! File: 4249C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:19:00:21 coverpage: title_1: BLACK HOLES, STELLAR DYNAMICS AND POPULATIONS IN THE NUCLEI OF A title_2: COMPLETE SAMPLE OF ELLIPTICAL GALAXIES - CONT OF 2607 sci_cat: GALAXIES & CLUSTERS proposal_for: GO longterm: 2 cont_id: 2607 pi_title: DR. pi_fname: WALTER pi_lname: JAFFE pi_inst: LEIDEN UNIVERSITY pi_country: NETHERLANDS pi_phone: 011-3171-275883 keywords_1: MASSIVE BLACK HOLES; GALACTIC NUCLEI; STELLAR keywords_2: DYNAMICS, STELLAR POPULATIONS, ACTIVITY hours_pri: 23.70 num_pri: 11 wf_pc: X foc: X fos: X funds_amount: 243602 funds_length: 24 funds_date: JUL-91 off_fname: W. off_mi: B. off_lname: BURTON off_title: DEPT. CHAIRMAN off_inst: LEIDEN OBSERVATORY off_addr_1: ASTRONOMY DEPARTMENT off_addr_2: UNIVERSITY OF LEIDEN off_addr_3: P.O. BOX 9513 off_city: LEIDEN off_zip: 2300 RA off_country: NETHERLANDS ! end of coverpage abstract: line_1: We will determine the prevalence of massive black holes in a complete sample of line_2: bright Virgo ellipticals using FOS spectra and WFPC surface photometry. We line_3: will correlate the dynamical evidence for massive black holes with indicators line_4: of nuclear activity (radio and optical emission, and star formation). line_5: Additionally, we will use our data to study the stellar dynamics and demography line_6: of the 'cores' of these elliptical galaxies. Our observations will establish line_7: the fundamental properties of the nuclear regions: photometric profiles, line_8: rotation and dispersion velocities, and spectroscopic metallicity indicies. line_9: FOC-UV images will reveal the presence of young stars and/or nonthermal line_10: emission. We will determine black hole masses by comparing the predictions of line_11: self-consistent dynamical models of the core to the observed surface photometry line_12: and kinematics. We wil model the stellar populations by comparing the observed line_13: metallicities and spectral energy distributions to synthetic spectra line_14: constructed from stellar libraries. ! ! end of abstract general_form_proposers: lname: JAFFE fname: WALTER title: P.I. inst: LEIDEN UNIVERSITY country: NETHERLANDS esa: X ! lname: O'CONNELL fname: ROBERT mi: W. inst: VIRGINIA, UNIVERSITY OF country: USA ! lname: FORD fname: H. mi: C. inst: JHU AND STSCI country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: WE WISH TO MEASURE THE MASS OF A CENTRAL BODY line_2: EXCLUDING EFFECTS OF VELOCITY ANISOTROPIES, NON- line_3: SPHERICAL SYMMETRY, NONSTELLAR EMISSION, INDIVIDUAL line_4: STARS, AND SO FORTH. WE PLAN TO MAKE 9 FOS G570 line_5: EXPOSURES OF EACH GALAXY: ONE ON THE NUCLEUS, line_6: FOUR AT A RADIUS OF 0.25 ARCSEC, AND FOUR AT line_7: A RADIUS OF 0.50 ARCSEC. THE FIVE INNER EXPOSURES line_8: WILL USE THE 0.25 ARCSEC APERTURE. THE FOUR line_9: OUTER ONES WILL USE A 0.50 ARCSEC APERTURE AND line_10: PROVIDE AN EXTRA-NUCLEAR BASELINE. VELOCITY line_11: DISPERSIONS WILL BE MEASURED FROM THE STRONG line_12: METALLIC ABSORPTION FEATURES IN THE G570 REGION, line_13: INCLUDING MG I AND NA I. THE OFF-NUCLEAR SPECTRA line_14: WILL BE ARRANGED ON A CROSS. FOS RED PRISM SPECTRA line_15: COVERING 2000-8000 A WILL PROVIDE INFORMATION ON line_16: THE TEMPERATURE AND METALLICITY OF THE STELLAR line_17: POPULATION AND THEIR GRADIENTS. IMAGES WILL BE line_18: TAKEN FOR ACCURATE POSITIONING (WF), THE NUCLEAR line_19: BRIGHTNESS GRADIENT AT V (PC), AND FOR IDENTIFICATION line_20: OF NONTHERMAL NUCLEI OR HOT OB STARS (FOC WITH F220W line_21: FILTER). TEMPLATE STARS WILL BE OBSERVED WITH line_22: THE FOS TO DETERMINE THE EFFECTIVE SPECTRAL POINT line_23: SPREAD FUNCTION. ! question: 4 section: 1 line_1: THE HIGH SPATIAL RESOLUTION OF HST IS CRUCIAL line_2: IN ORDER TO DETERMINE THE LIGHT DISTRIBUTION AND line_3: THE VELOCITY DISPERSION AS NEAR TO THE PUTATIVE line_4: BLACK HOLES AS POSSIBLE. ! question: 5 section: 1 line_1: THE TOTAL EXPOSURE TIME IS DOMINATED BY THE FOS line_2: SPECTRA. TIMES WERE CALCULATED BY COMBINING