Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 5381 Report Date: 18-Jul-95:17:16 Version: ********** Check-in Date: ********** 1.Proposal Title: UV SPECTRAL DISTRIBUTION IN LOW LUMINOSITY ACTIVE GALAXIES - IMAGING: CYCLE 4 MEDIUM ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID QUASARS & AGN GO Sub Category OTHER ACTIVE NUCLEI ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone Anuradha P. Koratkar 3470 USA (410) 338-4470 ------------------------------------------------------------------------------------ 7. Abstract Observations of activity in the nuclei of galaxies from the most energetic (QSOs) to the mildly energetic (LINERs) show that many of the properties are similar and the objects might be related to each other. A crucial question that arises is, ``Is the basic mechanism that powers the activity the same in all these galaxies and do the properties of active nuclei just scale with luminosity\?'' Many studies suggest that QSOs and luminous Seyfert nuclei have the same basic energy source. This continuity of properties suggests an extension to still lower luminosities, but there might be a lower limit to the activity (analogous to the mass limit in main sequence stars). Hence, it is important to determine whether Low Luminosity AGNs (LLAGNs; or a certain sub-class of them) are genuinely related to classical AGNs, or whether instead their properties might be due to other physical processes. In this proposal we request FOS and PC observations of 4 LLAGNs (detected with ROSAT) to determine the physical processes responsible for UV radiation in these objects. The results of this analysis will not only help bridge the gap between LLAGNs and normal galaxies, but answer the following question: How similar are the LLAGNs to the higher luminosity AGNs\? More specifically, what is the dominant mechanism for the production of ionizing radiation\? ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 12.84 par: 0 10. Num targs pri: 4 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: WF/PC ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 5381 PI: Anuradha P. Koratkar Proposal Title: UV SPECTRAL DISTRIBUTION IN LOW LUMINOSITY ACTIVE GALAXIES - IMAGING: CYCLE 4 MEDIUM ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Anuradha P. Koratkar 3470 USA Susana E. Deustua 2460 USA Ian N. Evans 3470 USA Alexei V. Filippenko 1500 USA Timothy M. Heckman 3470 USA Luis C. Ho 1500 USA ------------------------------------------------------------------------------------ 3. Description of proposed observations. We plan to use the WFPC2 PC to observe the objects in our sample using four filters to determine the spatial extent of the nuclear UV continuum source for comparison with X-ray imaging data. Since the spatial resolution of the WFPC2 PC is an order of magnitude better than the ROSAT HRI resolution, the morphology of the UV continuum source will enable us to investigate the central source on much smaller spatial scales than would otherwise be possible. We have selected the F218W filter because of its high UV efficiency and the absence of strong UV emission lines in the filter bandpass. The WFPC2 images in the F300W, F439W and F547M will be used not only to determine the spatial extent of the nuclear source , but will also be used to determine the spectral energy distribution of the nuclear source. The targets should be placed at the PC1 aperture position, with the exposures split 1:1 to maximize our dynamic range given the uncertain UV flux distribution. ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. These observations can only be obtained in the satellite ultraviolet. We have obtained all relevant IUE data relating to the nuclei of the objects in this sample. The brightest of the the objects in our sample was observed by IUE, but the S/N is very low. The UV continua of these objects is too faint to obtain adequate S/N using IUE. We have observed the objects in this sample using the ROSAT HRI imager, and have recently been awarded ROSAT PSPC time to obtain X-ray spectra for these targets. We also have high resolution optical imaging data and optical spectra of these objects. It is possible that the blue bump could be a major contributor to the energy budget for these objects. Therefore, HST data in the effectively unobserved UV waveband are critical to understanding the spectral energy distribution for these objects. We have estimated the nuclear continuum flux we expect from the nuclei of these objects from the UV/H-BETA and UV/X-ray luminosity correlations for AGNs. The predicted flux for all of these objects is similar to 1.0E-15 erg/cms^2/s/A, consistent with that determined from the existing NGC 5273 IUE data. We have therefore assumed that the nuclear continuum flux will be present at this level in our exposure time calculations. Since we do not have additional UV flux information for any of the objects in the sample, we have assumed the same exposure times for each object. The WFPC2 exposure times have been chosen so as not to saturate the CCD even in the unlikely event that all of the nuclear flux arises from a point source, and to provide a mean S/N ratio per pixel of approx. 