28. S. A. Hawley, Astrophys. J., 224, 417 (1978). 29. A. G. W. Cameron, in: Essays in Nuclear Astrophysics (eds. S. A. Barnes, 0. D. Clayton, and D. M. Schramm), Cambridge University Press, Cambridge. 30. D. Kunth and F. Sevre, Preprint No. 114, inst. Astrophys. Paris (1985). 31. W. K. Stein and B. T. Soifer, Ann. Rev. Astron. Astrophys., 21, 177 (1983). 32. N. K. Andreasyan and E. s Khachikyan, Astrofizika, 15, 577 (1979). 33. N. K. Andreasyan, Astrofizika, 31, 74 (1984).
ON THE CONNECTION BETWEEN SEYFERT GALAXIES AND CLUSTERS A. R. Petrosyan To identify Seyfert galaxies that are members of clusters, the sample of known Seyfert galaxies (464 objects) is tested against the Zwicky, Abell, and southern clusters. On the basis of the criteria adopted in the paper, 67 Seyfert galaxies are selected as probable members of Zwicky clusters, 15 as members of Abell clusters, and 18 as members of southern clusters. Lists of these objects are given. i. Introduction A number of papers published in the second half of the seventies gave for the first time data on the connection between Seyfert galaxies and clusters; the results were contradictory. According to the data of [1-4], galaxies with Seyfert nuclei avoid rich clusters, whereas according to [5] the number of Seyfert galaxies in clusters corresponds to the general growth in the number of galaxies in clusters. Observations of recent years have identified many new galaxies with active nuclei in clusters [6-11], and in the cluster around 3C 295 three Seyfert objects have been found at once [12]. New statistical investigations based on more extensive samples of Seyfert galaxies and separately for samples of Zwicky [13] and Abell [14} clusters have shown that the Seyfert galaxies participate in the tendency to crowd into clusters. An analogous result in the special case of the Virgo cluster was obtained in [15]. In the present paper, we compare the sample of known Seyfert galaxies with clusters in the Zwicky and Abell catalogs and southern clusters, and as a result we select all cases of probably real membership of Seyfert galaxies in clusters. 2. Sample of Seyfert Galaxies and Clusters Our sample of Seyfert galaxies contains all objects in the catalog [16] classified as Sy 1 and Sy 2 (~390 galaxies) and about a further 75 new objects. The total size of the sample is 464 objects. For brevity, we designate the objects of this sample by SG. The sample of clusters of galaxies contains the clusters from the Zwicky [17] and Abell [18] catalogs and the catalog [19] for the southern sky. 3. Method of Identifying Seyfert Galaxies that are Members of Clusters a) Seyfert Galaxies in Zwicky Clusters. It is assumed that a Seyfert galaxy is a real member of a Zwicky cluster if it is within the contour line of the cluster given in [17] and the absolute magnitude of the different