! Database: PEPDB ! Date: 20-FEB-1994:02:36:04 coverpage: title_1: PHYSICAL CONDITIONS IN THE NARROW-LINED REGION sci_cat: QUASARS & AGN sci_subcat: SEYFERTS proposal_for: GO/CAR longterm: 1 cont_id: 3982 pi_title: PROF. pi_fname: JACK pi_mi: A. pi_lname: BALDWIN pi_inst: CERRO TOLOLO INTER-AMERICAN OBS. NATIONAL OPTICAL ASTRON.OBS pi_country: USA pi_phone: 011-56-51-225415 keywords_1: ACTIVE GALACTIC NUCLEUS: AGN, SEYFERT GALAXY hours_pri: 11.60 num_pri: 1 wf_pc: X foc: X fos: X hrs: X time_crit: X funds_amount: 121803 funds_length: 24 funds_date: JUL-91 pi_position: ASTRONOMER off_fname: ROBERT off_mi: E off_lname: WILLIAMS off_title: DIRECTOR off_inst: CERRO TOLOLO INTER-AMERICAN OBSERVATORY off_addr_1: CASILLA 603 off_city: LA SERENA off_country: CHILE off_phone: 011-56-51-225415 off_telex: 620301 ! end of coverpage abstract: line_1: We are making a comprehensive study of the emission-line gas in the line_2: narrow-lined region (NLR) of active galactic nuclei (AGN), concentrating line_3: on Seyfert 2 galaxies (initially NGC3393) to avoid confusion with the spectrum line_4: of the broad line region (BLR). We are using a wide variety of the HST line_5: instruments, to ensure a comprehensive and high-quality data set. line_6: These data should immediately allow us to address several important, line_7: inter-related questions about AGN: line_8: a. What is the velocity field in the innermost part of the NLR? line_9: b. Where does the reddening occur in AGN? line_10: c. What is the chemical composition of the gas associated with the AGN? line_11: d. How do the Seyfert 1 and Seyfert 2 continuum sources differ? line_12: e. Do most Seyfert 2 galaxies contain "hidden" BLRs? line_13: We have used the FOS and PC to study extended structure in a few strong lines line_14: This has given us information on the structure, ionisation, and peculiar line_15: motions in the core of the galaxy. However, the nuclear morphology is more line_16: complex than we expected. We therefore intend to take an image in the UV, line_17: using WFPC2 to observe nucleus and offset star. From this we can calculate line_18: an accurate offset to obtain FOS spectra of whatever structure we detect. ! ! end of abstract general_form_proposers: lname: FERLAND fname: GARY title: DR. mi: J. inst: OHIO STATE UNIVERSITY country: USA ! lname: WILLS fname: BEVERLEY title: PROF. mi: J. inst: TEXAS, UNIVERSITY OF country: USA ! lname: WILLS fname: DEREK title: PROF. inst: TEXAS, UNIVERSITY OF country: USA ! lname: NETZER fname: H. title: PROF. inst: TEL AVIV UNIVERSITY country: ISRAEL ! lname: BALDWIN fname: JACK title: P.I. mi: A. inst: CTIO country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Our goal is to make a comprehensive study of the Narrow Lined Region (NLR) of line_2: the seyfert galaxy NGC3393. Specifically, we were awarded HST time to try to line_3: answer the questions: line_5: a. What is the velocity field in the innermost part of the NLR? line_6: b. Where does the reddening occur in AGN? line_7: c. What is the chemical composition of the gas associated with the AGN? line_8: d. How do the Seyfert 1 and Seyfert 2 continuum sources differ? line_9: e. Do most Seyfert 2 galaxies contain "hidden" BLRs? line_11: Following our reassesment to take account of the spherical aberration problem, line_12: we had planned to use WFC, PC, FOS, and GHRS. The GHRS observations were line_13: requested on the expectation that most of the NLR emission would come from a line_14: nearly unresolved source coincident with the continuum nucleus, and that the line_15: best way to differentiate between general inflow or outflow in the NLR line_16: therefore would be to use high spectral resolution (e.g. GHRS) to look for line_17: asymmetries in the Ly-alpha emission profile. ! question: 3 section: 2 line_1: However, we now have obtained a series of short early acquisition exposures line_2: with WFC and PC. These very clearly show that the NLR emission comes from two line_3: regions which straddle the nucleus. There is no NLR emission from the nucleus line_4: itself. We therefore wish to abandon the GHRS observations, since they won't line_5: tell us anything, and instead use that spacecraft time to (1) take WFPC2 line_6: exposures (in order to study this newly-discovered morphology at higher line_7: signal:noise), and (2) take FOS spectra of the brightest emission-line knot line_8: and also of the nuclear continuum source (since what we had previously thought line_9: was one target is now two targets). line_11: This revised observing plan will fit into exactly the same number of line_12: spacecraft hours as our previous (approved) observing plan, and will answer line_13: the exact same scientific questions that we were awarded HST time to answer. line_14: The change is needed in order to take into account what has been learned line_15: from the early acquisition exposures. ! question: 5 section: 1 line_1: As explained above (question 3, section 2) we now have to deal with a line_2: a new morphology for this object. We need to obtain spectra from the main line_3: nuclear UV source, but are unsure of the exact positions. We therefore line_4: propose the following procedure: line_5: 1. An EARLY ACQUISITION IMAGE using the WFPC2 positioned to include both line_7: both the galaxy and the offset star (required for accurate pointing). line_8: 2. Once this image has been studied we will supply accurate coordinates line_9: (as rapidly as possible) for the next observations (below). line_10: 3. FOS/BL (ACQ/BINARY and ACQ/PEAK) acquisition of the offset star. line_12: 4. Offset and FOS/BL (ACCUM) spectra (G160L) of the knot. line_13: 5. FOS/BL (ACQ) confiramtion of the target. line_14: Steps 3,4 and 5 will be submitted separately from this proposal. ! !end of general form text general_form_address: lname: BALDWIN fname: JACK title: PROF. category: PI inst: NATIONAL OPTICAL ASTRONOMY OBSERVATORIES addr_1: CHILE OFFICE addr_2: P.O. BOX 26732 city: TUCSON state: AZ zip: 85726 country: USA phone: 011-56-51-225415 telex: 620-301 AURA CT ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC3393-AND-STAR descr_1: E,301,312, descr_2: A,134 pos_1: RA=10H48M23.25S+/-0.10", pos_2: DEC=-25D09'37.3"+/-1.0" equinox: 2000 rv_or_z: Z=.0124 fluxnum_1: 1 fluxval_1: F(5500) = 1.7 +/- 0.4 E-16 fluxnum_2: 2 fluxval_2: F(2300) = 3.8 +/- 0.8 E-15 fluxnum_3: 3 fluxval_3: F-LINE(4959) = 4.46 +/- 0.9 E-14 fluxnum_4: 4 fluxval_4: W-LINE(4959) = 7.1 fluxnum_5: 5 fluxval_5: F-LINE(6562) = 3.45 +/- 0.7 E-14 fluxnum_6: 6 fluxval_6: W-LINE(6562) = 9.4 fluxnum_7: 7 fluxval_7: F-LINE(3727) = 2.65 +/- 0.5 E-14 fluxnum_8: 8 fluxval_8: W-LINE(3727) = 5.3 ! ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: ! ! linenum: 6.000 targname: NGC3393-AND-STAR config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F218W wavelength: 1800-2517 num_exp: 1 time_per_exp: 280S s_to_n: 20 fluxnum_1: 2 priority: 1 req_1: CYCLE 4 linenum: 7.000 targname: NGC3393-AND-STAR config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F218W wavelength: 1800-2517 num_exp: 1 time_per_exp: 280S s_to_n: 20 fluxnum_1: 2 priority: 1 req_1: POS TARG +1.0, +1.0 ; req_2: CYCLE 4 linenum: 8.000 targname: NGC3393-AND-STAR config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F218W wavelength: 1800-2517 num_exp: 1 time_per_exp: 280S s_to_n: 20 fluxnum_1: 2 priority: 1 req_1: POS TARG -1.0, -1.0 ; req_2: CYCLE 4 ! ! end of exposure logsheet ! No scan data records found