! $Id: 5616,v 6.1 1995/05/26 14:15:13 pepsa Exp $ coverpage: title_1: COLLIMATED RADIO AND IONIZING RADIATION IN NGC 5252 - PART II sci_cat: GALAXIES sci_subcat: SEYFERT proposal_for: GO cont_id: 5426 pi_fname: ZLATAN pi_mi: I pi_lname: TSVETANOV pi_inst: JOHNS HOPKINS UNIVERSITY pi_country: USA pi_phone: 410-516-8585 hours_pri: 3.50 num_pri: 1 wf_pc: Y off_fname: CHERYL-LEE off_lname: HOWARD off_title: ASSISTANT DEAN off_inst: 2380 off_addr_1: HOMEWOOD RESEARCH ADMINISTRATION off_addr_2: 105 AMES HALL off_addr_3: 34TH & NORTH CHARLES STREET off_city: BALTIMORE off_state: MD off_zip: 21218 off_country: USA off_phone: 410-516-8668 ! end of coverpage abstract: line_1: Ground-based emission-line images of the Seyfert 2 galaxy NGC5252 reveal line_2: perhaps the most spectacular ionization cone known. The bi-conical structure line_3: extends to large distances from the nucleus and is significantly misaligned line_4: w.r.t. the major axis of the host galaxy. Our VLA radio maps show a clear line_5: nuclear jet, which is coaligned with the ionization cone axis to within the line_6: measurement errors. In addition, ground-based long-slit spectra and our line_7: Fabry-Perot imagessuggest possible helical motions. We propose to obtain line_8: narrow-band WFPC2 images in the OIII 5007, Halpha and OII 3727 and 2 continuum line_9: bands. These will be used to map the ionizing radiation field all the way in line_10: to the nucleus and study the correlation between the radio and optical line_11: emission on sub-arcsecond scales. We will also use the line ratio maps to try line_12: to put constraints on the angular dependence of the ionizing field as well as line_13: continuum color maps to look for the presence of local ionizing sources such line_14: as hot stars in addition to the hard nuclear radiation. ! ! end of abstract general_form_proposers: lname: TSVETANOV fname: ZLATAN mi: I inst: 2380 country: USA ! lname: WILSON fname: ANDREW mi: S inst: 3470 country: USA ! lname: MORSE fname: JON inst: 3470 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: NGC5252 will be imaged in two continuum and three emission lines bands. line_2: (1) The [OIII]5007 image. We will use the ramp filter FR533N. This will provide line_3: us with a 0.1 "/px resolution image which than can be compared with our radio line_4: VLA map of the same resolution. This will be a 5x--10x improvement compared line_5: with the best available ground-based images. line_6: (2) The H-alpha image. Because of the redshift of NGC 5252, cz=6925, km s-1, line_7: the H-alpha+[NII] complex of lines falls into the passband of F673N. We will line_8: take a PC image through this filter to achieve the highest possible resolution line_9: of 0.046 "/px. line_10: (3) The [OII]3727 image. The redshited position of this line (lambda=3813 A) line_11: falls into the passband of one of the quadrand filters - FQUVN-B. This image line_12: will be ratioed with the [OIII]5007 image to construct a line-ratio map line_13: sensitive to the ionisation parameter U. line_14: (4) Continuum images. We plan to take 2 continuum images - one in the line_15: wavelength range between [OIII]5007 and H-alpha and one next to [OII]3727. line_16: Unfortunately, because of the redshift of NGC5252 we can not use F547M - the line_17: 5007 line is in the bandpass. Instead, we will use F588N, which has a bandwith line_18: of only approx.50 A, but because of the higher system troughput does not line_19: increase unreasonably the exposure time. For the UV continuum image we will line_20: use F336W. ! question: 3 section: 2 line_1: Our estimates of the exposure time are based on the following formula and line_2: assumptions (see WFPC2 Handbook for more details): line_3: N(el) = 2.3e12 t(exp) QT(max) lambda F(line) line_4: where N(el) is the number of electrons detected, t(exp) is the exposure time in line_5: seconds, lambda is the wavelength in A, and F(line) is the observed integrated line_6: line flux in ergs cm-2 s-1. These e- will be spread over the area covered by line_7: the resolved emission-line structure. Exposure time estimates through each of line_8: the proposed filters are based on the fluxes measured from our calibrated line_9: ground-based images. From our [oiii]5007 image we measure approx. 