! $Id: 5441,v 19.1 1994/07/27 18:01:55 pepsa Exp $ coverpage: title_1: THE INNER REGIONS OF QUASARS title_2: CYC4 sci_cat: QUASARS & AGN sci_subcat: QUASAR EMISSION proposal_for: GO cont_id: 2578 pi_fname: BEVERLEY pi_mi: J. pi_lname: WILLS pi_inst: UNIVERSITY OF TEXAS pi_country: USA pi_phone: 512-471-3424 hours_pri: 24.00 num_pri: 18 fos: Y funds_amount: 191062 funds_length: 12 funds_date: AUG-94 ! end of coverpage abstract: line_1: We propose to complete our program to produce THE definitive sample of radio line_2: loud quasar spectra, each measured from rest wavelength below Ly-alpha to line_3: beyond H-alpha. This is the ONLY large complete HST sample being used to line_4: investigate the intrinsic properties of quasars. The FOS data are being line_5: supplemented with quasi-simultaneous optical and infrared spectroscopy from line_6: McDonald Observatory, KPNO, UKIRT, and CTIO. The ~ 50 objects are selected to line_7: cover a wide range in radio-core dominance - a measure of inclination of the line_8: central engine's axis; we constrain the range in extended radio luminosity, line_9: which is inclination INDEPENDENT, in order to test the dependence of spectro- line_10: scopic parameters on inclination alone. This is a minumum sample size for line_11: meaningful statistics. We accurately compare strengths of different emission line_12: lines, their profiles and profile shifts, and continuum shapes, and use exist- line_13: ing radio & X-ray data to investigate some basic questions: Are there inclined line_14: accretion disks\? Is there stratification of the broad line region (BLR)\? Is line_15: there angle dependent and luminosity-dependent ionization of the BLR\? What is line_16: the origin of the Fe II emission\? What is the importance of line & continuum line_17: reddening\? How is X-ray & radio emission related to optical & UV properties\? line_18: The spectroscopy is being complemented by our VLA mapping, B, R & radio-core line_19: variability monitoring. In a recent preprint we demonstrate the usefulness of line_20: our optical-UV data in a first extensive study of the NLR in very luminous AGNs. ! ! end of abstract general_form_proposers: lname: WILLS fname: BEVERLEY mi: J. inst: UNIVERSITY OF TEXAS country: USA ! lname: WILLS fname: DEREK inst: UNIVERSITY OF TEXAS country: USA ! lname: BALDWIN fname: JACK mi: A. inst: CTIO country: CHILE ! lname: FERLAND fname: GARY mi: J. inst: UNIVERSITY OF KENTUCKY country: USA ! lname: NETZER fname: HAGAI inst: TEL AVIV UNIVERSITY country: ISRAEL ! lname: BROWNE fname: IAN mi: W. inst: NUFFIELD RADIO ASTRONOMY LABORATORIES country: UNITED KINGDOM ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The sample is described in \S 2, where Table 1 gives a list of the quasars. line_2: We indicate those with completed observations, and those hoped for in Cycle 3 line_3: but for which observing time is not guaranteed. line_5: We have selected quasars with luminosity in the extended radio emission, line_6: log L(ext), from 26.5 to 27.6 (erg/s, q=0, H=50 km/s/Mpc). For HST observations line_7: we plan to observe those with z < 1.8 and V < 18, which allows us to observe line_8: all Ly-alpha and CIV broad emission lines with HST. (The remainder of our sample line_9: of higher z either have been or will be observed from the ground.) line_11: This sample gives us a wide range of the ratio of core to extended radio line_12: emission from about 0.01 to 100 (at 6 cm rest wavelength), and a similar range line_13: in X-ray and radio core luminosity. line_15: In cycle 4 we propose to obtain FOS spectra for 18 quasars (depending on line_16: execution of Cycle 3 observations). We plan to cover rest wavelengths from 1160 line_17: A, to observed wavelengths of 3300 A or 4800 A, where the spectra will connect line_18: with our ground based observations. We plan to cover the region near 3200 line_19: - 3500 A with the G400H FOS grating setting in cases where important emission line_20: lines lie near the atmospheric cutoff. We aim for s/n = 19.5 per diode in the line_21: continuum in the region of strong emission lines. In this way we will cover all line_22: available strong lines with sufficient s/n to measure accurate line intensities, line_23: