! $Id: 5404,v 4.1 1994/07/27 17:35:26 pepsa Exp $ coverpage: title_1: NARROW-BAND IMAGING OF HYDROGEN-POOR PLANETARY NEBULAE title_2: CYCLE 4 HIGH sci_cat: INTERSTELLAR MEDIUM sci_subcat: PLANETARY NEBULAE proposal_for: GO pi_fname: PATRICK pi_mi: J pi_lname: HARRINGTON pi_inst: 2620 pi_country: USA pi_phone: 301-405-1517 hours_pri: 3.77 num_pri: 3 wf_pc: Y off_fname: VICTOR off_lname: MEDINA off_title: DIR RESRCH ADMN ADV. off_inst: 2620 off_addr_1: UNIVERSITY OF MARYLAND off_addr_2: LEE BUILDING off_city: COLLEGE PARK off_state: MD off_zip: 20742 off_country: USA off_phone: 301-405-6266 ! end of coverpage abstract: line_1: There is an exceptional group of PNe with nebular gas that consists of nearly line_2: undiluted products of nuclear burning. These hydrogen-poor PNe are thought to line_3: result when a final helium shell flash occurs after the complete removal of the line_4: hydrogen envelope. Four of the five currently known H-poor PNe are Cycle 2 HST line_5: spectroscopic targets. Complementary [O III] 5007 HST imaging of two nebulae line_6: has revealed remarkable `cometary' structures, consisting of compact (0".15 line_7: - 0".5) knots with radial tails several arcsec in length. We interpret this line_8: morphology in terms of dense H-poor condensations whose outer expanding layers line_9: are swept outwards by mass-loaded stellar winds. We propose narrow-band (He I, line_10: He II, and [O III]) imaging of these cometary structures in A30, and [O III] line_11: imaging of two remaining H-poor PNe where such dynamical structures are line_12: expected. These images are crucial for interpreting UV spectra of H-poor PNe. line_13: Optical imaging combined with UV data will provide fundamental information: (1) line_14: on helium-burning nucleosynthesis, by determining the ionic concentrations of line_15: H and He burning products; (2) on the interaction of the several thousand line_16: km/sec stellar winds with the nearby clumps of nebular material, resulting in line_17: mass-loaded outflows; (3) on the ram-pressure stripping of a H-poor PN in the line_18: globular cluster M22 by the interstellar medium; (4) on physics of very dusty line_19: H-poor gas, with grain photoelectrons dominating energy balance. ! ! end of abstract general_form_proposers: lname: HARRINGTON fname: PATRICK mi: J inst: 2620 country: USA esa: N ! lname: BORKOWSKI fname: KAZIMIERZ mi: J inst: 2620 country: USA esa: N ! lname: TSVETANOV fname: ZLATAN mi: I inst: 2380 country: USA esa: N ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We plan to obtain WFPC2 images in [OIII] 5007, HeII 4686 and HeI 5878 of A30 line_2: as well as [OIII] 5007 images of the M22 PN (IRAS18333-2357) and line_3: IRAS15154-5258. In all cases the central star will be placed in the center of line_4: the PC chip, so that most or even all of the inner part of the PNe is imaged line_5: at the highest possible resolution. Part of the outer structure of A30 will line_6: fall onto the WFC chips (depending upon the exact orientation). line_8: We will not use CR split since we are taking several images, which then can line_9: be combined to clean the cosmic ray events. Exposure times are set with the line_10: requirement not to saturate the central star, which will allow us to penetrate line_11: as close as possible to it. The star, however, will be numerically saturated. line_12: Long integration time is very important, since we want to achieve as high as line_13: possible signal-to-noise ratio in the spatially extended structure. ! question: 4 section: 1 line_1: Our goal is to obtain narrow-band images of