The Astronomical Journal

1985AJ 90 . . 9270 a) 927 Astron.J.90 (6),June1985 0004-6256/85/060927-27$00.90 © 1985Am.Astron. Soc.927 versities, Inc.,undercontractwiththe National ScienceFoundation. jets notavailableinstraightjets.Inprinciple,thestudyof NationalRadioAstronomyObservatory isoperatedbyAssociatedUni- Using theNRAO300-ft.telescope, 1478Abellclusterswere by O’DeaandOwen(1985b,hereafterreferredtoaspaper III). servations oftheprototypicalNATNGC1265arepresented radio jetsarediscussedbyO’Dea(1984).Multifrequencyob- referred toaspaperII).Constraintsonthepropertiesofbent clusters arediscussedbyO’DeaandOwen(1985a,hereafter cal, aswelldetailed,studiesoftheirproperties.Theglobal that arepresentativesamplecanbeconstructedforstatisti- high-sensitivity mapsofalargeenoughnumberNATsso tion. ture ofNATsisstronglyaffectedbyprojectioneffects(Reyn- and statisticalpropertiesofasample51NATsinAbell olds 1980),aswellbytheavailablesensitivityandresolu- environment inthegalaxyandintraclustermedium. tions withintheradiojets,aswellimmediate However, theinterpretationofobservationsstruc- NATs canimproveourunderstandingofthephysicalcondi- NATs providesimportantconstraintsonthephysicsof Pacholczyk, andScott1981).Thebendingoftheradiojetsin and Blandford1979;JonesOwenChristiansen, Perola 1973;PacholczykandScott1976;Begelman,Rees, ejected byamovinggalaxywiththeintraclustermedium (e.g., Mileyetal.1972;Wellington1973;Jaffeand the interactionofbeamsorcloudsradioluminousplasma dram 1968;HillandLongair1971;RudnickOwen tion istheclassofnarrow-angle-tailsources(RyleandWin- Ekers etal.1981).Themostextremeexampleofthisinterac- ture arepreferentiallyfoundinclustersofgalaxies(e.g., of thesesources(e.g.,DeYoung1976;Burns1979;Miley ter mediummaydeterminemanyoftheobservedproperties 1976). TheNATmorphologyisattributedpredominantlyto 1980). Radiosourceswithbentorotherwisedistortedstruc- THE ASTRONOMICALJOURNAL The detailsofthesourceselection aregiveninpaperII. The purposeofthispaperistoprovidehigh-resolution, The interactionofclusterradiosourceswiththeintraclus- © American Astronomical Society • Provided by the NASA Astrophysics Data System -1 II. OBSERVATIONSANDDATAREDUCTION interesting featuresofthedifferentsubgroupssourcesaresummarized. on thepropertiesofindividualradiosourcesaremade.Finally,generalcharacteristicsand are presented.Opticalfindingchartsfor25previouslyunidentifiedsourcesgiven.Briefcomments observations increasethenumberofNATsforwhichtherearehigh-sensitivity(root-mean-squarenoise seven sourceswithcomplexmorphology.Twin-jetstructureisfoundin~75%oftheNATs.These include observationsof41narrow-angle-tail(NAT)sources,ninewide-angle-tail(WAT)sourcesand VLA observationsof57radiosourcesinthedirectionsclustersgalaxiesarepresented.Thedata —0.1 mJybeam),high-resolution(—T')mapsbyaboutafactorof10.Contourplotsthesources VLA OBSERVATIONSOF57SOURCESINCLUSTERSGALAXIES I. INTRODUCTION a) National RadioAstronomyObservatory,Charlottesville,Virginia22903 National RadioAstronomyObservatory,Socorro,NewMexico87801 Received 20September1984;revised10January1985 Christopher P.O’Dea Frazer N.Owen VOLUME 90,NUMBER6 ABSTRACT -1 -1 -1 on thePSSEprintstoanaccuracy of—1"usingtheNRAO sources properly. coverage, whichmakesitmore difficult toremoveconfusing noise inthesnapshotmapsisdue mainlytothepoorer(«,u) beam forthe1-hrobservations and—1mJybeamfor the snapshots(—10minobservations). Themuchlarger final noiselevelinthemapswastypically—0.15mJy- Abell clustercenter(Owenetal.1982).Atotalof485radio searched forradioemissionwithfluxdensities>0.1Jyat1.4 all mapswherethesourcewaslargerthan—2'insize.The rection forattenuationbytheprimarybeamwasappliedto The single-dishsurveyhasbeenfollowedbyVLAsnapshot sources inthedirectionsof442Abellclusterswerefound. GHz locatedwithin0.5correctedAbellclusterradiiofan relatively large-scalestructurewithhighresolution.Acor- The sourcenameisgivenincolumn1.Abellcluster has resultedinthediscoveryofmanytailedsources.Poten- observations ofthedetectedsources(Owenetal.1984)and The VLAconfigurationisgivenincolumn4.observing tions takenfromtheAbellclustersurvey(Owenetal.1984). Zwicky cluster(seeetal.1961).Thedateoftheob- number (Abell1958)isgivenincolumn2.Zwdenotesa marily intheAandBconfigurationsofVLAat20cm clusters (Owenetal.1984).Thesourceswereobservedpri- and fromtheVLAsnapshotsurveyofradiosourcesinAbell tial orknownNATsourceswerechosenfromtheliterature age considerablyandpermittedamaptobemadeofthe rations. Thiswasdesirablesinceitimprovedthe(w,u)cover- kiloparsecs/arcsecond isgivenincolumn8.Thedistances captions toFig.1andinthetext.Thelinear/angularscale given incolumn7.Theangularresolutionsarethe frequency andbandwidthinmegahertzaregivencolumns servations isgivenincolumn3.Anasteriskmarksobserva- (1977) wasused. (Thompson etal.1980).Theflux-densityscaleofBaars to addtogetherdatasetsobtainedindifferentVLAconfigu- were obtainedfromtheredshiftsinTableIII,assuminga as describedbyO’Dea(1984).Inmostcases,itwaspossible tion parameterofq=0.1. 