line_3: LAUER'S BRIGHTNESS PROFILES WITH THE FOS SIMULATOR. line_4: USING FOURIER DISPERSION MEASURING TECHNIQUES line_5: WE ESTIMATE THAT WE NEED 200 PHOTONS/ANGSTROM TO line_6: ACHIEVE A DISPERSION ACCURACY OF 15 KM/SEC. THIS line_7: WILL ENABLE US TO DETECT BLACK HOLES WITH MASSES line_8: LESS THAN 1.5E8 M(SUN). THE INDICATED EXPOSURE line_9: TIMES ARE 3.3 HOURS ON THE NUCLEUS; THE TOTAL OFF- line_10: NUCLEAR EXPOSURE WILL BE THE SAME BUT BROKEN line_11: INTO FOUR PIECES AT 90D SEPARATED POSITION ANGLES line_12: TO YIELD A SIMILAR S/N BUT ADDITIONAL INFORMATION line_13: ON ROTATION OR ASYMMETRIES. ! question: 6 section: 2 line_1: WE EXPECT THE FOS TO HAVE AN INTERNAL WAVELENGTH line_2: STABILITY OF BETTER THAN 0.1 DIODES OVER SEVERAL line_3: ORBITS AFTER INITIAL WARMUP. IF STABILITY IS line_4: NOT THIS GOOD, WE REQUIRE A CALIBRATION LAMP line_5: SPECTRUM BE TAKEN SUFFICIENTLY OFTEN TO INSURE line_6: THIS LEVEL OF ACCURACY. ! question: 7 section: 1 line_1: PRELIMINARY REDUCTION WILL BE DONE WITH SDAS AND line_2: IRAF AT STSCI. JAFFE HAS WRITTEN A FOURIER line_3: TRANSFORM VELOCITY DISPERION PROGRAM WHICH WORKS line_4: WITHIN SDAS. DYNAMICAL MODELS WILL BE MADE OF THE line_5: GALAXIES USING THE SURFACE PHOTOMETRY AND DISPERSION line_6: MEASURES. SPECTRAL SYNTHESIS WILL BE PERFORMED line_7: USING PROGRAMS AND DATA BASES DEVELOPED BY O'CONNELL. ! question: 8 section: 1 line_1: A PROGRAM TO OBTAIN MULTICOLOR IMAGES AND LONG line_2: SLIT SPECTRA OF OUR GALAXIES USING THE HERSCHEL line_3: TELESCOPE ON LA PALMA IS UNDER WAY. TWO GALAXIES line_4: (N4476 AND 4621) HAVE SCHEDULED GTO F555W PC IMAGES. line_5: WE WILL USE THE GTO FRAMES FOR THESE WHEN THEY line_6: BECOME PUBLIC. F4406 AND 4374 HAVE SCHEDULED GTO line_7: FOC FRAMES WHICH WILL YIELD 20 TIMES FEWER ELECTRONS line_8: PER PIXEL THAN OUR PROPOSED PC EXPOSURES. WE WISH line_9: TO RETAIN OUR PC EXPOSURES OF THESE. SOME OBJECTS line_10: HAVE UNPROTECTED CONDITIONAL EXPOSURES LISTED IN line_11: THE GTO PROGRAMS. THERE APPEARS TO BE LITTLE line_12: LIKELIHOOD THAT THESE WILL BE ACTUALLY BE MADE. ! question: 9 section: 1 line_1: NONE ! question: 10 section: 1 line_1: SALARY AND TRAVEL SUPPORT FOR JAFFE WILL BE line_2: PROVIDED BY THE UNIVERSITY OF LEIDEN. JAFFE WILL line_3: BE ASSISTED BY A GRADUATE STUDENT. JAFFE, line_4: FORD AND O'CONNELL HAVE REQUISITE COMPUTER RESOURCES, line_5: INCLUDING IVAS IMAGE DISPLAYS AND IRAF OR IDL line_6: IMAGE ANALYSIS PACKAGES, AVAILABLE AT THEIR INSTITUTIONS. ! !end of general form text general_form_address: lname: JAFFE fname: WALTER title: DR. category: PI inst: LEIDEN UNIVERSITY addr_1: P.O. BOX 9513 city: LEIDEN 2300 RA country: NETHERLANDS ! ! end of general_form_address records fixed_targets: targnum: 10 name_1: NGC4342 name_2: IC 3256 descr_1: E,303 pos_1: RA = 12H 23M 39.035S +/- 0.3", pos_2: DEC = +07D 03' 13.0" +/- 0.3" equinox: 2000.0 rv_or_z: V = 714 comment_1: THE POSITION IS FROM GSSS GASP. comment_2: PLACE GALAXY NUCLEUS AT DEFAULT comment_3: PC POSITION. fluxnum_1: 1 fluxval_1: SURF(V) = 15.8 +/- 0.3 ! targnum: 20 name_1: NGC4623 descr_1: E,303 pos_1: RA = 12H 42M 10.606S +/- 0.3", pos_2: DEC = +7D 40' 35.96" +/- 0.3" equinox: 2000.0 comment_1: THE POSITION IS FROM GSSS GASP. comment_2: PLACE GALAXY NUCLEUS AT DEFAULT comment_3: PC POSITION. fluxnum_1: 1 fluxval_1: SURF(V) = 16.0 +/- 0.3 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 10.000 sequence_1: DEFINE sequence_2: PCEXP targname: # config: PC opmode: IMAGE aperture: P6 sp_element: F555W wavelength: 5555 num_exp: 1 time_per_exp: 42M s_to_n: # fluxnum_1: 1 priority: 1 param_1: READ = YES, param_2: CR-SPLIT = 0.286, param_3: PRE-FLASH = YES req_1: CYCLE 1 comment_1: PC SCIENCE EXPOSURE OF NUCLEUS ! linenum: 20.000 sequence_1: USE PCEXP targname: NGC4342 s_to_n: 64 req_1: PCS MODE C; comment_1: EXECUTE IN COARSE TRACK ! linenum: 30.000 sequence_1: USE PCEXP targname: NGC4623 s_to_n: 64 req_1: PCS MODE F; comment_1: EXECUTE IN FINE LOCK ! ! end of exposure logsheet ! No scan data records found