! File: 4566C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:17:58:09 coverpage: title_1: POST ASYMPTOTIC GIANT BRANCH EVOLUTION IN THE MAGELLANIC CLOUDS - title_2: SPECTROSCOPY: CYCLE 3 HIGH sci_cat: INTERSTELLAR MEDIUM sci_subcat: PLANETARY NEBULAE proposal_for: GO longterm: 3 cont_id: 2266 pi_fname: MICHAEL pi_mi: A pi_lname: DOPITA pi_inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES hours_pri: 6.04 num_pri: 6 fos: Y funds_length: 24 off_fname: DONALD off_mi: J off_lname: FAULKNER off_title: ACTING 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 6 249-0258 ! end of coverpage abstract: line_1: Planetary Nebulae (PN) represent a critical stage of stellar evolution which is line_2: relatively poorly understood. More reliable observational estimates line_3: of stellar luminosity, mass, effective temperature, and age are required line_4: to constrain evolutionary models and determine mass-loss rates, line_5: He shell flash phases, and the role of dredge-up. This proposal represents the line_6: continuation of our systematic and definitive study with HST of a line_7: large sample of nebulae at known distance in the Magellanic Clouds and line_8: requires approximately 50 hours for completion. line_9: All parameters needed for confrontation of theory with observation can be line_10: derived from direct PC imaging and FOS spectra in the 1150-3200A range. The line_11: images give spatial structure, sizes, ionized mass, dynamical ages, and an line_12: estimate of the final mass-loss rate on the AGB. The spectra will be line_13: combined with the images and with stellar atmospheric and line_14: evolutionary models to derive the effective temperature, luminosity, and line_15: core mass of each of the exciting stars. line_16: These data will define the evolutionary status of each of the PN observed. line_17: We will use two independent ionization codes to interpret the spatial structure line_18: derived from PC images and the FOS data, in conjuction with optical and IR line_19: spectra. This analysis will also yield chemical abundances of many elements, line_20: including the astrophysically important species He, C, N, O, and Si. ! ! end of abstract general_form_proposers: lname: DOPITA fname: MICHAEL title: PI mi: A inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES country: AUSTRALIA ! lname: MEATHERINGHAM fname: STEPHEN mi: J inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES country: AUSTRALIA ! lname: WOOD fname: PETER mi: R inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES country: AUSTRALIA ! lname: BOHLIN fname: RALPH mi: C inst: STSCI country: USA ! lname: FORD fname: HOLLAND mi: C inst: STSCI country: USA ! lname: VASSILIADIS fname: EMANUEL inst: STSCI country: USA ! lname: HARRINGTON fname: PATRICK mi: J inst: UNIVERSITY OF MARYLAND country: USA ! lname: STECHER fname: THEODORE mi: P inst: NASA GODDARD SPACE FLIGHT CENTER country: USA ! lname: MARAN fname: STEPHEN mi: P inst: NASA GODDARD SPACE FLIGHT CENTER country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Imaging Program: This part of the program has been transferred to proposal line_2: 4940, which must be completed before the FOS observations are attempted. line_3: Cycle 3 UV Spectrophotometry: We are undertaking FOS spectrophotometry line_4: during Cycle 3 in the range 1150 - 5000 Angstroms using the G130H line_5: and G190H gratings, and the PRISM. We aim to achieve an average signal line_6: to noise in the nebular continuum of 3 per pixel. Since it proves to be line_7: very inefficient to do separate AQU/PEAK for both the blue and red line_8: sides of the spectrograph, we have elected to observe on the blue side line_9: only, accepting the lower efficiency in order to have data in the line_10: G130H bandpass. Similarly, Cycle 2 experience has shown us that the PRISM line_11: gives adequate resolution in the pass-band previously covered by the G270H line_12: grating, and additional coverage into the optical. line_13: Since the Magellanic Clouds are close enough that even the faintest line_14: PN can be detected, the flux and spectral distribution of line_15: the PN nuclei can be measured over their entire ~5 mag in luminosity. line_16: Our aim is to accomplish this objective, and to achieve a good line_17: detection of the central star against the nebular continuum, even when line_18: the stellar flux is only 10% of this nebular continuum. This line_19: objective will also ensure that uniform, high quality, high dynamic line_20: range nebular spectra are obtained for the full range of nebular line_21: conditions. ! question: 3 section: 2 line_1: For the purposes of computing exposure times for spectra, line_2: a mean extinction E(B-V) of 0.15 and an LMC or SMC-like extinction law line_3: have been assumed. The counts/diode/second C-d, is given in terms of line_4: the flux at 1650 Angstroms (F_1650):log(C_d) =- f(Phi) C + log(F_1650), line_5: where C has the values 13.53 (G130H, blue digicon) and 13.56 (G190H, line_6: blue digicon) and 14.10 (G270H,again the blue digicon). line_7: The function f(Phi) is a function of the diameter of the PN, line_8: accounting for spherical abberation and is calculated from a line_9: modelling of the PSF and the PN. line_10: These data will be combined with our ground-based data line_11: of comparable quality covering the wavelength range 3200 - 10000 line_12: Angstroms. In the decade of frequency covered by these observations, line_13: we will see emission lines of the astrophysically important elements line_14: such as He, C, N, O, Si and S in the full range of ionisation stages line_15: expected to be present in the nebula. For this reason, and also line_16: because the allowable nebular models are strongly constrained by the line_17: imaging results, we expect that the chemical abundances we will derive line_18: will be much more accurate than any previously obtained. ! question: 3 section: 3 line_1: The proper method of acquisition can only be determined once the PC line_2: images from proposal 4940 have been analysed. As was found for the line_3: Cycle 2 proposal 3441, most acquisitions will probably become BINARY line_4: ACQs, and will consequently reduce the overhead times significantly. line_5: This will be the case for objects found to have a diameter less than line_6: a FOS diode width (0.35 arcsec). line_7: For those targets larger than a FOS diode width, line_8: a 5x5 PEAK-UP acquistion, with 0.5 arcsec steps using the 1 arcsec line_9: aperture, will be performed. This gives an effective field coverage of line_10: 3x3 arcsec, and will achieve 0.25*(2**0.5) = 0.35 arcsec accuracy on any line_11: PN within 1.25 arcsec of the initial pointing position. line_12: References: line_13: Jacoby, G., 1980, Ap. J. Suppl. Ser.,42, p. 1 line_14: Wood, P.R., Bessell, M.S., and Dopita, M.A., 1986, Ap. J.,311, p. 632 line_15: Wood, P.R., Meatheringham, S.J., Dopita, M.A., and