Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://mavr.sao.ru/hq/marat/publ/articles/ds1713.ps Äàòà èçìåíåíèÿ: Wed Feb 24 17:32:54 2010 Äàòà èíäåêñèðîâàíèÿ: Tue Oct 2 16:23:26 2012 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: propulsion

ASTRONOMY & ASTROPHYSICS NOVEMBER I 1999, PAGE 545
SUPPLEMENT SERIES
Astron. Astrophys. Suppl. Ser. 139, 545--554 (1999)
Survey of instantaneous 1 \Gamma 22 GHz spectra of 550 compact
extragalactic objects with declinations from \Gamma30 ffi to +43 ffi?
Y.Y. Kovalev 1 , N.A. Nizhelsky 2 , Yu.A. Kovalev 1 , A.B. Berlin 3 , G.V. Zhekanis 2 , M.G. Mingaliev 2 , and
A.V. Bogdantsov 2
1 Astro Space Center of the Lebedev Physical Institute, Profsoyuznaya 84/32, Moscow, 117810, Russia
2 Special Astrophysical Observatory, Nizhny Arkhyz, Karachaevo--Cherkessia, 357147, Russia
3 Special Astrophysical Observatory, St. Petersburg Branch, St. Petersburg, 196140, Russia
Received March 26; accepted August 13, 1999
Abstract. We present observational results for extra­
galactic radio sources with milliarcsecond components,
obtained with the 600 meter ring radio telescope
RATAN--600 from 1st to 22nd December, 1997. For each
source, a six frequency broad band radio spectrum was
obtained by observing simultaneously with an accuracy
up to a minute at 1.4, 2.7, 3.9, 7.7, 13 and 31 cm. The
observed list is selected from Preston et al. (1985) VLBI
survey and contains all the sources in the declinations
between \Gamma30 ffi and +43 ffi with a correlated flux density
exceeding 0.1 Jy at 13 cm. The sample includes the
majority of sources to be studied in the current VSOP
survey and the future RadioAstron Space VLBI mission.
Key words: galaxies: active --- galaxies:
compact --- BL Lacertae objects: general --- quasars:
general --- radio continuum: galaxies --- radio
continuum: general
1. Introduction
One of the main characteristics of an extragalactic radio
source is the shape of the broad band spectrum, which
provides a considerable amount of physical information
about the object. The extragalactic radio sources are of­
ten separated into different samples on the basis of the
shape of the spectra (e.g. flat, inverted, steep, gigahertz
peaked spectrum sources). This shows the importance of
Send offprint requests to: Y.Y. Kovalev
? Tables 1 and 5 are available at CDS to cdsarc.u­strasbg.fr
(130.79.128.5) or via http://cdsweb.u­strasbg.fr/Abstract.html
Figure 4 is only available in electronic form at
http://www.edpsciences.org
Correspondence to: yyk@dpc.asc.rssi.ru
the multifrequency broad band spectra surveys of com­
pact extragalactic objects among long term flux variability
monitoring programs (e.g. Aller et al. 1985; Mitchell et al.
1994; Stevens et al. 1994, etc.) and VLBI imaging surveys
(e.g. Kellermann et al. 1998 and references therein).
Most of the earlier multifrequency spectra results were
obtained by combining measurements carried out quasi­
simultaneously (over a period of one or more months) at
radio and shorter wavelengths, using several telescopes
on some samples of tens of objects, selected by various
criteria. For example, we refer to the measurements of
19 active extragalactic sources from 20 cm to 1400 š A by
Landau et al. 1986). Valtaoja et al. (1988) investigated
quiescent spectra for a sample of 27 radio sources ob­
served at centimeter and millimeter wavelengths. Gear
et al. (1994) compared quasi­simultaneous 5 \Gamma 375 GHz
spectra of 22 BL Lacertae objects with 24 radio­loud,
violently variable quasars. K¨uhr et al. (1981) compiled
radio measurements at more than two frequencies for
494 sources from the combined NRAO--MPI 5 GHz Strong
Source Surveys and the Parkes 2.7 GHz Surveys. Herbig &
Readhead (1992) composed non­simultaneous radio data
from 10 MHz to 100 GHz on a complete sample of 256 ob­
jects. We also refer to papers, cited in the O'Dea (1998)
survey of compact steep­spectrum and gigahertz peaked­
spectrum sources, as well as a number of other works.
Some earlier RATAN--600 results on broad band spec­
tra observations were presented for samples from 8.7 GHz
Zelenchuk sky survey by Amirkhanyan et al. (1992) and
87GB survey by Mingaliev & Khabrakhmanov (1995),
for strong compact extragalactic objects by Kovalev
et al. (1996) and weak radio sources from the RATAN--
600 ``Cold'' deep sky survey by Bursov (1997).
