! File: 3441C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:07:56:27 coverpage: title_1: POST ASYMPTOTIC GIANT BRANCH EVOLUTION IN THE MAGELLANIC CLOUDS. sci_cat: STELLAR ASTROPHYSICS sci_subcat: LATE EVOLUTION proposal_for: GO longterm: 2 cont_id: 2266 pi_fname: MICHAEL pi_mi: A. pi_lname: DOPITA pi_inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES pi_country: AUSTRALIA pi_phone: 61-62490212 hours_pri: 16.43 num_pri: 16 fos: Y funds_amount: 593475 funds_length: 36 off_fname: ALEX off_mi: W off_lname: RODGERS off_title: DIRECTOR off_inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES off_addr_1: PRIVATE BAG, WESTON CREEK P.O. off_addr_2: ACT, 2611 off_city: CANBERRA off_country: AUSTRALIA off_phone: 011 +61 6 249-0262 ! end of coverpage abstract: line_1: Planetary Nebulae (PN) represent a critical stage of stellar evolution which is line_2: still poorly understood. We still lack reliable observational estimates of line_3: stellar luminosity, mass, effective temperature and age, which could be used to line_4: constrain evolutionary models, and determine key data such as mass-loss rates, line_5: He shell flash phases and the role of dredge-up. This proposal represents the line_6: first stage in a systematic and definitive study using HST observations, which line_7: will require approximately a further 150 hours for completion, of a large sample line_8: of nebulae at known distance in the Magellanic Clouds. The following line_9: observations allow us to derive all parameters needed for proper confrontation line_10: between theory and observation: \* Direct PC imaging to detect central stars and line_11: to derive the physical dimensions, masses, ages, and spatial structure of the line_12: nebulae. \* FOS spectrophotometry of the central stars and nebulae in the range line_13: 1150 - 2332 Angstroms. This data will be used in combination with stellar models line_14: to derive the effective temperature, bolometric luminosity, and mass of each of line_15: the exciting stars. The combination of these parameters with the dynamical age line_16: of the PN will define the evolutionary tracks in the Luminosity/T-eff diagram. line_17: We will use two independent ionisation codes to interpret the FOS spectra, line_18: optical and IR spectra, and the ionisation structure derived from the PC images. line_19: This analysis will yield chemical abundances of many elements, including the line_20: astrophysically important species He, C, N, O, and Si. ! ! end of abstract general_form_proposers: lname: WOOD fname: PETER mi: R inst: MOUNT STROMLO AND SIDING SPRING OBSERVATORIES country: AUSTRALIA ! lname: MEATHERINGHAM fname: STEPHEN mi: J inst: MOUNT STROMLO AND SIDING SPRING OBSERVATORIES country: AUSTRALIA ! lname: BOHLIN fname: RALPH mi: C inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: FORD fname: HOLLAND mi: C inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: HARRINGTON fname: PATRICK mi: J inst: UNIVERSITY OF MARYLAND country: USA ! lname: STECHER fname: THEODORE mi: P inst: GODDARD SPACE FLIGHT CENTER country: USA ! lname: MARAN fname: STEPHEN mi: P inst: GODDARD SPACE FLIGHT CENTER country: USA ! lname: WEBSTER (DECEASED) fname: LOUISE mi: B inst: UNIVERSITY OF NEW SOUTH WALES country: AUSTRALIA ! lname: DOPITA fname: MICHAEL title: PI mi: A. inst: MOUNT STROMLO AND SIDING SPRING OBSERVATORIES country: AUSTRALIA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Imaging Program: The Magellanic Cloud PN range in size from 0.05 - 4.0 line_2: arcseconds, with a typical size of about 0.6 arcseconds (Jacoby 1980; line_3: Wood, Bessell and Dopita 1986; Wood et. al. 1987). Consequently, line_4: they are ideally suited for imaging with the PC camera. Our Cycle 1 line_5: [O III] 5007 Angstrom (F502N) images are designed to give a typical line_6: signal to noise of 20 per pixel to provide data on angular diameters line_7: and nebular morphology (spherical,bipolar, multiple shell, etc.), line_8: which in conjunction with our ground-based [O III] expansion velocity line_9: measurements will provide a dynamical age model. line_10: Cycle 2 UV Spectrophotometry: We are undertaking in Cycle 2 line_11: FOS spectrophotometry in the range 1150 - 3200 Angstroms using the line_12: G130H, G190H and G270H gratings. We aim to achieve an average signal line_13: to noise in the nebular continuum of 3 per pixel. Since it proves to line_14: very inefficient to do separate AQU/PEAK for both