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ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 139, 545­554 (1999)

NOVEMBER I 1999, PAGE 545

Survey of instantaneous 1 - 22 GHz spectra of 550 compact extragalactic ob jects with declinations from -30 to +43
Y.Y. Kovalev1 , N.A. Nizhelsky2 , Yu.A. Kovalev1 , A.B. Berlin3 , G.V. Zhekanis2 , M.G. Mingaliev2 , and A.V. Bogdantsov2
1 2 3

Astro Space Center of the Lebedev Physical Institute, Profsoyuznaya 84/32, Moscow, 117810, Russia Special Astrophysical Observatory, Nizhny Arkhyz, Karachaevo­Cherkessia, 357147, Russia Special Astrophysical Observatory, St. Petersburg Branch, St. Petersburg, 196140, Russia

Received March 26; accepted August 13, 1999

Abstract. We present observational results for extragalactic radio sources with milliarcsecond components, obtained with the 600 meter ring radio telescope RATAN­600 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 -30 and +43 with a correlated flux density exceeding 0.1 Jy at 13 cm. The sample includes the ma jority 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 ob jects: 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 ob ject. The extragalactic radio sources are often 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.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.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 compact extragalactic ob jects 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 quasisimultaneously (over a period of one or more months) at radio and shorter wavelengths, using several telescopes on some samples of tens of ob jects, selected by various criteria. For example, we refer to the measurements of 19 active extragalactic sources from 20 cm to 1400 ° by A Landau et al. 1986). Valtao ja et al. (1988) investigated quiescent spectra for a sample of 27 radio sources observed at centimeter and millimeter wavelengths. Gear et al. (1994) compared quasi-simultaneous 5 - 375 GHz spectra of 22 BL Lacertae ob jects with 24 radio-loud, violently variable quasars. Kuhr et al. (1981) compiled ¨ radio measurements at more than two frequencies for 494 sources from the combined NRAO­MPI 5 GHz Strong Source Surveys and the Parkes 2.7 GHz Surveys. Herbig & Readhead (1992) composed non-simultaneous radio data from 10 MHz to 100 GHz on a complete sample of 256 objects. We also refer to papers, cited in the O'Dea (1998) survey of compact steep-spectrum and gigahertz peakedspectrum sources, as well as a number of other works. Some earlier RATAN­600 results on broad band spectra 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 ob jects 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 radio source is usually considered to be the sum of spectra of several compact and extended components in a source structure. The components are located at various


546 Table 1. Source sample IAU 0003+38 0003-06 0005-23 0005-26 0007+10 0007+17 0008-26 0010+40 0011-04 0012+31 0013-00 0019+05 0022+39 0024+34 0026+34 0027+05 0035+23 0035+12 0035-02 0038-02 0047+02 0048-09 0048-07 0054-00 0055+30 0055-05 0056-00 0106+01 0108-07 0108+38 0109+22 0110+31 0111+02 0112-01 0113-11 0116+08 0118-27 0119+11 0119+04 0119+24 0122-00 0123+25 0127+14 0130-17 0133-20 0134+32 0135-24 0136+17 0138-09 0142-27 0144+20 0146+05 0147+18 0148+27 0149+21 0149+33 0156-14a Other NRAO 5 OB -210 III Zw 2 4C 17.04 OB -214 4C 40.01 3C 6 OB OA OB OB 34 26 338 343

Y.Y. Kovalev et al.: 1 - 22 GHz spectra of 550 extragalactic ob jects

CTD 5 4C 12.05 3C 17 OB 78 OB -80 OB -82 NGC 315 DA 4C OC OC 32 01.02 -14 314

NRAO 62 UGC 773

4C 08.06 OC -230.4 OC 33

4C 25.05 4C 14.06 OC -255.3 3C 48 OC -259 OC -65 OC -270 OC 79 OC 178

OC 383

OI G BL Q G G Q Q Q Q G Q BL Q G G Q Q Q G Q BL BL Q Q G Q Q Q Q G BL Q G Q Q G BL Q Q Q Q Q Q Q Q Q Q Q BL Q RS Q Q Q Q Q RS

