ground-based optical spectra for each of our line_13: targets. These spectra will provide precise measurements of critical diagnostic line_14: emission-line ratios which will allow us to determine accurately the physical line_15: conditions in the H II regions, and thus the C and O abundances as well. line_16: We also have a scheduled Cycle 2 FOS program to study C and O abundances in line_17: metal-poor blue compact dwarf galaxies. The program is complementary to the line_18: one proposed here, with the overlapping goal of determining the variation of line_19: C abundances over the widest possible range of metallicity. line_20: Our sample of 6 targets was chosen to provide an adequate sampling of the line_21: largest possible range of O/H and radius in NGC 2403, to assure that the line_22: determination of any abundance gradient is not dominated by a measurement line_23: for any single H II region. ! question: 5 section: 1 line_1: No special scheduling requirements. ! question: 6 section: 1 line_1: No special calibration requirements. ! question: 7 section: 1 line_1: OUR FOS SPECTRA REQUIRE NO SPECIAL DATA REDUCTION PROCEDURES, BECAUSE SPECTRO- line_2: SCOPY OF EXTENDED OBJECTS WITH THE FOS ARE MINIMALLY AFFECTED BY SPHERICAL line_3: ABERRATION IN THE HST PRIMARY MIRROR. The spectra will be extracted and line_4: calibrated using STSDAS software at Rice University and the University of line_5: Minnesota. We will measure line fluxes for the C III], [O III], H-beta, line_6: H-alpha, and Si III] emission lines (as well as any weaker lines that may line_7: appear in our spectra), and the shape of the stellar continuum. line_8: The scientific analysis will generally follow procedures established in the line_9: studies of NGC 2363 (Peimbert, Pena, & Torres-Peimbert 1986) and I Zw 18 line_10: (Dufour, Garnett, & Shields 1988). We have limited the targets to those for line_11: which we have excellent ground based optical spectra The ground-based optical line_12: data enable us to determine accurately physical conditions (electron temperature line_13: and density) from diagnostic emission line ratios in the H II regions. We will line_14: compute abundances for C++ and O++ within each H II region will be calculated line_15: directly from the emission lines observed in the FOS spectra, guided by photo- line_16: ionization models (based on the code developed by Shields) to account for line_17: ionization effects. Both Skillman and Garnett also have extensive experience line_18: in using this code to study H II regions. If the UV spectra have sufficient S/N line_19: in the continuum, we may pursue a more sophisticated analysis of the stellar line_20: population content and the IMF via comparison with UV spectra for hot stars in line_21: the IUE spectral atlas. In particular, our spectra will include the He II 1640 line_22: A and N IV 1720 A features. These lines are weak or absent in normal O stars, line_23: but display prominent P Cygni profiles in the presence of dense stellar winds, ! question: 7 section: 2 line_1: and therefore are sensitive indicators of the presence of highly evolved line_2: massive stars such as supergiants and Wolf-Rayet stars. ! question: 8 section: 1 line_1: We wish to emphasize that OUR PROPOSED OBSERVATIONS ARE ESSENTIALLY UNAFFECTED line_2: BY THE SPHERICAL ABERRATION PRESENT IN THE PRIMARY MIRROR. Most of our targets line_3: fill the 1" apertures