the blue and red line_15: sides of the spectrograph, we have elected to observe on the blue side line_16: only, accepting the lower efficiency in order to have data in the line_17: G130H bandpass. line_18: Since the Magellanic Clouds are close enough that even the faintest line_19: PN can be detected, the flux and spectral distribution of line_20: the PN nuclei can be measured over their entire ~5 mag in luminosity. line_21: Our aim is to accomplish this objective, and to achieve a good ! question: 3 section: 2 line_1: detection of the central star against the nebular continuum, even when line_2: the stellar flux is only 10% of this nebular continuum. This line_3: objective will also ensure that uniform, high quality, high dynamic line_4: range nebular spectra are obtained for the full range of nebular line_5: conditions. For the purposes of computing exposure times for spectra, line_6: a mean extinction E(B-V) of 0.15 and an LMC or SMC-like extinction law line_7: have been assumed. The counts/diode/second C-d, is given in terms of line_8: the flux at 1650 Angstroms (F_1650):log(C_d) =- f(Phi) C + log(F_1650), line_9: where C has the values 13.53 (G130H, blue digicon) and 13.56 (G190H, line_10: blue digicon) and 14.10 (G270H,again the blue digicon). line_11: The function f(Phi) is a function of the diameter of the PN, line_12: accounting for spherical abberation and is calculated from a line_13: modelling of the PSF and the PN. line_14: These data will be combined with our ground-based data line_15: of comparable quality covering the wavelength range 3200 - 10000 line_16: Angstroms. In the decade of frequency covered by these observations, line_17: we will see emission lines of the astrophysically important elements line_18: such as He, C, N, O, Si and S in the full range of ionisation stages line_19: expected to be present in the nebula. For this reason, and also ! question: 3 section: 3 line_1: because the allowable nebular models are strongly constrained by the line_2: imaging results, we expect that the chemical abundances we will derive line_3: will be much more accurate than any previously obtained. line_4: References: line_5: Jacoby, G., 1980, Ap. J. Suppl. Ser.,42, p. 1 line_6: Wood, P.R., Bessell, M.S., and Dopita, M.A., 1986, Ap. J.,311, p. 632 line_7: Wood, P.R., Meatheringham, S.J., Dopita, M.A., and Morgan, D.H., line_8: Ap. J., 320, p. 178 line_10: Following initial PIT review, this cycle 2 proposal (GO3441) was line_11: modified to update acquisition and science procedures (December 1992). line_12: The observations of LMC-SMP85 have been deleted from this proposal as line_13: they are being conducted under the Cycle 1 proposal GO4040. line_14: As all observations are being conducted on the blue side, obsolete line_15: definitions referring to the red side have been deleted from the line_16: exposure logsheet. Similarly, new definitions have been added to line_17: define the new acquisition methods described below. line_18: Most PEAK_UP acquistions have been converted to BINARY acquisitions as line_19: nearly all targets in this sample were observed with PC8 (GO2266) to line_20: be smaller in size than a FOS diode width (0.35 arcsec). New line_21: acquisition exposure times have been derived using the FOS Exposure line_22: Time Simulator, using ground-based optical spectra, and generic UV line_23: photoionisation models, as input. ! question: 3 section: 4 line_1: For those targets larger than a FOS diode width (LMC-SMP35, LMC-SMP87), line_2: a 5x5 PEAK-UP acquistion, with 0.5 arcsec steps using the 1 arcsec line_3: aperture, will be performed. This gives an effective field coverage of line_4: 3x3 arcsec, and will achieve 0.25*(2**0.5) = 0.35 arcsec accuracy on any line_5: PN within 1.25 arcsec of the initial pointing position. line_6: Finally, a PEAK-UP acquisition in the [OIII] 5007 Angstrom line is line_7: required for LMC_SMP20 (using the G570H grating), as it is in a line_8: relatively crowded field with neighbours of greater brightness in V. line_9: No offset star could be found for which we could determine sufficently line_10: accurate V and B-V. line_11: All target coordinates have been updated using re-measured line_12: positions from GSSS. COMMENT lines in the exposure logsheet have been line_13: updated to include relevant GSSS information for each target. line_14: An ACQ mode exposure has been added after each target acquisition to line_15: record the final