! $Id: 5403,v 4.1 1994/07/27 17:34:59 pepsa Exp $ coverpage: title_1: X-RAY EMITTING 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: 5.39 num_pri: 2 wf_pc: Y time_crit: 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: The ROSAT X-ray satellite detected for the first time hot, X-ray emitting gas line_2: from from a number of planetary nebulae (PNe). This hot gas is produced in line_3: the dynamical interaction of fast stellar winds with the nebular gas. The line_4: interaction is poorly understood -- PN dynamical models had failed to predict line_5: X-ray emission from PNe. The most plausible hypothesis for the presence of line_6: X-ray emission involves stellar wind interactions with inhomogeneous media, line_7: leading to mass-loaded outflows. Because mass-loaded outflows are important line_8: in a broad astrophysical context, further studies of X-ray emitting PNe are line_9: warranted. We propose to study mass-loaded outflows in two optically bright, line_10: X-ray emitting PNe, NGC6543 and BD+30 3639, through WFPC2 imaging with a line_11: complete set of narrow-band filters. High quality, good signal-to-noise images line_12: would provide spectral (through image ratios) information on small angular line_13: scales where mass-loading and associated interface phenomena occur. We expect line_14: to find radiative shocks, cometary structures, bow-shocks and wind-blown line_15: tails, as suggested by numerous ground-based studies and our recent HST line_16: observations. Information on these small-scale structures is essential for line_17: X-ray emission modeling, and for understanding mass-loaded flows. ! ! 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 ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We propose to image both NGC 6543 and BD+30 with the WFPC2 using the full set of line_2: narrow filters (excluding the \[Ne V\] and He II filters, since these lines have line_3: not been detected in these low-ionization PNe). Thus we would employ 10 filters line_4: which cover \[OII\] 3727, \[OIII\] 4363, Hbeta, \[OIII\] 5007, HeI 5876, \[OI\] line_5: 6300, Halpha, \[NII\] 6584, \[SII\] 6731, and \[SIII\] 9532. The ratios of these line_6: lines will provide many diagnostics: temperature through \[OIII\] 4363/5007; line_7: ionization state through \[OII\]/\[OIII\], \[OI\]/\[OII\], \[SII\]/\[SIII\] and line_8: HeI/Halpha; shock excitation through Halpha/Hbeta and \[SII\]/Halpha; possible line_9: abundance anomalies through \[NII\]/Halpha. Altogether we will have a wealth of line_10: information for comparison with predictions of ionization, shock, and conduction line_11: front models. Such diagnostics require, however, a higher S/N ratio than simple line_12: morphology. line_13: Since NGC 6543 is bright, we need to consider possible saturation of the pixels line_14: in the strongest lines. If the features are very compact, this is a concern. line_15: From the VLA radio map with 0.3" resolution (Balick, Bignell, et al. 1987) we line_16: find that the peak flux/arcsec is 0.015 times the total flux. If we apply this line_17: factor to the strongest line, \[OIII\] 5007, with a total flux of 1.6 x 10^-9 line_18: ergs/cm^2/s, we find a peak electron detection rate of 22 e^-/s/pixel in the PC line_19: camera. We would then reach numerical saturation (30000 e^-) in 23 minutes. (The line_20: count rate is 4 times greater in the WF camera pixels, but they will be line_21: observing the faint halo.) The weakest line is \[OIII\] 4363, which may produce line_22: a count rate 10^-3 that of 5007. This line is very important, as the ratio with line_23: \[OIII\] 5007 will allow to map the temperature in the more highly ionized gas. ! question: 3 section: 2 line_1: A similar estimate for BD+30 shows that the strongest line in this