between its radial velocity and that of the cluster is less than or equal to 2000 km/sec (see, for example, [20, 21]). The radial velocities of the clusters are taken from [22-26]. b) Seyfert Galaxies in Abell Clusters. In this case we used the record of the sample Byurakan Astrophysical Observatory. Translated from Astrofizika, Vol. 27, No. 2, pp. 275-281, September-October, 1987. Original article submitted July i, 1986; accepted for publication July 20, 1987. 0571-7132/87/2702-0501512.50
9 1988 Plenum Publishing Corporation
501
TABLE i. Seyfert Clusters. Zwicky cluster
that are Members
Clust.]cl~st. type im/se~
SG
3 I
4
1
2 I
O007.7+1056 O024,0+1652 O107.5+3212 a
AC C AC
0228,0+2600 0233,0+0124 0240.6+0740 O303.0+41~5 b
O AC O AC
~449.3--0437 0510.04 0458A 0628.9+5232 0642.0+7334 0712.4+4523 0733.4+6102B 0739,8+4949 0745.5+4020 0801.3+3954 0810,1+5813
O O AC AC
Io
0837.0+2506 0909.7+1814B 0941.7+2430 1006.3+2320 1051.4+4041 1054.6+2017 1058.6+1049 1112.7+7259B 1123.9+3541 1138,7+5650A 1138.7+5650B 1138.7+5650C
1202.0--2028 1217.5+2915A 1257.1-}-2806~ 1339.9-~3030 1348.7+0249 1351.3+3333A 1352.9+3856 1354.0+1834 1510.0+0315 1517.3+2910 1555.1+4146
502
Galaxies
O AC C AC O AC AC O O AC AC
of Zwicky
I SG ~6 [ Morph.type R/Ref f Positof SGi~ ttype kin/see[ of SG
151
III Zw2 0024+1652~42 NGC 513 Mark.1 Mark.352 Mark. 993 Mark. 1040 NGC 1019 Mark. 595 NGC 1275 Mark. 1073 NGC 1685 X0459+034 UGC 3255 ~ark. 374 lark. 6 Mark.376 e Mark. 10 Mark. 79 Mark.382 Mark. 622 SBS0807+581 SBS0808+587 Mark. 1218 Mark. 704 Mark. 403 Mark.716 Mark, 1269 Mark. 634 Tol 1059+105 Mark. 728 NGC 3516 Mark.423 NGC 3982 Mark.40 Mark. 176 1213,6+51 Mark. 1469 Arak. 347 3990[ Mark. 766 6830 NGC 4922B 11080 Mark. 268 ~9201 Tel 1347 + 023 23401 NGC 5347 31401 NGC 5350 15020[Mark.463 11600l Mark.1395 24150 Mark, 849 10580 Mark. 1102 Mark. t103
6 I
7
8
0.354 26754 N* 120000 1.096 58401 48031SB0/SBa 0~ 0.776 4475/ SO 1,084 4910/ Sa 1.091 4910[ Sb 0.565 1 7251 SBb 0.416 8000 1 5220 pec. 0,352 5 6980 SBb 0.234 4200 0.771 2 4800 1,019 1 5689 SBb 0.864 2 1308C S0 1.624 1 559C S0/a 0.799 1.5 1183C SOpe~ 0.347 1 0.635 8710 Sb I 6560 SBS 0.138 I 102G0 SBe 1.039 I 6990 1.075 2 83701 0.420 2 0.703 8040 2 9400 SB 0.341 1 8960 0.766 1 72601 1.008 2 7190 0.511 6000 0.939 1 9420 0.481 0200 0.672 0430 S0/a 1,077 1 2600 SB0 0.70I 9610 0.606 | 975 S [ 0,556 2 6200 E-S0 0.680 I 7910 SO a pe~l 0.832 2 9330 ]I 1.674 1.5 1.5 93401 1.673 6600[ 0.141 2 3370 SBa 0:315 1 7226! 0.579 2 2 12000 SO,'a 0.241 1 97001 0,856 2 2340' SBa/b 0.334 0.827 2 23001SBb/e 15020! pee 0.170 2 12780] 0.438 1 1.019 1 2415O 2 10430 0.112 2 I0310i 0.152
l 2 2 2 1 2 1
9 2/3 3/3 1/3 2/3
2/3 3/3 1/3 2/3 , 1/3 2/3 3/3 3/'3 3/3 3/3 2/3 1/3 1/3 1t3 3/3 2/3 3/3 3/3 2/3
2/3 3/3 2/3 3/3 1/3 3/3 3/3 2/3 1/3 3/3 3!3 3/3 3/3 3,3 ] '3 2/3
2/3. 2/3. 3/'3,
1/3 2/3, 1/3:
2/3 2/3. 1/3, 1/3
TABLE
i (ctd.)