we plan to use, and have spatial profiles which fall off line_4: much less rapidly than point sources. Therefore, we expect our integration line_5: times and concomitant S/N ratios will be identical to those for a healthy HST. line_6: Related HST proposals: line_7: Garnett is on a Cycle 2 program with Heckman et al. (#3840) for FOS UV spectro- line_8: scopy of starburst galaxies. The primary scientific goal of this program is to line_9: study the massive star populations of starbursts through the UV stellar absorp- line_10: tion lines. However, nebular emission lines may be visible as well in the spec- line_11: tra, and can be used to study carbon abundances in luminous starburst galaxies. line_13: Five of the investigators on this proposal are also on a cycle 3 proposal line_14: (#4382) to study two compact H II regions in the SMC, one of which is very line_15: dusty, the other non-dusty. We will use FOS UV spectroscopy of these two line_16: nebulae to study the scattering and absorption characteristics of SMC dust line_17: and compare the properties of the dust with Galactic dust. We will also be line_18: able to derive carbon abundances from the UV spectra, the results of which line_19: will be available for analysis in the program proposed here. ! question: 9 section: 1 line_1: Program GO 2416 "Imagery and Spectroscopy of Super Metal Poor Galaxies" (PI: line_2: Dufour; CoIs common to this proposal: Shields, Skillman). The goal of this line_3: program is to obtain UV-visible-near-IR imagery of the dwarf irregular galaxy line_4: GR8. WFC images of GR8 were successfully obtained in 1991 July. The wide band line_5: images in B,V,R, and I have been calibrated (several times) and were presented line_6: at the January 1992 AAS meeting. FOS spectra of an H II region are scheduled line_7: for February 1993. line_8: Program GO 3840 "The Abundances and Time Evolution of C, N, & O in Star Forming line_9: Galaxies" (PI: Skillman; CoIs common to this proposal: all). The goal of this line_10: program is FOS spectra of HII regions in dwarf irregular galaxies. The relation- line_11: ship of this program to the current proposal has been discussed extensively line_12: throughout the proposal. Spectra for three of our seven targets have been line_13: obtained. line_14: Program GO 3589 "Parallel High Resolution Imaging of Diffuse Objects in the line_15: Magellanic Clouds (PI: J. Walsh; CoI in common: Garnett). Parallel imaging line_16: with WF/PC of a wide variety of ionized nebulae in the Magellanic Clouds. Not line_17: related to proposed program. No data obtained yet. line_18: Program GO 3591 "Massive Stars in Starburst Galaxies" (PI: T. Heckman; CoI in line_19: common: Garnett). FOC imaging and FOS UV spectroscopy of starburst galaxies to line_20: study the UV morphology and massive star population of starbursts. Nebular UV line_21: emission lines may be detectable in the FOS spectra as well, and could be used line_22: to determine carbon abundances. First FOC images scheduled for February 1993. ! question: 10 section: 1 line_1: Data Analysis Capabilities: line_2: The bulk of the data reduction will take place at the University of Minnesota line_3: and Rice University. Skillman has a SUN SPARCstation 1 which is dedicated to line_4: astronomical data reduction, while Garnett has a Sparcstation 2 IPX; both line_5: systems have IRAF and STSDAS installed and running