! File: 1217C.PROP ! Database: PEPDB ! Date: 16-FEB-1994:06:30:10 coverpage: title_1: THE NUCLEUS OF NGC 1052 sci_cat: QUASARS & AGN proposal_for: GTO/FOC pi_fname: ALEC pi_lname: BOKSENBERG pi_inst: ROYAL GREENWICH OBSERVATORY pi_country: UNITED KINGDOM pi_phone: 0223-374000 keywords_1: GALAXIES : INDIVIDUAL - GALAXIES : NUCLEI - GALAXIES : keywords_2: LINERS - RADIATION MECHANISMS - RADIOGALAXY hours_pri: 2.50 num_pri: 1 time_crit: X pi_position: PROFESSOR ! end of coverpage abstract: line_1: We show that the ST-FOC (in the first order of the long-slit spectrographic line_2: mode) allows to decide unambiguously which mechanism - photoionization by a line_3: central source or shock heating - is at work in this nucleus and thus to answer line_4: a fundamental question concerning active nuclei in general. line_6: In addition, the imaging mode of the FOC can provide the basic data with which line_7: to answer questions about the interaction between the nuclear activity and the line_8: interstellar medium. This is of relevance to ideas about the formation and line_9: maintenance of beams which power double radio sources. line_11: The question of stratification in nearby AGN is a general one, but we believe line_12: that NGC 1052 should be considered as a priority object because of the interest line_13: of the problems that can be solved in a reasonable observing time. ! ! end of abstract general_form_proposers: lname: PEQUIGUOT fname: DAVID inst: MEUDON OBSERVATORY country: FRANCE esa: X ! lname: BOISSON fname: CATHERINE inst: MEUDON OBSERVATORY country: FRANCE esa: X ! lname: BOKSENBERG fname: ALEC inst: ROYAL GREENWICH OBSERVATORY country: UNITED KINGDOM esa: X ! lname: FOSBURY fname: ROBERT A. mi: E. inst: ESA, EUROPEAN COORDINATING FACILITY country: GERMANY, WEST esa: X ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: 3a - Image of [OIII]5007 line_2: --------------------- line_3: The immediate surroundings of the nucleus in any direction and one of the radio line_4: lobes can be mapped with the f/96 FOC direct mode with a field of view of 22.5" line_5: x 11.2" (1024 x 256, iD Zoom) orientated approximatley east-west: line_6: - the 22.5" side parallel to the radio axis (at PA 95D) line_7: - the nucleus at approximately (within a few 0.1"): line_8: 4.5" from the west (short) side line_9: 5" from the north (long) side line_11: The [OIII] map is obtained by means of two successive exposures at the same line_12: position with: line_13: - filter F501N for [OIII] 5007: 4000 sec (total) line_14: - filter F502M for continuum : 500 sec line_16: Even with roughly homogeneous gas emission a S/N of order of 4 is still line_17: obtained at 10 arcsec from the nucleus. Thus any filamentary structure should line_18: be easily detected. ! question: 3 section: 2 line_1: 3b - Long-slit spectroscopy line_2: ---------------------- line_4: The long-slit of the f/48 FOC spectrograph (1024x256,1D Zoom) at PA 95D should line_5: cross the nucleus, with the west end of the slit at approximately 4" from the line_6: nucleus. line_8: The position of the slit should be known to better than 0.1" relative to the line_9: [OIII]map. line_11: Observations in the first order (F305LP filter ~/= 3400 - 5200 A) during 4500 line_12: sec. (total). line_14: Some idea of the S/N can be get from Table 1 (section 2b). ! question: 4 section: 1 line_1: Very high spatial resolution is required. The fine structure in the [OIII] line_2: image (filaments, etc ...) will be an important key to understand the nature of line_3: the interactions and the evolution of the gas. In addition a precise position line_4: of the centre is obtained. line_6: Concerning spectrography, the FOC is essential in two respects : (1) the line_7: behaviour of stratification in the inner arcsecond will best decide between the line_8: different models of the nucleus and (2) velocity information and a few line line_9: ratios will be obtained at a comparable resolution to the map up to the edge of line_10: the nebulosity. The wavelength range covered by the 1st order of the line_11: spectroscopic code contains enough relevant lines to allow a conclusive line_12: discussion. line_14: The ground-based observations can in the next years usefully improve some line line_15: intensities values such as the controversial [OIII]4363 (Appendix 1). line_16: However, nothing can be firmly concluded for the ionizing mechanism unless much line_17: better than 1 arcsec resolution is achieved. Moreover, maps at the line_18: [OIII]5007 obtained from the ground will give a reasonably good idea of the line_19: large scale gas distribution but information on any filamentary structure will line_20: be missing. ! question: 6 section: 1 line_1: a - Calibration requirements: line_2: ------------------------ line_4: f/96 : the absolute flux is not required to be better than 5% relative to line_5: celestial standards. Relative fluxes to 5% within the frame are required. line_6: Since the f/96 exposure serves in part to determine the pointing postion for line_7: the f/48 observations, these direct exposures will require good geometric line_8: fidelity. It should be possible to determine the coordinates of an object to line_9: better than 0.05 arcsec. line_11: f/48 : wavelength calibration should be known to +/- 1/2 pixel across the line_12: entire spectral range available. Relative intensities to 5% will be required. line_14: b - Dark time : line_15: --------- line_17: Extended object with faint outer zones. ! question: 7 section: 1 line_1: We are familiar with data reduction and analysis of IPCS frames (spectroscopic line_2: mode) and CCD images. The software facilities available to us are a VAX 11/780 line_3: (VMS 3.4 operating system) at Meudon and an HP 1000 (RTE 6 operating system) at line_4: the Institut d'Astrophysique de Paris on which the SPICA-STARLINK + line_5: MIDAS-ESO-ECF and IHAP-ESO data resolution packages are installed respectively. line_7: There is also a software center (VAX equipped) in Marseille (at the "French line_8: Pilot Center for the Space Telescope") which is to remain in close contact with line_9: the STScI and ECF. Finally we have access to the STARLINK VAX at RGO. line_11: In addition, A. Bijaoui, M. Caillat and D. Pelat are developing on the VAX at line_12: Meudon a 2D-data reduction package (EVE) which has the great advantage to be line_13: used directly in DCL mode. Part of this package is already user friendly. line_15: We rely on the STScI for software related to first step geometric and line_16: photometric corrections, wavelength calibrations. However these first steps line_17: can be achieved at our home institutes if we receive all the frames allowing to line_18: define the instrument characteristics. line_20: Concerning modellings, one of us is directly implicated in the building and line_21: constant improvement of the detailed photoionization code "PHOTO" (see line_22: publications of the last 7 years by Stasinska and/or Pequignot), which is well line_23: suited for studying active galactic nuclei (e.g. Pequignot, 1984). ! question: 7 section: 2 line_1: Also a new code treating shocks (with or without external radiation source) is line_2: now reaching a test phase and should be