object, line_2: \[NII\] 6584, could saturate in 11 minutes. line_4: The central stars of both objects will saturate quickly and "bloom" along a few line_5: columns of pixels. For NGC 6543, the 11.1 mag star will yield 2600 e^-/sec, or line_6: 1.6 x 10^6 e^- for a 10 min exposure. This is still less than the few 10^7 e^- line_7: needed to bleed to adjacent columns. The loss of a few columns to blooming is line_8: not serious. line_9: We will take all WFPC2 images with the central star at the center of the PC line_10: array. This will provide the highest resolution and cover all of BD+30 and the line_11: whole inner complex of NGC 6543. In the case of the later object, the more line_12: sensitive WF arrays will record most of the halo. line_13: Altogether, we will take 10 exposures of NGC 6543 and 9 of BD+30. We omit line_14: \[OIII\] 4363 from BD+30 as it is likely to be too faint for good S/N. ! question: 4 section: 1 line_1: Both NGC 6543 and BD+30 3639 have been extensively observed to the limit of line_2: ground-based resolution. They are among the best observed PNe, and further line_3: ground-based work would be unlikely to be very useful. line_5: We want to clarify the process by which these objects produce X-ray emission. line_6: The leading candidate is mass-loading of the stellar wind, and our experience line_7: with A 30 and A 78 indicates that the morphological features characteristic of line_8: this process only emerge when we have images with sub-arcsecond resolution. line_9: Other phenomena which may be involved, shock and/or conduction fronts, will be line_10: intrinsically very narrow, and the highest resolution is needed to pick out the line_11: characteristic spectral features from the background of photoionized gas. ! question: 5 section: 1 line_1: We would like to request a special orientation of the WFPC2 for NGC 6543. This line_2: request should not significantly restrict scheduling for this object for two line_3: reasons: (1) our requirement is to place one of the WF cameras to the west of line_4: the central core, and (2) NGC 6543 is located close to the North Ecliptic Pole, line_5: and hence in the Continuous Viewing Zone. In order to prevent creating a `hole' line_6: in the west, we would like to exclude position angles for the U3 axis from line_7: 210 to 330D. We defined this requirement by specifying ORIENT 90D +/- 120D for line_8: all exposures of NGC 6543. The scientific justification for this restriction is line_9: as follows: the core of NGC 6543 is surrounded by a much fainter, highly line_10: filamentary halo 165 arcsec in radius. Most of this halo can be imaged by the line_11: WF camera when the PC observes the core, but a particularly bright halo line_12: condensation is located in the west. The halo is of great interest. line_13: Middlemass, Clegg, and Walsh (1989) found that the halo temperatures are line_14: higher than the core temperature by an amount that requires a non-radiative line_15: energy source. This discovery was possible with ground-based resolution line_16: because in the faint halo, non-photoionization heating is not swamped by line_17: intense emission from the photoionized gas. Middlemass et al. (1991) showed line_18: that shocks driven into the outer filaments by the (mass-loaded? Dyson 1992) line_19: stellar wind would explain the heating. The radiative shocks proposed by line_20: Middlemass et al. (1991) are a little over 1 arcsec in thickness. HST line_21: observations might well resolve their structure. ! question: 6 section: 1 line_1: ! ! question: 8 section: 1 line_1: ! question: 9 section: 1 line_1: We have been involved in the following HST projects: line_3: No. 2266: Post-Asymptotic Giant Branch Evolution in the Magellanic Clouds, PI line_4: M.A. Dopita, P. Harrington