routinely. Rice University line_6: has contributed to an astronomy department SPARC-station 2GX based image analy- line_7: sis facility which is currently running both IRAF and STSDAS. The Royal Green- line_8: wich Observatory provides a complete VAX and SUN based data reduction facility. line_9: Elena Terlevich has experience with STSDAS at the RGO. line_11: Research Assistance/Students: line_12: We expect to involve graduate students as research assistants in this line_13: project at both Rice University and the University of Minnesota. line_15: Funds: line_17: All five institutes represented in this proposal currently provide salary line_18: support for the investigators, with a significant fraction of their time line_19: devoted to research. Garnett has a Hubble Fellowship at the University of line_20: Minnesota from September 1992. ! !end of general form text general_form_address: lname: GARNETT fname: DONALD mi: R. category: PI inst: University of Minnesota addr_1: ASTRONOMY DEPARTMENT addr_2: 116 CHURCH ST. S.E. city: MINNEAPOLIS state: MN zip: 55455 country: USA phone: (612) 624-1084 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC2403-VS9 descr_1: H,503 pos_1: PLATE-ID=00MC, pos_2: RA-OFF = +12.05S +/- 0.05S, pos_3: DEC-OFF = +17.4" +/- 0.3", pos_4: FROM 2 equinox: J2000 pm_or_par: NO rv_or_z: V = +130 fluxnum_1: 1 fluxval_1: F-LINE(1909) = 3.0 E-16 fluxnum_2: 2 fluxval_2: F-CONT(1909) = 1.3 E-16 fluxnum_3: 3 fluxval_3: W-LINE(1909) = 4.0 fluxnum_4: 4 fluxval_4: F-LINE(4861) = 1.8 E-15 fluxnum_5: 5 fluxval_5: F-CONT(4861) = 6.0 E-18 fluxnum_6: 6 fluxval_6: W-LINE(4861) = 10 ! targnum: 2 name_1: NGC2403-VS9-OFFSET name_2: GSC4120-708 descr_1: A pos_1: PLATE-ID=00MC, pos_2: RA = 7H 36M 16.58S +/- 0.19S, pos_3: DEC = +65D 33' 31.6" +/- 1.2" equinox: J2000 pm_or_par: N rv_or_z: V = 0 fluxnum_1: 1 fluxval_1: V = 13.6 +/- 0.4 ! targnum: 3 name_1: NGC2403-VS44 descr_1: H,503 pos_1: PLATE-ID=00MC, pos_2: RA-OFF = -2.09S +/- 0.05S, pos_3: DEC-OFF = -43.0" +/- 0.3", pos_4: FROM 4 equinox: J2000 pm_or_par: N rv_or_z: V = +130 fluxnum_1: 1 fluxval_1: F-LINE(1909) = 3.3 E-16 fluxnum_2: 2 fluxval_2: F-CONT(1909) = 8.3 E-16 fluxnum_3: 3 fluxval_3: W-LINE(1909) = 4.0 fluxnum_4: 4 fluxval_4: F-LINE(4861) = 6.0 E-15 fluxnum_5: 5 fluxval_5: F-CONT(4861) = 3.5 E-17 fluxnum_6: 6 fluxval_6: W-LINE(4861) = 10 ! targnum: 4 name_1: NGC2403-VS44-OFFSET name_2: GSC4120-786 descr_1: A pos_1: PLATE-ID=00MC, pos_2: RA = 7H 37M 8.78S +/- 0.19S, pos_3: DEC = +65D 37' 20.7" +/- 1.2" equinox: J2000 pm_or_par: N rv_or_z: V = 0 fluxnum_1: 1 fluxval_1: V = 14.9 +/- 0.4 ! targnum: 5 name_1: NGC2403-VS51 descr_1: H,503 pos_1: PLATE-ID=00MC, pos_2: RA-OFF = 12.64S +/- 0.05S, pos_3: DEC-OFF = -54.3" +/- 0.3", pos_4: FROM 6 equinox: J2000 pm_or_par: N rv_or_z: V = +130 fluxnum_1: 1 fluxval_1: F-LINE(1909) = 3.5 E-17 fluxnum_2: 2 fluxval_2: F-CONT(1909) = 5.5 E-17 fluxnum_3: 3 fluxval_3: W-LINE(1909) = 4.0 fluxnum_4: 4 fluxval_4: F-LINE(4861) = 9.0 E-16 fluxnum_5: 5 fluxval_5: F-CONT(4861) = 2.9 E-18 fluxnum_6: 6 fluxval_6: W-LINE(4861) = 10 ! targnum: 6 name_1: NGC2403-VS51-OFFSET name_2: GSC4120-916 descr_1: A pos_1: PLATE-ID=00MC, pos_2: RA = 7H 37M 5.57S +/- 0.04S, pos_3: DEC = +65D 34' 43.5" +/- 0.3" equinox: J2000 pm_or_par: N rv_or_z: V = 0 fluxnum_1: 1 fluxval_1: V = 13.5 +/- 0.4 ! targnum: 7 name_1: NGC2403-VS3 descr_1: H,503 pos_1: PLATE-ID=00MC, pos_2: RA-OFF = -5.40S +/- 