! File: 3671C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:15:47:04 coverpage: title_1: ULTRAVIOLET SPECTROSCOPY OF HYDROGEN-POOR PLANETARY NEBULAE sci_cat: INTERSTELLAR MEDIUM sci_subcat: PLANETARY NEBULAE proposal_for: GO 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: 9.75 num_pri: 5 foc: Y fos: Y hrs: 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 5 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: 2 section: 1 line_1: ! question: 3 section: 1 line_1: We plan to use the FOC to image the hydrogen-poor gas in the two brightest and line_2: largest nebulae, A30 and A78. The primary goal is to obtain images in the UV, line_3: dominated by the C IV 1550 resonance line. In order to reduce the background, line_4: particularly a strong contribution from the geocoronal L-ALPHA emission, we plan line_5: to use the F152M filter. The chosen field of view is 22 arcsec squared in the line_6: FOC/96 configuration. UV images will be used later in the program to refine line_7: positions for spectroscopic work and to ease the aquisition of spectroscopic line_8: targets. We also plan to take O III images in the optical to obtain a comparable line_9: spatial resolution in this wavelength range. A comparison of optical and UV line_10: images should be interesting in view of differences in optical and UV spectra line_11: mentioned previously. line_13: The optical spectra of the two brightest emission knots in A30 (knots 3 and 4, line_14: Jacoby & Ford 1983) differ significantly. We chose these knots, as well as the line_15: bright central knot of emission in A78, for UV spectroscopy with the FOS and the line_16: blue digicon. We plan to obtain UV spectra with the large 4''.3 aperture in the line_17: high-resolution mode in order to obtain a good S/N ratio and not to degrade line_18: spectral resolution excessively due to the finite extent of the knots. We would line_19: like to reserve a choice as to the final combination of apertures and gratings line_20: upon examination of UV images. For example, bright, point-like knots of UV line_21: emission could be observed more efficiently in the lower resolution mode of the line_22: FOS. ! question: 3 section: 2 line_1: We plan to take high-resolution spectra with the GHRS to investigate broad C IV line_2: 1548, 1551 lines. We will obtain a spectrum of knot 3 in A30 centered on the CIV line_3: emission lines, in the medium-resolution mode of the GHRS and through the LSA. line_4: These lines (several independent components) are also seen in absorption in the line_5: central star of A78 - we will take a spectrum of the central star through the line_6: SSA to obtain a high quality data on these features. line_8: Positions of spectroscopic apertures in the fainter Galactic nebulae, the M22 PN line_9: and IRAS 15154-5258, were chosen on the basis of high-resolution O III images line_10: taken with the New Technology Telescope in La Silla. In both cases bright knots line_11: of emission can be seen in the east. We will take far-UV, low-resolution (G160L) line_12: FOS spectra of these knots, with the one arcsec aperture in the M22 nebula, and line_13: with the 4''.3 aperture in IRAS 15154-5258. An investigation of the stellar wind line_14: from the central star of the M22 PN, predicted theoretically to be dynamically line_15: important in the interaction of this nebula with the ISM, will be pursued by line_16: taking a high-resolution, far-UV FOS spectrum of the star