1995ApJS...97..285K THE © 1995. 9 24 23 22 21 20 4 8 6 3 7 5 2 14 10 1 19 18 16 13 12 17 15 11 Sterrekundig Space Center Observatoire ISO Department Department Present Astronomy ASTROPHYSICAL Computer European ESA/UEObservatory, Postal Department Department Department Universidad Universities Nuflield Space Sternberg School Harvard-Smithsonian Dominion STEPS The K. Observatory, A. American T. Telescope B. Sciences for address: D. address: P. of Radio M. KORISTA, © Physics Astrdphysics Astronomical J. KORATKAR, Space TOWARD Sciences Astrophysical Program, K. K. of of M. Space de Instituut, of of of Nacional PETERSON, AXON, Astronomical American C. Physics Astronomy, Lowell Laboratory, Astronomy, Astronomy, Astrophysics, Astronomy Paris, Department Science N. Agency, J.P. Astrophysics BOISSON, JOURNAL and G. Research CHUVAEV, Corporation, ENGLAND, 1 Computer M. 17 URA • Astronomy 2 Observatory, and Center University Autonoma T. HUCHRA, and • P.O. Society. D. 18 Institute, Institute, Space Observatory, DETERMINATION MAcALPINE, I MATHESON, H. E. 13 Astronomy, IN University G. Laboratories, ALLOIN, SUPPLEMENT G. Space University New Ohio 173 Box Association, of 3 G. Astronomical Oxford BENITEZ, for R. All M. Division A. Physics C. ACTIVE Telescope CNRS, Sciences 26 A. 50727, Mexico rights Astrophysics, NASA 23 State MILLER, of 3700 University Science, de and KRISS, CARINI, PEROLA, 20 M. M. B. Mars REICHERT, Utrecht, Mexico, University, A. X. reserved. 3 I. of Wise of 5071 DIETRICH, c. and University, R. San Johns P. 92195 ofESA, M. AND S. 28080 PRONIK, Goddard M.A. California, I. J. Corporation, J.M. 30 W. State University 19 California NASA SERIES, 34 Hill Science D. RECONDO-GONZALEZ, 8 C-011, BARR, ESPEY, SHAPOVALOVA, TOKARZ, Astronomy, JIANG, Martin B. P. Received GALACTIC Observatory, SANTOS-LLEO, J. 37 J. 23 West Printed of P.O. ROMANISHIN, 40 Instituto Hopkins R. R. Road, Meudon, University, R. M. McCOLLUM, BERLIND, H. w. 60 Madrid, Moscow, SHULL, ESTEC, J. J. GROUND-BASED Goddard Keble SKILLMAN, S. E. 97:285-330, 14 University Saanich Space Garden Box Institute, CARRILLO, Society L. KROLIK, 4 SNUDERS, G. in 26 MAcKENTY, 17 Drive, R. 8 32 S. at Math-Science 27 J. OF P. ofManchester, VEILLEUX, STONER, A. U.S.A. 1400 T. 4 1994 PERSAUD, V. • S. Berkeley, Berkeley, Berkeley, 28 B. NASA J. PASTORIZA, 80000, de CLAVEL, J. 20 West University, Road, M. University Spain. France. V. Flight Postbus WANG, 51 J. I. WEYMANN, Universitetskij KASPI, THE Tel-Aviv WAGNER, Z. C. J. Astronomia, Baltimore, Space West, Street, Box Road, Victoria, 20 September N. RoDR.iGUEZ-PASCUAL, PRONIK, J. FILIPPENKO, 3700 NUCLEI. WILKES, I. WINGE, 18th of R. 8 Goddard 3 Oxford NL-3508 47 AND DOKTER, 44 23 Center, M.A. 1995 A. • 3000 TSVETANOV, 55 54 42 K. California 19 Flagstaff, Flight J.C. BERTRAM, SIZE 299, A. Cambridge, San N. 4 L. 25 H. 49 A II Provided W.-H. 41 T. SILBERMANN, Building, Baltimore, University, of 1 R. SEKIGUCHI, venue, • Macclesfield, z. 60 W. April I, W. C. Yu. J. S. MERKULOV~ 38 MD A. Kentucky, OX Martin E. 28 2200-AG, 8; 285 26 15 Department MALKAN, D. 13,38 SHIELDS, Code 20 R. Apartado Center, Space PETERsf L. SADUN, TA, 63 D. SPARKE, 1. accepted AND prosp. KOLLATSCHNY, F. J. R. SMITH, CARONE, STUDY B. VIII. I 29 21218. AZ CA F. SUN, at COHEN, M. R. BC, Zou Columbus, WANDERS, 3RH, 3 M. PELAT, H. WELSH, ° Los L. Utrecht, V. 684.9, J. San MALKov, Drive, Flight MA C. J. MD 86001. 13 94720. WAGNER, Tel Canada Code 8 Wu, WILLS, RODRIGUEZ-ESPINOSA, PTAK, 13, • DoROSHENKO, The 32 21 Angeles, STRUCTURE 57 WHITE, D. Lexington, by AN Postal Diego, M. England, 45 Cheshire, 46 1994 52 13 02138. 56 0 Aviv 21218. 9 Moscow J. U. 4500, Greenbelt, 52 • 1. Center, R. 5 Baltimore, A. S. 3 24 48 s. s. 668, Netherlands. G. OF 32 1J. The GASKELL, the H. 1 D. M. 26 • SALAMANCA, OH • INTENSIVE THIELE, 49 F.-Z. September G. V8X 13 42 L. M. TURNSHEK, PITTS, 15 70-264, 69978, 64 9500 61 PENFOLD, M. L. • BLACKWELL, C. CA 62 Las M. 26 Greenbelt, Netherlands. L. W. L. 13 • NGC MORRIS, 43210. SERGEEV, UK. 13 13 NASA SMITH, SKI 27 Code V-234, • METIK, D. KY 9 4M6. STIRPE, • SHRADER, RAWLEY, 21 SITKO, 90024. Cruces, CHENG, CRENSHAW, Gillman w A. MD Israel. 23 MD MAoz, 04510 I 40506; 58 AMSTEKER, 29 9DL, 681, LAOR, R. 28 5548 22 20771. Russia. OF 21218. M. • 13 MD 39 26 26 Astrophysics W. NM 10 53 36 59 Mexico Greenbelt, 3 Drive, 26 HST, D. 25 England, M. [email protected]. M. H. R. II 23 THE 5 20771. JR., POGGE, 33 J. 88003. o P. DULTZIN-HACYAN, PEREZ, NETZER, GoAD, 43 MIGNOLI, 6 J.-P. A. La G. 1. 6 D.F., 15 JUE, CHRISTENSEN, N. BROAD-LINE N. Jolla, UK. MARTIN, K. MD LUMINET, 13 G. EVANS, 31 Mexico. 23 s. CA 20771. L. II BOCHKAREV, J. 36 P. Data C. 92093-0111. ANDERSON, T. 35 Ho, 1 K. 3 O'BRIEN, System 1 HORNE, 30 19 REGION 22 16 12 1 • 7 1995ApJS...97..285K 286 C080309. ematics, Porto 60 59 58 56 55 53 5 64 63 62 61 54 52 57 27 28 51 39 38 36 35 34 33 32 31 30 37 29 26 25 49 48 47 46 45 43 42 41 44 40 ° Observatories Center Computer Institute IRAM, Department Joint Max-Planck-Institut Astronomiska Osservatorio Canadian Crimean Center Department Department Department Department Department Departamento Department Department Department Department Department Department Landesstemwarte, McDonald Kitt Beijing Universitiits-Stemwarte Steward Special South Institute Istituto Instituto Hubble Department Department Department Alegre, Physics, Peak Institute ( timescale tude the highest slightly contribution this the satellite-based and optical campaign monitoring nearly with higher beginning 1350 African for for l) Astronomical 300 Astrophysical Astronomico Fellow. Observatory, RS, During of We of © de Astrophysical National Institute basis Basement that period Astrophysics, Sciences corrected program. Observatory Astronomy, Astronomy, Madingley Rue the of Astrofisica and A of of of of of of of of of of of of American Brazil. of of of Astronomico present a of temporal Observatoriet, for Astronomical spectra ionization de smaller continuum Physics Physics Physics Astronomy, Astronomy, Astronomy, Astronomy, Physics Physics, Physics Physics, variability Physics Physics Physics Physics factor the de Engineering, HST the of variability Astronomia, the Laboratory on on Konigstuhl, for Observatory, 1992 la Corporation, simple Carnegie of fiir Astrophysics, ultraviolet Observatory, dell'Universita, we Piscine, Observatory, the University 1993 Theoretical HST for We and and and and and and the Faint de and and and Observatory, program. this Keele M.L. of2. and National Gottingen, and than Astronomie, University resolution October-1993 describe Canarias, Seyfert di various Astronomy, Astronomy, Astronomy, Astronomy, Astronomy, Astronomy, describe Caltech lines University University University Astronomy Astronomy, Astronomy, data is March Department time-series Astronomical galaxy 77 Observatory, portion and Bologna, Box 11, Institution Mount In University, Astrophysics 38046 the Object at larger Instituto D-69117 photometric National University other GRO Central of shorter and observed, 515, and the Astrophysics, UV 9517 Chinese These Road, Geismarlandstrasse Russian of l Arizona, 130-33, anomalies. E-38200 the Saint P 14. Royal Konigstuhl, in galaxy via Science in and at /0 S- of of via 5100 of of Science Spectrograph initial optical continuum and de Georgia Michigan University University University wave University Bowling University Washington Heidelberg, 751 acquisition of 1988-1989. During Lancisi of University, California Wisconsin, Michigan, detail shorter Keele Nauchny, Cambridge the analysis Optical Zamboni P.O. Martin wavelengths. Fisica, data and Washington, higher Academy September, College, Astronomy, Bradley Pasadena, Academy of 20 Tucson, La A He NGC and Cincinnati, monitoring bands, Support results Box observations National ST5 Uppsala, continuum University Laguna, State continuum various 29, Green constitute Universidade D-69117 II Society Astronomy State d'Heres, the Technology, wavelengths, College of of of of signal-to-noise 9, at Dennison Observatory, of 33, Calgary, A. 334413 Germany. 1-00161 5BG, Chung-Li, 475 5 Avenue, variations Pittsburgh, Pittsburgh, Nebraska, of CB3 AZ Oklahoma, Calgary, University, 1640 of last Observatory Berkeley, Berkeley, Berkeley, CA 548 and the the from University, JUE Center, (FOS) 11, 1-40126, State Sciences, University Science, 813 Tenerife, North Institute Sweden. 85721. although 400 Staffordshire, 91125. photometric OHA, The London, France. Heidelberg, 39 D-37083 of that UV continuum reduction and Crimea, KORISTA campaign, Rome, Santa Canada University, a spectra Observatories, Toronto, Toronto, Laurel, amounting a Building, days Geology • 2500 variations Federal {both Hefei, NASA Taiwan Charter fifth broad on Lincoln, combined Bologna, ABSTRACT was and England, Nizhny N v N Provided Atlanta, Agnes Norman, Zhongguancun, and of Spain. and Barbara 7935, East of a Gower Italy. University of Gottingen, Ukraine. Standards T3E many ratios MD year Texas, undertaken Anhui, optical daily Goddard CCD A. with Germany. were /Physics do this emission 32054, Street, Lansing, the Ann England, Scott 1240, of Bowling NE Arkhyz, South shows CA the problems Italy. 6K6. GA Rio 20723. UK. ET Street, OK are of Street, all to campaign, PA continuum P.O. a than basis. RLM of Arbor, 68588. HST/ imaging obtained People's College, 94720. Grande 30303. intensive small 1350 continuum less Madison, Republic of Drive lag and 73019. Germany. Africa. AL. virtually by the Space Building, 15260. ON, MI nearly Green, Box UK. Stavropolsky Beijing, London the Pasadena, were lines 15.308, behind than Technology, Ground-based in MI JUE/ground-based data the 48824. A NW, time Canada with 26732, do Republic Decatur, Flight satellite order and 48109. continuum of once WI spectroscopic also obtained OH Sul, identical about Cincinnati, optical People's NASA are light curves WC Calgary, Austin, simultaneous, China. delay the the 53706. aperture Center, and CA 43403. Tucson, Avenida M5S to vary concentrated IE every Kraj, GA of FOS continuum and 9110 University address l 6BT, emission-line China. relative TX Republic monitoring day; IA Canada 30030. in in Astrophysics behavior, Code 357140, OH observations, ground-based flux I. AZ I. Bento and 2 78712. our photometry), flux, England, days ( observations appear 45221. 85726. 2) 668.1, questions is explain to previous AB of with spectroscopic of Gom;alves, with that Russia. found variations Colorado, the China. for around T2N except UK. Greenbelt, of to any light curves, the UV a amplitudes this IN4; how show period to consisting that multiwavelength data variations lag continuum. are 9500, were Data that the have Campus galaxy. and by we require between MD more reported obtained monitoring time of the CPI somewhat also Department identified varied System 20771. that 7 4 we Box ampli­ 5051, In of short­ of in made both days find this 165 the On the the are 440, for by in CEP of Boulder, Vol. 91500, Math- 97 1995ApJS...97..285K line integral the tions AGN the transfer termination solved sary fundamental erable discussion), McKee BLR BLR. variations the tion noise travel where tion some scales. effectively erated ized BLR C(t) rect metrical region. the over region rate ravel No. 1991, The At High photon light-travel International 2, stages calculations, profile, from usual to BLR with extended gas means is any time the ratio, time as once This hereafter attention (BLR) at bright for '11'( By 1995 the Thus, break and 1982). function temporal in determmations. Subject radial with~ emission-line on core. distribution "h~d~r" some less results a r) structure a measuring position in using the gas and tis number convolution from providing phase extra assumptions every transfer temporal © function this solve yielding is the the of importance, of than Seyfert determination the in the continuum responds The periods comparing American determined previous A iomzation time the time Paper L(t) in on light continuum emission-line .sa~e active mapping the headings: dimension solutions, response one space. spectroscopic 4 for 2 near-degeneracy ~ Ultraviolet these frequency density optical within the and days function days; responsivity-weighted continuum across lag it. 1 the = curves a resolution, I. '11'( is of of spatial galaxy. I). has galaxy C galactic gets wings 1: two-dimensional of able INTRODUCTION physical to time efforts. of r). for IV response the as radius. and We (see The the stratification the source the observations incident proved to the around galaxies: galaxies: the bri~ter by velocity the '1F(r)C(t- they are allowing variability The Astronomical at to of an '11'( provides the line-emitting (I t ( confirm results NGC observed monitoring However, resolution Explorer light BLR, the optical 3) - different infer nuclei the variations Peterson ~v BLR BLR data Beginning r 8 source and ionizing transfer conditions ), r, Such that with month to for I line 2 responsivity-weighted on i.e., in where ~nd curve 5548 active ~ photometry field the the weeks, set from be the for duration and (AGNs). emissivity lines the the the 3000 spectral two some is a to response of continuum r)dr, show measurements a ( only of run velocities (JUE) the a required emission-line are delay 2) function period map continuum line-emitting that has powerful velocity the L(t) on a 1993 in model - r information in less sufficient of distribution BROAD-LINE trends of gas broad-line that about km is of preliminary lags of way one-dimensional the that 1988 galaxies: received geometry different Seyfert microarcsecond position. Society set to physical ambiguous '11'( variability determined over The the (Blandford s observed th~ for provides - ( energy measured photoioniza­ -i) sample to distribution, Clavel to by v, the reported v field twice can December, way light galaxies: broad-line highe~t across photoion­ determine invert the signal-to­ r) respond the a flux variations galaxies individual gas. consid­ region also of ioniza­ flux Under are condi­ of of neces­ recent to of the entire curve input light­ et and • wide the a di­ gen­ geo­ was this un­ the the the the (1) de­ the earlier, al. REGION ionization be Provided by for lag of & at Seyfert C quite to that Lya, for IV-emitting continuum in (NGC spans Lya the uncertain, namely, - the within straints front also object. ization with servations, continuum ground-based Blackwell the temporal high-ionization higher ( 4 quired experiments, continuum These the neous scope monitoring through undertaken and of et lyzed Welsh, respectively). results, Seyfert "small strongest (Peterson continuum Papers monitored C emission IN 3. 2. In broad Peterson 1. al. IV, days) ultraviolet: NGC and velocity by original over variations 5548) investigated lead § Clavel What What within Is (HST) AGNs. the 1994 and are can a 2 velocities The additional region blue C ( the & lines 1 variations there II-IV, on Maoz few we 1992 H{j an 1) but galaxy to 5548 sampling but UV optical IV, the ( Peterson et provide H{j - and 1990) lines that and is emission. results variations? is emission. order ( the JUE outline field a campaigns to a NASA ( line light bump," higher al. with as 1993) important indicates there monitoring following: 1991 the a galaxies: lines few October. direct the VIII. galaxies is Peterson are and in address et over in respectively). in phase lines? Stirpe 1991, the NGC origin not have flux the close and provides continuum velocity arguing days the of light response al. data; each our § 4 slightly from ) a are than and ultraviolet ( a signal-to-noise the reviewed UV/ dominated arguing fundamental magnitude determination one-dimensional the 1991 follow Astrophysics a ground-based different the (1993) The More the difference 3783 previous 1992 et some of to nuclei- days concurrent The that three of H{j. blend slightly et HST of in new the was 4 optical al. the shortest campaign the for }, field fifth al. more some the NGC this rapid year establishment was time and original By the of recently, and there achieved weak questions 1994, for central gravitational ( and key observations, central in analyzed of 1994, the Krolik BLR year JUE wave of particular combining smaller monitoring continuum by range similarly rapidly period Dietrich of variability Ferland random continuum detail 5548. between ultraviolet of lags, unanswered the H{j constraint indications continuum is radial hereafter ratios the ofNGC of of campaigns campaign the ground-based and hereafter source, and a bands the source BLR? emission-line in in transfer Data the the arose thus et strongest He+ As the than from than the the most radius. southern motion. as et monitored Hubble et cloud case physical al. oflimits the ground-based infall. mass in the in indicating results of variations campaign -He++ al. original well. al. are Determination and whose 5548 Fe variability Papers and becomes for previous does System many ( that 1988 UV § Paper source. the rapidly functions are questions UV not ( 1991 1993, of 11 3 truly 1992) motions of models indeed possible An Crenshaw The the was Space and highest ambiguous, 1988-1989. the the hemisphere and on of and answers only the conditions ionization December V variability ), successful campaign campaign (Reichert VII) intensive hereafter JUE simulta­ the whether recently and varying derived Balmer central Horne, optical optical of might of better of cam- from Tele­ with con­ ana­ ion­ past ob­ the VI, 287 the the re­ of & 1995ApJS...97..285K JD last exposure minimize nuclear centerings one cause roll, briefly paign, (PSF) effects aperture the Gaussian, 0':175 Digicon the separated The trograph April 288 terized § paign, sets ried 6. FIG. Using 2,449 4''.3 effective stage in We whereas and mode out. of 19 the of due in 1.-G130H each during (but ,097. square and summarize a sources diodes through the (FOS admits their the of in later We malfunction by photometric position falling of to © of the 1295 of aperture the note blue-side approximately the PSF the spherical describe which the measurements American aperture, sections. ), the project peak-up; the original cross-correlation NGC of 2.1. (solid 1993 2. wings s object off that target-centering two angle occurred our THE light. broad the steeply for The detector May " of line) z the ·a Oi VJ 5548 p, Q) ... >< to uncertainties functioning aberration the results All on using (P.A.) HST on proposal the in these HST/FOS 1 30 35 20 40 25 FOS On intercalibration 10 15 wings the and ':4 5 observations 0 27, error 24 Astronomical the the was in solar at in§ a perpendicular and in hr. spectrophotometry G190H 26 1200 data a of the of three-stage other Observations larger diode observed total § of the the distribution arrays called The 5. functions in JUE visits, 7. same error SPECTRA fine is the due The variability the telescope HST (dotted of39 13 4''.3 nucleus array miscenterings). observations point guidance just for visits, orbit distribution used primary to the every X 1 X "peak-up" of separate Faint 1400 a any line) to will prior are constant the Society G spread two ~4. (second) was is the was the day 190H possible signal-to-noise calculated be Object Such various highly sensors. mirror. to guide due centered three-stage dispersion, allowed from visits discussed is this were function is routine. grating P.A. to charac­ KORISTA As a as about • Spec­ stars, Observed 1600 cam­ non­ large 1993 non­ each mis­ data The car­ Be­ the the Provided to to in in ratio Wavelength per ET with seven G gives the to be paign features of ciencies object quisition electrons, The in The time ratios peak-up G array one-quarter the with and diodes, tion (Junkkarinen on-board geomagnetically pixel 1800 190H 190H The 259 the map read by AL. signal-to-noise response perpendicular dispersed G was of323.75 the an a as of as for first during separate FOS 130H the s log the out. a the exposure observations drop are duration, overscan 2064 (A) was performed a (re-centering function previous GIMP which both of and result photocathode detector NASA standard of The the grating of the the near 2000 completed et photons pixels, the s last each gratings. 250 result forthe al. electron correction are of FOS lowest occurring of induced total while of ratio one the to wavelength 20 1991; is in Astrophysics the exposure diode s then accelerated consisted five exposure each the a observations. of pixels readouts. ends upon real strike integration G190H after per Digicon, observed the overscanning the The trajectories Fitch entirely diode surface diodes and 2200 pixel image-motion time pixel after was of G guide bad have correcting for a square-bottomed of 130H spectra to of photocathode et technique and437.5 array. done the a on having with for Each was 17 diodes onto overall al. minimize five reacquisition diminishing in stars) time first 50 board Columns the observations are 1993). Data the used. a in onto separate as In technique; s the readout day linear full in for followed an directions in magnetically in flux well. order first s of each Digicon the in the problem the the array. forthe effective This integration the GIMP the System the quarter-stepping level 512 which ( spacecraft. Figure third orbit readouts, signal-to-noise diode 1)-(8) to effects case. in was FOS effects "absorption" produces after consisted diode grating oversample of the G130H, compensa­ both array. orbit. campaign, produces exposure summed The with the (GIMP) array Table focused 1 second. of are a on of shows array. along cam­ reac­ dead each data The The effi­ the the the the an to or of 1 1995ApJS...97..285K © American Astronomical FOS Day Campaign Number (1) 39 39 38 38 37 37 36 36 26 25 25 23 35 35 34 34 33 33 32 32 31 30 24 24 26 23 22 22 21 21 20 31 30 07 06 06 04 03 03 02 02 01 01 29 29 28 28 27 27 20 19 19 18 18 17 17 16 15 09 08 08 07 05 05 04 09 16 15 14 14 13 12 10 13 12 10 11 11 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 Society Date LoG 2 (3) (2) May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May May Apr Apr Apr Apr Apr Apr Apr Apr Apr Apr Apr Apr Apr Apr Apr Apr Apr Apr Apr Apr Apr Apr Apr Apr UT OF 20 27 26 25 25 24 24 23 23 22 22 20 21 21 19 19 30 30 25 24 23 24 23 20 22 22 26 29 29 28 27 27 27 26 25 21 21 28 26 13 14 14 13 08 07 09 09 06 06 05 05 04 04 03 03 02 02 07 20 19 19 17 16 16 15 18 17 12 12 10 10 11 11 08 18 15 01 01 FOS 09:53:54 06:52:32 10:15:07 15:00:06 13:39:15 11:36:00 08:33:03 09:57:54 05:31:39 09:34:06 09:27:52 11:24:34 10:03:42 11:07:02 11:18:46 12:18:49 10:48:46 12:49:20 11:28:27 12:05:50 10:31:39 11:59:06 10:24:54 11 09:40:09 08:27:49 09:46:10 12:54:38 11:01:04 10:54:59 13:01:17 12:12:24 11:52:16 10:57:54 10:38:11 10:18:05 11:45:24 10:11:11 11:31:38 10:10:42 11:27:06 12:48:06 11:27:11 12:41:42 11:20:49 12:35:27 11:14:34 12:29:19 13:59:44 12:25:36 13:13:18 11:40:59 12:56:06 11:35:14 14:26:42 10:02:01 11:20:26 12:52:34 12:44:28 11:23:36 12:20:21 12:17:22 10:44:48 13:36:16 12:02:08 11:56:23 13:24:47 12:03:55 14:55:25 13:21:17 11:52:27 13:07:35 11:46:45 13:01:50 13:30:32 10:56:30 12:05:40 10:50:37 • Time :08:27 Provided SPECTROSCOPIC TABLE Julian (2440000+) 9118.99 9135.12 9135.07 9133.79 9133.73 9132.98 9132.93 9131.91 9131.85 9122.00 9121.93 9121.00 9120.93 9110.08 9110.02 9116.04 9115.04 9114.97 9114.03 9113.97 9113.03 9112.97 9112.02 9111.96 9111.02 9110.96 9130.97 9130.92 9129.97 9129.91 9129.03 9128.98 9127.96 9127.90 9126.96 9126.90 9125.95 9125.89 9124.95 9124.89 9124.01 9123.95 9122.94 9119.99 9119.93 9118.92 9117.91 9117.85 9116.98 9116.92 9099.04 9098.10 9098.04 9115.97 9123.00 9104.05 9103.12 9103.05 9102.05 9101.99 9101.04 9100.99 9100.04 9099.98 9098.98 9097.03 9096.97 9109.01 9107.95 9106.95 9106.06 9106.00 9105.06 9105.00 9104.00 9108.95 9108.01 9107.00 (4) Date I by 0BSERV Grating Gl30H Gl30H Gl90H Gl30H G190H G190H Gl90H Gl30H Gl90H Gl30H Gl90H Gl30H Gl90H Gl30H Gl90H Gl90H Gl90H Gl90H Gl30H Gl90H Gl90H G130H G190H G190H G190H G190H Gl90H Gl30H Gl30H Gl90H Gl30H Gl30H Gl90H Gl30H Gl30H Gl90H G130H G190H Gl90H Gl30H Gl30H Gl30H Gl30H Gl30H Gl90H Gl30H Gl30H G190H G130H G190H G190H G130H G130H G130H G130H G190H G130H G190H G130H G190H Gl90H Gl90H G190H G190H Gl30H Gl30H Gl30H Gl30H Gl90H Gl30H Gl30H Gl90H G190H Gl30H Gl90H Gl30H Gl90H Gl30H the (5) NASA ATIONS P.A. 320 322 322 317 317 318 318 319 319 320 321 321 3Z3 323 324 324 325 325 325 325 325 325 325 325 334 334 334 334 334 334 334 334 334 334 335 340 344 359 325 325 335 337 337 338 338 339 339 340 342 342 343 343 344 350 346 346 347 347 348 348 350 351 351 353 353 354 354 356 356 357 357 359 (6) 2 4 0 0 2 4 Comments Astrophysics (7) u u u u u u u u D D D D u u D file n59099 n59099 n59098 n59098 n59097 n59097 n59118 n59117 n59115 n59114 n59114 n59113 n59113 n59112 n59111 n59102 n59101 n59101 n59100 n59100 n59135 n59135 n59134 n59134 n59133 n59133 n59132 n59132 n59131 n59131 n59130 n59130 n59129 n59129 n59128 n59128 n59127 n59126 n59125 n59124 n59124 n59123 n59122 n59122 n59121 n59121 n59120 n59120 n59119 n59119 n59118 n59117 n59116 n59116 n59115 n59112 n59111 n59110 n59110 n59105 n59103 n59103 n59102 n59127 n59126 n59125 n59123 n59109 n59107 n59107 n59106 n59106 n59105 n59104 n59104 n59109 n59108 n59108 IRAF (8) name Data System 1995ApJS...97..285K of POOPS present 290 wavelength Ne curred count the verted resulting nonuniformities Cerenkov overscan, counts netic rected pulses Processing day The single exposure, comment describe call night users HST start ment, absorption FIG. The spectra dependence was "dropouts" separation field campaign of in (also variations) rates and (negligible day for prediction STScl 2.