is a Co-I. Not related beyond the fact that both line_5: deal with planetary nebulae. line_7: No. 3671, 4226: Ultraviolet Spectroscopy of Hydrogen-Poor Planetary Nebulae, PI line_8: P. Harrington, K. Borkowski is a Co-I, cycle 2. Split into two parts for line_9: technical reasons. Some relation, in that the cometary structures found in this line_10: proposal demonstrate the power of HST imaging to elucidate wind-nebular line_11: interactions. line_13: Our complementary short (15 min) \[OIII\] 5007 FOC images of A30 and A78 line_14: revealed that H-poor gas is concentrated in remarkable ``cometary'' structures line_15: (Borkowski et al. 1993). Most of them consist of compact line_16: (0.15" -- 0.5") knots with radial tails several arcsec in length. Both stars line_17: have energetic winds which are responsible for the knot morphology. These line_18: ``cometary'' structures are not visible in our UV FOC images of A30 and A78. line_19: Instead, we detected extended emission concentrated around central stars, line_20: mostly interior of the optical knots. We interpret this emission in terms of line_21: mass-loaded stellar winds, heated mostly by photoelectric emission from dust line_22: grains. ! 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 and line_3: supporting technical staff provides an excellent environment for data reduction line_4: 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 ! lname: category: CON ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC6543 name_2: PK96+29D1 name_3: GSC4212-508 descr_1: G,502 pos_1: PLATE-ID=00T0, pos_2: RA = 17H 58M 33.29S +/- 0.07S, pos_3: DEC = +66D 37' 58.9" +/- 1.0" equinox: 2000 rv_or_z: V = -66 comment_1: FLUXVAL_1 REFERS TO CENTRAL STAR. comment_2: THIS IS A CVZ TARGET. comment_3: SURF-LINE(6731) = 2.4 +/- 0.48 E-12 comment_4: SURF-LINE(9532) = 1.1 +/- 0.22 E-11 comment_5: W-LINE(ALL) = 0.17 +/- 0.03 comment_6: FLUXES ARE LOWER LIMITS FOR comment_7: BRIGHTEST NEBULAR REGIONS. fluxnum_1: 1 fluxval_1: V=11.23+/-0.1,TYPE=OF/WR,A(V)=0.0+/-0.15 fluxnum_2: 2 fluxval_2: SURF-LINE(3728) = 5.2 +/- 1.0 E-12 fluxnum_3: 3 fluxval_3: W-LINE(3728) = 0.17 +/- 0.03 fluxnum_4: 4 fluxval_4: SURF-LINE(4363) = 3.9 +/- 0.78 E-13 fluxnum_5: 5 fluxval_5: SURF-LINE(4861) = 2.2 +/- 0.44 E-11 fluxnum_6: 6 fluxval_6: SURF-LINE(5007) = 1.4 +/- 0.29 E-10 fluxnum_7: 7 fluxval_7: SURF-LINE(5876) = 3.5 +/- 0.70 E-12 fluxnum_8: 8 fluxval_8: SURF-LINE(6300) = 2.0 +/- 0.39 E-13 fluxnum_9: 9 fluxval_9: SURF-LINE(6563) = 6.7 +/- 1.4 E-11 fluxnum_10: 10 fluxval_10: SURF-LINE(6584) = 5.2 +/- 1.0 E-12 ! targnum: 2 name_1: PK64+5D1 name_2: BD+30D3639 name_3: GSC2655-4032 descr_1: G,502 pos_1: PLATE-ID=000J, pos_2: RA = 19H 34M 45.25S +/- 0.07S, pos_3: DEC = +30D 30' 59.3" +/- 1.0" equinox: 2000 rv_or_z: V = -66 comment_1: FLUXVAL_1 REFERS TO CENTRAL STAR. comment_2: SURF-LINE(9532) = 4.5 +/- 0.89 E-11 comment_3: W-LINE(ALL) = 0.17 +/- 0.03 comment_4: FLUXES ARE LOWER LIMITS TO comment_5: BRIGHTEST NEBULAR REGIONS. fluxnum_1: 1 fluxval_1: V=12.50+/-0.10,TYPE=WR,A(V)=1.26+/-0.09 fluxnum_2: 2 fluxval_2: SURF-LINE(3728) = 1.5 +/- 0.30 E-11 fluxnum_3: 3 fluxval_3: W-LINE(3728) = 0.17 +/- 0.03 fluxnum_4: 4 fluxval_4: SURF-LINE(4861) = 2.4 +/- 0.47 E-11 fluxnum_5: 5 fluxval_5: SURF-LINE(5007) = 9.4 +/- 1.9 E-13 fluxnum_6: 6 fluxval_6: SURF-LINE(5876) = 1.5 +/- 0.30 E-12 fluxnum_7: 7 fluxval_7: SURF-LINE(6300) = 7.8 +/- 1.6 E-13 fluxnum_8: 8 fluxval_8: SURF-LINE(6563) = 9.4 +/- 1.9 E-11 fluxnum_9: 9 fluxval_9: SURF-LINE(6584) = 1.1 +/- 0.22 E-10 fluxnum_10: 10 fluxval_10: SURF-LINE(6731) = 6.1 +/- 1.2 E-12 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: NGC6543 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F375N num_exp: 1 time_per_exp: 1800S s_to_n: 5 fluxnum_1: 2 fluxnum_2: 3 priority: 2 req_1: CYCLE 