0.05S, pos_3: DEC-OFF = -44.6" +/- 0.3", pos_4: FROM 8 equinox: J2000 pm_or_par: N rv_or_z: V = +130 fluxnum_1: 1 fluxval_1: F-LINE(1909) = 5.1 E-17 fluxnum_2: 2 fluxval_2: F-CONT(1909) = 6.4 E-16 fluxnum_3: 3 fluxval_3: W-LINE(1909) = 4.0 fluxnum_4: 4 fluxval_4: F-LINE(4861) = 2.5 E-15 fluxnum_5: 5 fluxval_5: F-CONT(4861) = 2.5 E-17 fluxnum_6: 6 fluxval_6: W-LINE(4861) = 10 ! targnum: 8 name_1: NGC2403-VS3-OFFSET name_2: GSC4124-550 descr_1: A pos_1: PLATE-ID=00MC, pos_2: RA = 7H 36M 24.99S +/- 0.03S, pos_3: DEC = +65D 37' 49.7" +/- 0.2" equinox: J2000 pm_or_par: N rv_or_z: V = 0 fluxnum_1: 1 fluxval_1: V = 13.1 +/- 0.4 ! targnum: 9 name_1: NGC2403-VS41 descr_1: H,503 pos_1: PLATE-ID=00MC, pos_2: RA-OFF = -11.00S +/- 0.05S, pos_3: DEC-OFF = +2.2" +/- 0.3", pos_4: FROM 10 equinox: J2000 pm_or_par: N rv_or_z: V = +130 fluxnum_1: 1 fluxval_1: F-LINE(1909) = 3.8 E-17 fluxnum_2: 2 fluxval_2: F-CONT(1909) = 3.1 E-16 fluxnum_3: 3 fluxval_3: W-LINE(1909) = 4.0 fluxnum_4: 4 fluxval_4: F-LINE(4861) = 2.2 E-15 fluxnum_5: 5 fluxval_5: F-CONT(4861) = 1.2 E-17 fluxnum_6: 6 fluxval_6: W-LINE(4861) = 10 ! targnum: 10 name_1: NGC2403-VS41-OFFSET name_2: GSC4120-786 descr_1: A pos_1: PLATE-ID=00MC, pos_2: RA = 7H 37M 8.78S +/- 0.19S, pos_3: DEC = +65D 37' 20.7" +/- 1.2" equinox: J2000 pm_or_par: N rv_or_z: V = 0 fluxnum_1: 1 fluxval_1: V = 14.9 +/- 0.4 ! targnum: 11 name_1: NGC2403-VS38 descr_1: H,503 pos_1: PLATE-ID=00MC, pos_2: RA-OFF = -16.78S +/- 0.05S, pos_3: DEC-OFF = -33.2" +/- 0.3", pos_4: FROM 12 equinox: J2000 pm_or_par: N rv_or_z: V = +130 fluxnum_1: 1 fluxval_1: F-LINE(1909) = 4.8 E-17 fluxnum_2: 2 fluxval_2: F-CONT(1909) = 3.8 E-16 fluxnum_3: 3 fluxval_3: W-LINE(1909) = 4.0 fluxnum_4: 4 fluxval_4: F-LINE(4861) = 3.0 E-15 fluxnum_5: 5 fluxval_5: F-CONT(4861) = 1.5 E-17 fluxnum_6: 6 fluxval_6: W-LINE(4861) = 10 ! targnum: 12 name_1: NGC2403-VS38-OFFSET name_2: GSC4120-786 descr_1: A pos_1: PLATE-ID=00MC, pos_2: RA = 7H 37M 8.78S +/- 0.19S, pos_3: DEC = +65D 37' 20.7" +/- 1.2" equinox: J2000 pm_or_par: N rv_or_z: V = 0 fluxnum_1: 1 fluxval_1: V = 14.9 +/- 0.4 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.100 targname: NGC2403-VS9-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 2.2S fluxnum_1: 1 priority: 1 req_1: CYCLE 3 / 1.1-6.4; req_2: SEQ 1.1-1.4 NO GAP; req_3: ONBOARD ACQ FOR 1.2-1.4 comment_1: EXPOSURE TIME COMPUTED ASSUMING G2V ! linenum: 1.200 targname: NGC2403-VS9 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 900S s_to_n: 5 fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 priority: 1 ! linenum: 1.300 targname: NGC2403-VS9 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G570H num_exp: 1 time_per_exp: 360S s_to_n: 50 fluxnum_1: 4 fluxnum_2: 5 fluxnum_3: 6 priority: 1 ! linenum: 1.400 targname: NGC2403-VS9 config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 60S fluxnum_1: 1 priority: 1 comment_1: VERIFICATION OF FIELD AFTER EXPOSURE ! linenum: 2.100 targname: NGC2403-VS44-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 3.5S fluxnum_1: 1 priority: 1 req_1: SEQ 2.1-2.4 NO GAP; req_2: ONBOARD ACQ FOR 2.2-2.4 comment_1: EXPOSURE TIME COMPUTED ASSUMING G2V ! linenum: 2.200 targname: NGC2403-VS44 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 1800S s_to_n: 10 fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 priority: 1 ! linenum: 2.300 targname: NGC2403-VS44 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G570H