5 and6,respectively.Theintegrationtime(inminutes)is Hubble constantof=75kmsMpcandadecelera- 0 The positionsoftheopticalidentifications weremeasured The parametersoftheobservationsaregiveninTableI. The datawereedited,calibrated,mapped,andCLEANed JUNE 1985 1985AJ 90 . . 9270 928 C.P.O’DEAANDF.N.OWEN:RADIOSOURCESINCLUSTERSOFGALAXIES © American Astronomical Society • Provided by the NASA Astrophysics Data System 1330+507 1758 1257+282 1256+282 1656 1250-150 1631 1244+699 1614 1132+492 1314 1108+411 1190 1055+570 1132 0907-091 0754 0905-098 0754 0704+351 0568 0658+330 0567 0457+054 0526 0647+693 0562 0431-134 0496 0335+096 Zw 0327+246 0439 0309+411 0426 0304-123 0415 0258+356 0407 0256+132 0401 0154+319 0278 0123-016 0194 0053-015 0119 0053-016 0119 0039-097 0085 0039-095 0085 0039+211 0084 Source Cluster Table I.Theparametersoftheobservations. 09-25-82 03-19-82 03-19-82 06- 14-82 12-26-81* 05- 08-81* 08-06-82 03-25-82 08-06-82 09-25-82* 03-19-82 08-26-82 08-26-82 09-25-82* 05-28-82 12-26-81* 03-19-82 05-08-81* 08-26-82 05-08-81* 12-26-81* 09-25-82* 01-23-82 09-20-80* 01-23-82 03-19-82 01-23-82 01-23-82 03-19-82 05-28-82 03-19-82 01-23-82 06- 2 5-82 12-26-81* 05- 0 8-81* 06- 2 5-82 12-26-81* 01-23-82 05- 0 8-81* 05-30-82 01-23-82 08-26-82 08-26-82 12-26-81* 08-26-82 12-26-81* 08-26-82 12-26-81* 12-26-81* 05-08-81* 03-19-82 05-08-81* 03-19-82 " 4 Array (MHz) A C B A C B A C Frequency 1452 1452 1452 1446 1452 1413 1452 1452 1452 1452 1452 1452 1452 1452 1452 1452 1452 1452 1413 4885 1452 1452 4885 1413 1465 1452 1452 1452 1452 1452 1452 1452 1452 1452 1413 1452 1452 1452 4885 4885 1413 1411 1452 1452 1452 1452 1452 1452 1452 1413 1452 1413 1452 50 25 25 25 12.5 25 25 25 25 25 25 25 25 25 25 25 25 25 25 25 25 Bandwidth TimeScale 25 25 25 (MHz) (Min)(kpc/”) 50 25 25 25 25 25 25 25 25 25 25 25 25 25 25 50 50 12.5 25 25 25 25 25 25 25 25 25 25 10 50 50 50 10 10 50 50 50 10 50 10 10 20 10 50 20 10 10 10 50 50 10 10 50 50 10 10 50 50 50 10 10 50 10 10 50 50 10 50 50 50 10 50 10 50 10 50 10 10 50 10 50 0.46 6.1 1.1 0.67 3.3 1.5 2.8 1.0 1.0 1.6 2.6 2.2 0.62 0.70 1.1 0.35 2.2 0.93 1.8 1.5 1.8 0.36 0.86 0.86 1.0 1.0 2.1 928 1985AJ 90 . . 9270 maps isgivenincolumn3forthose sourceswhereareliable 2. Thefractionofthetotalflux density observedintheVLA values anddividesbyanormalized beam)isgivenincolumn tained usingtheAIPStaskimean, whichsumsthepixel designated byB.Theintegrated fluxdensity,injansky,(ob- and theeasternmostsource(i.e., higherrightascension)is most source(i.e.,lowerrightascension) isdesignatedbyA the IAUcoordinatedesignationissame,western- 4.9-GHz mapsaregiveninTableII.Thesourcenameis pictures arepresentedbyO’Dea(1984). the structurenotseenincontourplots.AdditionalB/W radiophotographs ofselectedsourcesareshowninFig.2 tour levelsaregiveninthefigurecaptions.Blackandwhite to halfmaximum(FWHM)andpositionanglethecon- cations areshownascrosses.TheCLEANbeamfullwidth are presentedinFig.1.Thepositionsoftheopticalidentifi- Mann measuringmachine.Contourplotsofallthesources given incolumn1.Wheretwosourcesarecloseenoughthat [Plates 74and75].Theseradiophotographsrevealdetailsof 929 C.P.O’DEAANDF.N.OWEN:RADIOSOURCESINCLUSTERSOFGALAXIES The sourceparametersmeasuredontheVLA1.4-and © American Astronomical Society • Provided by the NASA Astrophysics Data System 2322+143 2316+184 1918+439 1850+702 1753+580 1707+787 1706+787 1706+786 1705+786 1712+638 1709+397 1658+326 1624+406 1615+351 1621+380 1619+428 1556+274 1519+488 1615+425 1339+266 Observations takenfromtheVLAsnapshotsurveyofAbellclustersby Owen etal.(1984). Source Cluster 2593 2572 2319 2311 2256 2289 2255 Zw 2250 2142 2241 2064 2197 Zw 1775 2183 2172 03-19-82 A 08-07-82 05-30-82 01-23-82 C 05-08-81* 08-07-82 08-07-82 08-06-82 08-06- 06- 14- 03-19- 05-01-82 03-19-82 09-25- 06-14- 08-06-82 03-19- 04- 05- 08-06- 05-10- 03- 19- 05- 08- 01-23- 08-06- 03-19- 05- 10- 01-23- 03-19- ■82 •82 ■82 ■82 ■82 82 82 82 82 82 81* 82 82 82* 82 82 82 Table I.(continued) Array (MHz) 2in Frequency the GaussianCLEANbeam; and foraresolvedcylinder the twin-jetNATs.For an unresolvedcylinder, verse profile(orslice)acrossthejet,isgivenincolumn6for The averagejetfluxdensity(injansky)forthetwin-jet and halfwidthtomaximum (HWHM),respectively,of Vj <GALAXIES 930 O'!o 0039+211 A0084 1452 MHz 0039-095A A0085 1452 MHz LO O'!00