4; req_2: ORIENT 90D +/- 120D / 1.0-1.9 ! linenum: 1.100 targname: NGC6543 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F437N num_exp: 1 time_per_exp: 2400S s_to_n: 3 fluxnum_1: 4 fluxnum_2: 3 priority: 1 req_1: CYCLE 4; req_2: SAME POS FOR 1.100-1.900 AS 1.00 ! linenum: 1.200 targname: NGC6543 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F487N num_exp: 1 time_per_exp: 1400S s_to_n: 23 fluxnum_1: 5 fluxnum_2: 3 priority: 1 req_1: CYCLE 4; ! linenum: 1.300 targname: NGC6543 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F502N num_exp: 2 time_per_exp: 800S s_to_n: 60 s_to_n_time: 1200S fluxnum_1: 6 fluxnum_2: 3 priority: 1 param_1: CR-SPLIT=0.25 param_2: CR-TOLERANCE=0.0 req_1: CYCLE 4; ! linenum: 1.400 targname: NGC6543 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F588N num_exp: 1 time_per_exp: 1000S s_to_n: 14 fluxnum_1: 7 fluxnum_2: 3 priority: 3 req_1: CYCLE 4; ! linenum: 1.500 targname: NGC6543 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F631N num_exp: 1 time_per_exp: 1800S s_to_n: 5 fluxnum_1: 8 fluxnum_2: 3 priority: 3 req_1: CYCLE 4; ! linenum: 1.600 targname: NGC6543 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F656N num_exp: 1 time_per_exp: 800S s_to_n: 60 fluxnum_1: 9 fluxnum_2: 3 priority: 1 param_1: CR-SPLIT=0.25 param_2: CR-TOLERANCE=0.0 req_1: CYCLE 4; ! linenum: 1.700 targname: NGC6543 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F658N num_exp: 1 time_per_exp: 1000S s_to_n: 18 fluxnum_1: 10 fluxnum_2: 3 priority: 2 req_1: CYCLE 4; ! linenum: 1.800 targname: NGC6543 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F673N num_exp: 1 time_per_exp: 800S s_to_n: 12 fluxnum_1: 10 fluxnum_2: 3 priority: 2 req_1: CYCLE 4; ! linenum: 1.900 targname: NGC6543 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F953N num_exp: 1 time_per_exp: 800S s_to_n: 12 fluxnum_1: 10 fluxnum_2: 3 priority: 3 req_1: CYCLE 4; ! linenum: 2.000 targname: PK64+5D1 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F375N num_exp: 1 time_per_exp: 600S s_to_n: 5 fluxnum_1: 2 fluxnum_2: 3 priority: 2 req_1: CYCLE 4; ! linenum: 2.200 targname: PK64+5D1 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F487N num_exp: 1 time_per_exp: 600S s_to_n: 17 fluxnum_1: 4 fluxnum_2: 3 priority: 1 req_1: CYCLE 4; req_2: SAME POS FOR 2.20-2.900 AS 2.00 ! linenum: 2.300 targname: PK64+5D1 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F502N num_exp: 1 time_per_exp: 600S s_to_n: 6 fluxnum_1: 5 fluxnum_2: 3 priority: 1 req_1: CYCLE 4; ! linenum: 2.400 targname: PK64+5D1 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F588N num_exp: 1 time_per_exp: 600S s_to_n: 8 fluxnum_1: 6 fluxnum_2: 3 priority: 3 req_1: CYCLE 4; ! linenum: 2.500 targname: PK64+5D1 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F631N num_exp: 1 time_per_exp: 1000S s_to_n: 8 fluxnum_1: 7 fluxnum_2: 3 priority: 3 req_1: CYCLE 4; ! linenum: 2.600 targname: PK64+5D1 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F656N num_exp: 1 time_per_exp: 500S s_to_n: 55 fluxnum_1: 8 fluxnum_2: 3 priority: 1 param_1: CR-SPLIT=0.4 param_2: CR-TOLERANCE=0.0 req_1: CYCLE 4; ! linenum: 2.700 targname: PK64+5D1 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F658N num_exp: 1 time_per_exp: 500S s_to_n: 65 fluxnum_1: 9 fluxnum_2: 3 priority: 2 param_1: CR-SPLIT=0.4 param_2: CR-TOLERANCE=0.0 req_1: CYCLE 4; ! linenum: 2.800 targname: PK64+5D1 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F673N num_exp: 1 time_per_exp: 800S s_to_n: 18 fluxnum_1: 10 fluxnum_2: 3 priority: 2 req_1: CYCLE 4; ! linenum: 2.900 targname: PK64+5D1 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F953N num_exp: 1 time_per_exp: 800S s_to_n: 26 fluxnum_1: 10 fluxnum_2: 3 priority: 3 req_1: CYCLE 4; ! ! end of exposure logsheet ! No scan data records found