A broad band spectrum of a compact extragalactic ra­
dio source is usually considered to be the sum of spec­
tra of several compact and extended components in a
source structure. The components are located at various

546 Y.Y. Kovalev et al.: 1 \Gamma 22 GHz spectra of 550 extragalactic objects
Tab le 1. Source sample
IAU Other OI Z IAU Other OI Z IAU Other OI Z
0003+38 G 0.229 0159\Gamma11 3C 57 Q 0.669 0420\Gamma01 OA 129 Q 0.915
0003\Gamma06 NRAO 5 BL 0.347 0201+11 OD 101 Q 3.56 0421+01 OF 36 Q 2.055
0005\Gamma23 Q 1.410 0202+14 NRAO 91 G 0.405 0422+00 OF 38 BL
0005\Gamma26 OB \Gamma210 G 0202+31 Q 1.466 0423+23 RS
0007+10 III Zw 2 G 0.090 0202\Gamma17 Q 1.740 0423+05 Q 1.333
0007+17 4C 17.04 Q 1.601 0211+17 Q 0.472 0425+04 OF 42 Q
0008\Gamma26 OB \Gamma214 Q 1.093 0216+01 Q 1.623 0428+20 OF 247 G 0.219
0010+40 4C 40.01 Q 0.256 0217\Gamma18 Q 0429+41 3C 119 Q 1.023
0011\Gamma04 Q 0219+42 3C 66A BL 0.444 0430+05 3C 120 G 0.033
0012+31 3C 6 G 0219\Gamma16 Q 0.698 0434\Gamma18 Q 2.702
0013\Gamma00 Q 1.574 0221+06 4C 06.11 Q 0.511 0440\Gamma00 NRAO 190 Q 0.844
0019+05 OB 34 BL 0223+34 4C 34.07 Q 0446+11 G 1.207
0022+39 OA 26 Q 1.946 0226\Gamma03 4C \Gamma03.07 Q 2.066 0451\Gamma28 OF \Gamma285 Q 2.560
0024+34 OB 338 G 0.333 0229+13 4C 13.14 Q 2.065 0454+03 OF 92 Q 1.349
0026+34 OB 343 G 0.6 0234+28 CTD 20 Q 1.207 0454+06 4C 06.21 G 0.405
0027+05 Q 0235+16 OD 160 BL 0.940 0454\Gamma23 OF \Gamma292 Q 1.003
0035+23 CTD 5 Q 2.27 0237\Gamma02 Q 1.116 0456+06 OF 94 Q 1.08
0035+12 4C 12.05 Q 1.395 0237+04 OD 62 Q 0.978 0457+02 OF 97 Q 2.384
0035\Gamma02 3C 17 G 0.220 0237\Gamma23 OD \Gamma263 Q 2.225 0458\Gamma02 DA 157 Q 2.286
0038\Gamma02 Q 1.176 0238\Gamma08 NGC 1052 G 0.005 0458+13 RS
0047+02 OB 78 BL 0239+10 OD 166 Q 0459+06 OF 99.3 Q 1.106
0048\Gamma09 OB \Gamma80 BL 0240\Gamma21 OD \Gamma267 Q 0.314 0459+13 BL
0048\Gamma07 OB \Gamma82 Q 1.975 0248+43 Q 1.310 0459+25 3C 133 G 0.277
0054\Gamma00 Q 2.795 0250+17 Q 0500+01 OG 3 Q 0.585
0055+30 NGC 315 G 0.016 0256+07 OD 94.7 Q 0.893 0502+04 OG 5 Q 0.954
0055\Gamma05 Q 0301+33 4C 33.06 G 0507+17 G 0.416
0056\Gamma00 DA 32 Q 0.717 0306+10 OE 110 Q 0.863 0509+15 RS
0106+01 4C 01.02 Q 2.107 0309+41 NRAO 128 G 0.136 0511\Gamma22 OG \Gamma220 Q 1.296
0108\Gamma07 OC \Gamma14 Q 1.776 0312+10 4C 10.10 G 0514\Gamma16 OG \Gamma123 Q 1.270
0108+38 OC 314 G 0.668 0316+16 CTA 21 Q 0518+16 3C 138 Q 0.759
0109+22 BL 0316+41 3C 84 G 0.017 0521\Gamma26 OG \Gamma236 RS
0110+31 NRAO 62 Q 0.603 0317+18 OE 129 G 0528\Gamma25 OG \Gamma247 Q 2.765
0111+02 UGC 773 G 0.047 0319+12 OE 131 Q 2.67 0528+13 OG 147 Q 2.07
0112\Gamma01 Q 1.365 0322+22 RS 0537\Gamma15 Q 0.947
0113\Gamma11 Q 0.672 0326+27 Q 1.533 0537\Gamma28 OG \Gamma263 Q 3.104
0116+08 4C 08.06 G 0.594 0327\Gamma24 OE \Gamma246.3 Q 0.888 0552+39 DA 193 Q 2.365
0118\Gamma27 OC \Gamma230.4 BL ?0.557 0329\Gamma25 OE \Gamma248 Q 2.685 0555\Gamma13 Q
0119+11 Q 0.570 0333+32 NRAO 140 Q 1.259 0601+24 4C 24.11 RS
0119+04 OC 33 Q 0.637 0336\Gamma01 CTA 26 Q 0.852 0602+40 OH 404.1 RS
0119+24 Q 2.025 0338\Gamma21 OE \Gamma263.9 BL 0605\Gamma08 OH \Gamma10 Q 0.872
0122\Gamma00 Q 1.070 0340+36 OE 367 Q 1.484 0606\Gamma22 OH \Gamma212 Q 1.926
0123+25 4C 25.05 Q 2.364 0344+19 RS 0607\Gamma15 OH \Gamma112 Q 0.324
0127+14 4C 14.06 Q 0346\Gamma16 Q 0610+26 3C 154 Q 0.580
0130\Gamma17 Q 1.020 0348\Gamma12 OE \Gamma182 Q 1.520 0611+13 c
0133\Gamma20 OC \Gamma255.3 Q 1.141 0400+25 CTD 26 Q 2.109 0618\Gamma25 OH \Gamma230 Q 1.90
0134+32 3C 48 Q 0.367 0402+37 4C 37.11 G 0.054 0620+38 OH 335 Q 3.469
0135\Gamma24 OC \Gamma259 Q 0.831 0403\Gamma13 OF \Gamma105 Q 0.571 0641+39 OH 368.8 Q 1.266
0136+17 Q 2.716 0405\Gamma12 OF \Gamma109 Q 0.574 0642+21 3C 166 G 0.245
0138\Gamma09 OC \Gamma65 BL ?0.501 0406+12 BL 1.02 0650+37 Q 1.982
0142\Gamma27 OC \Gamma270 Q 1.157 0406\Gamma12 OF \Gamma111 Q 1.563 0653\Gamma03 OH \Gamma90 Q
0144+20 RS 0409+22 3C 108 Q 1.213 0711+35 OI 318 Q 1.620
0146+05 OC 79 Q 2.345 0410+11 3C 109 G 0.306 0722+14 4C 14.23 Q
0147+18 OC 178 Q 0413\Gamma21 Q 0.807 0723\Gamma00 OI \Gamma39 BL 0.127
0148+27 Q 1.26 0414\Gamma18 Q 1.536 0727+40 OI 446 Q 2.501
0149+21 Q 1.32 0415+37 b 3C 111 G 0.048 0727\Gamma11 RS
0149+33 OC 383 Q 2.431 0420+02 BL 0729+25 Q
0156\Gamma14 a RS 0420+41 4C 41.11 RS 0733+30 RS