V ÿ-

l 21°07 00" - i ^ o h m s b d 00 39 05 04 03 0039-097 A0085

O$°42'00

00h39m22s Right Ascension (1950.0)

Fig. 1 (a). Total-intensity contour maps. The crosses mark the positions of the optical objects in the field. The positions of the optical objects are given in Table III. The FWHM of the CLEAN beam is shown as a shaded ellipse. Negative contours are dashed. Starting at the top left and going clockwise, the contour levels in multiples of 1 mJy beam -1 and the FWHM and position angle of the CLEAN beam are as follows: 0039 + 211: -0.3, 0.3, 1, 2, 5, 9, 16, (1.17" X 1.13" @13.9°); 0039 - 095A: -0.5, 0.5, 1, 2.5, (1.6"Xl.2"@ - 1.6°); 0039-097: -0.6, 0.6, 1, 2, 4, (5.3" X4.2" @0°); 0039 — 095B: -0.5, 0.5, 1, 2, 4, 7, 11, (1.6" X 1.2" @ - 1.6°).

particles and magnetic fields in the radio jets assuming equal denotes a galaxy whose brightness is comparable to that of energies in relativisitic protons and electrons, a filling factor the dominant galaxy, and rank 3 denotes a galaxy which is of unity, a spectral index oía = — 0.65, and lower and up- much fainter than the dominant galaxy. Notes on the identi- per frequency cutoffs of 100 MHz and 15 GHz, respectively fication are given in column 8. Finding charts for those (see for example Bums, Owens, and Rudnick 1979; Pacholc- sources previously unidentified or without published finding zyk 1970), is given in column 7. charts are given in Fig. 3 [Plates 76-80]. The coordinates of the optical identifications are given in Brief comments on the individual sources are given below. Table III. For completeness, the positions of the previously A84: 0039 -f 211 was first shown to be a twin-tail source identified sources are also given. The source name is given in by Rudnick and Owen (1976). It has also been mapped by column 1. The source redshift and a reference are given in Riley (1975) and Simon (1979). The jets appear to become column 2. The right ascension and declination (epoch diffuse very quickly and only bits and pieces of the tails are 1950.0) are given in columns 3 and 4, respectively. Where seen in the 1 "2 X1 " 1 -resolution map. appropriate, a reference for the position is given in column 5. A85:0039 — 095A and 0039 — 097 are two NAT sources A reference to a previously published finding chart is given located on roughly opposite sides of the central cD galaxy in column 6. The rank of the galaxy is given in column 7. The (0039 — 095B), which is also a radio source (Owen et al. nomenclature is that given by Rudnick and Owen (1976): 1984). 0039 — 095A is a single-tail source (at 1"6X 1"2 reso- rank 1 denotes the dominant galaxy in the cluster, rank 2 lution) reminiscent in appearance to IC 310 (Miley et al.

LO 0053 - 015 A0119 1452 MHz O'!00

Right Ascension (1950.0) Fig. 1(b). See Fig. 1(a). 0053 - 016: - 1, 1,2, 5, 9, 16, (5.54”X4.95" @ - 55.3“); 0053 - 015: - 2.5, 2.5, 5, 9, 15, 28, (6.6” X4.9" @ - 59“).

0123-016A A0194 1452 MHz

Fig. 1(c). See Fig 1(a). 0123 - 016A.B: - 1.5, 1.5,4, 8, 20,40 (10.7" X8.4" @ - 62“); 0123 - 016A: - 1, 1, 2, 4, 8,14, (5.8" X 5.5" @ - 53").

© American Astronomical Society • Provided by the NASA Astrophysics Data System r"o O'!CM 932 C. P. O’DEA AND F. N. OWEN: RADIO SOURCES IN CLUSTERS OF GALAXIES 932 O'!o 0154 + 319 Ä0278 4885 MHz 0256+132 A0401 1452 MHz

LO O'!00

o 0258 + 356 A0407 1413 MHz ‘-p 0256+132 A0401 1452 MHz o Q

02h58m46s 44s Right Ascension

Fig. 1(d). See Fig. 1(a). 0154+ 139: -0.3, 0.3, 1, 2, 4, 7, ^"X^O" @57.5°); (0256+ 132: -0.3, 0.3, 0.8, 1.5, 2.5, (1.3" Xl^" @ -32°); 0256+ 132: - 0.3, 0.3, 0.8, 1.5, 2.5, (1.3X 1.2" @32°); 0256 + 132; - 0.8, 0.8, 1.5, 3, 6, (7.1" X 5.7" @ - 85°); 0258 + 356: - 0.7,0.7, 2, 3, 5, (1.3" X 1.2" @26.5°).

1972; Gower 1983, private communication). 0039 — 097 is a A194: Low-resolution observations of 0123 —016A,B twin-tail source (at 5"4x4"2 resolution) whose tails merge (3C 40) have been discussed by Schilizzi, Lockhart, and Wall into a diffuse tail about 30" ( — 30 kpc) behind the nucleus. (1972); Schilizzi and McAdam (1975); and Andemach, A119:A119is another cluster with two twin-tail NATs, Waldthausen, and Wielebinski (1980). Both a tapered map 0053 — 016 and 0053 — 015. This cluster has been mapped (10"7X8"4) of both sources and a higher-resolution map by Schilizzi and McAdam (1975) and Andemach, Waldth- (5"8x5"5) of the NAT (0123 - 016A) are shown. The dis- ausen, and Wielebinski (1980), though only the observations torted double source (0123 — 016B) is associated with NGC by Owen, Bums, and White (1984) were of sufficient resolu- 547, the southeasternmost galaxy of the binary galaxy pair tion to show the NAT nature of the two sources. 0053 — 015 NGC 545-547 Andemach (1982). Note the four roughly 90° (shown at 6"6x4"9 resolution) is very asymmetric and ex- bends in the northern lobe of this source. The twin-tail hibits gaps in the jets and tails. Higher-resolution observa- source is associated with NGC 541, which is also an x-ray 41 -1 tions of the region near the core are needed in order to exa- source of luminosity Lx — 10 erg s (Forman and Jones mine the possibility that the structure in this source is due to 1982). Van Breugel etal. (1985) have suggested that the NAT alternating one-sided ejection (e.g., Rudnick 1982; Rudnick is interacting with Minkowski’s object. and Edgar 1984). In contrast, 0053 — 016 (shown at A278:0154 + 319 was previously mapped by Owen, Rud- 5"5 X4"9 resolution) is very symmetric. The wiggles in the nick, and Peterson (1977), who identified it with the domi- jets (due to precession of the central collimator of the jets?) nant galaxy in the center of the cluster. The source has also continue into the diffuse tails. These two sources have tails been mapped at low resolution by Fanti et al. (1983). It was which point in the same direction in the sky (SW), but at very reobserved because it appeared to be an example of an unre- different angles to the direction to the cluster center. solved twin-tail source. However, higher resolution observa-

