Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://hea-www.harvard.edu/~pgreen/Papers/postcos_04.pdf Äàòà èçìåíåíèÿ: Tue Nov 16 21:40:25 2004 Äàòà èíäåêñèðîâàíèÿ: Tue Oct 2 01:32:20 2012 Êîäèðîâêà: koi8-r Ïîèñêîâûå ñëîâà: arp 220

The Astrophysical Journal Supplement Series, 150:165 ­ 180, 2004 January
# 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A.

A

EMISSION LINE PROPERTIES OF ACTIVE GALACTIC NUCLEI FROM A POST-COSTAR HUBBLE SPACE TELESCOPE FAINT OBJECT SPECTROGRAPH SPECTRAL ATLAS
Joanna K. Kuraszkiewicz and Paul J. Green
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; jkuraszkiewicz@cfa.harvard.edu, pgreen@cfa.harvard.edu

D. Michael Crenshaw and Jay Dunn
Department of Physics and Astronomy, Georgia State University, Astronomy Offices, One Park Place South SE, Suite 700, Atlanta, GA 30303; crenshaw@chara.gsu.edu, dunn@chara.gsu.edu

Karl Forster
California Institute of Technology, 1200 East California Boulevard, MC 405-47, Pasadena, CA 91125; krl@srl.caltech.edu

Marianne Vestergaard
Ohio State University, Columbus, 140 West 18th Avenue, Columbus, OH 43210; vester@astronomy.ohio-state.edu

and Tom L. Aldcroft
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; taldcroft@cfa.harvard.edu Received 2003 July 24; accepted 2003 September 12

ABSTRACT We present consistent emission-line measurements for active galactic nuclei (AGNs), useful for reliable statistical studies of emission line properties. This paper joins a series including similar measurements of 993 spectra from the Large Bright Quasar Survey and 174 spectra of AGNs obtained from the Faint Object Spectrograph (FOS) on the Hubble Space Telescope (HST ) prior to the installation of COSTAR. This time we concentrate on 220 spectra obtained with the FOS after the installation of COSTAR, completing the emission line analysis of all FOS archival spectra. We use the same automated technique as in previous papers, which accounts for Galactic extinction, models blended optical and UV iron emission, includes Galactic and intrinsic absorption lines, and models emission lines using multiple Gaussians. We present UV and optical emission line parameters (equivalent widths, fluxes, FWHM, and line positions) for a large number (28) of emission lines including upper limits for undetected lines. Further scientific analyses will be presented in subsequent papers. Subject headings: atlases -- galaxies: active -- quasars: emission lines -- quasars: general -- ultraviolet: galaxies On-line material: color figure, machine-readable tables

1. INTRODUCTION It is broadly acknowledged that the quasar central engine ( presumably a massive black hole with an accretion disk) photoionizes gas lying farther out. This gas emits broad permitted emission lines that are distinctive of quasar spectra. At first glance, quasar spectra look quite similar; this may be the result of simple averaging. Baldwin et al. (1995) showed that although the broad line region (BLR) consists of clouds with a wide range of properties (gas density, ionization flux, and column density), the bulk of emission line flux is most likely produced in the g as clouds with the o ptimum parameters for efficient emission in that line. A closer look at the quasar spectra, however, reveals that the spectra differ in detail and, intriguingly, behave in a correlated manner. For example, it was found that active galactic nuclei (AGNs) that show strong optical iron emission (Fe ii k4570) have weaker [O iii] k5007, and narrower, blueasymmetric H lines. This set of correlations was found to be the primary eigenvector of the emission line correlation matrix 165

of PG quasars studied by Boroson & Green (1992). This eigenvector 1 was later found to correlate with UV properties such as C iv shift/asymmetry (Marziani et al. 1996), Si iii]/C iii] ratio, and C iv and N v strength (Wills et al. 1999; Shang et al. 2003). Since eigenvector 1 was found to correlate significantly with X-ray properties (Laor et al. 1997; Brandt & Boller 1998), which are determined in the vicinity of the central black hole, it was suggested that differences in emission line properties revealed by eigenvector 1 are caused by differing central engine parameters (e.g., L/LEdd, accretion rate, orientation, and/ or black hole spin). It was found that eigenvector 1 together with eigenvector 2 provide a parameter-space in which all major classes of broad-line sources can be discriminated, constituting a possible ``H-R diagram'' for quasars (Sulentic et al. 2000; Boroson 2002). Another famous correlation involving quasar spectra is the anticorrelation between the equivalent width of the broad emission lines and the UV luminosity, called the Baldwin effect (Baldwin 1977). The appeal of this correlation was soon realized, since the luminosity of a distant quasar could


TABLE 1 List of Obje cts and Spec tr a Designation (J2000) (1) 0005+0203 ................... 0006+2012 ................... 0018+1629 ................... 0020+0226 ................... 0020+2842 ................... 0029+1316 ................... 0039þ5117................... 0044þ2434 .................. 0044+1026 ................... 0048+3157 ................... 0053+1241 ................... 0103+0221 ................... 0104þ2657 .................. 0109þ1521 .................. 0110þ0216................... 0110þ0219................... 0120+2133 ................... 0122þ0421 .................. 0124+0343 ................... 0139+0131 ................... 0143+0220 ................... 0201þ1132 ................... 0206þ0017 .................. 0217+1104 ................... 0235þ0402 .................. 0238+1636* ................. 0241þ0815 .................. 0251+4315 ................... 0256þ3315 .................. 0304þ2211................... 0320þ1926 .................. 0336+3218 ................... 0347+0105 ................... 0351þ2744 .................. 0357þ4812 .................. 0417þ0553 .................. 0423þ0120 .................. 0424+0204 ................... 0452þ2953 .................. 0456+0400 ................... 0516þ0008 .................. 0519þ4546 .................. 0552þ0727 .................. 0630+6905 ................... 0741+3111.................... 0742+6510 ................... 0743þ6726 .................. 0804+0506 ................... 0813+4813 ................... 0830+2410 ................... 0838+2453 ................... 0851+1612 ................... 0853+5118 ................... 0909þ0932 .................. 0948+4039 ................... 0950+3926 ................... 0955+6903 ................... 1001+5553 ................... 1004+0513 ................... 1004+2225 ................... 1017þ2046 .................. Name (2) Q0003+0146 Mrk 335 QSO 0015+162 Q0017+0209 QSO 0020+287 PG 0026+129 WPVS 007 Q0042þ248 MC 0042+101 Mrk 348 I ZW 1 UM 301 CT 336 QSO 0107þ156 Q0107þ0232 Q0107þ025A Q0107þ025B PG 0117+213 PKS 0119þ04 NGC 520.48 PHL 1093 Mrk 573 3C 57 Mrk 1018 PKS 0214+10 PKS 0232þ04 AO 0235+164 NGC 1052 S4 0248+43 PKS 0254þ33 1E 0302þ223 0318þ196 NRAO 140 IRAS 0345+0055 PKS 0349þ27 PKS 0355þ48 PKS 0414þ06 PKS 0420þ01 PKS 0421+01 IRAS 0450þ2958 PKS 0454+039 AKN 120 PKS 0518þ45 NGC 2110 HS 0624+6907 OI 363 Mrk 78 PKS 0743þ67 Mrk 1210 3C 196.0 B2 0827+24 NGC 2622 Q0848+163 NGC 2681 QSO 0909þ095 4C 40.24 PG 0947+396 NGC 3031 0957+561A 0957+561B PG 1001+054 PKS 1001+22 J03.13A J03.13B Typea (3) Q Sy 1.2 Q Q Q Q/Sy 1 NLS 1 Q Q Sy 2 NLS 1 Q Q Q Q Q Q Q Q Q Q Sy 2 Q Sy 1.5 Sy 1 Q BL Lac Sy 2 Q Q Q Q Q Q NLRG Q Q Q Q Q Q Sy 1 Sy 1 Sy 2/LINER Q Q Sy 2 Q Sy 2 Q Q Sy 1.8 Q Q Q Q Sy 1 Sy 1.8 Q Q Q Q Q Q Redshift (4) 0.234 0.026 0.553 0.401 0.513 0.142 0.029 0.807 0.583 0.015 0.061 0.393 0.780 0.861 0.728 0.960 0.960 1.493 1.925 0.336 0.260 0.017 0.669 0.042 0.408 1.450 0.940 0.005 1.310 1.915 1.400 0.104 1.258 0.031 0.066 1.005 0.775 0.915 2.044 0.286 1.345 0.033 0.035 0.008 0.370 0.635 0.037 1.510 0.014 0.871 0.939 0.029 1.936 0.002 0.646 1.252 0.206 0.000 1.414 1.414 0.161 0.974 2.545 2.545 NHb (5) 3.00 3.70 4.00 3.10 4.30 4.90 2.40 1.50 5.20 5.90 5.00 2.40 1.90 1.70 8.00 4.00 4.00 4.80 4.20 2.00 3.10 2.60 1.80 2.50 6.40 2.20 7.60 2.90 10.10 2.30 1.80 2.80 14.20 8.80 0.90 1.10 4.30 9.40 10.50 1.30 6.60 10.30 4.10 18.60 6.30 4.90 4.00 11.90 3.40 4.90 3.00 3.30 2.40 2.50 4.50 1.30 1.90 4.30 0.70 0.70 1.80 3.10 6.00 6.00 Spectra (6) 0005+0203oa 0006+2012oa 0018+1629oa 0020+0226oa 0020+2842oa 0029+1316[oa ­ ob] 0039þ5117oa 0044þ2434oa 0044+1026oa 0048+3157oa 0053+1241oa 0103+0221oa 0104þ2657oa 0109þ1521oa 0110þ0216oa 0110þ0219oA 0110þ0219oB 0120+2133[oa ­ ob] 0122þ0421oa 0124+0343oa 0139+0131oa 0143+0220oa 0201þ1132oa 0206þ0017oa 0217+1104oa 0235þ0402oa 0238+1636ob 0241þ0815[oa ­ ob] 0251+4315oa 0256þ3315[oa ­ ob] 0304þ2211oa 0320þ1926oa 0336+3218oa 0347+0105oa 0351þ2744oa 0357þ4812[oa ­ ob] 0417þ0553oa 0423þ0120oa 0424+0204oa 0452þ2953oa 0456+0400oa 0516þ0008oa 0519þ4546oa 0552þ0727oa 0630+6905oa 0741+3111oa 0742+6510[oa ­ oj] 0743þ6726oa 0804+0506oa 0813+4813oa 0830+2410[0a ­ ob] 0838+2453oa 0851+1612oa 0853+5118oa 0909þ0932oa 0948+4039oa 0950+3926oa 0955+6903[oa ­ oc] 1001+5553oA 1001+5553oB 1004+0513oa 1004+2225oa 1017þ2046oA 1017þ2046oB