Y.Y. Kovalev et al.: 1 \Gamma 22 GHz spectra of 550 extragalactic objects 547
Tab le 1. continued
IAU Other OI Z IAU Other OI Z IAU Other OI Z
0733\Gamma17 RS 0953+25 OK 290 Q 0.712 1148\Gamma17 OM \Gamma181 Q 1.751
0733+26 RS 0955+32 3C 232 Q 0.530 1156\Gamma22 G 0.565
0735+17 OI 158 BL ?0.424 1004\Gamma01 Q 1.214 1156\Gamma09 OM \Gamma94 RS
0736\Gamma06 OI \Gamma61 Q 1.901 1004+14 OL 108.1 Q 2.707 1156+29 4C 29.45 Q 0.729
0736+01 OI 61 Q 0.191 1008\Gamma01 4C \Gamma01.21 Q 0.887 1157\Gamma21 Q 0.927
0738+31 OI 363 Q 0.630 1010+35 OL 318 Q 1.414 1200\Gamma05 ON \Gamma1 Q 0.381
0738+27 RS 1012+23 4C 23.24 Q 0.565 1200+04 RS
0742+31 4C 31.30 Q 0.462 1013+20 OL 224 Q 3.11 1202\Gamma26 Q 0.790
0742+10 OI 471 RS 1015+35 OL 326 Q 1.226 1204+28 ON 208 Q 2.177
0743\Gamma00 4C \Gamma00.28 Q 0.994 1018+34 OL 331 Q 1.400 1210+13 4C 13.46 Q 1.137
0743+25 RS 1019+42 RS 1211+33 ON 319 Q 1.598
0743+27 RS 1019+30 OL 333 Q 1.319 1213\Gamma17 ON \Gamma122 G
0745+24 OI 275 Q 0.409 1020\Gamma10 OL \Gamma133 Q 0.197 1213+35 4C 35.28 Q 0.857
0748+12 OI 280 Q 0.889 1020+19 OL 133 Q 2.136 1215+30 ON 325 BL 0.237
0748+33 OI 380 Q 1.932 1020+40 4C 40.25 Q 1.254 1216\Gamma01 Q 0.415
0752\Gamma11 OI \Gamma187 RS 1021\Gamma00 Q 2.552 1217+02 ON 29 Q 0.240
0754+10 OI 90.4 BL 0.66 1022+19 4C 19.34 Q 0.828 1218+33 3C 270.1 Q 1.519
0759+18 Q 1030+41 Q 1.120 1218\Gamma02 4C \Gamma02.53 G 0.665
0802+21 RS 1030+39 Q 1.095 1219+28 ON 231 BL 0.102
0805+41 Q 1.420 1032\Gamma19 Q 2.198 1219+04 4C 04.42 Q 0.965
0805+26 RS 1034\Gamma05 OL \Gamma257 G 1222+03 4C 03.23 Q 0.960
0805\Gamma07 Q 1.837 1034\Gamma29 OL \Gamma259 Q 0.312 1222+21 4C 21.35 Q 0.435
0808+01 OJ 14 BL 1036\Gamma15 OL \Gamma161 G 0.525 1225+36 ON 343 Q 1.975
0812+36 OJ 320 Q 1.025 1038+06 4C 06.41 Q 1.265 1226+02 3C 273 Q 0.158
0812+02 4C 02.23 Q 0.402 1040+12 3C 245 Q 1.028 1228+12 b 3C 274 G 0.004
0814+42 OJ 425 BL 1042+07 G 0.698 1228\Gamma11 ON \Gamma147 Q 3.528
0818\Gamma12 OJ \Gamma131 BL 1045\Gamma18 OL \Gamma176 Q 0.595 1236+07 G 0.400
0820+22 4C 22.21 BL 0.951 1046\Gamma02 4C \Gamma02.43 RS 1237\Gamma10 ON \Gamma162 Q 0.750
0820+29 OJ 234 Q 2.368 1054+00 OL 91 RS 1240+38 Q 1.316
0821+39 4C 39.23 Q 1.216 1055+20 4C 20.24 Q 1.11 1240\Gamma29 Q 1.133
0823+03 OJ 38 BL 0.506 1055+01 OL 93 Q 0.888 1243\Gamma07 ON \Gamma73 Q 1.286
0827+24 OJ 248 Q 0.941 1058+39 RS 1244\Gamma25 Q 0.638
0829+04 OJ 49 BL 0.180 1100+22 OM 201 RS 1252+11 ON 187 Q 0.870
0830+42 OJ 451 Q 0.253 1101+38 Mark 421 BL 0.031 1253\Gamma05 3C 279 Q 0.538
0834+25 OJ 259 Q 1.122 1102\Gamma24 OM \Gamma204 Q 1.666 1255+32 ON 393 RS
0837+03 Q 1.57 1104+16 4C 16.30 Q 0.632 1256\Gamma220 ON \Gamma293.9 Q 1.306
0838+13 3C 207 Q 0.684 1106+38 G 2.290 1256\Gamma229 Q 1.365
0839+18 Q 1.272 1109+35 RS 1257+14 OW 197 Q
0851+07 RS 1110\Gamma21 OM \Gamma218 RS 1302\Gamma03 Q 1.250
0851+20 OJ 287 BL 0.306 1111+14 OM 118 Q 0.869 1302\Gamma10 OP \Gamma106 Q 0.286
0854+21 RS 1116+12 4C 12.39 Q 2.118 1308+32 OP 313 BL 0.997
0855+14 3C 212 Q 1.043 1119+18 OM 133 Q 1.040 1308+14 OP 114 Q
0859\Gamma14 OJ \Gamma199 Q 1.339 1120\Gamma27 OM \Gamma234 RS 1315+34 OP 326 Q 1.050
0900+42 4C 42.28 G 1123+26 CTD 74 Q 2.341 1317\Gamma00 4C \Gamma00.50 Q 0.892
0906+43 3C 216 Q 0.670 1124\Gamma18 Q 1.048 1318\Gamma26 Q 2.027
0906+01 DA 263 Q 1.018 1127\Gamma14 OM \Gamma146 Q 1.187 1330+02 3C 287.1 G 0.215
0912+02 G 0.427 1128+38 Q 1.733 1331+17 OP 151 Q 2.084
0912+29 OK 222 BL 1128\Gamma04 OM \Gamma48 G 0.266 1334\Gamma12 OP \Gamma158.3 Q 0.539
0913+39 4C 38.28 Q 1.269 1130+00 Q 1336\Gamma23 OP \Gamma260.5 Q
0915\Gamma21 Q 0.847 1136\Gamma13 CTS 667 Q 0.554 1336\Gamma26 Q 1.51
0922+00 OK 37 Q 1.719 1142+05 4C 05.52 Q 1.342 1337\Gamma03 Q
0923+39 4C 39.25 Q 0.698 1142\Gamma22 OM \Gamma271 Q 1.141 1345+12 4C 12.50 G 0.121
0925\Gamma20 Q 0.348 1143\Gamma24 OM \Gamma272 Q 1.940 1347\Gamma21 OP \Gamma279 RS
0931\Gamma11 OK \Gamma152 RS 1143\Gamma28 OM \Gamma273 Q 0.45 1348\Gamma28 Q
0938+11 Q 3.191 1144+40 Q 1.089 1349\Gamma14 OP \Gamma182 RS
0945+40 4C 40.24 Q 1.252 1145\Gamma07 OM \Gamma76 Q 1.342 1351\Gamma01 Q 3.707
0952+17 OK 186 Q 1.478 1148\Gamma00 4C \Gamma00.47 Q 1.980 1352\Gamma10 OP \Gamma187 Q 0.332

548 Y.Y. Kovalev et al.: 1 \Gamma 22 GHz spectra of 550 extragalactic objects
Tab le 1. continued
IAU Other OI Z IAU Other OI Z IAU Other OI Z
