! File: 2295C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:04:49:20 coverpage: title_1: BLACK HOLES IN ELLIPTICAL GALAXIES sci_cat: GALAXIES & CLUSTERS sci_subcat: NUCLEI/CORES proposal_for: GO pi_title: DR. pi_fname: GIUSEPPINA pi_lname: FABBIANO pi_inst: CFA pi_country: USA pi_phone: 617-495-7203 hours_pri: 4.50 num_pri: 8 foc: Y funds_amount: 46963 funds_length: 12 funds_date: JUN-90 off_fname: GEORGE off_mi: D off_lname: DICK off_title: MANAGER off_inst: SMITHSONIAN INSTITUTION off_addr_1: 60 GARDEN STREET off_city: CAMBRIDGE off_state: MA off_zip: 02138 off_country: USA off_phone: 617-495-7401 off_telex: 921428 ! end of coverpage abstract: line_1: We propose to observe at high resolution the central regions of eight line_2: early-type galaxies, for which X-ray and radio continuum data are available. line_3: Four of these have radio core power comparable with that of M87, and four are line_4: radio quiet. We seek to measure the UV emission of a nonthermal nuclear source, line_5: and/or to find evidence of a central stellar spike, which could indicate the line_6: presence of a central mass concentration. These measurements will enable us to line_7: investigate the origin of nuclear activity in ellipticals with particular line_8: reference on the mass of the central black hole as a crucial element. ! ! end of abstract general_form_proposers: lname: TRINCHIERI fname: GINEVRA inst: CFA country: USA ! lname: FABBIANO fname: GIUSEPPINA title: P.I. inst: CFA country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 0 line_1: We have selected eight bright elliptical galaxies of similar optical and line_2: x-ray luminosities (Mv ~ -21;-23 and Lx ~1-6 x 10exp(41) line_3: ergs/s), but with quite different radio power and line_4: morphology. Three of these galaxies host extended, double lobed radio line_5: sources, with a powerful radio nucleus; one has a compact central line_6: source; the others have a low level line_7: radio emission, with low luminosities and small spatial extent. line_8: Similar objects are included in the GTO observing programs, usually line_9: in studies of the nuclei and central regions of normal galaxies, but line_10: with no specific emphasis in comparing similar objects with vastly line_11: different radio properties. Three galaxies are in common with the GTO line_12: program, and we propose complementary observations to those. line_13: The program galaxies are bright and nearby (mb ~ 10-13, D ~ line_14: 20-150 Mpc), and the FOC F/96 resolution corresponds to linear line_15: resolutions of 2-20 pc. We shall observe each galaxy in three wide line_16: band filters, in the ultraviolet, blue and red bands: F175W, F342W and line_17: F480LP. The exposure times are calculated to provide a line_18: S/N of 10 in each filter. We want to obtain colors in the line_19: optical band, that will extend to the very inner regions the shape of line_20: the stellar continuum observed at larger radii. They will also line_21: provide the normal stellar profile at small radii, so that we can line_22: discern a stellar cusp from a non-thermal point source, which should be line_23: more prominent in the ultraviolet. ! question: 4 section: 0 line_1: The aim of our program is to observe the signature of a central mass line_2: concentration, which should give rise, if present, to a stellar spike, line_3: as observed in M87 (Young et al. 1978, Ap. J. 221, line_4: 721). The high resolution of HST, corresponding to a linear resolution line_5: of < 2 pc for the closer galaxies, and of ~ 20 pc for the line_6: farthest, will allow the detection of a small light concentration over line_7: the stellar background. The availability of high resolution imaging in line_8: the ultraviolet adds crucial information in obtaining reliable