! $Id: 5486,v 4.1 1994/07/27 18:33:37 pepsa Exp $ coverpage: title_1: I ZW 1: A TEMPLATE FE II QUASAR sci_cat: QUASARS & AGN sci_subcat: QUASAR EMISSION proposal_for: GO pi_fname: ARI pi_lname: LAOR pi_inst: INSTITUTE FOR ADVANCED STUDY pi_country: USA pi_phone: (609) 734-8023 hours_pri: 10.17 num_pri: 1 fos: Y off_fname: ALLEN off_lname: ROWE off_title: ASSOCIATE DIRECTOR off_inst: 2280 off_addr_1: INSTITUTE FOR ADVANCED STUDY off_addr_2: OLDEN LANE off_city: PRINCETON off_state: NJ off_zip: 08540 off_country: USA off_phone: (609) 734-8205 ! end of coverpage abstract: line_1: Quasars have strong Fe~II emission lines, however the emission mechanism is not line_2: well understood, and the enormous strength of the Fe II emission in some AGNs line_3: remains an enigma. Many other emission lines that are important diagnostics of line_4: the physical conditions of the Broad Line Regions of quasars are strongly line_5: blended with the rest frame UV Fe II emission. We have developed a technique line_6: for accurately measuring and subtracting the rest frame optical Fe II emission line_7: from quasars. This technique depends on having a high S/N ratio Fe II emission line_8: template generated from optical spectroscopy of the bright quasar I Zw 1. line_9: Similar detailed analysis can be done in the rest frame UV provided a high line_10: signal to noise template of the UV FeII emission is available. We will use the line_11: FOS to obtain high S/N and high spectral resolution spectra of the quasar line_12: I Zw 1 (z=0.061) in order to obtain the necessary template of Fe II emission line_13: in the 1200-3200A wavelength range. ! ! end of abstract general_form_proposers: lname: LAOR fname: ARI inst: 2280 country: USA ! lname: GREEN fname: RICHARD inst: 2902 country: USA ! lname: BOROSON fname: TODD inst: 2902 country: USA ! lname: JANNUZI fname: BUELL mi: T inst: 2280 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will observe I Zw 1 with the FOS and the higher resolution gratings line_2: (G130H, G190H, and G270H, R$=1300$) over the wavelength range 1100 to line_3: 3300A. This will require 3 exposures. Previous IUE and HST line_4: observations provide measurements of the UV flux over the wavelength line_5: regime of the planned observations and these flux values were used in line_6: calculating the exposure times. line_7: Acquisition of the targets will be performed using the 4.3 arcsecond line_8: aperture and the onboard Binary Search (as described in the FOS line_9: handbook). Prior to COSTAR the 0.25x2.0 arcsecond slit aperture line_10: provided the best tradeoff between the competing needs of maintaining line_11: spectral resolution while collecting as many photons as possible. Post line_12: COSTAR we can use the 1.0 arcsecond aperture without any significant line_13: loss in spectral resolution and with the savings in spacecraft time line_14: of the peak up acquisition that would be required to place an object line_15: in the slit. For this reason all of our proposed observations use line_16: the 1.0 arcsecond circular aperture. ! question: 4 section: 1 line_1: Past IUE observations of I Zw 1 have yielded only poor, low signal-to- line_2: noise and low spectral resolution observations of the UV emission. line_3: A prior HST program in cycle 2 obtained a G270H spectrum of S/N = 60. line_4: We are proposing to extend the wavelength coverage over which I Zw 1 has line_5: been well observed by obtaining G130H and G190H exposures. Since the bulk line_6: of the spacecraft overhead is the single target acquisition we are also line_7: proposing to obtain a new G270H exposure since the additional exposure line_8: time (30 minutes) is less than a 10\% increase to the total spacecraft time line_9: requested by the proposal and will produce a spectrum with S/N=100 at 2700A. ! question: 5 section: 1 line_1: We have NO special scheduling or observing requests. ! question: 6 section: 1 line_1: None. ! ! question: 8 section: 1 line_1: We already have the measured (accurate to 1$''$) position in the GASP line_2: system for I~Zw~1. We have no special