Z 0.229 0.347 1.410 0.090 1.601 1.093 0.256

1.574 1.946 0.333 0.6 2.27 1.395 0.220 1.176

1.975 2.795 0.016 0.717 2.107 1.776 0.668 0.603 0.047 1.365 0.672 0.594 >0.557 0.570 0.637 2.025 1.070 2.364 1.020 1.141 0.367 0.831 2.716 >0.501 1.157 2.345 1.26 1.32 2.431

IAU 0159-11 0201+11 0202+14 0202+31 0202-17 0211+17 0216+01 0217-18 0219+42 0219-16 0221+06 0223+34 0226-03 0229+13 0234+28 0235+16 0237-02 0237+04 0237-23 0238-08 0239+10 0240-21 0248+43 0250+17 0256+07 0301+33 0306+10 0309+41 0312+10 0316+16 0316+41 0317+18 0319+12 0322+22 0326+27 0327-24 0329-25 0333+32 0336-01 0338-21 0340+36 0344+19 0346-16 0348-12 0400+25 0402+37 0403-13 0405-12 0406+12 0406-12 0409+22 0410+11 0413-21 0414-18 0415+37b 0420+02 0420+41

Other 3C 57 OD 101 NRAO 91

3C 66A 4C 06.11 4C 34.07 4C -03.07 4C 13.14 CTD 20 OD 160 OD 62 OD -263 NGC 1052 OD 166 OD -267

OD 94.7 4C 33.06 OE 110 NRAO 128 4C 10.10 CTA 21 3C 84 OE 129 OE 131 OE -246.3 OE -248 NRAO 140 CTA 26 OE -263.9 OE 367 OE -182 CTD 26 4C 37.11 OF -105 OF -109 OF -111 3C 108 3C 109

3C 111 4C 41.11

OI Q Q G Q Q Q Q Q BL Q Q Q Q Q Q BL Q Q Q G Q Q Q Q Q G Q G G Q G G Q RS Q Q Q Q Q BL Q RS Q Q Q G Q Q BL Q Q G Q Q G BL RS

Z 0.669 3.56 0.405 1.466 1.740 0.472 1.623 0.444 0.698 0.511 2.066 2.065 1.207 0.940 1.116 0.978 2.225 0.005 0.314 1.310 0.893 0.863 0.136

0.017 2.67 1.533 0.888 2.685 1.259 0.852 1.484

1.520 2.109 0.054 0.571 0.574 1.02 1.563 1.213 0.306 0.807 1.536 0.048

IAU 0420-01 0421+01 0422+00 0423+23 0423+05 0425+04 0428+20 0429+41 0430+05 0434-18 0440-00 0446+11 0451-28 0454+03 0454+06 0454-23 0456+06 0457+02 0458-02 0458+13 0459+06 0459+13 0459+25 0500+01 0502+04 0507+17 0509+15 0511-22 0514-16 0518+16 0521-26 0528-25 0528+13 0537-15 0537-28 0552+39 0555-13 0601+24 0602+40 0605-08 0606-22 0607-15 0610+26 0611+13c 0618-25 0620+38 0641+39 0642+21 0650+37 0653-03 0711+35 0722+14 0723-00 0727+40 0727-11 0729+25 0733+30

Other OA 129 OF 36 OF 38

OF OF 3C 3C

42 247 119 120

NRAO 190 OF OF 4C OF OF OF DA -285 92 06.21 -292 94 97 157

OF 99.3 3C 133 OG 3 OG 5 OG -220 OG -123 3C 138 OG -236 OG -247 OG 147 OG -263 DA 193 4C OH OH OH OH 3C OH OH OH 3C 24.11 404.1 -10 -212 -112 154 -230 335 368.8 166

OI Q Q BL RS Q Q G Q G Q Q G Q Q G Q Q Q Q RS Q BL G Q Q G RS Q Q Q RS Q Q Q Q Q Q RS RS Q Q Q Q Q Q Q G Q Q Q Q BL Q RS Q RS

Z 0.915 2.055

1.333 0.219 1.023 0.033 2.702 0.844 1.207 2.560 1.349 0.405 1.003 1.08 2.384 2.286 1.106 0.277 0.585 0.954 0.416 1.296 1.270 0.759 2.765 2.07 0.947 3.104 2.365

