! $Id: 5638,v 8.1 1994/07/27 19:58:51 pepsa Exp $ coverpage: title_1: HIGH RESOLUTION OBSERVATIONS OF title_2: NOVA CYG 92 Cycle 4 sci_cat: INTERSTELLAR MEDIUM sci_subcat: SUBLUMINOUS STARS proposal_for: GO/DD longterm: 3 pi_fname: BOB pi_lname: WILLIAMS pi_inst: SPACE TELESCOPE SCIENCE INSTITUTE pi_country: USA pi_phone: 410-338-4710 keywords_1: NOVAE, SHELLS hours_pri: 10.06 num_pri: 10 TIME_CRIT: X ! end of coverpage abstract: line_1: We propose to obtain low resolution spectra of the shell line_2: around Nova Cyg/92 in order to determine element abundances line_3: and the nature of the ejecta. FOS spectra will provide line line_4: fluxes and give information on the kinematics of the shell, line_5: and the FOC will be used with a prism to acquire line_6: monochromatic images of the ejecta so surface brightnesses line_7: can be determined in the various emission lines. Because of line_8: HST's aperture and the FOS UV sensitivity we plan to line_9: concentrate on the weaker emission lines that are not line_10: normally detected in novae ejecta in order to determine line_11: abundances for as many post-neon elements as possible. We line_12: also plan to determine the extent to which there are line_13: dense condensations in the shell, and their influence in line_14: dictating the ionization and providing for dust formation. ! ! end of abstract general_form_proposers: lname: WILLIAMS fname: BOB inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA esa: N ! lname: PANAGIA fname: NINO inst: ESA, SPACE TELESCOPE SCIENCE INSTITUTE country: USA esa: X ! lname: HACK fname: WARREN inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: PARESCE fname: FRANCESCO inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA esa: X ! lname: LIVIO fname: MARIO inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: We propose here to obtain low dispersion spectra of Nova line_2: Cyg/92, which is a member of the relatively new class of line_3: "neon" novae, in the light of various emission lines for line_4: the purpose of an abundance analysis. The spectra will be line_5: obtained with the FOS. It line_6: will be used to obtain low resolution (150 km/sec) spectra line_7: from two of the higher surface brightness regions of the line_8: nova shell over the extended wavelength interval from line_9: Ly-alpha to H-alpha. These data should result in the line_10: detection of numerous faint lines which are important for line_11: the abundance analysis. HST is especially important for line_12: this purpose since many of the lines of the post-Ne line_13: elements such as Mg, Si, and Al occur in the UV, and we line_14: will attempt to study these lines in several distinct line_15: regions of the nova shell. question: 2 section: 2 line_1: line_2: Once the spectra have been obtained and reduced, we will line_3: use the emission line fluxes to determine physical line_4: conditions in the ejecta. Two methods will be explored to line_5: accomplish this: one using a pre-existing code such as line_6: CLOUDY to model the ionization based on parameters which line_7: can be determined from certain line ratios, and another line_8: which is more semi-empirical in nature but which takes line_9: density inhomogeneities into account better than line_10: photoionization codes such as CLOUDY. An outline for the line_11: latter approach has been given in a recent paper by one of line_12: us (ApJ, 392, 99, 1992), and the analysis of Nova Cyg/92 line_13: will afford us the opportunity of refining this new line_14: method. question: 2 section: 3 line_1: The major goals of this project are thus to (1) acquire low line_2: dispersion UV and visible spectra of the HST-resolved line_3: ejecta of Nova Cyg/92, (2) determine emission line fluxes line_4: in different regions of the shell, and (3) model the ejecta line_5: to determine abundances and physical conditions, and deduce line_6: the fundamental properties of the outburst that led to the line_7: present conditions. ! question: 3 section: 1 line_1: The FOS will be used to obtain a complete medium- line_2: resolution spectrum of the entire system, from 1150 - 7000 line_3: Angstroms. A binary search in the 4.3" aperture will locate line_4: the star for more precise centering in the smallest 0.3" line_5: circular aperture. A series of spectra will then be taken of line_6: the entire system using the high resolutions gratings from line_7: G190H to G570H on the RED side. line_8: An offset will then take place to position the star outside line_9: the aperture to obtain the same series of spectra for the line_10: nebulosity only. The same procedure will then be used for line_11: the G130H grating on the Blue side to get the far-UV line_12: spectra of the star and nebula. question: 13 section: 1 line_1: It is proposed to explore at high spatial and moderate line_2: spectral resolution