! File: 4793C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:03:42:41 coverpage: title_1: THE EXTENDED FEATURELESS CONTINUUM SOURCE IN CYGNUS A title_2: - CYCLE 1 SPECTROSCOPIC FOLLOW-UP sci_cat: QUASARS & AGN sci_subcat: RADIO GALAXIES proposal_for: GO cont_id: 2177 pi_fname: ROBERT pi_lname: ANTONUCCI pi_inst: STSCI pi_country: USA keywords_1: GALAXY; RADIO GALAXY hours_pri: 4.66 num_pri: 1 wf_pc: X fos: X funds_amount: 19152 funds_length: 12 funds_date: JUN-91 pi_position: PROF. off_fname: RAY off_lname: SAWYER off_title: CHAIR off_inst: UCSB PHYSICS DEPT off_addr_1: SANTA BARBARA off_city: SANTA BARBARA off_state: CA off_zip: 93106 off_country: USA off_phone: 805-893-4350 ! end of coverpage abstract: line_1: Cygnus A is by far the nearest luminous Classical Double radio galaxy.The line_2: nuclear spectrum shows the canonical mix of light from old stars, a strong line_3: featureless continuum (FC), and a very strong, high ionization emission line line_4: spectrum. Several observers have recently come to the astonishing conclusion line_5: that the featureless continuum is spatially resolved.(There is no reason to line_6: think Cygnus A is unusual in this respect: if other luminous Classical Doubles line_7: had the same size optical source, their angular sizes would be too small to line_8: resolve from the ground).Furthermore, the obvious explanations of scattered line_9: light from a point source, and of optical synchrotron radiation, are strongly line_10: disfavored by optical polarization mapping. The only idea seriously considered line_11: in the literature for such an extended, unpolarized continuum is the Warmer line_12: theory, which unequivocally predicts Fv=v1 in the UV. We want to know whether line_13: the spectrum is Fv=v-1 as for quasars, or whether it rises rapidly with line_14: frequency as for Warmers. Also, if the 1550A continuum is dominated by normal O line_15: stars as in the starburst and some Warmer models we can diagnose it line_16: unequivocally via the CIV wind absorption. We cannot reliably determine the line_17: spectrum of the featureless continuum from the ground because of contamination line_18: by the light of old stars.We would also like to take a WFC picure in the UV, to line_19: understand the morphology of the featureless continuum source without confusion line_20: with the old stars. ! ! end of abstract general_form_proposers: lname: ANTONUCCI fname: ROBERT title: PROF. inst: UCSB country: USA ! lname: KINNEY fname: A mi: L inst: STSCI country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: First we will take a WFC image with the F336W filter. The line_2: Featureless Continuum flux at 5135A is 3.0x10-16 ergs/cm2 line_3: sec A (Osterbrock and Miller 1975),equivalent to 7.0x10-16 line_4: ergs/cm2 sec A at 3360A if Fv alpha nu0 (Warmer hypothesis line_5: with Galactic reddening allowance), and 3.0x10-16 ergs/cm2 line_6: sec A if Fv alpha nu-2. Imaging work described in the Sci. line_7: Just. shows that this will be spread over about 3 sq. arcsec. line_8: The WFC simulator (Ewald 1987) and ests. from the WF/PC Hand- line_9: book show that SNR=10/pix can be reached in 80 min under the line_10: conservative flux assumption. (Complimentary optical images line_11: are planned in the WF/PC IDT GTO program). In order to line_12: characterize the UV continuum, we request an exposure with line_13: the FOS Blue Tube, G160L grating, and also with the Red Tube line_14: and G270H grating. We will use the WFC picture to place the line_15: 4."3 aperture on the region brightest in the UV. line_16: We assume this includes half the UV flux, and make the con- line_17: servative nu -2 assumption. The FOS simulator indicates that line_18: that SNR=5 can be achieved with G160L in 76 min (with an line_19: approx. correction for the psf and aperture change). We can line_20: get SNR=6 in 76 minutes with G270H. We show our simulations line_21: below. (If the UV continuum is from hot stars, it will be line_22: much bluer so our SNR will be much higher, and the CIV line_23: absorption troughs easy to distinguish.) ! question: 3 section: 2 line_1: NOTE: Coords have been updated from WF/PC EARLY ACQ image line_2: taken in Program 2177, and ACQ/BINARY exposure time in Exp line_3: Log line 2 has been updated also. - 7 December, 1992 ! !end of general form text general_form_address: lname: ANTONUCCI fname: ROBERT category: PI inst: STSCI addr_1: PHYSICS DEPARTMENT city: SANTA BARBARA state: CA zip: 93106 country: USA ! ! end of general_form_address records fixed_targets: targnum: 2 name_1: CYGNUS-A-OFFSET descr_1: J,707 pos_1: PLATE-ID=003S, pos_2: RA=19H 59M 26.01S +/- 1.0", pos_3: DEC=40D 43' 51.76" +/- 1.0" equinox: 2000 acqpr_1: BKG fluxnum_1: 1 fluxval_1: V=15.0 +/- 0.5 ! targnum: 3 name_1: CYGNUS-A-NUCLEUS descr_1: E,315,910 pos_1: RA=19H 59M 28.47S +/- 0.3", pos_2: DEC=40D 44' 01.94" +/- 0.3", equinox: 2000 fluxnum_1: 1 fluxval_1: F(2700)=3.0 +/- 2.0E-16 fluxnum_2: 2 fluxval_2: F(1600)=5.0 +/- 4.0E-16 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 2.000 targname: CYGNUS-A-OFFSET config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.7S priority: 1 req_1: CYCLE 2; req_2: ONBOARD ACQ FOR 3-4 ! linenum: 3.000 targname: CYGNUS-A-NUCLEUS config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 5716S s_to_n: 5 fluxnum_1: 2 priority: 1 req_1: CYCLE 2 comment_1: NUCLEUS POSITION WAS DETERMINED comment_2: FROM WFC IMAGE IN PROPOSAL 2177. ! linenum: 4.000 targname: CYGNUS-A-NUCLEUS config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 5716S s_to_n: 6 fluxnum_1: 1 priority: 1 req_1: CYCLE 2 comment_1: NUCLEUS POSITION WAS DETERMINED comment_2: FROM WFC IMAGE IN PROPOSAL 2177. ! ! end of exposure logsheet ! No scan data records found