166


TABLE 1--Continued Designation (J2000) (1) 1019+2744 ................... 1028þ0100 .................. 1030+3102 ................... 1034+3938 ................... 1041+0610 ................... 1048þ2509 .................. 1052+6125 ................... 1058+1951 ................... 1101+1102.................... 1106+7234 ................... 1117+4413.................... 1118+0745.................... 1118+4025.................... 1119+2119 .................... 1121+1236 ................... 1124+4201 ................... 1126+3515 ................... 1127+2654 ................... 1130þ1449................... 1135þ0318................... 1139+3154 ................... 1141+0148 ................... 1147þ0132................... 1148+1047 ................... 1148+1050 ................... 1148+1046 ................... 1148+1054 ................... 1151+5437 ................... 1151+3825 ................... 1153+4931 ................... 1159+2106 ................... 1159+2914 ................... 1204+2754 ................... 1204+3110 ................... 1210+3924 ................... 1216+1748 ................... 1217+6407 ................... 1219+0545 ................... 1221+0430 ................... 1223+1545 ................... 1230+1223 ................... 1231þ0224 .................. 1237+1149 ................... 1239þ1137................... 1240þ3645 .................. 1250+2631 ................... 1250+3016 ................... 1250+3125 ................... 1250+3951 ................... 1252+2913 ................... 1253+3105 ................... 1256þ0547 .................. 1256+5652 ................... 1301+2819 ................... 1305þ1033 .................. 1307+0642 ................... 1310+4601 ................... 1312+3515 ................... 1314+0201 ................... 1321+2847 ................... 1323+2910 ................... 1323+6541 ................... 1324+0537 ................... 1325+6515 ................... Name (2) TON 34 Q1026þ0045þA Q1026þ0045þB B2 1028+313 ZW 212.025 4C 06.41 NGC 3393 4C 61.20 PKS 1055+20 Mrk 728 NGC 3516 PG 1114+445 PG 1115+080A1 PG 1115+080A2 PG 1115+407 PG 1116+215 MC 1118+12 Q1121+423 Mrk 423 QSO 1127+269 PKS 1127þ14 Q1132þ0302 NGC 3786 Q1138+0204 Q1144þ0115 1146+111B 1146+111C 1146+111E MC 1146+111 PG 1148+549 B2 1148+387 LB 2136 TEX 1156+213 4C 29.45 GQ COMAE UGC 7064 NGC 4151 Q1214+1804 4C 64.15 QSO1219+057 1219+047 1220+1601 NGC 4486 PKS 1229þ02 NGC 4579 NGC 4594 IC 3639 PG 1247+267 B2 1248+30 CSO 173 PG 1248+401 CSO 176 CSO 179 3C 279 Mrk 231 Q1258+285 PKS 1302þ102 3C 281 HS 1307+4617 PG 1309+355 Q1311+0217 TON 156 TON 157 PG 1322+659 IRAS 1321+0552 4C 65.15 Type (3)
a

Redshift (4) 1.928 1.437 1.437 0.178 0.042 1.270 0.012 0.422 1.110 0.036 0.009 0.144 1.718 1.718 0.154 0.176 0.685 0.234 0.032 0.378 1.187 0.237 0.009 0.383 0.382 1.010 1.010 1.100 0.863 0.969 1.303 0.334 0.349 0.729 0.165 0.025 0.003 0.374 1.288 0.114 0.094 0.081 0.004 1.045 0.005 0.004 0.011 2.038 1.061 1.020 1.030 0.820 0.780 0.536 0.042 1.360 0.278 0.602 2.080 0.184 0.306 0.549 0.960 0.168 0.205 1.618

NHb (5) 2.60 4.80 4.80 0.50 1.40 2.80 5.80 0.90 1.80 2.10 2.90 1.90 3.50 3.50 1.70 1.40 2.30 2.30 1.90 1.40 3.80 3.50 2.20 2.30 2.30 3.60 3.60 3.60 3.60 0.90 2.10 2.10 2.20 1.50 1.70 1.60 2.10 2.70 2.30 1.60 1.60 2.30 2.50 2.30 3.00 3.70 5.60 0.80 1.10 1.20 1.30 1.10 1.20 2.20 1.00 3.00 3.20 2.20 1.20 1.00 2.00 1.20 1.10 1.80 2.30 1.90

Spectra (6) 1019+2744oa 1028þ0100oA 1028þ0100oB 1030+3102oa 1034+3938oa 1041+0610oa 1048þ2509oa 1052+6125oa 1058+1951oa 1101+1102oa 1106+7234[oa ­ oe] 1117+4413[oa ­ ob] 1118+0745oA 1118+0745oB 1118+4025oa 1119+2119oa 1121+1236oa 1124+4201oa 1126+3515oa 1127+2654oa 1130þ1449oa 1135þ0318oa 1139+3154oa 1141+0148oa 1147þ0132oa 1148+1047oB 1148+1050oC 1148+1046oE 1148+1054oa 1151+5437oa 1151+3825oa 1153+4931oa 1159+2106oa 1159+2914oa 1204+2754oa 1204+3110oa 1210+3924oa 1216+1748oa 1217+6407oa 1219+0545oa 1221+0430[oa ­ ob] 1223+1545[oa ­ ob] 1230+1223[ob ­ od] 1231þ0224oa 1237+1149oa 1239þ1137oa 1240þ3645oa 1250+2631[oa ­ ob] 1250+3016oa 1250+3125oa 1250+3951oa 1252+2913oa 1253+3105oa 1256þ0547oa 1256+5652oa 1301+2819oa 1305þ1033oa 1307+0642oa 1310+4601oa 1312+3515oa 1314+0201oa 1321+2847oa 1323+2910oa 1323+6541[oa ­ ob] 1324+0537oa 1325+6515oa

