! File: 4772C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:02:47:01 coverpage: title_1: BLACK HOLES, STELLAR DYNAMICS AND POPULATIONS IN THE NUCLEI OF A title_2: COMPLETE SAMPLE OF ELLIPTICAL GALAXIES - CONT OF 2607 - PART II 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: 1 foc: X fos: X funds_amount: 266452 funds_length: 24 funds_date: DEC-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: NGC4365-OFFSET descr_1: A,140 pos_1: RA = 12H 24M 29.652S +/- 0.5", pos_2: DEC = +7D 18' 52.100" +/- 0.5" equinox: 2000.0 comment_1: FAINT OFFSET STAR FOR comment_2: NUCLEAR POINTINGS fluxnum_1: 1 fluxval_1: V = 17.1 +/- 0.6 ! targnum: 20 name_1: NGC4365-NUCLEUS descr_1: E,303 pos_1: RA-OFF = -1.315S +/- 0.003S, pos_2: DEC-OFF = +11.002" +/- 0.05", pos_3: FROM 10 equinox: 2000.0 rv_or_z: V = 1230 comment_1: NUCLEAR POSN FOR FOS SPECTRUM comment_2: MEASURED FROM EARLY comment_3: ACQ WF IMAGE. comment_4: FLUXVAL_2 HERE AND IN LATER comment_5: ENTRIES IS FOR BRIGHTEST OB comment_6: STARS fluxnum_1: 1 fluxval_1: SURF(V) = 16.2 +/- 0.3 fluxnum_2: 2 fluxval_2: F(2200) = 5.6 +/- 5 E-18 ! targnum: 30 name_1: NGC4473-OFFSET descr_1: A,140 pos_1: RA = 12H 29M 42.600S +/- 0.5", pos_2: DEC = +13D 26' 47.220" +/- 0.5" equinox: 2000.0 comment_1: OFFSET STAR FOR NUCLEAR comment_2: POINTINGS fluxnum_1: 1 fluxval_1: V = 15.6 +/- 0.3 ! targnum: 40 name_1: NGC4473-NUCLEUS name_2: M84 descr_1: E,303 pos_1: RA-OFF = +6.284S +/- 0.003S, pos_2: DEC-OFF = -1.116" +/- 0.05", pos_3: FROM 30 equinox: 2000.0 rv_or_z: V = 952 comment_1: NUCLEAR POSN FOR FOS SPECTRUM comment_2: MEASURED FROM EARLY comment_3: ACQ WF IMAGE. comment_4: FLUXVAL_2 HERE AND IN LATER comment_5: ENTRIES IS FOR BRIGHTEST OB comment_6: STARS fluxnum_1: 1 fluxval_1: SURF(V) = 15.4 +/- 0.3 fluxnum_2: 2 fluxval_2: F(2200) = 5.6 +/- 5 E-18 ! targnum: 50 name_1: NGC4261-OFFSET descr_1: A,140 pos_1: RA = 12H 19M 27.586S +/- 0.5", pos_2: DEC = +5D 49' 54.640" +/- 0.5" equinox: 2000.0 comment_1: OFFSET STAR FOR NUCLEAR comment_2: POINTINGS fluxnum_1: 1 fluxval_1: V = 15.7 +/- 0.3 ! targnum: 60 name_1: NGC4261-NUCLEUS name_2: 3C270 descr_1: E,303 pos_1: RA-OFF = -4.358S +/- 0.003S, pos_2: DEC-OFF = -24.907" +/- 0.05", pos_3: FROM 50 rv_or_z: V = 2227 comment_1: NUCLEAR POSN FOR FOS SPECTRUM comment_2: DETERMINED FROM THE comment_3: EARLY ACQ WF IMAGE fluxnum_1: 1 fluxval_1: SURF(V) = 16.6 +/- 0.3 fluxnum_2: 2 fluxval_2: F(2200) = 5.6 +/- 5 E-18 ! targnum: 70 name_1: NGC4476-NUCLEUS descr_1: E,303 pos_1: RA = 12H 29M 59.18S +/- 2", pos_2: DEC = +12D 20' 53.49" +/- 2" equinox: 2000.0 rv_or_z: V = 1978 comment_1: POSITION FOR FOS AND comment_2: FOC DETERMINED FROM comment_3: PC IMAGE fluxnum_1: 1 fluxval_1: SURF(V) = 17.2 +/- 0.4 fluxnum_2: 2 fluxval_2: F(2200) = 5.6 +/- 5 E-18 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.100 sequence_1: DEFINE sequence_2: PEAK1 targname: # config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; comment_1: MULTIPLE PEAKUP ACQ comment_2: ON OFFSET STAR. comment_3: FIRST OF FOUR STAGES. ! linenum: 1.200 sequence_1: DEFINE sequence_2: PEAK2 targname: # config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 1S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; comment_1: MULTIPLE PEAKUP ACQ comment_2: ON OFFSET STAR. comment_3: SECOND OF FOUR STAGES. ! linenum: 1.300 sequence_1: DEFINE sequence_2: PEAK3 targname: # config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 1S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP=0.35, param_2: SEARCH-SIZE=3 comment_1: MULTIPLE PEAKUP ACQ comment_2: ON OFFSET STAR. comment_3: THIRD OF FOUR STAGES. ! linenum: 1.400 sequence_1: DEFINE sequence_2: PEAK4 targname: # config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP=0.1, param_2: SEARCH-SIZE=5 comment_1: MULTIPLE PEAKUP ACQ comment_2: ON OFFSET STAR. comment_3: FOURTH OF FOUR STAGES. ! linenum: 3.000 sequence_1: DEFINE sequence_2: FOSPIC targname: # config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 64S fluxnum_1: 1 priority: 1 comment_1: VERIFICATION IMAGE AFTER comment_2: OFFSET TO GALAXY NUCLEUS. ! linenum: 4.000 sequence_1: DEFINE sequence_2: PRISM targname: # config: FOS/RD opmode: ACCUM aperture: # sp_element: PRISM wavelength: 3500 num_exp: 1 time_per_exp: 1M s_to_n: # fluxnum_1: 1 priority: 1 comment_1: SNR CALCULATED AT 3500 ANG comment_2: FOR K0III SPECTRUM WITH SURF comment_3: BRIGHTNESS OF FLUXNUM_1 ! linenum: 5.000 sequence_1: DEFINE sequence_2: FOCEXP targname: # config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F220W num_exp: 1 time_per_exp: 3300S s_to_n: 20 fluxnum_1: 2 priority: 1 comment_1: EXPOSURE TO DETECT BRIGHT comment_2: OB STARS OR NONTHERMAL comment_3: NUCLEUS; ACQUISITION comment_4: SHOULD NOT BE PROBLEM AFTER comment_5: WF EARLY-ACQ EXPOSURE ! linenum: 10.100 sequence_1: USE PEAK1 targname: NGC4473-OFFSET time_per_exp: X10.0 req_1: SEQ 10.1-13 NO GAP; req_2: ONBOARD ACQ FOR 10.2; req_3: CYCLE 1 / 10.1-46; comment_1: ACQUIRE OFFSET STAR comment_2: IN 4.3 ARCSEC APERTURE. ! linenum: 10.200 sequence_1: USE PEAK2 targname: NGC4473-OFFSET time_per_exp: X10.0 req_1: ONBOARD ACQ FOR 10.3; comment_1: ACQUIRE OFFSET STAR comment_2: IN 1.0 ARCSEC APERTURE. ! linenum: 10.300 sequence_1: USE sequence_2: PEAK3 targname: NGC4473-OFFSET time_per_exp: X15.0 req_1: ONBOARD ACQ FOR 10.4; comment_1: ACQUIRE OFFSET STAR comment_2: IN 0.5 ARCSEC APERTURE. ! linenum: 10.400 sequence_1: USE sequence_2: PEAK4 targname: NGC4473-OFFSET time_per_exp: X23.6 req_1: ONBOARD ACQ FOR 12-13; comment_1: ACQUIRE OFFSET STAR comment_2: IN 0.3 ARCSEC APERTURE comment_3: THEN OFFSET TO GALAXY comment_4: NUCLEUS. ! linenum: 12.000 sequence_1: USE FOSPIC targname: NGC4473-NUCLEUS comment_1: VERIFICATION IMAGE AFTER OFFSET comment_2: TO THE NUCLEUS. OFFSET IS LESS comment_3: THAN 2'. ! linenum: 13.000 sequence_1: USE PRISM targname: NGC4473-NUCLEUS aperture: 0.5 time_per_exp: X30 s_to_n: 14 comment_1: THE SNR IS PER RESOLUTION ELEMENT. ! linenum: 20.100 sequence_1: USE PEAK1 targname: NGC4261-OFFSET time_per_exp: X11.0 req_1: SEQ 20.1-23 NO GAP; req_2: ONBOARD ACQ FOR 20.2; comment_1: ACQUIRE OFFSET STAR comment_2: IN 4.3 ARCSEC APERTURE. ! linenum: 20.200 sequence_1: USE PEAK2 targname: NGC4261-OFFSET time_per_exp: X11.0 req_1: ONBOARD ACQ FOR 20.3; comment_1: ACQUIRE OFFSET STAR comment_2: IN 1.0 ARCSEC APERTURE. ! linenum: 20.300 sequence_1: USE PEAK3 targname: NGC4261-OFFSET time_per_exp: X17.0 req_1: ONBOARD ACQ FOR 20.4; comment_1: ACQUIRE OFFSET STAR comment_2: IN 0.5 ARCSEC APERTURE. ! linenum: 20.400 sequence_1: USE PEAK4 targname: NGC4261-OFFSET time_per_exp: X26.0 req_1: ONBOARD ACQ FOR 22-23; comment_1: ACQUIRE OFFSET STAR comment_2: IN 0.3 ARCSEC APERTURE comment_3: THEN OFFSET TO GALAXY comment_4: NUCLEUS. ! linenum: 22.000 sequence_1: USE FOSPIC targname: NGC4261-NUCLEUS comment_1: VERIFICATION IMAGE AFTER OFFSET comment_2: TO THE NUCLEUS. OFFSET IS LESS comment_3: THAN 2'. ! linenum: 23.000 