H-poor PNe with the spatial line_2: resolution limited only by the HST optics. This super-resolution is essential line_3: for achieving objectives presented in the scientific justification for this line_4: proposal. The basic reason for this is the presence of small-scale structures line_5: in H-poor nebulae which are not resolved (or resolved in only one direction) line_6: in ground-based images of our targets obtained in sub-arcsecond seeing. ! question: 5 section: 1 line_1: The essense of this program is to penetrate as close as possible to the line_2: central star at the highest spatial resolution of WFPC2. Therefore, we will line_3: not use the CR-SPLIT option, and we will take instead several images in each line_4: filter, which will then be combined to clean up the cosmic ray events. The line_5: exposure times are calculated to avoid physical saturation (image "blooming") line_6: of the central stars in A30 and IRAS18333-2357. However, these two central line_7: stars will be saturated numerically. ! question: 6 section: 1 line_1: We have no special calibration requirements. ! ! question: 8 section: 1 line_1: ! question: 9 section: 1 line_1: We have been involved in the following HST projects: line_2: No. 2266: Post-Asymptotic Giant Branch Evolution in the Magellanic Clouds, PI line_3: M.A. Dopita, P. Harrington is a Co-I. Not related beyond the fact that both line_4: deal with planetary nebulae. line_5: No. 3671, 4226: Ultraviolet Spectroscopy of Hydrogen-Poor Planetary Nebulae, PI line_6: P. Harrington, K. Borkowski and Z. Tsvetanov are Co-I, cycle 2. Related. Split line_7: into two parts for technical reasons. line_8: No. 4371: FOS spectroscopy of resolved structure in the nucleus of Mrk 3. PI line_9: Tsvetanov, cycle 3. Not related to this proposal. line_10: No. 4503: Absorption line spectra of Seyfert galaxies. PI Kriss, Z.Tsvetanov line_11: is Co-I, cycle 3. Not related to this proposal. line_12: No. 4668: FOS spectroscopy of NGC1052 and NGC4258. PI Ford, Z.Tsvetanov is line_13: Co-I, cycle 3. Not related to this proposal. line_14: No. Z570: Collimated radio and ionizing radiation in NGC5252. PI Z.Tsvetanov, line_15: cycle 4. Not related to this proposal. ! question: 9 section: 2 line_1: Recent unexpected results from our HST project No.3671 prompted us to ask for line_2: high spatial resolution imaging in this proposal. This would complement our line_3: Cycle 2 HST program concentrated on UV spectroscopy, allowing us to take the line_4: full advantage of the HST capabilities in studying these unique objects. The line_5: primary objective of our Cycle 2 project is to determine the chemical line_6: abundances of H and He burning products, from C to Mg. Our complementary line_7: short (15 min) [OIII] 5007 FOC images of A30 and A78 revealed that H-poor gas line_8: is concentrated in remarkable `cometary' structures (Borkowski, Harrington, & line_9: Tsvetanov 1993, ApJ, 415, L47). Most of them consist of compact (0.15" - 0.5") line_10: knots with radial tails several arcsec in length. Both stars have energetic line_11: winds which are responsible for the knot morphology. line_12: These `cometary' structures are not visible in our UV FOC images of A30 and line_13: A78. Instead, we detected extended emission concentrated around central stars, line_14: mostly interior of the optical knots. We interpret this emission in terms of line_15: mass-loaded stellar winds, heated mostly by photoelectric emission from dust line_16: grains. line_17: We have also obtained an FOC image of LMC26, a candidate for H-poor PN in the line_18: Large Magellanic Cloud, and obtained ground-based images and spectra. An line_19: analysis of this peculiar object is in progress, but it appears that chemical line_20: abundances are those typical for LMC PNe. ! 