-0bserved to during to all roughly in§ 2.2. the data an and nonlinearities the are radiation codes the G (epoch) obtained System count at scales by © contained 130H 2.3.3 absolute pipeline exposure, the grating computed The are defective passage root the American of between day on in (D) 80 FOS using exposures. in then are the FOS and and rates count appropriate column names [POOPS]) geomagnetic minutes. was from this number, during faceplate. and charged-particle-induced name, assigned reduction flux u 0:: +> +> over Appendix " Ill ;::l corrected 0 ~ then within Pipeline appropriate diodes. the rate in the case). based 0.03 0.04 0.02 0.01 by the charged "U-shape of the The scale 0 ( the the vs. Gl90H, the Astronomical 7) the subtracted. Julian correcting two f­ f- ~~~~-~'~~~~'~~~~-~'~~~~'~~~~~'~~~~~ the This based pixel Digicon upon dotted the Background These inverse begins indicate aperture South system Reduction Science spectra by for latitude grating D. UT particles zero-sensitivity number IRAF multiplying anomaly" flat Date The small-scale a line upon followed date, count Atlantic model by sensitivity detectors (Post for FOS shows fields, position for ·-·- Verification No first lf exposures 50 and first FITS for a G at the in Procedure background the reference count rates quarter-stepping, ------that problems observations exposure Operations the the the longitude template Society converting by (U), UT Anomaly. and region photocathode 130H header). the due adopted angle, Earth's are accounts the start curves. rates time in then --- which corrected then to by thus observation. phase level. 100 Gl30H. a in we KO a paired due Pt-Cr­ of future background (day/ single at ---· mag­ com­ Data • allows con­ each The The cor­ The raw will The oc­ RIST the the for we Provided of to Pixel large ,_ for ~··· The A -- a 150 level. difference ET Number direct does first pixel --- ground toward the the was sensitivity above about exists length direct count cause internal tions which plate, measurement pixel HST are and In Because ·-· AL. -180 phenomenon by essentially observed cubic checked measurement practice number. of not -200. for operations. the the the rate photons calibration, 1130 we the between the is ·- various accuracy pixels receive the detector first POOPS will ·-·-·-·- arise very terms. in to of shorter 200 A. NASA G l The for absorption the count the first-order 45 discuss of 2.3. linear the It (from important 90H 2.3.1. simply magnitudes of all or For first the is which error The POOPS required predicted model sensitivity and wavelengths. the in The Modified so rate G l no spectra. Astrophysics with background both - in NGC background this G l Background diodes flux counts in 30H from is 250 180 turn: in photons in particle 90H the present in pipeline and small gratings, region for calibration. ~Jl]llll the the 5548) were pixels An observations the with from in background observed an this background and FOS zero-sensitivity Figure a G l a accurate coefficients level. case background made that FOS inaccurate first-order of for this count Subtraction project, were is proved G l wavelength magnesium wavelength 300 very 30H all - The of background Data grating one 30H Pipeline 2 shows in G l being the rate; estimate dot-dash nearly spectrum three to estimate, direct may and inadequate subtraction, 30H wavelength G l for System confirm charged-particle prediction. declines no detected thus an region increases 30H make light areas, the observations: count fluoride shorter flat, line such of example on modifica­ have quadratic the however, data, shows and rates a that each rapidly account Vol. lies for region below wave­ direct scales back­ face­ than This with zero this was the be­ the far no 97 of of 1995ApJS...97..285K dividual those the tracting tra spectrum steps. and are each correlated The this the major the wavelength peaksofHe11 spans spectra estimate G130H ofLya G correlating calibration, ing ground gratings ground length known tered-light tions backgrounds became plained probable few offset dicted in +28°4211, Kinney measuring ties trum. background see from lows. region, pixels region, ±4.4%, No. 130H The The The the were shifts the Appendix G expected detector about procedure cross-correlations in 2, spectra 2.3.3. grating near-ultraviolet were 130H The First, spectra amplitude roughly image between particle This background 1995 spectra alignments + N v N + the calibrated is (see to based spectra absolute fits rate below) significantly to & are shifted spectra 2.3.2. excess the were was derived 0.36 with mean have applied The the Bohlin the contribution the the amplitude BD to and © Appendix justified. which mean which or to model; sensitivity is misplacement were uncertainty from +Orn] and formed, A. which 28-128, their upon a the background spectra in upon G190H individual American A the FOS their background correct . The (see scaling background the single G to been +75°325, count We of As were for detail from ultraviolet C 190H, respectively. wavelength ranges applied by (1993). same was the was the to filter-grating-wheel correction had continua. Intercalibration for we Flux Fig. counting measured IV the the respective sharper found did and and The assuming misplaced in A), were be pixel and then and particle nearest was for rate spectrum and a describe in five performed is in determined much G peaks 2). wavelength across the discussion Calibration not spectra Si optical ±0.5 1155-1605 in Appendix so G 190H the to the the flux BD in performed determined problems Since shape in that (about spectrophotometric This then III]+ shifted in counts vicinity 130H Astronomical this much in the suffer statistics. This the following G flux method of a process whole background, larger covera&e mean the background the the pixels. that +33°2642, was in portion data). 130H the G the is wavelengths in from for subtracting procedure zero-sensitivity C we of spectra Appendix 190H was to the 0.25 G of mean greater, over diode accordingly, III] of calibration from the the to B. of Galactic scales, strong and done every spectra, the 190H the described have pixel, shifts A bring The was grating, the on each employed correction the Shifts No done fortheG190Hgrating. a Given corrections nonrepeatability. for PODPS A and FOS the of Related FOS for data. scattered-light the spectrum relative one array, particle for background emission-line repeated. relative BROAD-LINE before the no further epoch. emission was each HZ grating spectra, ( no and and all PO and of iteratively 2-4 1574-2330 the ofthis spectra A, based aperture absorption the also a Spectra Society or and the way zero-sensitivity corrections the DPS-predicted below. done relative constant the standards scattered 44, in Problems particle of G reflecting a here two region G PODPS-pre­ pixels) suggested more background accuracy contributes. joining uncertainty wavelength We 130H around were most new spectra shifting for 130H after amplitude of uncertain­ upon and The the and after lines. by is gra!ings directly The the discuss (as correc­ in of wave­ as cross­ cross­ mean peaks of back­ back­ A shift­ spec­ cases since spec­ • were lines FOS scat­ only data WD sub­ light The two two BD We the the fol­ the the the ex­ for for for in­ REGION by Provided in of exposure dix less mated this tempt problems, dent. level, The tions trum the nated were photometric should stand spectrum. spacecraft, age a are light corrections made bottom smaller spectra spectrophotometry are Date, the tral the the which rate briefly NGC associated most the white "U-shape derivation These the tainty region peated 0501+527 photometric -1.4% U IN The In Fortunately, Several D. FOS, comparable by former G differences present obvious "tainted" uncertainty in brightness region blue-side readouts). magnitudes Figure joined for and curves. All 190H AGNs. 5548 out serious only although dwarf for by column to in "dropout" we differences to describe of be the panel (Bohlin levels. observations demonstrated which are or the to the interest bring its range each in anomaly," will fairly uncertainties their This treated of to for of spectra. by (=G191-B2B). project. 4a by and the are in NASA model where apparently Figure uncertainty 1 absolute 2.4. combination C accuracy those This this of spectra, of VIII. FOS reasons u the refer between ( we combinations state Figure of Problem all Problem corrections IV them next them the 7) due (-20), typically statistical G Figure occurred relatively effects, well of 1993a; these here. the separate and show absolute are The and of 130H of optical with their effect atmosphere In in have spectra 3 all Two "dropouts" to to for and the Table Astrophysics and and except understood to photometric addition, 10 i.e., in suspected 3, which of these Combined He as three We problems of 3. the a the three had the some and and Lindler gratings, respective 1 FOS 3 which a of of is in the combined been from was ( ( 1 ) Problem their error the well-centered at affected II, telescope errors 3) affected similar uncertain, were scale of flux a chose which were the result 1. the the Bohlin HST systematic their as problems the well function will thereof. range corrections about "subgroup the It photometric problems FOS present caution. subgroup other 7 8 identified. impact abrupt 2% three ofG191-B2B the shows majority bar calibration is made derived above were "U-shape & region of become to minimum G of FOS away in have photometric campaign. important spectra, five level 2 to NGC scale Bohlin signal-to-noise a for most 5%-10% et blue 130H G adopt mispointing, total assembly 1595 had problems few photometric 130H 4.5%. of more and Data the are al. G130H in 1 Spectrum upon are JD effects most been from of The 2 of day variations." wavelength. arises exposures of a side, calibration percent. 5548 in spectra counts clear (1990) all denoted "dropouts," and A, raw primary and In the 2,449,105, anomaly" -10% wavelength-depen­ problems uncertainty that 1994). scale. spectra effects plus strongly detail We to excursions this corrections affected over the System corrected The other (Bohlin Appendix in varied latter (OT based do light HST and spectra; 3. ( primarily (Nos. problems note § these the G discuss versus end data either at The The 5.1). effect not describe The two the with in The A), 190H ratio interest that in was (i.e., spectra curves problems, campaign scale that the from and observed the upon It in of affected. observa­ so 1 stars, an set. 1993b). Appen­ spectral internal level level spectra spectra ( see and within from on is Julian uncer­ a in by domi­ as 2) in either an easily levels C -1 these sepa­ spec­ these aver­ spec­ from were their D with over esti­ The one the the the the the the 291 the the for for we at­ re­ 3) or of of at % is a 1995ApJS...97..285K (LWP; campaign. tween thermore, to tic lent weak struction G multiplets, 1 1150-1980 pixel was wavelength on Gl30H the We the and, tra frame, the bars, 292 month The l30H NGC FIG. and a G were joining widths wavelength refer smoothed vs. log-log -i). as !JOH emission 1993 JUE other on 1950-3300 J.-Total Julian a 5548 plus "dropout" joined before result, of the The two counts the There ranging -20 © A) observations March this procedure. scale plot absorption G190H, Date reader are red or American combined lightly camera features, in there observed G fell where and mean weak 3.1. three also to were wing minus this appropriate A) drastically. over 14 J. highlight exposures to spanned is observed. by weighted The and camera THE spectrum. separate .. T Galactic Appendix the I manner; of u a 0 u ...., ...., ...... 0 observations 0 ::i ::i "' "' Q Q 0 >< x 2,440,000. a In roughly features resampling were total small many the spectra 190H JUE May G l 24 20 22 Figure 14 16 18 JUE Astronomical 2 4 8 6 C the 9095 the 9095 30H obtained observations, of counts were systems Observations ( IV mean Further for absorption 27. SPECTRA 0.08-0.6 of no -1 are The weak In 40 B entire which emission 4b _ which and G190H G130H scale These for addition % ) the deferred - both ... short-wavelength excluded subgroups, and (top we spectrum - ii 9100 9100 features. discontinuity more of once analyses -- G l duration Gl90H corresponded panel) factors A show 35 spectra absorption counts counts observations are 90H - line. - lines are all to long-wavelength to every details Society or probably from ·-··- and observed. 9105 of 9105 future the the The ofNGC All spectra were of separate with (0.36725 to of which GI the 2 numerous combined FOS the spectrum regarding the the in days intrinsic JOH applied, papers. equiva­ (SWP; Galac­ KORIST to began flux -·-- 9110 9110 linear exposures, meet. • HST were Fe 5548 spec­ con­ Fur­ counts be­ the Provided at A II . (bottom . - A 9115 9115 for . ET time the respectively. SWP epoch ing 2B. pared from of of enough was background an could level nucleus --­ sensor antisolar obtained taken the 50-200 in tions high been ofmiscentering: each view nearby the panel) by - optical AL. error large The exposure, put day's in ... =- fJ prevented present a 9120 9120 and were to in not the - telescope - the nearby (FES; angles was seconds, to in image of in the summed in apertures verify at direction). observation bright expected L cause an be light complicated NGC used fJ the WP NASA the to low-resolution since aperture. < the "locked" 9125 (i.e., 9125 SAO the number, aperture the that the direct 55°, curve stars. slow-track/ and observations for any tube Jongward SWP 5548 optical 1991 ( corresponding SWP and the star, tracking are the 10" comments Astrophysics problems However, Also, (Weinstein detection could - 9130 However, 9130 shown was 47421 to angle background by and UT actual X ··--­ which offset ofless of star and 20"). a the at geocoronal therefore overlap mode date, has during specific not individually. are this between tracker) L and presence slew with positions results than since are WP 9135 9135 become of Two be the • and presented level, & (5-8 Julian the LWP listed each the was obtained counts spectra 1 FES mode. Carini background the Lya, exposures acquired ". Data time in Seyfert were telescope detection the A A of accurate. particularly Note an exposure, of observations in 25305. coordinate Date, with star resolution) scattered of contribution the expected from columns in only This 1992), is System the the and nucleus, their in Tables negligible. star by failed 5 the The pointing the the beginning and was in days background Logs the blind and Poisson were which solar intense the FES ( 1 fine exposure position­ before observa­ tracking not through were 2A on nucleus because at so )-(6), of of range offset com­ which error each field light high error The that and and the the has all of at it 1995ApJS...97..285K spectrum spectrum. on FIG. the blue 4.-(a) of wing NGC © Combined of American 5548. the Lya The .. i :i: i i .. i :i: i i I .3 .... I i:: 0 .... i:: 0 " ... Ill Ill El CJ tlO tlO broad " ... Ill Ill "" El CJ Gl30H spectrum 0.4 0.6 0.8 1.2 1.4 1.6 30 35 20 40 25 10 15 5 0 Astronomical Society emission and 1200 is Gl90H plotted line. 3.1 Note the observed-frame in log 1400 FA many vs. 3.15 weak log Log spectrum Observed • X 1600 emission Observed to Provided highlight FIG.4a FIG.4b ofNGC 3.2 Wavelength and Wavelength the absorption 5548 for 5548 1800 by weak 3.25 the (A) emission JD features. (A) NASA 2,449,105, 2000 and ( b) 3.3 Astrophysics absorption Combined and its 2200 Poisson G l features 3.35 30H error Data and in bar. this G l Geocoronal 90H high System weighted-mean signal-to-noise Lya lies 1995ApJS...97..285K

TABLE 2A TABLE 2B LOG OF SWP SPECTROSCOPIC 0BSERV ATIONS LOG OF L WP SPECTROSCOPIC 0BSERVA TIONS

Image UT Julian Date Exposure Image UT Julian Date Exposure @ Number Date Time (2440000+) Time Comments Number Date Time (2440000+) Time Comments (1) (2) (3) (4) (5) (6) (1) (2) (3) (4) (5) (6) > SWP47274 1993 Mar 14 03:49:25 9060.64 7200 LWP25088 1993 Mar 14 05:54:32 9060.75 3600 a SWP47290 1993 Mar 16 12:59:32 9063.04 1680 very weak spectrum LWP25158 1993 Mar 20 13:24:13 9067.06 3000 ~ SWP47305 1993 Mar 18 12:14:15 9065.01 3600 LWP25174 1993 Mar 22 13:23:22 9069.06 3000 ""l ..... SWP47324 1993 Mar 20 12:00:13 9067.00 4800 LWP25191 1993 Mar 24 13:33:59 9071.07 3600 header exp. time incorrect ~ SWP47333 1993 Mar 22 11:59:52 9069.00 4800 LWP25207 1993 Mar 26 13:18:21 9073.05 3300 = SWP47349 1993 Mar 24 12:06:30 9071.00 4800 strange He II region LWP25223 1993 Mar 28 13:01:53 9075.04 3300 = SWP47364 1993 Mar 26 11:54:21 9073.00 4800 ion hit 1460-1472A LWP25263 1993 Apr 03 23:25:04 9081.48 3600 >[IJ SWP47380 1993 Mar 28 11:38:00 9074.98 4800 .... LWP25269 1993 Apr 05 03:03:03 9082.63 3600 label says LWP25270 ""l SWP47387 1993 Mar 30 15:44:08 9077.16 3600 very weak spectrum LWP25286 1993 Apr 07 06:08:53 9084.76 3300 Q SWP47402 1993 Apr 01 19:40:50 9079.32 4200 very weak spectrum LPW25305 1993 Apr 09 04:02:30 9086.67 3300 no signal Q SWP47414 1993 Apr 03 21:44:55 9081.41 5400 LWP25318 1993 Apr 11 04:37:59 9088.69 1320 weak = SWP47421 1993 Apr 05 02:24:11 9082.60 1920 no signal; miscentered LWP25337 1993 Apr 13 03:42:40 9090.65 3600 a..... SWP47422 1993 Apr 05 04:26:20 9082.68 6000 lines and continuum weak LWP25351 1993 Apr 15 11:51:20 9092.99 3600 ~ SWP47434 1993 Apr 07 07:11:13 9084.80 5700 LWP25358 1993 Apr 17 12:09:27 9095.01 3600 = SWP47448 1993 Apr 09 02:15:54 9086.59 6000 LWP25367 1993 Apr 19 11:46:05 9096.99 3600 00- SWP47459 1993 Apr 11 03:02:02 9088.63 5400 Q LWP25383 1993 Apr 21 11:41:02 9098.99 3600 ~ SWP47474 1993 Apr 13 01:58:13 9090.58 6000 LWP25399 1993 Apr 23 11:27:43 9100.98 3900 ..... 1993 Apr 15 10:23:12 ~ SWP47488 9092.93 4800 LWP25409 1993 Apr 25 11:45:33 9102.99 3900 .... SWP47496 1993 Apr 17 10:22:52 9094.93 4800 very weak spectrum '-< LWP25422 1993 Apr 27 11:20:00 9104.97 3900 SWP47505 1993 Apr 19 10:22:36 9096.93 4800 very weak spectrum LWP25440 1993 Apr 29 11:18:26 9106.97 3900 • SWP47517 1993 Apr 21 10:16:26 9098.93 4800 LWP25452 1993 May 01 09:51:43 9108.91 3900 ~ SWP47532 1993 Apr 23 09:59:36 9100.92 5100 LWP25464 1993 May 03 09:47:48 9110.91 3900 ""l SWP47544 1993 Apr 25 10:15:30 9102.93 5100 03:06:32 9112.63 3900 Q LWP25472 1993 May 05 SWP47557 1993 Apr 27 09:50:04 9104.91 5100 LWP25483 1993 May 07 04:07:31 9114.67 3900 <..... Q. SWP47568 1993 Apr 29 09:52:59 9106.91 4800 strange He II region LWP25496 1993 May 09 03:59:23 9116.67 3900 ~ SWP47577 1993 May 01 08:15:39 9108.84 5100 LWP25514 1993 May 10 23:53:06 9118.50 3600 Q. SWP47595 1993 May 03 08:11:12 9110.84 5100 LWP25522 1993 May 13 00:24:23 9120.52 3900 "r:::;' SWP47606 1993 May 05 01:27:32 9112.56 5400 LWP25531 1993 May 15 09:36:22 9122.90 3900 '-< SWP47618 1993 May 07 05:16:29 9114.72 5400 LWP25547 1993 May 17 09:40:43 9124.90 3900 SWP47629 1993 May 09 05:09:57 9116.72 6000 ~ LWP25556 1993 May 19 09:11:04 9126.88 3900 ~ SWP47641 1993 May 11 01:05:14 9118.55 6000 LWP25569 1993 May 20 23:38:33 9128.49 3900 SWP47660 1993 May 13 01:35:56 9120.57 5400 LWP25575 1993 May 21 07:47:57 9128.83 3900 z SWP47672 1993 May 15 08:06:34 9122.84 5100 LWP25585 1993 May 23 07:52:04 9130.83 3600 00> SWP47684 1993 May 17 08:11:38 9124.84 5100 LWP25595 1993 May 25 05:55:18 9132.75 3120 SWP47692 1993 May 19 07:41:57 9126.82 5100 weak emission lines LWP25607 1993 May 27 01:43:59 9134.57 3900 > SWP47704 1993 May 21 00:48:15 9128.53 6000 SWP47705 1993 May 21 08:55:50 9128.87 5100 ion hit 1420-1520A >[IJ .... SWP47716 1993 May 23 08:54:28 9130.87 5100 strange He II region ""l Q SWP47728 1993 May 25 04:18:24 9132.68 5400 SWP47743 1993 May 27 23:58:55 9134.50 6000 "O:r '-< [IJ..... ~ [IJ ~ ....= 00= '-<[IJ .... a~ 1995ApJS...97..285K spectra a affected. at cause lems 47402, to wavelength- parent SWP sometimes spectrum spectrum; extraction exposure of average length cases, is Horne the temperature various noise up processing, paper. by paign served sensitivity automatically extracted. extraction orators, dwarf cross-dispersion Archive trum tant hits that project pattern spectrograph et one rectified raw 1988-1989 campaign, 100 Cosmic-ray A a The linear. The al. compromise the Kinney, to specific hi&h resampling can intensity ways. this are combination 1993). 47290 to is A their 50% (see SWP model scale JUE LWP SWP ( during in (see problems are noise thus band SWP 3.2. 1986) -25% the be specifically pipeline. and not fiducial We angle The is times the many technique Paper Here by functions lower 3.3. exposure affecting rejected 47496 and at goals similarly © had and Bohlin, the spectra. due spectra spectra and note This extracted, rotated (THDA) atmosphere and The data. its between to continua transfer applied. least 47459, spectra hits optimal the of American or somewhat of CSC-GSFC we Low since not cross-correlate which signal-to-noise HST to is spectral of I), than incidence LWP associated NEWS/PS that of This method intensity-dependent. the so and extraction. present that This of errors 50% describe the during been and were & were for this In times image (Bohlin developed areas fainter Signal-to-Noise affected; their data the are in detector the campaign, function and SWP a We Neill differs sensitivity extraction are 25318 the were and spectra. were G weaker technique UV possibly program, an finalized profile, calculations processed not in GEX-extracted Si extracted takes the l were note is also even several worst 9 the measurements raised whose SWP NEWSIPS 47505, with adjacent the many, those Astronomical than ( IV nuclear done, l-B2B, generally Final not in 1993a, from 1991 quality This are thus, weak. and extraction. the that for ratio. sensitivity far than image. NEWSIPS advantage at line The underexposed errors case, weighting during the the removed technique degradation 47692 most spectral extremely at the they are pixels ) , low-dispersion utilizes Archive too resulting raw though IUESIPS C taken calibration using the using to for continuum these b). the the Ratio which (in In errors flux An IV of emission-line ofD. lowest SWP low. publication less determine science The in NEWSIPS relevant immediate SWP In the emission time Finally, two time) the estimated wide, were near versions the level centering the dispersion The information were of BROAD-LINE photometric extractions. degradation, not Processing Spectra during deferred two than SWP Finley SWP is each in induced advantage 47705, for weak in adjacent 1988-1989 light the NEWSIPS 4 our Society based signal-weighted minimum a 7 corrections significantly image all, better fluxes uses several spectra probably added long-slit 422 not geometrically which to of the camera 47387, those point spectra. spectra lines. JUE levels. of the SWP and spectra the extraction, cosmic-ray by NEWSIPS error an the fluxes conspired the central the to upon time the are function exposed are with spectra. Nichols relative present further spectra was impor­ ion are collab­ here on a of whole in wave­ prob­ worst white SWP SWP CCD cam­ Final SWP spec­ Only • fixed were both light later con­ The also and ap­ the be­ are the the the the are hit on REGION Provided in to is between time times the which jected shows galaxy. in given 5"}, as column in II, Julian known the trograph viously tions. tion, that tially ambiguity. ( 5 ) . and observatory dispersion differences, character mensional these tor was were 8954) several south sured and eastward case differences imaging FWHM make umn solute Penston, recalibrated part IN Table Optical this the used III, response spectrum; by galaxy the characterizes The Vil recorded of our of at and made (6), are AGNs. unresolved, in The FITS the for of in indicates the calibration contain experiment. and Date, radius this in to the because The the occasions 3 ( the approximate column of of 1992 or first observation the fifth entrance from accounted 10) a is & data is previous the corresponding 4. broadband the measured nominal direction the position as detectors). this VII; photoelectric project among a file Ohio for added in format beginning NASA Sandage magnitudes code, THE functions, cross-dispersion gives complete as parameter second VIII. at NGC IRAF these November observing 8'~0. the north; as broad Johnson header. example series, the of in the the (9). homogeneous State of GROUND-BASED 4.1. this provides both the four with a aperture, when 4.2. as papers: by Columns column observatory the Nevertheless, angle spectral of codes the most unique 5548, (i.e., for reduction telescope, Astrophysics component the in flux parameter are Finally, ( in wavelength shorter Romanishin whenever log this 1971), Optical The The least of atmospheric spectra we sets Optical photometry in a is the in column necessary V season Julian cross-dispersion for and aperture given 0°. the of measurements, significant are the each number the the table various and find through file (3). identifier slit of spectroscopic significant resolution conventional in this An ( 1 ) "extraction timescales slit direction; the to 1993 first which next Spectroscopy data, system arcseconds, is naming (set Date. the that Photometry position and observation, a to as estimate of closely aid is star, and The possible. width ( of given same good range primarily 4). two photometry, possible, greater to filter the optical et section. of September next OBSERVATIONS the A), circular instrument there archival is tied seeing and ( change eliminate by has Column next namely, al. An 2) Data telescopes. and characters is slit figures convention description as in HtJ in follows covered bandpasses the since which that angle four ( given give of observations direction window" based we been the are in additional 1994); The manner, precision column to length character which and monitoring emission is the most In value because apertures Papers use will star is and will System given the dispersion some characters the in ( (hereafter general, V is the in projected that tracking recalibrated seeing, any 4) on were that used by the of = given UT be ( we 1 observations column in is discuss column BLR gives n5 given In spectrum either runs of (7). is the of these for 13.75, in the systematic remaining and in examined contained II, dates truncated the than of adopt line to gives ) made arbitrary date Penston, of obtained order the identify column when degrees two-di­ of III, the Papers of data in obtain a is north­ In detec­ varia­ cross­ direc­ is slight "year same CCD (e.g., mea­ spec­ data, code how pro­ PSF pre­ spa­ ( B and and this col­ 295 ( IV, the the the ab­ the 8), on 3) to as - is is it 1995ApJS...97..285K TABLE 3 Loo OF SPECTROSCOPIC 0BSERVA TIONS