through the large line_17: 4''.3 aperture. Finally, imaging in the optical and UV spectroscopy of a small, line_18: 3''.2 diameter PN in the Large Magellanic Cloud will be performed. Again, we line_19: chose the high-resolution mode of the FOS with the 4''.3 aperture for the same line_20: reasons as in A30 and A78. And again, we would like to make a final choice of line_21: apertures and gratings and of the exact position upon examination of an HST line_22: image. THE FOS OBSERVATIONS HAVE BEEN BROKEN OFF INTO PROPOSAL 4226. ! 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: We would like to obtain images with the FOC at least several weeks before line_2: spectroscopic observations of A30, A78, and the LMC PN. This would help us with line_3: the target aquisition and would be useful in refining positions, apertures, and line_4: filters for spectroscopic work. ! question: 7 section: 1 line_1: We expect to reduce the FOC images and the FOS and GHRS spectra at the line_2: University of Maryland. We have an extensive network of Sun workstations and a line_3: number of faculty with HST time, so that there should be ample local expertise line_4: in the handling of HST data. line_6: We have already obtained ground-based optical data for several of our targets, line_7: including filter images, spectra of the nebulae, and spectra of the central line_8: stars. We will continue to pursue this support work. line_10: The analysis will involve use of the photoionization modeling codes developed by line_11: J. P. Harrington for planetary nebulae, and modified in collaboration with K. line_12: Borkowski to include heating by ejection of grain photoelectrons. We have line_13: already used this code to investigate the nebular emission from the M22 object line_14: (Borkowski & Harrington 1991). The basic idea is to obtain the mass of dust and line_15: its optical depth from the far-IR (IRAS) emission, and then construct models of line_16: the photoionized gas including the heat input from the dust. UV observations of line_17: the M22 nebula with HST will establish the energy loss rate from the gas and line_18: immediately put constraints of the physics of the grain photoemission process. line_19: We will attempt to apply the same procedure to the other hydrogen-poor PNe. If line_20: we succeed in matching the UV and optical data for other objects, as well as the line_21: thermal IR fluxes, we can then feel secure in the ionization correction factors line_22: and the dust-to-gas ratio for these important objects. ! 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 = 7.2", pos_2: PA = 334D, 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 = 4.1", pos_2: PA = 229D, 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: 5 name_1: PK81-14D1 name_2: ABELL78 name_3: GSC2704-1582 descr_1: G,502,A,184 pos_1: PLATE-ID = 0054, pos_2: RA = 21H 35M 29.39S +/- 0.02S, pos_3: DEC = +31D 41' 46.0" +/- 0.3" equinox: 2000 rv_or_z: V = +17 comment_1: FLUXVAL_1 REFERS TO CENTRAL STAR. comment_2: FLUXVAL_2 FOR BRIGHTEST KNOTS. fluxnum_1: 1 fluxval_1: V=13.25+/-0.01,TYPE=OVI,A(V)=0.46+/-0.10 fluxnum_2: 2 fluxval_2: SURF-LINE(5007) = 4 +/- 1 E-14 fluxnum_3: 3 fluxval_3: SURF-LINE(1550) = 14 +/- 4 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: 6 name_1: PK81-14D1-CENTRAL-STAR name_2: ABELL78-CENTRAL-STAR name_3: GSC2704-1582 descr_1: A,184 pos_1: PLATE-ID = 0054, pos_2: RA = 21H 35M 29.39S +/- 0.02S, pos_3: DEC = +31D 41' 46.0" +/- 0.3" equinox: 