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 X's. This network line_3: and supporting technical staff provides an excellent environment for data line_4: reduction and modeling. ! !end of general form text general_form_address: lname: HARRINGTON fname: PATRICK mi: J category: PI inst: 2620 addr_1: DEPARTMENT OF ASTRONOMY addr_2: UNIVERSITY OF MARYLAND city: COLLEGE PARK state: MD zip: 20742 country: USA phone: 301-405-1517 telex: jph@astro.umd.edu ! ! 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 pos_1: PLATE-ID=0204, 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. 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) = 1.5 +/- 0.5 E-12 fluxnum_3: 3 fluxval_3: W-LINE(5007) = 0.17 +/- 0.03 fluxnum_4: 4 fluxval_4: SURF-LINE(4686) = 2.4 +/- 1.5 E-13 fluxnum_5: 5 fluxval_5: W-LINE(4686) = 0.17 +/- 0.03 fluxnum_6: 6 fluxval_6: SURF-LINE(5878) = 8 +/- 4 E-14 fluxnum_7: 7 fluxval_7: W-LINE(5878) = 0.17 +/- 0.03 ! targnum: 2 name_1: IRAS1833-2357 descr_1: G,502 pos_1: RA = 18H 36M 22.78S +/- 0.02S, pos_2: DEC = -23D 55' 19.26" +/- 0.3", pos_3: PLATE-ID=067T equinox: 2000 rv_or_z: V = -153 comment_1: FLUXVAL_1 REFERS TO CENTRAL STAR. comment_2: LINE INFORMATION FOR EMISSION KNOTS fluxnum_1: 1 fluxval_1: V=14.3+/-0.2,TYPE=O,A(V)=1.5+/-0.15 fluxnum_2: 2 fluxval_2: SURF-LINE(5007) = 3 +/- 2 E-14 fluxnum_3: 3 fluxval_3: W-LINE(5007) = 0.17 +/- 0.03 ! targnum: 3 name_1: IRAS15154-5258 descr_1: G,502 pos_1: RA = 15H 19M 08.62S +/- 0.02S, pos_2: DEC = -53D 09' 52.2" +/- 0.3", pos_3: PLATE-ID=00H6 equinox: 2000 rv_or_z: V=0 comment_1: FLUXVAL_1 REFERS TO CENTRAL STAR. comment_2: LINE INFORMATION FOR EMISSION KNOTS fluxnum_1: 1 fluxval_1: V=16.2+/-0.2 fluxnum_2: 2 fluxval_2: SURF-LINE(5007) = 5 +/- 3 E-14 fluxnum_3: 3 fluxval_3: W-LINE(5007) = 0.17 +/- 0.03 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.100 targname: PK208+33D1 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F502N wavelength: 5007 num_exp: 4 time_per_exp: 900S s_to_n: 170 s_to_n_time: 48M fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; comment_1: FOUR [OIII]5007 IMAGES. comment_2: CENTRAL STAR WILL BE comment_3: NUMERICALLY SATURATED. ! linenum: 1.200 targname: PK208+33D1 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F469N num_exp: 4 time_per_exp: 900S fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: SAME POS FOR 1.2-1.3 AS 1.1 comment_1: FOUR HEII4686 IMAGES. comment_2: CENTRAL STAR WILL BE comment_3: NUMERICALLY SATURATED. ! linenum: 1.300 targname: PK208+33D1 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F588N num_exp: 4 time_per_exp: 500S fluxnum_1: 6 fluxnum_2: 7 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; comment_1: FOUR HEI5878 IMAGES. comment_2: CENTRAL STAR WILL BE comment_3: NUMERICALLY SATURATED. ! linenum: 2.100 targname: IRAS1833-2357 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F502N wavelength: 5007 num_exp: 4 time_per_exp: 900S s_to_n: 170 s_to_n_time: 48M fluxnum_1: 2 fluxnum_2: 3 priority: 2 param_1: CR-SPLIT=NO req_1: CYCLE 4; comment_1: FOUR [OIII]5007 IMAGES. comment_2: CENTRAL STAR WILL BE comment_3: NUMERICALLY SATURATED. ! linenum: 3.100 targname: IRAS15154-5258 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F502N num_exp: 1 time_per_exp: 2900S fluxnum_1: 2 fluxnum_2: 3 priority: 3 param_1: CR-SPLIT=DEF param_2: CR-TOLERANCE=0.1 req_1: CYCLE 4; ! ! end of exposure logsheet ! No scan data records found