1354\Gamma17 Q 3.147 1611+34 DA 406 Q 1.401 2044\Gamma16 OW \Gamma174 Q 1.932
1354\Gamma15 OP \Gamma192 Q 1.89 1614+05 OS 23 Q 3.217 2047+09 RS
1354+19 4C 19.44 Q 0.719 1615+36 4C 36.27 RS 2047+03 BL
1356+02 Q 1.319 1615+02 Q 1.341 2053\Gamma04 4C \Gamma04.80 Q 1.176
1402\Gamma01 Q 2.522 1616+06 OS 28 Q 2.088 2058\Gamma29 Q 1.492
1402+04 Q 3.211 1622\Gamma25 OS \Gamma237.8 Q 0.786 2059+03 OW 98 Q 1.015
1403\Gamma08 Q 1.763 1622\Gamma29 Q 0.815 2113+29 Q 1.514
1404+28 OQ 208 G 0.077 1624+41 4C 41.32 Q 2.55 2121+05 OX 36 Q 1.941
1406\Gamma07 OQ \Gamma10 Q 1.493 1625\Gamma14 Q 1.10 2126\Gamma15 OX \Gamma146 Q 3.266
1406\Gamma26 Q 2.43 1633+38 4C 38.41 Q 1.807 2126\Gamma18 OX \Gamma145 Q 0.680
1413+34 OQ 323 RS 1635\Gamma03 a Q 2.856 2127\Gamma09 Q ?0.780
1416+06 3C 298 Q 1.439 1638+39 NRAO 512 Q 1.666 2128+04 OX 46 G 0.990
1427+10 OQ 147 Q 1.71 1641+39 3C 345 Q 0.594 2128\Gamma12 OX \Gamma148 Q 0.501
1430\Gamma17 OQ \Gamma151 Q 2.331 1647\Gamma29 RS 2131\Gamma02 4C \Gamma02.81 BL 1.285
1430\Gamma15 OQ \Gamma150.2 Q 1.573 1648+01 RS 2134+00 OX 57 Q 1.932
1434+23 OQ 257 Q 1652+39 Mark 501 BL 0.033 2135\Gamma24 Q 0.819
1435\Gamma21 OQ \Gamma259 Q 1.187 1655+07 OS 92 Q 0.621 2136+14 OX 161 Q 2.427
1437\Gamma15 OQ \Gamma162 BL 1656+05 OS 94 Q 0.879 2140\Gamma04 Q 0.344
1438+38 OQ 363 Q 1.775 1656+34 OS 392 Q 1.936 2143\Gamma15 OX \Gamma173 Q 0.698
1439+32 OQ 366 Q 2.12 1657\Gamma26 RS 2144+09 OX 74 Q 1.113
1441+25 Q 0.062 1705+01 Q 2.576 2145+06 DA 562 Q 0.999
1442+10 OQ 172 Q 3.535 1706+00 G 0.449 2147+14 RS
1443\Gamma16 OQ \Gamma171 Q 1706\Gamma17 OT \Gamma111 RS 2149+06 OX 81 Q 1.364
1445\Gamma16 OQ \Gamma176 Q 2.417 1717+17 OT 129 BL 2149+05 OX 82 Q 0.740
1449\Gamma01 OQ \Gamma81 Q 1.314 1721+34 4C 34.47 Q 0.206 2150+17 OX 183 BL
1452+30 OQ 287 Q 0.580 1722+40 Q 1.049 2155\Gamma15 OX \Gamma192 Q 0.672
1456+04 4C 04.49 G 0.394 1725+12 OT 143.3 Q 2200\Gamma23 Q 2.118
1502+10 4C 10.39 Q 1.833 1725+04 Q 0.293 2200+42 BL Lacertae BL 0.069
1502+03 G 0.413 1730\Gamma13 NRAO 530 Q 0.902 2201+31 4C 31.63 Q 0.298
1504+37 OR 306 G 0.674 1732+09 OT 54 G 2201+17 OY 101 Q 1.076
1504\Gamma16 OR \Gamma102 Q 0.876 1741\Gamma03 OT \Gamma68 Q 1.057 2201+04 4C 04.77 G 0.028
1508\Gamma05 4C \Gamma05.64 Q 1.191 1743+17 OT 172 Q 1.702 2207+35 OY 313 RS
1510\Gamma08 OR \Gamma17 Q 0.360 1749+09 OT 81 BL 0.320 2208\Gamma13 Q 0.391
1511\Gamma10 OR \Gamma118 Q 1.513 1751+28 RS 2209+08 DA 574 Q 0.484
1511\Gamma21 OR \Gamma218 G 1.179 1756+23 OT 295 Q 1.721 2209+23 Q
1514+00 GNZ 25 G 0.052 1758+38 OT 398 Q 2.092 2214+35 OY 324 Q 0.510
1514+19 BL 1807+27 4C 27.41 Q 1.760 2215+02 Q 3.581
1514\Gamma24 AP Librae BL 0.048 1821+10 Q 1.364 2216\Gamma03 4C \Gamma03.79 Q 0.901
1518+04 4C 04.51 G 1.294 1830+28 CTD 108 Q 0.594 2223\Gamma05 3C 446 Q 1.404
1519\Gamma27 BL 1848+28 Q 2.56 2223+21 DA 580 Q 1.953
1525+31 OR 342 Q 1.380 1901+31 3C 395 Q 0.635 2227\Gamma08 Q 1.562
1532+01 Q 1.420 1908\Gamma20 OV \Gamma213 Q 2229\Gamma17 OY \Gamma150 Q 1.780
1535+00 Q 3.497 1908\Gamma21 OV \Gamma214 RS 2230+11 CTA 102 Q 1.037
1538+14 4C 14.60 BL 0.605 1920\Gamma21 OV \Gamma235 RS 2233\Gamma14 OY \Gamma156 BL ?0.609
1543+00 G 0.550 1921\Gamma29 OV \Gamma236 BL 0.352 2234+28 CTD 135 Q 0.795
1546+02 OR 78 Q 0.412 1923+21 OV 239.7 RS 2236+12 OY 160 Q
1548+05 4C 05.64 Q 1.422 1936\Gamma15 OV \Gamma161 Q 1.657 2239+09 Q 1.707
1548+11 OR 181 Q 0.436 1937\Gamma10 Q 3.787 2240\Gamma26 OY \Gamma268 BL 0.774
1550\Gamma26 Q 2.145 1947+07 OV 80 Q 2243\Gamma12 OY \Gamma172.6 Q 0.630
1551+13 OR 186 Q 1.29 1958\Gamma17 OV \Gamma198 Q 0.652 2245\Gamma12 Q 1.892
1555+00 Q 1.772 2002\Gamma18 OW \Gamma185 Q 0.868 2245+02 Q
1555\Gamma14 G 0.097 2008\Gamma15 OW \Gamma115 Q 1.180 2246+20 RS
1556\Gamma24 Q 2.818 2008\Gamma06 OW \Gamma15 G 1.047 2247+13 4C 13.84 Q 0.767
1600+33 OS 300 G 2012\Gamma01 BL 2251+15 3C 454.3 Q 0.859
1604+31 G 2029+12 OW 149 BL 1.215 2251+24 DA 587 Q 2.327
1606+10 DA 401 Q 1.226 2032+10 OW 154.9 BL 0.601 2251+13 4C 13.85 Q 0.677
1607+26 OS 111 G 0.473 2037\Gamma25 Q 1.574 2252\Gamma09 Q 0.606

Y.Y. Kovalev et al.: 1 \Gamma 22 GHz spectra of 550 extragalactic objects 549
Tab le 1. continued
IAU Other OI Z
2253+41 OY 489 Q 1.476
2254+02 OY 91.3 Q 2.089
2254+07 OY 091 BL 0.190
2255+41 4C 41.45 Q 2.15
2255\Gamma28 Q 0.926
2256+01 Q 2.663