pointing position. ! question: 4 section: 1 line_1: The angular diameters of the Magellanic Cloud PN line in the range line_2: 0.05 - 4.0 arcseconds, ideally suited to the HST capabilities. the line_3: dimensions or morphologies of these objects cannot, in general, be line_4: obtained from the ground. Preliminary ground-based work has been line_5: done, as far as it is possible, using direct imaging and image line_6: reconstruction (Jacoby 1980; Wood et. al. 1987) or speckle line_7: interferometry (Wood, Bessell, and Dopita 1986). However, imaging line_8: resolves only the largest, and speckle interferometry resolves only line_9: the brightest nebulae, leaving the vast majority of objects line_10: unresolved. line_11: Some of us have obtained low resolution UV spectra of a few of these line_12: objects using the IUE satellite. However, only the brightest objects line_13: are observable, many of the same objects chosen for the GTO program. line_14: The UV data is crucial for measurement of the stellar flux line_15: distribution and to obtain densities and ionic abundances for dominant line_16: ionisation stages of many elements. Only the combination of high line_17: resolution and a spectral range which extends shortward of the peak in line_18: the hydrogen two-photon nebular continuum (about 1450 Angstroms) will line_19: enable us to detect the star in the cases where the nebular continuum line_20: is strong. line_21: Our HST program is supported by a comprehensive and continuing line_22: ground-based program. We have used the 1-metre, 2.3-metre and line_23: 3.9-metre telescopes at Siding Spring to measure fluxes, sizes, ! question: 4 section: 2 line_1: expansion velocities, radial velocities and nebular spectra from 3200 line_2: to 10000 Angstroms. These observations already provide an excellent line_3: set of homogeneous and high-quality data which gives the best possible line_4: ground-based characteristics of the Magellanic Cloud population of PN. line_5: this data set will allow us to extend our population classifications line_6: from the HST subset to the entire population of PN in the Magellanic line_7: Clouds. line_8: References: line_9: Jacoby, G., 1980, Ap. J. Suppl. Ser.,42, p. 1 line_10: Wood, P.R., Bessell, M.S., and Dopita, M.A., 1986, Ap. J.,311, p. 632 line_11: Wood, P.R., Meatheringham, S.J., Dopita, M.A., and Morgan, D.H., line_12: Ap. J., 320, p. 178 ! question: 6 section: 1 line_1: As high-quality astrometric determination of the nebular centroid will line_2: be obtained on the basis of the PC images, we may seek to give an line_3: improved estimate of the position based on these data, for input to the line_4: Cycle 2 spectroscopy program. line_6: The spectroscopic observations are required to be non-interrupted line_7: because we need to be sure that the same part of the nebula is being line_8: observed in all three spectral bands. This is a requirement for the line_9: spectrophotometry to be valid. ! question: 7 section: 1 line_1: All PC images and FOS spectra will be reduced at STScI and then line_2: distributed by H.Ford and R.Bohlin to the team members. The line_3: dynamical ages of the nebulae will be derived by creating models of line_4: expanding prolate shells with varying azimuthal intensities whose line_5: projections onto the sky reproduce the [O III] line profiles (already line_6: obtained for the whole sample, Dopita et. al. 1985, 1988) and the PC line_7: image structure. The software needed for this program has already line_8: been written by H.Ford and his collaborators. line_9: We plan to combine the FOS UV spectrophotometry with ground-based and line_10: near-IR spectrophotometry to produce dereddened spectra. Theoretical line_11: models of the nebular continuum and of the central star will be used line_12: to separate the two continuum contributions and to place the star on line_13: the L-T(eff) diagram. By using the dynamical age already obtained, line_14: we will compare the evolutionary tracks implied for the PN nuclei with line_15: the theoretical evolutionary models (e.g. Wood and Faulkner 1986). line_16: This will enable us to determine the mass distribution of the PN line_17: nuclei, to determine whether PN ejection occurs at the time of the line_18: Helium shell flash, and to put strong observational restraints on the line_19: post-AGB mass-loss. line_20: Using the observed parameters of the central star, the FOS line_21: spectrophotometry