! File: 4668C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:21:49:29 coverpage: title_1: FOS SPECTROSCOPY OF N1052 AND N4258: THE RELATIONSHIP BETWEEN LINERS title_2: AND SEYFERTS sci_cat: QUASARS & AGN sci_subcat: OTHER ACTIVE NUCLEI proposal_for: GO pi_fname: HOLLAND pi_mi: C pi_lname: FORD pi_inst: 2380 pi_country: USA hours_pri: 8.87 num_pri: 2 fos: Y funds_length: 12 off_fname: CHERLY-LEE off_lname: HOWARD off_title: ASSISTANT DEAN off_inst: JOHNS HOPKINS UNIVERSITY off_addr_1: HOMEWOOD RESEARCH ADMINISTRATION off_addr_2: HOMEWOOD CAMPUS off_city: BALTIMORE off_state: MD off_zip: 21218 off_country: USA off_phone: 516-8668 ! end of coverpage abstract: line_1: The relationship between Liners and Seyferts is poorly understood. We do not line_2: know if Liners are powered by nuclear black holes, and if the nuclei are line_3: sometimes hidden by obscuring tori or disks of cold gas and dust. Put another line_4: way, we do not know how Liners fit into the AGN paradigm. A combination of HST line_5: images, ground-based spectroscopy, and VLA images suggest that at least three line_6: Liners do fit the paradigm. One of these, M51, is well described as a miniature line_7: -Seyfert 2 galaxy. We hypothesize that all Liners are miniature Seyferts line_8: (though with interesting differences in detail), and propose to test this line_9: hypothesis by obtaining FOS spectra of two additional Liners, NGC 1052 and line_10: NGC 4258.Small aperture FOS spectra of the high contrast, stellar emission line line_11: nuclei seen in our HST images will allow us to determine if the nuclei harbor a line_12: hidden broad-line source and a power-law source of continuum radiation which line_13: ionizes the gas near the nucleus. Detection of broad-lines in Lyman alpha, line_14: CIV, or halpha, either directly or from scattered light, will be strong line_15: evidence for a black hole. Because of dilution by the starlight in the parent line_16: galaxy, neither IUE nor ground-based observations can cleanly isolate these line_17: faint, high contrast nuclei. ! ! end of abstract general_form_proposers: lname: FORD fname: HOLLAND title: PI mi: C inst: 2380 country: USA ! lname: EVANS fname: IAN inst: STSCI country: USA ! lname: KINNEY fname: ANNE inst: STSCI country: USA ! lname: KRISS fname: GERALD inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: TSVETANOV fname: ZLATAN inst: JOHNS HOPKINS UNIVERSITY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will do an FOS binary acquisition of a nearby bright seen in WF images we line_2: have already taken. We will follow this with an FOS peak-up acquisition line_3: through the 0.3'' aperture. We then will offset to the nucleus, using offsets line_4: measured from our WF and PC broadband and narrow band images of the galaxies. line_5: After offsetting, we will take FOS spectra of the nuclei using G130H, G190H, line_6: G270H, G400H, and G570H. ! question: 4 section: 1 line_1: The first phase of this program, HST broad band and narrow band imaging, line_2: already been done. We also have high quality KPNO 4-m [OIII] and H_alpha line_3: images and spectra of NGC 4258. These images and spectra do not reveal the line_4: faint, but high contrast emission line nucleus which we propose to observe line_5: here. HST images and small aperture spectra of high contrast features yield line_6: spatial and spatial-spectral information which cannot be obtained from the line_7: ground. Empirical evidence for this is the many discoveries of sub-arc line_8: second features in HST images which had not been seen from the ground. These line_9: discoveries are a consequence of the fact that the diffraction-limited core line_10: of the PSF, though reduced in amplitude by a factor of 5 to 6 from what it line_11: should have been, encodes spatial information with significant power in the line_12: MTF up tofrequencies of ~ 12 cycles/arcsecond (White, 1991). When the line_13: contrast