UT Julian Date Aperture Seeing Res. Range IRAF UT Julian Date Aperture Seeing Res. Range IRAF Date Time (2440000+) Code Size P.A. (") (A) (A) file name Date Time (2440000+) Code Size P.A. (") (A) (A) file name @ (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) 1992 Nov 27 12:41 8954.03 A 5.0 x 7.5 90 5.0 9 4550 - 5710 n58954a 1993 Mar 25 11:20 9071.98 F 3.2 x 6.4 90 5 4720 - 7150 n59071fb > 1992 Dec 10 12:00 8967.00 A 5.0 x 7.5 90 4.4 9 4520 - 5680 n58967a 1993 Mar 28 00:40 9074.53 w 3.0 x 10.0 90 5 9 4500 ~ 5630 n59074w 9 1992 Dec 16 12:19 8973.01 A 5.0 x 7.5 90 4.2 9 4510 - 5670 n58973a 1993 Mar 28 12:06 9075.01 F 3.2 x 6.4 90 5 4720 - 7150 n59075f 1'1:1 .....'"I 1992 Dec 24 12:47 8981.03 A 5.0 x 7.5 90 3.2 9 4500 - 5660 n5898la 1993 Mar 30 21:30 9077.39 w 3.0 x 10.0 90 3 9 4390 - 5590 n59077w ~ 1993 Dec 25 13:16 8982.05 F 3.2 x 6.4 90 5 4670 - 7160 n58982f 1993 Mar 31 21:00 9078.41 w 3.0 x 10.0 90 3 9 4450 - 5630 n59078w ~ 1993 Jan 4 12:16 8992.01 A 5.0 x 7.5 90 3.1 9 4540- 5700 n58992a 1993 Mar 31 22:34 9078.44 M 3.0 x 10.0 0 2.5 5 4430 - 7130 n59078m 1993 Jan 12 12:29 9000.02 A 5.0 x 7.5 90 3.1 9 4650 - 5670 n59000a 1993 Apr 2 08:20 9079.85 A 5.0 x 7.5 90 4.4 9 4500 - 5670 n59079a = 1993 Jan 17 03:32 9004.65 B 15.0 x 11.0 3.6 2-3 15 4510 - 7910 n59004b 1993 Apr 2 23:10 9080.46 M 3.0 x 10.0 0 3 5 4420 - 7120 n59080m >[IJ .... 1993 Jan 21 11:42 9008.99 A 5.0 x 7.5 90 3.1 9 4510 - 5680 n59008a 1993 Apr 5 22:58 9083.46 M 3.0 x 10.0 0 2 5 4470 - 7170 n59083m '"I 1993 Jan 22 12:58 9010.04 F 3.2 x 6.4 90 5 4660- 7140 n59010f 1993 Apr 7 17:14 9085.22 y 4.0 x 11.5 90 3-4 11 4300 - 7000 n59085y 0 1993 Jan 23 01:25 9010.56 w 3.0 x 10.0 90 3 9 4350 - 5550 n59010wa 1993 Apr 8 07:38 9085.82 A 5.0 x 7.5 90 3.0 9 4510 - 5670 n59085a =0 1993 Jan 23 03:10 9010.63 w 3.0 x 10.0 90 3 9 6120 - 7240 n59010wb 1993 Apr 9 16:53 9087.20 y 4.0 x 11.5 90 3-4 11 4300 - 7000 n59087y 9 1993 Jan 23 12:48 9011.03 F 3.2 x 6.4 90 5 4660 - 7140 n59011f 1993 Apr 10 16:43 9088.20 y 4.0 x 11.5 90 2-3 11 4300 - 7000 n59088y ..... 1993 Jan 24 12:45 9012.03 F 3.2 x 6.4 90 5 4660 - 7140 n59012f ~ 1993 Apr 10 19:35 9088.32 w 3.0 x 10.0 90 3 9 4500 - 5540 n59088wa ~ 1993 Jan 25 03:24 9012.64 B 15.0 x 11.0 3.6 2-3 15 4510 - 7910 n59012b 1993 Apr 10 21:45 9088.41 w 3.0 x 10.0 90 3 9 6180 - 7200 n59088wb 1993 Jan 25 12:48 9013.03 F 3.2 x 6.4 90 5 4660- 7140 n59013f 1993 Apr 11 16:05 9089.17 y 4.0 x 11.5 90 2-3 11 4300 - 7000 n59089y rJ).- 0 1993 Jan 26 06:40 9013.78 T 1.4 x 17.7 160 3 2.5 6218 - 7131 n59013t 1993 Apr 11 21:40 9089.40 w 3.0 x 10.0 90 3 9 4400 - 5570 n59089w y .....~ 1993 Jan 26 10:30 9013.94 A 5.0 x 7.5 90 2.8 9 4540 - 5700 n59013a 1993 Apr 12 16:07 9090.17 4.0 x 11.5 90 2 11 4300 - 7000 n59090y 1'1:1 1993 Jan 26 13:09 9014.05 F 3.2 x 6.4 90 5 4660 - 7140 n59014f 1993 Apr 13 07:37 9090.82 F 3.2 x 6.4 90 5 4720- 7150 n59090f .... N "< IQ 1993 Jan 27 00:20 9014.51 w 3.0 x 10.0 90 3 9 4370 - 5550 n59014wa 1993 Apr 13 08:20 9090.85 A 5.0 x 7.5 90 5.2 9 4510 - 5680 n59090a 0\ 1993 Jan 27 02:10 9014.59 w 3.0 x 10.0 90 2 9 6070 - 7200 n59014wb 1993 Apr 13 10:09 9090.92 H 4.0 x 10.0 ·51 1 8 3140 - 8038 n59090h • 1993 Jan 29 06:46 9016.78 T 1.3 x 4.8 160 2 2.5 6158- 7071 n59016t 1993 Apr 13 15:41 9091.15 y 4.0 x 11.5 90 2 11 4300 - 7000 n5909ly ~ 1993 Jan 29 13:58 9017.08 H 4.0 x 10.0 0 3 8 3262 - 10500 n59017ha 1993 Apr 14 08:26 9091.86 F 3.2 x 6.4 90 5 4720 - 7150 n59091f '"I 1993 Jan 29 14:11 9017.09 H 4.0 x 10.0 0 3 4 5830 - 7100 n59017hb 1993 Apr 14 11:37 9091.98 H 4.0 x 10.0 61 1 8 3120 - 8040 n59091h 0 1993 Feb 2 11:11 9020.97 A 5.0 x 7.5 90 4.3 9 4520- 5690 n59020a 1993 Apr 15 08:37 9092.86 H 4.0 x 10.0 146 2 8 3120 - 8040 n59092h <..... Q. 1993 Feb 11 10:55 9029.95 A 5.0 x 7.5 90 4.3 9 4540 - 5680 n59029a 1993 Apr 15 08:40 9092.86 F 3.2 x 6.4 90 5 4720 - 7150 n59092f y 1'1:1 1993 Feb 13 00:58 9031.54 R 1.5 x 12.5 0 10 4540 - 7030 m5903lr 1993 Apr 16 18:04 9094.25 4.0 x 11.5 90 4 11 4300 - 7000 n59094y Q. 1993 Feb 13 13:52 9032.08 H 4.0 x 10.0 44 3-4 8 3090 - 8056 n59032h 1993 Apr 17 01:38 9094.57 B 15.0 x 11.0 3.6 2-3 15 4510 - 7910 n59094b C" 1993 Feb 16 00:10 9034.50 w 3.0 x 10.0 90 9 9 4340 - 5520 n59034wa 1993 Apr 17 11:46 9094.99 F 3.2 x 6.4 90 5 4720 - 7150 n59094f "< 1993 Feb 16 02:25 9034.60 w 3.0 x 10.0 90 9 9 6050 - 7180 n59034wb 1993 Apr 17 17:31 9095.23 y 4.0 x 11.5 90 2 11 4300 - 7000 n59095y 12:00 9036.00 F 3.2 x 6.4 90 5 4660 - 7140 n59036f 9096.99 F 3.2 x 6.4 4720 - 7150 n59096f ~ 1993 Feb 17 1993 Apr 19 11:38 90 5 1'1:1 1993 Feb 21 01:13 9039.55 L 3.0 round - 3 3 4240- 5262 n590391 1993 Apr 21 07:36 9098.82 F 3.2 x 6.4 90 5 4720 - 7150 n59098f 1993 Feb 21 23:58 9040.50 L 3.0 round - 4 3 4240 '- 5262 n590401 1993 Apr 21 07:06 9098.80 z 2.0 x 10.0 0 2.5 5 4630 - 5900 n59098za z 1993 Feb 26 13:09 9045.04 F 3.2 x 6.4 90 5 4660 - 7140 n59045fa 1993 Apr 21 07:36 9098.82 z 2.0 x 10.0 0 2.5 5 5850- 6960 n59098zl;> rJ).> 1993 Feb 27 11:03 9045.96 F 3.2 x 6.4 90 5 4660 - 7140 n59045fb 1993 Apr 22 07:11 9099.80 A 5.0 x 7.5 90 2.1 9 4570 - 5720 n59099a 1993 Mar 2 10:36 9048.94 A 5.0 x 7.5 90 3.9 9 4530 - 5700 n59048a 1993 Apr 23 16:41 9101.19 y 4.0 x 11.5 90 3-4 11 4300 - 7000 n59101y > 1993 Mar 10 09:32 9056.89 A 5.0 x 7.5 90 4.5 9 4540 - 5690 n59056a 1993 Apr 23 22:09 9101.42 B 15.0 x 11.0 3.6 2-3 15 4510 - 7910 n5910lb 1993 Mar 15 09:33 9061.90 F 3.2 x 6.4 90 5 4660- 7140 n5906lf 1993 Apr 24 16:50 9102.20 y 4.0 x 11.5 90 3-4 11 4300 - 7000 n59102y >[IJ .... 1993 Mar 16 08:56 9062.87 A 5.0 x 7.5 90 3.4 9 4540 - 5700 n59062a 1993 Apr 25 11:32 9102.98 F 3.2 x 6.4 90 5 4720 - 7150 n59102f '"I 0 1993 Mar 18 07:16 9064.80 A 5.0 x 7.5 90 3.5 9 4530 - 5680 n59064a 1993 Apr 26 03:21 9103.64 z 2.0 x 10.0 0 3.0 5 4620 - 5900 n59103za "O 1993 Mar 18 12:11 9065.01 F 3.2 x 6.4 90 5 4660 - 7140 n59065f 1993 Apr 26 03:59 9103.67 z 2.0 x 10.0 0 3.0 5 5850 - 6960 n59103zb =- 1993 Mar 19 12:19 9066.02 F 3.2 x 6.4 90 5 4720 - 7150 n59066f 1993 Apr 29 05:24 9106.73 z 2.0 x 10.0 0 3.0 5 4620 - 5900 n59106za "<[IJ 1993 Mar 20 12:26 9067.02 F 3.2 x 6.4 90 5 4720 - 7150 n59067f 1993 Apr 29 05:51 9106.74 z 2.0 x 10.0 0 3.0 5 5850 - 6970 n59106zb ..... 1993 Mar 23 11:56 9070.00 F 3.2 x 6.4 90 5 4720 - 7150 n59070f 1993 Apr 29 21:58 9107.42 1.8 x 6.0 90 7 3700 - 6950 n59107u ~ u [IJ 1993 Mar 23 23:05 9070.46 w 3.0 x 10.0 90 2 9 4370 - 5560 n59070wa 1993 Apr 30 07:40 9107.82 A 5.0 x 7.5 90 4.5 9 4510 - 5660 n59107a ~ 1993 Mar 24 00:40 9070.53 w 3.0 x 10.0 90 2 9 6140 - 7266 n59070wb 1993 Apr 30 11:36 9107.98 H 4.0 x 10.0 61 2-3 8 3114 - 8032 n59107h 1993 Mar 24 12:02 9071.00 F 3.2 x 6.4 90 5 4720 - 7150 n5907lfa 1993 May 4 17:42 9112.24 y 4.0 x 11.5 90 3 11 4300 - 7000 n59112y ....~ ~ rJ).

"<[IJ .... 1'1:1 9 1995ApJS...97..285K TABLE 3-Continued

UT Julian Date Aperture Seeing Res. Range !RAF UT Julian Date Aperture Seeing Res. Range !RAF Date Time (2440000+) Code Size P.A. (") (A) (Al file name Date Time (2440000+) Code Size P.A. (") (A) (A) file name (1) (2) (3) (4) (5) {6) (7) (8) (9) (10) (1) (2) (3) (4) (5) (6) (7) (8) {9) (10) @ 1993 May 5 17:47 9113.24 y 4.0 x 11.5 90 3 11 4300 - 7000 n59113y 1993 Jun 21 04:32 9159.69 F 3.2 x 6.4 90 5 4720 - 7170 n59159f 1993 May 6 22:04 9114.42 M 3.0 x 10.0 0 2 5 4950 - 7440 n59114mb 1993 Jun 22 03:53 9160.66 F 3.2 x 6.4 90 5 4660 - 7170 n59160f > 1993 May 7 00:14 9114.51 M 3.0 x 10.0 0 2.5 5 4740 - 7440 n59114ma 1993 Jun 25 04:29 9163.69 A 5.0 x 7.5 90 3.5 9 4530 - 5680 n59163a a 1993 May 7 07:25 9114.81 A 5.0 x 7.5 90 3.1 9 4470 - 5630 n59114a 1993 Jun 25 20:57 9164.37 B 15.0 x 11.0 3.6 2-3 15 4510 - 7910 n59164b ~ 05:52 9120.74 J 2.1x10.0 90 1.5 5 4570 - 7260 n59120j 1993 Jun 28 08:13 9166.84 H 4.0 x 10.0 61 1.5 8 3110 - 8040 n59166h .....'"I 1993 May 13 ~ 1993 May 13 07:17 9120.81 F 3.2 x 6.4 90 5 4720 - 7150 n59120f 1993 Jul 1 04:31 9169.69 A 5.0 x 7.5 90 3.1 9 4530~5680 n59169a 1993 May 14 06:35 9121.77 J 2.1x10.0 90 1.5 5 4570 - 7260 n59122j 1993 Jul 8 04:28 9176.69 A 5.0 x 7.5 90 3.1 9 4530 - 5690 n59176a = 1993 May 15 08:10 9122.84 A 5.0 x 7.5 90 1.5 9 4530 - 5600 n59122a 1993 Jul 14 08:19 9182.85 H 4.0 x 10.0 57 2.0 8 3112 - 8034 n59182h = 1993 May 18 03:48 9125.66 F 3.2 x 6.4 90 5 4660 - 7160 n59125f 1993 Jul 15 04:27 9183.69 A 5.0 x 7.5 90 3.2 9 4540 - 5700 n59183a >[IJ .... 1993 May 19 04:36 9126.69 F 3.2 x 6.4 90 5 4720 - 7160 n59126f 1993 Jul 19 03:48 9187.66 F 3.2 x 6.4 90 5 4660 - 7170 n59187f '"I 1993 May 20 04:16 9127.68 F 3.2 x 6.4 90 5 4610 - 7170 n59127f 1993 Jul 20 04:06 9188.67 F 3.2 x 6.4 90 5 4660 - 7170 n59188f Q 1993 May 21 05:55 9128.75 A 5.0 x 7.5 90 3.7 9 4530 - 5670 n59128a 1993 Jul 21 04:31 9189.69 F 3.2 x 6.4 90 5 4610 - 7220 n59189f Q 1993 May 21 05:28 9128.73 F 3.2 x 6.4 90 5 4660- 7170 n59128f 1993 Jul 22 03:42 9190.65 A 5.0 x 7.5 90 3.1 9 4560 - 5720 n59190a = 1993 May 21 23:05 9129.46 w 3.0 x 10.0 90 3 9 4430 - 5620 n59129w 1993 Jul 23 03:53 9191.66 F 3.2 x 6.4 90 5 4660 - 7170 n59191f a..... 1993 May 22 22:55 9130.46 w 3.0 x 10.0 90 2 9 4410- 5560 n59130wa 1993 Jul 28 06:05 9196.77 H 4.0 x 10.0 60 1-1.5 8 3140 - 8030 n59196h ~ 1993 May 23 00:42 9130.53 w 3.0 x 10.0 90 2.5 9 6100 - 7230 n59130wb 1993 Jul 29 04:52 9197.70 A 5.0 x 7.5 90 3.6 9 4530 - 5690 n59197a = 1993 May 23 20:17 9131.35 B 15.0 x 11.0 3.6 2-3 15 4510 - 7910 n5913lb 1993 Aug 6 04:23 9205.68 A 5.0 x 7.5 90 3.5 9 4540 - 5700 n59205a 00- 3.5 4520 - 5680 n59211a Q 1993 May 23 20:30 9131.35 w 3.0 x 10.0 90 1 9 4470 - 5630 n5913lwa 1993 Aug 12 03:52 9211.66 A 5.0 x 7.5 90 9 1.5 3120- 8020 ~..... 1993 May 23 22:50 9131.45 w 3.0 x 10.0 90 1 9 6060 - 7190 n59131wb 1993 Aug 13 05:44 9212.74 H 4.0 x 10.0 60 8 n59212h 1993 May 24 13:09 9132.05 E 5.0 x 8.4 90 5 4670 - 5330 n59132e 1993 Sep 10 03:08 9240.63 A 5.0 x 7.5 90 4.4 9 4530 - 5690 n59240a ....~ "< 1993 May 24 21:35 9132.40 w 3.0 x 10.0 90 2 9 4430 - 5600 n59132wa 1993 Sep 10 04:02 9240.67 H 4.0 x 10.0 62 1 8 3120 - 9900 n59240h 1993 May 24 23:45 9132.49 w 3.0 x 10.0 90 2 9 6110 - 7230 n59132wb 1993 Sep 12 04:05 9242.67 H 4.0 x 10.0 59 2 8 3160 - 8040 n59242h • N 1993 May 28 06:19 9135.76 A 5.0 x 7.5 90 3.1 9 4510 - 5660 n59135a 1993 Sep 13 03:54 9243.66 H 4.0 x 10.0 61 2 8 3120 - 8040 n59243h 1993 May 28 09:53 9135.92 F 3.2 x 6.4 90 5 4660 - 7140 n59135f 1993 Sep 25 03:15 9255.63 H 4.0 x 10.0 59 1.5 8 3200 - 8030 n59255h ~ -.J '"I '° 1993 Jun 1 23:00 9140.46 w 3.0 x 10.0 90 3 9 4380 - 5570 n59140w Q 1993 Jun 2 21:25 9141.39 w 3.0 x 10.0 90 3 9 4360 - 5550 n59141wa <..... Q. 1993 Jun 2 23:10 9141.46 w 3.0 x 10.0 90 3 9 6230 - 7350 n5914lwb ~ 1993 Jun 4 05:20 9142.72 A 5.0 x 7.5 90 4.5 9 4500 - 5650 n59142a Q. 1993 Jun 11 05:47 9149.74 A 5.0 x 7.5 90 4.2 9 4500 - 5660 n59149a 'r:::;' 1993 Jun 12 08:22 9150.85 F 3.2 x 6.4 90 5 4720 - 7170 n59150f "< 1993 Jun 13 03:52 9151.66 F 3.2 x 6.4 90 5 4720 - 7170 n59151f 1993 Jun 14 04:01 9152.67 F 3.2 x 6.4 90 5 4720 - 7170 n59152f ~ ~ 1993 Jun 16 20:25 9155.41 w 3.0 x 10.0 90 2-5 9 4310 - 5450 n59155wa 1993 Jun 16 23:05 9155.46 w 3.0 x 10.0 90 2 9 6090 - 7220 n59155wb z 1993 Jun 17 04:01 9155.67 F 3.2 x 6.4 90 5 4720 - 7170 n59155f 00> 1993 Jun 17 21:05 9156.39 w 3.0 x 10.0 90 3 9 4310- 5510 n59156wa 1993 Jun 17 23:05 9156.46 w 3.0 x 10.0 90 3 9 6020 - 7160 n59156wb > 1993 Jun 18 04:00 9156.67 F 3.2 x 6.4 90 5 4720- 7170 n59156f 1993 Jun 18 05:59 9156.75 A 5.0 x 7.5 90 4.2 9 4530 - 5690 n59156a >[IJ .... 1993 Jun 18 21:45 9157.41 w 3.0 x 10.0 90 2 9 4240 - 5450 n59157wa '"I Q 1993 Jun 18 22:50 9157.45 w 3.0 x 10.0 90 2 9 6080 - 7210 n59157wb "O 1993 Jun 19 04:01 9157.67 F 3.2 x 6.4 90 5 4660 - 7170 n59157f :r 1993 Jun 19 20:20 9158.35 w 3.0 x 10.0 90 2 9 4350 - 5530 n59158wa "<[IJ 1993 Jun 19 21:20 9158.39 w 3.0 x 10.0 90 2 9 6080 - 7200 n59158wb ..... 1993 Jun 20 03:55 9158.66 F 3.2 x 6.4 90 5 4660- 7170 n59158f ~ [IJ 1993 Jun 20 20:15 9159.34 w 3.0 x 10.0 90 1.5 9 6080- 7230 n59159wb ~ 1993 Jun 20 21:15 9159.38 w 3.0 x 10.0 90 1.5 9 4340 - 5550 n59159wa .... = NoTE.-Codes for data origin in col. (4): (A) 1.8 m Perkins telescope+ Ohio State CCD spectrograph; (B) 1.0 m Wise telescope + CCD spectrograph; (E) 1.8 m DAO telescope+ CCD spectrograph; =00 (F) 1.6 m Mount Hopkins telescope + Reticon scanner; (H) 3.0 m Shane telescope + Kast spectrograph; (J) 2.1 m McDonald telescope + Cassegrain Grating spectrograph; (L) 6.0 m Special "<[IJ Astrophysical Observatory + TV scanner; (M) 2.2 m Calar Alto Observatory + CCD spectrographs; (R) 1.5 m Loiano telescope + CCD spectrograph; (T) 4.2 m William Herschel Telescope + CCD .... spectrograph; (U) 1.9 m SAAO telescope + Reticon; (W) 2.6 m Shajn telescope + CCD spectrograph; (Y) 2.2 m Beijing Astronomical Observatory telescope + CCD spectrograph; (Z) 2.2 m ESO a~ telescope + CCD spectrograph. 1995ApJS...97..285K (1989). CCD are al. out THX31156 less camera East Martir, tained umn based sponse scale and observation, Mead, vatory by CCD carefully ments 298 V A In CCD = Romanishin ( given otherwise aperture 1994). Table 1994). with program 0.71, Table Lansing, ( is system images 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 on 3). with Nebraska, as 1.1 function 0'26 images on Columns Date Baja chosen in counting (1) a Aug Aug the Aug Aug Aug Aug Aug Aug Aug Aug Aug Aug Apr Aug Aug Aug Aug Aug Aug Aug Aug Aug Aug Aug Aug The Mar Mar Mar Ma.r Apr Apr Apr V- m 5 the a check column © chip UT and we on radius CCD by of telescope, 1 1 1 1 16 16 16 16 15 15 15 15 15 15 14 16 16 14 14 14 14 14 14 14 17 17 17 17 pixe1- 16 16 15 15 Michigan. noted. 0.60 magnitudes, R American California. Michigan were LoWELL et photoelectric give the measuring annuli. 04:00 03:39 03:30 03:04 09:56 03:56 03:56 03:30 03:04 02:43 02:43 04:00 03:39 03:14 03:14 02:47 02:47 04:03 04:03 03:37 03:37 03:16 03:16 02:54 02:54 the 09:45 09:37 09:26 08:03 07:52 07:40 07:27 Time with are = are (2) al., 6 on (1) camera statistics, given m 0.39, Behlen 1 gives ( obtained corresponding V • given 6). it the a as Measurements -band and Julian telescope (2440000+) 1.1 is as Metachrome When 9214.67 9214.65 9215.61 9214.67 9215.65 9215.63 9078.91 9215.66 9215.66 9215.65 9215.63 9215.61 9214.65 9214.63 9214.63 9214.62 9214.62 9213.67 9213.67 9213.65 9213.65 9213.64 9213.64 9213.62 9213.62 9063.84 9063.83 9063.82 9063.81 9078.91 9078.90 9078.89 This also described in andR absolute the State (3) TABLE m given on in the (2) as Observatory Date columns The Astronomical CCD are measurements aperture Table the measurements possible measured in system possible, brightness give University - in in BVRI Filter of PHOTOMETRY 2.0 4 detector (4) v v v v v v v v B B R R R R B B B B B B R R R R J I I I I I I I I calibration. Table every Julian 7. by the the = ( m II is 4) made to photometry 0.31 Aperture with (a.rcsec) we telescope UV described Beckert through 0. UT Crimean and calibrate 25.0 25.0 25.0 25.0 25.0 25.0 25.0 25.0 25.0 25.0 25.0 25.0 8.0 8.0 8.0 8.0 8.0 8.0 8.0 8.0 8.0 8.0 8.0 8.0 8.0 8.0 8.0 8.0 8.0 8.0 8.0 8.0 case 5 (6) (5) 4. of 76 Date used 0.6 mag. coating. The the made is the with date ( 5 ) , from m -0.01 Society m Formal errors, magnitude is a such Lowell telescope host filters & the at As 12.52 13.50 12.93 14.16 12.92 12.92 13.51 14.17 14.18 12.54 13.49 12.37 12.93 13.64 12.37 13.63 13.63 11.88 12.53 11.89 11.91 12.53 12.93 13.52 12.94 13.57 14.26 12.88 14.16 12.93 12.36 12.50 respectively, given high-quality and the telescope with by Laboratory was Thompson images San Newberry described The bandpass measure­ galaxy Smith mag OPTEC time and carried KORISTA a Obser­ in Pedro CCD • pixel near col­ un­ ob­ re­ Provided in of in et ET tion Crimean Center measurements obtained tometry there tra Sternberg SWP sphere scribed surements ( function comparison applicable and ilar Laurel, FOS tion ments. uncertainty of 1993a, Bohlin In the V AL. smoothed by flux HST -band is but order flux spectra JUE were based of In the b) for by Maryland, was scales is thought 1994). between 1993 1993 1993 1993 1993 1993 1993 1993 1993 Astrophysical 1993 1993 1993 1993 campaigns, calibration the bottom 5.1. G Institute and Skillman to measurements that SWP are Basement Date NASA 191-B2B, Date in contemporaneous between on (1) also (1) Apr Apr Apr Apr Jun May May May Apr MSU the were Apr Apr Apr Apr to as was given this Jnterca/ibration we UT UT stars In SAN SWP 16 data 23 22 22 27 18 5. 24 22 21 20 26 14 17 sub-Lya undertaken possible. the 0.5 may first the (CLSI) ANALYSIS to are simply new the & PEDRO 09:27 07:22 09:38 Time 11:25 04:32 04:34 03:54 04:31 04:41 06:03 04:42 04:42 04:38 Time from Astrophysics 2 (3) (2) (2) in is the m scale the panel Astrophysics spectral lie two the Patterson top CCD based shifted given combine JUE Observatory V-BAND absolute Table are between mean two Julian obtained (2440000+) Julian major (2440000+) region TABLE the calibration MARTIR panel multiplied at TABLE Because to 9098.98 9099.81 9097.90 9101.89 9095.69 9154.69 9133.66 9124.69 9100.70 9099.70 9099.69 9104.75 9121.69 PHOTOMETRY of given SWP (3) upon Nauchny, with in sets the list resolution Figure OF onto 8. Date CCD Date SWP of observations Table ( the step of of scale ofLyutyi Photoelectric the 199 same in of 2% 5 THE 2.0 Spectra the 6 a (CBA) with Figure the the PHOTOMETRY the (R=8") light Table (R=7") data (CAO), white and m 3). HST 5 and 13.59 13.60 13.60 13.62 involved 13.62 13.62 13.54 13.49 13.59 13.59 13.49 13.54 13.59 bases into Data (4) 4 (5) (4) V 1.25 V is we DATA 10. spectra V-BAND NEWSIPS basis. peak and (magnitudes) (magnitudes) an in still should curves corrected 4%, show 9. dwarf FOS the 5 0.3 This ( the m RCA is the 1972). (R= we System (R=25") Here of and under in The telescope known the 13.43 13.40 13.35 13.33 13.37 13.39 13.31 13.39 13.36 12.96 12.96 12.96 12.97 FOS m converting presented 20 (5) aperture the and the from show system V-band be 9''.8) model both CCD telescope the larger cases the conversion calibration on FOS Civ ratio. data. investiga­ the ( V calibra­ a Vol. as Bohlin instru­ on where atmo­ -band of direct is emis- value spec­ mea­ pho­ JUE sim­ here The The the de­ the the 97 in 1995ApJS...97..285K individual greater level, trum. tainly wavelength SWP sion shorter feature of artifacts ically longer lower than multiplicative, residual ror ple NEWSIPS NEWSIPS 1500 No. Looking the in could 2, line, its A). lower the with spectrum state C A due wavelengths 1995 than as wavelengths. contemporaneous 1993 1993 1993 1993 1993 1993 IV nonlinearity in similar flux The it whose have CRIMEAN Date spectra SWP some emission at 0.6 to spectra. calibration 1993 1993 1993 1993 1993 1993 the 1993 1993 1993 1993 1993 1993 1993 1993 1993 1993 (1) © May May May Mar Apr Apr SWP is misalignment, 1 the calibration BEHLEN the in m Date UT "flip-flop" at American (1) since Jun Jun Jun Jun 24 21 Mar May Mar Apr Apr Apr Apr Jan Mar Mar Mar Mar SWP 27 20 14 13 an which ratio wavelength the V-BAND the systematic ratio wavelength flux UT SWP 4 9 7 10 11 24 22 21 13 as 22 1 17 15 12 16 23 08:26 07:04 08:44 06:10 06:07 Time 10:46 LABORATORY Some extended is (2) line neighboring longer it OBSERVATORY spectra is We well. not with at CCD in 20:40 21:00 21:10 21:12 21:39 22:19 20:46 22:42 19:14 02:19 00:52 01:24 01:47 02:49 21:32 19:34 Time is had removed (2) certainly PHOTOELECTRIC nonlinearity the is Julian the in (2440000+) Figure effect note understood. of 9120.86 9073.95 9127.85 9121.79 9101.76 9098.75 TABLE FOS TABLE not some The PHOTOMETRY this wavelengths a (3) Astronomical although shorter Julian trend that (2440000+) the scale same (e.g., was 9149.37 9150.36 9146.30 9148.32 nonnuclear 9131.38 9102.38 9100.40 9099.43 9069.45 9091.37 9063.54 9062.56 8991.62 9047.60 9061.57 9059.40 Date lower simply that in (3) spectrum region. ratio STERNBERG 5 structure part still dispersion continuum Date in could set the 7 for 0.76 8 between wavelengths SWP more flux present, varies at by region the of a the The V m PHOTOMETRY V The the 13.65 13.63 13.59 13.62 13.55 13.64 13.63 13.67 13.68 13.61 13.59 13.57 13.59 13.56 13.56 13.47 problem in 13.41 13.38 13.44 13.48 13.50 13.55 (R (magnitudes) low and (magnitudes) this the V-BAND at (R= (JD C in 47505 detail, contribution turn = INSTITUTE uncertainty offset BROAD-LINE SWP (4) higher (4) roughly ± ± ± ± III at ± ± ± ± ± ± ± ± is ± ± ± ± every 7''.15) the ± ± ± ± ± ± count near (which less mean effect, 8") 0.02 0.02 0.02 0.01 especially O.Ql 0.02 0.02 0.02 0.01 0.03 0.02 0.02 0.02 0.02 0.02 0.01 2,449,097). Society 0.03 O.Q2 0.04 0.02 0.04 0.02 observed broad about produce ratio /FOS is the was of is than the SWP wavelength almost apparently zero-point FOS rates. but systemat­ 1470 in emission the is the position 1 ratio princi­ in due flux in in in an at some • spec­ ±6% only The and cer­ the the the the the er­ Provided REGION to at is wings, dows trum. served below. emission-line 0.017 continuum observed will here: rest measurement windows, and for factors served and differences, the measurements below. larger narrow 1663 IN Eight In Finally, by easy FOS be frame. wavelengths not this 4. A. direct We AGNs. measure frame, aperture in the the of( higher He "continuum" The referencing spectra, just paper the emphasize frame we 1 Balmer 1993 1993 1993 1993 1993 1993 Wavelengths II NASA 5.2. integration 1993 1993 1993 1993 CRIMEAN band they + SWP continuum were >..1640 note Date the CBA and VIII. than Date (1) z) for Jun Jun Jun May Apr Apr a (1) all Apr Apr May Mar SWP l.25 and The 3 designating a are true UT UT will contemporaneous 23 20 10 SWP 27 26 and ultraviolet chosen spectra 0.3 continuum 13 that, 5.2.1. significant 30 24 recombination 7 7 those m that Astrophysics feature with ASTROPHYSICAL then FOS acceptably m windows, 20:22 20:55 21:22 20:57 Time 20:29 19:51 spectra). continuum 05:25 06:45 01:14 02:06 Time V-BAND ( 1 be (2) and (2) based PHOTOMETRY V-BAND reseau will none referring fluxes + Direct measured TABLE by the quoted must TABLE Spectral converted z) Julian (2440000+) spectral observed Julian (2440000+) inspection be the 9149.33 9162.35 9159.37 9105.35 9121.39 9104.37 measurements 9114.59 9101.73 9053.78 9107.55 spectra. fraction PHOTOELECTRIC 2 of upon measurements (3) , CCD (3) also ( artifact Integration quoted generally Whatever respectively. the F>.) Date small. name Date 9 10 in to level; Measurements continuum, OBSERVATORY the so-called in be PHOTOMETRY fitting. FOS and spectral to the Data peaking V of V The the narrow 13.57 13.58 13.57 13.51 13.50 13.56 of of 13.67 13.68 13.62 13.68 in (magnitudes) presence We nominally (R= (magnitudes) and broad (R= the emission-line 20 rest SWP the an the (4) observed (4) the component ± We ± ± ± ± ± ± ± ± ± compare 7".5) were System A same presented 8 Two continuum O.Ql emission O.Ql 0.02 0.01 0.03 0.01 mean regions, 0.06 0.06 0.06 0.06 11 frame, were observed near He ) wide spectra origins describe emission and of made II methods feature located FOS employed the 1667 in emission, frame the for spectral such in§ the line strong of in frame fluxes fluxes in these spec­ Fe win­ A z line 299 ob­ ob­ the the the 5 by or as of in at .3 = II 1995ApJS...97..285K uum. emission-line C lead ered and continuum The various termined wavelength that within countered Only 2195 tions which significant all in tents. with We s- defines length ing mean ultraviolet pseudo-continuum 300 IV Flo. The 1 six subsequent abscissa cm- time plot we contemporaneous >.. blue suspect their of A 3 of 1549 Table rest These occur was 3000 continuum 5.