! $Id: 5690,v 8.1 1994/07/27 20:24:18 pepsa Exp $ coverpage: title_1: ULTRAVIOLET SPECTROSCOPY OF HYDROGEN-POOR PLANETARY NEBULAE title_2: CYCLE 4 CARRYOVER sci_cat: INTERSTELLAR MEDIUM sci_subcat: PLANETARY NEBULAE proposal_for: GO/CAR cont_id: 4226 pi_fname: PATRICK pi_lname: HARRINGTON pi_inst: UNIVERSITY OF MARYLAND, DEPT. OF ASTRONOMY, COLLEGE PARK pi_country: USA pi_phone: 301-405-6266 hours_pri: 6.96 num_pri: 2 fos: Y funds_amount: 109988 funds_length: 12 off_fname: ERICA off_lname: MARGUM off_title: MGR. RESEARCH ADM. off_inst: UNIVERSITY OF MARYLAND off_city: COLLEGE PARK off_state: MD off_zip: 20742 off_country: USA off_phone: (301) 4056266 ! end of coverpage abstract: line_1: Planetary nebulae (PNe) form in the final stages of evolution of line_2: intermediate- and low-mass stars, and show abundances consistent with line_3: contamination by modest amounts of processed material. There is however an line_4: exceptional group of PNe with nebular gas that consists of nearly undiluted line_5: products of nuclear burning. These hydrogen-poor PNe are thought to result line_6: when a final helium shell flash occurs after the complete removal of the line_7: hydrogen envelope. We propose to study 2 of the 6 currently known H-poor PNe line_8: with HST. The best studied object, Abell 30, shows that the majority of the line_9: emission line radiation is in the UV, and thus UV spectrophotometry is line_10: indispensable for quantitative analysis. Our proposed HST observations (in line_11: conjunction with our ground based work) will provide fundamental information line_12: (1) on helium-burning nucleosynthesis, by determining the ionic line_13: concentrations of H and He burning products; line_14: (2) on the physics of very dusty gas, by determining the energy balance; line_15: this is crucial since it now appears that due to the high dust-to-gas ratio, line_16: the energy input may be partially, and in some cases, primarily, due to line_17: photoelectric ejection by grains rather than by photoionization; and line_18: (3) on the interaction of the several thousand km/sec stellar winds with line_19: the nearby clumps of nebular material, by analysis of the velocity structure line_20: of the C IV 1550 line. ! ! end of abstract general_form_proposers: lname: HARRINGTON fname: PATRICK title: PI inst: UNIVERSITY OF MARYLAND, DEPT. OF ASTRONOMY, COLLEGE PARK country: USA ! lname: BORKOWSKI fname: KAZIMIERZ mi: J inst: UNIVERSITY OF MARYLAND, DEPT. OF ASTRONOMY, COLLEGE PARK country: USA ! lname: CLEGG fname: ROBIN mi: E inst: ROYAL GREENWICH OBSERVATORY, CAMBRIDGE country: UK esa: Y ! lname: TSVETANOV fname: ZLATAN inst: JOHNS HOPKINS U., DEPT. PHYSICS AND ASTRONOMY, BALTIMORE country: USA ! ! end of general_form_proposers block general_form_text: ! question: 3 section: 1 line_1: We plan to take O III images in the optical to obtain a comparable line_2: spatial resolution in this wavelength range. A comparison of optical and UV line_3: images should be interesting in view of differences in optical and UV spectra line_4: mentioned previously. The optical spectra of the two brightest emission knots line_5: in A30 (knots 3 and 4, Jacoby & Ford 1983) differ significantly. We chose these line_6: knots for UV spectroscopy with the FOS and the blue digicon. line_7: We plan to obtain UV spectra with the large 4''.3 aperture in the line_9: high-resolution mode in order to obtain a good S/N ratio and not to degrade line_10: spectral resolution excessively due to the finite extent of the knots. line_11: Positions of spectroscopic apertures in the fainter Galactic nebulae, the M22 PN line_12: were chosen on the basis of high-resolution O III images line_13: taken with the New Technology Telescope in La Silla. In both cases bright knots line_14: of emission can be seen in the east. We will take far-UV, low-resolution (G160L) line_15: FOS spectra of these knots, with the one arcsec aperture in