! File: 4040C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:06:10:47 coverpage: title_1: POST ASYMPTOTIC GIANT BRANCH EVOLUTION IN THE MAGELLANIC CLOUDS. title_2: CONT OF 2266 sci_cat: STELLAR ASTROPHYSICS sci_subcat: LATE EVOLUTION proposal_for: GO cont_id: 2266 pi_title: DR. pi_fname: MICHAEL pi_mi: A. pi_lname: DOPITA pi_inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES pi_country: AUSTRALIA pi_phone: (011 61) 62-49-0212 keywords_1: STARS:HB STAR, INTERSTELLAR MEDIUM:PLANETARY NEBULA, keywords_2: GALAXY:MAGELLANIC CLOUDS, ASTROPHYSICS:EVOLUTION, STELLAR POPULATION, ABUNDANCE hours_pri: 40.00 num_pri: 19 wf_pc: Y fos: Y funds_amount: 593475 funds_length: 3 funds_date: OCT-90 pi_position: SENIOR FELLOW 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 off_addr_2: WODEN P.O. off_city: WODEN off_state: ACT off_zip: 2606 off_country: AUSTRALIA off_phone: (011 61) 62-49-0262 off_telex: AA62270 CANOPUS ! 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 title: DR mi: R inst: MOUNT STROMLO AND SIDING SPRING OBSERVATORIES country: AUSTRALIA ! lname: MEATHERINGHAM fname: STEPHEN title: DR mi: J inst: MOUNT STROMLO AND SIDING SPRING OBSERVATORIES country: AUSTRALIA ! lname: BOHLIN fname: RALPH title: DR mi: C inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: FORD fname: HOLLAND title: DR mi: C inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: HARRINGTON fname: PATRICK title: DR mi: J inst: UNIVERSITY OF MARYLAND country: USA ! lname: STECHER fname: THEODORE title: DR mi: P inst: GODDARD SPACE FLIGHT CENTER country: USA ! lname: MARAN fname: STEPHEN title: DR mi: P inst: GODDARD SPACE FLIGHT CENTER country: USA ! lname: WEBSTER(DECEASED) fname: LOUISE title: DR mi: B inst: UNIVERSITY OF NEW SOUTH WALES country: AUSTRALIA ! lname: DOPITA fname: MICHAEL title: DR 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. We prefer to line_5: use the PC rather than the FOC, because the FOC has a limited dynamic line_6: range, would saturate on many of our objects, and does not carry the line_7: required set of filters. Our [O III] 5007 Angstrom (F502N) images line_8: are designed to give a typical signal to noise of 20 per pixel to line_9: provide data on angular diameters and nebular morphology (spherical, line_10: bipolar, multiple shell, etc.), which in conjunction with our line_11: ground-based [O III] expansion velocity measurements will provide a line_12: dynamical age model. line_13: UV Spectrophotometry: We are proposing FOS spectrophotometry in the line_14: range 1150 - 2332 Angstroms using the G130H and G190H gratings. We line_15: aim to achieve an average signal to noise in the nebular continuum of line_16: 5 per pixel. Since the Magellanic Clouds are close enough that even line_17: the faintest PN can be detected, the flux and spectral distribution of line_18: the PN nuclei can be measured over their entire ~5 mag in luminosity. line_19: 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. These data will be combined with our ground-based data line_6: of comparable quality covering the wavelength range 3200 - 10000 line_7: Angstroms. In the decade of frequency covered by these observations, line_8: we will see emission lines of the astrophysically important elements line_9: such as He, C, N, O, Si and S in the full range of ionisation stages line_10: expected to be present in the nebula. For this reason, and also line_11: because the allowable nebular models are strongly constrained by the line_12: imaging results, we expect that the chemical abundances we will derive line_13: will be much more accurate than any previously obtained. line_14: References: line_15: Jacoby, G., 1980, Ap. J. Suppl. Ser., vol. 42, p. 1 line_16: Wood, P.R., Bessell, M.S., and Dopita, M.A., 1986, Ap. J., vol. 311, p. 632 line_17: Wood, P.R., Meatheringham, S.J., Dopita, M.A., and Morgan, D.H., Ap. J., line_18: vol. 320, p. 178 line_19: NOTE: ALL OBSERVATIONS NOW DONE ON ONE SIDE ( BLUE ) PER PI's OK. line_20: 03/27/92 - RAL line_21: NOTE: METHOD OF ACQUISITION REVISED. line_22: PN ACQUIRED DIRECTLY USING BINARY SEARCH. line_23: 08/04/92. ! 