31 1556.2+2725 1600,4+ 1925f
C AC
1609.0 +82i2 1625.5+4006 1628. O-k2438 170 I. 4~2830 1701.9+3056 1722.8@3120 1916.8q-4855A 2231.2+3732 2256.8+2445 2259.6+0746 2316.5+0046 2320.0.4-0845 2335.5+2449
AC AC AC O AC AC
6
2712( E1556+274 1096( Mark. 291 Mark. 2c8 654-= NGC 6251 911( IIlZ~v 77 It32( Mark. 883 I090C Mark. 504 1323C 430g 608C 7200
O O AC AC
4860 8870 3940 8370
'7
270001
10631 ~Ba 10180 pee 6900 E 10220 11320 10900 SBa 10100 12850 SBb 5070 6622 SB
1021C Mark. 700
AC O O
]
Mark. 506 Arak. 539 N G C 319 Mark. 1127
J
71501 Sb 4835 t SBa 8730 t Sb 4394 Sb 7080
NGC 7469 Mark. 530
NGC 7672 Mark. 1133
0.116 0,561 0.520 0.643 0.837 0.178 0,723 0.982 0.638 1,179 1.298 1.401
0.635 O. 830 1.136 0,977
1/33/3 1/3. 3/3, 3/3. 2/3. 2/3-. 2/3-
Us. 3/3
3i3 313 2/3 3/3
3/3 2/3
Note. a) Cluster of galaxies in Pisces, b) cluster of galaxies in Perseus, c) on the connection of Mark. 376 with a cluster, see [3], d) the galaxy SBS 0807 + 581 is also a member of the open cluster Zw 0756.1 + 5616 with v r = 9630 km/sec. In this case, R/Ref f = 1.540, and the position of the SG is 3/3, e) cluster of galaxies in Coma (Coma I), f) cluster of galaxies in Hercules.
of S e y f e r t g a l a x i e s and A b e l l c l u s t e r s on a c o m p u t e r m a g n e t i c disk. We a s s u m e that a S e y f e r t g a l a x y is a real m e m b e r of a c l u s t e r if its a n g u l a r p r o j e c t i o n d i s t a n c e from the c e n t e r of the c l u s t e r is less t h a n the A b e l l a n g u l a r radius of the c l u s t e r and the absolute v a l u e of the d i f f e r e n c e b e t w e e n its r a d i a l v e l o c i t y and t h a t of the c l u s t e r is ~2000 km/sec. To c a l c u l a t e the A b e l l r a d i u s H = 75 k m . s e c - l . M p c -I)
of the cluster, we u s e d the e x p r e s s i o n
T A B L E 2. S e y f e r t G a l a x i e s Clusters. m~ ~ =m ~u
Type BM
1 R S - Zclust"
that are M e m b e r s
SG
SG type
A419 426 634
H--ill ,
HI
1142
II--IiI:
1257 1455 1781 2142 215i 2197 2534 2597
III II III II 11I NI II--tlI IIl
C7 L9 F C7 F B
F Bb F LSa eD
(J~0406 NGC 1229 0.0183 NGC 1275 1 Mark.1073 0.0266 SBS 0807+581 SBS 0808+587 0.0373 Mark.728 1 Tel 1059+105 0.0339 Mark. 423 0,165 IGQ Corn 1 0,0762 Mark. 69 0.09041E1556+274 0.0365 [Mark. 298 0.0303tlii" Zw 77 0.191 /1E2304--2259 0.08521PKS 2322--12
of A b e l l
zSG -
CO
(for q0 = 0 and
.