central wavelengths and line widths. ! question: 3 section: 2 line_1: line_2: We plan to use the 4.3 or 1'' aperture for spectrophotometry and to minimize line_3: background radiation. Spectrophotometry is important for the comparison of line line_4: strengths and spectral energy distributions between the HST and ground-based line_5: spectrophotometry. The point source resolution will be about 850 (~350 km/s) -- line_6: sufficient for the definition of broad line profiles, and probably sufficient, line_7: in nearly all cases, for taking into account the effects of Galactic, line_8: intergalactic, and intrinsic absorption features on our measurements of line and line_9: continuum emission. line_11: There is a very loose time constraint in that we want the quasars to be line_12: available in the night time sky as seen from the ground, at the time of FOS line_13: observations. It is extremely important to complete the sample as soon as line_14: possible so that the science, including our previous cycle observations can be line_15: investigated statistically in a timely way. ! question: 4 section: 1 line_1: The heart of the project is the comparison of UV lines (Ly-alpha, NV 1240, 1400, line_2: CIV 1549, CIII]1909, Mg II 2798, Fe II 2000 - 3000 A) with optical and IR ground line_3: based spectra including hydrogen Balmer lines, Fe II 4570 and 5300 A etc, line_4: CIII], Mg II, He 4686, (and Paschen beta for a significant subset) that we are line_5: obtaining at McDonald, KPNO, CTIO and UKIRT. Therefore this project can only be line_6: done with HST and for a low to medium redshift sample. line_7: The statistical spectral analyses we are proposing would be impossible without line_8: HST, and so have never been attempted before. line_10: Why not IUE? The sensitivity, wavelength resolution and calibration accuracy line_11: are too low for the line wavelength, profile, and line and continuum flux line_12: measurements we are proposing. line_13: Number of objects: line_14: The total number of objects (52 in our HST program, supplemented by 3-4 line_15: archival spectra) is not very large considering the number of parameters we wish line_16: to investigate statistically, and our previous statistical studies of less line_17: complete samples suggest that we cannot do with fewer objects. We have line_18: intriguing correlations at the 2.6 to 3.3 sigma level with about 40% of our line_19: sample, and with the sample size we propose it should be possible to confirm line_20: or reject these correlations. The sample size is limited by the redshift, line_21: magnitude and extended radio luminosity selection criteria. The quasars must line_22: have good radio maps. ! question: 4 section: 2 line_1: Exposure time calculations: line_2: The correctness of our previous exposure time calculations is borne out by line_3: the SNR of our data already obtained (Fig.1). line_5: We have formed a composite quasar spectrum from below Ly alpha to beyond H-a, line_6: using quasars observed with IUE and at McDonald Observatory. We proceed for line_7: each quasar of our HST sample as follows: 1. Redshift the standard spectrum to line_8: that of the quasar. 2. Apply a standard Galactic reddening curve, 3. Scale line_9: this spectrum so that the V-magnitude in the observer's frame agrees with line_10: published values or our own photometry. 4. Multiply this spectrum by the line_11: expected HST FOS COSTAR response for different grating settings and cameras, and line_12: by the curve representing the wavelength dependent light losses in the 1'' line_13: aperture. line_14: Thus we convert the spectrum to the number of counts expected per diode per line_15: second. 5. We have then calculated the exposure time according to the FOS Hand line_16: Book formula, assuming standard observing procedures and for s/n = 19.5 per line_17: diode, in the continuum in the regions of strong emission lines. (1 diode is the line_18: instrumental resolution for the 1'' aperture.) 