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., vol. 42, p. 1 line_10: Wood, P.R., Bessell, M.S., and Dopita, M.A., 1986, Ap. J., vol. 311, p. 632 line_11: Wood, P.R., Meatheringham, S.J., Dopita, M.A., and Morgan, D.H., Ap. J., line_12: vol. 320, p. 178 ! question: 5 section: 1 line_1: Our observational objective is no less than to make the definitive line_2: study of PN evolution in the Magellanic Clouds. This program line_3: represents the first stage in this quest. To complete this objective line_4: will require approximately a further 150 hours of HST time. Our line_5: sample is therefore carefully chosen to eliminate selection bias in line_6: excitation class and flux, down to log(Flux(H-Beta)) ~13.7. By line_7: contrast, the GTO program shows a strong bias towards bright, high line_8: excitation, optically thick nebulae. This bias ensures that only PN line_9: with more massive nuclei are observed, and nothing can be concluded line_10: about the mass or age distribution from the GTO sample. By having a line_11: sufficiently large number of objects in the HR diagram we aim to study line_12: both the mass distribution and the rate of evolution through the HR line_13: diagram. The latter constraint is a particularly important one for line_14: stellar evolution; it will tell us at what phase of evolution on the line_15: AGB, and when in a Helium shell flash cycle PN ejection occurs. line_16: Abundances derived from these observations will show which PN nuclei line_17: have C-star progenitors, which, combined with the mass estimates will line_18: give mass, and hence age, limits for C-star formation, which can be line_19: linked with existing studies of this class of star. With the GTO line_20: program objects included, the total sample of some 25 PN will provide a line_21: suitable sample to begin to group the planetaries into statistically line_22: significant families in the three prime observational quantities. Our line_23: imaging program has been configured to provide [O III] images with an ! question: 5 section: 2 line_1: average S/N of 15 per pixel (850 photoelectrons per pixel) to ensure line_2: that high-quality images are obtained in the same line in which the line_3: expansion velocity profile is measured. line_4: The counts/pixel N are given in terms of the surface flux density (F_surf) line_5: by : log(N) = - f(Phi) C + log(F_surf), line_6: where C has the values 12.34, 12.28 for the F502N and F487N, line_7: filters, respectively. f(Phi) is a function of the diameter, and line_8: is calculated from the HST PSFfrom models. The spectroscopy program is line_9: configured to give a measurement of the C III] 1960/1990 Angstrom line_10: density and to give the nebular flux distribution to an accuracy of 3% line_11: in bins of 50 Angstroms. This ensures that the flux and flux line_12: distribution of the central star can be measured in the 1 arcsecond line_13: aperture down to 10% of the nebular continuum contributions. A mean line_14: extinction E(B-V) of 0.15 and an LMC or SMC-like extinction law has line_15: been assumed. The counts/diode/second C-d, is given in terms of the line_16: flux at 1650 Angstroms (F_1650)by : log(C_d) =- f(Phi) C + log(F_1650), where line_17: C has the values 13.53 (G130H, blue digicon) and 13.69 (G190H, red line_18: digicon). The red digicon rapidly increases in sensitivity at longer line_19: wavelengths so exposure times are shorter. The function f(Phi) is a line_20: function of the diameter of the PN, accounting for spherical abberation line_21: and is calculated from a modelling of the PSF and the PN. ! 