COVERPAGE: TITLE_1: HIGH SPATIAL RESOLUTION KINEMATICS OF THE DISK AROUND THE ACTIVE TITLE_2: NUCLEUS OF NGC 4261 SCI_CAT: GALAXIES & CLUSTERS SCI_SUBCAT: NUCLEI/CORES PROPOSAL_FOR: GO LARGE_PROJ: ! Is this a Large Project(>60 hrs)? Y or blank KEY_PROJ: ! Is this a Key Project? Y or blank TARG_OF_OPP: ! Any Target of Opportunity exposures? Y or blank REALTIME: ! Are real-time observations involved? Y or blank TIME_CRIT: ! Are observations time-critical? CVZ targets? Y or blank ! LONGTERM: ! Number of years: 2 or 3 (if long-term) or delete item PI_FNAME: Holland ! PI's first name, X20 PI_MI: C. ! PI's middle initial, X2 PI_LNAME: Ford ! PI's last name, X20 PI_INST: Johns Hopkins University ! PI's institution, X60 PI_COUNTRY: USA ! PI's country, X20 PI_PHONE: (410) 516 8653 ! PI's telephone number, X20 HOURS_PRI: 7.59 ! Hours of primary exposure time, F3.2 HOURS_PAR: 0.0 ! Hours of parallel exposure time, F2.2 NUM_PRI: 1 ! Number of primary targets, I4 NUM_PAR: 0 ! Number of parallel targets, I4 ! Indicate which instruments will be used (enter Y or leave blank/delete): WF_PC: ! Wide Field Planetary Camera 2 FOC: ! Faint Object Camera FOS: Y ! Faint Object Spectrograph HRS: ! (Goddard) High Resolution Spectrograph FGS: ! Fine Guidance Sensor ! Authorizing Institution Official: OFF_FNAME: temp ! First name of authorizing official, X20 OFF_LNAME: temp ! Last name of authorizing official, X20 OFF_TITLE: temp ! Title of authorizing official, X20 OFF_INST: temp ! Institution number OFF_ADDR_1:temp ! Address of authorizing official, X60 OFF_ADDR_2: temp ! OFF_ADDR_3: temp ! OFF_CITY: temp ! X20 OFF_STATE: tem ! X3 OFF_ZIP: temp ! X9 OFF_COUNTRY: temp ! X20 OFF_PHONE: temp ! Telephone number of authorizing official, X20 ABSTRACT: ! Enter abstract text: use < 80 characters per line LINE_1:HST F555W images of NGC 4261 (E3), the seventh brightest early type LINE_2:galaxy in Virgo, show a small (1".7 x 0".74), dusty disk with sharp LINE_3:edges and a point-like nucleus. The disk's minor axis is aligned with LINE_4:the axis of the large scale bi-directional radio jet which originates in LINE_5:the nucleus. The face-on optical depth of the dust is 0.3. The disk LINE_6:contains HI and CO, and the nucleus is a LINER with unusually strong and LINE_7:broad (FWZI ~ 4500 km/s) emission lines of \[NII\] and \[SII\]. We conclude LINE_8:that we are looking directly at the structure, i.e. the nuclear disk, LINE_9:which fuels the engine and determines the direction of the radio jet. LINE_10:WHT spectra show subtle but unmistakeable evidence for rotation of the LINE_11:narrow component of \[NII\] emission. Our models of the emission suggest, LINE_12:but by no means prove, that there is a ~ 4 x 10\*\*7 M black hole in the LINE_13:nucleus. Our models of the light and mass distribution show that the LINE_14:definitive signature of a massive black hole will be a transition