20:1 if the emission is extended 1". ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. All observations must occur within 2 days after a WFPC2 decontamination. Page 3 ------------------------------------------------------------------------------------ 6. Description of special calibration exposures. None. ------------------------------------------------------------------------------------ 7. Data reduction and analysis plans. Post-reduction analysis of the data will be performed using the IRAF and STSDAS packages. The images will be analysed to determine the extent of the UV emission. The spectra will be analysed for both the absorption and emission feature. The line intensities will be used to investigate the properties of the emission-line gas. The roles of the investigators are as follows: A. Koratkar - Project direction, processing techniques, data analysis, interpretation and publication. S. Deustua - Data analysis and interpretation. I. Evans - Instrumental effects, processing techniques, data analysis, and interpretation. A. Filippenko - Data analysis and interpretation. T. Heckman - Data analysis and interpretation. L. Ho - Data analysis and interpretation. ------------------------------------------------------------------------------------ 8. Additional comments or special requests. None. ------------------------------------------------------------------------------------ 9. Description of previous HST work. 3591 - "Massive Stars in Starburst Galaxies" (Heckman, PI) 3837 - "Sectropolarimetry of Low Red-shift Active Galactic Nuclei: Test of the Quasar Emission Mechanism" (Koratkar, PI) 4302 - "Supernovae and their Local Environment" (Filippenko, PI) 4312 - "Circumstellar Matter around Supernovae" (Filippenko, PI) 4340 - "Origin of Blue Featureless Continuum in Seyfert 2 Nuclei" (Filippenko, PI; Ho, Co-I) 4350 - "FOS Observations of LINER Galaxy Nuclei" (Filippenko & Ho, Co-I) 4364 - "Ultraviolet and Optical Nebular Diagnostics for Photoionization and Shock Heated Emission Line Gas" (Evans PI, Koratkar Co-I) 4370 - "Space-UV Imaging of Nearby Powerful Radio Galaxies" (Heckman, PI) 4967 - "Carbon, Nitrogen, and Oxygen abundances in Nearby Seyfert Galaxies" (Koratkar, PI, Evans Co-I) Except for 4350 none of the above programs are related to this proposal. The main emphasis of 4350 is on measuring emission to determine excitation mechanism and absorption lines to detect hot, young stars. Observations for the program 3837, 4370 have not yet begun. Observations for 3591 are currently in progress. Data for programs 4364, and 4967 have only recently been obtained, and are being analyzed. 2590 and 3507 have been completed and the results are in press and these programs are not mentioned above. Data for others have not yet been obtained. "HST Imaging of the Inner 3 Arcseconds of NGC1068 in the light of [OIII] 5007", Evans, I.N., Ford, H.C., Kinney, A.L., Antonucci, R.R.J., Armus, L. & Caganoff, S., Ap.J.Lett., 369, L31, 1991. "Faint Object Spectrograph Spectroscopy of Resolved Structure in the Nucleus of NGC1068", Caganoff, S., Antonucci, R.R.J., Ford, H.C., Kriss, G.A., Hartig, G., Armus, L., Evans, I.N., Rosenblatt, E., Bohlin, R.C., & Kinney, A.L., Ap.J.Lett., 377, L9, 1991. "Hubble Space Telescope Imaging of the Narrow Line Region of NGC 4151", Evans, I.N., Tsvetanov, Z., Kriss, G.A., Ford, H.C., Caganoff, S., & Koratkar, A.P., Ap. J., in press, 1993. "A Gravitational Lens Candidate Discovered with the Hubble Space Telescope," Maoz, D., Bahcall, J.N., Schneider, D.P., Doxsey, R., Bahcall, N.A., Filippenko, A.V., Goss, W.M., Lahav, O., & Sargent, W.L.W., Ap.J.Lett., 386, L1, 1992. "HST Observations of NGC 4395, the Least Luminous Seyfert 1 Nucleus: Evidence Against the Starburst Hypothesis for Broad-Lined Active Galactic Nuclei," Filippenko, A.V., Ho, L.C., & Sargent, W.L.W., Ap.J.Lett., in press. "NGC 4395: Evidence Against the Starburst Hypothesis for Seyfert 1 Nuclei and QSOs," Filippenko, A.V., Ho, L.C., & Sargent, W.L.W., in 16th Texas Symposium/3rd Symposium on Particles, Strings, and Cosmology, ed. C. Akerlof and M. Srednicki (New York: New York Academy of Sciences), 1993, in press. Page 4 ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). The investigators on this proposal have access to the standard data analysis and research support facilities provided by their home institutions. No special support for this project will be provided by any of the proposers' home institutions. ------------------------------------------------------------------------------------ 11. Address Information Name: ANURADHA P. KORATKAR Category: PI Institution: 3470 Address: 3700 SAN MARTIN DRIVE City: BALTIMORE State: MD Zip Code: 21218 Country: USA Telephone: (410) 338-4470 Telex (or e-mail): KORATKAR@STSCI.EDU ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 5381 [ 5] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial |Acqui|FLX| Flux data No | Name | Description | Position |Eqnx | Vel. |Prblm|REF| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 1 NGC4278 E,303,312,910,923,924 RA = 