is high, as in the nuclei considered here, the nucleus can be line_14: imaged, and a small aperture can be used to exclude light from the line_15: surrounding galaxy which dilutes ground-based spectra. ! question: 5 section: 1 line_1: The FOS IDT GTO Science Assessment Observations, and Cycle 0 and 1 line_2: observations of NGC 1068 serve as our point of comparison for line_3: estimating exposure times for the UV and red spectra of the nucleus and line_4: the nuclear emission-line clouds. From the NGC 1068 spectra, for Cloud line_5: C (Evans et al 1991) exposures of 1500S and 1000S using G130H and G190H line_6: yield a S/N ratio of approx. 5 in the continuum, and a broad component line_7: on C IV 1549 is detected at a confidence level of > 5 sigma. Exposures line_8: of 700S, 600S, and 600S through G270H, G400H, and G570H typically give line_9: a S/N of 10 in the continuum. With these exposures as a fiducial, we line_10: estimated the net [O III], H-alpha, and continuum fluxes which would be line_11: measured through the 0.3" FOS aperture from existing Cycle 0 images of line_12: the objects, and scaled the FOS exposure times accordingly to yield a line_13: minimum S/N of approximately 5 in the continuum for both the UV and red line_14: spectra. We have also used ground based and IUE spectra to estimate line_15: the monochromatic line fluxes as a cross check to determine the line_16: exposure times. ! question: 6 section: 1 line_1: We have no special calibration requirements. ! question: 7 section: 1 line_1: We will use IRAF and STSDAS routines to measure the wavelengths, line line_2: widths, and line fluxes. The emission line spectra will be modeled with line_3: the ionization cods CLOUDY and MAPPING. ! question: 8 section: 1 line_1: We do not have any additional requests. ! question: 9 section: 1 line_1: For a description of previous HST programs and list of publications line_2: please consult our Phase I proposal. ! question: 10 section: 1 line_1: The data will be analyzed on the JHU FOS cluster of Sun workstations. line_2: The communications network within the cluster and the connection to line_3: other networks is provided by the JHU Department of Physics and Astronomy. ! !end of general form text general_form_address: lname: FORD fname: HOLLAND mi: C category: PI inst: JOHNS HOPKINS UNIVERSITY addr_1: DEPARTMENT OF PHYSICS AND ASTRONOMY addr_2: HOMEWOOD CAMPUS city: BALTIMORE state: MD zip: 21218 country: USA phone: 516-8653/338-4803 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC1052-OFFSET descr_1: A,140 pos_1: PLATE-ID=00DW, pos_2: RA = 2H 41M 3.46S +/- 0.3", pos_3: DEC = -8D 16' 36.3" +/- 0.3" equinox: 2000 comment_1: THIS IS THE GSC MAG. comment_2: B-V ESTIMATED FROM comment_3: GROUND-BASED CCD IMAGES. fluxnum_1: 1 fluxval_1: V=15.29 fluxnum_2: 1 fluxval_2: B-V=0.3 ! targnum: 2 name_1: NGC1052-NUC descr_1: E,317 pos_1: RA-OFF = 1.2415S +/- 0.004S, pos_2: DEC-OFF = +75.558" +/- 0.02", pos_3: FROM 1 equinox: 2000 rv_or_z: V=1507 comment_1: THIS IS THE 0.5" CONTINUUM FLUX comment_2: CALCULATED FROM OUR F547M PC comment_3: IMAGE. fluxnum_1: 1 fluxval_1: F(5470)=4.0 +/- 0.2 E-16 ! targnum: 3 name_1: NGC4258-OFFSET descr_1: A,140 pos_1: PLATE-ID=024D, pos_2: RA = 12H 18M 47.43S +/- 1.2", pos_3: DEC = +47D 18' 21.0" +/- 1.2" equinox: 2000 comment_1: THIS IS THE GSC MAG. fluxnum_1: 1 fluxval_1: V=15.15 ! targnum: 4 name_1: NGC4258-NUC descr_1: E,317 pos_1: RA-OFF = 10.0765S +/- 0.004S, pos_2: DEC-OFF = -6.376" +/- 0.02", pos_3: FROM 3 equinox: 2000 rv_or_z: V=448 comment_1: THIS IS THE 0.5" CONTINUUM FLUX comment_2: CALCULATED FROM OUR F547M PC comment_3: IMAGE. fluxnum_1: 1 fluxval_1: F(5470)=5.82 +/- 0.2 E-15 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.100 targname: NGC1052-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 11.64S priority: 1 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 1.11 ! linenum: 1.110 targname: NGC1052-OFFSET