COVERPAGE: TITLE_1: UV SPECTRAL DISTRIBUTION IN LOW LUMINOSITY ACTIVE GALAXIES - TITLE_2: IMAGING: CYCLE 4 MEDIUM SCI_CAT: QUASARS & AGN SCI_SUBCAT: OTHER ACTIVE NUCLEI PROPOSAL_FOR: GO PI_FNAME: ANURADHA PI_MI: P. PI_LNAME: KORATKAR PI_INST: 3470 PI_COUNTRY: USA PI_PHONE: (410) 338-4470 HOURS_PRI: 12.84 NUM_PRI: 4 WF_PC: Y OFF_FNAME: HERVEY OFF_LNAME: STOCKMAN OFF_TITLE: DEPUTY DIRECTOR OFF_INST: 3470 OFF_ADDR_1: 3700 SAN MARTIN DRIVE OFF_CITY: BALTIMORE OFF_STATE: MD OFF_ZIP: 21218 OFF_COUNTRY: USA OFF_PHONE: (410) 338-4730 ABSTRACT: LINE_1: Observations of activity in the nuclei of galaxies from the most LINE_2: energetic (QSOs) to the mildly energetic (LINERs) show that many of the LINE_3: properties are similar and the objects might be related to each other. LINE_4: A crucial question that arises is, ``Is the basic mechanism that powers LINE_5: the activity the same in all these galaxies and do the properties of LINE_6: active nuclei just scale with luminosity\?'' Many studies suggest that LINE_7: QSOs and luminous Seyfert nuclei have the same basic energy source. LINE_8: This continuity of properties suggests an extension to still lower LINE_9: luminosities, but there might be a lower limit to the activity LINE_10: (analogous to the mass limit in main sequence stars). Hence, it is LINE_11: important to determine whether Low Luminosity AGNs (LLAGNs; or a LINE_12: certain sub-class of them) are genuinely related to classical AGNs, or LINE_13: whether instead their properties might be due to other physical LINE_14: processes. In this proposal we request FOS and PC observations of 4 LINE_15: LLAGNs (detected with ROSAT) to determine the physical processes LINE_16: responsible for UV radiation in these objects. The results of this LINE_17: analysis will not only help bridge the gap between LLAGNs and normal LINE_18: galaxies, but answer the following question: How similar are the LINE_19: LLAGNs to the higher luminosity AGNs\? More specifically, what is the LINE_20: dominant mechanism for the production of ionizing radiation\? GENERAL_FORM_PROPOSERS: LNAME: KORATKAR FNAME: ANURADHA MI: P. INST: 3470 COUNTRY: USA LNAME: DEUSTUA FNAME: SUSANA MI: E. INST: 2460 COUNTRY: USA LNAME: EVANS FNAME: IAN MI: N. INST: 3470 COUNTRY: USA LNAME: FILIPPENKO FNAME: ALEXEI MI: V. INST: 1500 COUNTRY: USA LNAME: HECKMAN FNAME: TIMOTHY MI: M. INST: 3470 COUNTRY: USA LNAME: HO FNAME: LUIS MI: C. INST: 1500 COUNTRY: USA GENERAL_FORM_ADDRESS: LNAME: KORATKAR FNAME: ANURADHA MI: P. CATEGORY: PI INST: 3470 ADDR_1: 3700 SAN MARTIN DRIVE CITY: BALTIMORE STATE: MD ZIP: 21218 COUNTRY: USA PHONE: (410) 338-4470 TELEX: KORATKAR@STSCI.EDU GENERAL_FORM_TEXT: QUESTION: 3 SECTION: 1 LINE_1: We plan to use the WFPC2 PC to observe the objects in our sample using LINE_2: four filters to determine the spatial extent of the nuclear UV LINE_3: continuum source for comparison with X-ray imaging data. Since the LINE_4: spatial resolution of the WFPC2 PC is an order of magnitude better than LINE_5: the ROSAT HRI resolution, the morphology of the UV continuum source will LINE_6: enable us to investigate the central source on much smaller spatial LINE_7: scales than would otherwise be possible. We have selected the F218W LINE_8: filter because of its high UV efficiency and the absence of strong UV LINE_9: emission lines in the filter bandpass. The WFPC2 images in the LINE_10: F300W, F439W and F547M will be used not only to determine the LINE_11: spatial extent of the nuclear source , but will also be used to