© American Astronomical Society • Provided by the NASA Astrophysics Data System 1985AJ 90 . . 9270 -1 933 C.P.O’DEAANDF.N.OWEN:RADIOSOURCESINCLUSTERSOFGALAXIES jets) thaninNGC1265(Paper III). jet. Thelower-resolution20-cmmapofOwenetal.(1984) cleus. Thegeneralstructureis similar tothatseeninNGC here forthefirsttime)atabout 30"(45kpc)behindthenu- The twinjetsmergeintoalow-surface-brightness tail(seen (1975), RudnickandOwen(1977), HarrisandMiley(1978), map (T.1X5"7)andahigher-resolution(Y'.l)areshown. reobserved inordertoobtainabettermap.Bothtapered found twin-tailstructureinthissource.Thissourcewas reobserved here.0256+132hasbeenobservedbyHarris, Kapahi, andEkers(1980)BumsUlmer(1980),who 0255 +133iswellknownandhasbeenmappedbySlingo 0256+ 132(4C13.17B)arefoundinthiscluster. (1980), andHarris,Kapahi,Ekerssowasnot reveals thatthejetcontinuessouthforanadditional—1"5 beam .The4"4X4"resolution6-cmmapshownsuggestsa (1974b), McHardy(1978),Simon(1979),BumsandUlmer (160 kpc). one-sided jetwithaslightedgebrighteningattheendof tions (—2";3.6kpc)showednostructureabove—0.6mJy 1265; however,thetailismuch weaker(withrespecttothe m ö o (D Fig. 1(e).See1(a).0304-123AJB:3,8,20,50,125,300,500,(19.85"X16.14"@6.6°);123B:10,40,100,200,(1.6"U" @ -10.6°);0309+411:1,1,2,4,20,50,125,(3.1"X3.0"38°);0304-123A:-0.6,0.6,1.5,4,9,(1.75"X1.26"9.3°). A407:0258 +356(4C35.06A) has beenmappedbyRiley o A401: TwoNATs,0255+133(4C13.17A)and © American Astronomical Society • Provided by the NASA Astrophysics Data System - 1217'00" 1800 0304-123 A A0415 hm, 1452 MHz the cD,itwasreobservedwithVLA.The1"3X1-^-reso- possibility thatitmightsimplybeseeninprojectionagainst axy (SchneiderandGunn1982)inthecenterofcluster. that thesourcewasassociatedwithnine-nucleuscDgal- and Simon(1979).Thesepreviousobservationssuggested ciated. TheWATanda—5"double source(0304—123B) determine whetherthetwooptical imagesareindeedasso- through theinteractionofcDnuclei(Wirth,Smarr,and lution mapshowsthatthesourceiscomplex,featuring: However, becauseofitsapparentHTmorphologyandthe are shownataresolutionof 1"7X 1"3.Thetaperedmap Gallagher 1982). (at aposition=025844?08,<535°3832";Simon (260 kpc)andcurvesbacktowards thepositionofdouble. ( 19"8X16T1)revealsthatthetail oftheWATstretches~2!5 [see Fig.3(b)].Opticalspectroscopy isneededinorderto 1984) associatedwithonenucleus ofapossiblebinarysystem 1979); 0258 +356couldbeanexampleofajetbeing“torqued” A415: 0304—123AappearstobeaWAT(Owenetal. (3) andverydiffusestructurewithanoverall"Z"shape. (2) twinjets; ( 1)anunresolvedcorecoincidentwithoneofthecDnuclei 0304-123 BA04151452MHz 933 934 C. P. O’DEA AND F. N. OWEN: RADIO SOURCES IN CLUSTERS OF GALAXIES 934

0335+096 1452 MHz h)

Right Ascension (1950.0) Fig. 1(f). See Fig. 1(a). 0327 + 246A, B: - 0.3, 0.3, 1, 2, 3, 7, (1.2"); 0335 + 096: - 0.7, 0.7, 2, 5, 10, 17, 25, 50, (12.4" @58°); 0431 - 134: - 0.4, 0.4, 1,3,7, 13, 21, (5.0" X4.1" @ - 28.4°); 0335 + 096: - 0.3, 0.3, 1,3,7, 12, (1.2").

No identification for the double was found on the PSS, sug- motions of the two galaxies. It would be interesting to know gesting that it is a background source. whether the two galaxies share a common envelope, as is the A426 (Perseus): The Perseus cluster contains three defi- case in 3C 75 (Owen and White 1984). nite NAT sources NGC 1265 (e.g., Miley 1973; Owen, Zw 0335.1 + 0956: 0335 + 096 was shown to be a NAT Burns, and Rüdnick 1978; Paper III) IC 310 (Ryle and Win- by Owen et al. (1984). It is identified with a prominent mem- dram 1968), and CR15 (Miley et al 1972). Based on their ber of a medium distant Zwicky cluster (Zwicky, low-resolution observations at 610 MHz, Gisler and Miley Karpowicz, and Kowal 1965), which is also an x-ray source (1979) suggested that 0309 + 411 was a possible HT source. (Schwartz, Schwarz, and Tucker 1980). The 1 "2-resolution The A-array observations appear to have resolved out most map of the region near the core shows twin jets that are swept of the structure. A tapered map ( ~ 3 " ) shows only a north- back into a diffuse tail over a projected distance of —5" (4 eastern extension to the core in the direction of a blob at kpc). The tapered map(12"4x9"8) shows that the diffuse tail — 30" ( 11 kpc) from the core. bends by about 40° at 1Í 5 (60 kpc) behind the core and contin- A439: 0327 + 246A,B have been observed by Kapahi et ues south for at least another 1!5. al. (1973), Owen, Rudnick, and Peterson (1977), Menon A496: Observations of 0431 — 134 by Owen et al. (1984) (1980), and Harris etal. (1980a). The 1 "2-resolution observa- suggested that this source was a NAT. The 6-cm, 5"x4"l- tions presented here are the first to show that there are actu- resolution map reveals that 0431 — 134 is a twin-tail source. ally two twin-jet-tailed sources. The associated galaxies are There is a suggestion of curvature in the diffuse tails. separated by —15" ( — 30 kpc) and are located near the cen- A526: 0457 + 054 (discovered by Owen et al. 1984) is a ter of the cluster. Some of the details of the structure (includ- strange twin-jet source. The 4"4 X 4"3-resolution map shows ing the bending of the jets in the WAT) may be due to orbital that one jet fades suddenly after bending through about 70°;