6. For the fainter objects line_19: we have checked the importance of the contribution of the Galactic background, line_20: using formulae from the previous FOS Handbook, and more recently the increased line_21: background contribution from the detector faceplate. We use the blue digicon line_22: rather than the red for G190H if an important emission line falls between about line_23: 1550 and 1700 A. We use G400H only when important emission lines fall close to ! question: 4 section: 3 line_1: the atmospheric cutoff and so cannot be observed accurately from the ground. ! question: 5 section: 1 line_1: THE SCHEDULING REQUIREMENTS ARE GIVEN SEPARATELY, IN A TABLE TOO LARGE TO line_2: APPEAR HERE. (This para added 1994 February for Tony Roman). line_3: Note that, within the table scheduling constraints, it is prefereable to line_4: group observations within a few days of New Moon, so that several objects line_5: can be observed efficiently in one dark-moon observing run. About 4-6 objects line_6: per month is manageable: 4 in summer, 6 in winter. They should not be at all line_7: the same right ascensions in a given month because then we can't spread the line_8: observations throughout a ground-based night. line_9: ------------------------------------------------------------------------------- line_10: We have the weak constraint that the HST observations should be made while the line_11: quasars are in the night sky as observed from the ground. We attempt to line_12: co-ordinate ground-based observations with the scheduled HST times, the line_13: quasi-simultaneity required depending on the degree of time variability. We are line_14: monitoring the flux variability from the ground. ! question: 6 section: 1 line_1: ! ! question: 8 section: 1 line_1: THE SCHEDULING REQUIREMENTS ARE GIVEN SEPARATELY, IN A TABLE TOO LARGE TO line_2: APPEAR HERE. (This para added 1994 February for Tony Roman). line_3: Note that, within the table scheduling constraints, it is prefereable to line_4: group observations within a few days of New Moon, so that several objects line_5: can be observed efficiently in one dark-moon observing run. About 4-6 objects line_6: per month is manageable: 4 in summer, 6 in winter. They should not be at all line_7: the same right ascensions in a given month because then we can't spread the line_8: observations throughout a ground-based night. line_9: ------------------------------------------------------------------------------- line_11: We attempt to co-ordinate ground and space-based observations, but this does not line_12: fall into a `time-critical' category. We prefer HST observations to be scheduled line_13: near dark-moon time, when the quasars are available at night from the ground. line_14: It is preferable for the few highly variable objects to be observed as line_15: simultaneously as practicable. The ground-based spectroscopy will be obtained line_16: at McDonald Observatory, and also CTIO, KPNO, and UKIRT. An line_17: imminent improvement at McDonald will be the availability of a dual beam line_18: (red/blue) spectrograph with resolution similar to that of the G...H settings of line_19: the FOS, allowing the entire 3300 to 1 micron region to be observed line_20: simultaneously and efficiently (project of B.J. Wills and G.J. Hill). line_22: We are monitoring the photometric variability of our sample quasars line_23: (Netzer, Wills, Wills and Ferland - observations at Wise Observatory, Tel Aviv ! question: 8 section: 2 line_1: University, Israel), with some additional photometry from McDonald Observatory line_2: and CTIO, a program that will give us information on changes in optical flux line_3: density for improved estimates of HST exposure times (and for more astronomical line_4: reasons). line_5: We have measured accurate positions for nearly all quasars of our sample, using line_6: the STScI's GASP. line_7: Data rights: We would prefer to have the data released for archival use, as line_8: soon as we have had a chance to examine the sample statistically. In view of line_9: the spread over 4 cycles, we do not know if this is a reasonable request. ! question: 9 section: 1 line_1: The Inner Regions of Quasars' (This project): Cycle 1 (2578), Cycle 1 line_2: (repeats...) (4052), Cycle 2 (3858), Cycle 2 repeats (5002), Cycle 3 (4502). line_3: 2306 `Physical Conditions in the NLR' (J.A. Baldwin. P.I.) line_4: 3982 `Physical Conditions in the NLR Part 2' (J.A. Baldwin. P.I.) line_6: The same investigators are involved