config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 10S priority: 1 param_1: SEARCH-SIZE-X=3, param_2: SCAN-STEP-X=0.15, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-Y=0.15 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 1.200 ! linenum: 1.200 targname: NGC1052-NUC config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 60S priority: 1 param_1: SEARCH-SIZE-X=3, param_2: SCAN-STEP-X=0.12, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-Y=0.12 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 1.300-1.7; req_3: GROUP 1.3-1.8 NO GAP ! linenum: 1.300 targname: NGC1052-NUC config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G190H num_exp: 1 time_per_exp: 4020S priority: 1 req_1: CYCLE 3 ! linenum: 1.400 targname: NGC1052-NUC config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G270H num_exp: 1 time_per_exp: 1500S priority: 1 req_1: CYCLE 3 ! linenum: 1.500 targname: NGC1052-NUC config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G400H num_exp: 1 time_per_exp: 1200S priority: 1 req_1: CYCLE 3 ! linenum: 1.600 targname: NGC1052-NUC config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G570H num_exp: 1 time_per_exp: 1200S priority: 1 req_1: CYCLE 3 ! linenum: 1.700 targname: NGC1052-NUC config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 120S priority: 1 param_1: SEARCH-SIZE-X=3, param_2: SCAN-STEP-X=0.12, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-Y=0.12 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 1.8 ! linenum: 1.800 targname: NGC1052-NUC config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G130H num_exp: 1 time_per_exp: 7560S priority: 1 req_1: CYCLE 3 ! linenum: 2.100 targname: NGC4258-OFFSET config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.0S priority: 1 param_1: SEARCH-SIZE-X=1, param_2: SEARCH-SIZE-Y=3, param_3: SCAN-STEP-Y=1.4 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 2.101 ! linenum: 2.101 targname: NGC4258-OFFSET config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 1.5S priority: 1 param_1: SEARCH-SIZE-X=6, param_2: SEARCH-SIZE-Y=2, param_3: SCAN-STEP-X=0.7, param_4: SCAN-STEP-Y=0.7 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 2.11 ! linenum: 2.110 targname: NGC4258-OFFSET config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 10S priority: 1 param_1: SEARCH-SIZE-X=3, param_2: SCAN-STEP-X=0.15, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-Y=0.15 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 2.200 ! linenum: 2.200 targname: NGC4258-NUC config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 60S priority: 1 param_1: SEARCH-SIZE-X=3, param_2: SCAN-STEP-X=0.12, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-Y=0.12 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 2.300-2.7; req_3: GROUP 2.3-2.8 NO GAP ! linenum: 2.300 targname: NGC4258-NUC config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G190H num_exp: 1 time_per_exp: 4020S priority: 1 req_1: CYCLE 3 ! linenum: 2.400 targname: NGC4258-NUC config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G270H num_exp: 1 time_per_exp: 1500S priority: 1 req_1: CYCLE 3 ! linenum: 2.500 targname: NGC4258-NUC config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G400H num_exp: 1 time_per_exp: 1200S priority: 1 req_1: CYCLE 3 ! linenum: 2.600 targname: NGC4258-NUC config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G570H num_exp: 1 time_per_exp: 1200S priority: 1 req_1: CYCLE 3 ! linenum: 2.700 targname: NGC4258-NUC config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 120S priority: 1 param_1: SEARCH-SIZE-X=3, param_2: SCAN-STEP-X=0.12, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-Y=0.12 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 2.8 ! linenum: 2.800 targname: NGC4258-NUC config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G130H num_exp: 1 time_per_exp: 7560S priority: 1 req_1: CYCLE 3 ! ! end of exposure logsheet ! No scan data records found