1.5e-13 ergs line_10: cm-2 s-1 in the central 2". This leads to roughly 12000 counts in a 20 min line_11: exposure distributed over the area covered by the emission-line structure line_12: (maximum of 400 WFC 0.1" pixels). Therefore, there will be no numerical line_13: saturation in the low read-out-noise mode (7 e- RON) even if all of the line_14: emission is concentrated in one or few point-like sources. Estimates for the line_15: exposure times in [oii]3727 line and two continuum bands are based on a line_16: ground-based long-slit spectrum obtained at with the 3.6m telescope at ESO. line_17: These estimates assume that the velocity dispersion in the extended regions is line_18: not larger than +/- 300-350 km s-1 around the systemic velocity (as suggested line_19: by our Fabry-Perot data), so the line remains within the filter bandpass. line_20: Estimated exposure times are as follows: line_21: F336W (UV cont.) - 50 min, FQUVN-B ([oii]3727) - 50 min, FR533N ([oiii]5007) - line_22: 40 min, F588N (cont.) - 40 min, F673N (H-alpha) - 30 min. line_23: Note - Each exposure will be taken in CR split mode. ! question: 4 section: 1 line_1: NGC5252 offers one of the best laboratories to study many important line_2: questions related to the collimated nuclear emission and radio jet -- line_3: host galaxy interaction. For this one needs to obtain optical images line_4: with resolution approximately matching that of the VLA radio map. This line_5: is possible only with the HST. line_6: Prior to this proposal we have obtained ground-based emission-line line_7: and Fabry-Perot images, as well as VLA radio maps. All these have line_8: been used in planing the HST observations. ! question: 5 section: 1 line_1: We have no special requests. ! question: 6 section: 1 line_1: We have no special calibration requirements. ! ! question: 8 section: 1 line_1: ! question: 9 section: 1 line_1: 1036: Imaging and Spectrophotometry of Seyfert Nuclei (GTO/FOS 14) - Ford line_2: (PI) plus the FOS team. line_3: 3671: UV Spectroscopy of Hydrogen-Poor Planetary Nebulae - Harrington (PI), line_4: Borkowski, Tsvetanov, Clegg. Not related to this proposal. line_5: 3724: Ionizing Cones, Obscuring Tori, and the Narrow line Regions of line_6: Seyfert Galaxies - Wilson (PI), Heckman, Bower. line_7: 4371: FOS Spectroscopy of Resolved Structure in the Nucleus of Mrk 3 - line_8: Tsvetanov (PI), Evans, Ford, Kriss, Uomoto, Davidsen. line_9: 4503: Absorption-Line spectra of Seyfert Galaxies - Kriss (PI), Ford, line_10: Tsvetanov, Davidsen. Completion of observations pending. line_11: 4668: FOS Spectroscopy of NGC1052 and NGC4258 - Ford (PI), Evans, Kriss, line_12: Kinney, Tsvetanov. Completion of observations pending. line_13: Analysis of the HST images and spectra taken as part of GTO 1036 has inspired line_14: some of the ideas presented here. In particular, we would like to mention line_15: Mrk 3, which shows signatures of possible jet -- local ISM interaction and line_16: NGC4151, where HST observations present a clear problem for the simplest line_17: version of the Unified Model of AGN. Imaging part of 1036 is completed and line_18: FOS observations continue being taken in cycle 3. From these observations we line_19: have identified (1) a general association between the radio and emission-line line_20: structures, (2) ionization cones, but with (presumably) obscured apices, and line_21: (3) very red continuum colors at the inferred position of the nucleus, line_22: possibly due to differential reddening. Several papers discussing ``unified line_23: models" for Seyfert galaxies are forthcoming. ! question: 10 section: 1 line_1: At the Center for Astrophysical Sciences, the Johns Hopkins University line_2: and at STScI, we have access to a network of Sun Workstations and the line_3: appropriate software (IRAS, STSDAS) is installed. The network maintenance line_4: and other supproting technical assistance is provided through group line_5: maintenance contracts for computer equipment. The university provides line_6: opportunities for graduate students as well as undergraduates to assist line_7: in research projects for academic credit. ! !end of general form text general_form_address: lname: TSVETANOV fname: Zlatan mi: I category: PI inst: 2380 addr_1: Center for Astrophysical Sciences addr_2: Department of Physics and Astronomy addr_3: 34th & North Charles Street city: Baltimore state: MD zip: 21218 country: USA phone: 410-516-8585 telex: zlatan@pha.jhu.edu ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC5252 name_2: UGC8622 descr_1: E,312,910,924 pos_1: RA = 13H 38M 15.867S +/- 0.1", pos_2: DEC = +4D 32' 33.53" +/- 0.1", pos_3: PLATE-ID=019P equinox: 2000 rv_or_z: V = 6890 comment_1: LINE FLUX IS 2" APERTURE MEASURED comment_2: FROM GROUND-BASED IMAGES. fluxnum_1: 1 fluxval_1: B=14.11 +/- 0.3 fluxnum_2: 1 fluxval_2: F-LINE(5007)=1.5 +/- 0.05 E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.200 targname: NGC5252 config: WFPC2 opmode: IMAGE aperture: LRF sp_element: LRF wavelength: 5122 num_exp: 1 time_per_exp: 2400S priority: 1 param_1: CR-SPLIT=DEF, param_2: CR-TOLERANCE=0.2 req_1: CYCLE 4; ! ! end of exposure logsheet ! No scan data records found