and ionisation structure implied by the PC images, line_22: we will construct detailed photoionisation models using independent line_23: codes by Harrington, and by Dopita and Binette. The nebular size and ! question: 7 section: 2 line_1: structure, the shape of the stellar spectrum, and the ratio of stellar line_2: to nebular continua will enable us to obtain the mean ionisation line_3: parameter (Q), the ionisation temperature (T*), and the optical line_4: thickness of the nebula, which together define the nebular model. line_5: The FOS spectra are vital in the determination of the abundances of line_6: the dominant ionic species of N, C and Si. Likewise the ratio of the line_7: C III] doublet at 1906, 1909 Angstroms will give the electron density line_8: in the region of the PN containing the dominant ionisation stage. line_9: From the complete spectrophotometric data we will be able to derive line_10: the abundances of the elements : He, C, N, O, Ne, S, Cl, and Ar and line_11: possibly, Mg, Fe and Ni as well. We wish to stress that the PC line_12: nebular images and the wealth of FOS ultraviolet data will enable us line_13: to construct models with a level of detail which has previously been line_14: obtained in only a few Galactic PN such as NGC7662 (Harrington et. al. line_15: 1982), and IC3918 (Clegg et. al. 1987). line_16: References: line_17: Clegg, R.E.S., Harrington, J.P., Barlow, M.J., and Walsh, J.R., 1987, line_18: Ap. J. vol. 314, p. 575 line_19: Dopita, M.A., Ford, H.C., Lawrence, C.J., and Webster, B.L.,1985, line_20: Ap. J. vol. 296, p. 390 line_21: Dopita, M.A., Meatheringham, S.J., Webster, B.L., and Ford, H.C.,1988, line_22: Ap. J. vol. 327, p. 639 line_23: Harrington, J.P., Seaton, M.J., Adams, S., and Lutz, J.H., 1982, ! question: 7 section: 3 line_1: M.N.R.A.S., vol. 199, p. 517 line_2: Wood, P.R., and Faulkner, D.J., 1986, Ap. J., vol. 307, p. 659 ! question: 8 section: 1 line_1: Since the full analysis of the data will take a total of three years, line_2: we request that release of the data be delayed a full year after the line_3: completion of the observational program. line_4: Full archival use will be made of data obtained under the GTO program line_5: on Magellanic Cloud PN as this is released. line_6: Primary team responsibilities are as follows: line_7: 1. Image reduction, astrometry, analysis and distribution : Ford and line_8: Bohlin. line_9: 2. FOS data reduction and distribution : Bohlin and Meatheringham line_10: 3. Analysis and evolution of central stars : Dopita, Wood, Bohlin, line_11: Maran and Stecher line_12: 4. Nebular modelling and chemical composition : Dopita, Harrington, line_13: and Maran line_14: 5. Analysis of stellar populations and astrophysical interpretation : line_15: all team. ! question: 9 section: 1 line_1: As described above, this project was awarded time for HST imaging in line_2: Cycle 1. In Cycle 2, the objects which were imaged in [O III] will be line_3: subjected to spectroscopic investigation. ! question: 10 section: 1 line_1: The manpower, fiscal and hardware resources necessary to support the line_2: work of the P.I. and the other Australian members of this group will line_3: be supplied from within the internal budget of MSSSO as necessary. line_4: Funding will also be available to support any short overseas visits line_5: that may be necessary to coordinate activities of the various team line_6: members, as summarised in question 8. ! !end of general form text general_form_address: lname: DOPITA fname: MICHAEL mi: A category: PI inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES addr_1: PRIVATE BAG addr_2: WESTON CREEK P.O. city: WESTON zip: ACT 2611 country: AUSTRALIA phone: 61 6 2490212 telex: AA62270 ! ! end of general_form_address records fixed_targets: targnum: 101 name_1: SMC-SMP1 name_2: N1 name_3: LN2 descr_1: H,502 pos_1: RA = 00H 23M 58.80S +/- 0.02S, pos_2: DEC = -73D 38' 04.10" +/- 0.1", pos_3: PLATE-ID=0024 equinox: 2000.0 rv_or_z: V = 155 comment_1: FOR ALL TARGETS, IDENT # FROM comment_2: FOLLOWING REFS: SMP=SANDULEAK ET AL comment_3: 1978, PASP 90,621. N = HENIZE 1956, comment_4: APJS 2,315. LN = LINDSAY 1961, AJ, comment_5: 66, 169. FINAL POSITION OF PN comment_6: DETERMINED FROM GSSS: comment_7: REGION/PLATE/SCRIPT=S028/0024/03DE comment_8: TRY TO USE SAME GUIDE STARS AS comment_9: FOR W0SK0201T. fluxnum_1: 1 fluxval_1: F-CONT(1650) = 1.6 +/- 0.8 E-15 fluxnum_2: 2 fluxval_2: F-LINE(5007) = 