Q Q Q Q Sy 1 Q Sy 2 Q Q Sy 1.9 Sy 1.5 Q Q Q Sy 1 Q Q Q Sy 1.9 Q Q Q Sy 1.8 Q Q Q Q Q Q Q Q Q Q Q Sy 1 Sy 1.9 Q Q Q Q Q Q NLRG Q Sy 1.9 Q Sy 2 Q Q Q Q Q Q Q Sy 1 Q Q Q Q Sy 1.2 Q Q Q Q Q Q

167


TABLE 1-- Contin ue d Designation (J2000) (1) 1331+3030 ................... 1331+4101 ................... 1337+2423 ................... 1338+0432 ................... 1341+6740 ................... 1342þ0053 .................. 1348+2622 ................... 1354+3139 ................... 1354+1805 ................... 1354+0052 ................... 1405+2555 ................... 1406+2223 ................... 1417+4456 ................... 1419þ1310 .................. 1419+0628 ................... 1424+2256 ................... Name (2) 3C 286.0 PG 1329+412 IRAS13349+2438 NGC 5252 Mrk 270 Q1340þ0038 QSO 1348+263 B2 1351+31 PG 1352+183 PG 1352+011 PG 1402+261 PG 1404+226 PG 1415+451 PG 1416þ129 3C 298 QSO 1422+231A QSO 1422+231B QSO 1422+231C QSO 1422+231D B2 1425+267 PG 1427+480 NGC 5643 Q1435þ0134 Mrk 478 NGC 5728 PG 1444+407 PKS 1451þ375 B2 1503+691 LB 9612 LB 9605 PG 1522+101 NGC 5929 1543+489 Mrk 493 3C 332 3C 336.0 PG 1626+554 Mrk 883 PG 1630+377 3C 345 PKS 1656+053 PG 1715+535 ARP 102B PG 1718+481 NGC 6500 S5 1803+78 3C 390.3 3C 395 4C 73.18 Cygnus A NGC 7052 Mrk 516 AKN 564 3C 454.3 MR 2251þ178 NGC 7469 PG 2302+029 Typea (3) Q Q Sy 1 Sy 1.9 Sy 2 Q Q Q Q Q Sy 1 Sy 1 Q Q Q Q Q Q Q Q Q Sy 2 Q NLS 1 Sy 2 Sy 1 Q Q Q Q Q Sy 2 Q Sy 1 Sy 1? Q Sy 1 Sy 1.9 Q Q Q Q LINER Q LINER Q Sy 1 Sy 1.5 Q Q Q Sy 1.8 Sy 1.8 Q Sy 1 Sy 1.2 Q Redshift (4) 0.849 1.930 0.108 0.023 0.009 0.326 0.597 1.326 0.152 1.117 0.164 0.098 0.114 0.129 1.436 3.620 3.620 3.620 3.620 0.366 0.221 0.004 1.310 0.079 0.009 0.267 0.314 0.318 1.898 1.834 1.321 0.008 0.400 0.032 0.152 0.927 0.133 0.038 1.466 0.593 0.879 1.920 0.024 1.084 0.010 0.680 0.056 0.635 0.302 0.056 0.014 0.028 0.024 0.859 0.068 0.016 1.044 NHb (5) 1.10 0.70 1.00 2.00 1.80 2.10 1.10 1.20 1.80 2.00 1.40 2.00 0.90 7.20 2.00 2.50 2.50 2.50 2.50 1.50 1.60 8.50 3.60 0.90 7.60 1.00 6.20 2.20 3.90 3.90 2.60 1.90 1.60 2.00 2.00 4.50 1.50 3.80 0.90 0.80 6.10 2.40 2.20 2.10 6.90 3.60 3.60 11.00 7.20 33.00 9.60 4.50 6.20 6.90 2.70 4.80 4.90 Spectra (6) 1331+3030oa 1331+4101oa 1337+2423[oa ­ ob] 1338+0432[oa ­ ob] 1341+6740oa 1342þ0053oa 1348+2622oa 1354+3139oa 1354+1805oa 1354+0052oa 1405+2555[oa ­ ob] 1406+2223oa 1417+4456oa 1419þ1310oa 1419+0628oa 1424+2256oA 1424+2256oB 1424+2256oC 1424+2256oD 1427+2632oa 1429+4747oa 1432þ4410oa 1437þ0147[oa ­ ob] 1442+3526[oa ­ ob] 1442þ1715oa 1446+4035oa 1454þ3747oa 1504+6856oa 1519+2346oa 1519+2347oa 1524+0958oa 1526+4140oa 1545+4846oa 1559+3501oa 1617+3222oa 1624+2345oa 1627+5522oa 1629+2426oa 1632+3737oa 1642+3948oa 1658+0515oa 1716+5328oa 1719+4858oa 1719+4804oa 1755+1820oa 1800+7828oa 1842+7946oa 1902+3159oa 1927+7358oa 1959+4044oa 2118+2626oa 2156+0722oa 2242+2943oa 2253+1608oa 2254þ1734oa 2303+0852oa 2304+0311oa

1427+2632 ................... 1429+4747 ................... 1432þ4410 .................. 1437þ0147 .................. 1442+3526 ................... 1442þ1715 .................. 1446+4035 ................... 1454þ3747 .................. 1504+6856 ................... 1519+2346 ................... 1519+2347 ................... 1524+0958 ................... 1526+4140 ................... 1545+4846 ................... 1559+3501 ................... 1617+3222 ................... 1624+2345 ................... 1627+5522 ................... 1629+2426 ................... 1632+3737 ................... 1642+3948 ................... 1658+0515 ................... 1716+5328 ................... 1719+4858 ................... 1719+4804 ................... 1755+1820 ................... 1800+7828 ................... 1842+7946 ................... 1902+3159 ................... 1927+7358 ................... 1959+4044 ................... 2118+2626 ................... 2156+0722 ................... 2242+2943 ................... 2253+1608 ................... 2254þ1734 .................. 2303+0852 ................... 2304+0311 ...................

Note.--Table 1 is also available in machine-readable form in the electronic edition of the Astrophysical Journal Supplement. a AGN type: (Q) QSO, (Sy) Seyfert, (N LS 1) narrow-line Seyfert 1, and (N LRG) narrow-line radio galaxy. b NH is in units of 1020 cmþ2. (*) We include this BL Lac object as it shows weak emission lines.