from LINE_15:the solid body rotation observed from the ground to a rising Keplerian LINE_16:rotation curve for r < 0".3. We propose to use the FOS 0".09 aperture LINE_17:with G570H to map the rotation curve in the disk in the crucial region LINE_18:r < 0".3 which is unobservable from the ground. The observations of this LINE_19:nearly unique small nuclear disk provide an opportunity to make an LINE_20:unambiguous measurement of the mass of an active nucleus. GENERAL_FORM_PROPOSERS: ! Replicate the section below for each investigator (PI and CoI's): LNAME: Ford ! Last name of investigator, X20 FNAME: Holland ! First name of investigator, X20 MI: C. ! Middle initial of investigator, X2 INST: 2380 ! Institution number COUNTRY: USA ! Country, X20 ESA: ! Is CoI affiliated with ESA or an ! ESA member-state institution? Y or blank LNAME: Jaffe ! Last name of investigator, X20 FNAME: Walter ! First name of investigator, X20 MI: ! Middle initial of investigator, X2 INST: 6870 ! Institution number COUNTRY: Netherlands ! Country, X20 ESA: Y ! Is CoI affiliated with ESA or an ! ESA member-state institution? Y or blank LNAME: O'Connell ! Last name of investigator, X20 FNAME: Robert ! First name of investigator, X20 MI: W. ! Middle initial of investigator, X2 INST: 3730 ! Institution number COUNTRY: USA ! Country, X20 ESA: ! Is CoI affiliated with ESA or an ! ESA member-state institution? Y or blank LNAME: Ferrarese ! Last name of investigator, X20 FNAME: Laura ! First name of investigator, X20 MI: ! Middle initial of investigator, X2 INST: 2380 ! Institution number COUNTRY: USA ! Country, X20 ESA: ! Is CoI affiliated with ESA or an ! ESA member-state institution? Y or blank LNAME: van den Bosch ! Last name of investigator, X20 FNAME: Frank ! First name of investigator, X20 MI: C. ! Middle initial of investigator, X2 INST: 6870 ! Institution number COUNTRY: Netherlands ! Country, X20 ESA: Y ! Is CoI affiliated with ESA or an ! ESA member-state institution? Y or blank GENERAL_FORM_ADDRESS: ! The PI's address: LNAME: Ford ! PI's last name, X20 FNAME: Holland ! PI's first name, X20 MI: C. ! PI's middle initial, X2 CATEGORY: PI ! DO NOT CHANGE INST: 2380 ! PI's institution number, X60 ADDR_1: Department of Physics and Astronomy ADDR_2: Homewood Campus ADDR_3: CITY: Baltimore ! X30 STATE: MD ! X2 ZIP: 21218 ! X9 COUNTRY: USA ! X20 PHONE: (410) 516 8653 ! PI's telephone number, X20 TELEX: ford@stsci.edu ! PI's EMAIL address or FAX number, X60 ! The address of the primary contact for this proposal (if not PI): LNAME: ! Contact's last name, X20 FNAME: ! Contact's first name, X20 MI: ! Contact's middle initial, X2 CATEGORY: CON ! DO NOT CHANGE INST: ! Contact's institution number, X60 ADDR_1: ! Contact's address, X60 ADDR_2: ADDR_3: CITY: ! X30 STATE: ! X2 ZIP: ! X9 COUNTRY: ! X20 PHONE: ! Contact's telephone number, X20 TELEX: ! Contact's EMAIL address or FAX