0.872 1.926 0.324 0.580 1.90 3.469 1.266 0.245 1.982 1.620 0.127 2.501

OH -90 OI 318 4C 14.23 OI -39 OI 446


Y.Y. Kovalev et al.: 1 - 22 GHz spectra of 550 extragalactic ob jects Table 1. continued IAU Other 0733-17 0733+26 0735+17 OI 158 0736-06 OI -61 0736+01 OI 61 0738+31 OI 363 0738+27 0742+31 4C 31.30 0742+10 OI 471 0743-00 4C -00.28 0743+25 0743+27 0745+24 OI 275 0748+12 OI 280 0748+33 OI 380 0752-11 OI -187 0754+10 OI 90.4 0759+18 0802+21 0805+41 0805+26 0805-07 0808+01 OJ 14 0812+36 OJ 320 0812+02 4C 02.23 0814+42 OJ 425 0818-12 OJ -131 0820+22 4C 22.21 0820+29 OJ 234 0821+39 4C 39.23 0823+03 OJ 38 0827+24 OJ 248 0829+04 OJ 49 0830+42 OJ 451 0834+25 OJ 259 0837+03 0838+13 3C 207 0839+18 0851+07 0851+20 OJ 287 0854+21 0855+14 3C 212 0859-14 OJ -199 0900+42 4C 42.28 0906+43 3C 216 0906+01 DA 263 0912+02 0912+29 OK 222 0913+39 4C 38.28 0915-21 0922+00 OK 37 0923+39 4C 39.25 0925-20 0931-11 OK -152 0938+11 0945+40 4C 40.24 0952+17 OK 186

547

OI RS RS BL Q Q Q RS Q RS Q RS RS Q Q Q RS BL Q RS Q RS Q BL Q Q BL BL BL Q Q BL Q BL Q Q Q Q Q RS BL RS Q Q G Q Q G BL Q Q Q Q Q RS Q Q Q

Z

>0.424 1.901 0.191 0.630 0.462 0.994

0.409 0.889 1.932 0.66

1.420 1.837 1.025 0.402

0.951 2.368 1.216 0.506 0.941 0.180 0.253 1.122 1.57 0.684 1.272 0.306 1.043 1.339 0.670 1.018 0.427 1.269 0.847 1.719 0.698 0.348 3.191 1.252 1.478

IAU 0953+25 0955+32 1004-01 1004+14 1008-01 1010+35 1012+23 1013+20 1015+35 1018+34 1019+42 1019+30 1020-10 1020+19 1020+40 1021-00 1022+19 1030+41 1030+39 1032-19 1034-05 1034-29 1036-15 1038+06 1040+12 1042+07 1045-18 1046-02 1054+00 1055+20 1055+01 1058+39 1100+22 1101+38 1102-24 1104+16 1106+38 1109+35 1110-21 1111+14 1116+12 1119+18 1120-27 1123+26 1124-18 1127-14 1128+38 1128-04 1130+00 1136-13 1142+05 1142-22 1143-24 1143-28 1144+40 1145-07 1148-00

Other OK 290 3C 232 OL 4C OL 4C OL OL OL OL OL OL 4C 108.1 -01.21 318 23.24 224 326 331 333 -133 133 40.25

4C 19.34

OL OL OL 4C 3C OL 4C OL 4C OL

-257 -259 -161 06.41 245 -176 -02.43 91 20.24 93

OM 201 Mark 421 OM -204 4C 16.30 OM -218 OM 118 4C 12.39 OM 133 OM -234 CTD 74 OM -146 OM -48 CTS 667 4C 05.52 OM -271 OM -272 OM -273 OM -76 4C -00.47

OI Q Q Q Q Q Q Q Q Q Q RS Q Q Q Q Q Q Q Q Q G Q G Q Q G Q RS RS Q Q RS RS BL Q Q G RS RS Q Q Q RS Q Q Q Q G Q Q Q Q Q Q Q Q Q

Z 0.712 0.530 1.214 2.707 0.887 1.414 0.565 3.11 1.226 1.400 1.319 0.197 2.136 1.254 2.552 0.828 1.120 1.095 2.198 0.312 0.525 1.265 1.028 0.698 0.595

1.11 0.888

0.031 1.666 0.632 2.290

0.869 2.118 1.040 2.341 1.048 1.187 1.733 0.266 0.554 1.342 1.141 1.940 0.45 1.089 1.342 1.980