in all of the above. line_8: Cycle 3: `Hidden QSOs in Ultraluminous IRAS AGN' (4351) -- P.I. B.Wills. line_10: This proposal is (unofficially?) a continuation of `The Inner Regions of line_11: Quasars' above. line_12: (See also the Scientific Justification where previous results are described in line_13: detail.) line_15: - We conclude that the narrow lines in the UV, in particular narrow L-alpha, are line_16: more than a factor of 5-10 weaker than can be accounted for by reasonable photo- line_17: ionization models. Comparison of H-alpha, H-beta and L-alpha strongly suggests line_18: significant dust reddening. This is the first extensive study of the NLR in line_19: high luminosity AGN. line_21: - Fortuitously, we discovered that the Egret telescope on the Compton Gamma Ray line_22: Observatory made gamma-ray observations of 3C279 simultaneously with our HST/FOS line_23: spectroscopy. HST and ground-based spectra reveal a steep UV spectrum and a ! question: 9 section: 2 line_1: high gamma-ray flux that is impossible to explain by beamed or unbeamed inverse line_2: Compton scattering. This paper also points out the extremely unusual strong red line_3: wing on some of the broad UV lines in this object. line_5: - A related ground-based program to study line profiles of H-beta, C IV and line_6: other lines is being carried out with graduate student Michael Brotherton. (This line_7: program is an important part of his PhD work). line_8: We find and discuss several striking new correlations that involve the density, line_9: ionization and dynamics of the BLR. This program is strongly related to, and line_10: supports, our HST astrophysics. line_12: Status of HST analysis: About 22 quasars out of our sample of 52 have been line_13: observed with HST (early May 1993). Data corrected for GIMP and instrumental line_14: background, along with appropriate flat fields, became available in May 1992 line_15: but correct flat fields were not available for all until February-March 1993. line_16: We have corrected all the data for spurious effects (spikes, dead and noisy line_17: diodes), and measured all line strengths and equivalent widths in both the HST line_18: and ground-based data. We have also compared all broad and narrow line line_19: profiles, and are currently making a special effort to tie down the wavelength line_20: scales using absorption features in the UV and optical (e.g. Mg II, Fe II line_21: interstellar lines). line_23: Our available observations make up about 40% of the complete sample. In the ! question: 9 section: 3 line_1: Scientific Justification we present trends that the data appear to show, but line_2: the analysis as far from complete as we need the Cycle 3 and 4 observations. line_3: However we expect to have a preprint by the end of May, concerning broad line line_4: profile comparisons, and trends with core-dominance and luminosity. line_6: Publications resulting from the above data: line_8: The Narrow Line Region of Quasars: HST and McDonald Spectroscopy, Wills, Wills, line_9: Netzer, Brotherton, Han, Baldwin, Ferland and Browne, ApJ, 410, 680 (1993). line_11: The Optical-UV Spectrum of 3C279 During Outburst, Shrader, Webb, Balonek, line_12: Brotherton, Wills, Wills & McCollum, Astronomy & Astrophysics, submitted. line_13: (results also appeared in GRO Conference 1992 October, St Louis). line_15: The Statistics of QSO Broad Emission Line Profiles I: The CIV 1549 Line and the line_16: 1400 Feature, Wills, Brotherton, Steidel, and Sargent, ApJ, 415, 000 (1993). line_18: Simultaneous Gamma Ray Observations and the Ultraviolet-Optical Spectrum of line_19: 3C279, B.Wills, Kazanas, D., Han, Brotherton, Netzer, Wills, Baldwin, Ferland line_20: and Browne, ApJ, to be submitted. ! question: 10 section: 1 line_1: Data analysis facilities, ground-based telescope support and observing time line_2: (University of Texas' McDonald Observatory), salaries for senior personnel line_3: beyond those specified in the budget. Availability of personnel to update line_4: IRAF/STSDAS, etc., availability of student researchers. Student assistance line_5: beyond that specified in the proposal budget. line_6: The University is supporting construction of the dual-beam faint object