number, X60 GENERAL_FORM_TEXT: QUESTION: 3 ! Description of proposed observations. SECTION: 1 ! Provide a detailed description of the proposed observing plan. ! This description is used during scheduling to ensure that the ! observations are implemented properly, so please answer with care. LINE_1:We propose to map the disk in NGC 4261 with the FOS 0.''1 aperture LINE_2:and grating G570H. The patter adopted includes a 3X3 grid centered LINE_3:on the nucleus and with axes aligned with the major and minor axes LINE_4:of the disk, plus 4 additional positions along the major and minor LINE_5:axes of the disk, on either side of the nucleus, placed just LINE_6:outside the 3X3 grid. LINE_7:We are aiming for a S/N between 10 and 30 in the peak of the [NII] LINE_8:lambda6584 emission line, corresponding to S/N between 6 and 17 in the LINE_9:adjacent continuum. Our models show that the analysis of the LINE_10:[NII]+Halpha emissions, for S/N ~ 16 and given the spatial sampling LINE_11:proposed here, will allow us to resolve a keplerian rise in the LINE_12:rotation curve due to a nuclear black hole with mass larger than LINE_13:5X10^6 solar masses. The exposure times have been calculated using LINE_14:formula 1, page 25, of the FOS Instrument Handbook (Version 5.0), by LINE_15:neglecting the aperture throughput, as appropriate for an extended LINE_16:source. The flux at the [NII] peak has been derived from the WFPC2 LINE_17:H alpha images and the WHT spectra, and is reported in the parameter LINE_18:FLUXNUM_1 in the TARGET LIST for each individual position. LINE_19:The acquisition procedure includes an ACQ/BIN on an offset star LINE_20:located about 1 arcmin away from the nucleus, followed by a LINE_21:three stages ACQ/PEAK on the same star. The pointing accuracy for QUESTION: 3 ! Description of proposed observations. SECTION: 2 LINE_1:the star at the end of the acquisition procedure will be 0".03 LINE_2:(4 sigma measurement). The offset between the star and the LINE_3:nucleus is known with a 0".03 accuracy, and since the 1 sigma LINE_4:error associated with the slew is 0".08, the final 1 sigma pointing LINE_5:error on the nucleus will be 0".09. We therefore require that a one LINE_6:stage peak-up is executed on the nucleus using the 0".1 aperture LINE_7:and the G570 grating. Since the nucleus is bright in emission lines, LINE_8:we require that only the wavelenght region including Halpha, [NII] LINE_9:and [SII] is read out. QUESTION: 4 ! Justification of need for HST observations. SECTION: 1 LINE_1:We have observed NGC 4261 at 21 cm with the VLA and at 1.3 mm with the LINE_2:James Clerk Maxwell Telescope in Hawaii. We detected HI and CO in LINE_3:absorption at the systemic velocity of the galaxy. We have obtained LINE_4:high signal-to-noise ratio NTT H-alpha on-band and off-band images of LINE_5:NGC 4261 during seeing with a FWHM ~ 0.''8. These observations