© American Astronomical Society • Provided by the NASA Astrophysics Data System 1985AJ 90 . . 9270 W 935 C.P.O’DEAANDF.N.OWEN:RADIOSOURCESINCLUSTERSOFGALAXIES much shorterprojecteddistance. while theotherjetbreaksupintodiffuseemissionovera The sourceisassociatedwithoneofthemoredominant members ofA562.The57X3!'8-resolutionmapat6cm the core.Thegeneralmorphologyisintermediatebetween shows twotails,whichexitfromhotspotsoneithersideof angle (definedastheatcoresubtendedbyends NATs andWATs(seediscussioninPaperII).Theopening WATs notedbyValentijn(1979a). of thetails)is80°,whichfallsingapbetweenNATsand the moredominantgalaxiesin clusterandappearstobea and Harrisetal(1980a).Thesourceisassociatedwithoneof WAT source.The5"0x4"0-resolution mapshowstwinjets lobes. Notetheregularlyspaced knotsintheeastjet. which bendgraduallybeforemaking atransitiontodiffuse nick andOwen(1977),Harriset al.(1980a),andFantiet (1983). The1"2-resolution mapshownherereveals complex © American Astronomical Society • Provided by the NASA Astrophysics Data System A562:0647 +693wasfirstmappedbyOwen¿fa/.(1984). A567: 0658+330hasbeenmappedbyValentijn(1979b) A568:0704 +351hasbeenmapped byRiley(1975),Rud- 0754 +351:-0.4,0.4,1,2,7,(1.2");0647693:-0.3,0.3,1,3,7,13,(5.7"X3.8"@63.4°). Fig. 1(g).See(la),0457+-054:-0.5,0.5,1,2,4,(4.4"X4.3"@41.3°);0658+330:-1.5,3,5,12,30,(5.0"X4.0"@20.4°); 0647+693 A05624855MHz 0457+054 A05261413MHz 421 structure surprisinglydifferentfromthatseenintheearlier the variousregionsofradioemissionwithopticalgalax- low-resolution, low-sensitivitymaps.Theidentificationof The emissiontotheeastandsouthofbrightpoint ies isuncertain.Onepossibleinterpretationthefollowing. pears tobendawayfromtheWAT.Thismaybeaunique west isadistortedtwin-jetsourcewhosesoutheastjetap- source formpartofaWATsource.Theobjecttothenorth- both radioandx-raywavelengths.High-resolutionobserva- example ofphysicallyinteractingradiosources. 0704+351 A05681413MHz The observationsofOwenetal.(1984)suggestthatthereisat tions oftwotheNATsinthisclusterarepresentedhere. least oneotherNATinthecluster. The4"5x4:2-resolution bends byalmost90°at—2'(—130 kpc)fromthecore.Har- map of0905—098showsasingle trailofemissionthat sion (L~10ergs')coincident withthetailatposi- ship inthecluster.Theyfindthat thereisweakx-rayemis- radio observationsofthissource, andconfirmitsmember- ris, Costain,andDewdney(1984) presentoptical,x-ray,and x A754: A754hasbeenstudiedbyHarrisetal.(1980b)at 935 r"o O':CM 936 C. P. O’DEA AND F. N. OWEN: RADIO SOURCES IN CLUSTERS OF GALAXIES 936 O':o

LO CT:00

Fig. 1(h). See Fig. (la). 0907 - 091: - 0.6,0.6,2,4,7,20, (5.3" X4.5" © - 30°); 0905 - 098: - 0.7,0.7,2,4,15,50, (4.5" X4.2" @ - 40.6°); 1055 + 570B: - 0.4, 0.4, 1, 2, 3.5, (1.25" X 1.0" @ - 16.5°); 1055 + 570A: - 0.4, 0.4, 0.8, 1.2, 2, (1.25" X 1.0" © - 16.5°).

tion where it exits the optical galaxy. Their observations are very diffuse tails, which appear to curve through about 90°. consistent with 0905 — 098 being either a single jet or a A1314:1132 -h 492 (IC 711) is one of the two well-known tailed source. 0907 — 091 has been mapped at low resolution NATs in A1314. Both IC 711) and 1131 + 493 (IC 708) have by Mills, Hunstead, and Skellem (1978). The 5"3 X 4"5-reso- been mapped by Vallee and Wilson (1976) and Wilson and lution map shows twin-tail structure, though the two jets Vallee (1977). Possible explanations for the structure of IC differ in brightness by a factor of — 4, and the surface bright- 708 are discussed by Vallee, Wilson, and van der Laan ( 1979) ness of the southern jet falls below the 0.6 mly beam -1 level and Vallee, Bridle, and Wilson (1981). The 3"9X 3"5-resolu- on the map. The jets expand by more than an order of magni- tion map of the region near the core in IC 711 confirms the tude into diffuse tails. suggestion of twin-tail structure seen in the data of Vallee A1132:1055 -h 570A,B are two NATs (Owen et aL 1984) and Wilson (1976). There is a hint that the twin jets extend shown here at 1"2X 1”0 resolution. The 1055 + 570B is a continuously from the core to the diffuse tails. However, this twin-tail source with no visible compact core. 1055 + 570A structure is just at the noise level and is not seen in the con- appears to be a weak (—17 mly) twin-tailed source. tour plot. A1190: 1108 + 411 (4C 41.23) has been mapped by Rud- A1614: Observations of 1244 + 699 by Owen et al. (1984) nick and Owen (1977), Valentijn (1979b), and Harris et al. suggested that this source was a NAT. The source is shown (1980b). The 1 "2X TT -resolution map shows twin-tail struc- to be a twin-tail source by the 4"8 X 3"5-resolution map. The ture similar to that seen in 0431 — 134. The jets expand into jet-tail transition occurs at the position of the hotspots locat-

41°06'45" 1244+699 A1614 1452 MHz

69°5e'0Ö'-

O Ö 11h 08m54s 12h44m00s 1132+492 A1314 1452 MHz 49016f

14'

Fig. l(i). See Fig. 1(a). 1108 +-411: - 0.5,0.5,2,4, 8,14, (1.2" X 1.1" @ - 33°); 1244 + 699: -0.5,0.5,1,2,4,6,9, (4.8" X 3.5" @2.6°); 1250- 150: -0.5, 0.5, 1,2, (1.9" X 1.3" @ -21°); 1132 + 492: - 0.4, 0.4, 1, 3, 9, 25, (3.9" X 3.5" @16.4°).

ed at a projected distance of ~ 15" 050 kpc) on either side of tion of the two hot spots. It appears (at least in projection) the core. Note the sudden change in direction of the tails to that the beams are ejected at an angle of ~ 35° to the galaxy’s the east. direction of motion. Also shown is a slightly tapered map A1631:1250 — 150 has complex morphology (Owen et al. (3:3) of the small (~ 20", 9 kpc) bent double 1257 + 282 (5C 1984). The 1"9X T'3-resolution map shows very diffuse 4.85). This source is associated with NGC 4874, one of the structure, and a ridge of brightness which may be a jet. The two dominant galaxies in the Coma cluster (e.g., Willson location of the core is not obvious. The tapered map 1970; Jaffe and Perola 1974). ( 10"0 X 6"9) shows two tails of emission which (in projection) A1758: 1330-b 507 (shown to be a NAT by Owen et al. curve through almost 90°. This may be another example of a 1984) is located in the direction of the Distance Class 6 clus- NAT following a curved trajectory. Another possibility is ter A1758. If the source is at the distance of the cluster that the tail is influenced by buoyancy (e.g., Cowie and [z = 0.280; Sandage, Kristian, and Westphal 1976), it would McKee 1975; Gisler and Miley 1979; Harris 1982). be one of the most powerful NATs known (P^ ;s3x 1025 A1656 (Coma): 1256 + 282 (5C 4.81) is a NAT associated W Hz-1). The i:2x TT-resolution map shows that the sin- with NGC 4869). The source has been mapped by Willson gle-tail structure near the core appears to split into two tails (1970), Jaffe and Perola (1974), Jaffe, Perola, and Valentijn at ~ 10" ( — 60 kpc) from the core. The blob of emission (1976), and Owen, Rudnick, and Peterson (1977). Roland —10" south of the core appears to be associated with an- (1982) has estimated various physical parameters for this other galaxy. source. The 1" 1-resolution map presented here is the first to A1775: The radio source in the center of A1775 has been show the twin-tail structure. The initially straight jets are mapped by Slingo (1974a, b), Owen, Rudnick, and Peterson bent and make a sudden transition to diffuse tails at the posi- (1977), Miley and Harris (1977), Simon (1979), and Harris,