line_9: parameters for a central compact nucleus. Typical elliptical galaxies line_10: show a rapid decline in their ultraviolet spectra, with a drop in the line_11: continuum of a factor of 15 between emission around 3600 A and 2000 line_12: A. A non-thermal source will then be enhanced against the weaker line_13: background by an equivalent amount. line_14: For one of the radio loud galaxies, IC 4296, ground based observations line_15: suggest this possibility. These observations are not able to resolve the line_16: emission from this source against the strong galactic starlight. The line_17: small pixel size of the FOC F/96, corresponding to 6 pc, is line_18: crucial for this purpose, because it will reduce the average starlight line_19: contamination in the central pixels and enhance the contrast for the line_20: detection of a central point source. The average surface brightness of line_21: 18 mb arcsecexp(-2) observed in the central few arcsec will be line_22: reduced to an average mb 26 per pixel (if the surface line_23: brightness has a flat distribution). ! question: 5 section: 0 line_1: The observations of these eight galaxies, complemented by the GTO line_2: program, will be able to provide good optical and ultraviolet data for line_3: the central regions of galaxies with similar x-ray and optical line_4: properties and vastly different radio characteristics, to study the line_5: range of parameters for central compact sources and their relation to line_6: the radio activity of elliptical and S0 galaxies. line_7: If we assume M87 as a model galaxy on which to base our expectations, line_8: which has comparable radio nuclear luminosities to the radio loud line_9: galaxies, a central spike (in M87, mv 16.5, from Young et line_10: 1978, Ap. J. 221, 721) should have mv = 20 at line_11: the distance of the radio loud objects. For a central surface line_12: brightness of 16-18 V magnitudes arcsecexp(-2), the source should be line_13: evident against an average surface brightness from stellar light of line_14: 24-26 per FOC pixel. With our exposure times, we should moreover be line_15: able to detect point sources of about 24 mag in each band (S/N line_16: 3), which will ensure the detection of much fainter nuclei than line_17: the M87 example. line_18: The set of three filter observations, including one minute per line_19: observation for a filter change, gives observation lenghts for each line_20: galaxy close to the optimum time of 45 minutes. ! question: 7 section: 0 line_1: Initial data reduction and analysis will be performed at STScI so that line_2: we may become familiar with the details of the FOC and its operation line_3: and with S/W tools. SAO will have the complete HST IRAF package line_4: running on its SUN network, so that the bulk of the data analysis line_5: will be done at SAO. ! question: 10 section: 0 line_1: Resources to be supplied by the Smithsonian Institution in support of line_2: the project include a fully supported SUN network consisting of line_3: individual workstations and system S/W. The system presently runs line_4: IRAF and is planned to support the STScI data analysis system. An line_5: image processing laboratory is also available. ! !end of general form text general_form_address: lname: FABBIANO fname: GIUSEPPINA title: DR. category: PI inst: SMITHSONIAN INSTITUTION addr_1: 60 GARDEN STREET city: CAMBRIDGE state: MA zip: 02138 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC1316 descr_1: GALAXY; EARLY TYPE; CORE pos_1: RA = 03H 20M 47.209S +/- 0.015S, pos_2: DEC = -37D 23' 08.22" +/- 0.23" equinox: 1950 fluxnum_1: 1 fluxval_1: B = 23 ! targnum: 2 name_1: NGC3998 descr_1: GALAXY; EARLY TYPE; CORE pos_1: RA = 11H 55M 20.9S +/- 1", pos_2: DEC = +55D 43' 54.6" +/- 1" equinox: 1950 