2300\Gamma18 OZ \Gamma102 G 0.129
2303\Gamma05 4C \Gamma05.95 Q 1.139
2307+10 4C 10.70 RS
2318+04 OZ 031 Q 0.623
2318\Gamma19 OZ \Gamma130 G
2319+31 G
2319+27 CTD 139 Q 1.253
2320+07 DA 599 Q 2.090
2320\Gamma02 Q
2320\Gamma03 Q 1.411
2325\Gamma15 Q 2.465
2327+33 Q 1.809
2328+10 4C 10.73 Q 1.489
2328+31 OZ 347 RS
2329\Gamma16 OZ \Gamma149 Q 1.153
2330+08 OZ 50.8 RS
2331\Gamma24 OZ \Gamma252 G 0.048
2332\Gamma01 Q 1.184
2335\Gamma18 OZ \Gamma160 Q 1.450
2335\Gamma02 Q 1.072
2337+26 Q
2338+33 RS
2344+09 4C 09.74 Q 0.673
2344+092 RS
2345\Gamma16 OZ \Gamma176 Q 0.576
2349\Gamma01 4C \Gamma01.61 Q 0.174
2351\Gamma00 Q 0.463
2351\Gamma15 OZ \Gamma187 Q 2.675
2354\Gamma11 Q 0.960
2355\Gamma10 Q 1.622
2356+19 OZ 193 Q 1.066
2356+38 OZ 395 Q 2.704
a The source was not observed in December, 1997.
b The source was partly resolved at all frequencies.
c We have not registered emission from this object at any
frequency (nothing is present at these coordinates in NED
too).
distances from the central nucleus of the object, and are
likely to have resulted from activity within the nucleus.
The nucleus may be a black hole, which converts an ac­
creted ambient gas to ejected relativistic particles along
magnetic fields. Some of the components can be variable
in time. The variability can misrepresent the true shape
of a spectrum if measurements at all or especially high
frequencies are not simultaneous.
In this work we present observational results of more
than five hundred sources at six frequencies from 1 to
22 GHz using a single radio telescope. Flux densities at
all frequencies are measured practically instantaneously --
over a period of a few minutes. This is the shortest time
scale of broad band six frequency measurements for the
largest sample of sources so far, which has been used for
a spectra survey of compact extragalactic radio sources.
These observations are part of a long­term program
of instantaneous spectra monitoring of compact extra­
galactic objects (Kovalev 1998), which have milliarcsec­
ond components and are studied by VLBI networks. They
also give a ground spectra support for the VSOP sur­
vey and a pre­launch spectra study of the objects for the
RadioAstron project. The goal of the long­term program
is a mass study of the spectra and their variability for
many hundreds of compact extragalactic radio sources. It
is also among our intentions to find a relationship between
instantaneous multifrequency spectra and the VLBI radio
structure.
2. Source sample
We have selected about 700 sources from the Preston et al.
(1985) VLBI survey. These sources have a correlated flux
density F corr
13 – 0:1 Jy at the wavelength of 13 cm, and are
located north of declination \Gamma30 ffi . The northern sector of
RATAN--600 restricts this declination range from \Gamma30 ffi to
+43 ffi . Measurements of the sources located north of dec­
lination +49 ffi were made in 1998 with the southern sector
of RATAN--600 and will be published at a later date.
The list of 551 sources for northern sector observations
is presented in Table 1. The columns of this table are as
follows: (1) the IAU name, (2) possible other name, (3) the
optical identification (OI) and (4) the red shift. The OI
and red shifts are taken from Veron--Cetty & Veron (1998)
or, if not found there, are taken from the NASA/IPAC
Extragalactic database (NED). The abbreviations used
are ``Q'' for quasars, ``BL'' for BL Lacertae objects, ``G'' for
galaxies, ``RS'' for radio sources. In the latter case we do
not have OI. An extended version of this table is available
in electronic form at the CDS. This also includes B1950
coordinates taken from Preston et al. (1985) and Morabito
et al. (1986), correlated flux densities at 13 cm with errors
from Preston et al. (1985) and optical spectrum classifi­
cations from Veron--Cetty & Veron (1998).
3. Observations
We performed continuous six frequency 1 \Gamma 22 GHz
spectra observations of compact extragalactic sources
from 1st to 22nd December, 1997. We used the 600 me­
ter ring radio telescope RATAN--600 (Korolkov &
Parijskij 1979; Parijskij 1993) at the Russian Academy
of Sciences' Special Astrophysical Observatory, located
in Karachaevo­Cherkessia Republic (Russia) near Nizhny
Arkhyz and Zelenchukskaya at the North Caucasus.