1250-150 A1631 1446 MHz 1257+282 A1656 1452 MHz

1256+282 A1656 1452 MHz

12h56m58s 56s Right Ascension (1950.0)

Fig. l(j). See Fig. 1(a). 1250 - 150: - 1,1,3,5,10,15, (10.0" X 6.9" @7.2°); 1257 + 282: - 0.6,0.6,2,5,10,17, (3.32" X3.26" @ - 50.4°); 1330 + 507: — 0.3,0.3, 0. 8, 1.6,4, (1.2" X 1.1" @ - 29° 1256+■ 282: - 0.3,0.3, 0.7, 1.3, 1.9, (1.14" X 1.07" @-IT).

Kapahi, and Ekers (1980). The 1"3-resolution maps of sources are shown here at 1 "1X 1 "0 resolution. 1519 + 488B 1339 -f 266 are the first to show clearly that there are actual- is a —10" (22 kpc) bent double similar to 1257 + 282 asso- ly two separate sources. Each radio source is associated with ciated with the dominant galaxy in A2064. The structure of one of the bright galaxies in the center of the cluster. In 1519 + 488 A is complex, exhibiting an “hour glass”-shaped addition to the previously known NAT ( 1339 + 266B), there head. This source could be either a WAT or a NAT in which is a small ( — 10"; 14 kpc) bent double (1339 -h 266A) similar ejection occurs nearly along the direction of motion of the to 1257 + 282. The highest-resolution map (—0.4" at 6 cm) galaxy. This might produce a leading blob similar to that shows only three knots in the front of the NAT. (The WAT is seen in 2247 + 11 (Hardee, Eilek, and Owen 1980) and completely resolved by these observations). If the suggestion 1615 + 351 and would result in the optical ID being dis- of double structure in the first knot is real, then the jets are placed from the front of the source. Higher-resolution obser- swept back with a projected radius of curvature of—0.8 kpc. vations are needed in order to test these hypotheses. Chincarini et al (1971) suggested that the two galaxies A2142: Previous low-resolution (>23") observations of formed a bound system with a radial-velocity difference of 1556 + 274 suggested that this source was a NAT (Harris et 1650 km s~\ However, both Miley and Harris (1977) and al. 1977; Harris et al. 1980a). The 472x4"0-resolution map Hintzen (1979) have argued against that interpretation. The presented here shows only a single trail of emission, consis- observations presented here are consistent with a scenario in tent with the earlier maps. which the eastern galaxy (the NAT) is moving rapidly Zw 1615.8 + 3505: The NAT 1615 + 351 (4C 35.40) has through the ICM, while the western galaxy (the WAT) is been studied by Ekers et al. (1978), Bums (1979), Owen et al. nearly at rest with respect to the ICM. (1979), Fanti et al. (1981), and Bums and Gregory (1982). A2064: Observations of 1519 -b 488A,B by Owen et al The 1 "0-resolution map shows an edge-brightened blob to (1984) suggested that 1519-I-488A was a NAT. Both the east (in front?) of the unresolved core. There is a hint of a

26°37'

o d 1339+266 B A1775 4885 MHz 1519+488B A 2064 1452 MHz

Right Ascension ( 1950.0 )

Fig. l(k). See Fig. 1(a). 1339 + 266A,B: - 0.3,0.3,0.8,1.5, 3, 7, H^l.S"); 1519 + 488A: - 0.4,0.4,0.8, 1.2, 2,4, (1.1" X 1.0" @ - 35.2°); 1519 + 488B: -0.4, 0.4, 1,2,4, 7,(1.1"X 1.0" @35.2°); 1519 +-488B: -0.4, 0.4, 1, 2, 4, 7, (1.1" X 1.0" @ - 35.2°); 1339 + 266B: - 0.3, 0.3, 0.4, 0.6, (0.38" X0.37" @52°). faint jet (—0.2 mJy beam-1; not seen in the contour map) blob is part of the source, it would increase the source length connecting the blob with the core. This structure might be to —256 kpc and would imply a projected curvature in the produced if the beams were ejected parallel and antiparallel tail of about 50°. to the direction of motion of the galaxy (as suggested for Zw 1611.6 + 3717: The NAT 1621 + 380 has been stud- 2247 + 11 by Hardee, Eilek, and Owen 1980). In this model, ied by Ekers et al. (1978). The 1 "4 X 1 "2-resolution map the beam ejected into the direction of motion would interact shows a rather sudden transition between the two collimated with the ICM in a manner more typical of double radio jets to the diffuse tail. Because of this, and its short projected sources and might form the observed edge-brightened lobe. length (—16 kpc), it seems likely that this source is seen at a A2172: Observations of 1615 + 425 by Owen etal (1984) small angle to its direction of motion. The two jets appear to suggested that the source was a NAT. The 1" 1X1 "0-resolu- be oriented parallel to the major axis of the optical galaxy tion map presented here shows twin (initially fairly straight) (see Ulrich 1978 for an optical picture). jets which expand and change direction in hot spots located A2197: 1624 + 406 has been mapped at 610 MHz (with a —10" (26 kpc) from the core. This structure is similar to that resolution of 53" X 81") by Gavazzi and Perola (1980), who observed in WATs (e.g., Owen and Rudnick 1976; Eilek et suggest the source is a NAT associated with NGC 6150. The al. 1984) leading to the classfication of this source as a WAT. 1452-MHz (3"7 resolution) map shows only a slight exten- A2183: 1619 + 428 was shown to be NAT by Owen et al. sion to the core in the direction of the single tail seen by (1984). The source is shown to be a twin-tail source by the Gavazzi and Perola. l"5x l"3-resolution map presented here. The tapered map A2241: Riley (1975) suggested that 1658 + 326 (4C (22"7 X13"4) reveals a detached low surface brightness blob 32.52E) was a tailed source. Low-resolution observations by about 25" (68 kpc) beyond the main body of the NAT. If this Bijleveld and Valentijn (1982) showed that the tail splits and