Morph. type
R / R A.
of SG
9.035 SBb pee 0.960 0.0174[ pec 0.134 0.02331 SBb 0,528 0.0279 ] 0.341 0.0268 t 0.534 0.0348 [ S0/a 0.606 0.0340 I 0.456 0.0320 ] pec 0.791 0.165 0.974 0,076 SO? 0.979 0,190 0.090 0.0339 pee 0.126 !0,853 0.0341 D,276 0.193 0.013 0.082
503
TABLE 3. Seyferts that Belong to Southern Clusters ~7r Morph. L ~ SG Name of Cluster clust. SG eratype km/ser cluster No. in [19 ] ture km/sec
I
Formax I
S 0321--374
0415--557 D o r a d o a 0428--540 I Hor. r e g i o n 0944--310 1027--353 A n t l i a 1334--337 Gr, IC 4296
1440 930 11520 54O 2599 3660
r
1347--305 l e l u s t . [ C 4329 1843--634 Antlia 2004--485 2159--322 Clemola 34 2209--469 Gr. NGC 7213 2254--367 Grus
2355--616 Gr. NGC 6300
RA
=
4320 4320 2765 2400 1900 1580
28770 1410
NGC 1365 NGC 1386 NGC 1566 F 303 A 0945--30 NGC 3281 MCG-6--30--15 NGC 5135 IC 4329A F 51 NGC 6890 NGC 7172 NGC 7213 NGC 7496 NGC 7582 NGC 7590 PKS 2356--61 NGC 6300
o Zp G
1800 SBb 600 Sa 1230 SXbe 1400 E 2400 3300 Sb? 2310 S? ~157 SBab 4651 S0/'a 4290 2409 Sb 2400 Sab pee 1740 Sa 1500 SBb 1427 SBab pe~ 1500 Sbe? 28800 1120 SBb
[311
[311 [321
[331 I
[321 [341 [321
[321 [351 [321
[321 [321
1321 [31] [361
0 . 0 2 8 7 " z - 1 ( 1 + z)~(1 + z/2) -1 arc degrees,
(i)
where for the cluster red shift (z) we have used its exactly measured value taken from ~L7, 28], or, when such is absent, the mean value of the red shift corresponding to the distance class of the cluster. c) Seyfert Galaxies in Southern Clusters. For the southern clusters contained in the catalog [19] definite sizes and red shifts are not given for the overwhelming majority of them; therefore in identifying Seyfert galaxies as members of southern clusters we used individual reports of real membership of a Seyfert galaxy in a cluster.
4. Results Table 1 gives data on the SG members of Zwicky clusters and on the clusters themselves. The table contains in its successive columns the designation of the cluster, the cluster type (O for open, AC for average compactness, and C for compact); its heliocentric radial velocity; the designation of the SG; the type of the SG and its heliocentric radial velocity; the morphological type of the SG; the ratio of the distance of the SG from the center of the cluster (R) to the effective radius of the cluster (Ref f according to [17]); the position of the SG with respect to the contour lines of the clusters, where 3/3 means that the SG is outside 2/3 of the radius of the circle whose center is the concentration of galaxies nearest the SG, and the radius is the distance from this concentration to the corresponding section of the contour line of the cluster. The simple 1/3 means that the SG is situated within 1/3 of the radius of the circle of concentration of galaxies in the cluster, and 2/3 means that the SG occupies an intermediate position. In Table 2 we give data on Seyfert galaxies that are members of Abell clusters and on the clusters themselves. The successive columns of the table contain the number of the cluster in [18]; the richness class; the cluster type according to Bautz and Morgan [29]; the revised (RS) cluster type according to [30]; the cluster red shift; the designation of the SG; the type and heliocentric red shift of the SG; the morphological type of the SG; the distance (in projection) of each SG from the center of the cluster, expressed in fractions of the Abell radius. Table 3 gives the list of Seyfert galaxies that are members of southern clusters. It contains the cluster number in accordance with [19]; the designation of the cluster; its heliocentric radial velocity; the designation, type, and heliocentric radial velocity
504
of the SG; the morphological type of the SG; and references to the literature that establishes the SG as a member of the cluster. LITERATURE CITED I. 2. 3. 4. 5. 6. 7. 8. 9. i0. Ii. 12. 13. 14. 15. 16. 17.
18. 19. 20. 21. 22. 23. 24. 25. 26. 27. 28. 29. 30. 31. 32. 33. 34. 35. 36.
