! $Id: 5367,v 6.1 1994/07/27 17:09:31 pepsa Exp $ coverpage: title_1: "SUB--ARCSECOND STRUCTURE OF OPTICAL JETS AND ITS ORIGIN" sci_cat: INTERSTELLAR MEDIUM sci_subcat: HERBIG-HARO OBJECTS proposal_for: GO pi_fname: JOHN pi_lname: RAYMOND pi_inst: 2166 pi_country: USA pi_phone: 617-495-7416 hours_pri: 3.50 num_pri: 1 wf_pc: Y off_fname: IRWIN off_lname: SHAPIRO off_title: DIRECTOR off_inst: 2166 off_city: CAMBRIDGE off_state: MA off_zip: 02138 off_country: USA off_phone: 617-495-7100 ! end of coverpage abstract: line_1: Direct narrow band images of the jet-like HH 32 (Herbig-Haro) object line_2: taken with the Wide Field and Planetary Camera 2 will be used to test line_3: predictions from theoretical models. We propose to take advantage of line_4: the high sensitivity and high angular resolution provided by this camera line_5: to resolve the detailed morphology of the knots along the body of the line_6: jet in emission lines of different excitation. Both the characteristics line_7: of individual knots (e.g., excitation, positions, spacings, and sizes line_8: along and across the outflow axis measured in the three emission lines) line_9: and possible trends of these characteristics as a function of distance line_10: from the source will provide a new and unique insight on the origin of line_11: the knotty structure. This will help to discriminate among a wide range line_12: of proposed theoretical possibilities, through detailed comparisons line_13: between the observational results and analytic and numerical models line_14: which we have developed in the recent past. ! ! end of abstract general_form_proposers: lname: RAYMOND fname: JOHN inst: 2166 country: USA ! lname: CURIEL fname: SALVADOR inst: 2166 country: USA ! lname: RAGA fname: ALEJANDRO inst: 8046 country: UK ! lname: NORIEGA-CRESPO fname: ALBERTO inst: 3760 country: USA ! lname: BIRO fname: SUSANA inst: 8046 country: UK ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We request time to observe one optical jet (HH 32) line_2: using the WFPC2 camera. This camera provides a field of view and line_3: resolution that will allow us to study in detail the morphology of line_4: individual knots, and at the same time to cover the main body of the line_5: jet in single frames, including a number of stars that can be used to line_6: align the images. Halpha, [S II] and [N II] narrow band images will line_7: be obtained for each object. A broad band continuum image will also be line_8: obtained for this jet, which will be used to subtract the continuum line_9: emission from the line images. Since the bright portions of this line_10: jet is only ~30''long, only four images will be needed line_11: to study the knotty structure along the main body. ! question: 4 section: 1 line_1: Recent observational results have shown that under conditions of line_2: excellent seeing (~0.6''-0.8'' FWHM) and using line_3: deconvolution techniques, angular resolutions of about line_4: 0.4''-0.6'' can be reached with ground-based observations. line_5: However, this extraordinary resolution is not enough to properly line_6: resolve most of the knots on optical jets (with sizes between ~0.3'' line_7: and 0.8''), which is necessary in order to establish their nature. line_8: The mapping of optical jets in the light of several lines line_9: with an angular resolution of ~0.1'', can provide detailed line_10: information of individual knots (e.g., morphologies, ionization line_11: gradients, and offsets between the knot positions line_12: in different emission lines) that can be directly compared with line_13: predictions from numerical