© American Astronomical Society • Provided by the NASA Astrophysics Data System r"o O'!CM 940 C. P. O’DEA AND F. N. OWEN: RADIO SOURCES IN CLUSTERS OF GALAXIES 940 O'!o 1556+274 A2142 1452 MHz 1615+425 A2172 1452 MHz

LO O'!00

Right Ascension (1950.0)

Fig. 1(1). See Fig. 1(a). 1556+-274; - 0.4, 0.4, 1,3,7,12, 18, (4.2" X4.0" @-79.5°); 1615 + 425: - 0.4, 0.4, 0.8, 1.2, 1.8, (1.1" X 1.0" @ - 38.2°); 1619 + 428: - 0.3, 0.3, 0.7, 1.2, 2.5, (1.5" X 1.3" @ - 54°); 1615 + 351: - 0.4, 0.4, 1, 2, 6, 15, (1.0").

bends, as in 1250— 150. The tapered map (20"9Xl4"4) and tail” morphology. The 4"4x 3"6-resolution map shows shown here is in agreement with Bijleveld and Valentijn. In twin jets bending back from the core, towards the diffuse tail. addition, the 2"2-resolution map reveals the following fea- The other twin-tail source, 1712 4-640 (4C 64.20.1), has tures: been studied by Slingo (1974b), Rudnick and Owen (1976), (1) a one-sided jet directed south from the 3.5-mJy core; Simon (1979), Owen et al. (1979), and Harris, Kapahi, and and Ekers (1980), and so was not reobserved. (2) the originally single tail splits into two tails at a project- A2256: A2256 has been studied in detail by Bridle and ed distance of — 30" (62 kpc) from the compact core. Fomalont (1976), and Bridle et al. (1979), who find five A2250: 1709 + 397 has been mapped by Rudnick and NATs along with several other complex sources and a dif- Owen (1976), Miley and Harris (1977), Simon (1979), Owen fuse radio halo. The tapered map (4"0X 3"6) of the center of et al. (1979), Harris et al. (1980a), and Harris, Kapahi, and the cluster shows four sources (including three NATs) also Ekers (1980). A single tail is seen in the l"8x 1 "4-resolution mapped at comparable resolution by Valentijn (1981). A map of the region of the core. The tapered map (6"7X6"5) close-up of the twin-tail source 1705 4-786 (source B of Bri- shows that the tail forks (as suggested by Miley and Harris) dle et al.) at this resolution is also shown. The three other at a distance of ~2!5 (195 kpc) from the core. sources are shown at higher resolution (2"1 X 1"1). A2255: 1712 + 638 is the lesser known of the two NATs 1706 4- 786 (A), also mapped by Rudnick and Owen (1976), in A2255. It has been mapped by Harris, Kapahi, and Ekers and 1706 4- 787 (C) are both single-tail sources. 1707 4- 787 (1980), who christened it “The Beaver” because of its “body (D) appears to be a bent double similar to 1257 4- 282.

1619+428 A2183 1452 MHz 1624+ 406 A2197 1452 MHz T— 1 h)

52'

40 36‘00'

51'

o 50' dir> a> 16h20m00s 50s

16h58m21s

Fig. l(m). See Fig. 1(a). 1619 + 428: - 0.5, 0.5, 2, 4, 6, 10, 15, 30, 50, (29.6" X 16.6" @67.7°); 1624 + 406: - 0.6, 0.6, 2, 5, 9, 15, (3.7"); 1658 + 326: - 0.5, 0.5, 1, 2, 3, (2.2"); 1621 + 380: - 0.4, 0.4, 1, 2.5, 5, 8, (1.4" X 1.2" @ - 71°).

A2289:1753 + 580 was shown to be a twin-tail source by den transition from well-collimated jets to a diffuse tail. This Owen et al (1984). The source is shown here at l?6x 1"3 source, as well as NGC 1265 and 1850 + 702, are the best resolution. The jets are strikingly asymmetric and differ in examples of the type of morpholgy expected from a galaxy brightness by a factor of —23, with a gap in the west jet, with a turbulent galactic wake. where the surface brightness falls below 0.3 mJy beam-1. A2593: Lower-resolution observations of 2322 + 143A,B A2311: 1850 + 702 is a twin-tail source (Owen et al. by Owen et al. (1984) suggested that these two sources might 1984), shown here at 2"4X 2"2 resolution. The two jets make be NATs. The 1 "2-resolution map shows a single tail or jet a sudden transition to a diffuse tail at —30" ( — 50 kpc) be- source (2322 + 143B), with wiggles in the tail. 2322 + 143A hind the core. appears to be a straight twin-jet source embedded in diffuse A2319: Observations of 1918 + 439 by Birkinshaw (1978) emission. The latter source might be a tailed source seen at a and Harris and Miley (1978) suggested that the source was a very small angle to its direction of motion (perhaps a more NAT. The tapered map (7"5 X 7"4) shows twin-tail structure, extreme version of 1621 + 380). It could be also a leaky reminiscent of the early maps of NGC 1265 (e.g., Miley beam (cf. B2 1321 + 31, Fanti et al. 1982; or NGC 1265, 1973). paper III). [The faint stripes in the diffuse emission on A2572: 2316+ 184 (OZ 127) was shown to be a twin-tail 2322 + 143A are probably due to an instability in CLEAN source by Owen et al. (1984). The lower-resolution 1.4-GHz (Cornwell 1983)]. map by Fanti et al. (1983) (their A2572-4) suggests that the tail does not extend much beyond what is seen in the IV. DISCUSSION 1 "4 X1 "3-resolution map shown here. However, the inte- The sources presented in this paper make up a diverse grated spectral index is rather steep ( 0.8 between 750 rogues’ gallery. It is clear from these observations that the and 1410 MHz; Hoglund 1967). The source exhibits a sud- NAT phenomenon encompasses a much larger variation in

© American Astronomical Society • Provided by the NASA Astrophysics Data System r"o O'!CM 942 C. P. O’DEA AND F. N. OWEN: RADIO SOURCES IN CLUSTERS OF GALAXIES 942 O'!o 1658+326 A2241 1452 MHz 1709+397 A2250 1452 MHz