-Top days these band place 2 the emission past these for A.- by cores wavelength statistical in the figures has determined light-curve emission-line continuum © windows interval or km the near 1 because 11 continuum suffers continuum a most • attempts units flux panel: continuum American The FOS more. linear lists s- two corresponding FOS JD as features 1 of level confidence was statistical redward contaminate Comparison light-curve the the FOS errors after observed the separate 2,449,101 of Single-day on .. i i ~ "" I ~ spectra interpolation ..., :;.: [/) .Sl p.. ""' 0 P:: tables within ~ ..., [/) 0 ... Ill Ill "" El () al Q) in windows of then most the flux underneath SWP wavelength windows. either region each windows 0.8 0.9 1.2 1.1 30 20 removing 10 light were measuring in 0 systematic Astronomical Society value. and wavelength are integrated from observations 1200 1200 errors each (see Table G l in continuum of tables side and ( I I curves , I , I 'I to ,, ,, ,, ,, , JI "events," are ,, given integrated. blueward, the these Clavel light-curve , , 30H r \t I I § these window. A The will emission-line tabulated in JD mean of 2 between an this 12, intervals mean refers and and (A). the windows to this photometric 1300 the 1300 Julian in 2,449, emission 1991 be in within errors. were interpolated FOS the Figure window. such Appendix emission G and kinematics respectively, units flux designated to Table We "events" included ) 190H same spectrum the in Date 131, and over the all as per its to the 1400 1400 followed of 6. line nearest the flux mean defined subsequent 11 are various designated number exposures. in unit The which 10- rest errors We line. in D). lists (solid of dimples this was contin­ consid­ KORISTA the by of falling 14 frame of wave­ fluxes dura­ stress start­ • The The ergs two and and 1500 means. 1500 red the the the en­ the de­ the ex­ line), Provided of smoothed Bottom ET frame. emission-line 1600 velocity >..1486 1600 1519 AL. by panel: to A, emission The the the symmetric near Ratio 1700 1700 lengths. SWP Hen Si1v CIV Cm] C1v C CIV Nv C Lya FA(2195A) FA(2030A) FA(l985A) FA(1790A) FA{1720A) FA{1460A) FA{l350A) FA(1145A) blue •Component b NASA IV IV FOS Window >.1240 peak Red Red Blue Blue >.1549 >.1216 the of >.1640 >.1400 >.1909 resolution, Component• wing line. the DIRECT-lNTEGRA Core Wing Core Wing local (core) 1800 + + 1800 + at mean about Astrophysics given 01v] 0 Sim] We was approximately m] minimum with name SWP >.1402 >.1663 >.1893 defined TABLE in then WINDOWS the observed the 1900 1900 spectrum peak arbitrarily uses mean TJON Wavelength 11 the just frame. rest-frame with 1865-2010 1645-1730 2224-2242 2056-2076 WAVELENGTH 1592-1633 1576-1592 1519-1560 1519-1633 1560-1576 1380-1455 1260-1300 1223-1250 2010-2030 1s10-1830 1370-1380 1475-1495 1155-1175 1740-1760 SWP Data 1576 red to redward the spectrum the defined wing Windowb A mean A A A A A A A A A A A A A A A A A A System blue in the wave­ to of FOS to (dashed extend wing, the extend observed spectrum. Vol. N line). near to IV] 97 to a 1995ApJS...97..285K are and (N 0 to the sion small ofLya. The the N sions (e.g., chosen ity most broad No. 1633 III] The v avoid offsets tabulated v wavelength Lya C and 2, wavelength from in A. of Al240, contribution Xl663), Xl608). III] He rest-frame 1995 to The Figure its The core has the Al909 of Fe avoid II blue-side © approximately wavelength 3000 emission C II. the Si in emission; and American 7. The IV interval Table IV geocoronal +Si interval unidentified The wings emission-line and in Al400 from wavelength flux III] Table red 13 as 10,840 however, designated were interval Al893 Al and forthe for well wing + III the 15 emission Astronomical 0 N thus is Julian (2440000+) km as emission Xl859, may forthe 9135.09 9133.76 9132.95 9131.88 9130.94 9129.94 9129.00 9127.93 9118.95 9120.96 9121.97 9119.96 9122.97 9123.98 9125.92 9124.92 9126.93 9116.01 9117.88 9116.95 9115.00 9114.00 9113.00 IV] 9108.98 9107.98 9106.97 9098.07 9110.99 9111.99 9100.01 9106.03 9110.05 9099.01 9097.00 9104.03 9103.09 9102.02 9101.02 9105.03 ), v •Rest-frame same certain interval strong fluxes for possible in was the s - defined Date as Al402, be Table 1 Si width measured • C as and chosen C contaminated We and lines to IV+ III] 3.04±0.139 3.13±0.140 3.25±0.141 3.46±0.144 3.59±0.149 3.85±0.363 3.92±0.148 2.73±0.131 4.01±0.285 4.87±0.169 4.17±0.218 4.62±0.168 4.95±0.165 4.01±0.153 4.76±0.163 4.31±0.156 3.94±0.151 3.77±0.147 5.25±0.167 4.05±0.146 4.67±0.157 near 3.62±0.144 3.88±0.146 3.94±0.150 3.78±0.150 3.67±0.142 4.27±0.151 4.17±0.152 4.23±0.150 4.65±0.155 3.00±0.132 3.88±0.145 3.87±0.283 3.04±0.133 3.09±0.132 3.83±0.145 2.76±0.126 2.75±0.240 2.56±0.123 F,\(1145A) IV well for lie to emission 14 possibly (direct-integration) illustrate and emission-line BROAD-LINE as + their (Lycx, 0 lie the atop forthe as to 1465 Si the Society IV] between He emission flux avoid III] Lya uncertainties core the 2.93±0.0510 2.95±0.0513 4.04±0.0598 4.33±0.0616 3.16±0.0530 3.21±0.0535 3.86±0.0583 3.63±0.0566 3.41±0.0544 3.79±0.0576 4.01±0.0805 4.45±0.0627 4.00±0.0747 4.30±0.0619 4.62±0.0637 4.48±0.0628 3.47±0.0545 3.76±0.0574 3.56±0.0559 4.08±0.0595 3.88±0.0583 3.51±0.0555 3.45±0.0550 3.62±0.0541 3. 3.49±0.0539 3.47±0.0551 3.74±0.0571 3.43±0.0964 4.11±0.0598 3. 3.01±0.0514 3.60±0.0561 3.35±0.0542 2. 2.68±0.0486 2.88±0.0502 2.48±0.0468 3.50±0.105 CIV F,\(1350A) was weak A. II 72±0.0572 70±0.0568 77±0.0769 from these weak contains is with Xl640 red flux Finally, ofC most missing FOS chosen Al549, veloc­ emis­ com- • from wing lines Fe divi­ very was flux CONTINUUM IV. Provided REGION of + 3.84±0.0341 3.19±0.0550 3.13±0.0308 3.36±0.0319 2.48±0.0276 4.05±0.0351 4.12±0.0353 2.64±0.0285 2.90±0.0298 2.89±0.0298 4.08±0.0352 3.53±0.0416 3. 3.93±0.0347 3.58±0.0330 3.52±0.0327 3.03±0.0306 3.57±0.0328 3.31±0.0307 3.31±0.0313 3.31±0.0316 3.29±0.0316 3.29±0.0315 II 3.48±0.0324 3.38±0.0320 3.23±0.0313 3.13±0.0308 3. 3. 3.20±0.0305 3.17±0.0310 3.11±0.0509 3.24±0.0313 3.00±0.0301 2.52±0.0405 2.42±0.0271 2.60±0.0281 2.68±0.0285 2.25±0.0262 a TABLE F,\(1460A) 79±0.0406 7 72±0.0334 densities, 4±0.0335 gated berg-Marquardt ing Papers Al302, weak 1994) given tical be sources sion-line cussed certainty not ponents. 12 The IN BANDS" in at 2.40±0.0203 2.25±0.0197 2.61±0.0208 3.24±0.0236 3.29±0.0238 3.15±0.0232 3.00±0.0227 2.45±0.0205 2.55±0.0209 2.92±0.0224 2.76±0.0217 2.59±0.0218 2.86±0.0222 3.01±0.0227 3.14±0.0232 3.22±0.0235 3.33±0.0239 2.75±0.0214 2.94±0.0225 2. 2.80±0.0219 3.11±0.0231 3.04±0.0228 2.81±0.0219 2.88±0.0222 2.72±0.0216 2.63±0.0212 2. 2. 2.23±0.0195 2.73±0.0213 2.75±0.0217 2.09±0.0189 2.63±0.0212 2.67±0.0214 2.49±0.0206 2.22±0.0195 2.27±0.0197 1.95±0.0183 by alternating F,\(1790A) include 79±0.0219 76±0.0210 77±0.0218 units one, the emission-line AGNs. in through to spectral I in the C of and units perform components The 2%-4.5% of in II § and uncertainty 10- 2 Al335, NASA the the V, uncertainty and 2.61±0.0151 2.58±0.0150 2.49±0.0148 2.58±0.0150 2.01±0.0131 2.06±0.0132 2.32±0.0143 2.13±0.0137 2.08±0.0133 1.93±0.0130 2.20±0.0139 1.83±0.0127 2.17±0.0134 2.19±0.0139 2.37±0.0144 2.52±0.0149 2.57±0.0150 2.16±0.0133 2.17±0.0138 2.41±0.0145 1.93±0.0131 2.42±0.0146 2.39±0.0145 2.38±0.0144 2.21±0.0139 2.35±0.0144 2.19±0.0139 2.12±0.0136 2.20±0.0139 2.16±0.0131 2.13±0.0137 2.08±0.0135 2.19±0.0138 1.84±0.0127 1.70±0.0122 1.94±0.0130 1.75±0.0124 1.81±0.0126 1.61±0.0119 VIII. F,\(2030A) of includes 14 iterations the fitting ergs contributions continuum i.e., algorithm, 10- a Appendices levels fit. N light multidimensional s- 5.2.2. by Astrophysics 14 1 IV] in was cm- whose The ergs a using curves 2.40±0.0125 2.31±0.0123 2.26±0.0121 2.37±0.0124 2.18±0.0119 Figure 2.17±0.0119 2.33±0.0123 2.37±0.0124 2.10±0.0117 1.78±0.0108 1.70±0.0105 1.82±0.0109 1.86±0.0107 1.90±0.0108 1.92±0.0112 1.89±0.0106 1.99±0.0114 2.13±0.0118 2.16±0.0119 1.96±0.0109 1.98±0.0114 2.13±0.0118 2.05±0.0115 2.11±0.0117 2.04±0.0115 1.99±0.0114 1.94±0.0112 1.94±0.0112 1.97±0.0106 1.94±0.0112 1.95±0.0107 1.94±0.0112 1.93±0.0112 1.66±0.0104 1.56.-1:0.0101 1.72±0.0106 1.63±0.0103 1.80±0.0108 1.62±0.0103 of F,\(2195A) for contribution in Al486, 2 done Spectral ,.\- a s- weakest the placement. with most Simplex combined the 1 1 from • C in 9. cm- emission-line in and N IRAF the Figure observations. Fitting much 2 III] the emission • Data D. algorithm x errors We from 2 Al task The systematic amplitude These 8, minimization the 750, plot and the System SPECFIT uncertainty properly same flux lines the Al are additional the All statistical and is III strong is C errors values way the (i.e., a AA1855, likely IV Leven­ propa­ (Kriss utiliz­ statis­ emis­ as does and 0 dis­ un­ are 301 in to I 1995ApJS...97..285K minus FIG. 2,440,000. 6.-Six © 6 4 4 5 3 2 2 5 3 6 2 4 3 5 6 FOS American 'A.1350 II ::c I continuum 9100 9100 9100 A.1460 A.1145 :::E = 1 ;;[I I:r: = I rrr :r: I~III I }pr :r: :r: :r: light :r: I Astronomical 9110 9110 9110 'I. :r: I = II TI curves, 'I. I I ~rr1-o:II :I?= ::r:rIII :i:= as 9120 9120 9120 Il I given I 'I. I I rIIr :r=z. IJT I in Society :r: f :::i:c Table I II 9130 9130 9130 :r: rJ III I:r: :r: Ir 12. = II I~ ::c :r:::r:: • The = I Provided ordinate 2.5 2.5 2.5 3.5 1.5 1.5 1.5 3 2 2 3 2 3 4 1 1 has by units = ::c 9100 9100 9100 A.2195 A.2030 A.1790 = = = ::c = =s:: :CS: the = of ::c ::c :r: = 10- ::c ::i!=- = ~::c NASA = = 14 :::i::: :r::r: 9110 9110 9110 ergs = ~ 'I. ::i::::::i::i:.: 'I. 'I. s- 'I. Astrophysics ~ ~ z.r:i:e= 1 cm- 9120 9120 9120 2 A- ::c 'I. :::i::: ::c 'I. r:::i::: :::C-= z.F 1 , = and :::i::: ::c 'I. ::c 'I. the ::c ~ 9130 9130 9130 = ::c Data :::i;,.c= ::c 'I. abscissa ::i:c: :r;:r::r: ::c = = =s: :::i::: System ::c ::c shows Julian Date 1995ApJS...97..285K 1863, tinua, widths straddling fixed dling ent The tions that tures was regarding red were same Gaussians, and of example, occurring lines Lya We mined nique wavelengths profile. Si with The FIG. He III] wing within found forced C broader Xl216, these single to were modeled absorbed (LSFs; the and as employed II IV) along were 7.-Mean one >..1893, from N v N those (RW). were that these the the emission between various were the required to that described spectra Gaussians, important was © NV allowed were intrinsic with Evans widths emission of values spectral the be tied Also absorption with continuum American and modeled the FOS the forced that >..1240, here forced mean weak shown the two to lines were the weaker to C derived narrow to C 1993), of determined by lines. those fitting technique. and blueshifted .. :f< i' i' IV I aforementioned ..... 0 ~ continuum vary. III] ... "" difference Q) be s Ill Ill Cl to while the G C Si narrow, to is emission-line spectrum. with to fitted profile. have 130H IV constrained the that 25 II 20 15 10 plus be broad >..1909) determined 5 components be and from component), We Astronomical and >..1549, the designated identical Gaussians, employed a fitted. piecewise, all and assumed broad, their fixed Fe from stronger See the and absorption lines in windows 1500 emission were Galactic II He profile, G the fit Paper very features) Simple profile equivalent 190H the (but by He and II emission-line to for spectral of that modeled and in >..1640, II+ various emission the and fit BROAD-LINE marking the broad very C not (see§ V components blended Papers line-spread to which absorption the mean 0 IV, power-law their for Society their individual were necessarily the III] 1550 broad 0 their components intrinsic more widths 5.2.1) strad­ fitting means. the (Lya, region, with III] equivalent mean I was lines spectrum. flux modeled emission and divisions compo- widths. central >..1663, details deter­ func­ Observed three tech­ • pres­ ratio were N (i.e., lines con­ and C V fea­ For the fits Provided REGION IV v, is the 1600 of the interpolated Wavelength profile that three was bination spirit Gaussian emission-line contributions data emission This lines the method the the wings, pretation pendent: plates, shape served spectral above, ering FOS separately: nents, The IN continua very by entire adopted. spectra method components: we we and pieces of AGNs. in the mean which data in 1650 were linear the overlapped modeling over ends this have our ascribe continuum, lines (A) components the at our wavelength "remove" uncertainties 1155-1380 points NASA have for a continuum FOS lay fit fitted the forces long-standing The were of ability simple (e.g., wings VIII. minimum obtained, and are each the well blue direct their no spectrum is remaining continuum within then not simultaneously power-law, the spectra left everywhere. 1700 wing below and Astrophysics absorption of to physical parameterization Fe range comprising greatest running integration well continua A, the for applied "deblend" a in II (BW), in in the simple the future 1475-1760 (where was pseudo-continuum). individual spectra. constrained the papers philosophy in the advantages continuum through were amplitudes). significance the observed accretion blue fitted as strengths features. to various The work. an 1750 piecewise spectra, initial the are describing go core weakly fitted in individual first the Data through twofold, systematic continuum A, three of (BC), by pixel of two of disk, guesses possible simultaneously to windows. More their and of the this these keeping to blended derive The continuum fitting System red spectral values, the the Balmer resulting the We or spectral 1740-2030 but profiles emission emission-line core sophisticated data, Thus, to errors near monitoring very continuum fitting emphasize individual model-de­ procedure level When fitting the (RC), emission except windows consid­ regions recom­ the in fitting stated broad in fits inter­ tem­ line. over and ob­ the 303 and the the the A. to at 1995ApJS...97..285K said emission and line ing They to Xl909 which summed emission-line the blended (Lya, 0 meaningful these 01v] 304 III] show the profile two of (2) merely lines, blend >..1402 includes C +Sim] two emission-line the emission two IV strongest emission lying classes in © and no light curve. comparison is represent complex. emission order features. sufficiently Xl893). atop American a such its small of of from emission profile much to He attempt severely fluxes measure contribution a We While lines Notice We II+ the convenient between well stronger present components), when C also 0 Astronomical lines, was blended of every III] III]. separated that the comparable present Julian (2440000+) they the >.. made 9132.95 9131.88 9130.94 9126.93 9135.09 9133.76 9123.98 9129.94 9118.95 9122.97 9124.92 9121.97 9129.00 9120.96 9119.96 9117.88 9127.93 9125.92 9116.95 9116.01 9115.00 •Rest-frame 9114.00 9113.00 9111.99 9110.99 9110.05 9108.98 9107.98 9106.97 9106.03 9105.03 9104.03 9103.09 9102.02 9101.02 9100.01 9099.01 9098.07 9097.00 here Although emission 1909 least effort line from way in two Date emission are this the flux. for the + of from affected was Al methods and measuring Si 453.±2.89 480.±2.97 467.±2.97 462.±3.01 465.±3.06 445.±3.02 462.±3.07 471.±2.96 480.±5.96 461.±3.05 457.±2.97 458.±2.99 443.±2.85 459.±2.92 433.±4.18 465.±3.05 434.±2.92 419.±2.79 393.±2.79 399.±2.70 387.±2.76 394.±2.81 382.±2.82 394.±2.77 399.±2.76 429.±3.88 408.±2.72 388.±2.72 385.±2.68 363.±2.66 370.±2.66 368.±2.65 342.±4.59 322.±2.46 333.±2.49 353.±2.56 332.±2.44 325.±3.94 326.±2.44 parameterizing results the case (Direct) fitted III (e.g., weak, This fluxes III] flux madetodeblend Society C also >.. lines: Lycr Si 1859, IV the >.. by fluxes may N v N (e.g., of in IV 189 >.1216 the of that to 862.±13.9 808.±15.3 834.±43.5 819.±19.0 805.±18.4 821.±15.2 834.±28.5 830.±39.5 804.±16.9 810.±17.3 749.±22.8 678.±22.2 795.±20.9 796.±18.5 736.±21.9 784.±26.9 688.±20.3 792.±29.5 759.±28.2 798.±16.7 766.±22.2 735.±15.4 666.±19.9 672.±19.9 686.±18.3 739.±21.6 702.±17.0 658.±15.0 660.±16.5 609.±30.4 618.±15.2 657.±23.9 630.±25.3 623.±17.l 536.±16.5 592.±17.7 553.±14.6 562.±17.2 534.±15.0 units the blue-side ( 1 ) FOS the blending >..1400 measur­ 3 derive in (Fit) >.. He also KORISTA blend, of 1240) C of fits order weak same • of STRONG II+ the III] the the Provided 10- be to + a 741.±2.34 718.±2.31 706.±2.26 720.±2.29 689.±2.31 673.±2.32 724.±2.47 728.±3.64 740.±2.46 683.±2.27 725.±2.34 724.±2.40 732.±2.39 739.±2.41 735.±2.42 730.±2.47 719.±2.46 704.±2.43 670.±2.26 669.±2.30 717.±2.73 709.±2.74 701.±2.35 670.±2.34 659.±2.36 658.±2.35 657.±2.33 TABLE 654.±2.29 652.±2.27 633.±2.27 612.±2.26 612.±2.24 598.±3.16 564.±2.10 572.±2.16 569.±2.10 558.±2.72 554.±2.03 541.±2.04 (Direct) 14 ergs EMISSION C IV ET s- the tent the pose significantly for curve. lated ted these "Ly "Lya sum for feature continuum responding 13 ).1549 1 774.±5.13 755.±4.54 742.±6.59 757.±5.02 760.±4.16 760.±4.43 769.±5.14 771.±5.43 750.±4.72 729.±4.58 757.±5.12 754.±5.04 768.±4.95 740.±5.26 754.±5.02 698.±5.70 720.±4.96 698.±4.96 743.±4.91 739.±6.08 734.±5.05 719.±5.04 703.±5.24 699.±5.20 688.±4.62 685.±4.50 687.±4.63 689.±4.92 684.±4.73 658.±4.48 644.±4.34 642.±5.60 614.±7.60 598.±5.15 596.±4.39 573.±5.50 600.±4.53 568.±4.29 579.±4.33 The cm- significant C by the fit emission-line AL. a (Fit) with, of of fitted IV LINES" core") emission total" 2 to In fluxes • the total differed comparison, the components the contrast but emission-line 143.±1.16 143.±1.12 144.±1.14 136.±1.27 135.±1.19 138.±1.15 137.±1.19 143.±1.24 140.±1.26 141.±1.28 136.±1.20 137.±1.27 137.±1.26 141.±1.15 138.±1.22 132.±1.22 127.±1.19 131.±1.16 133.±1.25 121.±1.13 126.±1.18 126.±1.15 122.±1.17 121.±1.21 118.±1.22 123.±1.22 128.±1.20 119.±1.17 120.±1.15 116.±1.17 118.±1.18 119.±1.16 114.±1.15 109.±1.11 109.±1.07 111.±1.08 113.±1.08 114.±1.05 C 116.±1.03 direct-integration window Gaussian (Direct) NASA N v N in did Lya 111] derived from intrinsic noisier lines. Fig. >.1909 from not emission fluxes emission to its 8 include + the used plotted Astrophysics from in that In than, ), 141.±1.46 139.±1.40 142.±1.49 145.±1.48 135.±1.68 137.±1.54 134.±1.54 138.±1.63 136.±1.42 138.±1.64 137.±1.52 140.±1.61 136.±1.53 140.±1.72 137.±1.67 128.±1.56 132.±1.53 131.±1.50 130.±1.43 121.±1.45 126.±1.71 124.±1.49 121.±1.43 124.±1.64 119.±1.47 125.±1.63 123.±1.53 119.±1.66 119.±1.50 122.±1.54 117.±1.52 119.±1.57 117.±1.43 112.±1.40 111.±1.34 115.±1.28 117.±1.24 115.±1.29 115.±1.17 components Si Lya corresponding the are 111] (Fit) Figure sum Figure component for used the line >.1893 the absorption line, the direct the on of interpolation values fits in gave direct total 9 top the 8 wings because we the are we integration fitted of which results fluxes, whose show in direct show tabulated integration. the and Data in direct-integration Tables components it its corresponding did have the under the which was integrated integration. light core. System not of fitted fitted next 13-15. the been curve Lya We the For were compensate only to results flux note emission (labeled (labeled fitted the over differed the The consis­ Vol. direct tabu­ light only pur­ that cor­ the fit­ of to 97 1995ApJS...97..285K No. blue-wing but of emission-line core integrations. identical. they tends tually tion removed nents had proximately fitted -25% Julian (2440000+) Finally, 9132.95 9131.88 9129.94 9129.00 9126.93 9124.92 9123.98 9122.97 9121.97 9116.95 9133.76 9130.94 9135.09 •Rest-frame 9127.93 9125.92 9120.96 9119.96 9118.95 9117.88 9116.01 9115.00 9114.00 9113.00 9111.99 9110.99 9110.05 9108.98 9107.98 9098.07 9106.97 9102.02 9101.02 9100.01 9106.03 9105.03 9103.09 9104.03 9097.00 9099.01 Galactic otherwise 2, roughly of accounts constituted total to are Date identical, 1995 of Lya. higher a easily the based measurements Lya small 98.7±1.85 84.4±1.62 88.2±1.68 85.0±1.64 82.0±1.59 95.4±1.65 80.7±1.64 85.4±2.54 90.9±1.77 90.4±1.73 96.4±1.78 92.6±1.88 95.2±1.87 97.0±1.85 94.0±2.36 74.4±1.52 88.5±1.72 80.0±1.76 83.9±1.73 80.9±1.65 83.7±1.69 79.3±1.62 76.2±1.66 74.1±1.58 78.3±1.69 78.0±1.76 100.±3.50 101.±1.88 Nv 77.6±1.64 60.8±1.44 62.1±1.49 66.2±1.51 73.7±1.67 78.5±1.58 73.5±1.68 72.2±2.96 57.8±1.40 71.6±2.45 75.7±1.66 © absorption. (Direct) constant 0.8 The In fluxes the measurements directly for .H240 American flux. radial this and understood. from upon A). amount two the two in FOS We case, the Si units Together velocity separate differences equivalent -2% light IV these measured WEAK note small The .U400 of of the arise TABLE 86.2±1.46 86.0±1.49 89.3±1.58 85.7±1.60 92.7±1.49 87.2±1.68 82.9±1.66 84.0±1.65 90.2±1.44 91.0±2.80 90.0±1.56 93.0±1.68 90.2±1.65 79.9±1.51 80.7±2.09 82.7±1.49 80.1±1.47 77.4±1.39 79.0±1.96 76.9±1.51 76.6±1.46 76.6±1.53 56.4±1.36 77.1±1.49 62.4±1.35 2814 72.0±1.27 62.8±1.43 79.8±1.54 69.4±1.51 74.7±1.58 75.4±1.58 67.0±1.50 74.4±1.55 69.4±1.49 77.3±1.50 74.1±1.48 73.4±2.54 59.1±1.27 56.4±1.30 59.3±2.01 (Direct) curves 10- to Astronomical possible fits, The EMISSION here intrinsic + tabulated absorbed and differences red-core 14 -10% 0 with because ergs IV) the there. widths core differences that 14 corrects for Al402 s- intrinsic contaminating the LINES" 1 of the the flux absorption cm- line measurements In here, the (that the Galactic 94.8±1.32 86.7±1.30 87.1±1.27 80.2±1.23 93.7±1.32 94.8±1.39 98.9±1.41 89.1±1.37 89.2±1.33 99.7±1.40 98.4±1.48 99.4±1.46 91.5±1.36 92.2±1.42 90.9±1.38 91.9±1.35 103.±1.42 107.±1.48 106.±1.50 105.±1.51 106.±1.50 89.5±1.40 88.6±1.35 82.0±1.36 93.6±1.37 98.0±1.42 91.9±1.43 90.5±1.42 91.8±1.34 108.±1.45 82.3±1.34 59.3±1.16 65.4±1.21 65.9±1.20 66.0±1.20 90.8±1.37 78.3±1.34 63.0±1.13 He in intrinsic (Direct) red BROAD-LINE the 2 for and • II flux the fitted flux between Al640 absorption with wing Society a of red small other -15% amounted C in + wing absorption, in version absorption the IV any are 99.8±3.63 97.3±3.54 91.4±3.15 108.±4.22 117.±3.85 120.±5.25 105.±3.62 108.±3.86 118.±5.05 114.±3.71 120.±3.77 122.±3.40 118.±3.85 124.±4.24 116.±4.38 114.±4.10 108.±4.24 106.±4.25 107.±4.07 83.3±4.34 88.9±4.98 93.2±4.15 102.±3.93 102.±4.33 107.±3.96 109.±4.71 111.±4.04 102.±4.82 107.±4.12 104.±3.61 68.7±3.27 92.4±3.44 76.0±4.21 78.4±3.22 105.±4.08 101.±4.93 107.