fluxnum_1: 1 fluxval_1: B = 23 ! targnum: 3 name_1: NGC4382 descr_1: GALAXY; EARLY TYPE; CORE pos_1: RA = 12H 22M 53.2S +/- 4", pos_2: DEC = +18D 28' 03" +/- 4" equinox: 1950 fluxnum_1: 1 fluxval_1: B = 23 ! targnum: 4 name_1: NGC4636 descr_1: GALAXY; EARLY TYPE; CORE pos_1: RA = 12H 40M 16.68S +/- 0.5", pos_2: DEC = +02D 57' 41.4" +/- 0.5" equinox: 1950 fluxnum_1: 1 fluxval_1: B = 23 ! targnum: 5 name_1: IC4296 descr_1: GALAXY; EARLY TYPE; CORE pos_1: RA = 13H 33M 47.18S +/- 0.1", pos_2: DEC = -33D 42' 39.4" +/- 0.1" equinox: 1950 fluxnum_1: 1 fluxval_1: B = 23 ! targnum: 6 name_1: NGC5846 descr_1: GALAXY; EARLY TYPE; CORE pos_1: RA = 15H 03M 56.9S +/- 2", pos_2: DEC = +01D 47' 52.5" +/- 2" equinox: 1950 fluxnum_1: 1 fluxval_1: B = 23 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: NGC1316 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F480LP,F1ND,F2ND num_exp: 1 time_per_exp: 460S s_to_n: 3 fluxnum_1: 1 priority: 1 req_1: CYCLE 1 / 1-18 ! linenum: 2.000 targname: NGC1316 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F342W,F1ND num_exp: 1 time_per_exp: 240S s_to_n: 3 fluxnum_1: 1 priority: 1 ! linenum: 3.000 targname: NGC1316 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F175W num_exp: 1 time_per_exp: 2040S s_to_n: 3 fluxnum_1: 1 priority: 1 ! linenum: 4.000 targname: NGC3998 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F480LP,F1ND,F2ND num_exp: 1 time_per_exp: 460S s_to_n: 3 fluxnum_1: 1 priority: 2 ! linenum: 5.000 targname: NGC3998 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F342W,F1ND num_exp: 1 time_per_exp: 240S s_to_n: 3 fluxnum_1: 1 priority: 2 ! linenum: 6.000 targname: NGC3998 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F175W num_exp: 1 time_per_exp: 2040S s_to_n: 3 fluxnum_1: 1 priority: 2 ! linenum: 7.000 targname: NGC4382 config: FOC/48 opmode: IMAGE aperture: 512X512 sp_element: F430W num_exp: 1 time_per_exp: 460S s_to_n: 3 fluxnum_1: 1 priority: 3 ! linenum: 8.000 targname: NGC4382 config: FOC/48 opmode: IMAGE aperture: 512X512 sp_element: F342W num_exp: 1 time_per_exp: 240S s_to_n: 3 fluxnum_1: 1 priority: 3 ! linenum: 9.000 targname: NGC4382 config: FOC/48 opmode: IMAGE aperture: 512X512 sp_element: F175W num_exp: 1 time_per_exp: 2040S s_to_n: 3 fluxnum_1: 1 priority: 3 ! linenum: 10.000 targname: NGC4636 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F480LP num_exp: 1 time_per_exp: 460S s_to_n: 3 fluxnum_1: 1 priority: 1 ! linenum: 11.000 targname: NGC4636 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F342W num_exp: 1 time_per_exp: 240S s_to_n: 3 fluxnum_1: 1 priority: 1 ! linenum: 12.000 targname: NGC4636 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F175W num_exp: 1 time_per_exp: 2040S s_to_n: 3 fluxnum_1: 1 priority: 1 ! linenum: 13.000 targname: IC4296 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F480LP num_exp: 1 time_per_exp: 460S s_to_n: 3 fluxnum_1: 1 priority: 1 ! linenum: 14.000 targname: IC4296 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F342W num_exp: 1 time_per_exp: 240S s_to_n: 3 fluxnum_1: 1 priority: 1 ! linenum: 15.000 targname: IC4296 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F175W num_exp: 1 time_per_exp: 2040S s_to_n: 3 fluxnum_1: 1 priority: 1 ! linenum: 16.000 targname: NGC5846 config: FOC/48 opmode: IMAGE aperture: 512X512 sp_element: F430W num_exp: 1 time_per_exp: 460S s_to_n: 3 fluxnum_1: 1 priority: 2 ! linenum: 17.000 targname: NGC5846 config: FOC/48 opmode: IMAGE aperture: 512X512 sp_element: F342W num_exp: 1 time_per_exp: 240S s_to_n: 3 fluxnum_1: 1 priority: 2 ! linenum: 18.000 targname: NGC5846 config: FOC/48 opmode: IMAGE aperture: 512X512 sp_element: F175W num_exp: 1 time_per_exp: 2040S s_to_n: 3 fluxnum_1: 1 priority: 2 ! ! end of exposure logsheet ! No scan data records found