4.0 +/- 0.1 E-13 fluxnum_3: 3 fluxval_3: SURF-LINE(5007) = 4.9 +/- 1.0 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(4861) = 2.1 +/- 0.5 E-12 fluxnum_5: 5 fluxval_5: SURF-CONT(5470) = 9.0 +/- 4.5 E-15 fluxnum_6: 6 fluxval_6: W-LINE(5007) = 1.0, SIZE = 0.32 ! targnum: 103 name_1: SMC-SMP3 name_2: N 4 name_3: LN16 descr_1: H,502 pos_1: RA = 00H 34M 21.90S +/- 0.02S, pos_2: DEC = -73D 13' 20.84" +/- 0.1", pos_3: PLATE-ID=06B1 equinox: 2000.0 rv_or_z: V = 164 comment_1: FINAL POSITION OF PN DETERMINED comment_2: FROM GSSS: comment_3: REGION/PLATE/SCRIPT=XX002/06B1/06B3 comment_4: TRY TO USE SAME GUIDE STARS AS comment_5: FOR W0SK0301T. fluxnum_1: 1 fluxval_1: F-CONT(1650) = 2.0 +/- 1.0 E-15 fluxnum_2: 2 fluxval_2: F-LINE(5007) = 7.0 +/- 0.7 E-13 fluxnum_3: 3 fluxval_3: SURF-LINE(5007) = 2.1 +/- 0.5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(4861) = 2.5 +/- 0.5 E-13 fluxnum_5: 5 fluxval_5: SURF-CONT(5470) = 8.0 +/- 4.0 E-16 fluxnum_6: 6 fluxval_6: W-LINE(5007) = 1.0, SIZE = 0.67 ! targnum: 106 name_1: SMC-SMP6 descr_1: H,502 pos_1: RA = 00H 41M 27.76S +/- 0.02S, pos_2: DEC = -73D 47' 05.93" +/- 0.10", pos_3: PLATE-ID=06B1 equinox: 2000.0 rv_or_z: V = 153 comment_1: FINAL POSITION OF PN DETERMINED comment_2: FROM GSSS: comment_3: REGION/PLATE/SCRIPT=XX002/06B1/06B3 comment_4: TRY TO USE SAME GUIDE STARS AS comment_5: FOR W0SK0401T. fluxnum_1: 1 fluxval_1: F-CONT(1650) = 1.5 +/- 0.8 E-15 fluxnum_2: 2 fluxval_2: F-LINE(5007) = 1.4 +/- 0.1 E-12 fluxnum_3: 3 fluxval_3: SURF-LINE(5007) = 1.9 +/- 0.5 E-11 fluxnum_4: 4 fluxval_4: SURF-LINE(4861) = 2.3 +/- 0.5 E-12 fluxnum_5: 5 fluxval_5: SURF-CONT(5470) = 2.0 +/- 1.0 E-14 fluxnum_6: 6 fluxval_6: W-LINE(5007) = 1.0, SIZE = 0.30 ! targnum: 128 name_1: SMC-SMP28 name_2: LN536 descr_1: H,502 pos_1: RA = 01H 24M 11.84S +/- 0.02S, pos_2: DEC = -74D 02' 32.13" +/- 0.1", pos_3: PLATE-ID=02I5 equinox: 2000.0 rv_or_z: V = 150 comment_1: FINAL POSITION OF PN DETERMINED comment_2: FROM GSSS: comment_3: REGION/PLATE/SCRIPT= S029/02I5/02JS comment_4: TRY TO USE SAME GUIDE STARS AS comment_5: FOR W0SK0601T. fluxnum_1: 1 fluxval_1: F-CONT(1650) = 7.2 +/- 3.6 E-16 fluxnum_2: 2 fluxval_2: F-LINE(5007) = 2.0 +/- 0.1 E-13 fluxnum_3: 3 fluxval_3: SURF-LINE(5007) = 4.6 +/- 1.2 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(4861) = 1.7 +/- 0.7 E-13 fluxnum_5: 5 fluxval_5: SURF-CONT(5470) = 4.3 +/- 2.2 E-16 fluxnum_6: 6 fluxval_6: W-LINE(5007) = 1.0, SIZE = 0.75 ! targnum: 202 name_1: LMC-SMP2 descr_1: H,502 pos_1: RA = 04H 40M 56.74S +/- 0.02S, pos_2: DEC = -67D 48' 02.70" +/- 0.1", pos_3: PLATE-ID=0186 equinox: 2000.0 rv_or_z: V = 263 comment_1: FOR ALL TARGETS: IDENT # FROM FOLL- comment_2: OWING REFS: SMP=SANDULEAK ETAL.1978 comment_3: PASP 90,621. N=HENIZE 1956. APJS 2, comment_4: 315. WS=WESTERLUND AND SMITH 1964. comment_5: MNRAS 127,449 J=JACOBY 1980. APJS comment_6: 42,1. FINAL POSITION OF PN DETER- comment_7: MINED FROM GSSS: comment_8: REGION/PLATE/SCRIPT= S055/0186/05C9 comment_9: USE SAME GUIDE STARS AS W0SK0701T. fluxnum_1: 1 fluxval_1: F-CONT(1650) = 6.3 +/- 3.2 E-16 fluxnum_2: 2 fluxval_2: F-LINE(5007) = 1.7 +/- 0.1 E-13 fluxnum_3: 3 fluxval_3: SURF-LINE(5007) = 2.1 +/- 0.5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(4861) = 8.2 +/- 2.0 E-13 fluxnum_5: 5 fluxval_5: SURF-CONT(5470) = 2.1 +/- 1.1 E-14 fluxnum_6: 6 fluxval_6: W-LINE(5007) = 1.0, SIZE = 0.32 ! targnum: 208 name_1: LMC-SMP8 name_2: N78 descr_1: H,502 pos_1: RA = 04H 50M 13.10S +/- 0.02S, pos_2: DEC = -69D 33' 57.05" +/- 0.1", pos_3: PLATE-ID=05ZW equinox: 2000.0 rv_or_z: V = 298 comment_1: FINAL POSITION OF PN DETERMINED comment_2: FROM GSSS: comment_3: REGION/PLATE/SCRIPT=XV056/05ZW/065M comment_4: TRY TO USE SAME GUIDE STARS AS comment_5: FOR W0SK0801T. fluxnum_1: 1 fluxval_1: F-CONT(1650) = 1.7 +/- 0.9 E-15 fluxnum_2: 2 fluxval_2: F-LINE(5007) = 1.0 +/- 0.1 E-12 fluxnum_3: 3 fluxval_3: SURF-LINE(5007) = 4.2 +/- 1.0 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(4861) = 7.4 +/- 2.5 E-13 fluxnum_5: 5 fluxval_5: SURF-CONT(5470) = 2.9 +/- 1.5 E-15 fluxnum_6: 6 fluxval_6: W-LINE(5007) = 1.0, SIZE = 0.56 ! targnum: 220 name_1: LMC-SMP20 descr_1: H,502 pos_1: RA = 05H 04M 40.14S +/- 0.02S, pos_2: DEC = -69D 21' 39.32" +/- 0.1", pos_3: PLATE-ID=05ZW equinox: 2000.0 rv_or_z: V = 293 comment_1: FINAL POSITION OF PN DETERMINED comment_2: FROM GSSS: comment_3: REGION/PLATE/SCRIPT=XV056/05ZW/065M comment_4: TRY TO USE SAME GUIDE STARS AS comment_5: FOR