IAU 1148-17 1156-22 1156-09 1156+29 1157-21 1200-05 1200+04 1202-26 1204+28 1210+13 1211+33 1213-17 1213+35 1215+30 1216-01 1217+02 1218+33 1218-02 1219+28 1219+04 1222+03 1222+21 1225+36 1226+02 1228+12b 1228-11 1236+07 1237-10 1240+38 1240-29 1243-07 1244-25 1252+11 1253-05 1255+32 1256-220 1256-229 1257+14 1302-03 1302-10 1308+32 1308+14 1315+34 1317-00 1318-26 1330+02 1331+17 1334-12 1336-23 1336-26 1337-03 1345+12 1347-21 1348-28 1349-14 1351-01 1352-10

Other OM -181 OM -94 4C 29.45 ON -1

ON 4C ON ON 4C ON ON 3C 4C ON 4C 4C 4C ON 3C 3C ON

208 13.46 319 -122 35.28 325 29 270.1 -02.53 231 04.42 03.23 21.35 343 273 274 -147

ON -162 ON -73 ON 3C ON ON 187 279 393 -293.9

OW 197 OP OP OP OP 4C 3C OP OP OP -106 313 114 326 -00.50 287.1 151 -158.3 -260.5

4C 12.50 OP -279 OP -182 OP -187

OI Q G RS Q Q Q RS Q Q Q Q G Q BL Q Q Q G BL Q Q Q Q Q G Q G Q Q Q Q Q Q Q RS Q Q Q Q Q BL Q Q Q Q G Q Q Q Q Q G RS Q RS Q Q

Z 1.751 0.565 0.729 0.927 0.381 0.790 2.177 1.137 1.598 0.857 0.237 0.415 0.240 1.519 0.665 0.102 0.965 0.960 0.435 1.975 0.158 0.004 3.528 0.400 0.750 1.316 1.133 1.286 0.638 0.870 0.538 1.306 1.365 1.250 0.286 0.997 1.050 0.892 2.027 0.215 2.084 0.539 1.51 0.121

3.707 0.332


548 Table 1. cont IAU 1354-17 1354-15 1354+19 1356+02 1402-01 1402+04 1403-08 1404+28 1406-07 1406-26 1413+34 1416+06 1427+10 1430-17 1430-15 1434+23 1435-21 1437-15 1438+38 1439+32 1441+25 1442+10 1443-16 1445-16 1449-01 1452+30 1456+04 1502+10 1502+03 1504+37 1504-16 1508-05 1510-08 1511-10 1511-21 1514+00 1514+19 1514-24 1518+04 1519-27 1525+31 1532+01 1535+00 1538+14 1543+00 1546+02 1548+05 1548+11 1550-26 1551+13 1555+00 1555-14 1556-24 1600+33 1604+31 1606+10 1607+26 inued Other OP -192 4C 19.44

Y.Y. Kovalev et al.: 1 - 22 GHz spectra of 550 extragalactic ob jects

OQ 208 OQ -10 OQ 323 3C 298 OQ 147 OQ -151 OQ -150.2 OQ 257 OQ -259 OQ -162 OQ 363 OQ 366 OQ 172 OQ -171 OQ -176 OQ -81 OQ 287 4C 04.49 4C 10.39 OR OR 4C OR OR OR GN 306 -102 -05.64 -17 -118 -218 Z 25

AP Librae 4C 04.51 OR 342

4C 14.60 OR 78 4C 05.64 OR 181 OR 186

OS 300 DA 401 OS 111

OI Q Q Q Q Q Q Q G Q Q RS Q Q Q Q Q Q BL Q Q Q Q Q Q Q Q G Q G G Q Q Q Q G G BL BL G BL Q Q Q BL G Q Q Q Q Q Q G Q G G Q G

Z 3.147 1.89 0.719 1.319 2.522 3.211 1.763 0.077 1.493 2.43 1.439 1.71 2.331 1.573 1.187 1.775 2.12 0.062 3.535 2.417 1.314 0.580 0.394 1.833 0.413 0.674 0.876 1.191 0.360 1.513 1.179 0.052 0.048 1.294 1.380 1.420 3.497 0.605 0.550 0.412 1.422 0.436 2.145 1.29 1.772 0.097 2.818