550 Y.Y. Kovalev et al.: 1 \Gamma 22 GHz spectra of 550 extragalactic objects
Tab le 2. Parameters of RATAN--600 broad band receivers in
1997, used in this work
–, nh š0 , \Deltaš, T phys
LNA , TLNA , T sys , ffiT sys ,
cm GHz GHz K K K mK
1.4 2 21.65 2.5 15 23 77 3.5
2.7 2 11.2 1.4 15 18 70 3
3.9 2 7.70 1.0 15 14 62 3
7.7 1 3.90 0.6 15 8 37 2.5
13 1 2.30 0.4 310 35 95 8
31 1 0.96 0.12 310 21 105 15
Tab le 3. Measured and estimated beam widths and ratios r for
the RATAN--600 northern sector with the secondary mirror
No. 1 for different wavelengths – and elevations h
–, cm HPBWRA \Theta HPBWDec
h = 80 ffi h = 40 ffi h = 20 ffi
r ú 5 r ú 10 r ú 20
1.4 8: 00 0 \Theta 35 00 8: 00 5 \Theta 1: 0 4 13 00
\Theta 4: 0 3
2.7 16 00 \Theta 1: 0 3 17 00 \Theta 2: 0 8 24 00 \Theta 8: 0 0
3.9 23 00 \Theta 2: 0 0 26 00 \Theta 4: 0 3 39 00 \Theta 13 0
7.7 48 00
\Theta 4: 0 0 53 00
\Theta 8: 0 8 1: 0 4 \Theta 27 0
13 1: 0 3 \Theta 6: 0 5 1: 0 3 \Theta 13 0 1: 0 8 \Theta 37 0
31 3: 0 2 \Theta 16 0 3: 0 3 \Theta 33 0 5: 0 0 \Theta 100 0
The northern sector of the antenna (a part of the main
ring reflector) was used together with the secondary mir­
ror of cabin No. 1. Six broad band receivers are located
at this movable cabin. The cabin moves along 150 meter
long rails in order to be placed in the focus of the antenna
system at different elevations. The main (meridional)
transit method of observation was employed. Accuracy
and reliability of these spectra measurements were essen­
tially higher than earlier experiments conducted at the
RATAN--600 due to the following improvements made to
the receivers, antenna control system and the procedure
of observations.
We used a new set of broad band receivers at the wave­
lengths of 1.4, 2.7, 3.9, 7.7, 13 and 31 cm with low noise
HEMT amplifiers (LNA), cooled to a temperature of 15 K
at the four shortest wavelengths (Berlin et al. 1997, 1993).
Parameters of radiometers and antenna beams are given
in Tables 2, 3.
Table 2 lists wavelengths –; numbers of feedhorns n h ;
exact central frequencies š 0 ; band widths \Deltaš ; physical
temperatures of the LNA T phys
LNA ; noise temperatures of the
LNA TLNA ; total noise temperatures of systems T sys , in­
cluding the antenna noise at middle elevations; rms noise
temperature sensitivities of the system ffi T sys for a one sec­
ond integration time. Dual­feedhorn receivers are beam­
switched. Single­feedhorn receivers have a noise­added,
gain­balanced mode of operation. Linearly polarized sys­
tems were available at all frequencies: horizontal at 7.7 cm
and vertical at other wavelengths.
Fig. 1. Example of a full multifrequency scan for 4C 39.25, ob­
served on 16 December 1997 with 0.1 second integration time
Table 3 gives half power beam widths (HPBW)
in right ascensions HPBWRA and declinations
HPBW Dec = r HPBWRA , for various elevations. The val­
ues of HPBWRA were obtained from our measurements.
Ignoring the aberration effects, we estimated the factor
r using theoretical simulations of the RATAN--600 beam
by Esepkina et al. (1979) and their experimental testing
by Temirova (1983). A map of the knife­like beam of the
RATAN--600 northern sector is known to have different
shapes of contours cross­sections at high and low power
levels. In the absence of aberrations, the shapes can be
described as ordinary elliptical contours (elongated on
declinations) at half power level and higher levels. The
contours are transformed to ``the elongated eight'' at
lower levels or to ``a dumb­bell'' at 0.1 normalized power
level (see Esepkina et al. 1979 for details).
The full permanent automatic control of 225 elements
of the main ring reflector was achieved using the new
control system of the antenna (Zhekanis 1997; Golubchin
et al. 1995). Errors in position of each element of the main
reflector, if present, were recorded in order to check the
quality of the antenna surface for each observation. The
positioning of cabin No. 1 with the secondary mirror was
measured from one of the eight geodetic reference points,
located every 20 meters along the rails. The accuracy of
semi­automatic positioning of the cabin directed towards
the focus was again checked by us some minutes before
each observation. If an error of more than 2 mm with re­
spect to a value given in the schedule was found, it was
corrected.
All horns of the radiometers are horizontally located
and form a new configuration, which is an optimal one
for decreasing transversal aberrations. Observations were
carried out in the main meridian (transit mode). As a
result, a response to an object is obtained due to its hori­
zontal scanning by the antenna beam because of the daily

Y.Y. Kovalev et al.: 1 \Gamma 22 GHz spectra of 550 extragalactic objects 551
Fig. 2. Example of fitting the simulated beam of RATAN--600
(lines) to the source response (dots) for 4C 39.25 from Fig. 1
rotation of the Earth (see an example of 4C 39.25 full scan
on Fig. 1; the moment of culmination is at 2: m 5 here). The
total duration of each six frequency observations was usu­
ally about five minutes, and included also two sets of noise
temperature calibration for 30 \Gamma 40 seconds before and af­
ter the passing of the source. The data acquisition sys­
tem (Chernenkov & Tsibulev 1995) controls radiometers
and records the output signals. After each observation, the
main ring reflector and the cabin No. 1 with receivers and
the secondary mirror were repositioned for observation of
the next source on a new elevation.
We have optimized the observational schedule, using
new software (Zhekanis & Zhekanis 1997). To increase the
reliability of results by final averaging of the spectra, we
endeavoured to include each source in the schedule two or
more times during the set and each flux density calibra­
tor in more than 70% of the days. The typical number of
sources observed in a 24 hour observing session was about
80 in the optimized schedule. Several breaks in observa­
tions occurred because of weather conditions (snow­falls
or unusually low temperatures t ! \Gamma15 ffi C), nine hours of
technical maintenance per week, etc. As a result, the total
number of successful observations was about 1450 during
21 days, or about 69 observations per day on average and
2.6 spectra per source during the set (formal averaging).
