! File: 2290C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:04:44:20 coverpage: title_1: CHEMICAL ABUNDANCES IN LOCAL GROUP SUPERNOVA REMNANTS sci_cat: INTERSTELLAR MEDIUM sci_subcat: SN & SNR proposal_for: GO 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_2: ASTROPHYSICS:EVOLUTION,STELLAR POPULATION,ABUNDANCE, hours_pri: 8.00 num_pri: 4 fos: Y pi_position: SENIOR FELLOW off_mi: R. off_lname: RODGERS off_title: DIRECTOR off_inst: MT. STROMLO AND SIDING SPRING OBSERVATORY 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: There is an increasing body of data, based on abundance line_2: analyses of the interstellar medium, which suggests that Local line_3: Group disk galaxies have had a star-formation history which is line_4: quite different from the region of the Galaxy about the sun. For line_5: example, the solar region appears to have undergone a burst of line_6: high-mass star formation at the time of disk collapse, unlike line_7: Local Group systems of low metallicity. line_8: The evolved, radiative supernova remnants (SNR) can be used line_9: as a powerful probe of the chemical abundances in the line_10: Interstellar Medium (ISM). This proposal is to obtain FOS UV line_11: spectrophotometry of the brightest radiative SNR discovered by line_13: us in Local Group Galaxies. This data will complement our line_14: ground-based data in the optical to give abundances of a variety line_15: of elements with different nucleogenic origins. The data to be line_16: obtained in the LMC will complement the abundance analysis of line_17: the spectra of many supergiant stars, already performed, to give line_18: us a complete picture of the "cosmic" abundances of most ! ! end of abstract general_form_proposers: lname: TUOHY fname: IAN title: DR mi: R inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES country: AUSTRALIA ! lname: MATHEWSON fname: DONALD title: PROF mi: S inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES country: AUSTRALIA ! lname: RUSSELL fname: STEPHEN title: DR mi: C inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES country: AUSTRALIA ! lname: BENVENUTI fname: PIERO title: DR inst: SPACE TELESCOPE COORDINATING FACILITY esa: Y ! lname: DANZIGER fname: JOHN title: DR mi: I inst: EUROPEAN SOUTHERN OBSERVATORY esa: Y ! lname: D'ODORICO fname: SANDRO title: DR inst: EUROPEAN SOUTHERN OBSERVATORY esa: Y ! lname: MATTEUCCI fname: FRANCESCA title: DR inst: EUROPEAN SOUTHERN OBSERVATORY esa: Y ! lname: CHEVALIER fname: ROGER title: DR inst: UNIVERSITY OF VIRGINIA country: USA ! lname: DOPITA fname: MICHAEL title: DR mi: A. inst: MT. STROMLO AND SIDING SPRING OBSERVATORIES country: AUSTRALIA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We are proposing to obtain FOS spectra (between 1500 and line_2: 2332 angstroms) of radiative SNR in several nearby galaxies. A line_3: signal to noise of 4 per angstrom in the continuum is sought. A line_4: total of eight SNR in four galaxies have been targetted. Of these, line_5: three are in each of the LMC and M33, and are broadly line_6: distributed across the face of their parent galaxy. Whilst available line_7: data leads us to expect that abundance gradients across the line_8: LMC are negligible, an appreciable abundance gradient exists in line_9: M33. Thus, in this case, we should be able to assess the line_10: variability in relative chemical yields as a function of position in line_11: the galaxy. For the massive precursor stars of these Type II SNR, line_12: it is possible that pre-supernova mass-loss allows a certain line_13: enrichment of the surrounding ISM in nitrogen. The data line_14: obtained in the LMC will allow us to check out this possibility. line_15: Furthermore, this data will be complemented