EMISSION LINE PROPERTIES OF AGNs potentially be estimated from the emission line equivalent widths, providing a standard candle in measuring cosmological distances. In reality, the scatter of the Baldwin effect is too large to give meaningful results, and studies have concentrated on understanding and reducing this scatter (Shang et al. 2003; Dietrich et al. 2002). Conflicting results have also emerged, where radio-loud samples and samples with a wide range of luminosities show a stronger effect (e.g., Baldwin et al. 1978; Wampler et al. 1984; Kinney, Rivolo, & Koratkar 1990; Wang, Lu, & Zhou 1998), while radio-quiet samples and samples with a small luminosity range show weaker or no effect (e.g., Steidel & Sargent 1991; Wilkes et al. 1999). A number of explanations have been introduced to explain the Baldwin effect. It can be either due to geometry as in Netzer, Laor, & Gondhalekar (1992), where the inclination of the disk changes the apparent luminosity, or due to changes in spectral energy distribution with luminosity, where more luminous objects have softer ionizing continuum (Zheng & Malkan 1993; Green 1998) or due to a decrease of covering factor of the broad emission line clouds with luminosity (Wu, Boggess, & Gull 1983). There have also been claims that the Baldwin effect is affected by evolution (Green, Forster, & Kuraszkiewicz 2001) or may be due to selection effects (continuum beaming, biases in selection techniques--see Sulentic et al. 2000; Yuan, Siebert, & Brinkmann 1998). Despite a vigorous study of emission line properties of AGNs in the last 30 years, which resulted in few thousand published articles, questions about the structure and kinematics of the BLR and their relationship to the central engine (accretion mechanism, origin of the fuel, etc.) have not been answered. Nor is it clear how the BLR relates to the other components seen in AGN spectra: broad and narrow absorption lines, X-ray warm absorbers, high-ionization emission lines, and scattering regions. Despite attempts to unite these components (Elvis 2000; Laor & Brandt 2002; Ganguly et al. 2001; Murray & Chiang 1995) definitive tests have been elusive. Progress has been hampered by lack of large data sets with uniform and reliable measurements of emission lines that would consistently measure the continuum and account for bl ended iron emis sion, which heavil y contaminates emission lines such as H , Mg ii, and C iii] and forms a pseudocontinuum complicating the measurements of the broadband continuum, the weaker lines, and the wings of strong emission lines (Wills, Netzer, & Wills 1985; Boroson & Green 1992; Vestergaard & Wilkes 2001). Most studies have concentrated either on large nonuniform samples where emission line measur em ents have been co mpiled from literature (Zheng & Malkan 1993; Zamorani et al. 1992; Corbin & Boroson 1996; Dietrich et al. 2002) or small samples with uniform measurements (Boroson & Green 1992; Wills et al. 1999; Wilkes et al. 1999). We have therefore undertaken a major study of AGN emission lines, where our largely automated procedure accounts for Galactic extinction, models blended optical and UV iron emission, includes Galactic and intrinsic absorption lines, and models emission lines using multiple Gaussians. Using the same modeling procedure we have previously analyzed and published measurements of emission lines of two large data sets. The first 993 spectra from the Large Bright Quasar Survey has been presented by Forster et al. (2001, hereafter Paper I) together with detailed description of our analysis methods. The second includes 174 Hubble Space Telescope Faint Object Spectrograph (HST FOS) spectra obtained before t he installation of COSTAR and w as

169

presented in Kuraszkiewicz et al. (2002, hereafter Paper II). In the current paper we present the measurements of emission lines and plots of spectral fits of the remaining 220 HST FOS spectra that were observed after the installation of COSTAR, completing the analysis of all archival HST FOS spectra. Statistical comparison of the emission-line parameters and continuum parameters of these large samples will hopefully bring us closer to building an accurate model of emission line regions and their dependence on the central engine. 2. THE POST-COSTAR FOS ACTIVE GALACTIC NUCLEUS SAMPLE The sample was assembled by cross-correlating the VeronCetty & Veron (1996) catalog of AGNs with the MAST (Multimission Archive at Space Telescope) holdings. BL Lac objects were ignored, as their spectra show no emission lines. Starburst galaxies and broad absorption line (BAL) quasars (where emission lines are heavily disrupted by absorption features) were not included. We chose all available (UV and optical) spectrophotometric archival data that have been observed with the Faint Object Spectrograph (FOS; Keyes et al. 1995 and references therein) on HST after the installation of COSTAR (i.e., after 1993 December). FOS spectra obtained prior to 1993 December have been analyzed by us in Paper II. We include all spectra taken with the high-resolution gratings (G130H, G190H, G270H, G400H, G570H, G780H; spectral resolution k=àk $ 1300). Low-resolution (G160L, G650L; spectral resolution k=àk $ 250) gratings were also included when high-resolution gratings were not available in the matching wavelength range. Spectra obtained with the prism were excluded as their extremely low resolution precludes any reasonable emission line measurements. We analyzed only spectra with a mean signal-to-noise (S/N) per resolution element !5. The FOS spectra were uniformly calibrated to account for temporal, wavelength- and aperture-dependent variations that are seen in the instrumental response. We use the most recent version of the FOS calibration pipeline with the ST-ECF POA version of calfos. This pipeline provides an improved correction to the zero point offsets in the BLUE high-resolution spectra, removes hot pixel/hot diode regions from individual exposures, and calibrates spectra to the 4. 3 aperture. B We interpolated all of the spectra to a linear wavelength scale, ° retaining the original approximate wavelength intervals (in A per bin), and, for each object, we averaged all of the spectra obtained at a particular wavelength setting if the flux did not differ by more than 20%. If the difference in flux was larger, the spectra w er e analyzed s eparately. To obtain a r eliabl e continuum fit for each object, we combined spectra obtained at different wavelength settings and observed at different times if the flux levels did not differ by more than 20% in the overlap region. High-resolution gratings (G130H, G190H, G270H, G400H, G570H, G780H) were merged separately from the lowresolution gratings (G160L, G650L). In both cases, the longer wavelength spectrum was scaled to match the shorter wavelength spectrum and the spectra were then spliced at wavelengths in continuum regions away from emission or absorption lines by retaining as much of the higher S/N spectrum as possible. At this point the sample consisted of 327 spectra. Spectra that showed no emission lines, due to a too low S/N ( <5) in the line regions, or a redshift that placed strong emission lines outside the spectrum's wavelength range (mostly chosen for studies of


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KURASZKIEWICZ ET AL.
TABLE 2 Re presen tati ve Li st of Objects and FOS S pectra Exposure Time (s) 1379.9 1389.9 769.9 960.0 60.0 420.0 1080.0 2409.9 2409.9 2409.9 2409.9 2409.9 1519.9 1369.9 423.9 1479.9 2430.0 2430.0 2430.0 720.0 1469.9 2149.9 2149.9 2149.9 1680.0 539.9 827.9

Vol. 150

Spectrum 0005+0203oa............... 0006+2012oa...............

Data Set Y29C0102T Y29E0202T Y29E0203T Y29E0204T Y29E0205T Y29E0206T Y3IS0105T Y3IS0106T Y3IS0107T Y3IS0108T Y3IS0109T Y3IS010AT Y3IS010BT Y29C0202T Y29C0203T Y3AG0102T Y3AG0103T Y3AG0104T Y3AG0105T Y27O0302T Y2JK0102T Y2JK0103T Y2JK0104T Y2JK0105T Y2JK0106T Y2JK0108T Y2JK0109T

Configuration RD BL BL BL BL BL RD RD RD RD RD RD RD RD RD RD RD RD RD BL BL BL BL BL BL RD RD

Grating G190H G130H G130H G190H G270H G270H G190H G190H G190H G190H G190H G190H G190H G190H G190H G270H G270H G270H G270H G130H G130H G130H G130H G130H G130H G270H G190H

Time of Observation 1994 1994 1994 1994 1994 1994 1997 1997 1997 1997 1997 1997 1997 1994 1994 1996 1996 1996 1996 1994 1994 1994 1994 1994 1994 1994 1994 Jul 21 Dec 16 Dec 16 Dec 16 Dec 16 Dec 16 Jan 30 Jan 30 Jan 30 Jan 30 Jan 30 Jan 30 Jan 30 Aug 06 Aug 06 Nov 17 Nov 17 Nov 17 Nov 17 Jul 30 Nov 27 Nov 27 Nov 27 Nov 27 Nov 27 Nov 27 Nov 27

0018+1629oa...............

0020+0226oa............... 0020+2842oa...............

0029+1316oa............... 0029+1316ob ..............

