! File: 4940C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:11:24:23 coverpage: title_1: POST ASYMPTOTIC GIANT BRANCH EVOLUTION IN THE MAGELLANIC CLOUDS - title_2: IMAGING: 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: 4.51 num_pri: 7 wf_pc: 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: 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 3 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 3 UV Spectrophotometry: We are undertaking in Cycle 3 line_11: FOS spectrophotometry in the range 1150 - 3200 Angstroms using the line_12: G130H and G190H gratings, and the PRISM. These observations are described line_13: more fully in a separate proposal. The Cycle 3 imaging program needs to be line_14: executed first to determine the individual FOS acquisition methods. line_15: References: line_16: Jacoby, G., 1980, Ap. J. Suppl. Ser.,42, p. 1 line_17: Wood, P.R., Bessell, M.S., and Dopita, M.A., 1986, Ap. J.,311, p. 632 line_18: Wood, P.R., Meatheringham, S.J., Dopita, M.A., and Morgan, D.H., 1987, line_19: Ap. J., 320, p. 178 ! question: 3 section: 2 line_1: ###### The program ID which uses these early acq's for follow up line_2: spectroscopy is 4566. ! 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. 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. These observations are essential in determining the method line_11: of acquistion to be used in the subsequent Cycle 3 FOS observations. line_12: Our HST program is supported by a comprehensive and continuing line_13: ground-based program. We have used the 1-metre, 2.3-metre and line_14: 3.9-metre telescopes at Siding Spring to measure fluxes, sizes, line_15: expansion velocities, radial velocities and nebular spectra from 3200 line_16: to 10000 Angstroms. These observations already provide an excellent line_17: set of homogeneous and high-quality data which gives the best possible line_18: ground-based characteristics of the Magellanic Cloud population of PN. line_19: this data set will allow us to extend our population classifications line_20: from the HST subset to the entire population of PN in the Magellanic line_21: Clouds. line_22: References: line_23: 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. This is an EARLY ACQ proposal line_7: and needs to be executed sufficiently early for the FOS spectroscopy to be line_8: completed before the end of Cycle 3. line_10: ###### Proposal to later use these early acq's for spectroscopy is 4566. ! question: 6 section: 1 line_1: The PC exposures have been arranged in SEQUENCE, where a PSF exposure line_2: will be executed at the beginning, the middle, and the end of this sequence. line_3: From attempts at deconvolution of Cycle 1 PC images, this arrangement line_4: of PSF exposures should aid us in deconvolving the Cycle 3 PC images. ! 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. One object remains to be observed from this program: two attempts line_3: to observe this final object have failed due to Guide Star acquistion line_4: failures. All completed observations are currently being deconvolved. line_5: The completed Cycle 1 images have also been analysed to determine the best line_6: FOS acquisition method in Cycle 2. The Cycle 2 observations are currently line_7: being scheduled. ! 