line_7: spectrograph to be used in this project, at McDonald Observatory. ! !end of general form text general_form_address: lname: WILLS fname: BEVERLEY mi: J. category: PI inst: University of Texas addr_1: Department of Astronomy, RLM 15.308 addr_2: University of Texas at Austin city: Austin state: TX zip: 78712 country: USA phone: 512-471-3424 telex: bev@astro.as.utexas.edu ! ! This is the end of the General Form !FIXED_TARGETS: !include_file: romantarg fixed_targets: targnum: 1 name_1: PHL1093 name_2: 0137+01 descr_1: E,314,910 pos_1: PLATE-ID = 00GZ, pos_2: RA = 01H 39M 57.27S +/- 0.5", pos_3: DEC = +01D 31' 46.3" +/- 0.5" equinox: 2000 rv_or_z: Z = 0.258 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE fluxnum_1: 1 fluxval_1: V = 17.07 +/- 0.5 ! targnum: 2 name_1: PKS1001+22 descr_1: E,314,910 pos_1: PLATE-ID = 027Z, pos_2: RA = 10H 04M 45.74S +/- 0.5", pos_3: DEC = +22D 25' 19.1" +/- 0.5" equinox: 2000 rv_or_z: Z = 0.974 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE fluxnum_1: 1 fluxval_1: V = 18 +/- 1 ! targnum: 3 name_1: LB2136 name_2: 1150+497 descr_1: E,314,910 pos_1: PLATE-ID = 024C, pos_2: RA = 11H 53M 24.46S +/- 0.5", pos_3: DEC = +49D 31' 08.6" +/- 0.5" equinox: 2000 rv_or_z: Z = 0.334 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE fluxnum_1: 1 fluxval_1: V = 17.10 +/- 0.5 ! targnum: 4 name_1: B21248+30 descr_1: E,314,910 pos_1: PLATE-ID = 01PM, pos_2: RA = 12H 50M 25.54S +/- 0.5", pos_3: DEC = +30D 16' 39.8" +/- 0.5" equinox: 2000 rv_or_z: Z = 1.061 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE fluxnum_1: 1 fluxval_1: V = 18.3 +/- 1 ! targnum: 5 name_1: NRAO140 name_2: 0333+321 descr_1: E,314,910 pos_1: PLATE-ID = 0050, pos_2: RA = 03H 36M 30.17S +/- 0.5", pos_3: DEC = +32D 18' 29.0" +/- 0.5" equinox: 2000 rv_or_z: Z = 1.263 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE fluxnum_1: 1 fluxval_1: V = 17.25 +/- 0.3 ! targnum: 6 name_1: PKS1656+053 descr_1: E,314,910 pos_1: PLATE-ID = 01HA, pos_2: RA = 16H 58M 33.46S +/- 0.3", pos_3: DEC = +05D 15' 16.5" +/- 0.3" equinox: 2000 rv_or_z: Z = 0.879 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE comment_4: CHECK POSITION, FLUX fluxnum_1: 1 fluxval_1: V = 16.5 +/- 0.3 ! targnum: 7 name_1: 3C281 name_2: 1305+069 descr_1: E, 314, 910 pos_1: RA = 13H 07M 53.96S +/- 0.3", pos_2: DEC = +06D 42' 14.2" +/- 0.3" equinox: 2000 rv_or_z: Z = 0.599 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE comment_4: check position, flux fluxnum_1: 1 fluxval_1: V = 17.6 +/- 0.4 ! targnum: 8 name_1: B20827+24 descr_1: E,314,910 pos_1: PLATE-ID = 02UG, pos_2: RA = 08H 30M 52.09S +/- 0.3", pos_3: DEC = +24D 10' 59.7" +/- 0.3" equinox: 2000 rv_or_z: Z = 0.939 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE comment_4: CHECK POSITION, FLUX fluxnum_1: 1 fluxval_1: V = 17.26 +/- 0.5 ! targnum: 9 name_1: 4C29-45 descr_1: E,314,910 pos_1: PLATE-ID = 01TE, pos_2: RA = 11H 59M 31.85S +/- 0.4", pos_3: DEC = +29D 14' 43.5" +/- 0.4" equinox: 2000 rv_or_z: Z = 0.729 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE comment_4: CHECK POSITION, FLUX fluxnum_1: 1 fluxval_1: V = 18.0 +/- 1. ! targnum: 10 name_1: MC1118+12 descr_1: E,314,910 pos_1: PLATE-ID = 03QR, pos_2: RA = 11H 21M 29.76S +/- 0.4", pos_3: DEC = +12D 36' 16.9" +/- 0.4" equinox: 2000 rv_or_z: Z = 0.685 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE comment_4: CHECK POSITION, FLUX fluxnum_1: 1 fluxval_1: V = 18.0 +/- 1.0 ! targnum: 11 name_1: B21351+31 descr_1: E,314,910 pos_1: PLATE-ID = 019J, pos_2: RA = 13H 54M 05.39S +/- 0.4", pos_3: DEC = +31D 39' 2.4" +/- 0.4" equinox: 2000 rv_or_z: Z = 0.1.326 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE comment_4: CHECK POSITION, FLUX fluxnum_1: 1 fluxval_1: V = 17.4 +/- 1.0 ! targnum: 12 name_1: 4C40-24 descr_1: E,314,910 pos_1: PLATE-ID = 01BS, pos_2: RA = 09H 48M 55.33S +/- 0.4", pos_3: DEC = +40D 39' 45.0" +/- 0.4" equinox: 2000 rv_or_z: Z = 1.252 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE comment_4: CHECK POSITION, FLUX fluxnum_1: 1 fluxval_1: V = 17.5 +/- 1.0 ! targnum: 13 name_1: MC0042+101 descr_1: E,314,910 pos_1: PLATE-ID = 028Y, pos_2: RA = 00H 44M 58.78S +/- 0.4", pos_3: DEC = +10D 26' 52.8" +/- 0.4" equinox: 2000 rv_or_z: Z = 0.583 