S. Van den Bergh, Astrophys. J., 198, L1 (1975). B. V. Komberg, Preprint No. 274 [in Russian], IKI (1976). T. F. Adams, Astrophys. J. Suppl. Ser., 33, 19 (1977). G. R. Gisler, Mon. Not. R. Astron. Soc., 183 , 633 (1978). K.-N. Schmidt, in: The Large-Scale Structure of the Universe, IAU Symposium No. 79, Tollin, 1977 (eds. M. S. Longair and J. Einasto), Reidel, Dordrecht (1978), p. i01. G. O. Abell, T. S. Eastmond, and D. C. Jenner, Astrophys. J., 221, L1 (1978). A. S. Wilson and M. V. Penston, Astrophys. J., 232. 389 (1979). M. M. Phillips and J. A. Frogel, Astrophys J., 23___55,761 (1980). P. Veron, P. O. Linblad, E. J. Zuiderwijk, M. P. Veron, and G. Adam, Astron. Astrophys., 87, 245 (1980). M. M. Phillips and D. F. Malin, Mon. Not. R. Astron. Soc., !99, 905 (1982). J. P. Huchra, W. F. Wyatt, and M. Davis, Astron. J., 87, 1628 (1982). A. Dressler and J. E. Gunn, Astrophys. J., 270, 7 (1983). A. R. Petrosyan, Astrofizika, i_88, 548 (1982). M. A. Arakelyan and V. Yu. Terebizh, Pis'ma Astron. Zh., 8, 139 (1982). J. Stauffer, P h . D . Dissertation, Univ. California, Berkeley (1981). M. P. Veron-Cetty and P. Veron, A Catalog of Quasars and Active Nuclei, ESO Sci Rep. No. 1 (1984). F. Zwicky, E. Herzog, P. Wild, M. Karpowicz, and C. T. Kowal, Catalog of Galaxies and Clusters of Galaxies, Vols. 1-6, California Institute of Technology, Pasadena (19611968) (CGCG). G. O. Abell, Astrophys. J. Suppl. Ser., 35, 211 (1958). A. Duus and B. Newell, Astrophys. J. Suppl. Ser., 35, 209 (1977). G. O. Abell, in: The Large-Scale Structure of the Universe, IAU Symposium No. 79, Tollin, ifi77 (eds. M. S. Longair and J. Einasto), Reidel, Dordrecht (1978), p. 253. T. C. Beers, M. J. Geller, J. P. Huchra, D. W. Latham, and R. J. Davis, Astrophys. J., 283, 33 (1983). A. Dressler and J. E. Gunn, Astrophys. J., 263, 533 (1982). G. C. Baiesi-Pillastrini, G. G. C. Palumbo, and G. Vettolani, Astron. Astrophys. Suppl. Ser., 56, 363 (1984). T. W. Noonan, Astrophys. J. Suppl. Ser., 45, 613 (1981). M. Turatto and A. R. Petrosyan, Astron. Tsirk., No. 1371, 1 (1985). A. R. Petrosian and M. Turatto, Astron. Astrophys. Suppl. Ser., 65, 349 (1985). T. S. Fetisova, Astron. Zh., 58, 1137 (1981). C. L. Sarazin, H. J. Rood, and M. F. Struble, Astron. Astrophys., 108, L7 (1982). L. P. Bautz and W. W. Morgan, Astrophys. J., 162, L149 (1970). M. F. Struble and H. J. Rood, Astron. J., 87, 7 (1982). N. U. Mayall and A. de Vaucouleurs, Astron. J., 67, 363 (1962). A. Sandage, Astrophys. J., 202, 563 (1975). A. P. Fairall, Mort. Not. R. Astron. Soc., 196, 417 (1981). A. Sandage, Astron. J., 83, 904 (1978). V. C. Rubin, Astrophys. J., 191, 6~5 (1974). G. de Vaucouleurs, in: Stars and Stellar Systems, Vol. 9 (1975), p. 557.
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