1.226 0.473

IAU 1611+34 1614+05 1615+36 1615+02 1616+06 1622-25 1622-29 1624+41 1625-14 1633+38 1635-03a 1638+39 1641+39 1647-29 1648+01 1652+39 1655+07 1656+05 1656+34 1657-26 1705+01 1706+00 1706-17 1717+17 1721+34 1722+40 1725+12 1725+04 1730-13 1732+09 1741-03 1743+17 1749+09 1751+28 1756+23 1758+38 1807+27 1821+10 1830+28 1848+28 1901+31 1908-20 1908-21 1920-21 1921-29 1923+21 1936-15 1937-10 1947+07 1958-17 2002-18 2008-15 2008-06 2012-01 2029+12 2032+10 2037-25

Other DA 406 OS 23 4C 36.27 OS 28 OS -237.8 4C 41.32 4C 38.41 NRAO 512 3C 345

Mark 501 OS 92 OS 94 OS 392

OT -111 OT 129 4C 34.47 OT 143.3 NRAO 530 OT 54 OT -68 OT 172 OT 81 OT 295 OT 398 4C 27.41 CTD 108 3C OV OV OV OV OV OV 395 -213 -214 -235 -236 239.7 -161 80 -198 -185 -115 -15

OV OV OW OW OW

OW 149 OW 154.9

OI Q Q RS Q Q Q Q Q Q Q Q Q Q RS RS BL Q Q Q RS Q G RS BL Q Q Q Q Q G Q Q BL RS Q Q Q Q Q Q Q Q RS RS BL RS Q Q Q Q Q Q G BL BL BL Q

Z 1.401 3.217 1.341 2.088 0.786 0.815 2.55 1.10 1.807 2.856 1.666 0.594

0.033 0.621 0.879 1.936 2.576 0.449

0.206 1.049 0.293 0.902 1.057 1.702 0.320 1.721 2.092 1.760 1.364 0.594 2.56 0.635

0.352 1.657 3.787 0.652 0.868 1.180 1.047 1.215 0.601 1.574

IAU 2044-16 2047+09 2047+03 2053-04 2058-29 2059+03 2113+29 2121+05 2126-15 2126-18 2127-09 2128+04 2128-12 2131-02 2134+00 2135-24 2136+14 2140-04 2143-15 2144+09 2145+06 2147+14 2149+06 2149+05 2150+17 2155-15 2200-23 2200+42 2201+31 2201+17 2201+04 2207+35 2208-13 2209+08 2209+23 2214+35 2215+02 2216-03 2223-05 2223+21 2227-08 2229-17 2230+11 2233-14 2234+28 2236+12 2239+09 2240-26 2243-12 2245-12 2245+02 2246+20 2247+13 2251+15 2251+24 2251+13 2252-09

Other OW -174 4C -04.80 OW 98 OX 36 OX -146 OX -145 OX OX 4C OX 46 -148 -02.81 57

OX 161 OX -173 OX 74 DA 562 OX OX OX OX BL 4C OY 4C OY 81 82 183 -192 Lacertae 31.63 101 04.77 313

DA 574 OY 324 4C -03.79 3C 446 DA 580 OY -150 CTA 102 OY -156 CTD 135 OY 160 OY -268 OY -172.6

4C 3C DA 4C

13.84 454.3 587 13.85

OI Q RS BL Q Q Q Q Q Q Q Q G Q BL Q Q Q Q Q Q Q RS Q Q BL Q Q BL Q Q G RS Q Q Q Q Q Q Q Q Q Q Q BL Q Q Q BL Q Q Q RS Q Q Q Q Q

Z 1.932

1.176 1.492 1.015 1.514 1.941 3.266 0.680 >0.780 0.990 0.501 1.285 1.932 0.819 2.427 0.344 0.698 1.113 0.999 1.364 0.740 0.672 2.118 0.069 0.298 1.076 0.028 0.391 0.484 0.510 3.581 0.901 1.404 1.953 1.562 1.780 1.037 >0.609 0.795 1.707 0.774 0.630 1.892