W0SK0901T. fluxnum_1: 1 fluxval_1: F-CONT(1650) = 4.1 +/- 2.1 E-16 fluxnum_2: 2 fluxval_2: F-LINE(5007) = 2.7 +/- 0.2 E-13 fluxnum_3: 3 fluxval_3: SURF-LINE(5007) = 3.6 +/- 1.0 E-13 fluxnum_4: 4 fluxval_4: SURF-LINE(4861) = 5.6 +/- 2.0 E-14 fluxnum_5: 5 fluxval_5: SURF-CONT(5470) = 3.4 +/- 1.7 E-16 fluxnum_6: 6 fluxval_6: W-LINE(5007) = 1.0, SIZE = 0.98 ! targnum: 235 name_1: LMC-SMP35 name_2: WS 12 descr_1: H,502 pos_1: RA = 05H 10M 49.97S +/- 0.02S, pos_2: DEC = -65D 29' 30.67" +/- 0.1", pos_3: PLATE-ID=06AF equinox: 2000.0 rv_or_z: V = 314 comment_1: FINAL POSITION OF PN DETERMINED comment_2: FROM GSSS: comment_3: REGION/PLATE/SCRIPT=XV085/06AF/06C9 comment_4: TRY TO USE SAME GUIDE STARS AS comment_5: FOR W0SK0A01T. fluxnum_1: 1 fluxval_1: F-CONT(1650) = 1.5 +/- 0.8 E-15 fluxnum_2: 2 fluxval_2: F-LINE(5007) = 1.9 +/- 0.2 E-12 fluxnum_3: 3 fluxval_3: SURF-LINE(5007) = 3.8 +/- 0.9 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(4861) = 3.1 +/- 0.8 E-13 fluxnum_5: 5 fluxval_5: SURF-CONT(5470) = 1.2 +/- 0.6 E-15 fluxnum_6: 6 fluxval_6: W-LINE(5007) = 1.0, SIZE = 0.80 ! targnum: 240 name_1: LMC-SMP40 name_2: WS 16 descr_1: H,502 pos_1: RA = 05H 12M 15.63S +/- 0.02S, pos_2: DEC = -66D 22' 56.81" +/- 0.1", pos_3: PLATE-ID=06AF equinox: 2000.0 rv_or_z: V = 290 comment_1: FINAL POSITION OF PN DETERMINED comment_2: FROM GSSS: comment_3: REGION/PLATE/SCRIPT=XV085/06AF/06C9 comment_4: TRY TO USE SAME GUIDE STARS AS comment_5: FOR W0SK0B01T. fluxnum_1: 1 fluxval_1: F-CONT(1650) = 6.0 +/- 3.0 E-16 fluxnum_2: 2 fluxval_2: F-LINE(5007) = 4.8 +/- 0.4 E-13 fluxnum_3: 3 fluxval_3: SURF-LINE(5007) = 5.7 +/- 1.3 E-13 fluxnum_4: 4 fluxval_4: SURF-LINE(4861) = 6.7 +/- 2.0 E-14 fluxnum_5: 5 fluxval_5: SURF-CONT(5470) = 2.4 +/- 1.2 E-16 fluxnum_6: 6 fluxval_6: W-LINE(5007) = 1.0, SIZE = 1.03 ! targnum: 247 name_1: LMC-SMP47 name_2: N122 name_3: WS 18 descr_1: H,502 pos_1: RA = 05H 19M 54.71S +/- 0.02S, pos_2: DEC = -69D 31' 05.28" +/- 0.1", pos_3: PLATE-ID=05ZW equinox: 2000.0 rv_or_z: V = 280 comment_1: FINAL POSITION OF PN DETERMINED comment_2: FROM GSSS: comment_3: REGION/PLATE/SCRIPT=XV056/05ZW/065M comment_4: TRY TO USE SAME GUIDE STARS AS comment_5: FOR W0SK0C01T. fluxnum_1: 1 fluxval_1: F-CONT(1650) = 3.4 +/- 1.7 E-15 fluxnum_2: 2 fluxval_2: F-LINE(5007) = 3.3 +/- 0.3 E-12 fluxnum_3: 3 fluxval_3: SURF-LINE(5007) = 9.5 +/- 3.5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(4861) = 8.6 +/- 3.5 E-13 fluxnum_5: 5 fluxval_5: SURF-CONT(5470) = 4.5 +/- 2.3 E-15 fluxnum_6: 6 fluxval_6: W-LINE(5007) = 1.0, SIZE = 0.67 ! targnum: 276 name_1: LMC-SMP76 name_2: N60 name_3: WS 32 descr_1: H,502 pos_1: RA = 05H 33M 56.20S +/- 0.02S, pos_2: DEC = -67D 53' 08.38" +/- 0.1", pos_3: PLATE-ID=06B0 equinox: 2000.0 rv_or_z: V = 280 comment_1: FINAL POSITION OF PN DETERMINED comment_2: FROM GSSS: comment_3: REGION/PLATE/SCRIPT=XX001/06B0/06B4 comment_4: TRY TO USE SAME GUIDE STARS AS comment_5: FOR W0SK0E01T. fluxnum_1: 1 fluxval_1: F-CONT(1650) = 2.7 +/- 1.4 E-15 fluxnum_2: 2 fluxval_2: F-LINE(5007) = 1.6 +/- 0.2 E-12 fluxnum_3: 3 fluxval_3: SURF-LINE(5007) = 1.4 +/- 0.7 E-11 fluxnum_4: 4 fluxval_4: SURF-LINE(4861) = 2.5 +/- 1.3 E-12 fluxnum_5: 5 fluxval_5: SURF-CONT(5470) = 6.3 +/- 3.2 E-15 fluxnum_6: 6 fluxval_6: W-LINE(5007) = 1.0, SIZE = 0.38 ! targnum: 287 name_1: LMC-SMP87 name_2: N215 name_3: WS 37 descr_1: H,502 pos_1: RA = 05H 41M 08.12S +/- 0.02S, pos_2: DEC = -72D 42' 08.22" +/- 0.1", pos_3: PLATE-ID=00RG equinox: 2000.0 rv_or_z: V = 282 comment_1: FINAL POSITION OF PN DETERMINED comment_2: FROM GSSS: comment_3: REGION/PLATE/SCRIPT= S033/00RG/03N0 comment_4: TRY TO USE SAME GUIDE STARS AS comment_5: FOR W0SK0I01T. fluxnum_1: 1 fluxval_1: F-CONT(1650) = 1.2 +/- 0.6 E-15 fluxnum_2: 2 fluxval_2: F-LINE(5007) = 1.1 +/- 0.3 E-12 fluxnum_3: 3 fluxval_3: SURF-LINE(5007) = 8.6 +/- 2.5 E-13 fluxnum_4: 4 fluxval_4: SURF-LINE(4861) = 1.0 +/- 0.3 E-13 fluxnum_5: 5 fluxval_5: SURF-CONT(5470) = 4.0 +/- 2.0 E-16 fluxnum_6: 6 fluxval_6: W-LINE(5007) = 1.0, SIZE = 1.3 ! targnum: 296 name_1: LMC-SMP96 descr_1: H,502 pos_1: RA = 06H 06M 05.45S +/- 0.02S, pos_2: DEC = -71D 04' 14.88" +/- 0.1", pos_3: PLATE-ID=014D equinox: 2000.0 rv_or_z: V = 257 comment_1: FINAL POSITION OF PN DETERMINED comment_2: FROM GSSS: comment_3: REGION/PLATE/SCRIPT= S057/014D/04V4 comment_4: TRY TO USE SAME GUIDE STARS AS comment_5: FOR W0SK0J01T. fluxnum_1: 1 fluxval_1: F-CONT(1650) = 4.3 +/- 2.2 E-16 fluxnum_2: 2 fluxval_2: F-LINE(5007) = 3.0 +/- 