simulations. line_14: At present, this angular resolution can only be achieved with the HST. line_15: The HST provides an angular resolution that is better by at least a line_16: factor of four compared to ground-based observations. ! question: 4 section: 2 line_1: Single Halpha, [S II] 6717+31 and [N II] 6583 narrow band, and line_2: broad band continuum images will be obtained for the HH 32 jet. line_3: The bright knots in this jet have fluxes of about 15, 30 and 15 line_4: times 10^{-14} erg cm^{-2} s^{-1} (same units hereafter) for line_5: Halpha, [S II] and [N II] (Hartigan etal. 1986, AJ, 91, 1357) line_6: respectively, with typical sizes of 1 arcsec^2. line_7: On the other hand, the fainter structures that we want to study have line_8: fluxes of about 0.2 for the same three lines. The required sensitivity line_9: per pixel for this jet can be achieved in about 4000 seconds of line_10: integration time at Halpha, [S II] and [N II]. With these integration line_11: times, the expected SNR values per pixel are between 9 and line_12: 100 in Halpha and [N II], and and between 8 and 140 in [S II]. line_13: These values were obtained assuming that the knots are smooth. line_14: We estimate that an integration time of 1000 seconds will be required line_15: for the continuum image to properly subtract the continuum emission line_16: from the line images. Therefore, we request 3.5 hrs of integration line_17: time for the HH 32 jet (before the efficiency factor is taken into line_18: account). ! question: 5 section: 1 line_1: The HH32 jet has an orientation angle of PA=72.4 deg from North line_2: to West and a size of about 40'' (it fits in a single WF CCD). line_3: Since there is a bright star (mv=12.46) close to the center line_4: of the field, we will use the CLOCKS=YES option to suppress line_5: intercolumn bleeding. Please use CCD with read out nearly line_6: perpendicular to PA to avoid problems with the blooming of the line_7: CCD, or, schedule such that the readout of WF3 is nearly line_8: perpendicular to the jet. ! question: 6 section: 1 line_1: No spetial calibration requirements. ! ! question: 8 section: 1 line_1: ! question: 9 section: 1 line_1: 1.- J.C. Raymond and S. Curiel have received previous HST observing line_2: time on the following programs: line_3: {GO 4674.} Co-I on ''Molecular Emission in HH 47'', HIGH priority line_4: time: J.C. Raymond, PI. line_5: {GO 4428.} Co-I on ''Sub-arcsecond Structure of Optical Jets'', line_6: SUPPLEMENTAL time: J.C. Raymond, PI. line_7: These observations have not been carried out yet. line_9: 2.- J.C. Raymond has also received previous HST observing time on the line_10: following programs: line_11: {GO 2243.} Co-I on ''Shock Wave Structures of Herbig-Haro line_12: Objects'', R. Schwartz, PI. line_13: {GO 2356.} Co-I on ''Identification of Super Nova Remnants in M83 line_14: and other Spiral Galaxies'', K. Long, P.I. line_15: {GO 3683.} Co-I on '' Accretion Disk Mapping in Eclipsing line_16: Cataclysmic Variables'', K. Horne, PI. line_18: Results from GO 2243 have been submitted for publication in AJ. line_19: (Schwartz etal. 1993, to appear in AJ). Data acquisition and analysis line_20: are partially complete on GO 2356 and 3683. line_22: Publications: Hubble Space Telescope Images of Herbig-Haro Object line_23: No. 2, R.D. Schuartz etal., AJ, 106, 740. ! question: 10 section: 1 line_1: CFA will provide a SUN SPARCstation II class workstation line_2: for the exclusive use of the PI and Co-I on this project. line_3: CFA will also provide access to other SUN SPARCstations I and II line_4: to support the data reduction. line_6: We have developed numerical codes to calculate the structure of line_7: plane-parallel shock waves, and the characteristics of line_8: stationary and non-stationary jets (see item 2). line_9: With these codes, we will be able to calculate the line emission that line_10: arises from different theoretical possibilities. line_11: We will compare the observational results with those obtained from line_12: these theoretical models. A.C. Raga and S. Biro have a SUN line_13: SPARCstation II that will be used in most of the numerical simulations. ! !end of general form text general_form_address: lname: Raymond fname: John category: PI inst: 2166 addr_1: Center for Astrophysics addr_2: 60 Garden Street (MS 15) city: Cambridge state: MA zip: 02138 country: USA phone: 617-495-7416 telex: 921428 Satelite CAM ; raymond@cfa.harvard.edu ! lname: category: CON ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HH32 name_2: HH32-JET descr_1: G,501,907,929 pos_1: PLATE-ID=02V0, pos_2: RA = 19H 18M 09.41S +/- 1.0", pos_3: DEC = 10D 56' 14.7" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: SURF-LINE(6563) = 15+/-5E-14 fluxnum_2: 1 fluxval_2: SIZE = 1+/-0.3 fluxnum_3: 2 fluxval_3: SURF-LINE(6731) = 30+/-5E-14 fluxnum_4: 2 fluxval_4: SIZE = 1+/-0.3 fluxnum_5: 3 fluxval_5: SURF-LINE(6576) = 15+/-5E-14 fluxnum_6: 3 fluxval_6: SIZE = 1+/-0.3 fluxnum_7: 4 fluxval_7: SURF-CONT(6638) = 6+/-5E-15 fluxnum_8: 4 fluxval_8: SIZE = 1+/-0.3 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HH32 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F675W num_exp: 1 time_per_exp: 1700S s_to_n: 12 s_to_n_time: 1600S fluxnum_1: 4 priority: 1 param_1: CLOCKS=YES, param_2: CR-SPLIT=0.5, param_3: CR-TOLERANCE=0.0 req_1: CYCLE 4; req_2: SEQ 1-4 NO GAP; req_3: ORIENT 152D +/-15D comment_1: THE ORIENTATION OF THE JET IS comment_2: PA=72.4 DEG FROM NORTH TO WEST. USE comment_3: CCD WITH READ OUT PERPENDICULAR TO PA comment_4: TO AVOID PROBLEMS WITH THE BLOOMING OF comment_5: THE CCD. THERE IS A BRIGHT STAR IN THE comment_6: CENTER (MV=12.5). ! linenum: 2.000 targname: HH32 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F656N num_exp: 2 time_per_exp: 2000S s_to_n: 100 s_to_n_time: 4000S fluxnum_1: 1 priority: 1 param_1: CLOCKS=YES, param_2: CR-SPLIT=NO req_1: CYCLE 4; req_2: SAME POS FOR 2-4 AS 1 comment_1: THE ORIENTATION OF THE JET IS comment_2: PA=72.4 DEG FROM NORTH TO WEST. USE comment_3: CCD WITH READ OUT PERPENDICULAR TO PA comment_4: TO AVOID PROBLEMS WITH THE BLOOMING OF comment_5: THE CCD. THERE IS A BRIGHT STAR IN THE comment_6: CENTER (MV=12.5). ! linenum: 3.000 targname: HH32 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F673N num_exp: 2 time_per_exp: 2000S s_to_n: 150 s_to_n_time: 4000S fluxnum_1: 2 priority: 1 param_1: CLOCKS=YES, param_2: CR-SPLIT=NO req_1: CYCLE 4 comment_1: THE ORIENTATION OF THE JET IS comment_2: PA=72.4 DEG FROM NORTH TO WEST. USE comment_3: CCD WITH READ OUT PERPENDICULAR TO PA comment_4: TO AVOID PROBLEMS WITH THE BLOOMING OF comment_5: THE CCD. THERE IS A BRIGHT STAR IN THE comment_6: CENTER (MV=12.5). ! linenum: 4.000 targname: HH32 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F658N num_exp: 2 time_per_exp: 2000S s_to_n: 100 s_to_n_time: 4000S fluxnum_1: 3 priority: 1 param_1: CLOCKS=YES, param_2: CR-SPLIT=NO req_1: CYCLE 4 comment_1: THE ORIENTATION OF THE JET IS comment_2: PA=72.4 DEG FROM NORTH TO WEST. USE comment_3: CCD WITH READ OUT PERPENDICULAR TO PA comment_4: TO AVOID PROBLEMS WITH THE BLOOMING OF comment_5: THE CCD. THERE IS A BRIGHT STAR IN THE comment_6: CENTER (MV=12.5). ! ! end of exposure logsheet ! No scan data records found