0.767 0.859 2.327 0.677 0.606


Y.Y. Kovalev et al.: 1 - 22 GHz spectra of 550 extragalactic ob jects Table 1. continued IAU 2253+41 2254+02 2254+07 2255+41 2255-28 2256+01 2300-18 2303-05 2307+10 2318+04 2318-19 2319+31 2319+27 2320+07 2320-02 2320-03 2325-15 2327+33 2328+10 2328+31 2329-16 2330+08 2331-24 2332-01 2335-18 2335-02 2337+26 2338+33 2344+09 2344+092 2345-16 2349-01 2351-00 2351-15 2354-11 2355-10 2356+19 2356+38
a b c

549

Other OY 489 OY 91.3 OY 091 4C 41.45 -102 -05.95 10.70 031 -130

OZ 4C 4C OZ OZ

CTD 139 DA 599

4C OZ OZ OZ OZ

10.73 347 -149 50.8 -252

OZ -160

4C 09.74 OZ -176 4C -01.61 OZ -187

OZ 193 OZ 395

OI Q Q BL Q Q Q G Q RS Q G G Q Q Q Q Q Q Q RS Q RS G Q Q Q Q RS Q RS Q Q Q Q Q Q Q Q

Z 1.476 2.089 0.190 2.15 0.926 2.663 0.129 1.139 0.623

1.253 2.090 1.411 2.465 1.809 1.489 1.153 0.048 1.184 1.450 1.072

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 long-term program of instantaneous spectra monitoring of compact extragalactic ob jects (Kovalev 1998), which have milliarcsecond components and are studied by VLBI networks. They also give a ground spectra support for the VSOP survey and a pre-launch spectra study of the ob jects for the RadioAstron pro ject. The goal of the long-term 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 co density F13 rr 0.1 Jy at the wavelength of 13 cm, and are located north of declination -30 . The northern sector of RATAN­600 restricts this declination range from -30 to +43 . Measurements of the sources located north of declination +49 were made in 1998 with the southern sector of RATAN­600 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 Veron­Cetty & 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 ob jects, "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 classifications from Veron­Cetty & Veron (1998).

0.673 0.576 0.174 0.463 2.675 0.960 1.622 1.066 2.704

The source was not observed in December, 1997. The source was partly resolved at all frequencies. We have not registered emission from this ob ject at any frequency (nothing is present at these coordinates in NED too).

distances from the central nucleus of the ob ject, and are likely to have resulted from activity within the nucleus. The nucleus may be a black hole, which converts an accreted 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

3. Observations We performed continuous six frequency 1 - 22 GHz spectra observations of compact extragalactic sources from 1st to 22nd December, 1997. We used the 600 meter ring radio telescope RATAN­600 (Korolkov & Parijskij 1979; Parijskij 1993) at the Russian Academy of Sciences' Special Astrophysical Observatory, located in Karachaevo-Cherkessia Republic (Russia) near Nizhny Arkhyz and Zelenchukskaya at the North Caucasus.


550

Y.Y. Kovalev et al.: 1 - 22 GHz spectra of 550 extragalactic ob jects

Table 2. Parameters of RATAN­600 broad band receivers in 1997, used in this work , cm 1.4 2.7 3.9 7.7 13 31 nh 2 2 2 1 1 1 0 , GHz 21.65 11.2 7.70 3.90 2.30 0.96 , GHz 2.5 1.4 1.0 0.6 0.4 0.12
phys TLNA , K 15 15 15 15 310 310

TLNA , K 23 18 14 8 35 21

Tsys , K 77 70 62 37 95 105

Tsys , mK 3.5 3 3 2.5 8 15

Table 3. Measured and estimated beam widths and ratios r for the RATAN­600 northern sector with the secondary mirror No. 1 for different wavelengths and elevations h , cm HPBWRA â HPBWDec h = 80 h = 40 h = 20 r5 r 10 r 20 8. 0 â 35 8. 5 â 1. 4 13 â 4. 3 17 â 2. 8 24 â 8. 0 16 â 1. 3 23 â 2. 0 26 â 4. 3 39 â 13 48 â 4. 0 53 â 8. 8 1. 4 â 27 1. 3 â 6. 5 1. 3 â 13 1. 8 â 37 3. 2 â 16 3. 3 â 33 5. 0 â 100 Fig. 1. Example of a full multifrequency scan for 4C 39.25, observed on 16 December 1997 with 0.1 second integration time