In 20% of the sources the spectra have been measured only
once.
4. Data reduction and calibration
Data reduction has been done using a YURZUF soft­
ware package, which had been specially designed for the
automatic reduction of the broad band spectra monitor­
ing observations (Kovalev 1998). Fitting a beam which is
simulated at the source elevation allows us to compute
Tab le 4. Parameters of calibration sources: flux density, Jy, and
correction factors gext and gpol (from top to bottom)
Source –, cm
1.4 2.7 3.9 7.7 13 31
0134+32 1.216 2.431 3.540 6.765 10.79 21.90
(h = 79: ffi 3) 1.016 1.004 1.002 1.000 1.000 1.000
1.032 1.046 1.039 0.959 1.004 1.002
0237\Gamma23 0.700 1.470 2.200 4.030 5.590 6.610
(h = 23: ffi 0) 1.000 1.000 1.000 1.000 1.000 1.000
0.979 0.979 0.979 1.025 0.992 0.983
0518+16 1.135 2.008 2.700 4.413 6.221 10.28
(h = 62: ffi 8) 1.000 1.000 1.000 1.000 1.000 1.000
0.954 0.956 0.923 1.104 0.930 0.964
0624\Gamma05 1.400 2.764 4.156 8.112 12.80 24.10
(h = 40: ffi 3) 1.034 1.009 1.004 1.001 1.000 1.000
1.027 1.020 1.021 1.025 0.942 1.017
1328+30 2.563 4.244 5.529 8.576 11.50 17.20
(h = 76: ffi 7) 1.016 1.004 1.002 1.000 1.000 1.000
1.053 0.948 0.957 1.049 0.954 0.954
2037+42 . . . . . . . . . 17.40 12.10 5.000
(h = 88: ffi 5) . . . . . . . . . 1.099 1.077 1.013
. . . . . . . . . 1.000 1.000 1.000
2105+42 5.330 5.940 6.100 5.050 2.850 . . .
(h = 88: ffi 4) 1.297 1.078 1.034 1.008 1.003 . . .
0.992 0.992 0.999 1.000 1.000 . . .
the amplitude of a source response at each frequency. A
Singular Value Decomposition subroutine from Forsythe
et al. (1977) was applied. Routine functions, designed by
V.R. Amirkhanyan, were also included via an additional
interface as a subroutine to the YURZUF software to sim­
ulate the main antenna beam together with the secondary
lobe. Before the reduction, the quality of such a fitting
has been checked and a simulation of the beam has been
optimized by tuning control parameters using the sample
of 30 \Gamma 50 sources which are strong and compact at all fre­
quencies, and distributed on different elevations (see an
example of fitting in Fig. 2).
The following seven flux density calibrators were ap­
plied to obtain the calibration curve in the scale of Baars
et al. (1977): 0134+32, 0237\Gamma23, 0518+16, 0624\Gamma05,
1328+30, 2037+42 (for calibration at 7.7, 13 and 31 cm
only), 2105+42 (excluding 31 cm calibration). They were
recommended by Baars et al. (1977), excluding 0237\Gamma23
which is the traditional RATAN--600 flux density calibra­
tor at low elevations. Measurements of some calibrators
were corrected, where necessary, on angular size and
linear polarization, following the data, summarized in
Ott et al. (1994) and Tabara & Inoue (1980) respectively.
Response to an extended calibrator was simulated as a
two­dimensional convolution of the beam and brightness
distribution in the published model of a calibrator. The
best fit to the observed response was found by optimiza­
tion of the angular size of an extended calibrator at each
frequency. The correction factor due to an angular exten­
sion g ext was calculated numerically by integrating over
the solid angle of the optimized brightness distribution
and the convolution of the distribution with the beam.
Following Ott et al. (1994), we applied Gaussian profiles
of the brightness distribution over right ascension and

552 Y.Y. Kovalev et al.: 1 \Gamma 22 GHz spectra of 550 extragalactic objects
Fig. 3. The flux density calibration factor F cal versus elevation h
at all wavelengths. Solid and dashed lines at 1.4, 2.7 and 3.9 cm
represent F cal for each horn separately. All data (crosses and
points with errors), shown for 6\Gamma7 calibrators, were averaged
during the observational set. Seven calibrators are shown at
7.7 and 13 cm, but the data for two calibrators at h = 88: ffi 4
and h = 88: ffi 5 are plotted in the same spot
declination for 0134+32, 0625\Gamma05, 1328+30, 2037+42
and the elliptical disk model for 2105+42, additionally
making an axial ratio to be equal to the measured one
in Masson (1989). The correction factor due to linear
polarization g pol of the calibrators was calculated in the
standard way (Kuzmin & Salomonovich 1964; Kraus
1966) as g pol = 1=[1 + p cos(2')], where p is the linear
polarization degree and ' is the angle between polariza­
tion planes of a source and the antenna. The corrected
amplitude of the response to a calibrator is calculated as
the observed one, multiplied by the factors g ext and g pol .
The flux densities of the calibrators, in Janskies, the
factors g ext and g pol are summarized in Table 4 for each
source (at the elevation h) at each wavelength from top
to bottom respectively. The flux densities were calculated
from polynomial approximations (Taylor 1999) of the
VLA measurements (relative to the spectrum of 3C 295)
for 0134+32, 0518+16, 1328+30; from spline and polyno­
mial approximations of the data by Ott et al. (1994) for
0624\Gamma05, 2037+42, 2105+42 (in relation to the spectra of
3C 295 and 3C 286), and from the polynomial approxi­
mation (K¨uhr et al. 1979) of the spectrum for 0237\Gamma23.
For 0134+32 and 1328+30 at 31 cm, we give preference to
the flux densities extrapolated from the approximations of
Ott et al. (1994). Taking into account all available data,
we also used two following extrapolated values: 0.70 Jy
for 0237\Gamma23 and 1.4 Jy for 0624\Gamma05 at the wavelength
of 1.4 cm. With these extrapolations, we have obtained
reasonable results.