±3.96 70.8±2.96 78.2±4.03 0 emission, the m) amount (Fit) compo­ the was are excep­ nearly of the of Al663 • lines blue two vir­ ap­ the the ex­ REGION Provided to fit fluxes, direct exception listed the these the respectively. ter. were (-2 surements signal-to-noise error are campaign correlated distributions. imately The lowing is increased were evaluated. peaking bars stances and explained ably detailed For tral raneous, pairs broader, N and Gaussians C difference The in gions tegration mean were window. (F~), based spectral niques ( SWP IN apparently The The IV Before wavelength v by the SWP fitted We resolution. a x a Gaussian were NEWSIPS weakest V, left emission correlated regions for bars of AGNs. tables in based measured were upon measurement) integration, error FOS SWP the correct discussed the quantity where 2 found SWP the Tables x analyses near unchanged. analysis the the fitting, 5.3. Continuum making measurement 40 scaled fluxes 2 by on for technique in of in are whose , direct-integration not pixels, full and upon NASA but bars the spectrum. continuum a The well-measured median lines A detail the the subtracted fitting much C VIII. spectra 1, the those The The that factor so line, size. errors available IUE The 16 IV error Unlike continuum are by figures if their with SWP using results was SWP on of above. as and has v N measurements, Julian SWP fixed the and by were the IUE -1.6. the the described actual We in the whose direct to weaker the not at the spectra Astrophysics equal shown Shull found: were value bars applied this was peaks approximately value windows ;\.1240 spectrum error produce Paper pixel absorption the the 17 square fitting and intrinsic the widths the found SWP of Emission-line SWP omitted by SWP well for The Dates and a and Next, computed. integrations should start on the direct-integration not position constant to flux fitted this & case of FOS than a derived values that bars and were values). windows (FsWP constrained major V. emission-line measurements Spectral Sachs linear measurements the fluxes procedure the are root above; spectra their to the fit available. corresponded associated alignment ratio, of on in measurements absorption As the from observations was each thus that measurements square on the to plotted pixel generally the the look ratio Paper of were lines both distributions ( - is interpolation. difference in which in the value the 1993), measurement SWP the After fitted, The a found in two exposure. based NEWSIPS show Data Measurements was or FFOs) SWP were and Paper of the values distribution like (FOS found mean minimized root sides measured the median V, Instead, held in were the in with with measurement neighboring spectra that, temporarily in nearest were measurements greater to Figures continuum contemporaneous but considerable 2 with in upon a the used. were spectra are System case of /(u'§wP to C and V, were continuum fixed of later measurement)/ were, in to x FOS the the the modeled III] the we reported the as We only, 2 relatively the derived used these value were the pixel be components in evaluated distribution fitting were of a continuum The in 1988-1989 peak contempo­ SWP flux defer and work. than number during error 10 IUE of the present spectrum. too smoothed the therefore, statistical direct-in­ was + the with Papers approx­ because is and the two of scaling shifted Lya pixels. values u~os). effects small, major 20 fluxes of prob­ unity more error mea­ from spec­ tech­ their scat­ v N with here bars that flux low 305 fol­ the are the the 11, in­ re­ in of as + I 1995ApJS...97..285K tures feature and curves confirming dence ing cussed through panel power-law band, SWP somewhat fluxes, of ofFigure note 306 In Figure some FOS its that continuum often as in of and are dispersion above. of expected. many these Figure of 5. continuum in accounted the continuum better present their cosmic The © the 10 most measurements. continuum American of we Most closest localized IO reality. windows: than determined the We overplot in rays cases we Julian (2440000+) light for the of •Rest-frame 9125.92 9129.00 9131.88 data 9133.76 9132.95 9135.09 9120.96 9129.94 9127.93 9126.93 9124.92 9123.98 9121.97 9130.94 9116.95 9116.01 9119.96 9118.95 9117.88 9122.97 9110.99 9114.00 9113.00 9115.00 9111.99 9106.03 9108.98 9107.98 9106.97 9110.05 9103.09 9102.02 9101.02 9105.03 9100.01 9104.03 9099.01 9098.07 9097.00 note show fit match Figure prevalent In the the in SWP usually artifacts, Date the curves. variability 1350, that points in the Astronomical the fitted differences occurs The lower from heavy 5 spectra 94.0±0.993 98.3±0.985 117.±1.13 122.±1.15 122.±1.17 119.±1.17 121.±1.19 119.±1.12 118.±1.91 the 122.±1.11 ratios 119.±1.08 118.±1.10 118.±1.06 114.±1.19 119.±1.39 118.±1.21 118.±1.21 114.±1.20 118.±1.12 118.±1.11 121.±1.41 114.±1.13 119.±1.14 112.±1.09 113.±1.11 108.±1.13 110.±1.16 97.3±1.06 99.3±1.10 107.±1.11 105.±1.13 107.±1.11 107.±1.15 110.±1.10 98.7±1.02 97.8±1.03 96.0±1.43 102.±1.72 104.±1.10 median (Direct) fluxes would 1460, fell with which SWP Note power-law localized 1460 the right-hand in symbols Blue beneath given of in this within the and error-bar recorded indicate units flux the Wing A the between lay 127.±0.851 134.±0.730 134.±0.862 130.±0.762 131.±0.880 130.±0.882 132.±0.879 127.±0.849 128.±0.853 128.±0.910 126.±0.791 131.±0.869 130.±0.895 130.±0.917 129.±0.782 126.±0.792 129.±0.894 130.±0.912 126.±0.938 123.±0.828 119.±0.886 116.±0.784 118.±0.778 124.±0.883 122.±0.847 118.±0.841 118.±0.802 112.±0.755 110.±0.832 110.±0.940 109.±0.800 110.±0.822 105.±0.789 129.±1.15 132.±1.09 123.±1.01 112.±1.39 115.±1.00 107.±1.02 1350 light SWP 1790 or (Fit) close within HST of abnormally ratio the this the Society continua from comer 10- A curves data A. analysis because every correspond­ artifact continuum continuum 14 these FFosl correspon­ campaign, FOS 228.±1.22 3.20 240.±2.13 236.±2.03 232.±1.21 3.12 257.±1.66 236.±1.22 231.±1.21 237.±1.23 229.±1.19 234.±1.19 2.11 255.±1.70 245.±1.14 229.±1.18 256.±1.70 228.±1.18 2.11 26±.5 238.±1.12 246.±1.75 225.±1.16 228.±1.22 2.14 245.±1.63 228.±1.42 3.12 26±.4 246.±1.18 253.±1.59 233.±1.23 256.±1.54 248.±1.18 232.±1.23 253.±1.58 229.±1.23 220.±1.18 210.±1.13 1.11 240.±1.66 218.±1.16 215.±1.14 213.±1.16 2.14 242.±1.99 223.±1.42 207.±1.16 0.11 29±.3 2.11 229.±1.63 224.±1.11 229.±1.63 207.±1.15 208.±1.16 210.±1.16 203.±1.13 208.±1.16 204.±1.14 199.±1.13 ergs 191.±1. 193.±1.12 192.±1.11 178.±1.06 181.±1.08 182.±1.07 175.±1.04 177.±1.46 184.±1.06 the a (Direct) set. perusal of KO match major C s- three went • Fswr each Blue light IV 1 fea­ 72 dis­ low We the RIST cm- Provided A TABLE Core 1549 252.±1.68 254.±1.39 250.±1.46 252.±1.71 258.±1.71 4.15 241.±1.17 245.±1.54 262.±1.75 266.±1.87 4.17 229.±1.10 243.±1.70 246.±1.70 231.±1.89 3.17 224.±1.11 235.±1.75 230.±1.55 227.±1.52 2.14 221.±1.12 227.±1.49 233.±1.73 224.±1.54 229.±1.63 216.±1.47 212.±1.43 213.±1.86 197.±2.44 203.±1.49 197.±1.49 195.±1.68 8.17 185.±1.39 183.±1.76 203.±1.51 191.±1.45 2 • (Fit) A COMPONENTS" ET errors tween illustrate indicative He points such 15 spectral and cases, in mean window. ual priate upon spectra many Taken Figures 180.±0.981 179.±0.986 247.±1.18 244.±1.91 4.11 249.±1.37 246.±1.16 249.±1.17 246.±1.17 251.±1.18 5.11 254.±1.72 250.±1.16 252.±1.16 244.±1.14 243.±1.36 239.±1.15 249.±1.19 232.±1.11 242.±1.37 226.±1.09 219.±1.12 223.±1.12 223.±1.12 222.±1.11 218.±1.09 205.±1.08 207.±1.08 204.±1.07 190.±1.02 9.10 197.±1.69 193.±1.04 AL. 196.±1.60 187.±1.01 by II SWP (Direct) SWP outlier, visual + there instrumental present instances the (i.e., shown. the with Red 0 comparisons In ( in spectra FOS of I light III] IO is ) fitted) combination, Core Figure NASA inspection the 250.±1.67 250.±1.68 247.±2.20 252.±1.63 250.±1.46 254.±1.70 254.±1.79 256.±1.70 247.±1.65 243.±1.73 236.±1.6:1. 243.±1.53 248.±1.65 242.±1.67 246.±2.03 249.±1.50 the 234.±1.64 228.±1.70 230.±1.87 223.±1.49 227.±1.69 226.±1.48 228.±1.53 227.±1.61 224.±1.54 210.±1.41 207.±1.80 200.±2.46 195.±1.47 190.±1.40 182.±1.37 186.±1.79 182.±1.38 210±1.43 a suspected in JD and The light correspondence (Fit) and where curves quality this mean before 2,449,071, FOS 11 11 scatter differences. SWP curve SWP Astrophysics we shown the 132.±1.27 131.±1.26 127.±1.20 127.±1.20 134.±1.21 128.±1.18 125.±1.16 130.±1.35 132.±1.27 139.±1.29 132.±1.30 130.±1.31 128.±1.31 121.±1.28 are 127.±1.30 123.±1.23 124.±1.28 128.±1.31 121.±1.19 122.±1.23 122.±1.20 122.±1.21 122.±1.27 128.±1.26 125.±1.23 122.±1.26 120.±1.24 121.±1.22 122.±1.21 120.±1.22 98.3±1.10 99.6±1.14 114.±1.21 113.±1.20 109.±1.24 91.1±1.04 92.2±1.06 100.±1.14 103.±1.11 instrumental of and (Direct) emission-line of problems. overplot the and and differences Figures data noted this in in Red the measurements in the Figure (2) comparison falls portion set. Many Wing between 122.±0.812 128.±0.851 125.±0.837 124.±0.680 120.±0.818 124.±0.829 123.±0.874 117.±0.776 125.±0.809 129.±0.753 122.±0.816 121.±0.853 120.±0.754 115.±0.718 119.±0.718 114.±0.794 114.±0.851 114.±0.928 115.±0.791 117.±0.966 115.±0.788 116.±0.776 116.±0.826 115.±0.753 114.±0.764 117.±0.830 120.±0.894 115.±0.791 97.7±0.842 99.3±0.749 97.6±0.937 114.±0.774 84.2±0.629 89.1±0.672 94.3±0.695 111.±0.742 108.±0.937 differences 125.±1.12 Figure 106.±1.30 in C the in 5, (Fit) They off III] § differences heavy IO, cannot 11, amplitude of measurements. 3.3 Data of the + 5. the and the lying the were and Si However, among symbols differences plot single-day seen be III] 11 were System SWP in well noted due quantitatively remaining of light of in Table the spectra. made. systematic the entirely above the the there In curve individ­ as outliers in appro­ 2A mean some SWP such FOS One the be­ are as to is 1995ApJS...97..285K multicomponent FIG. 8.-FOS 1.4 1.6 1.2 1.8 © 8 5 6 7 4 6 9 8 1 fit. American direct-integration The =:r=- :S:=snI Ir ===r=""z 9100 9100 9100 C Lycx C Lycx = fluxes I II III] IV r1 :c have I=s:II """""' = ~rriifI total core Astronomical I + ~ -==-=="""' 9110 9110 9110 emission-light units I Si. ?I :==;= of III] II Jr = 10- =="" I I ~ III ==~ I 12 9120 9120 9120 I = = II ergs ~~~=== + curves, 1 I I1 =~:c==~ IE Al Society s- :i; rI == 1 nP:~r cm- as III :S:r 9130 9130 9130 given 2 ; the rII 1 • I n in abscissa Provided I = =: Tables shows 0.6 0.8 0.5 0.6 0.8 0.9 0.6 0.7 0.7 0.8 0.9 1.2 13 1.1 1 1 1 and Julian by 14. 1r1 I f 9100 9100 9100 He Si NV I the III III I Date The I I IV I I I II 1 NASA f I light minus JI I 1 IIIIII + rr + IlIJ: curve 9110 9110 9110 2,440,000. I 0 0 Ji:rl!J: Astrophysics !fa I I designated IV] III] II JI::crI I 9120 9120 9120 I I Ir II r1r IlI "Lya II I 1 III Irr IIIl total" II I Data 9130 9130 9130 JI I II IEI t~ I I II was I :n: System I I derived from the 1995ApJS...97..285K continue as The We year multicomponent nents, frame given All tegrated the tometric was reported cifically, checked X5007 the program. spectra assumed light-travel recombination 308 7" described FIG. The a - ~ heavy observed-frame also flux measurements used O.B 2.5 1.2 1.4 1.5 1.5 1.2 1.4 1 as 9095 9095 9095 2 in data, ofNGC flux 9.-FOS 5.4. absolute L.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL-'--' L.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL.LL-'--' ~--~~~~~~-----~~~~~~~ ~~~~~~~~~~~~~~~~~~~~~ given that by Table give when in of [O quality symbols to (to to ::t:ii: This in is C measuring Paper time but the © 9100 9100 9100 9100 %:i:"'% use Absolute be the in III] reduce about IV were z the J: fits, the American Table 5548, 18, emission-line time constant is text. the Red [Om] the calibration show and across X5007 f"' mean VII a and 9105 9105 9105 9105 :cisz=:zZ observing along obtained difference 5% Wing here absolute well-founded fluxes the exceed 15. ::cI:c:c:::CI~I:C::C:i:::c:c:::C::Ciz for whose the Calibration and the the X5007 lower the The values importance fluxes 9110 9110 9110 which sum 9110 with over light have flux earlier are narrow-line light abscissa I of redshift Astronomical conditions of 00 under flux than symbols is Z::z::::z::z::C:Z:::cz::z:: the narrow the in lower 9115 9115 measured 9115 9115 the the a measured been not curves years. the fairly references. of given mean assumption, emission-line duration the is optical statistically suitable the is of Julian [ are 9120 9120 9120 by 9120 transformed 0 value of emission This taken large seeing Optical region appeared III] in for for a the ::c:rI::cz:c:i:::c:c:r:~::c:c in in z Date factor Paper spectra the 9125 9125 X5007 ::z::Z assumption 9125 9125 the of obtained previous entrance C The to conditions-spe­ such effects). J: direct components Society IV the (NLR) significant. :Z::;i;:::C::C= minus be since year Spectra line, year II profile of to 9130 9130 9130 9130 line z is monitoring to spectra integrations, [F([O be (I = 5 based 2,440,000. from both years, as years, which aperture 5 [ the in spectra. 0.0174; and The =z= of compo­ + can KORISTA 9135 9135 9135 9135 0 those • in pho­ z) rest We III] the III] the the are in­ the Provided on be 2 is • ET of gest grouped of though trum the HfJ listed Dates X5007) uum While Continuum variability the by AL. measurements emission-line that and in in associated exposure. the the = Table this the which s-1 by 5.6. HtJ 5.58 Julian (2440000+) increasing •Rest-frame NASA cm-2 9106.91 9104.91 9108.84 9110.84 9112.56 9122.84 9120.57 9118.55 9116.72 9114.72 9128.53 9126.82 9124.84 9128.87 9130.87 9094.93 9092.93 9088.63 9090.58 9084.80 9082.68 9081.41 9079.32 9096.93 9100.92 9102.93 9098.93 9134.50 9132.68 9086.59 9071.01 9069.00 9073.00 9074.99 9077.16 larger 9060.64 9067.00 9063.04 9065.01 5.5. value individual in · emission-line Intercalibration (at 3 both X these Date with ,.\-1. as Optical measurements 5100 10- data is for described SWP Astrophysics . too the 4.08±0.193 3.11±0.225 3.69±0.223 3.81±0.160 3.74±0.156 3.62±0.173 3.73±0.167 3.50±0.175 4.28±0.225 4.44±0.175 4.08±0.157 4.22±0.161 3.17±0.170 3.28±0.184 3.26±0.165 3.71±0.177 3.51±0.200 2.18±0.184 3.15±0.173 2.17±0.194 2.28±0.128 2.13±0.155 2.76±0.373 2.31±0.236 2.98±0.165 2.85±0.171 2.09±0.132 2.85±0.179 2.29±0.279 3.40±0.218 3.50±0.193 3.52±0.238 3.20±0.227 2.78±0.375 2.94±0.191 1.85±0.163 1.44±0.131 1.94±0.154 3.66±0.176 F>.(1350A) these features number 13 flux all sets A ergs continuum homogeneous CONTINUUM high Spectral 5 in densities, TABLE measurements years in fluxes the s- in by Table of appear of 3.52±0.0952 3. 3.51±0.0950 2. 2.11±0.0820 2.03±0.0938 2.01±0.0836 1.82±0.0932 1.42±0.0830 1 3.00±0.139 3.46±0.137 3.97±0.134 3.74±0.112 3.39±0.103 3.92±0.101 3.32±0.107 4.17±0.105 3.12±0.113 3.05±0.101 3.48±0.100 3.48±0.106 3.37±0.123 3.03±0.107 2.09±0.120 2.61±0.226 2.91±0.101 2.65±0.102 3.20±0.136 2.04±0.114 2.22±0.142 2.84±0.119 2.73±0.111 2.15±0.165 1.81±0.100 3.33±0.120 3.32±0.145 3.08±0.140 3.44±0.105 2.65±0.232 F>.{1460A) Papers rest 79±0.0936 77±0.0986 approximately cm- measurements the were on Measurements 16 in measured and BANDS" frame units 19 the same Optical 2 Data ] are made II data in reveal the of and 3.28±0.0713 3.12±0.0638 3.21±0.0627 3.54±0.0675 3.03±0.0640 2.96±0.0623 2.29±0.0629 2. 2. 2. 2.85±0.0603 2.59±0.0629 2.98±0.0682 2.89±0.0659 2.96±0.0615 2.86±0.0678 2.89±0.0682 2.92±0.0642 2.02±0.0960 2.34±0.0619 2.22±0.0598 1.90±0.0594 1.73±0.0729 2.92±0.0807 2.85±0.0993 2. 2.61±0.0776 2.43±0.0657 1.72±0.0508 1.82±0.0573 1.83±0.0633 1.37±0.0500 1.54±0.0591 1.72±0.0715 1. 2.93±0.0521 2. are 2.28±0.110 order 2.37±0.110 F>.(1790A) listed ofNGC 73±0.0711 75±0.0669 72±0.0729 79±0.0584 73±0.0804 77±0.0687 10- HfJ System Spectra sets. from those from similar III. flux 14 2%. emission ergs begins to in The The the scale, keep at each 5548) Table patterns the contin­ spectra Vol. to Julian all spec­ even start line, sug­ and 19, 97 of 1995ApJS...97..285K equation agreement. determined correction dard AGN to this ments sampled surface factor effects, different the where offset No. a light series, common 2, and in continuum 'P F(H,8) from 1995 and brightness flux accounts amounts curves in apply factor we We time as © correction from the 0 attribute bs flux in corrections American define produced is two and our is source) one for oflight distribution the scale. in F(H,8) sets previous internally the another. a principle measured to point-source these We and fact that loss each from to = Astronomical the differences adopt the that ipF(H,8)obs, for are papers As Julian (2440000+) of of the very 9116.72 9120.57 9128.53 9122.84 9124.84 9128.87 9130.87 9126.82 9132.68 9134.50 a 9108.84 9110.84 9106.91 9114.72 9100.92 9112.56 9118.55 9104.91 •Rest-frame 9096.93 9094.93 9092.93 9088.63 9098.93 9102.93 9084.80 9086.59 9082.68 9081.41 9090.58 9065.01 9067.00 9079.32 9077.16 9074.99 9073.00 9071.01 9069.00 9063.04 9060.64 other the partially H,8 both described the function closely different individual Date set correction PSF homogeneous, flux data we sets the A, primarily 615.±15.8 627.±13.0 698.±22.0 635.±18.4 676.±17.6 639.±17.9 638.±21.2 661.±25.2 603.±17.4 729.±24.7 790.±22.3 692.±23.4 745.±18.1 773.±21.8 746.±31.9 726.±23.4 704.±16.6 418.±16.5 416.±18.8 529.±17.1 506.±16.3 556.±23.0 498.±15.9 499.±17.7 489.±14.4 566.±19.5 503.±21.2 610.±22.3 apply 417.±14.0 635.±24.9 641.±20.8 821.±21.4 729.±21.6 705.±22.0 708.±23.0 734.±17.0 765.±22.5 777.±30.l 786.±22.0 (which from spaced extended that broad which sets fluxes (Fit) BROAD-LINE of Lya apertures in seeing; earlier Society sets bring to an factor Table in lines describes in is adjust 85.6±6.78 59.1±5.74 65.2±6.14 64.2±6.10 50.8±5.44 66.7±5.98 67.3±6.50 63.9±5.97 68.4±7.12 65.8±6.11 62.6±6.11 64.2±6.51 78.1±6.19 75.5±7.12 65.2±6.38 78.7±6.32 71.5±6.43 44.6±5.06 41.6±5.50 35.4±5.73 51.5±5.68 74.1±6.03 45.2±5.09 50.1±6.10 33.0±4.05 32.5±4.24 32.8±4.53 29.4±4.53 47.1±8.83 42.8±4.64 50.5±6.56 66.3±6.24 68.6±6.08 66.9±6.74 51.0±11.8 75.4±7.89 70.6±6.27 95.9±5.68 74.2±6.43 empirically units to are (Direct) NLR. fairly time as measure­ Nv papers aperture since result 'P and 19. slightly a of by SWP them stan­ • 10-• into well The The (2) the the the no Provided Si1v+01v] REGION in in 89.8±9.37 85.8±8.26 68.7±8.58 58.8±7.90 61.4±9.45 64.4±8.44 9494 737.±16.8 69.4±9.48 54.7±9.10 74.7±9.50 91.0±10.3 97.7±11.1 48.8±8.10 85.6±13.2 82.4±14.8 33.8±8.20 58.0±8.86 79.7±12.7 70.7±8.67 77.3±8.95 43.3±8.42 113.±10.4 36.5±10.4 60.8±7.17 45.2±10.8 48.3±7.87 40.5±6.10 83.1±10.8 51.7±7.67 37.6±7.38 90.0±13.6 57.8±9.95 91.9±11.5 71.3±16.6 110.±24.5 102.±14.6 80.0±9.19 72.7±11.9 116.±26.2 112.±14.1 TABLE EMISSION 4 ergs (Fit) s- 1 the tures. attempt our line G 'P tercalibration we servations any if comparing days Determination sets. 17 cm- LINES• 657.±19.4 654.±19.0 695.±15.1 666.±14.5 670.±19.0 631.±20.0 690.±22.9 672.±30.2 608.±21.4 644.±27.5 689.±17.0 613.±21.0 758.±18.3 723.±18.6 756.±15.6 719.±18.7 758.±18.3 719.±18.4 415.±21.3 391.±22.0 567.±20.0 497.±16.7 576.±21.1 519.±23.8 506.±20.4 514.±17.1 623.±26.3 426.±13.6 578.±29.5 616.±24.6 670.±17.5 761.±19.7 by and 732.±26.3 715.±32.5 739.±20.4 753.±25.6 After we 702.±29.0 717.±14.8 IN can by different largest Ft (Fit) (Fit) 2 C1v ratio, real • tends the assume We AGNs. G the determine correcting is equation reflect variability define another from single made to Hen+ pairs 97.1±5.38 80.2±3.84 96.0±4.94 97.1±5.38 96.4±4.71 98.4±4.69 1.54 124.±3.49 116.±5.43 123.±5.24 116.±5.33 163.±5.43 126.±5.24 68.6±4.63 69.8±4.24 94.9±4.86 110.±4.71 140.±5.13 121.±5.08 125.±5.48 134.±4.82 124.±4.99 NASA 81.9±5.38 64.9±3.75 63.7±4.56 64.8±3.81 62.4±3.61 78.8±4.56 42.5±4.15 56.4±3.66 96.5±5.08 91.7±4.73 96.9±6.42 70.7±7.26 119.±5.67 193.±8.09 113.±7.06 112.±9.48 125.±4.44 120.±5.97 136.±5.13 Fx(5100 amounts that be process VIII. the of different for (but of Om] source to the the correction the for uncertainties nearly this correct that Astrophysics is that A)= errors Cm]+Sim] nominal constants of aperture 99.1±3.15 132.±3.29 139.±3.53 149.±3.40 147.±3.28 83.9±3.09 94.8±2.60 130.±3.04 112.±3.37 135.±3.71 137.±3.12 134.±3.72 122.±3.14 109.±3.16 118.±2.96 143.±3.26 69.1±2.67 120.±3.51 110.±3.01 124.±3.30 119.±3.51 66.5±2.62 104.±2.65 126.±2.68 144.±4.41 114.±3.03 125.±3.82 127.±5.71 115.±2.95 117.±4.64 139.±3.43 purpose 105.±4.54 153.±3.38 155.±3.99 122.±4.00 135.±3.55 142.±5.53 118.±2.17 not of data occurs starlight (Fit) simultaneous allows uncertainty. ipFx(5100 for completely) add needs sets. seeing uncertainties an effects on in 'P us in admitted The extended and the to to timescales quadrature. Data merge A)obs effects, be formal individual on G (to suppressed applied is the within - by source accomplished System the for this G. uncertainties PSF shorter different We different each to data is 2 correction to adjust by days) note probably data narrow sets, than the aper­ data that 309 (3) ob­ for in­ set by so in 2 · 1995ApJS...97..285K F(FOS)/ ble 310 The ner poraneous differences between errors dently of errors errors data continuum in large-aperture, viously, which starting sets; for fractional fractional of ually F(H/j) ': l ~ :::! " Ei FIG. In observations the 16, of u the abscissa 000 sets 3 3 3 2 2 4 4 2 these lL...l..-''-'-''-'-'....i....L....i....L...L...L-'--L-'--L..L..L"-1-L.'-L...l..-'-'--'--'-'....i....L--'--L...L...L...L...L-'--'-' 1~--'-'--'-'~~~~~~~~~--'-'--'-'~~~~~ 1'--'---'-'--'-'~~~~~~~~~~--'-'~~~~~ each practice, with building 9060 9060 9060 are continuum of are the i/F;1.(5100 from continuum I I I I F(SWP) >'1350 >..1460 A.1790 0.-SWP = with which are FOS closely I the I I taken the panel errors 0.036 smaller I errors I IrII is values 0.025 between and I © I well 9070 9070 Julian 9070 the FOS set and II I the II American is the we up high-quality separated to and Ir Ir continuum line, sampled F differences spaced SWP in the for continuum I largest for in are and be A)= Date sets believe I I I data and a 9080 9080 9080 intercalibration the both I I I median set closely the as large respectively, I I these I spectra. somewhat I I 0.050 dispersion, are minus the given Ir/ II are W pairs and H/j parameters. on by 0.025 9090 9090 9090 light were I I calibrated. H/j light homogenized are value I thus sets in spaced Astronomical data less short in line 2,440,000. IIi I in most of curves I= line, the 0.025 the curves too Netzer 9100 9100 of in ff can for 9100 than l~ found smaller observations. are sets timescales and the line. continuum similar /i each the respectively. conservative. r~f observations (light process Tr=l.r} be overplotted and adopted 2 distribution Fractional For A I In 9110 9110 et 9110 for days), to continuum For of ""I :i:i:I determined and the T0 I ratio ratio ratio than symbols), al. :c database 0.040, the be ~ set set data lower the ( is (i.e., 1990), 20 0.046 H, 9120 9120 9120 = = = Y B and Society those for .[± and carried (heavy The other 0.963±0.071 sets 0.963±0.061 pairs 1.022±0.087 ..I.c the the Similarly, of based again uncertainties right-hand within A several as the the the :c 'l..5007) ...... ················· ················· for Similarly, scale, as CALIBRATION x can 2 by differences value for flux, all determined and da~s possible, 7':5 from that optical which values measurement. V2, s-1) be each 223 Astrophysics them and the that fractional with data F(H/3), which these spectrograph of of constants or the accounted provides (as after ...... that, . . error the estimates measurements pairs if TABLE set 0.034 the for less. of the enters with fluxes the mean sets. described anything the CHECK are constants between 223 the of add on correcting in the quality corresponds from errors of The behavior the are measurements Most a known quoted average, adopted uncertainty Mean Mean Mean Mean n59243h n59240h n59212h n59183a n59182h n59176a n59166h n59163a n59091h continuum an observations 18 pairs uncertainties in H/j apertures given we given (adopted for For FOR can Optical given dispersion the estimate quadrature. entrance are have use below), line, of what of value value value value by Data are OPTICAL the be is FILENAME spectra, measurement and the for in the given for of slightly our the for 0.029, fractional in performed used the absolute continuum, been Photometry (2) from from from from the are Tables these spectra differences to of the flux, Table by differences each of quoted System quoted small aperture mean in in about SPECTRA in 5100 taken from different with years the measurements year year year but assuming conservative. differences more In slightly Table Table the same Fx flux) data 4-10 21. some typical systematic to 2 5 again I ( errors equations fractional 3-4 A errors other the by measure­ 5100 for to is those reliably contin­ we used among A 21 points. 19 set 0.030, exam­ be in lower mean sizes. show these cases with final find that that to sets A), un­ the are are are in­ in of in a 1995ApJS...97..285K fluxes symbols); FIG. have 11.-SWP tbe units 0. 1.5 fluxes © 4 5 6 4 8 1 8 6 of American 9060 9060 9060 .__.__.__...... __.___._....___..__._....__....._.__.__L...-L-_.__.__, emission-line 10- shown I 12 1 C Lycx I ergs 1 are II III] Ir s- based 9080 9080 9080 1 total r cm- light Astronomical rTJ_ + I I I on 2 curves ; Si tbe I tbe I abscissa I III] sum II 9100 9100 9100 (light I ~-JfFi of + I tbe is symbols), Julian Al Society fitted TT~ 9120 9120 9120 III Date components as I given I minus ~ • Provided in 2,440,000. Table for each 0.5 0.5 0.2 1.5 1. 