12H 20M 06.83S +/- J2000 V = +649 1 V = 16.3 2.0", DEC = +29D 16' 50.2" +/- 2.0", PLATE-ID = 00DJ ------------------------------------------------------------------------------------------------------------------------------------ 2 NGC4639 E,301,312,910,923,924 RA = 12H 42M 52.59S +/- J2000 V = 1 V = 16.3 2.0", +1010 DEC = +13D 15' 30.3" +/- 2.0", PLATE-ID = 00IY ------------------------------------------------------------------------------------------------------------------------------------ 3 NGC5033 E,303,312,910,923,924 RA = 13H 13M 27.82S +/- J2000 V = +878 1 V = 16.3 2.0", DEC = +36D 35' 39.9" +/- 2.0", PLATE-ID = 01PR ------------------------------------------------------------------------------------------------------------------------------------ 4 NGC5273 E,303,312,910,923,924 RA = 13H 42M 08.33S +/- J2000 V = 1 V = 16.3 2.0", +1054 DEC = +35D 39' 15.2" +/- 2.0", PLATE-ID = 01QW ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5381 [ 6] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 1 NGC4278 WFPC2 IMAGE PC1 F218W CR-SPLIT=0.5 1 4500S 1 CYCLE 4 / 1-4.3 GROUP 1-1.2 NO GAP SAME POS FOR 1.1- 1.2 AS 1 ------------------------------------------------------------------------------------------------------------------------------------ 1.1 NGC4278 WFPC2 IMAGE PC1 F300W CR-SPLIT=0.5 1 2000S 1 ------------------------------------------------------------------------------------------------------------------------------------ 1.2 NGC4278 WFPC2 IMAGE PC1 F439W CR-SPLIT=0.5 1 1500S 1 ------------------------------------------------------------------------------------------------------------------------------------ 2 NGC4639 WFPC2 IMAGE PC1 F218W CR-SPLIT=0.5 1 4500S 1 GROUP 2-2.3 NO GAP SAME POS FOR 2.1- 2.3 AS 2 ------------------------------------------------------------------------------------------------------------------------------------ 2.1 NGC4639 WFPC2 IMAGE PC1 F300W CR-SPLIT=0.5 1 2000S 1 ------------------------------------------------------------------------------------------------------------------------------------ 2.2 NGC4639 WFPC2 IMAGE PC1 F439W CR-SPLIT=0.5 1 1500S 1 ------------------------------------------------------------------------------------------------------------------------------------ 2.3 NGC4639 WFPC2 IMAGE PC1 F547M CR-SPLIT=0.5 1 495S 1 ------------------------------------------------------------------------------------------------------------------------------------ 3 NGC5033 WFPC2 IMAGE PC1 F218W CR-SPLIT=0.5 1 4500S 1 GROUP 3-3.3 NO GAP SAME POS FOR 3.1- 3.3 AS 3 ------------------------------------------------------------------------------------------------------------------------------------ 3.1 NGC5033 WFPC2 IMAGE PC1 F300W CR-SPLIT=0.5 1 2000S 1 ------------------------------------------------------------------------------------------------------------------------------------ 3.2 NGC5033 WFPC2 IMAGE PC1 F439W CR-SPLIT=0.5 1 1500S 1 ------------------------------------------------------------------------------------------------------------------------------------ 3.3 NGC5033 WFPC2 IMAGE PC1 F547M CR-SPLIT=0.5 1 495S 1 ------------------------------------------------------------------------------------------------------------------------------------ 4 NGC5273 WFPC2 IMAGE PC1 F218W CR-SPLIT=0.5 1 4500S 1 GROUP 4-4.3 NO GAP SAME POS FOR 4.1- 4.3 AS 4 ------------------------------------------------------------------------------------------------------------------------------------ 4.1 NGC5273 WFPC2 IMAGE PC1 F300W CR-SPLIT=0.5 1 2000S 1 ------------------------------------------------------------------------------------------------------------------------------------ 4.2 NGC5273 WFPC2 IMAGE PC1 F439W CR-SPLIT=0.5 1 1500S 1 ------------------------------------------------------------------------------------------------------------------------------------ 4.3 NGC5273 WFPC2 IMAGE PC1 F547M CR-SPLIT=0.5 1 495S 1 ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 5381 [ 7] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations WFPC2 ------------------------------------------------------------------------------------------------------------------------------------ Opmodes IMAGE ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters CR-SPLIT=0.5 ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 12.84 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category QUASARS & AGN ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category OTHER ACTIVE NUCLEI ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements CYCLE 4 / 1-4.3; GROUP 1-1.2 NO GAP; SAME POS FOR 1.1-1.2 AS 1 GROUP 2-2.3 NO GAP; SAME POS FOR 2.1-2.3 AS 2 GROUP 3-3.3 NO GAP; SAME POS FOR 3.1-3.3 AS 3 GROUP 4-4.3 NO GAP; SAME POS FOR 4.1-4.3 AS 4 ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements F218W F300W F439W F547M ------------------------------------------------------------------------------------------------------------------------------------ Target Names NGC4278 NGC4639 NGC5033 NGC5273 ------------------------------------------------------------------------------------------------------------------------------------