in operation in 1985 (Stasinska, line_3: Pequignot, in preparation). ! question: 10 section: 1 line_1: The applicants have free access to all computer facilities for either data line_2: analysis or modelling (see section 7). line_4: In France there are two organizations which have special lines of credit for line_5: Space Telescope observations : INAG and ATP - Telescope Spatial. Programs line_6: linked to ST will have high priority in our laboratory. ! question: 13 section: 1 line_1: Observation of the nucleus of NGC 1052 and its eastern 20 arcsecond line_2: surroundings with the FOC in both the first order of the long-slit line_3: spectroscopic mode and the imaging mode ([OIII]5007). The aim is deciding line_4: which mechanism -photoionization by a central source or shock heating - is at line_5: work in this archetypal nucleus and studying the interaction between the line_6: surrounding medium and the nuclear activity which powers the double line_7: radiosource. ! !end of general form text general_form_address: lname: BOISSON fname: CATHERINE category: CON inst: OBSERVATOIRE DE MEUDON city: MEUDON PRINCIPAL CEDEX country: FRANCE phone: (33)1-534-75-70 telex: 201571F ! lname: BOKSENBERG fname: ALEC title: PROF. category: PI inst: ROYAL GREENWICH OBSERVATORY addr_1: MADINGLEY ROAD addr_2: CB3 0EZ city: CAMBRIDGE country: UNITED KINGDOM phone: (44)223-374000 telex: 817235 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC1052 descr_1: NUCLEAR REGION OF THE ACTIVE ELLIPTICAL descr_2: GALAXY NGC 1052 pos_1: RA = 2H 38M 37.2S +/- 0.1S, pos_2: DEC = -08D 28' 08" +/- 0.1" equinox: 1950 pm_or_par: N rv_or_z: V=1424 acqpr_1: EXT acqpr_2: BKG plate_req: N plate_avail: N comment_1: POSITION IS FROM GASP. comment_2: IN AGREEMENT WITH THE comment_3: OPTICAL POSITION OF ARGYLE 1983. comment_4: FLUX REF. 2 FOR THE COMPACT comment_5: NUCLEUS, 3 AT 1 ARCSEC FROM comment_6: NUCLEUS, 4, 5 AT 3 ARCSEC; comment_7: POINTING TOLERANCE 0.1" FOR LONG comment_8: SLIT SPECTROSCOPY. fluxnum_1: 1 fluxval_1: V=12.2 +/- 0.5 fluxnum_2: 2 fluxval_2: F-LINE(4861)=1.3 E-15, W-LINE(4861)=15 + fluxval_3: /- 2 fluxnum_4: 3 fluxval_4: SURF-LINE(4861)=5 E-15, W-LINE(4861)=6 + fluxval_5: /- 0.6 fluxnum_6: 4 fluxval_6: SURF-LINE(5007)=6 E-15, W-LINE(5007)= fluxval_7: 3.5 +/- 0.4 fluxnum_8: 5 fluxval_8: SURF-CONT-BKG(4500)=1.5 +/- 0.2 E-16 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: NGC1052 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F501N wavelength: 5010 num_exp: 1 time_per_exp: 2150S s_to_n: 4 fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: PIXEL=25X25 req_1: ORIENT 301D +/- 5D; req_2: DARK TIME / 1-2; req_3: GROUP 1-2 WITHIN 1D; req_4: SAME ORIENT FOR 2 AS 1; req_5: CYCLE 2 / 1-4; req_6: GUID TOL 0.020" / 1-4; req_7: COND IF TAC OK / 1-4; comment_1: ORIENT 121D +/- 5D IS EQUALLY GOOD. ! linenum: 2.000 targname: NGC1052 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F502M wavelength: 4950 num_exp: 1 time_per_exp: 900S s_to_n: 4 fluxnum_1: 2,3 fluxnum_2: 4,5 priority: 1 param_1: PIXEL=25X25 ! linenum: 3.000 targname: NGC1052 config: FOC/48 opmode: ACQ aperture: 128X128-ASLIT sp_element: F220W num_exp: 1 time_per_exp: 300S priority: 1 req_1: ONBOARD ACQ FOR 4; ! linenum: 4.000 targname: NGC1052 config: FOC/48 opmode: SPEC aperture: 256X1024-SLIT sp_element: G450M wavelength: 3600-5300 num_exp: 1 time_per_exp: 3700S s_to_n: 4 fluxnum_1: 3 priority: 1 param_1: PIXEL=50X25 req_1: ORIENT 335D +/- 5D; comment_1: ORIENT 155D +/- 5D IS EQUALLY GOOD. comment_2: S/N GIVEN FOR A 0.1" X 0.1" comment_3: RESOLUTION ELEMENT ! ! end of exposure logsheet ! No scan data records found