17, 5 1 1 line 9060 9060 9060 with .---..---.--.---.--,.--.---r----..-...,---,--....-~--.--,--,,--, ~~~~~~~~~~~~ by lrII except He tbe NV 1 the I Irr corresponding I N II NASA 1 rI v, 9080 9080 9080 rI Irr + for I I which t1 0 I Si rJ~r Astrophysics I 11JrI III] FOS JV tbe 9100 9100 9100 emission direct-integration + ~T~I I I 0 light IV] 9120 9120 9120 Data curves rl\ results I System overplotted are shown. (heavy The 1995ApJS...97..285K 9014.05 9013.03 9012.03 9011.03 9010.04 9066.02 9065.01 9061.90 9045.96 9045.04 9036.00 9132.05 9094.57 8982.05 9029.95 9020.97 9013.94 9008.99 9000.02 9211.66 9205.68 9197.70 9190.65 9183.69 9176.69 9169.69 9163.69 9156.75 9149.74 9142.72 9135.76 9128.75 9122.84 9114.81 9107.82 9099.80 9090.85 9085.82 9079.85 9064.80 9062.87 9056.89 9048.94 9012.64 9004.65 9240.63 9164.37 9131.35 9101.42 8992.01 8981.03 8973.01 8967.00 8954.03 (2,440,000+) Julian (1) Date ...... ·········· ...... ·········· ...... ·········· ...... ·········· ...... ·········· ...... © American c10-•s B. Wise A. F. ergs FA(510(L.\) F. Ohio 11.61 11.44 10.32 10.32 10.10 10.49 12.05 10.10 12.78 13.28 11.05 11.10 11.33 10.49 10.16 10.21 SAO Observatory 8.48 9.88 7.64 7.76 7.98 7.98 9.49 8.26 8.31 8.09 8.54 8.70 8.48 9.77 7.92 7.81 9.21 9.49 9.21 9.49 9.88 9.21 9.49 9.26 9.49 9.71 9.82 8.09 8.03 8.54 8.09 8.98 8.15 8.54 8.59 8.59 7.81 7.48 (2) DAOCCD s-• Astronomical Society State cm- Reticon 2 CCD ,.\- 1 CCD ) (10-• 3 ergs F(HP) 8.59 8.93 8.82 8.87 9.21 9.15 7.87 8.59 8.37 8.31 8.31 8.15 8.70 6.81 6.86 7.59 7.53 7.92 7.92 7.25 8.26 8.15 8.31 9.26 7.81 7.98 7.81 7.53 7.20 8.37 8.26 8.31 8.37 8.03 8.03 8.09 8.48 8.59 8.03 8.43 8.09 8.65 8.54 7.42 7.87 7.70 7.98 7.64 7.25 7.25 7.70 7.09 7.09 7.98 (3) l'vlEASUREMENTSOFSPECTRA s-• • cm- Provided TABLE 2 ) 9039.55 9040.50 9080.46 9078.44 9121.77 9120.74 9255.64 9243.66 9166.84 9107.98 9090.92 9032.08 9017.08 9092.86 9091.98 9196.77 9182.85 9212.74 9242.67 9240.67 9160.66 9159.69 9158.66 9157.67 9127.68 9126.69 9125.66 9191.66 9189.69 9188.67 9187.66 9098.82 9075.01 9071.98 9071.00 9070.00 9128.73 9156.67 9155.67 9152.67 9151.66 9150.85 9135.92 9120.81 9102.98 9096.99 9094.99 9092.86 9091.86 9090.82 9067.02 19 (2,440,000+) Julian by (1) Date ...... ·········· ...... ·········· ...... •...... ·········· ...... the L. NASA Special ( 10-•s J. Astrophysical Astrophysics H. l'vl. l'vlcDonald2.1 ergs F. FA(5100A) Lick Calar 10.04 SAOReticon 9.60 9.26 8.82 8.43 8.48 9.15 9.04 7.42 7.53 7.92 9.04 9.93 8.37 8.04 8.70 8.15 6.92 6.36 7.59 7.64 7.09 7.25 7.42 8.43 8.20 8.37 5.80 6.08 6.86 6.36 6.42 6.30 6.36 6.36 6.36 6.53 7.64 7.42 7.87 8.15 5.97 7.42 7.14 7.48 7.70 7.42 7.81 7.14 7.59 7.48 (2) s-• Shane cm- Alto Observatory 2 CCD mCCD CCD ,.\- 1 Data ) Scanner (10-• System 3 ergs F(Hp) 10.16 10.38 8.15 8.31 7.42 7.48 7.70 7.98 7.92 8.31 8.15 8.31 8.15 8.03 8.15 7.59 7.70 7.59 7.37 7.31 7.48 7.37 7.53 8.93 8.98 8.03 8.43 8.98 8.65 8.26 8.26 8.26 8.37 6.81 7.87 7.81 9.10 7.81 8.93 8.76 8.54 8.48 8.03 7.64 7.14 7.98 7.81 7.53 9.15 7.31 8.65 (3) s-• cm- 2 ) 1995ApJS...97..285K affecting manishin model and each tector different offsets 9077.39 9114.51 9070.46 9130.46 9107.42 9031.54 9083.46 9014.51 9088.32 9078.41 9074.53 9141.39 9140.46 9132.40 9131.35 9034.50 9010.56 9129.46 9089.40 (2,440,000+) Julian In we data (!) order systems of Date remain...... ·········· ...... ·········· ...... ·········· ...... ·········· ...... therefore wavelength the set. et the to J y w u H M L © z E R F B A Set (1) Data al. various starlight that account American FLUX ( We 1994). 0.931 0.954 0.988 0.827 0.987 0.803 0.981 0.967 1.011 1.058 1.139 1.016 1.000 Point-Source Scale (10- compute were SCALE sensitivities ascribe. (2) ± ± ± ± data, ± ± ± ± ± ± ± '{' 15 Factor M. U. surface for 0.034 0.037 0.048 0.014 0.046 0.040 0.015 0.025 0.046 0.041 employed 0.020 This ergs FA(5100A) R. W. TABLE Calar SAAOReticon FACTORS 10.16 SPECTRA Loiano the 8.87 8.65 7.70 7.81 7.81 7.09 9.43 9.65 7.20 8.03 8.37 8.43 8.48 8.03 8.26 8.65 7.98 (2) 7.31 s-• we ShajnCCD Astronomical a model (10- these cm- small Alto brightness different use 15 Extended of -1.030 -1.507 20 -0.833 -2.893 -1.847 -2.687 -2.025 -0.711 -1.849 CCD at 2 Correction ergs 0.000 0.448 2.691 4.264 FOR CCD A.- the the gives differences the empirical 1 .- (3) ) OPTICAL ± ± ± ± ± ± ± ± ± ± ± different 1 various carefully Source amounts 0.482 0.336 0.293 0.320 0.250 0.494 0.335 0.231 0.384 0.433 0.193 cm- as distribution BROAD-LINE G 2 the (10- A.- Society correction 1 observatories, to stellar ) 13 filter constructed ergs of F(Htl) somewhat 8.37 8.37 8.82 8.59 8.31 8.48 8.48 8.31 8.59 8.26 8.98 8.54 7.03 7.53 7.98 7.76 8.20 8.59 8.59 (3) starlight s- and TABLE contri- of 1 • cm- Ro­ de­ for REGION Provided 2 ) 19-Continued are 9102.20 9101.19 9112.24 9113.24 9095.23 9094.25 9085.22 9156.39 9155.41 9103.64 9098.80 9106.73 9158.35 9157.41 9091.15 9090.17 9089.17 9087.20 9159.38 The 9088.20 where observed 22. values then the the tometrically by rived found al. light with between starlight-free) (Johnson the ble cm- broadband bution 7~5) (2,440,000+) Julian IN We separated aperture data 21. photometric ( by In 2 values the 1994) (!) compute curve Vpi comparison AGNs. compute A to the of Date general, We ...... ·········· ·········· ...... ·········· the through - sets spectroscopic F>. be values t::..m 1 = • 1966). V ( aperture first an very small. of The 14.99 0 and 5100 employed. in NASA hs measured in for magnitudes VIII. a t::..m appropriate Tables are a convert time the V comparison light values. the each zero-point starlight then 0 A) For mag, hs values (10- Y. the are with of photometric by and nominal Astrophysics Beijing 4-10 photometric 15 Z. each continuum As radius observed empirically We converting values or ergs We FA(5100A) the no W. spectroscopically to ESQ nuclear in contribution F>.(5100 Vnuc constant more can 6.75 6.97 6.86 6.81 6.92 7.76 7.87 6.92 by 8.03 8.09 8.20 6.97 7.31 6.47 7.64 7.37 7.98 7.87 7.25 7.03 (2) s- fluxes photometric ShajnCCD define Observatory of obtain the 1 R 2.2 comparing cm- spectroscopic with the by now = case values m than flux zero-point 2 curve using 8 in measurements a CCD derived photometric A.- data a ~O to A)= compare zero-point the starlight of Table systematic 1 given is 2 Data ) CCD the a given days. the through set V by spectroscopically correction these ga1 3.4 V spectroscopic derived 21 by are adding empirical by -magnitude = (10- aperture System adjustments contribution directly The X in to 14.09 comparing Romanishin given correction measurements 10- correction data 13 Tables nuclear the given appropriate ergs F(HP) values to for 7.92 7.64 15 8.37 8.31 8.20 8.15 8.54 8.03 8.20 8.15 8.76 6.92 7.92 7.42 7.31 6.92 7.98 7.98 7.03 7.92 (3) mag. in nominal the the sets, relation s- ergs ( each in 5'~0 1 Table 4-10. mea- cm- scale pho­ (i.e., that Vnuc t::..m Ta­ (4) the are de­ for s- 313 we to of et X 2 ) 1 1995ApJS...97..285K Julian (2440000+) 9075.01 9070.46 9070.00 9064.80 9031.54 9012.03 9090.17 9089.40 9089.17 9088.32 9088.20 9087.20 9085.82 9085.22 9083.46 9080.46 9079.85 9078.44 9078.41 9077.39 9074.53 9071.98 9071.00 9067.02 9066.02 9065.01 9062.87 9056.89 9048.94 9045.96 9045.04 9040.50 9039.55 9034.50 9032.08 9020.97 9017.08 9014.05 9013.94 8992.01 8982.05 8981.03 8973.01 8967.00 8954.03 9092.86 9091.98 9091.86 9091.15 9061.90 9029.95 9014.51 9013.03 9012.64 9011.03 9010.56 9010.04 9008.99 9004.65 9000.02 9090.92 9090.85 9090.82 9036.00 9094.25 9096.99 9095.23 9094.99 9094.57 9098.82 9098.80 (1) Date (10- 15 © 10.37 10.80 12.05 11.43 10.49 10.39 10.13 10.07 10.10 10.12 10.87 10.56 10.38 10.21 10.32 10.45 10.15 10.29 10.10 10.49 10.16 11.10 11.33 ergs 8.77 8.72 9.21 9.04 9.37 9.26 9.59 9.42 9.49 8.06 8.05 8.62 8.30 8.42 8.44 8.59 8.55 7.53 9.10 9.71 9.42 9.77 9.85 9.53 9.91 9.69 9.31 9.26 9.59 8.09 7.99 7.84 7.64 7.90 7.95 7.95 7.48 7.95 7.75 7.83 7.74 8.00 8.02 7.79 F,,(5100A) 8.77 8.50 9.10 7.80 American s- (2) ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 1 0.22 0.42 0.43 0.43 0.23 0.24 0.44 0.62 0.61 0.27 0.42 0.42 0.22 0.20 0.35 0.28 0.20 0.29 0.20 0.27 0.29 0.19 0.31 0.40 0.41 0.22 0.21 0.21 0.42 0.43 0.43 0.46 0.24 0.25 0.44 0.47 0.26 0.52 0.25 0.26 0.26 0.25 0.43 0.24 0.45 0.41 0.44 0.46 0.26 0.25 0.43 0.30 0.17 0.20 0.36 0.28 0.20 0.45 0.26 0.53 0.28 0.28 0.26 0.25 0.29 0.37 0.31 0.28 0.40 0.46 0.39 cm- 2 A- 1 OPTICAL ) Astronomical Society (10- 13 8.16 8.09 8.44 8.38 8.27 8.27 8.28 8.71 8.23 8.88 8.49 8.50 8.39 8.93 8.66 8.48 8.59 8.03 8.06 8.15 8.33 8.34 8.49 8.26 8.88 8.15 8.43 8.09 8.88 8.12 8.65 8.34 8.45 8.61 8.44 8.55 8..54 8.49 8.28 7.59 7.88 7.48 7.66 7.38 7.64 7.97 7.98 7.63 7.88 7.46 7.23 7.58 7.43 7.39 7.25 9.26 7.87 7.31 7.99 6.93 7.42 7.70 7.69 7.98 7.64 7.09 7.11 7.42 7.38 7.71 7.74 CONTINUUM ergs F(H,B) (3) ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± s- 0.27 0.31 0.27 0.31 0.27 0.29 0.20 0.28 0.28 0.29 0.21 0.29 0.33 0.33 0.28 0.35 0.28 0.30 0.34 0.29 0.28 0.30 0.29 0.21 0.22 0.30 0.20 0.20 0.26 0.27 0.53 0.54 0.28 0.34 0.20 0.33 0.21 0.20 0.20 0.35 0.28 0.22 0.28 0.42 0.29 0.29 0.34 0.21 0.15 0.18 0.26 0.27 0.19 0.18 0.25 0.29 0.41 0.23 0.20 0.26 0.19 0.20 0.19 0.19 0.24 0.25 0.25 0.27 0.24 0.39 0.28 1 cm- TABLE 2 ) AND Julian (2440000+) 9163.69 9158.66 9132.40 9132.05 9129.46 9128.75 9128.73 9126.69 9125.66 9122.84 9121.77 9120.81 9120.74 9114.51 9113.24 9107.82 9103.64 9240.67 9240.63 9211.66 9205.68 9197.70 9196.77 9191.66 9190.65 9189.69 9188.67 9187.66 9183.69 9182.85 9176.69 9169.69 9166.84 9164.37 9160.66 9159.69 9159.38 9158.35 9157.67 9157.41 9156.75 9156.67 9156.39 9155.67 9155.41 9152.67 9151.66 9150.85 9149.74 9142.72 9141.39 9140.46 9135.92 9135.76 9131.35 9130.46 9127.68 9114.81 9112.24 9107.98 9107.42 9106.73 9102.98 9102.20 9101.42 9101.19 9099.80 9255.64 9243.66 9242.67 9212.74 21 HtJ (1) Date LIGHT • (10- Provided CURVES 15 10.02 10.12 ergs 8.77 8.98 8.99 8.02 9.49 9.10 9.75 9.88 9.96 9.21 9.84 9.58 9.14 9.49 9.35 9.26 9.21 8.95 8.82 8.53 8.73 8.70 8.09 8.70 8.56 8.00 8.02 8.03 8.18 8.06 8.11 8.02 8.15 8.54 8.54 8.59 8.99 8.98 8.02 9.04 7.81 9.16 9.04 7.96 9.04 9.10 9.38 9.58 8.59 8.48 8.98 8.92 9.69 9.49 9.21 9.49 9.58 9.21 9.21 9.80 9.26 9.48 9.25 9.36 7.29 7.47 7.67 7.72 8.98 F,,(5100A) s- (2) ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 1 0.23 0.24 0.40 0.42 0.45 0.46 0.25 0.51 0.46 0.48 0.49 0.33 0.24 0.45 0.43 0.42 0.19 0.22 0.23 0.32 0.24 0.47 0.45 0.32 0.34 0.31 0.22 0.20 0.22 0.29 0.19 0.39 0.34 0.19 0.37 0.20 0.37 0.19 0.20 0.38 0.20 0.37 0.20 0.37 0.37 0.20 0.21 0.23 0.23 0.42 0.21 0.23 0.54 0.23 0.22 0.21 0.24 0.24 0.23 0.24 0.24 0.42 0.23 0.45 0.43 0.44 0.22 0.23 0.22 0.22 0.22 cm- by 2 A- the 1 ) (10- NASA 13 8.01 8.03 8.66 8.21 8.44 8.82 8.71 8.37 8.01 8.26 8.21 8.37 8.05 8.10 8.17 8.71 8.39 8.10 8.01 8.31 8.38 8.03 6.99 6.60 6.81 6.99 6.92 6.91 6.97 7.77 7.95 3,-12 7.93 7.79 7.70 7.44 8.31 8.16 8.15 8.06 8.66 8.26 8.25 7.81 7.55 7.53 7.17 7.79 7.23 7.09 7.09 7.11 7.20 7.25 7.63 7.58 7.55 7.83 7.79 7.88 7.36 7.28 7.34 7.55 7.45 7.53 7.99 7.81 7.98 7.90 7.58 ergs F(H,B) (3) ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± s- 0.29 0.28 0.26 0.27 0.26 0.29 0.18 0.33 0.34 0.20 0.30 0.30 0.27 0.20 0.19 0.28 0.18 0.28 0.25 0.25 0.22 0.25 0.35 0.25 0.18 0.18 0.18 0.26 0.26 0.30 0.28 0.32 0.27 0.21 0.27 0.32 0.26 0.31 0.28 0.30 0.28 0.21 0.21 0.33 0.29 0.34 Astrophysics 0.26 0.18 0.18 0.19 0.19 0.19 0.20 0.20 0.21 0.19 0.20 0.27 0.20 0.25 0.26 0.19 0.19 0.19 0.18 0.35 0.31 0.32 0.21 0.62 0.27 1 cm- 2 ) Data System 1995ApJS...97..285K tained of are Fvar. tures the the ysis, surements. and of The measurements these for occurred time HST campaign, campaign. missed An paign campaigns. observations, light given Marked mode photometric of again dataset. vert ric surements, more The Table The After the data, the exception featured data. ratio unfortunate HST CAO CBA the San combined CLSI Lowell Behlen MSU these the period curves two refer schedule, in to was later accurate after condition parameters the 6.1. effect combined FOS Pedro adjustment ratio 24 Table on yield 0.3 the of around 0.6 These 1.25 CCD measurements variability delayed to CCD CCD to large and IUE By for the The this © Figure maximum As of m Characteristics in m PHOTOMETRIC from measurements measurements. of appropriate values m of Martir the of which values CCD (Table (Table the many 23. American circumstance, that Figures light-curve beginning the (Table were (Table (Table noted intercalibration estimates therms decline the measurement values data parameters consequence JD that 6. direct-integration Data best Tables 5100 by (Table HST 12 we CCD total were VARIABILITY (1) of 5) of 8) were parameters 2,449,090. relatively of of would 4) 9) 7) was 2 earlier, are Set ...... the temporal use F~(5100 to 10 the are Vnuc ...... and weeks ...... fluctuation (Table A observations into Lya 10) obtained of ZERO-POINT arranged the 21 starlight minimum and TABLE of triggered data photometric continuum continuum to given of were the turnaround which merely Astronomical derived ...... It a and the flux). time the the the 6) characterize of on errors sparse 11, light is thus HST process are A), coverage ...... simply this then mean account in beginning 22 HST 23 Ultraviolet excluding ANALYSIS are spans before contribution to on add When measurements curve listed by consist for Table and ADJUSTMENTS flux. campaign. (see are near ...... delay the did based the and straightforward a and zero also observations in non-Poissonian appended the uncertainties of solar-array shown these mean the in not Paper of for The basis of combining the the BROAD-LINE emission-line 23 the the is of "HST -0.180 -0.045 allows -0.079 -0.025 columns H/j of the on the point Database a time-series HST 0.017 0.030 0.019 overlap Society end continuum that for those spacecraft mean the values flux, variability IUE the of The ground-based I), IUE (mag) emission-line in is !J,.m (2) the each to of for ± ± ± ± ± ± ± the only us HST campaign. photomet­ only" subtracted Figure and corrected inclusion and data 0.027 0.039 0.037 0.040 0.019 0.020 O.D18 problem. the the also flux data (5)-(7) the with to each original are in to optical of Rmax, (with noise make SWP anal­ mea­ • HST cam­ HST IUE safe­ each con­ that that and fea­ also just ob­ are the the 12. Provided REGION set are expect these tion duce 4 47290 misplaced ysis, "combined fore The to 7 IN 422 the by correlated lags being measurements errors four AGNs. either (JD light to the (JD toward Julian (2440000+) measure combined additional in 9047.60 9162.35 9159.37 9148.32 9133.66 9114.59 9105.35 9104.75 9104.37 9099.43 9063.54 9061.57 9102.38 9101.89 9101.76 9101.73 9100.70 9100.40 9099.81 9099.70 9099.69 9098.98 9098.75 9097.90 9095.69 9091.37 9078.90 9073.95 9069.45 9063.82 8991.62 9215.66 9214.65 9213.62 9154.69 9150.36 9149.37 9149.33 9146.30 9131.38 9127.85 9124.69 9121.69 9059.40 9053.78 9121.79 9121.39 9120.86 9107.55 9062.56 2,449 ultraviolet" between NASA are curve 2,449,063), (1) the VIII. OPTICAL Date in underexposed zero ,082), time, aperture. without from 14.58 14.60 14.43 14.53 14.58 14.40 14.54 14.47 14.45 14.53 14.51 14.54 14.50 14.53 14.53 14.50 14.65 14.61 14.63 14.57 14.52 14.47 14.38 14.45 14.61 14.42 14.40 14.42 14.51 14.54 14.55 14.49 14.42 14.42 14.31 14.31 14.31 14.31 14.42 14.42 14.45 14.47 14.36 14.33 14.31 14.24 14.41 14.38 14.36 14.17 BASED (magnitudes) were Astrophysics the in time SWP CONTINUUM Vnuc and thus (2) ± ± ± ± ± ± ± ± ± ± ± this ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± data these emission SWP TABLE not ON 0.02 0.06 0.02 0.02 0.06 0.02 0.06 0.02 O.Q2 O.Q2 0.06 0.06 0.06 0.06 0.06 0.02 0.02 0.02 0.01 0.02 0.06 0.06 0.01 0.06 0.06 0.02 0.06 0.03 0.02 0.02 0.02 0.03 0.04 0.06 0.01 0.02 0.01 0.06 0.02 0.06 0.04 0.06 0.06 0.02 0.06 0.06 O.Q2 O.Q2 O.Q2 O.Q2 delay improving These 7 SWP fashion. biasing spectra PHOTOMETRY set. scaled light or (10- 47387 ( For 23 4 are § LIGHT types lines 15 6.3). curves 496 10.86 10.37 the ergs or We also suspected 8.62 8.62 8.36 8.78 8.21 8.41 8.67 8.83 8.62 8.56 8.94 8.02 8.11 8.94 8.94 8.62 8.72 8.78 8.56 9.59 9.77 9.90 9.23 9.23 9.90 9.90 9.46 9.05 9.17 9.23 9.05 9.46 9.34 9.59 9.23 the 8.36 8.21 8.72 8.56 8.51 8.26 9.34 9.23 9.23 9.90 9.29 9.05 9.90 F~(5100A) Data the (JD otherwise and (JD of CURVE s- (3) derived ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± Since designate purposes 1 are 0.53 0.54 0.55 0.51 0.18 0.35 0.51 0.08 0.16 0.16 0.50 0.16 0.48 0.16 0.16 0.16 0.46 0.30 0.16 0.15 0.45 0.15 0.16 0.49 0.17 0.52 0.60 0.17 0.17 0.17 0.08 0.15 0.15 0.48 0.47 0.08 0.49 0.51 0.17 0.55 0.27 0.18 0.19 0.26 0.50 0.17 0.08 0.47 0.16 0.53 temporal are problems cm- continuum 2,449,077), 2,449 System 2 excluded: small, the of A- cross-correla­ 1 adjusted having ,095). of lags ) these sampling. this could the that which as All SWP anal­ most SWP been 315 the be­ in­ we of 1995ApJS...97..285K tude this tion tions tinuum, sion of campaign campaign ations distinct our I). in that the tively uum-band paign prior some first curves conservative another could observations days, ilar 2,449, continuum by NGC5548wasmonitoredby from frame line 316 As Inspection Note FIG. the HST(UT the It start understanding .c(' fluxes :c ;;: can a decrease. e .... 8 of lines, 10 the continuum of was 1992 is of in ofNGC to followed (Rmax clearly effect inactive, (see 117) light the shown days I2.-Continuum variability also the or this increase be the the the of (bottom significantly and He (Rmax November began. wings Figs. I more wavelength, further ,li1?~,iit general during 1993 the © curves = effect is Fe HST apparent may 1988-1989 fl! bias 5548, recorded approach of II 10- Following followed in 4.5 by American II and HST an 8-11 April Figure = panel) of I of 9000 13 smeared pseudo-continuum, Figure also The the I at may campaign a ,,I appears and ergs 2.5 substantiated, which of increase characteristics (local very -20% N through monotonic reached 1350 I9-I993 the result. campaign. and be in smaller v, dynamic at are s- fluxes a be for by 6 just is broad 6: 1 underwent campaign, large Figure IUE(UT a 1350 intrinsic nature and cm- in the Fvar due A; maxima NGC a to out over Jullan to span an small I993 at units as of Astronomical May27)arealsoshown. (Figs. Paper a 2 reject continuum decrease during and to Table 5100 initial forthe decrease A) at emission minimum was Dale the 5548, -30% 9100 range decrease 6 of dilution of September. of Both longer 1993 it than decrease. that to Rmax (2440000>) of the A next and I). seen 10- is 4 10 a the the line. 24 as the continuum the (top the rise days etc. potentially in March priori continuum. JUE 15 the and with in occurred given IUE in largest in shows minima) 4 lines, high-ionization in wavelengths. ergs the The FOS combined panel) from to of the just was days However, Table the continuum small-scale (JD Fluxes 1988-1989 This 12). and increasing nearly I9-1993 continuum - in periods s- those 1988-1989 continuum the apparently before 9200 1 50% amplitude Society some that and Tables and cm- 2,449,114-JD 24), ground-based It is over important Balmer are become followed is HP the points then during HST 2 the during May27)and some combina­ A.- source. while apparent 2I in the ti f about features At emission­ contin­ level (Paper KO 1 ampli­ I the and a varia­ I emis­ for cam­ HST which • vari­ least JUE con­ light rela­ sim­ part that just less the the RIST rest the by Provided 23, to at If 5 A ET tion of cross-correlation the showed table previous sponding eters, 1986; optical given varying can optical narrow sis acteristics the the of This infer tained this vations HST ations continuum is however, scale, emission C lines, tuation tions. timescale, not smoothed started C creasing complex. cludes character cated Lya mediate true variations As the The III] Figure the The consistent IV, of AL. optical by results continuum be quite blended cross-correlation fluctuations light decrease that in the an campaign in continuum Fvar complex. Gaskell and smaller SWP here, The at in optical compared in database monitoring a light the to line. just prior components, such components, less our amplitudes, Table approximate between functions years. 6.2. C contribution these least 8 to long during lines The the during curves of and and turn reported the continuum were version variability III] shows larger spectra since the variations NASA previous variability curves the The feature with data Characteristics may 1988-1989 amplitude & Lya enough 6 total Rmax• two response in variability 6.3. did JUE recorded down The shows continuum of are year smallest methods were Peterson in directly the the and sampling that the total to amplitude span Paper of core have program emission the of in in not of N v N also Lya Cross-Correlation C in and the Astrophysics has high-ionization first underwent time), papers, 5 N emission-line in lag this Paper at the only to nearly from and the the IV function in of both (as average flux, showed a respond rather been were given v the HST the HST sample line VII. continuum been by core total with a this of in parameters campaign. C in 6 region high-ionization direct-integration continuum H,8 1987) as characterized a and monotonically days variations III] are the the a lines. I. before cases Si 17 the end epne mainly responded rise "ramps" almost we the flux of the Neither continuum monitoring and preliminary separately Unfortunately, the of286 monitoring emission uncertain. campaign. adjusted IV summarized complex fluctuations days, 6-10 the JUE Lya variability ( adequately strongly have lower and a CCF; result renders of stellar and of results + showed larger total small they Optical variability. the the 0 certainly variations. wing. and days. The lines a which of for day the Data employed as Results (i.e., fall). light IV] of ionization fluxes cf. for line continuum campaign, the flattened campaign. than also for for described by more but this ground-based program to If the HST discrete variations and campaigns. time-series even response The lines complex increasing parameters Gaskell The Database the effects variability monotonically the larger than so, the The is previous Fvar in curve the measurement System responded large steady fifth that the had larger consistent Lya. Table sampling detailed The total-flux campaign then FOS periods larger mimicked This to shorter and C two in poor and than similar of correlation lines year NGC decrease above. IV during the These the & interpola­ any or times than was decrease. one the C behavior 24; Rmax) separate (a years, and analysis fashion; possibly It of fluctua­ param­ Sparke the Vol. quality for flux seen IV of analy­ longer obser­ corre­ of of to is char­ time­ time­ inter­ these 5548 C non­ vari­ indi­ with may fluc­ Lya The was and two our no­ the H,8 the ob­ the the the the III] in­ in­ 97 in as in in in 1995ApJS...97..285K in have ( function Cross-correlations campaign, data correlations various tion time culation. comer; 25). the tions 5100 curve as data variations 5100 amplitudes is is peak No. 1994). the In computed Table the result is 2, alone. As fell span Figure high of A value in A centroid nearly with 1995 pairs the explained continuum note The continuum, the 25. off (DCF; The of in values of The which of greater the CCF, © The substantially 13 between feature results symmetric the the oflight that using the cross-correlating UV/ American at we light DCF cf. parameter HST 1350 centroid the of which a earlier, of makes than present Edelson optical-continuum all are produce positive Ymax designated curves curve 50% all bin only various A campaign points shown 0. about other has continuum. (~0.96) width the during level.) 5 these atcentroid those the r designated atpea1c as & max. value Astronomical time virtually temporal FOS near a Krolik of described in H,B C Lya He F,(1350A) F>.(5100A) Si Cm]+ C Lya Lya F,(2195A) Nv F,(2030A) F,(1460A) F>.(1790A) F>.(1350A) F>.(1145A) correlation is the small in IV IV (This IV+ •In results Year b Year IUE HST points II are Figures the - - 1 the In is and delay A1240 Ymax· A1216 .X1216 A1549 A1549 A (in + day. each continuum the 1993 1993 1216 the units units 1350 campaign 5 ( 5 0Iv] 0 Sim] campaign included In second positive FOS (1992 1988) days) m] is identical yield 1992 HST cross-correlation in VARIABILITY coverage Combined core May May total Combined HST Also peak Combined location HST HST HST HST HST HST In the means somewhat which sometimes of panel of Al402 by HST HST 13-1 Feature the A each Nov Nov results HST 10-• BROAD-LINE 10-• 27) 27) only (1) HST continuum only only only only only only only White case (1993 of very are (1993 given only continuum of only half HST delay - upper - ...... 