LINE_12: determine the spectral energy distribution of the nuclear LINE_13: source. LINE_14: The targets should be placed at the PC1 aperture position, with the LINE_15: exposures split 1:1 to maximize our dynamic range given the uncertain LINE_16: UV flux distribution. QUESTION: 4 SECTION: 1 LINE_1: These observations can only be obtained in the satellite ultraviolet. LINE_2: We have obtained all relevant IUE data relating to the nuclei of the LINE_3: objects in this sample. The brightest of the the objects in our sample LINE_4: was observed by IUE, but the S/N is very low. The UV continua of these LINE_5: objects is too faint to obtain adequate S/N using IUE. We have observed LINE_6: the objects in this sample using the ROSAT HRI imager, and have LINE_7: recently been awarded ROSAT PSPC time to obtain X-ray spectra for these LINE_8: targets. We also have high resolution optical imaging data and optical LINE_9: spectra of these objects. LINE_10: It is possible that the blue bump could be a major contributor to the LINE_11: energy budget for these objects. Therefore, HST data in the LINE_12: effectively unobserved UV waveband are critical to understanding the LINE_13: spectral energy distribution for these objects. LINE_14: We have estimated the nuclear continuum flux we expect from the nuclei LINE_15: of these objects from the UV/H-BETA and UV/X-ray luminosity LINE_16: correlations for AGNs. The predicted flux for all of these objects is LINE_17: similar to 1.0E-15 erg/cms^2/s/A, consistent with that determined from LINE_18: the existing NGC 5273 IUE data. We have therefore assumed that the LINE_19: nuclear continuum flux will be present at this level in our exposure LINE_20: time calculations. Since we do not have additional UV flux LINE_21: information for any of the objects in the sample, we have assumed the LINE_22: same exposure times for each object. The WFPC2 exposure times have LINE_23: been chosen so as not to saturate the CCD even in the unlikely event QUESTION: 4 SECTION: 2 LINE_1: that all of the nuclear flux arises from a point source, and to provide LINE_2: a mean S/N ratio per pixel of approx. 20:1 if the emission is extended LINE_3: 1". QUESTION: 5 SECTION: 1 LINE_1: All observations must occur within 2 days after a WFPC2 decontamination. QUESTION: 6 SECTION: 1 LINE_1: None. QUESTION: 7 SECTION: 1 LINE_1: Post-reduction analysis of the data will be performed using the IRAF LINE_2: and STSDAS packages. The images will be analysed to determine the LINE_3: extent of the UV emission. The spectra will be analysed for both the LINE_4: absorption and emission feature. The line intensities will be used to LINE_5: investigate the properties of the emission-line gas. LINE_6: LINE_7: The roles of the investigators are as follows: LINE_8: A. Koratkar - Project direction, processing techniques, data analysis, LINE_9: interpretation and publication. LINE_10: S. Deustua - Data analysis and interpretation. LINE_11: I. Evans - Instrumental effects, processing techniques, data LINE_12: analysis, and interpretation. LINE_13: A. Filippenko - Data analysis and interpretation. LINE_14: T. Heckman - Data analysis and interpretation. LINE_15: L. Ho - Data analysis and interpretation. QUESTION: 8 SECTION: 1 LINE_1: None. QUESTION: 9 SECTION: 1 LINE_1: 3591 - "Massive Stars in Starburst Galaxies" (Heckman, PI) LINE_2: 3837 - "Sectropolarimetry of Low Red-shift Active Galactic Nuclei: Test LINE_3: of the Quasar Emission Mechanism" (Koratkar, PI) LINE_4: 4302 - "Supernovae