the circumstellar shell around line_3: Nova Cyg 1992. !end of general form text general_form_address: lname: WILLIAMS fname: BOB category: PI inst: SPACE TELESCOPE SCIENCE INSTITUTE addr_1: 3700 San Martin Drive city: BALTIMORE state: MD zip: 21218 country: USA ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NOVACYG1992 descr_1: A,150 pos_1: RA = 20H 30M 31.64S +/-0.3S, pos_2: DEC = 52D 37' 51.3" +/-0.3", pos_3: PLATE-ID=003I equinox: 2000 pm_or_par: NO fluxnum_1: 1 fluxval_1: V=12.4+/-0.1, fluxval_2: F-CONT(2600)=1.5 +/- 0.5 E-14 ! ! end of fixed targets ! No solar system records found exposure_logsheet: linenum: 1.000 targname: NOVACYG1992 config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2600-3000 num_exp: 1 time_per_exp: 11S priority: 1 param_1: SEARCH-SIZE-X=1, param_2: SEARCH-SIZE-Y=3, param_3: SCAN-STEP-Y=1.23 req_1: ONBOARD ACQ FOR 2; req_2: CYCLE 4/1.000-105.10; req_4: AT 18-AUG-1994 +/- 14D; comment_3: This ACQ procedure provides a position comment_4: accuracy of only +/- 1 diode in X, or comment_5: +/- 2 A in the dispersion direction. ! linenum: 2.000 targname: NOVACYG1992 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2600-3000 num_exp: 1 time_per_exp: 12S priority: 1 param_1: SEARCH-SIZE-X=6, param_2: SEARCH-SIZE-Y=2, param_3: SCAN-STEP-X=0.61, param_4: SCAN-STEP-Y=0.61 req_1: ONBOARD ACQ FOR 3 ! linenum: 3.000 targname: NOVACYG1992 config: FOS/RD opmode: ACQ/PEAK aperture: 2.0-BAR sp_element: G270H wavelength: 2600-3000 num_exp: 1 time_per_exp: 13S priority: 1 param_1: TYPE=DOWN, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=5, param_4: SCAN-STEP-Y=0.26 req_1: ONBOARD ACQ FOR 4 ! linenum: 4.000 targname: NOVACYG1992 config: FOS/RD opmode: ACQ/PEAK aperture: 2.0-BAR sp_element: G270H wavelength: 2600-3000 num_exp: 1 time_per_exp: 65S priority: 1 param_1: TYPE=DOWN, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=7, param_4: SCAN-STEP-Y=0.05 req_1: ONBOARD ACQ FOR 5.0-5.5 ! linenum: 5.000 targname: NOVACYG1992 config: FOS/RD opmode: ACCUM aperture: 2.0-BAR sp_element: G400H time_per_exp: 600S priority: 1 s_to_n: 30 comment_1: This S/N is for the continuum. ! linenum: 5.100 targname: NOVACYG1992 config: FOS/RD opmode: ACCUM aperture: 2.0-BAR sp_element: G570H time_per_exp: 600S priority: 1 s_to_n: 30 comment_1: This S/N is for the continuum. ! linenum: 5.200 targname: NOVACYG1992 config: FOS/RD opmode: ACCUM aperture: 2.0-BAR sp_element: G190H time_per_exp: 3600S priority: 1 s_to_n: 30 comment_1: This S/N is for the continuum. ! linenum: 5.300 targname: NOVACYG1992 config: FOS/RD opmode: ACCUM aperture: 2.0-BAR sp_element: G270H time_per_exp: 900S priority: 1 s_to_n: 30 comment_1: This S/N is for the continuum. ! linenum: 5.400 targname: NOVACYG1992 config: FOS/RD opmode: ACCUM aperture: 2.0-BAR sp_element: G780H time_per_exp: 1800S priority: 1 s_to_n: 30 comment_1: This S/N is for the continuum. ! linenum: 5.500 targname: NOVACYG1992 config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR time_per_exp: 128S priority: 1 comment_1: This will provide details on position comment_2: of the bar relative to the nebula. ! linenum: 101.000 targname: NOVACYG1992 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2600-3000 num_exp: 1 time_per_exp: 15S priority: 1 param_1: SEARCH-SIZE-X=1, param_2: SEARCH-SIZE-Y=3, param_3: SCAN-STEP-Y=1.23 req_1: ONBOARD ACQ FOR 102; req_2: AT 18-AUG-1994 +/- 14D; comment_3: This ACQ procedure provides a position comment_4: accuracy of only +/- 1 diode in X, or comment_5: +/- 2 A in the dispersion direction. ! linenum: 102.000 targname: NOVACYG1992 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2600-3000 num_exp: 1 time_per_exp: 17S priority: 1 param_1: SEARCH-SIZE-X=6, param_2: SEARCH-SIZE-Y=2, param_3: SCAN-STEP-X=0.61, param_4: SCAN-STEP-Y=0.61 req_1: ONBOARD ACQ FOR 103 ! linenum: 103.000 targname: NOVACYG1992 config: FOS/BL opmode: ACQ/PEAK aperture: 2.0-BAR sp_element: G270H wavelength: 2600-3000 num_exp: 1 time_per_exp: 19S priority: 1 param_1: TYPE=DOWN, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=5, param_4: SCAN-STEP-Y=0.26 req_1: ONBOARD ACQ FOR 104 ! linenum: 104.000 targname: NOVACYG1992 config: FOS/BL opmode: ACQ/PEAK aperture: 2.0-BAR sp_element: G270H wavelength: 2600-3000 num_exp: 1 time_per_exp: 94S priority: 1 param_1: TYPE=DOWN, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=7, param_4: SCAN-STEP-Y=0.05 req_1: ONBOARD ACQ FOR 105.000 ! linenum: 105.000 targname: NOVACYG1992 config: FOS/BL opmode: ACCUM aperture: 2.0-BAR sp_element: G130H time_per_exp: 145M priority: 1 s_to_n: 15 comment_1: This S/N is for the continuum. ! linenum: 105.100 targname: NOVACYG1992 config: FOS/BL opmode: ACQ aperture: 4.3 sp_element: MIRROR time_per_exp: 128S priority: 1 comment_1: This will provide details on position comment_2: of the bar relative to the nebula. ! ! end of exposure logsheet