! $Id: 5340,v 4.1 1994/08/02 18:40:25 pepsa Exp $ coverpage: title_1: LINE ABSORPTION DUE TO EJECTED NEBULA OF AN OLD NOVA sci_cat: INTERSTELLAR MEDIUM sci_subcat: NOVAE proposal_for: GO pi_fname: MICHAEL pi_lname: FRIEDJUNG pi_inst: INSTITUT D'ASTROPHYSIQUE, PARIS (CNRS) pi_country: FRANCE pi_phone: 33 1 43 20 14 25 hours_pri: 3.00 num_pri: 1 hrs: Y off_fname: ALAIN off_lname: OMONT off_title: DR off_inst: 5436 off_addr_1: INSTITUT D'ASTROPHYSIQUE off_addr_2: 98 BIS BOULEVARD ARAGO off_city: PARIS off_zip: 75014 off_country: FRANCE off_phone: 33 1 43 20 14 25 ! end of coverpage abstract: line_1: We plan to use the GHRS to observe ultra violet absorption lines with line_2: lower level excitation potentials at zero electron volts, produced by line_3: the nebula ejected by the old nova V603 Aql (1918). This old nova is line_4: very bright, while the line of sight to the central remnant seems to line_5: pass through or near the density maximum of the nebula, which is line_6: called a "polar cap". Following the repair of the HST it will be line_7: possible to obtain good line profiles. Analysis of them will give line_8: information about the velocity field of the nebula along the line line_9: of sight to the central remnant and from this about the nebular line_10: thickness. Limits to the column densities of different ions will line_11: be obtainable and when combined with ground based and IUE fluxes as line_12: well as with ionization calculations, will give conditions about line_13: relative element abundances. In addition we shall also be able to line_14: determine characteristics of a possible wind from an accretion line_15: disk, if present around the white dwarf component of the binary line_16: system. ! ! end of abstract general_form_proposers: lname: FRIEDJUNG fname: MICHAEL inst: 5436 country: FRANCE esa: Y ! lname: BIANCHINI fname: ANTONIO inst: 6470 country: ITALY esa: Y ! lname: CASSATELLA fname: ANGELO inst: 6406 country: ITALY esa: Y ! lname: SELVELLI fname: PIERLUIGI inst: 6440 country: ITALY esa: Y ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The proposal involves GHRS observations of the old nova V603 Aql in 3 line_2: spectral regions, using the G160 grating and the small science line_3: aperture. The spectral regions are centred near 1540 A (CIV), 1390 A line_4: (Si IV) and 1240 A (NV), the aim being to observe absorption components line_5: produced by the ejected envelope of the nova. The ejected nebula is line_6: much larger than either aperture (diameter of the order of 2 minutes line_7: arc), but the small science aperture will help to eliminate traces of line_8: it as much as possible, as well as providing better line profiles. line_9: We wish to have a signal to noise ratio of the order of 20/1, so as to line_10: be able to detect and measure weak features and obtain good line line_11: profiles. Onboard acquisition in the ACCUMULATION mode is very line_12: suitable. The exposure of each region has been broken down into short line_13: subexposures, so as to minimize long exposure problems. In view of line_14: the time alocated, we shall especially concentrate on obtaining this line_15: signal to noise ratio for the C IV region, as there is a very good line_16: chance of at least seeing the C IV doublet in absorption. Estimates of line_17: exposure times needed are based on IUE fluxes, combined with table line_18: 7.4.1 of the GHRS post COSTAR handbook large aperture sensitivities, line_19: multiplied by 2/3. ! question: 4 section: 1 line_1: The proposed observations are in the ultraviolet spectral domain, line_2: which is unaccesible from the ground. Though V603 Aql is the only line_3: old classical nova to have been observed at high spectral resolution line_4: with IUE, the signal to noise ratio was too low to do what is line_5: proposed. Note that the presence of CIV absorption was inspite of line_6: this suspected by one of us (P.L. Selvelli) in the IUE results. In line_7: addition the