by the fine line_16: analysis of the spectra of many Supergiant stars in these line_17: galaxies (Russell and Bessell 1988). ! question: 3 section: 2 line_1: The LMC SNR; N49 and a single SNR in M33 has been line_2: targetted by the GTO proposal #1048. This data is not of limited line_3: utility to our program, since the exposure times are too short to line_4: allow an accurate determination of the equivalent widths of lines line_5: against the two-photon continuum, which is a prime objective of line_6: our proposal. Nevertheless, we have avoided selecting these line_7: objects for this proposal. line_8: The remaining dwarf Magellanic galaxy; IC1613 and the line_9: late-type spirals NGC300 and M33 cover a metallicity range line_10: from about 1 : 30 solar (1 : 4 SMC) up to about 1: 2 solar. line_11: We therefore cover a wide range of chemical evolutionary stages, line_12: and therefore expect to be able to reach meaningful conclusions line_13: about the dependence of IMF and star formation history on the line_14: galaxian environment. ! question: 4 section: 0 line_1: Although valiant attempts have been made to use IUE, this line_2: satellite lacks the sensitivity and resolution to carry through the line_3: sort of program we are proposing. The results that have been line_4: obtained are interesting, but not definitive. We have obtained line_5: exhausive spectrophotometry in the optical, but the interpretation line_6: of this data remains ambiguous until UV data for important line_7: coolants such as C, N, O and Si have been obtained. line_8: It is vital for a program that we measure the equivalent widths of line_9: the lines against the nebular continuum, which arises principally line_10: from the two-photon continuum of hydrogen. By this method, we line_11: propose to eliminate the considerable errors resulting from line_12: assumed reddening and uncertainties in the form of the line_13: extinction law for the particular galaxy (it is well-known that the line_14: form of the reddening law is strongly dependent on metallicity line_15: and on the local environment). Only the FOS on the HST line_16: has the sensitivity and dynamic range for this purpose. ! question: 5 section: 1 line_1: Our program, covering five objects in three galaxies, is line_2: configured to sample the brightest radiative SNR, and to cover line_3: the widest possible range of metallicity. Our exposure times line_4: have been chosen so as to allow measurement of the nebular line_5: continuum to < 3% in bins of 100 angstroms. Since this nebular line_6: continuum is strongly dominated by the collisionally-enhanced line_7: two-photon continuum of Hydrogen (D'Odorico et.al. 1980), the line_8: equivialent widths of the emission lines can be used to derive line_9: the absolute intensity of these lines with respect to H-beta. This line_10: has the great advantage that neither the reddening curve, nor line_11: the absolute value of the reddening need be accurately known. line_12: In the 1200-2000 band, the integrated flux in the continuum line_13: and in the emission lines is expected to be about equal. line_14: The continuum fluxes at 1650 have been computed on the line_15: basis of the observed H-beta flux, the observed extinction and line_16: using theoretical models. IC 1613 was assumed to have an line_17: SMC-like extinction law and the other galaxies an LMC-like law. line_18: Using the Newsletter sensitivity figures, the FOS counts / second line_19: / angstrom, N, the effextive no. of angstroms transmitted by the line_20: aperture used, Aap, and the flux at 1650, F1650,, are related by: line_21: log(N) = 13.59 +log(F1650) +log(Aap). This formula represents the line_22: basis of the exposure time calculations, which