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE comment_4: CHECK POSITION, FLUX fluxnum_1: 1 fluxval_1: V = 17.5 +/- 1.0 ! targnum: 14 name_1: S51803+78 descr_1: E,314,910 pos_1: PLATE-ID = 01H6, pos_2: RA = 18H 00M 45.70S +/- 0.4", pos_3: DEC = +78D 28' 04.1" +/- 0.4" equinox: 2000 rv_or_z: Z = 0.684 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE comment_4: CHECK POSITION, FLUX fluxnum_1: 1 fluxval_1: V = 17.0 +/- 1.0 ! targnum: 15 name_1: PKS0214+10 descr_1: E,314,910 pos_1: PLATE-ID = 03QO, pos_2: RA = 02H 17M 07.67S +/- 0.4", pos_3: DEC = +11D 04' 09.6" +/- 0.4" equinox: 2000 rv_or_z: Z = 0.408 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE comment_4: CHECK POSITION, FLUX fluxnum_1: 1 fluxval_1: V = 16.0 +/- 1.0 ! targnum: 17 name_1: PKS1055+20 descr_1: E,314,910 pos_1: PLATE-ID = 01AJ, pos_2: RA = 10H 58M 17.90S +/- 0.4", pos_3: DEC = +19D 51' 50.7" +/- 0.4" equinox: 2000 rv_or_z: Z = 1.110 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE comment_4: CHECK POSITION, FLUX fluxnum_1: 1 fluxval_1: V = 17.1 +/- 1.0 ! targnum: 18 name_1: TEX1156+213 descr_1: E,314,910 pos_1: PLATE-ID = 01TG, pos_2: RA = 11H 59M 26.20S +/- 0.4", pos_3: DEC = +21D 06' 56.2" +/- 0.4" equinox: 2000 rv_or_z: Z = 0.349 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE comment_4: CHECK POSITION, FLUX fluxnum_1: 1 fluxval_1: V = 17.5 +/- 1.0 ! targnum: 19 name_1: 4C64-15 descr_1: E,314,910 pos_1: PLATE-ID = 00MD, pos_2: RA = 12H 17M 40.86S +/- 0.4", pos_3: DEC = +64D 07' 07.4" +/- 0.4" equinox: 2000 rv_or_z: Z = 1.294 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE comment_4: CHECK POSITION, FLUX fluxnum_1: 1 fluxval_1: V = 17.4 +/- 1.0 ! targnum: 21 name_1: 4C73-18 descr_1: E,314,910 pos_1: PLATE-ID = 00MA, pos_2: RA = 19H 27M 48.54S +/- 0.4", pos_3: DEC = +73D 58' 1.6" +/- 0.4" equinox: 2000 rv_or_z: Z = 0.302 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE comment_4: CHECK POSITION, FLUX fluxnum_1: 1 fluxval_1: V = 16.5 +/- 1.0 ! ! end of fixed targets !EXPOSURE_LOGSHEET: !include_file: romanexp exposure_logsheet: linenum: 1.110 targname: PHL1093 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 18S priority: 1 req_1: ONBOARD ACQ FOR 1.12-1.21; req_2: GROUP 1.11-1.21 NO GAP; req_3: CYCLE 4; req_4: AT 31-OCT-1994 +/- 72D; comment_1: BLUE SIDE ACQ BIN- EXP=40 ! linenum: 1.120 targname: PHL1093 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2767 num_exp: 1 time_per_exp: 6.04M s_to_n: 9.71 fluxnum_1: 1 priority: 1 req_1: CYCLE 4; ! linenum: 1.130 targname: PHL1093 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G190H wavelength: 1954 num_exp: 1 time_per_exp: 13.98M s_to_n: 9.71 fluxnum_1: 1 priority: 1 req_1: CYCLE 4; ! linenum: 1.210 targname: PHL1093 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 74.6M s_to_n: 9.16 fluxnum_1: 1 priority: 1 req_1: CYCLE 4; ! linenum: 2.110 targname: PKS1001+22 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 32S priority: 1 req_1: ONBOARD ACQ FOR 2.12; req_2: GROUP 2.11-2.12 NO GAP; req_3: CYCLE 4; req_4: AT 1-FEB-1995 +/- 67D; ! linenum: 2.120 targname: PKS1001+22 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2676 num_exp: 1 time_per_exp: 15.22M s_to_n: 9.44 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 3.110 targname: LB2136 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 31S priority: 1 req_1: ONBOARD ACQ FOR 3.12-3.21; req_2: GROUP 3.11-3.21 NO GAP; req_3: CYCLE 4; comment_1: BLUE SIDE ACQ BIN- EXP=22S comment_2: See Tony Roman for scheduling table ! linenum: 3.120 targname: LB2136 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2767 num_exp: 1 time_per_exp: 5.30M s_to_n: 9.71 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 3.210 targname: LB2136 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G190H wavelength: 1954 num_exp: 1 time_per_exp: 57.1M s_to_n: 9.71 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 4.110 targname: B21248+30 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 43S priority: 1 req_1: ONBOARD ACQ FOR 4.12; req_2: GROUP 4.11-4.12 NO GAP; req_3: CYCLE 4; req_4: AT 16-MAR-1995 +/- 81D; ! linenum: 4.120 targname: B21248+30 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2767 num_exp: 1 time_per_exp: 21.85M !10.17M s_to_n: 9.77 fluxnum_1: 