7 Society in the 4 4 lag ...... only bands fall JUE JUE that only JUE panel ergs-• ...... ergs-• results...... the 1993 1993 and computed in Mar of of Apr the ...... small only for of CCF, in & PARAMETERS behind days & & the the & within ...... uncertain. referred (see Sep) Sep) CCF the 19 tabulated 19 CCF left-hand the cm- HST HST cm- Peterson Table HST the we with ..... optical optical Cross­ delays bands .. which .. of Table varia­ func­ 2 2 show HST • . light FOS with A-•. cal­ the the the the for of Provided 25 REGION to Number TABLE Epochs 142 192 59 97 53 53 53 39 39 (2) 39 39 39 39 39 39 39 39 39 39 39 AND SAMPLING the tion cross-correlations continuum ever, during days, Their itive These minimum tained tion Average responses halfthe peak continuum. during 24 hand that the sponse sistent lations peaks, 0.73 0.67 2.14 Interval 1.58 1.43 1.00 1.43 1.43 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 3 (4) (3) IN In In Sampling by longer high-ionization is with are with and Figure the Figure which comer AGNs. responses lines tracked slightly while by the with the have (days) the Median CHARACTERISTICS times SWP consistent 0.99 0.51 0.37 0.77 1.00 1.01 1.01 1.01 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 uncertainty 1.00 centroid values the using are HST around time first before NASA is what 15 progressively of The the 14 temporal observed VIII. consistent asymmetric resolved 0.914" 0.881" 0.906" of each 3.38" 622. 699. 79.3 Mean 82.2 89.3 670. 3.26" 3.60" 2.17" 2.74" 410. 128. 718. 3.83" 77.6 1.99" and Flux 1988-1989 (5) campaign. the lagged Si coverage -1 we DCF these for 6 6 6 6 6 we of and 6 6 6 6 6 IV+ JD with the Table lines combined panel present day, the Astrophysics in 0.071 0.050 0.093 0.064 0.187 0.109 0.146 0.085 0.140 0.090 0.129 0.130 0.127 0.120 0.109 0.117 0.122 0.143 0.139 0.167 the Fvar know (6) during 2,449,090, bin resolution. character behind this large in 0 emission 5100 zero with consistent light have less and are IV], 25 toward the Rma:r: 2.50 1.29 1.40 1.39 1.65 1.53 1.76 1.32 1.82 1.37 1.65 1.75 1.61 1.49 1.53 2.05 width 1.62 1.71 1.83 1.86 value campaign (7) about the decline the the we (I computed A well curves C combined the ultraviolet the well-resolved TI continuum IV, cross-correlation HST present of results is is positive both lines, resolved The relatively the = 1350 also with the and 2 and shown Data 0.2 (Paper campaign, days approximate cross-correlation the continuum -1 presented relative Lya-core A the which the cross-correlation then ultraviolet days). data lags. continuum peaks. Lya CCF in day, FOS System in deep cross-correlation I), recovery each set. the On to were and which are As in respectively. result. cross-corre­ This continuum in the results account Again, upper variations case. combina­ expected, both mean data Paper the derived 1350 by is is in How­ func­ C one­ con­ pos­ left­ The -7 set. 317 ob­ the the re­ I. IV of A 1995ApJS...97..285K (ordinate) 5100 Fm. A continuum 13.-Interpolated and -0.5 -0.5 -0.5 0.5 0.5 0.5 © delay 0 0 0 1 1 1 -20 -20 -20 American and in Lya 5100 C days I the IV cross-correlation (abscissa). major core .A -10 -10 -10 Astronomical ultraviolet (solid emission-line 0 0 0 curves) Society and 10 10 10 measurements discrete • correlation Provided 20 20 20 during -0.5 -0.5 -0.5 0.5 0.5 0.5 functions 0 0 0 1 1 1 -20 -20 -20 the by HST He Si NV the (with IV II campaign. NASA + + -10 -10 -10 error 0 0 bars) IV] III] The Astrophysics of units the 0 0 0 1350 on the A continuum axes 10 10 10 Data are correlation with System the 20 20 20 overlapping coefficient 1995ApJS...97..285K axes autocorrelation) resolved curve. correlation ified results upper namely, FIG. are C panels Of for correlation 14.-Interpolated IV that response the component the © functions they show four C -0.5 and 0.5 0.5 American IV coefficient 0 0 1 1 increase to with profile emission-line the the the light cross-correlation cross-correlation 5100 show 1350 continuum -20 -20 overlapping components, (ordinate) with curves Astronomical A. A. the increasing profile same relative and variability. 5100 (soljd delay only components. functions A gross 0 0 time continuum to BROAD-LINE curves) in the the days Society All delay characteristics, red 1350 (abscissa). for and of wing and the but The the discrete 20 20 A the cross­ begin has spec­ • light four Lya REGION Provided a correlation and -0.5 -0.5 C 0.5 0.5 IV cores another, light that, to to 0 rapidly 0 1 1 emission IN functions level level by curves unlike did AGNs. C Ly in the -20 -20 off(by off IV a except not the lines (with at for NASA any first appear VIII. for positive the JD that error of the 11 blue 2,449,110). the "combined" the days to Astrophysics bars) delays level 0 0 other red and of of the core off the red of components, ultraviolet HST until In 1350 several cores rises contrast, campaign A about 20 20 Data slightly are continuum days. data very JD the set. the System more Figure before 2,449, similar The red blue with units rapidly wing 9 124; and it itself to shows began on rose one 319 the red (its the in 1995ApJS...97..285K (abscissa). emission-line FIG. 15.-Interpolated -0.5 -0.5 profile © 0.B 0.5 0.5 0. 0.6 0 0 4 1 1 1 -20 -20 American -20 w...J--L-L-...L-.L.-J.--'-.....L-...L-L...... 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Small the the the the Figure corresponding first core paper cross-correlation The to that delays small which similarity. lower sense profile can the more rapid it 16.-Close-up than near by contamination 11 vs. differences is CCF lower and the toward 16 red before and days direct be red state seen amount. © that (i.e., as right-hand light zero, C variations, we blue core accentuated red-core expected wing IV. and will American left-hand of the negative varies that the function The show the the comparison curves; with This ("RC"; the response variations wing be the comparison in is variations blue-core red corresponding Also the results function discussed elsewhere. campaign. the u u "" the a differently a can panel by light blue-core/blue-wing shows lag. slight which is leads wing panel direct solid this rise 0.5 0.6 0.9 0.7 0.8 response shows only He be shown These by of -20 Astronomical curves in of of line) in investigated reduces the of the leading asymmetry and the II, of in in direct is the comparison direct C Figure a the effects We the very which beyond Figure the the from strongest relatively red and IV two blue-wing is blue of interpolated are rise suspect blue-wing blue component -15 the light the cross-correlation the nearly wing the cross-correlation are the core 15. the given core, responds in 15 blue the somewhat various blue toward wing blue-core/red-wing The effect by BROAD-LINE other asymmetry curves the shows ofC strong components of that symmetric CCF light scope core as detailed in Society cross-correlation -10 core). blue-core/red­ blue-core the appear flux might Table IV components; of at C vs. that negative the much curves. asymmetry more (Fig. which blue-core is of IV least their red levels attribut­ result In analysis the compo­ be we 25 to to pronounced wing of of about 9) some more sum­ • -5 first­ flux. con­ by neg­ lead sug­ The cur­ and can the the de­ REGION off Provided in of ("RW"; a I functions Delay for 0 dashed uum primary and lation lists tions the with about and emission-line cross-correlating as lower more the those relation studied fifth variations however, 1988-1989 (days) the of IN As The 1. large by former the blue blue centroid the 5100 year, variations? the What described were complete obtained AGNs. panel line). function. the top C the as FWHMs in wing function objective wing IV 5 differences A the BLR by from the panels more resolved blue The is is campaign in continuum NASA and of about importance an the VIII. Lya Figure responds variations in red core analysis in the That velocity blue 1992 indication the detail of and year lag in of 10 core § 6.4. or CCF vs. 2 the in core. Figure addressing 1, 5100 found the Astrophysics between weeks; 17 Civ November the (Papers blue 1 ( CCF this the before autocorrelation light General may slightly shows field. latter for 1988-1989), optical lag lags, of A wing ground-based is program 17 for that 15 year the and curves. determine He centered behind I There the function and any the which ("BW"; and three other faster Discussion H,8 II most H,8 sampling 5 to UV optical contamination Table are conclusions II). lag 1993 was is light near specific is 20 years the than Data of dotted and somewhat but a is is whether The what functions weak zero 25 the undertaken approximately much campaign. continuum September. curves are optical window the the (Paper values show line) important System questions: delay was fairly suggestion optical blue narrower can this with for smaller found for the and needs continuum of autocorre­ VII). consistent the be is core, Table that the autocor­ the with result The is real. contin­ drawn slightly entire in varia­ twice to of peak 1350 than than The that and 321 H,8 the the the 26 be of 1995ApJS...97..285K shifting Carlo assumption data Random A the relation point point. simulations subsets cal consistently other lish UV (Papers optical tical tion for of autocorrelation and curves tainties. panel. 322 2. These 3. 2. interpolating FIG. l. continuum the continua, observations the (which, the continuum set continuum A A What What to words, (.) IL c IL shown (.) (.) realization, optical DCF This The continuum 17.-Shown model upper of model result. point the I to observations Gaussian and the bin as values is is model in © in continuum continuum that find (noise-free) we described the the function width Fig. limit ultraviolet the as we optical UV order These measurements II) American -40 by made necessary. by are is lag the velocity that data the 12. performed that in the about variations continuum for deviates on simply altering plotted The for the to calculations following and by quoted the continuum between more ( the the a continuum 5100 any assess Gaskell -20 top the possible interpolation was DCF data the 1 model field very optical as day a panel possible A) highest firmly were each Astronomical sampling individual Delay time-delayed errors is then a is observations) the obtained from of and & simple light or 1 procedure indeed series day. lag are Peterson the UV 0 flux used uncertainty were (days) light less. continuum the establish behavior. linearly ionization CCF the between curve are the The lag window Clv-emitting H~ points measurement continuum of assumption In to curve small. done cross-correlation in corresponding distributed is between combined emission 1987, simple order alter 20 are was shown this was version_ with interpolated our autocorrelation by the was shown For By in illustrates lines? Society lags followed: the experiment, produced to using associated earlier as the UV line Monte using generated the each better 40 a flux in that behind region? of in ultraviolet smooth normally. cross-cor­ under for continuum and the time; UV the functions the the various at finding the Monte the KORISTA estab­ Carlo uncer­ • from from 1350 opti­ each lower effect func­ and light UV line, op­ the the we Provided by in ET that the these between cross-correlated, continuum. Again, probability points pled preserve paign. approximate ation campaign component) model level The 4. 3. by AL. Ground-based Combined C C HST experimental F>.(5100 F>.(1350 F>.(1350 F>.(1350 F>.(1350 •Centroid F>.(1350 the F>.(1350 F>.(1350 F>.(1350 F>.(1350 b to IV IV The The simple Centroid in is Series to above The First blue random blue the obtain (1) FOS 2.0 the probability optical the simulate the model UV during core core A) A) A) A) A) A) A) A) A) A) days. distribution JUE measurements optical NASA optical simulations UV We and procedure consistency distribution measured measured measurments the F,(5100A)d F,(5100A)c F,(1350 F,(1350 paign. SWP Continuum and Gaussian C C C1v C Hen+ Si CONTINUUM F>.(5100 and F>.(5100 Civ Lya optical •During and IV b cYear5. d IV Nv diluted then IV continuum CROSS-CORRELATION same Iv+ value) the During F(Hfl) observational During Second Series blue blue continuum. & red points red (2) of optical A1240 A1549 A1216 Astrophysics the optical HST A)b A)• 0Iv] Om] at combined at only: wing core obtaining wing wing A) A) added number for was 80% only: continuum 80% HST HST combined is value the is deviates with ...... FOS Band TABLE of TABLE were that RESULTS ~tpeak less AUTOCORRELATION repeated LltPeak level. model dy) (days) (days) level. amplitude -0.5 -0.4 continua. 10.6 campaign. campaign. 4.6 0.7 measurements: 3.5 7.5 3.5 intervals 7.5 0.6 (3) 1.4 . 1.8 1.7 . . . . the a of we (to than of sampled errors. constant as a ultraviolet Mpeak The 26 JUE, were observed 25 can data lag .6.tcentroid a sample light represent -0.9 -1.2 14.7 many 4.8° RESULTS function l.2b centroid 6.9 7.0 4.3 8.3 2.4 0.6 (4) Data -0. HST of conservatively between applied was The points of FWHM (days) 0. curve in 34.0 15.3 variation l component 6.7 8.4 cam­ 7 times recorded. amplitude principal if points such monitoring System delay days as the of to was the observations. the in to Tmaz 0.90 0.92 0.90 the 0.79 0.99 0.96 0.81 0.87 at 0.80 0.81 0.94 a 0.7 or (5) actual the were to then build the way time less estimate sampled result starlight achieve of Vol. optical 50% to cam­ as sam­ (i.e., vari­ then shift shift up the 97 to of a 1995ApJS...97..285K in in radially spond inverse i.e., the was HST sponse signal-to-noise component continuum decidedly dependent lags. them. than taken the this that the try vations required not the be poorer SWP seems scribed campaign although and of of or The ization is tween tained not uncertain; between uncertainties N v N scopic are other marked No. somewhat The The The We the radius zero. centroid, the of nearly shape original blue cross-correlation valid, yet undertaken the finding. distinguish 2, the the X response the campaign. camera 1240) the words, here response C the The have clear with results most observations 1995 is lags monitoring lines be temporal correlation in will The stratified C lines red improvement IV line wing the slightly of before line-emitting the of nonzero. we terms UV ruled IV suggested identical, in also line emission red more HST for be of © campaign, are which core changes described in the rapidly that observations UV cores, line In problematic to can that particular, in of characteristic 7. magnitude of of and the required. the American wing the of measured yields response ratio the any the out, transfer SUMMARY to the the clearly of any Thus, He and more (0 ionization profile and the than sampling state various C affects original are optical address pure although between Evaluation observations highest extent blue search measurement km II IV case, reported to lags and line of which degree with optical analysis kinematics JUE and a >..1640. rapid -1 -emitting an an some in with continuum as region C weak between radial s- changed function. core(-3000km the of-2 more the is are of because order determination to reported well it IV continua lines show intensive that day in 1 for no campaign questions better fairly ionization and of ::;; ionization structure. occurred is this AND than -90% lags be the Astronomical of continua component He still responds 1993 suggestion here and The the are significant already the motion, Av::;; as or detailed of these slightly confidence days of preliminary II lower effect measured quite region in of a subtle. the the of less. the velocity-dependent CONCLUSIONS much time the further magnitude, of region, Uncertainties preliminary confirm most March-May. here fixed-pattern variations. confidence that is response NGC this set + for Monte that location response uncertainties that were possibilities no at uncertainties The is 3000 clear decidedly lines ambiguous, is level less signal-to-noise either analysis thus resolution and of He as larger highly There that region of the larger of barely s- required the time investigation left consistent 5548 original large than ultraviolet BROAD-LINE for can the radial II the km 1 and (He that contamination Carlo analysis have to ::;; beginning the BLR infall and this of of and Society than The the analysis existence than are Av::;; ionized delay the be He of s- 2 cannot as that discernible the This lag the in artifact blue-wing any II more days, motion resulted result N these 1 of highest in that both simulations has 1.2 ascribed indications the 1988-1989 or ) although differences X most than II depend the the (Paper CCF line v, 1.2 O appear 1640 with these here were an program velocity­ response and between outflow. spectro­ days. km ratio a geome­ it but rapidly but formal gas will under­ lag higher be days. obser­ of rather cores, in range rapid of infall has • were peak does a can­ ion­ N v N s- and lags in ob­ the the the are be­ de­ lag re­ I), re­ REGION Provided on an be by In to in to of 1 it a a ) days; the was basic stitute CCF and achieved ization ground-based same the variability the have that uum response preliminary pear per. shorter out cores emitting dom, difference gets variations tinuum this tical result. what by some sibility 90% 3783, find, and and at evidence dial dial days, idly lags Monte response pendent IN 6. The 4. We 5. 2. 3. this 1. the by period line of highest with found than might velocity N v N While optical motions. continuum confidence brighter, behind the in found however, The Our As conclusions: The is We see and The galaxy. is with smoother BLR or AGNs. we also the The time a Carlo the that blue acquisition suggestive lines at wavelengths. is subsequent core indeed in >..1240) response region longer Paper time larger time. fifth the find have that in variations fifth changing UV observations longer H,8 between occur in an present a be in 1992 more gas red our for temporal the NASA continuum whether gas time-series wing slightly our lower the or this simulations respond Paper uncertainty ascribed that VIII. and emission-line data the that year Neither complete i.e., is examined There admittedly wing the amplitude VII). earlier and what line the than (the level. wavelength November-1993 lag on light in wavelength extensive earlier source. UV BLR of ofa of ground-based the optical is radial other obtained them. the radial of rapidly, blue short behind I. how of and papers, wings of smaller line the Astrophysics about the are He level those curves Furthermore, frequency continuum The continuum to virialized coordinated contributions to the infall C reported amplitude kinematics analysis variations year IUE C wing, also much wings) 4 II cloud velocity in timescales, apparently an IV continuum reduction indicate Cross-correlation motion. of-1 continua than highest weak of respond analysis IV years peak twice >..1640, those at and a responds here infalling variations shows continuum are continuum. time confidence nor some of preliminary X program shorter but 1549 might lower motions monitoring this system, responds indications of day. described here of optical that variations the of outflow gas we ionization September. appears that delay by it indications the of is which that optical vary and involve more ground-based the could we emission of response is on (the have less component ionization allows more be confirm variations Data variability wavelengths, -1 the optical not in UV in the find interpretation although observations the with NGC due can are ( variations rapidly somewhat than line - is way has indicate NGC to lag in monitoring 1988-1989 undertaken day. clear optical rapidly predominantly the continuum of have that 11 indicated. organized lines to be us some space-based get System little detail between cores). line These time the that a continuum/H,8 that 5548 the contamination 1.2 days) optical ascribed to when lines. much "harder" 5548 the Some more how than been it is (He of UV coverage if velocity-de­ and reach that continuum indications C days higher than for is in are as and greater any more the higher data IV covering The not much than the II and yields the this will the on ( Lya, find contin­ rapidly though filtered shorter or at We simple simple by profile X some­ 18-19 C at either to phase NGC some clear 1640 con­ least con­ pos­ ion­ ran­ rap­ as and line this IV UV 323 -2 ap­ op­ pa­ the the we ra­ ra­ do no of of as at it - a 1995ApJS...97..285K spectra counts and archive Telescope To grating, versus were prior spectrum object's any assumes of of nately, plummeting spectra approximation), low background Earth's magnetic Verification. -90% tions. the scope edge coinvestigators responsible NEWSIPS line. problems special 324 of ley, portion especially and and Pierre Keyes, tience As The Assuming A scattered the We We At We his first NEWSIPS of geomagnetic latitudes certainly model Peter the to Science to a the the scattered blue-side those also time the landing pointing thank are Bely, consequence of occurring no and (Cunningham redward be order, the intrinsic due thanks Anne that Science ofthis is Goddard work stars (HUT). but deeply Stockman, compared scattered-light object wants for wish pipeline, first light ;$1 © hard in to for model Chris wavelengths detector sensitivity it The Data that all Richard also Kinney, the Cerenkov irregularities %. semirandomly and discussing American calibration. is go light project. who of running HST detector information to others within spectral of Planning higher one work. to field. count indebted The near model relative Blades, graciously to Cathy the Analysts, Archival elliptical with acknowledge Space geocoronal thank felt and is of Ralph to servicing can Cindy much & Griffiths due the charged-particle Michael However, as these the They K. "solar that by a rate, the Caldwell radiation for of energy is which Imhoff, experiments the Flight multipole Howard well. derive amount and and the center to the T. to the FOS roughly in project's answering Bohlin, FOS Astronomical galaxies their higher the made Taylor, A2. findings, from the FOS corrected across scattering share K. the blind" following same FOS Scheduling mission by A Lya for scatters distribution Rosa Center itself, HST the to the THE spent versus entire contribution the plot Joy 1993; of rulings. background ~30% Bushouse, flux of available his kindly sensitivity direct quadratic is in geomagnetic the who this factor support show the ratio and SWP scattered predicted data sensitive (ST Nichols, SCATTERED-LIGHT scientists of and were scattered-light our the parallel valuable of calibration FOS we Rosa for diode GHRS off off background array; STScl the ratio at not Al. Tom first-order Another /ECF), 1993 of unexpected offering in Branch many success from spectra as gratefully the the an FOS high done the as background Instrument the of particular John 1993; only in THE array. with in Society was estimate due did grating to light well ruled Wheeler. it or and WFC December staff several scale new and the time the geomagnetic background count inquiries BACKGROUND field is photons during HUT Peggy through for not spent Fitch, CHARGED-PARTICLE of to the effect and us small, Ayres as G scaled their Goddard Prelaunch versus FOS engineers, members: light. gratings. acknowl­ factors charged experiments the with observa­ is 130H the their is the ultraviolet warrant G or project the rate related KORISTA of data being 190H Team • the hours is Extra APPENDIX Tony Stan­ Science count pipe­ off HST staff, 1994), detector's at tele­ with into on and CONTRIBUTION the Although by that direct the strong Provided pa­ grating, across any have most for source counts particles three High a latitudes One derived grating experiments total wavelengths the rate constant objects demonstrate irregularity upturns.) first-order Verification. wavelength been were -0.07, the effect extreme stars Resolution ET sensitivity. then 04885a(N. in tory); background, Program (University (B. grants cies, Ko Astrophysics SUBTRACTION support based for of G. T. Williams Wu, 1824 E. Barthel, inclusion to we of at minimizes within We diode Finally, the A the J. (Fitch by Storchi-Bergmann, J. object recently of their performed AL. 857/13-1 M. all (spectral the cannot is BACKGROUND the and which A. including and Ferland, component different various are G130H but just and AST-9112870 the (Sirk P.); wings TO spanning light counts time for along Meurs, maximum support array, the R. for the W. dependence pleased (STScl), & on STScl counts it However, Spectrograph we A the the G. THE NASA of BMFT takes Russian measure shown D. Schneider Earth's & grant Zheng. presence detected rose the of shows grants recent the types (Universitiits-Stemwarte (±1000 ground-based B. thank the grating California, P. scattering for ground-based spectral Bohlin with this Blandford, the in E. effects grant BACKGROUND and of list ofthis to M. -1137 across rapidly into entire all A-01-057 Perez, M2 the Y. to grant this writing. difference acknowledge analysis a following: magnetic NAGW-2678 Astrophysics a ofauthors: Gondhalekar, R. A. the Basic the gratings at (Ohio of A) of very measured be G0-3484.0l-91A. Kondo 1985) minimum account distributions E. I, 1993; of project demanding zero-sensitivity I. Giacconi, scattered the the such ( optical present to of G deficient of Verbundforschung K5 GHRS) A. blueward S.). Berkeley); the van strong 190H T. Science photons the -5500 observatories FOS diode by observations demonstrated (Crimean Robinson, State III, Rosa in uncertainty field (/UE-GSFC), in and J.