Note.--Table 2 is available in its entirety in the electronic edition of the Astrophysical Journal Supplement. A portion is shown here for guidance regarding its form and content.

the Ly forest), were then removed. The final sample consists of 220 spectra of the 180 AGNs listed in Table 1. In the first column the coordinate designation based on the equinox J2000 position is given, followed by the AGN name (col. [2]), AGN type and redshift ( from the NASA/IPAC Extragalactic Database), and Galactic NH in units of 1020 cmþ2 (cols. [3] ­ [5]). The values of NH are in general taken from the Bell Laboratory H i survey (Stark et al. 1992). In a few cases for which NH had been specifically measured, we quote the values from the literature (Lockman & Savage 1995; Elvis, Wilkes, & Lockman 1989); for objects with declination greater than 40 , NH is from Heiles & Cleary (1979). The last column of Table 1 gives the list of spectra that were analyzed for each object. The name of the spectrum consists of the coordinate designation from column (1), followed by a two letter designation: ``o'' indicates a postCOSTAR spectrum (in Paper II pre-COSTAR spectra were designated with ``r ''); a second letter (a to z) indicates whether the AGN in question has more than one spectrum available. A capital letter indicates a spectrum of a lensed component as e.g., in 1001+5553oA and 1001+5553oB. In Table 2 we show a detailed list of FOS gratings, and data sets with exposure times that were used to compile spectra listed in Table 1. 3. ANALYSIS OF SPECTRA 3.1. Continuum and Blended Iron Fitting Since our goal was to assemble a uniform database of emission line measurements, we have analyzed our postCOSTAR spectra following the same fitting procedures as those used in the LBQS and pre-COSTAR/FOS spectral analysis ( for

details see Papers I and II). We used the modeling software Sherpa1 (Freeman, Doe, & Siemiginowska 2001) developed for the Chandra mission, where the model parameters were determined from a minimization of the 2 statistic with modified calculation of uncertainties in each bin (Gehrels 1986) and using the Powell optimization method for continuum, iron emission, and first emission line fits and the LevenbergMarquardt optimization method in the final emission line fits (see below). First, we fitted a reddened power-law continuum2 to regions of the spectrum redward of Ly and away from strong emission lines and blended iron emission. We use the same continuum windows as in the analysis of pre-COSTAR continuum spectra (see Table 2 in Paper II), with the addition ° of a new window redward of H at 6990 ­ 7020 A rest frame. Most of the post-COSTAR spectra were fitted by a single power law. However, in 21 spectra that covered a large wavelength range, two power laws were introduced: one (UV) ° extending at krest < 4200 A and another (optical) at krest > ° ° 4200 A, both normalized at k ¼ 4200 A. In Table 3 we present the slopes of the dereddened UV and optical continua (cols. [2] and [5], respectively) with the normalization of the ° continuum in units of 10þ14 ergs cmþ2 sþ1 Aþ1 (col. [3]) at the observed wavelength knorm (col. [4]). The slopes and normalizations are quoted with 2 errors. For spectra with only one continuum window present, a constant slope of þ ¼ 1 is quoted

http://cxc.harvard.edu/sherpa/index.html. We use the reddening curves of Cardelli et al. 1989 to account for Galactic extinction; see Paper I for details.
2

1


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EMISSION LINE PROPERTIES OF AGNs
TABLE 3 Continuum Pa rameters Designation (1) 0005+0203oa.................... 0006+2012oa.................... 0018+1629oa.................... 0020+0226oa.................... 0020+2842oa.................... 0029+1316oa.................... 0029+1316ob ................... 0039þ5117oa* ................. 0044+1026oa.................... 0044þ2434oa ................... 0048+3157oa.................... 0053+1241oa.................... 0103+0221oa.................... 0104þ2657oa ................... 0109þ1521oa ................... 0110þ0216oa ................... 0110þ0219oA .................. 0110þ0219oB .................. 0120+2133oa.................... 0120+2133ob ................... 0122þ0421oa ................... 0124+0343oa.................... 0139+0131oa.................... þUVa (2)
×0 19 0.17þ0::23 ×0 02 1.46þ0::01 ×0 25 1.92þ0::24 ×0 79 þ0:77þ0::86 ×0 12 2.08þ0::10 1 ×0 03 1.14þ0::02 ×0 04 0.28þ0::04 ×0 51 0.31þ0::48 ×0 83 0.91þ0::05 ×0 55 0.94þ0::88 ×0 01 0.89þ0::01 ×0 44 1.37þ0::46 1 ×0 12 1.44þ0::12 1 ×0 08 2.01þ0::32 ×0 13 1.86þ0::13 1 1 1 ×0 06 0.48þ0::05 ×0 12 1.03þ0::10

171

Norm.b (3)
× 0.382þ × 9.579þ × 0.058þ × 0.194þ × 0.049þ × 2.905þ × 2.028þ × 0.336þ × 0.036þ × 0.079þ × 0.019þ × 2.881þ × 0.267þ × 0.164þ × 0.070þ × 0.078þ × 0.100þ × 0.205þ × 0.565þ × 0.227þ × 0.086þ × 0.021þ × 0.084þ 0:009 0:009 0:057 0:068 0:001 0:001 0:006 0:006 0:001 0:001 0:189 0:189 0:016 0:018 0:019 0:001 0:002 0:002 0:006 0:000 0:006 0:003 0:009 0:011 0:007 0:007 0:002 0:002 0:001 0:001 0:001 0:001 0:000 0:002 0:002 0:002 0:011 0:011 0:020 0:020 0:003 0:003 0:000 0:000 0:003 0:003

knorm (4) 1804.7 1499.9 2271.3 2049.0 2227.3 1513.1 1670.2 3000.0 2315.1 2642.7 2271.3 1798.6 2037.3 2273.9 2721.7 2289.6 2866.5 2866.5 3184.8 3289.1 3272.2 2264.5 1842.8

þopta (5) .. . .. . .. . .. . .. . .. . .. . ×0 05 2.00þ0::02 .. . .. . .. . .. . .. . .. . .. . .. . .. . .. . .. . .. . .. . .. . .. .

Notes.-- Table 3 is published in its entirety in the electronic edition of the Astrophysical Journal Supplement. A portion is shown here for guidance regarding its form and content. (*) See Appendix for notes on individual spectra. a The power-law continuum slopes þUV and þopt are defined as fk / kþþ . þUV is fitted at krest < 4200, þopt at krest > 4200. Slopes with no listed errors show the assumed slope value in cases where only a single continuum window was available. b ° Normalization of the UV power law in units of 10þ14 ergs cmþ2 sþ1 Aþ1, at observed wavelength knorm.

without errors. This value was adopted since the mean slope of the pre- and post-COSTAR FOS sample is 0:97 ô 0:09. The next step in our fitting procedure was to model the blended iron emission lines. In the UV we used the Vestergaard & Wilkes (2001) iron template covering rest-frame wave° lengths between 1250 and 3100 A, while in the optical we used ° the Boroson & Green (1992) template covering 4250 ­ 7000 A. First, a crude estimate of the template's flux normalization was obtained by fitting the 2000 km sþ1 FWHM template to regions in which iron emission is known to be strongest (see col. [2] in Table 2 of Paper II). Then the FWHM of iron emission was estimated by comparing the spectrum with a grid of templates with FWHM between 900 and 10,000 km sþ1 in steps of 250 km sþ1. This was followed by a fit of both the FWHM and flux normalization at the iron fitting windows, followed by two iterations of the continuum and iron fits (refer to Paper I for more details). At this point the continuum and iron fits results were inspected and adjustments were made to spectra not fitted succes sfully (5% of s pectr a needed adjus tments of the continuum fit and three spectra needed adjustment of iron fits). 3.2. Emission and Absorption Line Fitting The emission lines were generally fitted with one Gaussian. However, since most (95%) FOS spectra have high S/N, the strong emission lines (Ly , C iv, C iii], Mg ii, H, H ) were fitted using two components: the very broad line region (VBLR) component and the intermediate line region (ILR; see Brotherton et al. 1994) here referred to as the broad and

narrow components, respectively. We use exactly the same emission line inventory as in the pre-COSTAR spectra (see Table 3 in Paper II). As a first stage, the FWHM and peak amplitude of the Gaussians are modeled while keeping the position of the emission line fixed at the expected wavelength (calculated from redshift). Then the position of the line is freed and modeled together with the FWHM and peak amplitude using Powell optimization. In the next step all Gaussian parameters are refitted, this time using distinct high and low sigma rejection criteria. We found that ¼ 3 for low rejection omits most of the absorption lines superimposed on the emission lines, while ¼ 7 for high rejection bypasses most spikes not associated with the emission line (e.g., geocoronal Ly , cosmic rays, etc.). At this stage we use the Levenberg-Marquardt optimization method, which is faster than the Powell method but only works well if the statistical surface is well behaved (after two runs of the emission line parameter fitting with the Powell method, this was certainly the case). It is nearly impossible to design a fully automated procedure that can deal with the wide range of spectral shapes that AGNs show, so at this point the fits were inspected and adjustments were made to spectra where necessary. About 5% of spectra needed adjustments at least in one emission line fit. For each spectrum, the continuum, iron, and emission line model obtained in the Sherpa fitting was next used as an input ``continuum'' to the FINDSL routine (Aldcroft 1993), which identifies narrow absorption lines and fits them with Gaussian