1.4 2.7 3.9 7.7 13 31

The northern sector of the antenna (a part of the main ring reflector) was used together with the secondary mirror 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 essentially higher than earlier experiments conducted at the RATAN­600 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 wavelengths 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 nh ; exact central frequencies 0 ; band widths ; physical phys temperatures of the LNA TLNA ; noise temperatures of the LNA TLNA ; total noise temperatures of systems Tsys , including the antenna noise at middle elevations; rms noise temperature sensitivities of the system Tsys for a one second integration time. Dual-feedhorn receivers are beamswitched. Single-feedhorn receivers have a noise-added, gain-balanced mode of operation. Linearly polarized systems were available at all frequencies: horizontal at 7.7 cm and vertical at other wavelengths.

Table 3 gives half power beam widths (HPBW) in right ascensions HPBWRA and declinations HPBWDec = r HPBWRA , for various elevations. The values of HPBWRA were obtained from our measurements. Ignoring the aberration effects, we estimated the factor r using theoretical simulations of the RATAN­600 beam by Esepkina et al. (1979) and their experimental testing by Temirova (1983). A map of the knife-like beam of the RATAN­600 northern sector is known to have different shapes of contours cross-sections 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 dumb-bell" 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 semi-automatic 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 respect 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 ob ject is obtained due to its horizontal scanning by the antenna beam because of the daily


Y.Y. Kovalev et al.: 1 - 22 GHz spectra of 550 extragalactic ob jects

551

Table 4. Parameters of calibration sources: flux density, Jy, and correction factors gext and gpol (from top to bottom)
Source 0134+32 (h = 79 3) . 0237-23 (h = 23 0) . 0518+16 (h = 62 8) . 0624-05 (h = 40 3) . 1328+30 (h = 76 7) . 2037+42 (h = 88 5) . 2105+42 (h = 88 4) . 1.4 1.216 1.016 1.032 0.700 1.000 0.979 1.135 1.000 0.954 1.400 1.034 1.027 2.563 1.016 1.053 ... ... ... 5.330 1.297 0.992 2.7 2.431 1.004 1.046 1.470 1.000 0.979 2.008 1.000 0.956 2.764 1.009 1.020 4.244 1.004 0.948 ... ... ... 5.940 1.078 0.992 , cm 3.9 7.7 3.540 6.765 1.002 1.000 1.039 0.959 2.200 4.030 1.000 1.000 0.979 1.025 2.700 4.413 1.000 1.000 0.923 1.104 4.156 8.112 1.004 1.001 1.021 1.025 5.529 8.576 1.002 1.000 0.957 1.049 ... 17.40 ... 1.099 ... 1.000 6.100 5.050 1.034 1.008 0.999 1.000 13 10.79 1.000 1.004 5.590 1.000 0.992 6.221 1.000 0.930 12.80 1.000 0.942 11.50 1.000 0.954 12.10 1.077 1.000 2.850 1.003 1.000 31 21.90 1.000 1.002 6.610 1.000 0.983 10.28 1.000 0.964 24.10 1.000 1.017 17.20 1.000 0.954 5.000 1.013 1.000 ... ... ...

Fig. 2. Example of fitting the simulated beam of RATAN­600 (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 2m 5 here). The . total duration of each six frequency observations was usually about five minutes, and included also two sets of noise temperature calibration for 30 - 40 seconds before and after the passing of the source. The data acquisition system (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 calibrator 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 observations occurred because of weather conditions (snow-falls or unusually low temperatures t < -15 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 software package, which had been specially designed for the automatic reduction of the broad band spectra monitoring observations (Kovalev 1998). Fitting a beam which is simulated at the source elevation allows us to compute

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 simulate 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 - 50 sources which are strong and compact at all frequencies, and distributed on different elevations (see an example of fitting in Fig. 2). The following seven flux density calibrators were applied to obtain the calibration curve in the scale of Baars et al. (1977): 0134+32, 0237-23, 0518+16, 0624-05, 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 0237-23 which is the traditional RATAN­600 flux density calibrator 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 two-dimensional convolution of the beam and brightness distribution in the published model of a calibrator. The best fit to the observed response was found by optimization of the angular size of an extended calibrator at each frequency. The correction factor due to an angular extension gext 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 - 22 GHz spectra of 550 extragalactic ob jects