Morgan, D.H., 1987, line_16: Ap. J., 320, p. 178 ! question: 4 section: 1 line_1: The angular diameters of the Magellanic Cloud PN lie in the range line_2: 0.05 - 4.0 arcseconds, ideally suited to the HST capabilities. line_3: Some of us have obtained low resolution UV spectra of a few of these line_4: objects using the IUE satellite. However, only the brightest objects line_5: are observable, many of the same objects chosen for the GTO program. line_6: The UV data is crucial for measurement of the stellar flux line_7: distribution and to obtain densities and ionic abundances for dominant line_8: ionisation stages of many elements. Only the combination of high line_9: resolution and a spectral range which extends shortward of the peak in line_10: the hydrogen two-photon nebular continuum (about 1450 Angstroms) will line_11: enable us to detect the star in the cases where the nebular continuum line_12: is strong. line_13: Our HST program is supported by a comprehensive and continuing line_14: ground-based program. We have used the 1-metre, 2.3-metre and line_15: 3.9-metre telescopes at Siding Spring to measure fluxes, sizes, line_16: expansion velocities, radial velocities and nebular spectra from 3200 line_17: to 10000 Angstroms. These observations already provide an excellent line_18: set of homogeneous and high-quality data which gives the best possible line_19: ground-based characteristics of the Magellanic Cloud population of PN. line_20: this data set will allow us to extend our population classifications line_21: from the HST subset to the entire population of PN in the Magellanic line_22: Clouds. line_23: References: See question 3. ! question: 5 section: 1 line_1: An 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 3 FOS spectroscopy program. Based on our experience with our Cycle 2 line_5: FOS exposures, the imaging program must be completed first to allow a proper line_6: determination of the method of FOS acquistion. The EARLY ACQ imaging proposal line_7: (4940) needs to be executed sufficiently early for the FOS spectroscopy (this line_8: proposal) to be completed before the end of Cycle 3. ! question: 6 section: 1 line_1: The FOS spectroscopic observations are required to be carried out in line_2: SEQ NO GAP mode because we need to be sure that the same part of the line_3: nebula is being observed in all three spectral bands. This is a line_4: requirement for the 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: (011 61) 6 2490212 telex: AA62270 ! ! end of general_form_address records fixed_targets: targnum: 101 name_1: SMC-SMP22 name_2: N67 name_3: LN333 descr_1: H,502 pos_1: RA = 00H 58M 37.22S +/- 0.02S, pos_2: DEC = -71D 35' 48.79" +/- 0.1" equinox: 2000.0 rv_or_z: V = 153 comment_1: FOR ALL TARGETS, comment_2: IDENT # FROM FOLLOWING REFS: comment_3: SMP=SANDULEAK ETAL.1978.PASP 90,621 comment_4: N = HENIZE 1956. AP J. SUPPL. 2,315 comment_5: LN = LINDSAY 1961. ASTR. J. 66, 169 fluxnum_1: 1 fluxval_1: F-CONT(1650) = 1.8 +/- 0.8 E-15 fluxnum_2: 2 fluxval_2: F-LINE(1666) = 1.9 +/- 0.6 E-14 fluxnum_3: 3 fluxval_3: F-LINE(5007) = 3.8 +/- 0.1 E-13 fluxnum_4: 4 fluxval_4: SURF-LINE(5007) = 3.0 +/- 1.0 E-12 fluxnum_5: 5 fluxval_5: W-LINE(5007) = 1.0, SIZE = 0.4 ! targnum: 104 name_1: LMC-SMP61 name_2: N203 descr_1: H,502 pos_1: RA = 05H 24M 35.97S +/- 0.02S, pos_2: DEC = -73D 40' 39.68" +/- 0.1" equinox: 2000.0 rv_or_z: V = 193 fluxnum_1: 1 fluxval_1: F-CONT(1650) = 2.1 +/- 0.6 E-14 fluxnum_2: 2 fluxval_2: F-LINE(1666) = 1.5 +/- 0.3 E-13 fluxnum_3: 3 fluxval_3: F-LINE(5007) = 2.9 +/- 0.1 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(5007) = 1.5 +/- 1.0 E-11 fluxnum_5: 5 fluxval_5: W-LINE(5007) = 1.0, SIZE = 0.5 ! targnum: 105 name_1: LMC-SMP67 name_2: N53 descr_1: H,502 pos_1: RA = 05H 29M 15.75S +/- 0.02S, pos_2: DEC = -67D 32' 47.58" +/- 0.1" equinox: 2000.0 rv_or_z: V = 289 fluxnum_1: 1 fluxval_1: F-CONT(1650) = 2.0 +/- 0.6 E-14 fluxnum_2: 2 fluxval_2: F-LINE(1666) = 2.7 +/- 0.6 E-14 fluxnum_3: 3 fluxval_3: F-LINE(5007) = 5.4 +/- 0.1 E-13 fluxnum_4: 4 fluxval_4: SURF-LINE(5007) = 2.8 +/- 1.0 E-12 fluxnum_5: 5 fluxval_5: W-LINE(5007) = 1.0, SIZE = 0.5 ! targnum: 106 name_1: LMC-SMP101 descr_1: H,502 pos_1: RA = 06H 23M 40.39S +/- 0.02S, pos_2: DEC = -69D 10' 38.35" +/- 0.1" equinox: 2000.0 rv_or_z: V = 281 fluxnum_1: 1 fluxval_1: F-CONT(1650) = 2.1 +/- 0.8 E-15 fluxnum_2: 2 fluxval_2: F-LINE(1666) = 7.3 +/- 0.6 E-14 fluxnum_3: 3 fluxval_3: F-LINE(5007) = 1.5 +/- 0.1 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(5007) = 1.3 +/- 1.0 E-12 fluxnum_5: 5 fluxval_5: W-LINE(5007) = 1.0, SIZE = 1.2 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 3.000 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 req_1: CYCLE 3 / 3.0-106.4 ! linenum: 4.000 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-X=5, param_3: SCAN-STEP-X=0.5, param_4: SEARCH-SIZE-Y=5, param_5: SCAN-STEP-Y=0.5 ! linenum: 5.000 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: 6.000 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: 7.000 sequence_1: DEFINE sequence_2: BLUPRI 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: 101.100 sequence_1: USE PKUPBL targname: SMC-SMP22 time_per_exp: X10.0 req_1: SEQ 101.1 - 101.4 NO GAP; req_2: ONBOARD ACQ FOR 101.2 - 101.4; ! linenum: 101.200 sequence_1: USE FOS130 targname: SMC-SMP22 time_per_exp: X1700 s_to_n: 3 ! linenum: 101.300 sequence_1: USE FOS190 targname: SMC-SMP22 time_per_exp: X700 s_to_n: 3 ! linenum: 101.400 sequence_1: USE BLUPRI targname: SMC-SMP22 time_per_exp: X200 s_to_n: 3 ! linenum: 104.100 sequence_1: USE BINACQ targname: LMC-SMP61 time_per_exp: X33.0 req_1: SEQ 104.1 - 104.4 NO GAP; req_2: ONBOARD ACQ FOR 104.2 - 104.4; ! linenum: 104.200 sequence_1: USE FOS130 targname: LMC-SMP61 time_per_exp: X400 s_to_n: 3 ! linenum: 104.300 sequence_1: USE FOS190 targname: LMC-SMP61 time_per_exp: X150 s_to_n: 3 ! linenum: 104.400 sequence_1: USE BLUPRI targname: LMC-SMP61 time_per_exp: X100 s_to_n: 3 ! linenum: 105.100 sequence_1: USE BINACQ targname: LMC-SMP67 time_per_exp: X33.0 req_1: SEQ 105.1 - 105.4 NO GAP; req_2: ONBOARD ACQ FOR 105.2 - 105.4; ! linenum: 105.200 sequence_1: USE FOS130 targname: LMC-SMP67 time_per_exp: X1100 s_to_n: 3 ! linenum: 105.300 sequence_1: USE FOS190 targname: LMC-SMP67 time_per_exp: X500 s_to_n: 3 ! linenum: 105.400 sequence_1: USE BLUPRI targname: LMC-SMP67 time_per_exp: X150 s_to_n: 3 ! linenum: 106.100 sequence_1: USE PKUPBL targname: LMC-SMP101 time_per_exp: X5.0 req_1: SEQ 106.1 - 106.4 NO GAP; req_2: ONBOARD ACQ FOR 106.2 - 106.4; ! linenum: 106.200 sequence_1: USE FOS130 targname: LMC-SMP101 time_per_exp: X1000 s_to_n: 3 ! linenum: 106.300 sequence_1: USE FOS190 targname: LMC-SMP101 time_per_exp: X500 s_to_n: 3 ! linenum: 106.400 sequence_1: USE BLUPRI targname: LMC-SMP101 time_per_exp: X150 s_to_n: 3 ! ! end of exposure logsheet ! No scan data records found