the M22 nebula. line_16: An investigation of the stellar wind from the central star of the M22 PN, line_17: predicted theoretically to be dynamically important in the interaction line_18: of this nebula with the ISM, will be pursued by taking a high-resolution, line_19: far-UV FOS spectrum of the star through the large 4''.3 aperture. line_20: (Edited from original proposal 4226 to contain only the descriptions line_21: of the obervations that are being carried-over. Bullock) ! question: 4 section: 1 line_1: The thrust of our efforts is concentrated in the UV, and requires space line_2: observations. A30, A78, and the M22 PN were extensively studied by the IUE line_3: satellite. Multi-hour exposures of A30 (Harrington & Feibelman 1984; Harrington line_4: 1986), A78 (Kaler, Feibelman, & Henrichs 1988), and M22 (Cohen & Gillett 1989) line_5: pushed the IUE to the limits and provided us with basic information about UV line_6: properties of these objects. This information is the basis for the current line_7: proposal. Further progress can now be made only with the HST, with its superior line_8: spatial resolution and with the much larger gathering power. The two recently line_9: discovered hydrogen-poor PNe, LMC 26 and IRAS 15154-5258, can be studied only line_10: with the HST because of their relative faintness. Note that our proposal line_11: concentrates on UV spectroscopy which suffered relatively little from problems line_12: connected with the spherical aberration of the primary mirror. line_14: We have started a ground-based observational program to support this project. line_15: The high-resolution, continuum subtracted O III images of the M22 PN and IRAS line_16: 15154-5258 have been already used to locate bright emission knots to be observed line_17: by the HST. We have also obtained spectroscopic data for IRAS 15154-5258, line_18: confirming high (T > 20,000 K) electron temperature and refining the line_19: interstellar reddening. We used these data to estimate the exposure time for line_20: this object. Further observational and theoretical work in support of this line_21: project is in progress. ! question: 5 section: 1 line_1: ! question: 6 section: 1 line_1: ! ! question: 8 section: 1 line_1: ! question: 9 section: 1 line_1: No. 2266: Post-Asymptotic Giant Branch Evolution in the Magellanic Clouds, PI line_2: M.A. Dopita, P. Harrington is a Co-I. Not related beyond the fact that both deal line_3: with planetary nebulae. ! question: 10 section: 1 line_1: The Department of Astronomy of the University of Maryland has an extensive line_2: network of Sun workstations, including a number of Sparc II's, as well as a line_3: Multiflow mini-super computer. This network and supporting technical staff line_4: provides an excellent environment for data reduction and modeling. ! !end of general form text general_form_address: lname: HARRINGTON fname: PATRICK category: PI inst: UNIVERSITY OF MARYLAND, DEPT. OF ASTRONOMY city: COLLEGE PARK state: MD zip: 20742 country: USA phone: (301) 405-1517 telex: 710-826-0352 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: PK208+33D1 name_2: ABELL30 name_3: GSC1396-1621 descr_1: G,502,A,184 pos_1: PLATE-ID=03DI, pos_2: RA = 8H 46M 53.46S +/- 0.02S, pos_3: DEC = +17D 52' 45.7" +/- 0.3" equinox: 2000 rv_or_z: V = +10 comment_1: FLUXVAL_1 REFERS TO CENTRAL STAR. comment_2: LINE INFORMATION FOR EMISSION KNOTS fluxnum_1: 1 fluxval_1: V=14.30+/-0.01,TYPE=OVI,A(V)=0.90+/-0.10 fluxnum_2: 2 fluxval_2: SURF-LINE(5007) = 9 +/- 2 E-14 fluxnum_3: 3 fluxval_3: SURF-LINE(1550) = 30 +/- 5 E-15 fluxnum_4: 4 fluxval_4: W-LINE(5007) = 0.17 +/- 0.03 fluxnum_5: 5 fluxval_5: W-LINE(1550) = 1.6 +/- 0.2 fluxnum_6: 6 fluxval_6: SIZE = 0.2 fluxnum_7: 7 fluxval_7: SIZE = 0.5 ! targnum: 2 name_1: PK208+33D1-OFFSET name_2: ABELL30-CENTRAL-STAR-OFFSET name_3: GSC1396-1621-OFFSET descr_1: A,184 pos_1: PLATE-ID=03DI, pos_2: RA = 8H 46M 53.46S +/- 0.02S, pos_3: DEC = +17D 52' 45.7" +/- 0.3" equinox: 2000 rv_or_z: V = +10 fluxnum_1: 1 fluxval_1: V=14.30+/-0.01, TYPE=OVI fluxnum_2: 2 fluxval_2: B-V=-0.07+/-0.01 fluxnum_3: 3 fluxval_3: E(B-V)=0.30+/-0.03 ! targnum: 3 name_1: PK208+33D1-KNOT3 name_2: ABELL30-KNOT3 descr_1: G,502,927 pos_1: R = 6.61", pos_2: PA = 329.7D, pos_3: FROM 2 equinox: 2000 fluxnum_1: 1 fluxval_1: SURF-LINE(5007) = 10 +/- 2 E-14 fluxnum_2: 2 fluxval_2: SURF-LINE(1550) = 20 +/- 3 E-15 fluxnum_3: 3 fluxval_3: W-LINE(1550) = 1.6 +/- 0.2 fluxnum_4: 4 fluxval_4: W-LINE(5007) = 0.17 +/- 0.03 fluxnum_5: 5 fluxval_5: SURF-LINE(1909) = 30 +/- 4 E-16 fluxnum_6: 6 fluxval_6: W-LINE(1909) = 1.0 +/- 0.2 ! targnum: 4 name_1: PK208+33D1-KNOT4 name_2: ABELL30-KNOT4 descr_1: G,502,927 pos_1: R = 3.53", pos_2: PA = 221.7D, pos_3: FROM 2 equinox: 2000 fluxnum_1: 1 fluxval_1: SURF-LINE(5007) = 8 +/- 2 E-14 fluxnum_2: 2 fluxval_2: SURF-LINE(1550) = 16 +/- 3 E-15 fluxnum_3: 3 fluxval_3: W-LINE(1550) = 1.6 +/- 0.2 fluxnum_4: 4 fluxval_4: W-LINE(5007) = 0.17 +/- 0.03 fluxnum_5: 5 fluxval_5: SURF-LINE(1909) = 20 +/- 3 E-16 fluxnum_6: 6 fluxval_6: W-LINE(1909) = 1.0 +/- 0.2 fluxnum_7: 7 fluxval_7: SURF-LINE(2423) = 25 +/- 4 E-15 fluxnum_8: 8 fluxval_8: W-LINE(2423) = 0.17 +/- 0.03 ! targnum: 8 name_1: IRAS1833-2357-CENTRAL-STAR descr_1: A,184,C,201 pos_1: RA = 18H 36M 22.78S +/- 0.02S, pos_2: DEC = -23D 55' 19.26" +/- 0.3" equinox: 2000 rv_or_z: V = -153 acqpr_1: COMP comment_1: COMPANION RED STAR 1" TO NORTH fluxnum_1: 1 fluxval_1: V=14.3+/-0.2,TYPE=O fluxnum_2: 2 fluxval_2: B-V=0.5+/-0.1 fluxnum_3: 3 fluxval_3: E(B-V)=0.5+/-0.05 fluxnum_4: 4 fluxval_4: F-CONT(1550) = 45 +/- 10 E-15 ! targnum: 9 name_1: IRAS1833-2357-KNOT descr_1: G,502,927,C,201 pos_1: R = 2.3", pos_2: PA = 77D, pos_3: FROM 8 equinox: 2000 rv_or_z: V = -153 comment_1: EXPECTED FLUX. fluxnum_1: 1 fluxval_1: SURF-LINE(1550) = 80 +/- 20 E-17 fluxnum_2: 2 fluxval_2: W-LINE(1550) = 0.17 +/- 0.03 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.300 targname: PK208+33D1-OFFSET config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.05S s_to_n: 17 fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 priority: 1 req_1: CYCLE 4 /1.3-3.2; req_2: ONBOARD ACQ FOR 1.31-1.43; req_3: GROUP 1.30 - 1.43 NO GAP ! linenum: 1.310 targname: PK208+33D1-KNOT3 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H num_exp: 1 time_per_exp: 51M s_to_n: 3 fluxnum_1: 2 fluxnum_2: 3 priority: 1 ! linenum: 1.320 targname: PK208+33D1-KNOT3 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 30M s_to_n: 15 fluxnum_1: 5 fluxnum_2: 6 priority: 1 ! linenum: 1.330 targname: PK208+33D1-KNOT3 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H num_exp: 1 time_per_exp: 30M s_to_n: 15 fluxnum_1: 5 fluxnum_2: 6 priority: 1 ! linenum: 1.410 targname: PK208+33D1-KNOT4 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H num_exp: 1 time_per_exp: 51M s_to_n: 30 fluxnum_1: 2 fluxnum_2: 3 priority: 1 ! linenum: 1.420 targname: PK208+33D1-KNOT4 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 30M s_to_n: 15 fluxnum_1: 5 fluxnum_2: 6 priority: 1 ! linenum: 1.430 targname: PK208+33D1-KNOT4 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H num_exp: 1 time_per_exp: 30M s_to_n: 15 fluxnum_1: 7 fluxnum_2: 8 priority: 2 ! linenum: 3.000 targname: IRAS1833-2357-CENTRAL-STAR config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.65S s_to_n: 17 fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 priority: 1 req_1: ONBOARD ACQ FOR 3.1-3.2 comment_1: CLOSE COMPANION 1" TO NORTH. ! linenum: 3.100 targname: IRAS1833-2357-CENTRAL-STAR config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H num_exp: 1 time_per_exp: 20M s_to_n: 17 fluxnum_1: 4 priority: 2 ! linenum: 3.200 targname: IRAS1833-2357-KNOT config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G160L num_exp: 1 time_per_exp: 40M s_to_n: 5 fluxnum_1: 1 fluxnum_2: 2 priority: 1 ! ! end of exposure logsheet ! No scan data records found