0.2 E-13 fluxnum_3: 3 fluxval_3: SURF-LINE(5007) = 1.0 +/- 0.3 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(4861) = 1.5 +/- 0.4 E-13 fluxnum_5: 5 fluxval_5: SURF-CONT(5470) = 4.0 +/- 2.0 E-16 fluxnum_6: 6 fluxval_6: W-LINE(5007) = 1.0, SIZE = 0.62 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: BINACQ targname: # config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 720000, param_2: FAINT = 660 comment_1: ALL ACQ/BIN EXPOSURE TIMES DERIVED comment_2: FROM FOS SIMULATOR USING OBSERVED comment_3: OPTICAL SPECTRA AND UV MODELS. ! linenum: 2.000 sequence_1: DEFINE sequence_2: PKUPBL targname: # config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 1S fluxnum_1: 1 priority: 1 param_1: TYPE=UP, param_2: SEARCH-SIZE=5, param_3: SCAN-STEP=0.5 ! linenum: 3.000 sequence_1: DEFINE sequence_2: IMGACQ targname: # config: FOS/BL opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1S fluxnum_1: 1 priority: 1 comment_1: EXPOSURE TIMES ARE A FACTOR 64/11 comment_2: OF THE RESPECTIVE ACQ/BIN TIMES. ! linenum: 4.000 sequence_1: DEFINE sequence_2: FOS130 targname: # config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 1S s_to_n: # fluxnum_1: 1 priority: 1 ! linenum: 5.000 sequence_1: DEFINE sequence_2: FOS190 targname: # config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 1S s_to_n: # fluxnum_1: 1 priority: 1 ! linenum: 6.000 sequence_1: DEFINE sequence_2: FOS270 targname: # config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: PRISM num_exp: 1 time_per_exp: 1S s_to_n: # fluxnum_1: 1 priority: 1 ! linenum: 200.100 sequence_1: USE BINACQ targname: SMC-SMP1 time_per_exp: X40 req_1: SEQ 200.1 - 200.4 NO GAP; req_2: ONBOARD ACQ FOR 200.15 - 200.4; req_3: CYCLE 2 / 200.1-200.4 ! linenum: 200.150 sequence_1: USE IMGACQ targname: SMC-SMP1 time_per_exp: X240 ! linenum: 200.200 sequence_1: USE FOS130 targname: SMC-SMP1 time_per_exp: X700 s_to_n: 3 ! linenum: 200.300 sequence_1: USE FOS190 targname: SMC-SMP1 time_per_exp: X350 s_to_n: 3 ! linenum: 200.400 sequence_1: USE FOS270 targname: SMC-SMP1 time_per_exp: X200 s_to_n: 3 ! linenum: 201.100 sequence_1: USE BINACQ targname: SMC-SMP3 time_per_exp: X50 req_1: SEQ 201.1 - 201.4 NO GAP; req_2: ONBOARD ACQ FOR 201.15 - 201.4; req_3: CYCLE 2 / 201.1-201.4 ! linenum: 201.150 sequence_1: USE IMGACQ targname: SMC-SMP3 time_per_exp: X290 ! linenum: 201.200 sequence_1: USE FOS130 targname: SMC-SMP3 time_per_exp: X700 s_to_n: 3 ! linenum: 201.300 sequence_1: USE FOS190 targname: SMC-SMP3 time_per_exp: X350 s_to_n: 3 ! linenum: 201.400 sequence_1: USE FOS270 targname: SMC-SMP3 time_per_exp: X200 s_to_n: 3 ! linenum: 202.100 sequence_1: USE BINACQ targname: SMC-SMP6 time_per_exp: X55 req_1: SEQ 202.1 - 202.4 NO GAP; req_2: ONBOARD ACQ FOR 202.15 - 202.4; req_3: CYCLE 2 / 202.1-202.4 ! linenum: 202.150 sequence_1: USE IMGACQ targname: SMC-SMP6 time_per_exp: X335 ! linenum: 202.200 sequence_1: USE FOS130 targname: SMC-SMP6 time_per_exp: X900 s_to_n: 3 ! linenum: 202.300 sequence_1: USE FOS190 targname: SMC-SMP6 time_per_exp: X400 s_to_n: 3 ! linenum: 202.400 sequence_1: USE FOS270 targname: SMC-SMP6 time_per_exp: X250 s_to_n: 3 ! linenum: 204.100 sequence_1: USE BINACQ targname: SMC-SMP28 time_per_exp: X135 req_1: SEQ 204.1 - 204.4 NO GAP; req_2: ONBOARD ACQ FOR 204.15 - 204.4; req_3: CYCLE 2 / 204.1-204.4 ! linenum: 204.150 sequence_1: USE IMGACQ targname: SMC-SMP28 time_per_exp: X795 ! linenum: 204.200 sequence_1: USE FOS130 targname: SMC-SMP28 time_per_exp: X2000 s_to_n: 3 ! linenum: 204.300 sequence_1: USE FOS190 targname: SMC-SMP28 time_per_exp: X1000 s_to_n: 3 ! linenum: 204.400 sequence_1: USE FOS270 targname: SMC-SMP28 time_per_exp: X450 s_to_n: 3 ! linenum: 300.100 sequence_1: USE BINACQ targname: LMC-SMP2 time_per_exp: X55 req_1: SEQ 300.1 - 300.4 NO GAP; req_2: ONBOARD ACQ FOR 300.15 - 300.4; req_3: CYCLE 2 / 300.1-300.4 ! linenum: 300.150 sequence_1: USE IMGACQ targname: LMC-SMP2 time_per_exp: X320 ! linenum: 300.200 sequence_1: USE FOS130 targname: LMC-SMP2 time_per_exp: X1600 s_to_n: 3 ! linenum: 300.300 sequence_1: USE FOS190 targname: LMC-SMP2 time_per_exp: X800 s_to_n: 3 ! linenum: 300.400 sequence_1: USE FOS270 targname: LMC-SMP2 time_per_exp: X350 s_to_n: 3 ! linenum: 301.100 sequence_1: USE BINACQ targname: LMC-SMP8 time_per_exp: X35 req_1: SEQ 301.1 - 301.4 NO GAP; req_2: ONBOARD ACQ FOR 301.15 - 301.4; req_3: CYCLE 2 / 301.1-301.4 ! linenum: 301.150 sequence_1: USE IMGACQ targname: LMC-SMP8 time_per_exp: X200 ! linenum: 301.200 sequence_1: USE FOS130 targname: LMC-SMP8 time_per_exp: X700 s_to_n: 3 ! linenum: 301.300 sequence_1: USE FOS190 targname: LMC-SMP8 time_per_exp: X350 s_to_n: 3 ! linenum: 301.400 sequence_1: USE FOS270 targname: LMC-SMP8 time_per_exp: X200 s_to_n: 3 ! linenum: 302.100 targname: LMC-SMP20 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G570H wavelength: 5007 num_exp: 1 time_per_exp: 34S fluxnum_1: 1 priority: 1 param_1: TYPE=UP, param_2: SEARCH-SIZE=5, param_3: SCAN-STEP=0.5 req_1: SEQ 302.1 - 302.4 NO GAP; req_2: ONBOARD ACQ FOR 302.15 - 302.4; req_3: CYCLE 2 / 302.1-302.4; comment_1: ACQ/PEAKUP ON 5007 ANGSTROM comment_2: LINE ONLY USING G570H GRATING. ! linenum: 302.150 sequence_1: USE IMGACQ targname: LMC-SMP20 time_per_exp: X320 ! linenum: 302.200 sequence_1: USE FOS130 targname: LMC-SMP20 time_per_exp: X2200 s_to_n: 3 ! linenum: 302.300 sequence_1: USE FOS190 targname: LMC-SMP20 time_per_exp: X1100 s_to_n: 3 ! linenum: 302.400 sequence_1: USE FOS270 targname: LMC-SMP20 time_per_exp: X500 s_to_n: 3 ! linenum: 303.100 sequence_1: USE PKUPBL targname: LMC-SMP35 time_per_exp: X4 req_1: SEQ 303.1 - 303.4 NO GAP; req_2: ONBOARD ACQ FOR 303.15 - 303.4; req_3: CYCLE 2 / 303.1-303.4 comment_1: MUST USE PEAK-UP AS PN IS comment_2: LARGER THAN DIODE WIDTH. ! linenum: 303.150 sequence_1: USE IMGACQ targname: LMC-SMP35 time_per_exp: X260 ! linenum: 303.200 sequence_1: USE FOS130 targname: LMC-SMP35 time_per_exp: X600 s_to_n: 3 ! linenum: 303.300 sequence_1: USE FOS190 targname: LMC-SMP35 time_per_exp: X300 s_to_n: 3 ! linenum: 303.400 sequence_1: USE FOS270 targname: LMC-SMP35 time_per_exp: X140 s_to_n: 3 ! linenum: 304.100 sequence_1: USE BINACQ targname: LMC-SMP40 time_per_exp: X60 req_1: SEQ 304.1 - 304.4 NO GAP; req_2: ONBOARD ACQ FOR 304.15 - 304.4; req_3: CYCLE 2 / 304.1-304.4 ! linenum: 304.150 sequence_1: USE IMGACQ targname: LMC-SMP40 time_per_exp: X360 ! linenum: 304.200 sequence_1: USE FOS130 targname: LMC-SMP40 time_per_exp: X2200 s_to_n: 3 ! linenum: 304.300 sequence_1: USE FOS190 targname: LMC-SMP40 time_per_exp: X1100 s_to_n: 3 ! linenum: 304.400 sequence_1: USE FOS270 targname: LMC-SMP40 time_per_exp: X500 s_to_n: 3 ! linenum: 305.100 sequence_1: USE BINACQ targname: LMC-SMP47 time_per_exp: X25 req_1: SEQ 305.1 - 305.4 NO GAP; req_2: ONBOARD ACQ FOR 305.15 - 305.4; req_3: CYCLE 2 / 305.1-305.4 ! linenum: 305.150 sequence_1: USE IMGACQ targname: LMC-SMP47 time_per_exp: X155 ! linenum: 305.200 sequence_1: USE FOS130 targname: LMC-SMP47 time_per_exp: X1200 s_to_n: 3 ! linenum: 305.300 sequence_1: USE FOS190 targname: LMC-SMP47 time_per_exp: X500 s_to_n: 3 ! linenum: 305.400 sequence_1: USE FOS270 targname: LMC-SMP47 time_per_exp: X300 s_to_n: 3 ! linenum: 307.100 sequence_1: USE BINACQ targname: LMC-SMP76 time_per_exp: X40 req_1: SEQ 307.1 - 307.4 NO GAP; req_2: ONBOARD ACQ FOR 307.15 - 307.4; req_3: CYCLE 2 / 307.1-307.4 ! linenum: 307.150 sequence_1: USE IMGACQ targname: LMC-SMP76 time_per_exp: X250 ! linenum: 307.200 sequence_1: USE FOS130 targname: LMC-SMP76 time_per_exp: X500 s_to_n: 3 ! linenum: 307.300 sequence_1: USE FOS190 targname: LMC-SMP76 time_per_exp: X250 s_to_n: 3 ! linenum: 307.400 sequence_1: USE FOS270 targname: LMC-SMP76 time_per_exp: X120 s_to_n: 3 ! linenum: 309.100 sequence_1: USE PKUPBL targname: LMC-SMP87 time_per_exp: X7 req_1: SEQ 309.1 - 309.4 NO GAP; req_2: ONBOARD ACQ FOR 309.15 - 309.4; req_3: CYCLE 2 / 309.1-309.4 comment_1: MUST USE PEAK-UP AS PN IS comment_2: LARGER THAN DIODE WIDTH. ! linenum: 309.150 sequence_1: USE IMGACQ targname: LMC-SMP87 time_per_exp: X445 ! linenum: 309.200 sequence_1: USE FOS130 targname: LMC-SMP87 time_per_exp: X1800 s_to_n: 3 ! linenum: 309.300 sequence_1: USE FOS190 targname: LMC-SMP87 time_per_exp: X800 s_to_n: 3 ! linenum: 309.400 sequence_1: USE FOS270 targname: LMC-SMP87 time_per_exp: X400 s_to_n: 3 ! linenum: 310.100 sequence_1: USE BINACQ targname: LMC-SMP96 time_per_exp: X80 req_1: SEQ 310.1 - 310.4 NO GAP; req_2: ONBOARD ACQ FOR 310.15 - 310.4; req_3: CYCLE 2 / 310.1-310.4 ! linenum: 310.150 sequence_1: USE IMGACQ targname: LMC-SMP96 time_per_exp: X465 ! linenum: 310.200 sequence_1: USE FOS130 targname: LMC-SMP96 time_per_exp: X2200 s_to_n: 3 ! linenum: 310.300 sequence_1: USE FOS190 targname: LMC-SMP96 time_per_exp: X1100 s_to_n: 3 ! linenum: 310.400 sequence_1: USE FOS270 targname: LMC-SMP96 time_per_exp: X500 s_to_n: 3 ! ! end of exposure logsheet ! No scan data records found