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Vol. 150

Fig. 1.--Example of spectral modeling of NGC 3516 (1106+7234oe, z ¼ 0:00880, NH Gal ¼ 2:90 á 1020 cmþ2). Panel (a) shows the reddened power-law continuum model fitted redward of Ly plotted over the observed spectrum. Below in (b) we show iron modeling, divided into three frames: (top) continuum+iron model plotted over the overall spectrum, (middle) iron-subtracted spectrum, and (bottom) fitted iron template. Panels (c), (d ), and (e)showmodelingofthe Ly ,C iv, and C iii] emission line regions, respectively. Each panel for each emission line region is divided into three frames: (top) total best-fit model plotted over the relevant region of each spectrum, (middle) residuals, and (bottom) individual Gaussian components. Strong emission lines such as Ly , C iv, and C iii] are modeled with two components--narrow and broad--while other emission lines are modeled using one Gaussian. The absorption lines that overlap each emission line are plotted at the top of the bottom frame. The dashed vertical lines in the emission line panels are drawn at the expected emission line position calculated using the redshift quoted at the top ° ° of the figure. Flux units are 10þ14 ergs cmþ2 sþ1 Aþ1, and wavelength units are in A and are observed frame values. [See the electronic edition of the Journal for a color version of this figure.]

profiles. We set the routine to find absorption lines away from ° the Ly forest region (blueward of krest ¼ 1065 A) and outside ° the Balmer continuum region (3360 ­ 3960 A), where the global power-law continuum may not fit the spectra well. The minimum significance level for identification of absorption lines was set to 4.5 (see Paper I for more details). We detect ° and fit absorption lines with Wk ! 0:3 A. The absorption line parameters were then used in the next iterative modeling step

where the position, peak amplitude, and FWHM of the absorption line were modeled simultaneously by the Sherpa program, followed by another iteration of the emission line fitting. After this stage the results were inspected and spectra refitted if the automated procedure did not perform well. An example of a full spectral fitting is shown in Figure 1. The top panel shows the reddened power-law continuum fit redward of Ly to the observed spectrum, followed below by panels


No. 1, 2004 showing blended iron C iv, C iii], and Mg ii Spectral Atlas includes other spectral fits only

EMISSION LINE PROPERTIES OF AGNs and emission line modeling of Ly , . Since the whole post-COSTAR FOS 220 spectra, we present similar plots of on our Web site.3

173

3.3. Error Analysis The error analysis follows the procedure from Paper I (see x 3.5 of that paper for details), in which the 2 errors for each emission line p aramete r were determined from t he 2 confidence interval bounds (à2 ¼ 4:0) using the uncertainty procedure in Sherpa. The upper limits of equivalent widths were determined by fixing the line position at the expected wavelength, by fixing the FWHM at the value of the median FWHM found for that line in the LBQS sample (see col. [3], Table 3 of Paper II), and by setting the amplitude of the line to the 2 positive error. 4. EMISSION LINE MEASUREMENTS In Table 4 we present the rest-frame emission line measuremen t s f or one ex amp l e o b j e c t NGC 35 16 (spe ctrum 1106+7234oe). The format of Table 4 is exactly the same as the format of the electronic tables of emission line measurement presented for the LBQS and pre-COSTAR FOS samples, making it simple to analyze the LBQS and FOS samples together. In the full Table 4, each spectrum is represented by 43 rows, one for each possible emission line measurement. In the first column the name of the spectrum is given, followed by the object's redshift (col. [2]), followed by information on the emission line parameters: name of the emission line (col. [3]), FWHM in km sþ1 (cols. [4] ­ [6] showing the value and ô 2 errors), the offset of the peak of the Gaussian emission line

model (all lines except iron) in km sþ1 from the expected position based on the tabulated redshift (cols. [7] ­ [9] value, ô 2 errors), the rest-frame equivalent width of the emission ° line in A (cols. [10] ­ [12]) and the observed frame flux in units of 10þ14 ergs cmþ2 sþ1 (cols. [13] ­ [15]). Errors quoted for flux and Wk are based on the uncertainties in the amplitude and FWHM of the Gaussian model and do not include an error from an uncertainty in the underlying continuum flux level, which we estimate to be about 10%. For emission lines where only an upper limit on flux and Wk is available, no values for the peak offset are quoted as the position of the line was fixed at the line's expected wavelength. Also, the FWHM value in this case was set to the median value for the LBQS sample (see Table 3 in Paper II) with no associated errors. Finally, the last column (16) in the full table gives the number of narrow absorption features used in the emission line modeling. Our Gaussian decomposition is not necessarily unique and may be sensitive to slight shifts in continuum placement. While the total flux and equivalent width are easily derived by summing values provided for individual Gaussian components, no s imple c ombination y ields a FWHM representative of the entire emission line. We therefore list in Table 4B the total line FWHM (with ô 2 errors) of those lines that have been modeled using two Gaussians. These are Ly ,C iv,C iii], Mg ii,H ,and H , where the width of the line was measured at half peak of the dereddened emission line model after excluding iron emission, absorption lines, and weaker emission lines (e.g., in the Ly region we exclude the N v line, in the H region [N ii] and [S ii]). 5. STATISTICS AND COMPARISON WITH THE POST-COSTAR SAMPLE The statistical properties of the rest-frame Wk and FWHM distributions of the emission line measurements of the postCOSTAR spectra are presented in Table 5. The numbers quoted

3

See http://hea-www.harvard.edu/ $ pgreen/HRCULES.html.

TABLE 4 Repres enta tive Emission Line Measuremen ts FWHM (km sþ1) (2) àvpeak (km sþ1) (3) Wk ° (A) (4) Observed Flux (10þ14 ergs cmþ2 sþ1) (5) Absorption Lines (6)

Emission Line (1)

1106+7234oe, z = 0.00880 UV iron ............. Optical iron ....... Ly .................... Ly narrow ....... Ly broad ......... N v .................... O i ..................... Si iv + O iv] ...... C iv narrow ....... C iv broad ......... He ii blend......... Al iii .................. Si iii] .................. C iii] narrow ...... C iii] broad ........ Mg ii narrow ..... Mg ii broad ....... 4250×5750 þ250 ... ... 950×20 þ80 5300×70 þ70 3750×240 þ90 ×320 2800þ280 4850×140 þ140 2300×60 þ60 6700×50 þ50 6800×240 þ300 9000×1700 þ1500 1800×20 þ900 1800×10 þ100 7400×40 þ260 2850×50 þ50 7550×30 þ260 0×0 þ0 ... ... 380×20 þ20 300×40 þ40 750×40 þ140 þ350×200 þ180 þ250×80 þ80 ×30 280þ30 þ340×30 þ30 1050×180 þ180 þ800×800 þ800 þ440×40 þ50 þ740×50 þ10 þ1950×50 þ80 þ620×30 þ30 þ650×20 þ100
× 164:40þ ... ... × 41:60þ × 225:40þ × 41:30þ 7:40× þ × 40:20þ × 63:60þ × 240:80þ × 27:60þ 6:80× þ × 12:90þ × 28:30þ × 54:10þ × 51:90þ × 103:40þ 2:10 2:10 × 195:90þ ... ... × 49:70þ × 269:50þ × 49:40þ 8:90× þ × 48:10þ × 76:20þ × 288:40þ × 33:10þ 8:10× þ × 15:50þ × 33:90þ × 64:90þ × 62:40þ × 124:40þ 2:50 2:50

0 .. . .. .