detect LINE_6:the dust but do not resolve the disk. We obtained green and red spectra LINE_7:of the disk and nucleus of NGC 4261 with the William Herschel Telescope LINE_8:during 1.''1 seeing. The spectra show evidence for rotation (cf Figure LINE_9:2), but cannot show if the rotation curve transitions from solid body LINE_10:decline to a rising Keplerian curve in the crucial region r < 0.''3. LINE_11:HST FOS spectra with a resolution of ~ 0.1'' are the only way to LINE_12:measure the rotation of the disk in the critical region close (r < 0.''3) LINE_13:to the nucleus. QUESTION: 5 ! Description of special scheduling requirements. SECTION: 1 ! Describe any special scheduling requirements such as real-time, time-critical, ! dark time, uninterrupted, Target of Opportunity, or Continuous Viewing Zone ! observations. LINE_1: No special scheduling requirements are needed QUESTION: 6 ! Description of special calibration exposures. SECTION: 1 LINE_1: No special calibration exposures are needed QUESTION: 7 ! Data reduction and analysis plans. SECTION: 1 LINE_1:We will derive a velocity map for the inner 0.3x0.3 arcsec of the galaxy. LINE_2:The continuum and emission lines of each of the FOS spectra will be LINE_3:fitted interactively by Chi-square minimization using a Simplex LINE_4:algorithm. This will allow us to derive the peak velocities of the LINE_5:emission lines. Our modeling shows that the S/N of the spectra and the LINE_6:spatial sampling will allow us to resolve a keplerian rise in the LINE_7:rotation curve due to a nuclear black hole with mass larger that 5 x 10^6 LINE_8:solar masses. The rotation curve will be modeled by assuming that the LINE_9:gas is embedded in the gravitational potential of the stellar LINE_10:component, plus the gravitational potential of the nuclear disk, and LINE_11:the central black hole. Since the mass of the disk is known to be 10^6 LINE_12:solar masses from radio observations (Jaffe and MacNamara 1993), the LINE_13:only two free parameters in the fit will be the stellar mass to light LINE_14:ratio and the mass of the central black hole. The shape of the LINE_15:gravitational potential of the stellar component has already been LINE_16:derived by fitting the brightness distribution obtained from HST/PC LINE_17:images with a double exponential law, and subsequently deprojecting LINE_18:the fit in order to otain a spatial luminosity density. For a black LINE_19:hole with mass a few times 10^7 solar masses (much larger masses are LINE_20:ruled out by our WHT spectrum), the expected velocity curve is LINE_21:given by the stellar potential at radii larger than 1-1.5 arcsec. LINE_22:The fit to the rotation curve in this region will allow us to constrain LINE_23:the range of possible values for the stellar mass to light ratio, so QUESTION: 7 SECTION: 2 LINE_1:that a more precise estimate of the black hole mass is