Amplitude measurement of a source in flux density
units has been done in relation to an amplitude of a
flux density calibrator by comparing both with the am­
plitude of a stable signal from a noise generator, using
standard methods. In our observations the elevations of
seven flux density calibrators are fixed. Because of this
fact we computed a regression curve to obtain depen­
dence of the flux density calibration factor F cal on the
elevation for each horn on each frequency (Fig. 3). F cal
is equal to the amplitude of the noise generator signal,
calibrated in flux density units. In fact, the obtained cal­
ibration curves F cal (h) show the dependence of the mean
measured flux density for a source on the elevation h, if
its antenna temperature is equal to that of the noise gen­
erator signal T ns (Kovalev 1998): F cal (h) = 2kT ns =A aa
eff (h),
where A aa
eff (h) = A eff (h) q ab (h) q atm (h), A eff (h) is the ef­
fective area of the antenna in the focus, q ab (h) -- the factor
of aberration (due to transversal shifts of a feedhorn from
the focus), q atm (h) -- the atmosphere attenuation factor,
k -- the Boltsman's constant. We did not make any addi­
tional atmospheric correction during the set (the altitude
of RATAN--600 site is 970 m above see­level).
The total relative rms error of each individual flux den­
sity measurement oe=F is estimated from the following re­
lation (Kovalev 1998):
i oe
F
j 2
š
=
`
oe s
A s
' 2
š
+
`
oe ns
A ns
' 2
š
+
`
oe cal
F cal
' 2
š
+ (oe r
scale ) 2
š
;
where the first term inside the brackets on the right hand
is the relative error of the amplitude A s of a source (af­
ter fitting the simulated response to the observed one),
the second -- the relative error of the amplitude A ns of a
response to the noise generator signal, the third -- the rela­
tive error of our flux density calibration F cal , averaged on
the set, and the last -- the relative error oe r
scale of the abso­
lute flux density scale. Usually, the last term is excluded
from presented errors, but we show it in the relation to em­
phasize its importance, because different calibrators may
be used in various works.
The total error oe is calculated, excluding only the oe r
scale
error, which is estimated by Baars et al. (1977), Ott et al.
(1994) and Taylor (1999) as about 10% at 1.4 cm and
3 \Gamma 5% at other wavelengths. It is better to increase oe r
scale
to 10 \Gamma 15% at 1.4 cm for the sources with declinations
less than \Gamma5 ffi because of the above mentioned extrapola­
tion of the flux density values for 0624\Gamma05 and 0237\Gamma23.
Errors (oe cal =F cal ) of the calibration depend on elevation
and are formally less than 2.6, 0.7, 1.4, 1.1, 0.7 and 0.9%
at 1.4, 2.7, 3.9, 7.7, 13 and 31 cm respectively (the errors
are averaged here over two horns at 1:4 \Gamma 3:9 cm, Fig. 3).
Mean values are always calculated as the mean
weighted values, if several measurements have been made,
with corrections by the Student's factor to increase the

Y.Y. Kovalev et al.: 1 \Gamma 22 GHz spectra of 550 extragalactic objects 553
reliability to the standard value 0.683 for one sigma error.
The dispersion of frequent measurements of calibrators
(and, consequently, oe cal and oe) as well as calculated
errors of mean spectra measurements represent also
random instrumental instabilities and a variability due to
atmosphere conditions during the set.
Systematic errors caused by various reasons including
calibration are known to be often the main real errors. We
have compared our results with published observations of
other authors to check the residual systematic errors, us­
ing several tens of strong objects distributed on elevations
with constant or slightly variable broad band spectra. The
agreement is found to be quite good within the total ac­
curacy of the data.
5. Results
Table 5 with the results of observations is available in
the electronic form only at the CDS via anonymous ftp.
It includes the flux density data (with one sigma errors
without scale errors oe r
scale ) at 1.4, 2.7, 3.9, 7.7, 13 and
31 cm for 546 of 551 objects of the source list from
Table 1. Instantaneous observations of the spectra are
shown at Fig. 4. Averaged instantaneous spectra are given
in Table 5 and Fig. 4, if two or more observations of a
source have been done.
The sources 0156\Gamma14, 1635\Gamma03 were not observed in
December, 1997. We have pointed the antenna to the coor­
dinates of 0611+13 several times, but we have not detected
an emission from the source at any frequency (nothing is
present at the coordinates of 0611+13 in NED too). The
object 3C 274 is resolved by RATAN--600 at all observed
frequencies; multifrequency response to 3C 111 has a dou­
ble maximum.We have excluded the data for these sources
from final results.
Absence of data for some sources at some frequencies is
a result, in general, of data exclusion for the following rea­
sons: possible confusion in declinations (especially at low
elevations) or partial resolution of a source at some fre­
quencies (e.g. 3C 154 at 1.4, 2.7, 3.9, 7.7 cm), a source is
too weak to be measured reliably (e.g. III Zw 2 at 31 cm),
a strong influence of man­made interferences (frequently
at 31 cm, sometimes at 13 cm), strong interferences from
a stationary placed satellite at 2.7 and 7.7 cm (in declina­
tions between \Gamma10 ffi and 0 ffi ). Nevertheless, in some cases
the data was not excluded in spite of the increase in errors
caused usually by interferences.
We believe that shapes of the instantaneous spectra
presented can be explained by continuous activity of the
nuclei of the objects in accordance with the basic hypoth­
esis of a source with two dominating general components
(compact and extended), following Kovalev et al. (1996),
Kovalev & Kovalev (1996). The detailed analysis of the
data is deferred to later papers.
Acknowledgements. We would like to thank the RATAN--600
staff for technical support of the observational process. Some
of our problems in achieving the twenty four hour observations
were resolved through the valuable assistance of Ira Morozova.
We are obliged to Harry Ter¨asranta for providing us with the
unpublished data of 22 GHz Mets¨ahovi observations to check
our calibration at this frequency, to Greg Taylor for observ­
ing the object 0237\Gamma23 at our request at the VLA in 1998
and 1999 in order to study known high frequency discrep­
ancy of the source spectrum, and to Vladimir Amirkhanyan
for kindly making his routine on simulating the RATAN--600
beam available at our disposal. We thank Tanya Downs and
an anonymous referee for carefully reading the manuscript and
for valuable comments. YYK and YAK are grateful to the ad­
ministration and employees of the observatory for their hospi­
tality during the visit for carrying out the observations. This
work has been partly supported by the Russian State Program
``Astronomy'' (grant 1.2.5.1). YYK acknowledges support from
International Soros Science Educational Program grants a97--
2965, a98--1932 and a99--1882. This research has made use of
the NASA/IPAC Extragalactic database (NED), which is oper­
ated by the Jet Propulsion Laboratory, Caltech, under contract
with the National Aeronautic and Space Administration.
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