1:80 6:60 6:20 6:20 4:80 1:90 1:90 1:60 2:40 2:30 3:30 3:20 4:10 4:00 2:20 2:40 2:20 1:80 0:40 7:30 0:40 3:00 0:80 4:00 1:70 1:70 1:10 5:60

2:10 7:90 7:40 7:40 5:70 2:20 2:30 1:90 2:90 2:80 4:00 3:80 4:90 4:80 2:60 2:90 2:70 2:10 0:40 8:70 0:50 3:60 0:90 4:80 2:10 2:10 1:30 6:80

0 2 3 0 0 0 1 0 0 0 0 0 0 2

Notes.--Table 4 is available in its entirety in the electronic edition of the Astrophysical Journal Supplement. A portion is shown here for guidance regarding its form and content. We present here line measurements for one, example spectrum 1106+7234oe. All measurements are rest frame except for flux. Spectral modeling of this object is shown in Fig. 1.


TABLE 5 Rest-Frame Emissi on Line Paramete r Distributions ° Wk (A) Detected Emission Line (1) UV iron ..................................... Optical iron ............................... Ly+O vi k1035 ....................... Ly k1216: Singlea ................................... Narrowb ................................. Broad ..................................... Sumc,d .................................... N v k1241.5 .............................. O i k1305 .................................. Si iv + O iv] k1400 .................. C iv k1549: Singlea ................................... Narrow .................................. Broad ..................................... Sumc ...................................... He ii k1640 ............................... Al iii k1859 ............................... Si iii] k1892 .............................. C iii] k1909: Singlea ................................... Narrow .................................. Broade ................................... Sumc,f .................................... Mg ii k2800: Singlea ................................... Narrow .................................. Broad ..................................... Sumc ...................................... [Ne v] k3426 ............................ [O ii] k3728............................... [Ne iii] k3869 ........................... H k4101.7 ............................... [S ii] k4072.5 ............................ H k4340.5 ............................... [O iii] k4363.............................. He ii k4686 ............................... H k4861: Singlea ................................... Narrow .................................. Broad ..................................... Sumc ...................................... [O iii] k4959.............................. Total (2) 77 18 77 13 96 97 108 108 102 102 4 92 92 94 89 68 59 .. . 68 68 66 4 44 44 47 21 21 21 17 17 15 15 17 5 12 12 17 17 Limits (3) 15 2 4 0 1 0 0 8 8 0 0 2 2 0 1 5 9 . .. 2 2 0 0 0 0 0 1 0 0 2 10 1 3 2 0 0 0 0 1 Mean (4) 67 ô 11 103 ô 42 22 ô 7 710 31 83 153 12 4 12 42 30 63 91 22 7 6 ô ô ô ô ô ô ô ô ô ô ô ô ô ô 360 5 13 28 2 1 2 27 5 10 13 3 1 2 SD (5) 87 169 57 1299 51 126 290 19 6 17 55 45 90 125 27 11 17 ... 28 36 48 152 86 70 143 32 469 87 85 23 37 27 18 48 42 129 141 69 Median (6) 54 18 10 145 19 64 87 7 2 9 32 22 43 67 18 5 2 ... 5 20 27 90 17 27 50 3 4 6 6 27 11 6 3 13 20 50 59 10 Kaplan-Meier Mean (7) 54 ô 7 91 ô 29 21 ô 6 .. 39 ô .. .. 12 ô 3ô .. . 4 . . 1 1 . Median (8) 45 24 10 . .. 19 . .. . .. 6 2 . .. . .. 22 42 . .. 19 4 2 . .. 5 20 . .. . . . . 6 . . 16 10 7 5 3 . . . . 13 .. .. .. .. 3 . .. . .. 4 1 10 1 2 . . . . .. .. .. .. 7 Num (9) 63 16 73 13 96 96 ... 98 92 102 4 89 90 ... 88 62 59 ... 66 66 ... 4 42 44 ... 18 20 21 14 7 14 12 15 5 12 12 ... 16 FWHM (km sþ1) Detected Mean (10) 4537 ô 716 5809 ô 1860 7110 ô 1068 4304 ô 1539 2526 ô 284 10993 ô 1242 ... 4038 ô 481 2722 ô 343 5329 ô 594 4525 ô 2683 2670 ô 316 10281 ô 1203 ... 9037 ô 1071 4341 ô 673 1306 ô 201 ... 1614 ô 222 6547 ô 965 ... 2887 ô 1846 2050 ô 347 6751 ô 1136 ... 940 ô 306 1008 ô 343 1318 ô 440 2654 ô 1177 717 ô 384 1309 ô 405 663 ô 240 2681 ô 1230 3220 ô 2190 1132 ô 411 9090 ô 3491 ... 1045 ô 325 SD (11) 5683 7438 9129 5549 2787 12167 . .. 4762 3294 5997 5366 2979 11413 . .. 10050 5307 1547 . .. 1807 7840 . .. 3692 2252 7535 . .. 1298 1534 2017 4404 1017 1514 831 4764 4897 1423 12094 . .. 1300 Median (12) 3500 7200 5800 4100 2365 11600 ... 3475 2450 5400 5100 2600 9910 ... 10000 4600 1350 ... 1575 5825 ... 2525 2050 6550 ... 700 570 800 1350 600 1325 500 1000 2100 1010 5150 ... 890

.. . 30 ô 3 62 ô 7 .. . 22 ô 2 7ô1 6ô2 .. . 12 ô 3 26 ô 3 .. . .. .. .. .. ô .. .. ô ô ô ô ô . . . .

174

.. . 13 ô 3 27 ô 5 35 ô 6 104 37 47 86 14 138 33 42 38 21 13 10 31 29 90 94 35 ô ô ô ô ô ô ô ô ô ô ô ô ô ô ô ô ô 76 13 11 21 7 102 19 22 9 10 8 5 22 12 37 34 17

13

37 16 20 11 9

.. .. .. .. 33 ô


TABLE 5--Continued ° Wk (A) Detected Emission Line (1) UV iron ..................................... [O iii] k5007.............................. He i k5875.6 ............................. [N ii] k6548............................... H k6563: Singlea ................................... Narrow .................................. Broad ..................................... Sumc ...................................... [N ii] k6583............................... [S ii] k6716.4 ............................ [S ii] k6731 ............................... Total (2) Limits (3) Mean (4) SD (5) Median (6) Kaplan-Meier Mean (7) Median (8) Num (9) FWHM (km sþ1) Detected Mean (10) SD (11) Median (12)

16 18 26 ... 26 26 26 26 21 20

0 2 1 ... 0 0 0 2 1 1

105 ô 52 15 ô 5 25 ô 7 ... ô ô ô ô ô ô

209 18 37 . .. 172 265 404 69 23 26

31 13 13 .. . 82 157 242 28 14 8

.. . 13 ô 2 24 ô 5 . .. .. . ô .. . ô ô ô

. .. 11 7 .. . . .. 145 . .. 23 13 7
k

16 16 24 . .. 26 25 .. . 24 20 20

1021 ô 297 2254 ô 684 615 ô 161 .. . 1362 ô 335 4918 ô 1289 . .. 518 ô 131 603 ô 193 376 ô 98

