! File: 4428C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:11:32:19 coverpage: title_1: "SUB--ARCSECOND STRUCTURE OF OPTICAL JETS" sci_cat: INTERSTELLAR MEDIUM sci_subcat: HERBIG-HARO OBJECTS proposal_for: GO pi_title: DR. pi_fname: JOHN pi_mi: C. pi_lname: RAYMOND pi_inst: 2166 pi_country: USA pi_phone: 617-495-7416 hours_pri: 8.00 num_pri: 1 wf_pc: Y funds_amount: 68432 funds_length: 12 funds_date: JUL-93 off_fname: IRWIN off_mi: I. off_lname: SHAPIRO off_title: DIRECTOR off_inst: 2166 off_addr_1: CENTER FOR ASTROPHYSICS off_addr_2: 60 GARDEN STREET off_addr_3: MS 45 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 HH46/47 optical jet taken with line_2: the Planetary Camera will be used to test predictions from theoretical line_3: models. We propose to take advantage of the high angular resolution line_4: provided by this camera to study the morphology of the knots along the line_5: body of this jet in detail. We will completely resolve most of them line_6: and study their spacing and changes in their morphology at different line_7: wavelengths. Likewise, these observations will give information about line_8: the excitation in individual knots, and gradients along the jet. line_9: A comparison between the results of these observations and those line_10: obtained from numerical simulations will provide a new and unique line_11: insight on the origin of the knotty structure that will help to line_12: discriminate among the wide range of proposed theoretical possibilities. ! ! end of abstract general_form_proposers: lname: RAYMOND fname: JOHN title: PI mi: C. inst: 2166 country: USA ! lname: CURIEL fname: SALVADOR inst: 2166 country: USA ! lname: RAGA fname: ALEJANDRO inst: 8046 country: UNITED KINGDOM ! lname: NISENSON fname: PETE inst: 2166 country: USA ! lname: NORIEGA-CRESPO fname: ALBERTO inst: 3760 country: USA ! lname: BIRO fname: SUSANA inst: 8046 country: UNITED KINGDOM ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We request time to observe the HH46/47 optical jet using the PC camera. line_2: This camera provides a field of view and resolution that will allow us to line_3: cover the main body of the jet in single frames, including a number of line_4: stars that can be used to align the images. H-alpha, [S II] and [N II] line_5: narrow band images will be obtained for this object. A narrow band line_6: continuum image will also be obtained for this jet, which will be line_7: used to subtract the continuum emission from the line images. Since line_8: the bright portion of this jet is only ~60'' long, only four images line_9: will be needed 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 deconvolution line_3: techniques, angular resolutions of about 0.4''-0.6'' can be reached line_4: with ground-based observations. However, this extraordinary resolution line_5: is not enough to properly resolve most of the knots on optical jets line_6: (with sizes between ~0.3'' and 0.8''), which is necessary in order to line_7: establish their nature. The mapping of optical jets in the light of line_8: several lines with an angular resolution of ~0.1'', can provide line_9: detailed information of individual knots (e.g., morphologies, ionization line_10: gradients, and offsets between the knot positions in different emission line_11: lines) that can be directly compared with predictions from numerical line_12: simulations. At present, this angular resolution can only be achieved line_13: with the HST. The HST provides an angular resolution that is better by line_14: at least a factor of three compared to ground-based observations. ! question: 4 section: 2 line_1: Single H-alpha, [S II] 6717/6731 and [N II] 6583 narrow band, and line_2: narrow band continuum images will be obtained for the HH 46/47 jet. line_3: The bright knots in this jet have fluxes of about 2, 7 and line_4: 1 (x10^{-14}) erg cm^{-2} s^{-1} (same units hereafter) for H-alpha, line_5: [S II] and [N II] (Raga and Mateo 1988), respectively, with typical line_6: sizes of 1 arcsec^2. On the other hand, the fainter structures that line_7: we want to study have fluxes of 0.2 for the same three lines. The line_8: required sensitivity per pixel for this jet can be achieved in about line_9: 7500 seconds of integration time at H-alpha, 5000 at [S II], and 3600 line_10: at [N II]. With these times, the expected SNR values per pixel line_11: are between 5 and 18 in H-alpha, 6 and 40 in [S II], and 3 and 9 in line_12: [N II]. These values were obtained assuming that the knots are smooth. line_13: To enhance the fainter features in this jet, we will bin the images to line_14: obtain ~10:1 SNR (e.g., a 2 x 2 binning would increase the SNR by a line_15: factor of ~2). We estimate that an integration time of 4000 seconds line_16: will be required for the narrow band continuum image of this jet to line_17: properly subtract the continuum emission from the line images. line_18: Therefore, we request 6 hrs of integration time for the HH 46/47 jet line_19: (before the efficiency factor is taken into account). ! question: 5 section: 1 line_1: No special requests. ! question: 6 section: 1 line_1: No special calibration requirements. ! question: 7 section: 1 line_1: --- The data will be first reduced by using standard procedures and then, line_2: the resultant images will be deconvolved, as described in item 2, to line_3: reach the needed angular resolution of ~0.1''-0.15''. Special care will line_4: be needed in the image deconvolution to reach this resolution. We plan line_5: to perform the deconvolutions with more than one of the different line_6: algorithms that are available (see item 2), and compare results in order line_7: to improve our confidence in the accuracy of the restorations. Since we line_8: are also interested in the faint structure, we will deconvolve the line_9: binned and un-binned images to determine the accuracy of the line_10: deconvolution by comparing the resultant images. line_11: --- In order to properly align the images, we will use the guide stars line_12: and the stars in the field to determine offsets between the position line_13: of the field center of the images, and to measure possible rotations line_14: between images. This alignment is very important to search for offsets line_15: between the position of the knots in the light of the emission lines. line_16: --- We will use results from ground-based observations, obtained by us line_17: and other authors, to constrain our numerical models of this jet. We line_18: also plan to obtain supplemental optical and infrared data with the line_19: 100'' telescope in Chile. In particular, imaging of lines such as line_20: [O I] 6300 and [C I] 9810 in the optical, and H2 1-0 S(1) at 2.1 line_21: microns and [Fe II] at 1.64 microns in the infrared will provide further line_22: information about the excitation state along the jet, and the physical line_23: conditions in the gas. ! question: 9 section: 1 line_1: 1.- J.C. Raymond and S. Curiel have received previous HST observing time line_2: on the following program: line_4: {GO 4674.} Co-I on ''Molecular Emission in HH 47'', HIGH priority time: line_5: 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_12: {GO 2243.} Co-I on ''Shock Wave Structures of Herbig-Haro Objects'', line_13: R. Schwartz, PI. line_15: {GO 2356.} Co-I on ''Identification of Super Nova Remnants in M83 line_16: and other Spiral Galaxies'', K. Long, P.I. line_18: {GO 3683.} Co-I on '' Accretion Disk Mapping in Eclipsing line_19: Cataclysmic Variables'', K. Horne, PI. line_21: Results from GO 2243 have been submitted for publication in AJ. line_22: (Schwartz etal. 1993, to appear in AJ). line_23: Data acquisition and analysis are partially complete on GO 2356 and 3683. ! question: 9 section: 2 line_1: We have been recently allocated HIGH priority HST time (ID 4674) line_2: to study the H2 UV emission in the HH 47A bow-shock, previously line_3: detected by IUE observations. From these observations, we will obtain line_4: an UV image (FOC) and an H2 UV spectrum (GHRS) of this working surface. line_5: By combining the HST optical images of HH 46/47 with these HST UV line_6: observations and ground-based H2 and FeII IR images, we will obtain line_7: significant new insight into the emission processes that govern this line_8: working surface. ! question: 9 section: 3 line_1: Hubble Space Telescope Images of Herbig-Haro Object No. 2, line_2: R.D. Schuartz etal., AJ, (in press). ! question: 10 section: 1 line_1: SAO will provide a SUN SPARCstation II class workstation for the line_2: exclusive use of the PI and Co-I on this project. CFA will also provide line_3: access to other SUN SPARCstations I and II to support the data reduction. line_4: Some of the algorithms that will be used for the deconvolution of the line_5: images are available at the CFA. We also plan to use software developed line_6: at Tufts and JPL for design of WF/PC II (or Tiny Tim from STEIS) to line_7: generate psf's for each subregion to be deconvolved. We have developed line_8: numerical codes to calculate the structure of plane-parallel shock waves, line_9: and the characteristics of stationary and non-stationary jets (see text). line_10: With these codes, we will be able to calculate the line emission that line_11: arises from different theoretical possibilities. We will compare the line_12: observational results with those obtained from these theoretical models. line_13: A.C. Raga and S. Biro have a SUN SPARCstation II that will be used in line_14: most of the numerical simulations. ! !end of general form text general_form_address: lname: RAYMOND fname: JOHN mi: C. title: DR. 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 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HH46-47 name_2: HH46-47-JET name_3: HH47 descr_1: G,501,907,929 pos_1: PLATE-ID=00AI, pos_2: RA = 08H 25M 50.18S +/- 0.4S, pos_3: DEC = -50D 59' 50.7" +/- 0.4" equinox: 2000 rv_or_z: V = -100 fluxnum_1: 1 fluxval_1: SURF-LINE(6563) = 20+/-5E-15 fluxnum_2: 1 fluxval_2: SIZE = 1+/-0.3 fluxnum_3: 2 fluxval_3: SURF-LINE(6731) = 70+/-5E-15 fluxnum_4: 2 fluxval_4: SIZE = 1+/-0.3 fluxnum_5: 3 fluxval_5: SURF-CONT(6638) = 8+/-5E-15 fluxnum_6: 3 fluxval_6: SIZE = 1+/-0.3 fluxnum_7: 4 fluxval_7: SURF-LINE(6576) = 10+/-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: HH46-47 config: PC opmode: IMAGE aperture: PC5 sp_element: F656N num_exp: 1 time_per_exp: 6750S s_to_n: 18 fluxnum_1: 1 priority: 1 req_1: CYCLE 3 ! linenum: 2.000 targname: HH46-47 config: PC opmode: IMAGE aperture: PC5 sp_element: F673N num_exp: 1 time_per_exp: 4900S s_to_n: 40 fluxnum_1: 2 priority: 1 req_1: CYCLE 3 ! linenum: 3.000 targname: HH46-47 config: PC opmode: IMAGE aperture: PC5 sp_element: F664N num_exp: 1 time_per_exp: 4000S s_to_n: 10 fluxnum_1: 3 priority: 1 req_1: CYCLE 3 ! linenum: 4.000 targname: HH46-47 config: PC opmode: IMAGE aperture: PC5 sp_element: F658N num_exp: 1 time_per_exp: 3600S s_to_n: 9 fluxnum_1: 4 priority: 1 req_1: CYCLE 3 ! ! end of exposure logsheet ! No scan data records found