requirements. ! question: 9 section: 1 line_1: The current proposal is to extend the results of the single observation o line_2: I Zw 1 (program 3879, Fe II Emission in AGNs) in both wavelength coverage line_3: and improve the S/N of the data. line_4: The Quasar Absorption Line Survey (2424) is closely related. This large line_5: database wil be used estensively to study the emission line properties of line_6: quasars (e.g. Weymann et al. 1993) and this analysis would benefit from the line_7: existence of the UV FeII emission line template our observations will produce. line_8: The initial scientific results of the Quasar Absorption Line Survey were line_9: reported in Bahcall \etal (1993). The data reduction and analysis procedures line_10: and the software that was developed to select and measure algorithmically line_11: absorption lines is described in Schneider et al. (1993). The fully calibrated line_12: data used in these papers has been made available to the community through line_13: STSCI. Observations obtained during the first six months of Cycle 1 determined line_14: the number densities at small redshifts of Lyman-alpha systems, of C IV lines line_15: and extragalactic halos, of Lyman-limit systems, of associated absorption line_16: systems, and of damped Lyman-alpha systems. The number density of C IV line_17: absorbers at small redshifts was found to be much less than at higher redshifts. line_18: The two-point correlation function of the Lyman-alpha lines was computed but line_19: the number of lines in the initial sample was too small to yield a definitive line_20: result. No obvious correlation was found between radio power of the quasars line_21: and the seven occurrences of associated absorption. ! question: 10 section: 1 line_1: The participating institutions will supply access to extensive computing line_2: facillities and experience computing and secretarial staff. line_3: Most of the academic year salaries for the members of this collaboration line_4: are provided by their home institutions or by other funds. ! !end of general form text general_form_address: lname: LAOR fname: ARI category: PI inst: 2280 addr_1: INSTITUTE FOR ADVANCED STUDY addr_2: OLDEN LANE city: PRINCETON state: NJ zip: 08540 country: USA phone: (609) 734-8023 telex: LAOR@GUINNESS.IAS.EDU, (609) 252-0738 ! lname: Jannuzi fname: Buell mi: T category: CON inst: 2280 city: Princeton state: NJ zip: 08540 country: U.S.A. phone: 609-734-8369 telex: jannuzi@guinness.ias.edu ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: IZW1 descr_1: E, descr_2: 313 pos_1: PLATE-ID=028Y, pos_2: RA = 00H 53M 35.02S +/- 0.1S, pos_3: DEC = +12D 41' 36.3" +/- 1.0" equinox: 2000 rv_or_z: Z=0.0611 fluxnum_1: 1 fluxval_1: V = 14.03 fluxnum_2: 2 fluxval_2: F(2700)=1.2 E-14 fluxnum_3: 3 fluxval_3: F(1700)=1.4 E-14 fluxnum_4: 4 fluxval_4: F(1350)=1.12 E-14 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: IZW1 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.0S priority: 1 req_1: ONBOARD ACQ FOR 2.00, 3.00; req_2: CYCLE 4 / 1-7 ! linenum: 2.000 targname: IZW1 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 110.0M s_to_n: 70 fluxnum_1: 3 priority: 1 req_1: SEQ 2.00, 3.00 NO GAP; comment_1: MINIMUM S TO N = 70 AT 1700 ANGSTROMS ! linenum: 3.000 targname: IZW1 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 35.0M s_to_n: 100 fluxnum_1: 2 priority: 1 comment_1: MINIMUM S TO N = 100 AT 2700 ANGSTROMS ! linenum: 4.000 targname: IZW1 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.9S priority: 1 req_1: ONBOARD ACQ FOR 5.00; ! linenum: 5.000 targname: IZW1 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 252.1M s_to_n: 50 fluxnum_1: 4 priority: 1 comment_1: MINIMUM S TO N = 50 AT 1350 ANGSTROMS ! linenum: 6.000 targname: IZW1 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.9S priority: 1 req_1: ONBOARD ACQ FOR 7; ! linenum: 7.000 targname: IZW1 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 252.1M s_to_n: 50 fluxnum_1: 4 priority: 1 comment_1: MINIMUM S TO N = 50 AT 1350 ANGSTROMS ! ! end of exposure logsheet ! No scan data records found