1 priority: 1 req_2: CYCLE 4 ! linenum: 5.110 targname: NRAO140 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 38S priority: 1 req_1: ONBOARD ACQ FOR 5.12; req_2: GROUP 5.11-5.12 NO GAP; req_3: CYCLE 4; comment_1: BLUE SIDE ACQ BIN- EXP=38S comment_2: See Tony Roman for scheduling table ! linenum: 5.120 targname: NRAO140 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 12.73M !16.03M s_to_n: 9.35 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 6.110 targname: PKS1656+053 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 12S priority: 1 param_1: BRIGHT=45000 req_1: ONBOARD ACQ FOR 6.120; req_2: GROUP 6.11-6.12 WITHIN 24H; req_3: CYCLE 4 comment_1: See Tony Roman for scheduling table ! linenum: 6.120 targname: PKS1656+053 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 7.48M !5.65M s_to_n: 10.9 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 7.110 targname: 3C281 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 22S priority: 1 param_1: BRIGHT=230000 req_1: ONBOARD ACQ FOR 7.12-7.22; req_2: GROUP 7.11-7.22 WITHIN 24H; req_3: CYCLE 4 comment_1: See Tony Roman for scheduling table ! linenum: 7.120 targname: 3C281 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 20.65M !11.20M s_to_n: 9.80 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 7.220 targname: 3C281 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 11.23M !6.12M s_to_n: 9.80 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 8.110 targname: B20827+24 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 23S priority: 1 req_1: ONBOARD ACQ FOR 8.12; req_2: GROUP 8.11-8.12 NO GAP; req_3: CYCLE 4; req_4: AT 3-DEC-1994 +/- 4D ! linenum: 8.120 targname: B20827+24 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 7.95M s_to_n: 9.71 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 9.110 targname: 4C29-45 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 32S priority: 1 req_1: ONBOARD ACQ FOR 9.12-9.14; req_2: GROUP 9.11-9.14 NO GAP; req_3: CYCLE 4 comment_1: See Tony Roman for scheduling table ! linenum: 9.120 targname: 4C29-45 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 22.45M s_to_n: 9.54 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 9.130 targname: 4C29-45 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 12.16M s_to_n: 9.53 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 9.140 targname: 4C29-45 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G400H wavelength: 4000 num_exp: 1 time_per_exp: 12.66M s_to_n: 9.53 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 10.110 targname: MC1118+12 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 32S priority: 1 req_1: ONBOARD ACQ FOR 10.12-10.14; req_2: GROUP 10.11-10.14 NO GAP; req_3: CYCLE 4; req_4: AT 23-FEB-1995 +/- 73D; ! linenum: 10.120 targname: MC1118+12 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 26.16M s_to_n: 9.71 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 10.130 targname: MC1118+12 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 16.5M s_to_n: 9.71 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 10.140 targname: MC1118+12 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G400H wavelength: 4000 num_exp: 1 time_per_exp: 13.35M s_to_n: 9.71 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 11.110 targname: B21351+31 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 31S priority: 1 req_1: ONBOARD ACQ FOR 11.12; req_2: GROUP 11.11-11.12 NO GAP; req_3: CYCLE 4; comment_1: See Tony Roman for scheduling table ! linenum: 11.120 targname: B21351+31 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 14.6M s_to_n: 9.71 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 12.110 targname: 4C40-24 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 20S priority: 1 req_1: ONBOARD ACQ FOR 12.12; req_2: GROUP 12.11-12.12 NO GAP; req_3: CYCLE 4; comment_1: See Tony Roman for scheduling table ! linenum: 12.120 targname: 4C40-24 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 8.98M s_to_n: 9.71 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 13.110 targname: MC0042+101 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 20S priority: 1 req_1: ONBOARD ACQ FOR 13.12-13.13; req_2: GROUP 13.11-13.13 NO GAP; req_3: CYCLE 4 