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 are requesting that the line_3: direct imaging observations precede the spectrophotometric line_4: observations by 2-4 months in order that these images can be evaluated line_5: and used for accurate astrometry. For the spectrophotometric line_6: observations, we expect to acquire the PN by a binary search of the FOS line_7: on a nearby bright star followed by a blind offset to the PN. line_8: NOTE: METHOD OF ACQUISITION REVISED. line_9: PN ACQUIRED DIRECTLY USING BINARY SEARCH. line_10: 08/04/92. ! 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, Ap. J., line_18: vol. 314, p. 575 line_19: Dopita, M.A., Ford, H.C., Lawrence, C.J., and Webster, B.L., 1985, Ap. J., line_20: vol. 296, p. 390 line_21: Dopita, M.A., Meatheringham, S.J., Webster, B.L., and Ford, H.C.,1988, Ap. J., line_22: vol. 327, p. 639 line_23: Harrington, J.P., Seaton, M.J., Adams, S., and Lutz, J.H., 1982, M.N.R.A.S., ! question: 7 section: 3 line_1: 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_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: 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. title: DR. category: PI inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES addr_1: PRIVATE BAG addr_2: WODEN P.O. city: CANBERRA, ACT zip: 2606 country: AUSTRALIA phone: (011 61) 62 49-0212 telex: AA62270 CANOPUS ! ! end of general_form_address records fixed_targets: targnum: 118 name_1: LMC-SMP85 name_2: N69 descr_1: H,502 pos_1: RA = 05H 40M 30.87S +/- 0.02S, pos_2: DEC = -66D 17' 37.53" +/- 0.1", pos_3: PLATE-ID=06B0 equinox: 2000.0 rv_or_z: V = 232 comment_1: PN POSITION DETERMINED FROM GASP: comment_2: PLATES=06B0,02I7. (PLATE 06B0 USED comment_3: FOR COORDS HERE.) fluxnum_1: 1 fluxval_1: F-CONT(1650) = 3.6 +/- 1.8 E-15 fluxnum_2: 2 fluxval_2: F-LINE(5007) = 1.3 +/- 0.1 E-12 fluxnum_3: 3 fluxval_3: SURF-LINE(5007) = 2.6 +/- 0.8 E-11 fluxnum_4: 4 fluxval_4: SURF-LINE(4861) = 7.7 +/- 2.5 E-12 fluxnum_5: 5 fluxval_5: SURF-CONT(5470) = 5.4 +/- 2.7 E-14 fluxnum_6: 6 fluxval_6: W-LINE(5007) = 1.0, SIZE = 0.25 ! ! 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: ACQUIRE PN DIRECTLY. ! linenum: 2.000 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 comment_1: 1989 SENSITIVITY FIGURES IN THE comment_2: EXPOSURE AND S/N CALCULATIONS. ! linenum: 3.000 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 comment_1: 1989 SENSITIVITY FIGURES IN THE comment_2: EXPOSURE AND S/N CALCULATIONS. ! linenum: 4.000 sequence_1: DEFINE sequence_2: CALPR targname: # config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: PRISM wavelength: 5007 num_exp: 1 time_per_exp: 1S s_to_n: # fluxnum_1: 3 priority: 1 comment_1: 1989 SENSITIVITY FIGURES IN THE comment_2: EXPOSURE AND S/N CALCULATIONS ? ! linenum: 5.000 sequence_1: DEFINE sequence_2: FOS270 targname: # config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 1S s_to_n: # fluxnum_1: 3 priority: 1 comment_1: 1989 SENSITIVITY FIGURES IN THE comment_2: EXPOSURE AND S/N CALCULATIONS. ! linenum: 6.000 sequence_1: USE BINACQ targname: LMC-SMP85 time_per_exp: X17 req_1: SEQ 6-11 NO GAP; req_2: ONBOARD ACQ FOR 7-11; req_3: CYCLE 1; comment_1: EXPOSURE TIME DERIVED FROM comment_2: OPTICAL SPECTRUM AND FOS comment_3: EXPOSURE SIMULATOR. ! linenum: 7.000 targname: LMC-SMP85 config: FOS/BL opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 63S fluxnum_1: 3 priority: 1 req_1: CYCLE 1; comment_1: PICTURE REQUIRED TO RECORD comment_2: FINAL POINTING POSITION. ! linenum: 8.000 sequence_1: USE CALPR targname: LMC-SMP85 time_per_exp: X270 s_to_n: 50 req_1: CYCLE 1; ! linenum: 9.000 sequence_1: USE FOS190 targname: LMC-SMP85 time_per_exp: X270 s_to_n: 5 req_1: CYCLE 1; ! linenum: 10.000 sequence_1: USE FOS270 targname: LMC-SMP85 time_per_exp: X180 s_to_n: 5 req_1: CYCLE 1; ! linenum: 11.000 sequence_1: USE FOS130 targname: LMC-SMP85 time_per_exp: X600 s_to_n: 5 req_1: CYCLE 1; ! ! end of exposure logsheet ! No scan data records found