possible from LINE_2:the analysis of the inner 0.3 arcsec of the rotation curve. QUESTION: 8 ! Additional comments or special requests. SECTION: 1 LINE_1: No additional comments QUESTION: 9 ! Description of previous HST work. SECTION: 1 LINE_1: H. Ford is the IDT-PI for the Following FOS GTO and GO Programs: LINE_2: 1034: M87's Jet, Nucleus, and Hot Corona. LINE_3: 1036: Imaging and Spectrophotometry of Seyfert Nuclei. LINE_4: 1038: Imaging and Spectrophotometry of Nuclear Activity in LINERs. LINE_5: 1040: Velocity Dispersions in the Nuclei of Giant Ellipticals. LINE_6: 1044: Stellar and Gas Dynamics in Normal Galaxies. LINE_7: 1046: Imaging and UV Spectrophotometry of Local Group Planetary Nebulae. LINE_8: 4668: FOS Spectroscopy of n1052 and n4258. LINE_9: H. Ford is a Co-I on the Following GO Programs: LINE_10: 2607: Black Holes, Stellar Dynamics and Populations in the Nuclei of a LINE_11: Complete Sample of Elliptical Galaxies. (PI Walter Jaffe) LINE_12: 2227: Determination of the Extragalactic Distance Scale (PI Jeremy Mould) LINE_13: 2266: Post-Asymptotic Giant Branch Evolution in the Magellanic Clouds LINE_14: (PI M Dopita). LINE_15: 4371: FOS Spectroscopy of Resolved Structure in the Nucleus of Markarian 3 LINE_16: (PI Zlatko Tsvetanov). QUESTION: 10 ! Resources to be supplied by investigator's institution(s). SECTION: 1 LINE_1:Holland Ford and Laura Ferrarese at Johns Hopkins University will analyze LINE_2:and modelthe data using a cluster of Sun Workstations within the department. LINE_3:The workstations are part of a network, and are connected to printers, tape LINE_4:readers, etc. The Sun cluster is supported by a system manager. ! This is the end of the General Form FIXED_TARGETS: ! Replicate this section as needed for each Fixed Target. ! Delete this entire section if none of your targets are fixed targets. ! See Section 5.1 of the Proposal Instructions for detailed instructions. TARGNUM: 1 NAME_1: NGC4261-OFF DESCR_1: A,140 POS_1: RA-OFF = +4.365S +/- 0.003S, POS_2: DEC-OFF = +24.875" +/- 0.05", POS_3: FROM 2 EQUINOX: RV_OR_Z: ACQPR_1: FLUXNUM_1: 1 FLUXVAL_1: V = 15.7 +/- 0.3 FLUXNUM_2: 2 FLUXVAL_2: V-I = 1.1 COMMENT_1: OFFSET STAR FOR NUCLEAR POINTING TARGNUM: 2 NAME_1: NGC4261-NUC DESCR_1: E,303,315,317,910 POS_1: RA = 12H 19M 23.145S +/- 0.04S, POS_2: DEC = +5D 49' 30.059" +/- 0.5" EQUINOX: 2000.0 RV_OR_Z: V = +2282 ACQPR_1: BKG FLUXNUM_1: 1 FLUXVAL_1: SURF(V) = 16.6 +/- 0.3 FLUXNUM_2: 2 FLUXVAL_2: F(6633) = 1.0 E-15 FLUXNUM_3: 3 FLUXVAL_3: SURF(4700) = 1.6 E-16 FLUXNUM_4: 4 FLUXVAL_4: SURF(2500) = 3.5 E-17 FLUXNUM_5: 5 FLUXVAL_5: R = 19.2 +/- 0.3 COMMENT_1: POSITION DETERMINED FROM WFPC2 COMMENT_2: H ALPHA IMAGE TARGNUM: 3 NAME_1: NGC4261-N1 DESCR_1: E,303,315,317,910 POS_1: XI-OFF = -0.026" +/- 0.003", POS_2: ETA-OFF = +0.086" +/- 0.001", POS_3: FROM 2 POS_4: EQUINOX: RV_OR_Z: V = +2282 ACQPR_1: FLUXNUM_1: 1 FLUXVAL_1: F(6633) = 4.4 E-16 COMMENT_1: 0.09 OFFSET ALONG MAJOR AXIS TARGNUM: 4 NAME_1: NGC4261-N2 DESCR_1: E,303,315,317,910 POS_1: XI-OFF = -0.052" +/- 0.006", POS_2: ETA-OFF = +0.172" +/- 0.002", POS_3: FROM 2 POS_4: EQUINOX: RV_OR_Z: V = +2282 ACQPR_1: FLUXNUM_1: 1 FLUXVAL_1: F(6633) = 8.5 E-17 COMMENT_1: ALONG MAJOR AXIS COMMENT_2: 0.018 OFFSET ALONG MAJOR AXIS TARGNUM: 5 NAME_1: NGC4261-S1 DESCR_1: E,303,315,317,910 POS_1: XI-OFF = 0.026" +/- 0.003", POS_2: ETA-OFF = -0.086" +/- 0.001", POS_3: FROM 2 POS_4: EQUINOX: RV_OR_Z: V = +2282 ACQPR_1: FLUXNUM_1: 1 FLUXVAL_1: F(6633) = 4.4 E-16 COMMENT_1: 0.09 OFFSET ALONG MAJOR AXIS TARGNUM: 6 NAME_1: NGC4261-S2 DESCR_1: E,303,315,317,910 POS_1: XI-OFF = 0.052" +/- 0.006", POS_2: ETA-OFF = -0.172" +/- 0.002", POS_3: FROM 2 POS_4: EQUINOX: RV_OR_Z: V = +2282 ACQPR_1: FLUXNUM_1: 1 FLUXVAL_1: F(6633) = 8.5 E-17 COMMENT_1: ALONG MAJOR AXIS COMMENT_2: 0.018 OFFSET ALONG MAJOR AXIS TARGNUM: 7 NAME_1: NGC4261-W1 DESCR_1: E,303,315,317,910 POS_1: XI-OFF = -0.086" +/- 0.001", POS_2: ETA-OFF = -0.026" +/- 0.003", POS_3: FROM 2 POS_4: EQUINOX: RV_OR_Z: V = +2282 ACQPR_1: FLUXNUM_1: 1 FLUXVAL_1: F(6633) = 4.4 E-16 COMMENT_1: 0.09 OFFSET ALONG MINOR AXIS TARGNUM: 8 NAME_1: NGC4261-W2 DESCR_1: E,303,315,317,910 POS_1: XI-OFF = -0.172" +/- 0.002", POS_2: ETA-OFF = -0.052" +/- 0.006", POS_3: FROM 2 POS_4: EQUINOX: RV_OR_Z: V = +2282 ACQPR_1: FLUXNUM_1: 1 FLUXVAL_1: F(6633) = 8.5 E-17 COMMENT_1: ALONG MAJOR AXIS COMMENT_2: 0.018 OFFSET ALONG MINOR AXIS TARGNUM: 9 NAME_1: NGC4261-E1 DESCR_1: E,303,315,317,910 POS_1: XI-OFF = +0.086" +/- 0.001", POS_2: ETA-OFF = +0.026" +/- 0.003", POS_3: FROM 2 POS_4: EQUINOX: RV_OR_Z: V = +2282 ACQPR_1: FLUXNUM_1: 1 FLUXVAL_1: F(6633) = 4.4 E-16 COMMENT_1: 0.09 ALONG MINOR AXIS TARGNUM: 10 NAME_1: NGC4261-E2 DESCR_1: E,303,315,317,910 POS_1: XI-OFF = 0.172" +/- 0.002", POS_2: ETA-OFF = 0.052" +/- 0.006", POS_3: FROM 2 POS_4: EQUINOX: RV_OR_Z: V = +2282 ACQPR_1: FLUXNUM_1: 1 FLUXVAL_1: F(6633) = 8.5 E-17 COMMENT_1: ALONG MAJOR AXIS COMMENT_2: 0.018 OFFSET ALONG MINOR AXIS TARGNUM: 11 NAME_1: NGC4261-NE1 DESCR_1: E,303,315,317,910 POS_1: XI-OFF = +0.060" +/- 0.004", POS_2: ETA-OFF = +0.112" +/- 0.002", POS_3: FROM 2 POS_4: EQUINOX: RV_OR_Z: V = +2282 ACQPR_1: FLUXNUM_1: 1 FLUXVAL_1: F(6633) = 2.3 E-16 COMMENT_1: OFF AXIS TARGNUM: 12 NAME_1: NGC4261-SE1 DESCR_1: E,303,315,317,910 POS_1: XI-OFF = +0.112" +/- 0.002", POS_2: ETA-OFF = -0.060" +/- 0.004", POS_3: FROM 2 POS_4: EQUINOX: RV_OR_Z: V = +2282 ACQPR_1: FLUXNUM_1: 1 FLUXVAL_1: F(6633) = 2.3 E-16 COMMENT_1: OFF AXIS TARGNUM: 13 NAME_1: NGC4261-NW1 DESCR_1: E,303,315,317,910 POS_1: XI-OFF = -0.112" +/- 0.002", POS_2: ETA-OFF = +0.060" +/- 0.004", POS_3: FROM 2 POS_4: EQUINOX: RV_OR_Z: V = +2282 ACQPR_1: FLUXNUM_1: 1 FLUXVAL_1: F(6633) = 2.3 E-16 COMMENT_1: OFF AXIS TARGNUM: 14 NAME_1: NGC4261-SW1 DESCR_1: E,303,315,317,910 POS_1: XI-OFF = -0.060" +/- 0.004", POS_2: ETA-OFF = -0.112" +/- 0.002", POS_3: FROM 2 POS_4: EQUINOX: RV_OR_Z: V = +2282 ACQPR_1: FLUXNUM_1: 1 FLUXVAL_1: F(6633) = 2.3 E-16 COMMENT_1: OFF AXIS EXPOSURE_LOGSHEET: ! Replicate this section as needed for each exposure. ! See Section 6 for detailed instructions. LINENUM: 1.0 SEQUENCE_1: DEFINE SEQUENCE_2: SP TARGNAME: # CONFIG: FOS/RD OPMODE: ACCUM APERTURE: # SP_ELEMENT: G570H WAVELENGTH: 4571-6820 NUM_EXP: 1 TIME_PER_EXP: 1S S_TO_N: # S_TO_N_TIME: # FLUXNUM_1: # PRIORITY: 1 REQ_1: CYCLE 4 LINENUM: 10.0 TARGNAME: NGC4261-OFF CONFIG: FOS/RD OPMODE: ACQ/BINARY APERTURE: 4.3 SP_ELEMENT: MIRROR PARAM_1: BRIGHT=132000 PARAM_2: FAINT=330 NUM_EXP: 1 TIME_PER_EXP: 11.8S S_TO_N: S_TO_N_TIME: FLUXNUM_1: 1 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: SEQ 10-271 NO GAP; REQ_3: ONBOARD ACQ FOR 190-271 COMMENT_1: BINARY ACQUISITION ON OFFSET STAR LINENUM: 20.0 TARGNAME: NGC4261-OFF CONFIG: FOS/RD OPMODE: ACQ/PEAK APERTURE: 0.5-PAIR SP_ELEMENT: MIRROR PARAM_1: SCAN-STEP-X=0.30 PARAM_2: SCAN-STEP-Y=0.30 PARAM_3: SEARCH-SIZE-X=3 PARAM_4: SEARCH-SIZE-Y=3 NUM_EXP: 1 TIME_PER_EXP: 10.0S S_TO_N: S_TO_N_TIME: FLUXNUM_1: 1 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: ONBOARD ACQ FOR 190-271 COMMENT_1: CRITICAL PEAK-UP ON STAR COMMENT_2: FIRST OF THREE STAGES LINENUM: 30.0 TARGNAME: NGC4261-OFF CONFIG: FOS/RD OPMODE: ACQ/PEAK APERTURE: 0.25-PAIR SP_ELEMENT: MIRROR PARAM_1: SCAN-STEP-X=0.17 PARAM_2: SCAN-STEP-Y=0.17 PARAM_3: SEARCH-SIZE-X=3 PARAM_4: SEARCH-SIZE-Y=3 NUM_EXP: 1 TIME_PER_EXP: 10.0S S_TO_N: S_TO_N_TIME: FLUXNUM_1: 1 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: ONBOARD ACQ FOR 190-271 COMMENT_1: CRITICAL PEAK-UP ON STAR COMMENT_2: SECOND OF THREE STAGES LINENUM: 40.0 TARGNAME: NGC4261-OFF CONFIG: FOS/RD OPMODE: ACQ/PEAK APERTURE: 0.1-PAIR-B SP_ELEMENT: MIRROR PARAM_1: SCAN-STEP-X=0.05 PARAM_2: SCAN-STEP-Y=0.05 PARAM_3: SEARCH-SIZE-X=5 PARAM_4: SEARCH-SIZE-Y=5 NUM_EXP: 1 TIME_PER_EXP: 10.0S S_TO_N: S_TO_N_TIME: FLUXNUM_1: 1 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: ONBOARD ACQ FOR 190-271 COMMENT_1: CRITICAL PEAK-UP ON STAR COMMENT_2: THIRD OF THREE STAGES LINENUM: 45.0 TARGNAME: NGC4261-NUC CONFIG: FOS/RD OPMODE: ACQ/PEAK APERTURE: 0.25-PAIR SP_ELEMENT: G570H WAVELENGTH: 6500-6820 PARAM_1: SCAN-STEP-X=0.17 PARAM_2: SCAN-STEP-Y=0.17 PARAM_3: SEARCH-SIZE-X=3 PARAM_4: SEARCH-SIZE-Y=3 NUM_EXP: 1 TIME_PER_EXP: 66.0S S_TO_N: S_TO_N_TIME: FLUXNUM_1: 5 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: ONBOARD ACQ FOR 190-271 COMMENT_1: CRITICAL PEAK-UP ON NUCLEUS COMMENT_2: FIRST OF TWO STAGES LINENUM: 46.0 TARGNAME: NGC4261-NUC CONFIG: FOS/RD OPMODE: ACQ/PEAK APERTURE: 0.1-PAIR-B SP_ELEMENT: G570H WAVELENGTH: 6500-6820 PARAM_1: SCAN-STEP-X=0.052 PARAM_2: SCAN-STEP-Y=0.052 PARAM_3: SEARCH-SIZE-X=5 PARAM_4: SEARCH-SIZE-Y=5 NUM_EXP: 1 TIME_PER_EXP: 50.0S S_TO_N: S_TO_N_TIME: FLUXNUM_1: 