num_exp: 1 time_per_exp: 120S s_to_n: 50 fluxnum_1: 4 fluxnum_2: 5 fluxnum_3: 6 priority: 1 ! linenum: 2.400 targname: NGC2403-VS44 config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 60S fluxnum_1: 1 priority: 1 comment_1: VERIFICATION OF FIELD AFTER EXPOSURE ! linenum: 3.100 targname: NGC2403-VS51-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 2.0S fluxnum_1: 1 priority: 1 req_1: SEQ 3.1-3.4 NO GAP; req_2: ONBOARD ACQ FOR 3.2-3.4 comment_1: EXPOSURE TIME COMPUTED ASSUMING G2V ! linenum: 3.200 targname: NGC2403-VS51 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 3600S s_to_n: 5 fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 priority: 1 ! linenum: 3.300 targname: NGC2403-VS51 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G570H num_exp: 1 time_per_exp: 660S s_to_n: 50 fluxnum_1: 4 fluxnum_2: 5 fluxnum_3: 6 priority: 1 ! linenum: 3.400 targname: NGC2403-VS51 config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 60S fluxnum_1: 1 priority: 1 comment_1: VERIFICATION OF FIELD AFTER EXPOSURE ! linenum: 4.100 targname: NGC2403-VS3-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.3S fluxnum_1: 1 priority: 1 req_1: SEQ 4.1-4.4 NO GAP; req_2: ONBOARD ACQ FOR 4.2-4.4 comment_1: EXPOSURE TIME COMPUTED ASSUMING G2V ! linenum: 4.200 targname: NGC2403-VS3 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 10600S s_to_n: 5 fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 priority: 1 ! linenum: 4.300 targname: NGC2403-VS3 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G570H num_exp: 1 time_per_exp: 300S s_to_n: 5 fluxnum_1: 4 fluxnum_2: 5 fluxnum_3: 6 priority: 1 ! linenum: 4.400 targname: NGC2403-VS3 config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 60S fluxnum_1: 1 priority: 1 comment_1: VERIFICATION OF FIELD AFTER EXPOSURE ! linenum: 5.100 targname: NGC2403-VS41-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 3.5S fluxnum_1: 1 priority: 1 req_1: SEQ 5.1-5.4 NO GAP; req_2: ONBOARD ACQ FOR 5.2-5.4 comment_1: EXPOSURE TIME COMPUTED ASSUMING G2V ! linenum: 5.200 targname: NGC2403-VS41 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 10500S s_to_n: 5 fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 priority: 1 ! linenum: 5.300 targname: NGC2403-VS41 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G570H num_exp: 1 time_per_exp: 300S s_to_n: 5 fluxnum_1: 4 fluxnum_2: 5 fluxnum_3: 6 priority: 1 ! linenum: 5.400 targname: NGC2403-VS41 config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 60S fluxnum_1: 1 priority: 1 comment_1: VERIFICATION OF FIELD AFTER EXPOSURE ! linenum: 6.100 targname: NGC2403-VS38-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 3.5S fluxnum_1: 1 priority: 1 req_1: SEQ 6.1-6.4 NO GAP; req_2: ONBOARD ACQ FOR 6.2-6.4 comment_1: EXPOSURE TIME COMPUTED ASSUMING G2V ! linenum: 6.200 targname: NGC2403-VS38 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 8100S s_to_n: 5 fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 priority: 1 ! linenum: 6.300 targname: NGC2403-VS38 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G570H num_exp: 1 time_per_exp: 240S s_to_n: 50 fluxnum_1: 4 fluxnum_2: 5 fluxnum_3: 6 priority: 1 ! linenum: 6.400 targname: NGC2403-VS38 config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 60S fluxnum_1: 1 priority: 1 comment_1: VERIFICATION OF FIELD AFTER EXPOSURE ! ! end of exposure logsheet ! No scan data records found