aim to give a line_23: mean signal / noise of 3 per angstrom, or 30 per 100 angstrom. ! question: 6 section: 0 line_1: Since we require to measure a very faint continuum, line_2: these targets would benefit from dark time. ! question: 7 section: 0 line_1: The MSSSO investigators will have the prime responsibility for line_2: the analysis phase of the HST observations. It is anticipated line_3: that the reduction of the raw data will be performed at STScI, line_4: however, we have installed the IRAF system at MSSSO, line_5: so that local analysis is possible. line_6: Analysis of calibrated HST data will be undertaken at MSSSO line_7: where the hardware environment (network of Vax 11/780, line_8: MicroVax computers and Sun Workstations with a variety of line_9: image and spectral reduction packages) is more than adequate line_10: for this task. line_11: The chemical abundances will be derived at MSSSO, using line_12: theoretical modelling based on the code MAPPINGS developed line_13: by Dopita and his collaborators. For this purpose, the FOS data line_15: will be combined with optical data in the range 3300 - 10000 line_16: angstroms, to give a complete table of reddening-corrected line line_17: intensities with respect to H-beta. line_18: The interpretation and theoretical modelling of the results in line_19: terms of galactic evolution theory, and the subsequent line_20: preparation of papers will be the joint responsibility of the team. line_21: Communications are to be maintained by e-mail, telephone and line_22: by overseas travel as necessary. ! question: 10 section: 0 line_1: The manpower, fiscal and hardware resources necessary to line_2: carry through the reduction and interpretation of the data will be line_3: supplied within the internal budget of MSSSO as necessary. line_4: Funding will also be available to support any short overseas line_5: visits that may be necessary to coordinate team members' line_6: activities. Similar facilities and arrangements will also be put line_7: in hand at ESA. ! !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 zip: 2606 country: AUSTRALIA phone: (011 61) 62 49-0212 telex: AA 62270 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: IC1613-S8 name_2: SA8 descr_1: ISM; SNR IN IC1613 pos_1: RA = 01H 02M 28.3S +/- 0.1S, pos_2: DEC = +01D 52' 36" +/- 1" equinox: 1950.0 rv_or_z: V=250 acqpr_1: EXT fluxnum_1: 1 fluxval_1: SURF-LINE(4861) = 6.0 +/- 1.5 E-15 fluxnum_2: 2 fluxval_2: SURF-CONT(1650) = 9.0 +/- 4.0 E-17 fluxnum_3: 3 fluxval_3: SURF-CONT(5500) = 1.5 +/- 1.0 E-13 fluxnum_4: 4 fluxval_4: W-LINE(4861) = 1.0, SIZE = 4.5 ! targnum: 2 name_1: M33-DBB6 name_2: 013040+30269 descr_1: ISM; SNR IN M33 pos_1: RA = 01H 30M 40.0S +/- 0.1S, pos_2: DEC = 30D 26' 55" +/- 1" equinox: 1950.0 rv_or_z: V=250 acqpr_1: EXT fluxnum_1: 1 fluxval_1: SURF-LINE(4861) = 2.5 +/- 0.5 E-15 fluxnum_2: 2 fluxval_2: SURF-CONT(1650) = 5.0 +/- 2.0 E-17 fluxnum_3: 3 fluxval_3: SURF-CONT(5500) = 6.0 +/- 4.0 E-14 fluxnum_4: 4 fluxval_4: W-LINE(4861) = 1.0, SIZE = 4.0 ! targnum: 4 name_1: LMC-N103B descr_1: SUPERNOVA REMNANT IN LMC pos_1: RA = 05H 09M 13.0S +/- 0.1S, pos_2: DEC = -68D 47' 15" +/- 1" equinox: 1950.0 rv_or_z: V=250 acqpr_1: EXT fluxnum_1: 1 fluxval_1: SURF-LINE(4861) = 3.0 +/- 1.0 E-15 fluxnum_2: 2 fluxval_2: SURF-CONT(1650) = 5.4 +/- 2.5 E-17 fluxnum_3: 3 fluxval_3: SURF-CONT(5500) = 8.0 +/- 4.0 E-14 fluxnum_4: 4 fluxval_4: W-LINE(4861) = 1.0, SIZE = 4.5 ! targnum: 5 name_1: LMC-N63A descr_1: SUPERNOVA REMNANT IN LMC pos_1: RA = 05H 35M 38.4S +/- 0.1S, pos_2: DEC = -66D 03' 46.4" +/- 1" equinox: 1950.0 rv_or_z: V=250 acqpr_1: EXT fluxnum_1: 1 fluxval_1: SURF-LINE(4861) = 2.6 +/- 1.0 E-15 fluxnum_2: 2 fluxval_2: SURF-CONT(1650) = 5.0 +/- 2.5 E-17 fluxnum_3: 