resolution of IUE is lower than that obtainable with line_8: the proposed grating of the GHRS. ! question: 5 section: 1 line_1: No special requirements. ! question: 6 section: 1 line_1: None. ! ! question: 8 section: 1 line_1: We intend to organize ourselves the acquisition of ground based line_2: observations of images of the nebula and spectra of the central line_3: object. These do not need to be exactly simultanious, as changes of line_4: the nebula should be slow. ! question: 9 section: 1 line_1: All present investigators were involved in a previous version of line_2: this proposal with a slightly different title, having the same PI, line_3: made for cycle 1 "Absorption lines due to ejected nebula of an old line_4: nova (no. 2345). line_5: Cycle 1 proposal no. 2345 was accepted with supplemental priority line_6: in 1989. Following the discovery of spherical aberration it was re- line_7: examined in 1991 and still only given supplemental priority. The line_8: repair of the HST should enable this similar programme to be carried line_9: out correctly. ! question: 10 section: 1 line_1: Funds are supplied by the french "Institut National des Sciences line_2: de l'Univers". ! !end of general form text general_form_address: lname: FRIEDJUNG fname: MICHAEL category: PI inst: 5436 addr_1: INSTITUT D'ASTROPHYSIQUE (CNRS) addr_2: 98 BIS BOULEVARD ARAGO city: PARIS zip: 75014 country: FRANCE phone: 33 1 43 20 14 25 telex: INTERNET FRIEDJUNG@IAP.FR FAX 33 1 43 29 86 73 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD174107 name_2: V603-AQL name_3: GSC448-423 descr_1: A,150,161,926 pos_1: PLATE-ID = 050T, pos_2: RA = 18H 48M 54.611S +/-0.2", pos_3: DEC = +00D 35' 2.95" +/-0.2" equinox: 2000 pos_epoch_bj: B pos_epoch_yr: 1984.00 an_prlx_val: 0.0030 an_prlx_unct: 0.0015 rv_or_z: V = -23 fluxnum_1: 1 fluxval_1: V=11.7 +/- 0.2 fluxnum_2: 2 fluxval_2: B-V=0.0 +/- 0.1 fluxnum_3: 3 fluxval_3: E(B-V)=0.1 fluxnum_4: 4 fluxval_4: F-CONT(1541)= 6 +/-2 E-13 fluxnum_5: 5 fluxval_5: F-CONT(1235)= 6 +/-2 E-13 fluxnum_6: 6 fluxval_6: F-CONT(1391)= 7 +/-2 E-13 fluxnum_7: 7 fluxval_7: F-CONT(2500)= 2.0 +/-0.5 E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HD174107 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 3.6S fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 fluxnum_4: 7 priority: 1 param_1: SEARCH-SIZE=3 param_2: BRIGHT=RETURN param_3: LOCATE=YES req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 2 comment_1: ONBOARD ACQUISITION OF FAIRLY BRIGHT comment_2: STAR WITH NORMAL 3X3 SEARCH. comment_3: STEP-TIME IS 0.4SEC comment_4: COUNT RATE IS 50000 CNTS/SEC ! linenum: 2.000 targname: HD174107 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 10.0S priority: 1 param_1: SEARCH-SIZE=5 req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 3-5 comment_1: PEAKUP IN SSA FOR LINES 3-5 comment_2: STEP-TIME IS 0.4SEC ! linenum: 3.000 targname: HD174107 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1541 num_exp: 1 time_per_exp: 44M s_to_n: 20 s_to_n_time: 44M fluxnum_1: 4 priority: 1 param_1: FP-SPLIT=FOUR param_2: COMB=FOUR param_3: STEP-PATT=5 param_4: DOPPLER=ON req_1: CYCLE 4 comment_1: OBTAIN 4 FP-SPLIT SPECTRA WITH A comment_2: TOTAL S/N NEAR 20 ! linenum: 4.000 targname: HD174107 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1235 num_exp: 1 time_per_exp: 42M s_to_n: 20 s_to_n_time: 42M fluxnum_1: 5 priority: 2 param_1: FP-SPLIT=FOUR param_2: COMB=FOUR param_3: STEP-PATT=5 param_4: DOPPLER=ON req_1: CYCLE 4 comment_1: OBTAIN 4 FP-SPLIT SPECTRA WITH A comment_2: TOTAL S/N OF ORDER OF 20 ! linenum: 5.000 targname: HD174107 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1391 num_exp: 1 time_per_exp: 32M s_to_n: 20 s_to_n_time: 32M fluxnum_1: 6 priority: 3 param_1: FP-SPLIT=FOUR param_2: COMB=FOUR param_3: STEP-PATT=5 param_4: DOPPLER=ON req_1: CYCLE 4 comment_1: OBTAIN 4 FP-SPLIT SPECTRA WITH A comment_2: TOTAL S/N OF ORDER OF 20 ! ! end of exposure logsheet ! No scan data records found