and their Local Environment" (Filippenko, PI) LINE_5: 4312 - "Circumstellar Matter around Supernovae" (Filippenko, PI) LINE_6: 4340 - "Origin of Blue Featureless Continuum in Seyfert 2 Nuclei" LINE_7: (Filippenko, PI; Ho, Co-I) LINE_8: 4350 - "FOS Observations of LINER Galaxy Nuclei" (Filippenko & Ho, Co-I) LINE_9: 4364 - "Ultraviolet and Optical Nebular Diagnostics for Photoionization LINE_10: and Shock Heated Emission Line Gas" (Evans PI, Koratkar Co-I) LINE_11: 4370 - "Space-UV Imaging of Nearby Powerful Radio Galaxies" (Heckman, LINE_12: PI) LINE_13: 4967 - "Carbon, Nitrogen, and Oxygen abundances in Nearby Seyfert LINE_14: Galaxies" (Koratkar, PI, Evans Co-I) LINE_15: Except for 4350 none of the above programs are related to this LINE_16: proposal. The main emphasis of 4350 is on measuring emission to LINE_17: determine excitation mechanism and absorption lines to detect hot, LINE_18: young stars. Observations for the program 3837, 4370 have not yet LINE_19: begun. Observations for 3591 are currently in progress. Data for LINE_20: programs 4364, and 4967 have only recently been obtained, and are LINE_21: being analyzed. 2590 and 3507 have been completed and the results are LINE_22: in press and these programs are not mentioned above. Data for others LINE_23: have not yet been obtained. QUESTION: 9 SECTION: 2 LINE_1: "HST Imaging of the Inner 3 Arcseconds of NGC1068 in the light of LINE_2: [OIII] 5007", Evans, I.N., Ford, H.C., Kinney, A.L., Antonucci, R.R.J., LINE_3: Armus, L. & Caganoff, S., Ap.J.Lett., 369, L31, 1991. LINE_4: "Faint Object Spectrograph Spectroscopy of Resolved Structure in the LINE_5: Nucleus of NGC1068", Caganoff, S., Antonucci, R.R.J., Ford, H.C., Kriss, LINE_6: G.A., Hartig, G., Armus, L., Evans, I.N., Rosenblatt, E., Bohlin, R.C., LINE_7: & Kinney, A.L., Ap.J.Lett., 377, L9, 1991. LINE_8: "Hubble Space Telescope Imaging of the Narrow Line Region of NGC 4151", LINE_9: Evans, I.N., Tsvetanov, Z., Kriss, G.A., Ford, H.C., Caganoff, S., & LINE_10: Koratkar, A.P., Ap. J., in press, 1993. LINE_11: "A Gravitational Lens Candidate Discovered with the Hubble Space LINE_12: Telescope," Maoz, D., Bahcall, J.N., Schneider, D.P., Doxsey, R., LINE_13: Bahcall, N.A., Filippenko, A.V., Goss, W.M., Lahav, O., & Sargent, LINE_14: W.L.W., Ap.J.Lett., 386, L1, 1992. LINE_15: "HST Observations of NGC 4395, the Least Luminous Seyfert 1 Nucleus: LINE_16: Evidence Against the Starburst Hypothesis for Broad-Lined Active LINE_17: Galactic Nuclei," Filippenko, A.V., Ho, L.C., & Sargent, W.L.W., LINE_18: Ap.J.Lett., in press. LINE_19: "NGC 4395: Evidence Against the Starburst Hypothesis for Seyfert 1 LINE_20: Nuclei and QSOs," Filippenko, A.V., Ho, L.C., & Sargent, W.L.W., in LINE_21: 16th Texas Symposium/3rd Symposium on Particles, Strings, and LINE_22: Cosmology, ed. C. Akerlof and M. Srednicki (New York: New York Academy LINE_23: of Sciences), 1993, in press. QUESTION: 10 SECTION: 1 LINE_1: The investigators on this proposal have access to the standard data LINE_2: analysis and research support facilities provided by their home LINE_3: institutions. No special support for this project will be provided by LINE_4: any of the proposers' home institutions. ! This is the end of the General Form FIXED_TARGETS: TARGNUM: 1 NAME_1: NGC4278 DESCR_1: E,303,312,910,923,924 POS_1: RA = 12H 20M 06.83S +/- 2.0", POS_2: DEC = +29D 16' 50.2" +/- 2.0", POS_3: PLATE-ID = 00DJ EQUINOX: J2000 RV_OR_Z: V = +649 FLUXNUM_1: 1 FLUXVAL_1: V = 16.3 ! TARGNUM: 2 NAME_1: NGC4639 DESCR_1: E,301,312,910,923,924 POS_1: RA = 12H 42M 52.59S +/- 2.0", POS_2: DEC = +13D 15' 30.3" +/- 2.0", POS_3: PLATE-ID = 00IY EQUINOX: J2000 RV_OR_Z: V = +1010 FLUXNUM_1: 1 FLUXVAL_1: V = 16.3 ! TARGNUM: 3 NAME_1: NGC5033 DESCR_1: E,303,312,910,923,924 POS_1: RA = 13H 13M 27.82S +/- 2.0", POS_2: DEC = +36D 35' 39.9" +/- 2.0", POS_3: PLATE-ID = 01PR EQUINOX: J2000 RV_OR_Z: V = +878 FLUXNUM_1: 1 FLUXVAL_1: V = 16.3 ! TARGNUM: 4 NAME_1: NGC5273 DESCR_1: E,303,312,910,923,924 POS_1: RA = 13H 42M 08.33S +/- 2.0", POS_2: DEC = +35D 39' 15.2" +/- 2.0", POS_3: PLATE-ID = 01QW EQUINOX: J2000 RV_OR_Z: V = +1054 FLUXNUM_1: 1 FLUXVAL_1: V = 16.3 EXPOSURE_LOGSHEET: LINENUM: 1.000 TARGNAME: NGC4278 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1 SP_ELEMENT: F218W PARAM_1: CR-SPLIT=0.5 NUM_EXP: 1 TIME_PER_EXP: 4500S PRIORITY: 1 REQ_1: CYCLE 4 / 1-4.3; REQ_2: GROUP 1-1.2 NO GAP; REQ_3: SAME POS FOR 1.1-1.2 AS 1 ! LINENUM: 1.100 TARGNAME: NGC4278 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1 SP_ELEMENT: F300W PARAM_1: CR-SPLIT=0.5 NUM_EXP: 1 TIME_PER_EXP: 2000S PRIORITY: 1 ! LINENUM: 1.200 TARGNAME: NGC4278 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1 SP_ELEMENT: F439W PARAM_1: CR-SPLIT=0.5 NUM_EXP: 1 TIME_PER_EXP: 1500S PRIORITY: 1 ! LINENUM: 2.000 TARGNAME: NGC4639 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1 SP_ELEMENT: F218W PARAM_1: CR-SPLIT=0.5 NUM_EXP: 1 TIME_PER_EXP: 4500S PRIORITY: 1 REQ_1: GROUP 2-2.3 NO GAP; REQ_2: SAME POS FOR 2.1-2.3 AS 2 ! LINENUM: 2.100 TARGNAME: NGC4639 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1 SP_ELEMENT: F300W PARAM_1: CR-SPLIT=0.5 NUM_EXP: 1 TIME_PER_EXP: 2000S PRIORITY: 1 ! LINENUM: 2.200 TARGNAME: NGC4639 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1 SP_ELEMENT: F439W PARAM_1: CR-SPLIT=0.5 NUM_EXP: 1 TIME_PER_EXP: 1500S PRIORITY: 1 ! LINENUM: 2.300 TARGNAME: NGC4639 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1 SP_ELEMENT: F547M PARAM_1: CR-SPLIT=0.5 NUM_EXP: 1 TIME_PER_EXP: 495S PRIORITY: 1 ! LINENUM: 3.000 TARGNAME: NGC5033 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1 SP_ELEMENT: F218W PARAM_1: CR-SPLIT=0.5 NUM_EXP: 1 TIME_PER_EXP: 4500S PRIORITY: 1 REQ_1: GROUP 3-3.3 NO GAP; REQ_2: SAME POS FOR 3.1-3.3 AS 3 ! LINENUM: 3.100 TARGNAME: NGC5033 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1 SP_ELEMENT: F300W PARAM_1: CR-SPLIT=0.5 NUM_EXP: 1 TIME_PER_EXP: 2000S PRIORITY: 1 ! LINENUM: 3.200 TARGNAME: NGC5033 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1 SP_ELEMENT: F439W PARAM_1: CR-SPLIT=0.5 NUM_EXP: 1 TIME_PER_EXP: 1500S PRIORITY: 1 ! LINENUM: 3.300 TARGNAME: NGC5033 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1 SP_ELEMENT: F547M PARAM_1: CR-SPLIT=0.5 NUM_EXP: 1 TIME_PER_EXP: 495S PRIORITY: 1 ! LINENUM: 4.000 TARGNAME: NGC5273 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1 SP_ELEMENT: F218W PARAM_1: CR-SPLIT=0.5 NUM_EXP: 1 TIME_PER_EXP: 4500S PRIORITY: 1 REQ_1: GROUP 4-4.3 NO GAP; REQ_2: SAME POS FOR 4.1-4.3 AS 4 ! LINENUM: 4.100 TARGNAME: NGC5273 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1 SP_ELEMENT: F300W PARAM_1: CR-SPLIT=0.5 NUM_EXP: 1 TIME_PER_EXP: 2000S PRIORITY: 1 ! LINENUM: 4.200 TARGNAME: NGC5273 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1 SP_ELEMENT: F439W PARAM_1: CR-SPLIT=0.5 NUM_EXP: 1 TIME_PER_EXP: 1500S PRIORITY: 1 ! LINENUM: 4.300 TARGNAME: NGC5273 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1 SP_ELEMENT: F547M PARAM_1: CR-SPLIT=0.5 NUM_EXP: 1 TIME_PER_EXP: 495S PRIORITY: 1 ! ! End of RPSS template