3 fluxval_3: SURF-CONT(5500) = 6.0 +/- 3.0 E-14 fluxnum_4: 4 fluxval_4: W-LINE(4861) = 1.0, SIZE = 14.0 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: GETOBJ targname: # config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: # time_per_exp: 1S s_to_n: 17 fluxnum_1: 3 priority: # param_1: TYPE = UP, param_2: SEARCH-SIZE = 4, param_3: SCAN-STEP = 1 comment_1: USED FOR PEAKUP ON MILDLY comment_2: EXTENDED SNRS. comment_3: FLUXNUM-3, ESTIMATED TOTAL FLUX comment_4: FOR THE OBJECT (LINES +CONT). ! linenum: 3.000 sequence_1: DEFINE sequence_2: FOS130 targname: # config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1300 num_exp: # time_per_exp: 1S s_to_n: # fluxnum_1: 2 priority: # comment_1: LATEST SENSITIVITY FIGURES USED comment_2: FOR EXPOSURE AND S/N CALCS. ! linenum: 4.000 sequence_1: DEFINE sequence_2: FOS190 targname: # config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1900 num_exp: # time_per_exp: 1S s_to_n: # fluxnum_1: 2 priority: # comment_1: LATEST SENSITIVITY FIGURES USED comment_2: FOR EXPOSURE AND S/N CALCS. ! linenum: 5.000 sequence_1: DEFINE sequence_2: FOSCAL targname: # config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: PRISM wavelength: 5007 num_exp: # time_per_exp: 1S s_to_n: # fluxnum_1: 1 priority: # comment_1: LATEST SENSITIVITY FIGURES USED comment_2: FOR EXPOSURE AND S/N CALCS. ! linenum: 10.000 sequence_1: USE GETOBJ targname: IC1613-S8 num_exp: 1 time_per_exp: X30 priority: 2 req_1: SEQ 10 - 13 NO GAP; req_2: ONBOARD ACQ FOR 11 - 13; req_3: CYCLE 1; req_4: DARK TIME / 10-53 ! linenum: 11.000 sequence_1: USE FOSCAL targname: IC1613-S8 num_exp: 2 time_per_exp: X1100 s_to_n: 40 s_to_n_time: 2200S priority: 2 req_1: CYCLE 1 ! linenum: 12.000 sequence_1: USE FOS190 targname: IC1613-S8 num_exp: 2 time_per_exp: X1100 s_to_n: 5 s_to_n_time: 2200S priority: 2 req_1: CYCLE 1 ! linenum: 13.000 sequence_1: USE FOS130 targname: IC1613-S8 num_exp: 2 time_per_exp: X2000 s_to_n: 4 s_to_n_time: 3600S priority: 2 req_1: CYCLE 1 ! linenum: 20.000 sequence_1: USE GETOBJ targname: M33-DBB6 num_exp: 1 time_per_exp: X40 priority: 4 req_1: SEQ 20 - 23 NO GAP; req_2: ONBOARD ACQ FOR 21 - 23; req_3: CYCLE 1 ! linenum: 21.000 sequence_1: USE FOSCAL targname: M33-DBB6 num_exp: 2 time_per_exp: X1200 s_to_n: 30 s_to_n_time: 2400S priority: 4 req_1: CYCLE 1 ! linenum: 22.000 sequence_1: USE FOS190 targname: M33-DBB6 num_exp: 2 time_per_exp: X1200 s_to_n: 4 s_to_n_time: 2400S priority: 4 req_1: CYCLE 1 ! linenum: 23.000 sequence_1: USE FOS130 targname: M33-DBB6 num_exp: 2 time_per_exp: X2000 s_to_n: 4 s_to_n_time: 3000S priority: 4 req_1: CYCLE 1 ! linenum: 40.000 sequence_1: USE GETOBJ targname: LMC-N103B num_exp: 1 time_per_exp: X10 priority: 2 req_1: SEQ 40 - 43 NO GAP; req_2: ONBOARD ACQ FOR 41 - 43; req_3: CYCLE 1 ! linenum: 41.000 sequence_1: USE FOSCAL targname: LMC-N103B num_exp: 2 time_per_exp: X1200 s_to_n: 30 priority: 2 req_1: CYCLE 1 ! linenum: 42.000 sequence_1: USE FOS190 targname: LMC-N103B num_exp: 2 time_per_exp: X1200 s_to_n: 4 priority: 2 req_1: CYCLE 1 ! linenum: 43.000 sequence_1: USE FOS130 targname: LMC-N103B num_exp: 2 time_per_exp: X1700 s_to_n: 4 s_to_n_time: 3000S priority: 2 req_1: CYCLE 1 ! linenum: 51.000 sequence_1: USE FOSCAL targname: LMC-N63A num_exp: 1 time_per_exp: X2000 s_to_n: 30 priority: 1 req_1: SEQ 51 - 53 NO GAP; req_2: CYCLE 1 comment_1: NO ACQ EXPOSURE NEEDED SINCE TARGET comment_2: IS 20 ARCSEC ACROSS. ! linenum: 52.000 sequence_1: USE FOS190 targname: LMC-N63A num_exp: 1 time_per_exp: X2000 s_to_n: 4 priority: 1 req_1: CYCLE 1 ! linenum: 53.000 sequence_1: USE FOS130 targname: LMC-N63A num_exp: 2 time_per_exp: X1750 s_to_n: 4 priority: 1 req_1: CYCLE 1 ! ! end of exposure logsheet ! No scan data records found