-L. by Groningen, Rosa National LSFs the B. the path in and the financial data, NASA diode whose background light or correlation. was array. on H. both (K. Balick, University), the 1993). program. spacecraft D. A. G l Courvoisier, (up Foundation count were in NASA ( the G2 scatter might Data average Gottingen), S. 1994) In for Kazanas, derived and zero-sensitivity 30H Astrophysical random H.) array E. sides region through to relative Stockman, We Hopkins V), principle, Even through Science in also used support the T. A Rokaki, rate the M. those -0.5) and produce grating. Long-Term the zeroth-order Astronomie System finds also and where charged-particle J. G l is of to by position directly, likely during in (Additionally, in J. in Balonek, related (a background. angles AST-8957063 grants the C. NAGW-3315 30H amplitude be grant R. this the acknowledge in several Ward, -12% the of Foundation, the that Ultraviolet ESO due light first-order J. F. analyzed. FOS FOS U and the the presence M. spurious Observa­ directors program grating, G Gl30H Science L. nfortu­ McKee, NAG5- off -90% region Vol. to if to in C&EE 94-02- 190H space­ Cutri, Space HST from Sanz, agen­ C.-C. data DFG R. near P. and just one the the the the D. is 97 E. 1995ApJS...97..285K which broad positions spectra addition, Galactic absorption upon In ground these not particle diodes observed measured spectra second-order In Even LSF LSF. regime object's No. 15 tion. To The While addition, FIG. Figure A significantly 2, plus of The data. at put broad emission fall much (our 1995 where in 18.-Ratio was the counts the spectral background absorption we these the of spectrum the 18 shape background each within lines, calibrated shortest © scattered adopted the the do emission we greater diode spectra light scattered American narrow over lines not plot grating absorption LSFs of energy blurred and of the the array into the know lines. is calibrated the sensitivity indicated the correction). and Gaussian light, obtained were spectrum, G190H '-.._ lines, ::550%. .E .,., l:Il .! ;:! "" ...... i:: 0 0 Q) Q) spectral counts distribution light are ratio first by POOPS response scattered-light 0.1 0.2 This 0.3 0.4 how we good errant features optimally local Astronomical overwhelms INTERCALIBRA order. of In of that do spectra. was wavelengths, are much in with features functions the light background and this fits particle the know The fits zero-point to due the not 1200 adopted and This in the to they the "spectrum" regime G l of to positions aligned largest the a the to We were that two the the trivial the 90H background approximately background scattered-light to the fell the mean observed counts BROAD-LINE measured 1250 total total detector fit where it spectra gratings heavily it wavelength spectrum first-order off differences particle Society was in the task, is TION of rapidly spectrum to background background wavelength, is not the broad small the the roughly since 1300 mean were smoothed sensitivity on to necessary Galactic model their equivalent total background detector OF should white light, the with the Observed contribution compared between corrections • emission-line APPENDIX the required. spectrum number of THE Provided REGION flat, total same 1350 are increasing Galactic counts each count the light via render absorption by sensitivity falls that when assumed background. G l spectrum the Wavelength of the the wavelength illuminating grating. is to We off observed rate Galactic made to we 90H virtually two 1400 the broad the method begins absorption the IN B the more widths profiles. wavelength. by used know as effects first-order extreme first-order lines is AND to AGNs. in total Because measured takes the counts PSF lowest, rapidly be (A) to the the absorption-line 1450 scale, described indistinguishable to precisely A lie it. The of observed become scattered NASA admitted G individual FOS spectrum on lines be within plotted any corrections VIII. 130H the all light we light resulting the with approximately in scattered-light G130H are 1500 of contribution attempted the shape the as in important ~ Astrophysics everywhere number dominates wavelength the SPECTRA light by very a 0 which § spectra. zero-sensitivity function relative .5 the profiles; absorption 2.3.2, fits were of pixels weak and whose 1550 from large a of of is to combination G190H found of regions when we counts in contributions of over corrected in of contribution longward (diode) measure amplitude thus, wavelength aperture. one the the this their attempted 1600 features the to the Data where total range object, in the least regions LSFs vacuum be scattered than the combination the assuming ofgeocoronal mean Assuming background for 1 of contaminated is %-2% System are the object 0.08-0.64 for positions insignificant especially the to of a the constant of G wavelengths. weak excess the measure the spectra ! wings our light. wing 30H in spectrum. all Galactic charged­ that the G l and observa­ of of of In to of in A. along those back­ were Lya. 30H first the the the the the the the the the 325 for by lie In 1995ApJS...97..285K those dependent in Below wavelengths photometric overlap G l individual illustrates Finally, within A), where brate pixel "blip" signal-to-noise spectrum in measured range 326 The 1991 1 pixel There There In Next FIG. 1. the the 90H vertical while error constructing and the Sensitivity in FOS overlap 1574-1605 either we in the 19.-Mean in we region. photometric spectrum this are are two the 1992. discuss rather the eitheJ in lines these in overlap and epochs, inverse-sensitivity compared © several joining several a repeatability 1594.60 C its the wavelength G l small region. designate American ratio are IV First, local This than differences degradation.-There spectrum) interval 30H G130H separately in A profile, the at region in known reasons procedure, shift across is the degradation uncertainties, wavelength the and least I ~ .. that ' ' 0 the ~ ..... data Unfortunately, s Ill Ill .... combined QO Q) tJ that very the (solid 1590-1600 G l in scales. between 1580-1600 25 of G l 20 1594. 10 15 of of wavelengths as 5 0 the 1570 sources do. the low, flux why might eight 90H between the Astronomical the a large KNOWN ~~~~~~~~~~~~~~~~~~~~~~~~~~~~ 90H line) functions large peak Extrapolation 71 will differences (typically Thus FOS we and mean scale, data spectrum, has known spectra and produce as A, 1595 due of introduce made mismatch A and a cross-correlation 1575 the blue where as been the A, we photometric error do the GI interval has as G to are indicated SOURCES and differences differed 90H red were potential not 130H well two no uncertainties peak side with at been the tracked, systematically a -1 the the core 1597 attempt (dot-dash have better two of as small left for sets between 1580 Society for %, the of and a G l -1 accompanying the b¥ gratings degradation of these with in the A, this but an sources of G and 30H %-2% alignment G l errors quoted the wavelength ::52.5% Figure OF of 130H to arc C line) mean probably epoch. comparing 90H two in KORISTA the the it reconcile C IV of in Observed 1585 were spectrum comparison PHOTOMETRIC • APPENDIX seems the spectra IV in level "rippled" of the the emission two JD spectra gratings above in 19. Provided spectra spectra joined: the emission photometric placement in C FOS all in 2,449, The in small spectra. a to scale the C IV in bit the some but Wavelength either 1590 the (see have IV was the in peak 1594.60 (Bohlin ET is uncertainties is blue-side line in larger across small 112 errors line broad spectra a beyond the 1.4% likely overlap line. Appendix joined C the handful individual The AL. leveled by spectrum) of lies in observation overlap which error and at the differences ( 1 the overlap Figure 1595 ( emission the the 1993a; G l a ERROR in ::51 the (A) region along sensitivity this a) manifestation 1594. spectral to two the off that 30H % ) of overlap falls for ends NASA D). the in region last pairs since epochs. or 19 71 in aroJmd first Lindler the gratings the region. well-centered affect spectrum in G 1600 line A, the a shows is of arc between IN image core small l the wavelength few respectively. mainly of the 90H of 1992. region of flux Astrophysics flux the line the THE G l & We -10% overlap the and This pixels could spectra. the of peak additive upon calibration. Bohlin spectrum FOS and 90H for does 1605 the also two gratings. these the wing in mean FOS figure spectra and the of which not profile. two the this spectra. result region and and lie, note The the 1994 of red two shift G l be diode Gl90H sets on fashion. the typifies flux at G l wing Gl90H 1610 90H occurred rippling (Lindler done that of Second, uncertainties. (the and in average, pixels Data of 30H C a calibrations, array, This wavelength of IV grating "blip" a data references reliably and nearest the significant what line spectra. The spectra corresponding in the System & region mainly C are could Gl30H 2. the in Bohlin in IV spectra 7% uncertainties mean occurred wavelength­ is the to emission the differences Third, at where below Figure (typically spans as cause therein). intercali­ between overlap, G upward -1621 spectra Vol. well 1994). fluxes, in 190H line. the the the the the 1 a for 19 to 97 as 1995ApJS...97..285K dependent. First, the No. spectrum, from of 2,449, PSF miscenterings. via these will aperture offsets correcting include the photometric effects essentially campaign. calibration probably skewness excursion the 3 after due distribution, This separating of array Here magnitude ular desorption, optimal nately, Y-base affect There It The Problems Problems the The 8. 6. 4. 7. 5. 3. 2. the the G190H rapid produce 1 2, to is forthe to %-3% jitter onset. five large the the Thermaljitter.-Mispointing Thermal-breathing Filter-grating-wheel Pointing Short-term Throughput Long-term emission has 129.03, image, important 1995 on combined this in manifestation focusing units the the this color position were for telescope ensures dates. temperature center of the been the while of for is wavelength systematic observations effect diode data from of 4~3 In level © drift or image the 7 the 4-6 wavelength-dependent (0':073 errors, a the about terms, due FOS effects the Y-direction respectively) the and five factor "outgassing," American errors.-ln lines drifting X The pointing-error of a on of observations. well-known is the was spectral array. spectral and are was error to that miscentering NGC to 1 bottom changes.-Long the 8 focus expected is photometry ':4 epochs timescales the assuming 32 the G remember [1 were insufficient optimal of appear of of roughly of effective found not is, offsets the electrons changes 190H shifts a] of problems diode positionally Y-base The 5548 1/2 effects of the more changes of ejfects.-A or effects missing, image image noticed effect panel lead the repeatability larger (FOS this where course, errors about to to to on-board Astronomical of2-4 exposures of which position spectra thermal twice array, these that flux aperture, concern, distribution, Since are be be as units) be in to that the program, are in of shielding of drift.-A drift.-The 1 PHOTOMETRIC and (about the 1-3 days the small about semirandom the until wavelength-dependent and which much 0.8 a are calibration problem induced Figure optical pixels timescale not, dependent of have Y-base as since flux along magnetic loses change the and telescope negative in the at G and the instability long pixels GIMP 2 large taken 3, (less 1993 130H limitations.-The as any since well-centered the + calibration is 0':25 less diode indicates been image thus ( the telescope the 7, 3 of 20 more shift the at 0.5-1 2 telescope of BROAD-LINE offsets compared by one most 4 center significant in in the along spectral 23, pixels than severe just the correction this Y-base June, throughput centering spectral is they star field, counts FOS [ Society Y-base have corrected effects crosses focus on in 44 the array in nature. shifts can negligible. instrument light 24, diode) problem - one pointings writing, are the 1 % ) and orbital that Y-base the of DI. FOS 10% along occur occurs than Y-axis and after no errors. clearly assembly. units, ANOMALIES and occurs image the centered were direction rather position orbit from slightly 5-7 with FOS image FOSX-direction). the observations using the impact error THE of were given ± is in they Y-direction diode APPENDIX • these units] 33 the variations position. photometric on day as in of When 5% done as the spectral anomalously in any standard or Problems repeatability earlier In should a REGION the see Provided due of from than G130H the in well is the the a =JD required post-pipeline time orbital about as would particular, FOS level the /night of about the object result on The important loses the observations curved the array blue to in various blue-side and NGC preservicing the combined, modeled, the the amount were any electrons "thermal since sudden real have positioning resolution and amplitude This Y- 2,449,099.04, "DROPOUTS" ofNGC 8% star more have have IN end 2.8 image the of terminator. timescales. produces as 5 Earth's in aperture to of IN and (covering and time 5548 D jitter unaffected. errors is of errors the by elements of low the pixels Science THE calibration position is align a our of wavelength-dependent. timescale been detector occurred light the AGNs. oflight miscentering and the X- recalibration. consistent on 6 but G130H the the leaving in aperture breathing" 5548. these by had a campaign conclusions magnetic may was lower mission rather height these of few directions, smaller filter-grating-wheel the a 1 a % FOS along itself or both from drastic if 25%-65%, it G Verification this NASA As a been -20-40 of a supporting is which 130H 2,449,103.12, minutes diode last two have Simulations VIII. with smaller Two change for on spectra the G believed (slightly the directions, determines image, DATA noted the ofa the than effect is with 130H drop than solar completed. field, account the data the "Y-base affected of other accurate for in photocathode overlap spectrum is array FOS diode These about Astrophysics respectively, just the aperture a Y-base contained with in is NGC sources after above, the large these with or in it panels, and positive is has SET wavelength-dependent) apparently that the shape (Koratkar effects secondary Y- will equal counts occurs influenced loss scatter show and ( the of variability problems crossing drift," this region the G components the ( 4 =256 secondary 5548 and exposures. 2,449,118.99, to their Note, units, changing the 190H be and For position ':3 of of of loss had and any about rest. effective to data ofthis Y-base that X-directions). within due square) for error somewhat the HSTFOS light. remaining and on-board Y-base the quoted combined of this with the oflight however, been depending residual damping can & data the mirror Second, the a the set image to by do O':l mode during Taylor Data drift landing error red data mirror might is direction, This Although the telescope day GIMP. a last to G our two not used. edge on along aperture. accurate units), 75 above. maximum 130H end highly some support of 2,449,119.99, broad /night on set, the photometric were for GIMP campaign more value. could affect choice gratings. Because the (the that ( error System out the result the 1993 of warp 1.4% on upon the and of The Because blue a the exposures loss narrow in the extent. in course also image problems as wavelength­ focus few mode wings the these the sensitive to terminator. diode occur the could ). perpendic­ the correction structures. time. because rms) in of drift measured deflection side. oflight. the aperture, about Unfortu­ expected present. grating) minutes G and the relative 1 2 %-4% due of errors of peaks of of 190H Their of diode array if years be error from after and this 4~3 327 the the the are for the the 1- to 13 at of to 1995ApJS...97..285K in lation we band "dropout" flux, 328 However, two this the matched the height uncertain ofNGC the shifts 50% shifts (producing errors. angle. centering dropout FOS FOS how diode observation. offering We -1 In FIG. Figure Parallel created G diode ", PSF note the displacements (JD but principle, 130H campaign. Y-direction of in deviations ranging spectrum array We 20.-Spectrum Because expected the the us 5548 off events. became that 2,449,099.04, reasonably 20 array in procedure. via "dropout." wide-field found and a G information wavelength "dropout" © telescope the were for practice spectrum 130H the the after from American one spectrum ( length diode the the A 0~7). was Nearly an in large that only nonrepeatability (producing properly it might would spectrum first detector declination increasingly The a of camera well then emerged the The pointing the These array few wings ...... of ..., detecting 0 '"C '"C l%l :;:l ..c 0:: which ~ the 0. CJ QJ QJ >< " > "' Ill Ci QJ QJ >< ;:! G JD shifts). was dashed-line all "dropout" from wings 130H the with be "dropouts" 0.8 0.6 ratio 0.2 0.4 divided be remaining 2,449,118.99, hundredths of derived. focused becomes Astronomical able (WFC) were on position a diode is by photometric the the from that of for of The substantial loss and an the and the bad the this to these accompanied Gl30H WFC function the by interpolation The in derived G PSF convert transformation Earth array) compared observed image wings exposures deviations approximation ratio. the 130H angle the few unreliable. had "dropouts" solid-line to functions due observations JD scaled filter-grating-wheel. is occultationjust G 0':2 displacements observations that errors), of and, via The exposure. lay the shifts flux 130H 2,444, to the in Society it predicted were function interpolation primary-mirror of near moved in to by simple by "dropout" of with are In right PSF in the light is observations, right correspondingly 119.99), and two good using is taken right addition, presently 0° at not expected a that which In and is shorter ascension off during simple ratio, and scaling the and KO ascension a this well Observed • in ascension the low-order throughout the prior in the offsets G Provided RIST the a the based all allowed interpolation and the G flux determined, information 130H zero-point edge unknown, the However, rotation the LSF. wavelengths. aberrations resulted 130H predicted to of FOS corresponding accompanying, in A upon use and actual in Wavelength the campaign, the which polynomial the of and large spectrum, This ET right a Y-direction of spectra the G much declination. G130H FOS G190H determination of in the declination 130H by AL. in wavelength position displacements but would loss were axes diode ascension so simulations. scheme a in ironically the accompanying To the fairly of the that on fit "dropout" oflight, the the (A) exposure. by and observations generally the three correct through array to indicate either error NASA unaffected, an which any offsets PSF of accurate HST we the They a to amount nearly the instances shift, low-order saved as would correction measured of must FOS and G side the spectrum, for in derived campaign. corresponded in image larger 130H the a are Astrophysics ratio, the the just large declination G LSF, of correspond us shifts recalibration have having have G corresponding relative of 190H the FOS from color 190H where and "dropout" as than on polynomial JD from the the mispointing which calculate occurred in "dropout" lost observed. the is 2,449,099. X-direction. We exposure. a dependency parallel Y-base mean amplitude the those spectrum. telescope complete FOS the nearly to diode thank involves are to adopted roughly of loss offsets throughput flux the during observations, expected essentially Data and to was the exposures See The all in array of R. of This the photometric offsets. in pointing loss correction X-base expected We time. text the of The moving C Griffiths fitted light in in cause the halfthe the detector System IV the match the is of the for then spectral effects from emission-line 1585-1600 made This was reacquisition data offsets through simulations, light explanation units loss had X-direction of the during function scaled had given for height is less the pointing interpo­ position on oflight, of relative for further core shown (along image. Vol. kindly in large, these these large than that this our the the the for of of A of 97 1995ApJS...97..285K --. Bohlin, Blandford, Beckert, Ayres, problem spectra G gratings metric polynomial shape" C, for Day Poissonian FOS might taken relative ranging were placements but spectrum; subgroups subexposures G l centered resulted ratio No. several emphasize from extent, others curves In the tion polation exposure. assumes ratio. ed. 130H The As This This It 2. 3. 1. the the 90H all continuum one 2, J.C. is with 34 lost examined days included other T. we Systematic Telescope Filter-grating-wheel This between epochs. R. typically following 199 strongly conceivable (e.g., errors, 1995 for individual D. correction more statistical in anomaly on R.1994, photometric "dropouts") spectrum over and (day image C. Blades & described becoming R. had that on 3b, C., the the various this This either 18, were epochs that fit 1993a, D., variations), © was of & counts in FOS the had so -±3% unaffected no and 34 worst was (or any 20, This Newberry, Proc. one is &McKee, American the the affected centering FOS separately and result at may the centering fitted are expected, compared, ), S. diode side. way strongly amplitudes Y-base private (Poisson days to spectra readouts) was continua 21, some no subsequently intrinsic appeared J. of the G l in combined that photometric Workshop less Instrument the cases in resulting the the Osmer(Baltimore: not variations to is corrections these Appendix in through of 34, 30H attempted the 35 anomalous consistent array emission important communication well-understood ±8% spectra on M. C. middle, wavelengths a drift G l even independently be errors via were affected and and few errors: for F. nonrepeatability: since middle V. counting) certain "anomalous" and 90H and wavelength-dependent correct, Astronomical we "U"-shaped, of on 1982, ofless about broadband (higher of "corrected" 1989, changes Sci. G l percent after a 36). for accumulated Calibrating 62.50 occurring this the emission often ratio C. G l the large with error used spectrum. lines 30H for ±32 were Rep. ApJ, with the both PASP, (and of occasions "U-shaped" As 90H It image we the G l than "U-shape" but only than STScl), the of the counts standard was CAL/FOS-115 enough to is s Gl90H in observed 255, Y-base photometric (i.e., of and attempted. an 90H had mean. the pixe1- gratings thus determining similar for correct 101, the spectral this sources region interpolation, Hubble combined ±1.5% lines the spectra additional in at Gl30H characterized i.e., on 419 G l BROAD-LINE anomalous some corrected spectral the 234 others. exposures counting ± 849 less in the writing, than most units diode 90H to generally 1 13 Society spectra across The deviations in for several amounted near Space spectrum a smaller the in about of combined uncertain) produce (other kind images Y-base D2. 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