2000 rv_or_z: V = +17 fluxnum_1: 1 fluxval_1: V=13.25+/-0.01,TYPE=OVI fluxnum_2: 2 fluxval_2: B-V=-0.21+/-0.01 fluxnum_3: 3 fluxval_3: E(B-V)=0.15+/-0.03 fluxnum_4: 4 fluxval_4: F-CONT(1550) = 12 +/- 1 E-13 ! targnum: 7 name_1: PK81-14D1-KNOT name_2: ABELL78-KNOT descr_1: G,502,927 pos_1: R = 4", pos_2: PA = 340D, pos_3: FROM 6 equinox: 2000 fluxnum_1: 1 fluxval_1: SURF-LINE(1550) = 14 +/- 4 E-15 fluxnum_2: 2 fluxval_2: W-LINE(1550) = 1.6 +/- 0.2 fluxnum_3: 3 fluxval_3: SURF-LINE(1909) = 18 +/- 4 E-16 fluxnum_4: 4 fluxval_4: W-LINE(1909) = 1.0 +/- 0.2 fluxnum_5: 5 fluxval_5: SURF-LINE(2423) = 20 +/- 4 E-15 fluxnum_6: 6 fluxval_6: 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 ! targnum: 10 name_1: IRAS15154-5258-OFFSET descr_1: A pos_1: RA = 15H 19M 8.19S +/- 1.0", pos_2: DEC = -53D 9' 47.1" +/- 1.0" equinox: J2000 fluxnum_1: 1 fluxval_1: V=16.2+/-0.2 ! targnum: 11 name_1: IRAS15154-5258-KNOT descr_1: G,502,927 pos_1: RA-OFF = +0.848S +/- 0.022S, pos_2: DEC-OFF = +5.5" +/- 0.2", pos_3: FROM 10 equinox: 2000 comment_1: EXPECTED FLUXES. fluxnum_1: 1 fluxval_1: SURF-LINE(1550) = 60 +/- 15 E-17 fluxnum_2: 2 fluxval_2: W-LINE(1550) = 0.17 +/- 0.03 ! targnum: 12 name_1: LMC26 descr_1: G,502,A,184 pos_1: RA = 5H 20M 0.75S +/- 0.2S, pos_2: DEC = -69D 26' 0.0" +/- 3" equinox: 2000 fluxnum_1: 1 fluxval_1: V=17.9+/-0.2,TYPE=B6V,A(V)=0.5+/-0.1 fluxnum_2: 2 fluxval_2: SURF-LINE(5007) = 37 +/- 5 E-15 fluxnum_3: 3 fluxval_3: W-LINE(5007) = 0.17 +/- 0.03 fluxnum_4: 4 fluxval_4: SIZE=0.2 ! targnum: 13 name_1: LMC26-OFFSET descr_1: A,184 pos_1: RA = 5H 20M 0.75S +/- 0.2S, pos_2: DEC = -69D 26' 0.0" +/- 3" equinox: 2000 acqpr_1: COMP comment_1: LOCATION OF KNOT AND OF OFFSET STAR comment_2: WILL BE DETERMINED FROM FOC IMAGE fluxnum_1: 1 fluxval_1: V=17.9+/-0.2 fluxnum_2: 2 fluxval_2: TYPE=B6V fluxnum_3: 3 fluxval_3: A(V)=0.5+/-0.1 ! targnum: 14 name_1: LMC26-KNOT descr_1: G,502,927 pos_1: R = 1", pos_2: PA = 0D, pos_3: FROM 13 equinox: 2000 comment_1: LOCATION OF KNOT AND OF OFFSET STAR comment_2: WILL BE DETERMINED FROM FOC IMAGE comment_3: EXPECTED FLUXES. fluxnum_1: 1 fluxval_1: SURF-LINE(1550) = 6 +/- 1 E-16 fluxnum_2: 2 fluxval_2: W-LINE(1550) = 1.6 +/- 0.2 fluxnum_3: 3 fluxval_3: SURF-LINE(1909) = 30 +/- 6 E-17 fluxnum_4: 4 fluxval_4: W-LINE(1909) = 1.0 +/- 0.2 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.100 targname: PK208+33D1 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F152M num_exp: 1 time_per_exp: 30M s_to_n: 5 fluxnum_1: 3 fluxnum_2: 7 priority: 1 param_1: PIXEL=50X25 req_1: CYCLE 2 ! linenum: 1.200 targname: PK208+33D1 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F501N num_exp: 1 time_per_exp: 15M s_to_n: 5 fluxnum_1: 2 fluxnum_2: 4 fluxnum_3: 6 priority: 3 param_1: PIXEL=50X25 req_1: CYCLE 2 ! linenum: 2.010 targname: PK81-14D1 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F152M num_exp: 1 time_per_exp: 30M s_to_n: 5 fluxnum_1: 3 fluxnum_2: 7 priority: 1 param_1: PIXEL=50X25 req_1: CYCLE 2 ! linenum: 2.020 targname: PK81-14D1 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F501N num_exp: 1 time_per_exp: 15M s_to_n: 5 fluxnum_1: 2 fluxnum_2: 4 fluxnum_3: 6 priority: 3 param_1: PIXEL=50X25 req_1: CYCLE 2 ! linenum: 5.000 targname: LMC26 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F501N num_exp: 1 time_per_exp: 15M s_to_n: 5 fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: PIXEL=50X25 req_1: CYCLE 2 ! ! end of exposure logsheet ! No scan data records found