1190 2737 786 ... 1708 6446 ... 642 864 438

1015 2400 330 .. . 950 3400 . .. 350 475 350

175

120 190 203 43 17 16

34 53 79 14 5 6

183 40 16 15

35 10 3 4

Notes.--Col. (1), emission line or line blend; col. (2), total number of emission lines modeled; col. (3), number of upper limits; col. (4), mean W measurements for detected emission lines; col. (6), median of Wk for detections; cols. (7) ­ (8), Kaplan-Meier reconstructed mean and median of number, mean, and median of the distribution of FWHM of the Gaussian components used to model each emission feature. a The distribution for single Gaussian component models are tabulated separately from narrow and broad components. b Means, medians, and SD of Wk calculated excluding objects with high equivalent width measurements (PKS 0518þ45 and NGC 3031). c The distribution of the sum of the broad and narrow component Wk measurements included with the single component measurements. d Means, medians, and SD of Wk calculated excluding objects with high equivalent width measurements (NGC 5728 and NGC 5643). e Means, medians, and SD of Wk calculated excluding objects with high equivalent width measurements (NGC 5252, NGC 4579, and NGC f Means, medians, and SD of Wk calculated excluding objects with high equivalent width measurements (NGC 5252, NGC 4579, and NGC

of detected emission lines; col. (5), standard deviation (SD) of Wk Wk distribution when upper limits are present. Cols. (9) ­ (12), the

5929). 5728).


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Fig. 2.--Distribution of rest-frame Wk (top and third row) and FWHM (second from top and bottom row) of the emission line properties of AGNs in the postCOSTAR FOS sample. When upper limits in Wk are present, we show the estimated Kaplan-Meier distributions with a dashed line. Shaded areas represent distributions for the single Gaussian components of the strong emission lines: Ly , C iv, C iii], and Mg ii.

were obtained by excluding off-nuclear spectra (e.g., the 10 different NLR knots of Mrk 78). To avoid excessive weight given to a single object, in cases of multiple spectra we tally only measurements from the spectrum with the highest S/ N and resolution. In total 1607 emission lines have been modeled among which 97 are upper limits. In Table 5 the name of the emission line is given in column (1), followed by the total number of emission lines modeled (col. [2]) and the number of upper limits (col. [3]). The mean, standard deviation and median of the Wk and FWHM for the detected lines are presented in columns (4) ­ (6) and (10) ­ (12), respectively. When upper limi t s i n Wk were present w e u sed t h e nonparametric survival analysis technique and a Kaplan-Meier estimator to reconstruct the true Wk distribution and to calculate the means and medians in columns (7) ­ (8) ( for reference, see Isobe, Feigelson, & Nelson 1986 and Lavalley, Isobe, & Feigelson 1992).

Since the strong emission lines such as Ly ,C iv,C iii], Mg ii, H , and H were fitted using either two (broad and narrow) components or one (single) component, we calculated the Wk and FWHM m eans and medians for these components separately. The mean and median Wk for the whole line (indicated as the ``Sum'' in Table 5) was calculated as either the sum of the broad and narrow components or the single component alone. Both the pre- a nd post-COSTA R F OS samples a re heterogeneous, and represent neither complete nor uniform selection. Nevertheless, as a check on our methods and on the consistency between these samples we compare the statistical properties of the Wk and FWHM of the pre-COSTAR sample analyzed in Paper II and the post-COSTAR sample presented here. Overall, the means and medians for the UV lines agree within the errors. We did not, however, attempt to compare the Wk of post-COSTAR single components of the strong


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EMISSION LINE PROPERTIES OF AGNs

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Fig. 2.--Continued

emission lines or optical lines redward of Ne v with the preCOSTAR sample measurements, s ince the n um ber o f available Wk in both or either samples is too small for meaningful analysis. Histograms of Wk and FWHM of the emission lines blueward of Mg ii are presented in Figure 2. The first and third rows represent the Wk distributions, while the second and fourth rows give the FWHM distributions. In all panels, solid lines represent distributions for detections, while the dotted lines show the estimated Wk distributions from the Kaplan-Meier estimator if upper limits are present. In the panels that show the sum of Ly ,C iv,C iii], and Mg ii distributions, the shaded histograms represent results from single Gaussian component fits. The luminosity and redshift range of the post-COSTAR sample is comparable to the pre-COSTAR sample analyzed in Paper II (see Fig. 3). However, the post-COSTAR sample shows a larger number of low-luminosity AGNs such as Seyferts, ° LINERs, and NLS1s. Objects with log LÏ2500 A÷ < 30 comprise of $ 30% of the post-COSTAR sample and only 15%

of the pre-COSTAR sample. In Figure 4 we show the ° distributions of log LÏ2500 A) for both samples. The twotailed Kolmogorov-Smirnow test gave a 99.9% probability that these distributions are different. 6. CONCLUSIONS We have presented the emission line measurements of a sample of AGNs that has been observed by the HST FOS after the installation of COSTAR. Our sample includes 180 objects and 220 spectra, which have been m odeled using an automated technique that fits multiple Gaussians to the emission lines, taking into account Galactic reddening, blended iron emission, and Galactic and intrinsic absorption lines. In this paper we present uniform measurements of 1607 emission lines including equivalent widths, FWHM, and shifts from the line's expected position and calculate upper limits for weak lines. We also present the underlying continuum parameters (slopes and normalization). This is the third paper


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Fig. 2.--Continued

in a series of papers aimed at uniformly measuring emission line properties in large AGN samples. It has been preceded by a presentation of emission line properties in $ 1000 optical spectra from the Large Bright Quasar Survey (Paper I) and $ 200 UV spectra observed by HST FOS in the pre-COSTAR era (Paper II). All 1387 spectral fits and tabulated results are available at our Web site (see footnote 3). Such large uniformly measured databases will hopefully bring us closer to a better understanding of the origin of the line emitting regions and their relationship to the central engine. P. J. G. and J. K. gratefully acknowledge support provided by NASA through grant NAG5-6410 (LTSA). P. J. G. and T. A. acknowledges support through NASA contract NAS839073 (CXC). M. V. acknowledges financial support for Proposal number AR-09549, provided by NASA through a

grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. We are grateful to Todd Boroson for providing the Fe ii optical template. This research was made based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute and using the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for nonHST data is provided by the NASA Office of Space Science via grant NAG5-7584 and by other grants and contracts. This research has also made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.


Fig. 2.--Continued

° Fig. 3.--Luminosity at 2500 A vs. redshift for the post-COSTAR sample analyzed here ( filled circles) and the pre-COSTAR sample analyzed in Paper II (open triangles).

° Fig. 4.--Distribution of luminosity at 2500 A for AGNs from the postCOSTAR sample (solid line) and the pre-COSTAR sample (dotted line). The two distributions are different at the 99.9% level with post-COSTAR sample having a higher percentage of low-luminosity [log L(2500÷ < 30] objects.


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° 0039þ5117oa.--Two power-law continua were fitted to this spectrum, which were joined at a nonstandard wavelength of 3000 A observed frame, for a better continuum fit. 0238+1636oa.--This BL Lac object is included in our sample as it shows weak emission lines. ° 0241þ0815oa.--Spectrum spans a large wavelength range from 2200 to 6800 A, so the power-law continuum does not fit the spectrum well, especially at H wavelengths. 0320þ1926oa, 1337+2423oa, 1959+4044oa.--Short spectra with only one standard continuum window; for a better continuum fit we added a nonstandard continuum window at red side of Mg ii. 0742+6510oa ­ oj.--Spectra of 10 different NLR knots in Mrk 78 (a Seyfert 2) showing interaction of the NLR gas with the ISM. 1048þ2509oa.--Very weak continuum. 1223+1545oa.--Very weak continuum. ° 1252+2913oa.--Used a nonstandard continuum window at wavelengths 2100 ­ 2130 A observed frame. 1719+4858oa.--Missing spectrum at C iv wavelengths. 1842+7946oa.--Missing spectrum at C iv wavelengths. 1902+3159oa.--Added additional window blue of Ly for better continuum fit. 1927+7358oa.--Missing spectrum at Ly wavelengths.
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