comment_1: See Tony Roman for scheduling table ! linenum: 13.120 targname: MC0042+101 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 37.1M s_to_n: 9.44 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 13.130 targname: MC0042+101 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 16.3M s_to_n: 9.44 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 14.110 targname: S51803+78 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 18S priority: 1 req_1: ONBOARD ACQ FOR 14.12-14.14; req_2: GROUP 14.11-14.14 NO GAP; req_3: CYCLE 4 comment_1: See Tony Roman for scheduling table ! linenum: 14.120 targname: S51803+78 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 11.47M s_to_n: 9.72 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 14.130 targname: S51803+78 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 7.68M s_to_n: 9.72 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 14.140 targname: S51803+78 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G400H wavelength: 4000 num_exp: 1 time_per_exp: 5.71M s_to_n: 9.72 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 15.110 targname: PKS0214+10 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 6S priority: 1 req_1: ONBOARD ACQ FOR 15.12-15.13; req_2: GROUP 15.11-15.13 NO GAP; req_3: CYCLE 4; req_4: AT 7-NOV-1994 +/- 84D; comment_1: BLUE SIDE ACQ BIN- EXP=14 ! linenum: 15.120 targname: PKS0214+10 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 2.65M !5.39M s_to_n: 9.71 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 15.130 targname: PKS0214+10 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 19.7M !46.6M s_to_n: 9.71 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 17.110 targname: PKS1055+20 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 16S priority: 1 req_1: ONBOARD ACQ FOR 17.12-17.13; req_2: GROUP 17.11-17.13 NO GAP; req_3: CYCLE 4 comment_1: See Tony Roman for scheduling table ! linenum: 17.120 targname: PKS1055+20 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 7.57M s_to_n: 9.71 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! ! linenum: 17.130 ! targname: PKS1055+20 ! config: FOS/RD ! opmode: ACCUM ! aperture: 4.3 ! sp_element: G400H ! wavelength: 4000 ! num_exp: 1 ! time_per_exp: 6.36M ! s_to_n: 9.71 ! fluxnum_1: 1 ! priority: 1 ! req_1: CYCLE 4 ! linenum: 17.130 targname: PKS1055+20 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G400H wavelength: 4000 num_exp: 1 time_per_exp: 5.72M s_to_n: 9.71 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 18.110 targname: TEX1156+213 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 20S priority: 1 req_1: ONBOARD ACQ FOR 18.12-18.13; req_2: GROUP 18.11-18.13 NO GAP; req_3: CYCLE 4; req_4: AT 1-MAR-1995 +/- 89D; comment_1: BLUE SIDE ACQ BIN- EXP=46S ! linenum: 18.120 targname: TEX1156+213 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 8.00M s_to_n: 9.72 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 18.130 targname: TEX1156+213 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 76.6M s_to_n: 9.58 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 19.110 targname: 4C64-15 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 18S priority: 1 req_1: ONBOARD ACQ FOR 19.12; req_2: GROUP 19.11-19.12 NO GAP; req_3: CYCLE 4; req_4: AT 1-MAR-1995 +/- 89D; ! linenum: 19.120 targname: 4C64-15 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 8.63M s_to_n: 9.72 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 21.110 targname: 4C73-18 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 12S priority: 1 req_1: ONBOARD ACQ FOR 21.12-21.14; req_2: GROUP 21.11-21.14 NO GAP; req_3: CYCLE 4; comment_1: See Tony Roman for scheduling table comment_2: BLUE SIDE ACQ BIN- EXP=28S ! linenum: 21.120 targname: 4C73-18 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 4.31M s_to_n: 9.72 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 21.130 targname: 4C73-18 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 48.3M s_to_n: 9.38 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! linenum: 21.140 targname: 4C73-18 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 48.3M s_to_n: 9.38 fluxnum_1: 1 priority: 1 req_1: CYCLE 4 ! ! end of exposure logsheet ! End of RPSS template