Fig. 3. The flux density calibration factor Fcal versus elevation h at all wavelengths. Solid and dashed lines at 1.4, 2.7 and 3.9 cm represent Fcal for each horn separately. All data (crosses and points with errors), shown for 6-7 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 4 . and h = 88 5 are plotted in the same spot .

for 0237-23 and 1.4 Jy for 0624-05 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 amplitude 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 dependence of the flux density calibration factor Fcal on the elevation for each horn on each frequency (Fig. 3). Fcal is equal to the amplitude of the noise generator signal, calibrated in flux density units. In fact, the obtained calibration curves Fcal (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 generator signal Tns (Kovalev 1998): Fcal (h) = 2kTns /Aaa (h), eff where Aaa (h) = Aeff (h) q ab (h) q atm (h), Aeff (h) is the efeff 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 additional atmospheric correction during the set (the altitude of RATAN­600 site is 970 m above see-level). The total relative rms error of each individual flux density measurement /F is estimated from the following relation (Kovalev 1998): F
2

declination for 0134+32, 0625-05, 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 gpol of the calibrators was calculated in the standard way (Kuzmin & Salomonovich 1964; Kraus 1966) as gpol = 1/[1 + p cos(2)], where p is the linear polarization degree and is the angle between polarization 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 gext and gpol . The flux densities of the calibrators, in Janskies, the factors gext and gpol 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 polynomial approximations of the data by Ott et al. (1994) for 0624-05, 2037+42, 2105+42 (in relation to the spectra of 3C 295 and 3C 286), and from the polynomial approximation (Kuhr et al. 1979) of the spectrum for 0237-23. ¨ 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

=


s As

2

+


ns Ans

2

+


cal Fcal

2 r +(sc 2 ale )

,

where the first term inside the brackets on the right hand is the relative error of the amplitude As of a source (after fitting the simulated response to the observed one), the second ­ the relative error of the amplitude Ans of a response to the noise generator signal, the third ­ the relative error of our flux density calibration Fcal , averaged on r the set, and the last ­ the relative error scale of the absolute flux density scale. Usually, the last term is excluded from presented errors, but we show it in the relation to emphasize its importance, because different calibrators may be used in various works. r The total error is calculated, excluding only the 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 r 3 - 5% at other wavelengths. It is better to increase scale to 10 - 15% at 1.4 cm for the sources with declinations less than -5 because of the above mentioned extrapolation of the flux density values for 0624-05 and 0237-23. Errors (cal /Fcal ) 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 - 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 - 22 GHz spectra of 550 extragalactic ob jects

553

reliability to the standard value 0.683 for one sigma error. The dispersion of frequent measurements of calibrators (and, consequently, cal and ) 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, using several tens of strong ob jects distributed on elevations with constant or slightly variable broad band spectra. The agreement is found to be quite good within the total accuracy 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 r without scale errors scale ) at 1.4, 2.7, 3.9, 7.7, 13 and 31 cm for 546 of 551 ob jects 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 0156-14, 1635-03 were not observed in December, 1997. We have pointed the antenna to the coordinates 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 ob ject 3C 274 is resolved by RATAN­600 at all observed frequencies; multifrequency response to 3C 111 has a double 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 reasons: possible confusion in declinations (especially at low elevations) or partial resolution of a source at some frequencies (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 man-made interferences (frequently at 31 cm, sometimes at 13 cm), strong interferences from a stationary placed satellite at 2.7 and 7.7 cm (in declinations between -10 and 0 ). 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 ob jects in accordance with the basic hypothesis 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.

Acknow ledgements. We would like to thank the RATAN­600 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¨ ovi observations to check ah our calibration at this frequency, to Greg Taylor for observing the ob ject 0237-23 at our request at the VLA in 1998 and 1999 in order to study known high frequency discrepancy of the source spectrum, and to Vladimir Amirkhanyan for kindly making his routine on simulating the RATAN­600 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 administration and employees of the observatory for their hospitality 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, a98­1932 and a99­1882. This research has made use of the NASA/IPAC Extragalactic database (NED), which is operated by the Jet Propulsion Laboratory, Caltech, under contract with the National Aeronautic and Space Administration.

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