! $Id: 6149,v 5.1 1995/06/13 19:33:39 pepsa Exp $ ! File: 5222O.PROP ! Database: PEPDB ! Date: 14-JAN-1994:08:10:14 coverpage: title_1: HIGH-RESOLUTION IMAGING OF NUCLEAR STELLAR CLUSTERS IN AGN title_2: N1365 - LRF sci_cat: QUASARS AND AGN sci_subcat: HOST GALAXIES proposal_for: GTO/WF2 cont_id: 5222 pi_fname: JOHN pi_mi: T pi_lname: TRAUGER pi_inst: 2370 pi_country: USA hours_pri: 1.17 num_pri: 1 wf_pc: Y realtime: N time_crit: N ! end of coverpage abstract: line_1: We plan to use the high-resolution available to the PC-II to investigate the line_2: central arcsec of a number of nearby AGN. This study is motivated by line_3: suggestions of connections between dense stellar clusters formed in starbursts line_4: and conventional active galactic nuclei. We shall image the nuclei of the line_5: sample in the UV, and in U, V, and I in a manner that will allow us to line_6: adequately remove scattered light from the central source and determine the line_7: structure of extended emission in the surrounding regions. By examining the line_8: radial distribution of starlight from the nucleus we will be able to place line_9: astrophysically useful limits on the magnitude and dimensions of the putative line_10: central star cluster. In particular, we will determine if the origin of the line_11: `big blue bump' is hot stars in the cluster rather than the central engine, line_12: look for extended UV emission from `warmers', and examine the structure of line_13: the extended OIII emission-line region ! ! end of abstract general_form_proposers: lname: TRAUGER fname: JOHN title: PI mi: T inst: JPL country: USA ! lname: BURROWS fname: CHRIS inst: STSCI country: USA ! lname: CLARKE fname: JOHN inst: UNIV. OF MICHIGAN country: USA ! lname: CRISP fname: DAVID inst: JPL country: USA ! lname: GALLAGHER fname: JAY inst: UNIV. OF WISCONSIN country: USA ! lname: GRIFFITHS fname: RICHARD inst: JOHNS HOPKINS UNIV country: USA ! lname: HESTER fname: JEFF inst: ARIZONA STATE UNIV. country: USA ! lname: HOESSEL fname: JOHN inst: UNIV. OF WISCONSIN country: USA ! lname: HOLTZMAN fname: JOHN inst: LOWELL OBSERVATORY country: USA ! lname: MOULD fname: JEREMY inst: CALTECH country: USA ! lname: WESTPHAL fname: JAMES inst: CALTECH country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We plan to observe all of the sample in the UV, in U, V, and I, and line_2: in OIII emission where appropriate. line_3: The PC-II has a limited dynamic range, so to provide adequate S/N to line_4: enable scattered light from the central source to be removed, we line_5: require exposures of three different durations. The shortest should line_6: remain within the dynamic range of the ADC but provide good S/N at the line_7: peak of the PSF; the longest should provide good S/N in the wings of line_8: the PSF whilst minimizing bleeding from the central pixels; the line_9: intermediate exposure will be used to bridge these exposures together. line_11: We shall split each exposure in two to allow cosmic ray events to be line_12: detected. line_14: All of these exposures will be read with a gain of 15 electrons/ADU. ! question: 4 section: 1 line_1: Ground-based telescopes simply cannot provide the resolution required line_2: for this programme. In addition, we require the UV capabilities of line_3: HST. line_5: We expect the limiting factor in these observations will be our line_6: ability to accurately subtract light from the central bright source. line_7: The OTA handbook predicts that the surface brightness of scattered line_8: light at about 1 arcsec is about 0.001 of the peak surface brightness line_9: at 2000A, 0.005 at 4000A, and 0.06 at 8000A. In the UV, the dominant line_10: effect is thought to be micro-structure in the primary, whereas in the line_11: red Airy diffraction dominates. The dynamic range of the PC-II is line_12: 4096; with a gain of 15 the ADC will saturate at about 60k counts. We line_13: expect the chips will physically saturate and begin to bleed shortly line_14: after this. We expect that the fraction of the total counts in the line_15: central PC-II pixel will be about 0.2. We shall allow a safety margin line_16: of a factor of 2, as the perils of over exposure are worse than line_17: (moderate) under exposure. ! question: 13 section: 1 line_1: This proposal forms an important part of the `Star Formation in line_2: Galaxies' section of the WFPC-2 GTO program. ! !end of general form text general_form_address: lname: Trauger fname: John mi: T category: PI inst: 2370 addr_1: JPL addr_2: 4800 Oak Grove Drive city: Pasadena state: CA zip: 91109 country: USA phone: 818 354 9594 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC1365 descr_1: E,301,312 descr_2: E,909,910,915,919,924 pos_1: RA = 03H 31M 41.33S +/- 1" , pos_2: DEC = -36D 18' 25.1" +/- 1" equinox: 1950 rv_or_z: V = +1639 fluxnum_1: 1 fluxval_1: SURF(V) = 17.5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 14.000 targname: NGC1365 config: WFPC2 opmode: IMAGE aperture: LRF sp_element: LRF wavelength: 5032 num_exp: 2 time_per_exp: 1200S priority: 1 param_1: CR-SPLIT = NO param_2: ATD-GAIN = 7 req_1: CYCLE 4; req_3: PCS MODE F ! ! end of exposure logsheet ! No scan data records found