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 comment_6: A MORE ACCURATE POSITION OF PN comment_7: MAY BE DETERMINED FROM PC IMAGE 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: 102 name_1: LMC-SMP7 name_2: N177F descr_1: H,502 pos_1: RA = 04H 48M 29.64S +/- 0.02S, pos_2: DEC = -69D 08' 13.24" +/- 0.1" equinox: 2000.0 rv_or_z: V = 220 fluxnum_1: 1 fluxval_1: F-CONT(1650) = 7.6 +/- 0.8 E-16 fluxnum_2: 2 fluxval_2: F-LINE(1666) = 4.5 +/- 0.6 E-14 fluxnum_3: 3 fluxval_3: F-LINE(5007) = 8.9 +/- 0.1 E-13 fluxnum_4: 4 fluxval_4: SURF-LINE(5007) = 9.3 +/- 1.0 E-13 fluxnum_5: 5 fluxval_5: W-LINE(5007) = 1.0, SIZE = 1.1 ! targnum: 103 name_1: LMC-SMP37 name_2: N28 descr_1: H,502 pos_1: RA = 05H 11M 03.00S +/- 0.02S, pos_2: DEC = -67D 47' 59.55" +/- 0.1" equinox: 2000.0 rv_or_z: V = 270 fluxnum_1: 1 fluxval_1: F-CONT(1650) = 1.9 +/- 0.8 E-15 fluxnum_2: 2 fluxval_2: F-LINE(1666) = 7.8 +/- 0.6 E-14 fluxnum_3: 3 fluxval_3: F-LINE(5007) = 1.6 +/- 0.1 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(5007) = 1.3 +/- 1.0 E-11 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 ! targnum: 107 name_1: LMC-PSF-STAR descr_1: H,704 pos_1: RA = 05H 40M 34.45S +/- 0.02S, pos_2: DEC = -66D 17' 23.11" +/- 0.1" equinox: 2000.0 fluxnum_1: 1 fluxval_1: V = 13.1 +/- 0.4 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: PCEXP targname: # config: PC opmode: IMAGE aperture: # sp_element: # num_exp: 1 time_per_exp: 1S s_to_n: # fluxnum_1: # priority: 1 param_1: READ = YES, param_2: CR-SPLIT = DEF, param_3: PRE-FLASH = YES req_1: CYCLE 3 / 1.0-16.5 comment_1: ALL SUBSEQENT PC EXPOSURES ARE comment_2: EARLY ACQ FOR FOS OBSERVATIONS comment_3: TO FOLLOW IN CYCLE 3, PROPOSAL comment_4: ID 4566. ! linenum: 2.000 sequence_1: DEFINE sequence_2: PCMEX targname: # config: PC opmode: IMAGE aperture: # sp_element: # num_exp: 1 time_per_exp: 1S s_to_n: # fluxnum_1: # priority: 1 param_1: READ = YES, param_2: CR-SPLIT = DEF, param_3: PRE-FLASH = YES ! linenum: 10.500 sequence_1: USE PCMEX targname: LMC-PSF-STAR aperture: PC6 sp_element: F502N time_per_exp: X800 s_to_n: 130 fluxnum_1: 1 req_1: NON-INT; comment_1: OBSERVATION OF CALIBRATION comment_2: STAR TO OBTAIN LOCAL PSF. comment_3: BEGIN SEQUENCE OF PC EXPOSURES comment_4: TO LATER AID FOS ACQUISITIONS. ! linenum: 11.000 sequence_1: USE PCEXP targname: SMC-SMP22 aperture: PC6 sp_element: F502N time_per_exp: X400 s_to_n: 15 fluxnum_1: 3 req_1: NON-INT ! linenum: 12.000 sequence_1: USE PCEXP targname: LMC-SMP7 aperture: PC6 sp_element: F502N time_per_exp: X800 s_to_n: 15 fluxnum_1: 3 req_1: NON-INT ! linenum: 13.000 sequence_1: USE PCEXP targname: LMC-SMP37 aperture: PC6 sp_element: F502N time_per_exp: X100 s_to_n: 15 fluxnum_1: 3 req_1: NON-INT ! linenum: 13.500 sequence_1: USE PCMEX targname: LMC-PSF-STAR aperture: PC6 sp_element: F502N time_per_exp: X800 s_to_n: 130 fluxnum_1: 1 req_1: NON-INT comment_1: OBSERVATION OF CALIBRATION comment_2: STAR TO OBTAIN LOCAL PSF. ! linenum: 14.000 sequence_1: USE PCEXP targname: LMC-SMP61 aperture: PC6 sp_element: F502N time_per_exp: X180 s_to_n: 15 fluxnum_1: 3 req_1: NON-INT ! linenum: 15.000 sequence_1: USE PCEXP targname: LMC-SMP67 aperture: PC6 sp_element: F502N time_per_exp: X500 s_to_n: 15 fluxnum_1: 3 req_1: NON-INT ! linenum: 16.000 sequence_1: USE PCEXP targname: LMC-SMP101 aperture: PC6 sp_element: F502N time_per_exp: X700 s_to_n: 15 fluxnum_1: 3 req_1: NON-INT ! linenum: 16.500 sequence_1: USE PCMEX targname: LMC-PSF-STAR aperture: PC6 sp_element: F502N time_per_exp: X800 s_to_n: 130 fluxnum_1: 1 req_1: NON-INT comment_1: OBSERVATION OF CALIBRATION comment_2: STAR TO OBTAIN LOCAL PSF. ! ! end of exposure logsheet ! No scan data records found