5 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: ONBOARD ACQ FOR 190-271 COMMENT_1: CRITICAL PEAK-UP ON NUCLEUS COMMENT_2: SECOND OF TWO STAGES LINENUM: 190.0 SEQUENCE_1: USE SP TARGNAME: NGC4261-NUC APERTURE: 0.1-PAIR-B TIME_PER_EXP: X2030.0 S_TO_N: 35 S_TO_N_TIME: FLUXNUM_1: 2 COMMENT_1: S/N AT THE PEAK OF THE [NII] LINE LINENUM: 191.0 TARGNAME: WAVE CONFIG: FOS/RD APERTURE: 0.1-PAIR-B OPMODE: ACCUM SP_ELEMENT: G570H NUM_EXP: 1 TIME_PER_EXP: DEF PRIORITY: 1 REQ_1: CYCLE 4 COMMENT_1: WAVECAL FOR LINE 190 LINENUM: 200.0 SEQUENCE_1: USE SP TARGNAME: NGC4261-N1 APERTURE: 0.1-PAIR-B TIME_PER_EXP: X2030.0 S_TO_N: 23 S_TO_N_TIME: FLUXNUM_1: 1 COMMENT_1: S/N AT THE PEAK OF THE [NII] LINE LINENUM: 205.0 SEQUENCE_1: USE SP TARGNAME: NGC4261-N2 APERTURE: 0.1-PAIR-B TIME_PER_EXP: X2030.0 S_TO_N: 10 S_TO_N_TIME: FLUXNUM_1: 1 COMMENT_1: S/N AT THE PEAK OF THE [NII] LINE LINENUM: 210.0 SEQUENCE_1: USE SP TARGNAME: NGC4261-S1 APERTURE: 0.1-PAIR-B TIME_PER_EXP: X2030.0 S_TO_N: 23 S_TO_N_TIME: FLUXNUM_1: 1 COMMENT_1: S/N AT THE PEAK OF THE [NII] LINE LINENUM: 215.0 SEQUENCE_1: USE SP TARGNAME: NGC4261-S2 APERTURE: 0.1-PAIR-B TIME_PER_EXP: X2030.0 S_TO_N: 10 S_TO_N_TIME: FLUXNUM_1: 1 COMMENT_1: S/N AT THE PEAK OF THE [NII] LINE LINENUM: 220.0 SEQUENCE_1: USE SP TARGNAME: NGC4261-W1 APERTURE: 0.1-PAIR-B TIME_PER_EXP: X2030.0 S_TO_N: 23 S_TO_N_TIME: FLUXNUM_1: 1 COMMENT_1: S/N AT THE PEAK OF THE [NII] LINE LINENUM: 225.0 SEQUENCE_1: USE SP TARGNAME: NGC4261-W2 APERTURE: 0.1-PAIR-B TIME_PER_EXP: X2030.0 S_TO_N: 10 S_TO_N_TIME: FLUXNUM_1: 1 COMMENT_1: S/N AT THE PEAK OF THE [NII] LINE LINENUM: 230.0 SEQUENCE_1: USE SP TARGNAME: NGC4261-E1 APERTURE: 0.1-PAIR-B TIME_PER_EXP: X2030.0 S_TO_N: 23 S_TO_N_TIME: FLUXNUM_1: 1 COMMENT_1: S/N AT THE PEAK OF THE [NII] LINE LINENUM: 235.0 SEQUENCE_1: USE SP TARGNAME: NGC4261-E2 APERTURE: 0.1-PAIR-B TIME_PER_EXP: X2030.0 S_TO_N: 10 S_TO_N_TIME: FLUXNUM_1: 1 COMMENT_1: S/N AT THE PEAK OF THE [NII] LINE LINENUM: 240.0 SEQUENCE_1: USE SP TARGNAME: NGC4261-NW1 APERTURE: 0.1-PAIR-B TIME_PER_EXP: X2030.0 S_TO_N: 17 S_TO_N_TIME: FLUXNUM_1: 1 COMMENT_1: S/N AT THE PEAK OF THE [NII] LINE LINENUM: 250.0 SEQUENCE_1: USE SP TARGNAME: NGC4261-SW1 APERTURE: 0.1-PAIR-B TIME_PER_EXP: X2030.0 S_TO_N: 17 S_TO_N_TIME: FLUXNUM_1: 1 COMMENT_1: S/N AT THE PEAK OF THE [NII] LINE LINENUM: 260.0 SEQUENCE_1: USE SP TARGNAME: NGC4261-SE1 APERTURE: 0.1-PAIR-B TIME_PER_EXP: X2030.0 S_TO_N: 17 S_TO_N_TIME: FLUXNUM_1: 1 COMMENT_1: S/N AT THE PEAK OF THE [NII] LINE LINENUM: 270.0 SEQUENCE_1: USE SP TARGNAME: NGC4261-NE1 APERTURE: 0.1-PAIR-B TIME_PER_EXP: X2030.0 S_TO_N: 17 S_TO_N_TIME: FLUXNUM_1: 1 COMMENT_1: S/N AT THE PEAK OF THE [NII] LINE LINENUM: 271.0 TARGNAME: WAVE CONFIG: FOS/RD APERTURE: 0.1-PAIR-B OPMODE: ACCUM SP_ELEMENT: G570H NUM_EXP: 1 TIME_PER_EXP: DEF PRIORITY: 1 REQ_1: CYCLE 4 COMMENT_1: WAVECAL FOR LINE 270 ! End of RPSS template