sequence_1: USE PRISM targname: NGC4261-NUCLEUS aperture: 0.5 time_per_exp: X30 s_to_n: 14 comment_1: THE SNR IS PER RESOLUTION ELEMENT. ! linenum: 30.100 sequence_1: USE PEAK1 targname: NGC4365-OFFSET time_per_exp: X30.0 req_1: SEQ 30.1-33 NO GAP; req_2: ONBOARD ACQ FOR 30.2; comment_1: ACQUIRE OFFSET STAR comment_2: IN 4.3 ARCSEC APERTURE. ! linenum: 30.200 sequence_1: USE PEAK2 targname: NGC4365-OFFSET time_per_exp: X30.0 req_1: ONBOARD ACQ FOR 30.3; comment_1: ACQUIRE OFFSET STAR comment_2: IN 1.0 ARCSEC APERTURE. ! linenum: 30.300 sequence_1: USE PEAK3 targname: NGC4365-OFFSET time_per_exp: X45.0 req_1: ONBOARD ACQ FOR 30.4; comment_1: ACQUIRE OFFSET STAR comment_2: IN 0.5 ARCSEC APERTURE. ! linenum: 30.400 sequence_1: USE PEAK4 targname: NGC4365-OFFSET time_per_exp: X47.0 req_1: ONBOARD ACQ FOR 32-33; comment_1: ACQUIRE OFFSET STAR comment_2: IN 0.3 ARCSEC APERTURE comment_3: THEN OFFSET TO GALAXY comment_4: NUCLEUS. ! linenum: 32.000 sequence_1: USE FOSPIC targname: NGC4365-NUCLEUS comment_1: VERIFICATION IMAGE AFTER OFFSET comment_2: TO THE NUCLEUS. OFFSET LESS comment_3: THAN 2'. ! linenum: 33.000 sequence_1: USE PRISM targname: NGC4365-NUCLEUS aperture: 0.5 time_per_exp: X30 s_to_n: 14 comment_1: THE SNR IS PER RESOLUTION ELEMENT. ! linenum: 40.000 sequence_1: USE FOCEXP targname: NGC4476-NUCLEUS ! linenum: 41.000 targname: NGC4476-NUCLEUS config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: PRISM wavelength: 3500 num_exp: 1 time_per_exp: 15S priority: 1 req_1: SEQ 41-46 NO GAP; req_2: ONBOARD ACQ FOR 42; req_3: SPATIAL SCAN; comment_1: ACQUIRE GALAXY NUCLEUS comment_2: DIRECTLY IN 4.3 ARCSEC comment_3: APERTURE USING PRISM. ! linenum: 42.000 targname: NGC4476-NUCLEUS config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: PRISM wavelength: 3500 num_exp: 1 time_per_exp: 15S priority: 1 req_1: ONBOARD ACQ FOR 43; req_2: SPATIAL SCAN; comment_1: ACQUIRE GALAXY NUCLEUS comment_2: DIRECTLY IN 1.0 ARCSEC comment_3: APERTURE USING PRISM. ! linenum: 43.000 targname: NGC4476-NUCLEUS config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: PRISM wavelength: 3500 num_exp: 1 time_per_exp: 20S priority: 1 param_1: SCAN-STEP=0.35, param_2: SEARCH-SIZE=3 req_1: ONBOARD ACQ FOR 44; comment_1: ACQUIRE GALAXY NUCLEUS comment_2: DIRECTLY IN 0.5 ARCSEC comment_3: APERTURE USING PRISM. ! linenum: 44.000 targname: NGC4476-NUCLEUS config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: PRISM wavelength: 3500 num_exp: 1 time_per_exp: 45S priority: 1 param_1: SCAN-STEP=0.1, param_2: SEARCH-SIZE=5 req_1: ONBOARD ACQ FOR 45-46; comment_1: ACQUIRE GALAXY NUCLEUS comment_2: DIRECTLY IN 0.3 ARCSEC comment_3: APERTURE USING PRISM. ! linenum: 45.000 sequence_1: USE FOSPIC targname: NGC4476-NUCLEUS comment_1: VERIFICATION IMAGE ! linenum: 46.000 sequence_1: USE PRISM targname: NGC4476-NUCLEUS aperture: 0.5 time_per_exp: X30 s_to_n: 14 comment_1: THE SNR IS PER RESOLUTION ELEMENT. ! ! end of exposure logsheet scan_data: line_list: 10.1,20.1,30.1,41 fgs_scan: cont_dwell: D dwell_pnts: 3 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 2.8000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 0.0000 scan_frame: S/C len_offset: 1.4 wid_offset: 0.0 ! line_list: 10.2,20.2,30.2,42 fgs_scan: cont_dwell: D dwell_pnts: 6 dwell_secs: 1.00 scan_width: 0.7000 scan_length: 3.5000 sides_angle: 90.0000 number_lines: 2 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 1.75 wid_offset: 0.35 ! ! end of scan data