LO O'!00

o ö mCD 1712+638 A2255 1452 MHz

Fig. l(n). See. Fig. 1(a). 1658 + 326: -2, 2, 4, 6, 10, 15, 20, 25, 30, 35, (20.9,/X 14.4" @64.2°); 1709 + 397: -0.5, 0.5, 2, 5, 15, 50, (6.7" X6.5" @14.1°); 1712 + 638: - 1.3, 1.3, 2.5, 3.5, 5, (4.4" X 3.6" @20°); 1709 + 397: - 0.4, 0.4, 1,3,7, 11, (1.8" X 1.4" @ -67°).

morphology than previously thought. The results are sum- tion into broad diffuse tails (e.g., NGC 1265, 1850 + 702, marized below for the various groups of objects. and 2316 + 184). In the other group, the jets do not change structure as radically, but expand much more gradually and a) Narrow-Angle-Tail Sources may eventually merge into a single tail, (e.g., 0039 + 211, Observations of 41 NATs are presented. Only ten of them 0647 + 693, 1055 + 570B, 1256 + 282, 1619 + 428, and are single-tail sources, i.e., 0039 — 095A, 0309 + 411, 1753 + 580). The possible significance of this is discussed in 0905-098, 1339 + 266B?, 1519 + 488A? 1556 + 274, paper II. 1624 + 406?, 1706 + 786, 1706 + 787, and 2322 + 143B. With the exception of NGC 1265, the jets in the twin-jet The observations presented here increase the percentage of sources are basically unresolved by these observations, with NATs with twin jets by a factor of 3 [from 25% (e.g., Simon typical upper limits to the jet radius of ~ 1-2 kpc. 1978; Valentijn 1979a) to 75%]. Since some of the single-tail Some of the NATs (e.g., 0039 + 211, 0431 — 134, NATs may be intrinsically one-sided single-jet sources in- 0907 - 091,1621 + 380,1712 + 638, and 2316 + 184) have stead of tail sources (e.g., 0905 — 098; Harris, Costain, and jets which are brightest right near the core and become dim- Dewdney 1984), it is likely that the actual percentage is even mer with increasing distance from the core. This is in con- higher. The nature of the single-tail sources is discussed strast with higher-luminosity jets which tend to have “gaps” further in paper II). in the jet emission right near the core (e.g., Perley etal 1980). The remaining twin-tail sources appear to fall into two If these gaps are greater than —2-3 kpc in size they would classes based on morphology (i.e., the nature of the jet/tail have been resolved by these observations and would have transition). In one group, the jets make a very sudden transi- been seen. NGC 1265 is the only clear example of a NAT

© American Astronomical Society • Provided by the NASA Astrophysics Data System 1985AJ 90 . . 9270 943 C.P.O’DEAANDF.N.OWEN:RADIOSOURCESINCLUSTERSOFGALAXIES through theICMandbuoyancy effects(e.g.,Cowieand McKee 1975;GislerandMiley 1979;BurnsHarris Possible explanationsforthis include curvedtrajectories tijn 1982),and1709-f397(seealsoMileyHarris1977)]. paper III),0335+096,0431-134,0905098, scale curvatureinthetails[i.e.,0314+416(Miley1973and particle accelerationto“turnon”thejetsclosercore. lower Machnumbersand/orbeamvelocities,whichallows this differencebetweenhigh-andlow-luminosityjetsexists. weak emissioninthegap(paperIII).Itisnotyetclearwhy with suchagap,andhigh-sensitivityobservationsshow One possibilityisthatthelower-luminositysourceshave 1982). 1970), 1619+428,1658326(seealsoBijleveldandValen- 1108 +411,1244699,1250-150,1256282(Willson Of these41NATs,thereare11sourcesthatexhibitlarge- © American Astronomical Society • Provided by the NASA Astrophysics Data System Observations arepresentedhere ofnineWATs,i.e., b) Wide-AngleTailSources A2256 Fig. 1(o).See1(a).ThecenterofAbell2256:-0.5,1,3,7,12,18,25,(4.0"X3.6")@60°). 0304 -123A,0327+246B,0658330,0704351, entirely withintheextentofopticalgalaxy. shaped, havenovisiblecompactcore,andmaybecontained and 1519+488B)havesmallradiosizes(<25kpc),are“V” axies (rank1or2).Threeofthem(1257+282,1339266a, 0154 +319and2322143A aresingleandtwin-jet is notobviouslyeitherWAT orNATweremapped. ter; rank1). galaxies (i.e.,verydominantinthecenterofclus- sources withcomplexdiffusestructureassociatedcD 1257 +282,1339266A,1519488A,1615426,and 1707 +787.Allareassociatedwithrelativelydominantgal- A fewsourceswithcomplexmorphology whosestructure 0039 -095B(A85)and0258+356(A407)areradio 2) “Jet”sources 1) cDgalaxies 1446 MHz 943 00 o CM LO r" o 944 C.P.O’DEAANDF.N.OWEN:RADIOSOURCESINCLUSTERSOFGALAXIES Fig. l(p).See1(a).1705+786:-0.5,1,1.5,2,3,(4.0"X3.6"@60°); 1706+787:-0.4,0.8,1.2,2,(2.1"X1.1"@71.6°);1707 © American Astronomical Society - 0.4,0.4,0Í6,0.8,1,1.5,(2.1"X1.1"@71.6°);1706+786:-0.4,0.4,1,2,4,7, 11,(2.1"X1.1"@71.6°). Declination ( 1950.0) 1705+786 A22561446MHz Right Ascension(1950.0) Provided bythe NASA Astrophysics Data System 1706+787 A22561446MHz 944 00 o CM LO r" o 945 C.P.O’DEAANDF.N.OWEN:RADIOSOURCESINCLUSTERSOFGALAXIES Fig. l(q).See1(a).1753+580:-0.4,0.8,1.5,2.5,5,(1.6"X1.3"@ -55.6°);1918+439:1,1,2,3,4,(7.5"X7.4"@4T);2316+184: -0.3,0.3, 1,4,8,(1.4"X1.3"@-38°);1850+702:0.4,0.8,1.5,4,(2.4" X2.2"@-37°).

© American Astronomical Society Declination (1950.0) Provided bythe NASA Astrophysics Data System 1918+439 A23191452MHz 945 00 o CM LO r" o 946 © American Astronomical Society • Provided by the NASA Astrophysics Data System Declination (1950.0) C. P.O’DEAANDF.N.OWEN:RADIOSOURCESINCLUSTERSOFGALAXIES Fig. l(r).See1(a).2322+143A,B:-0.5,1,2,4,7,(1.2"). 946 1985AJ 90 . . 9270 947 C.P.O’DEAANDF.N.OWEN:RADIOSOURCESINCLUSTERSOFGALAXIES © American Astronomical Society • Provided by the NASA Astrophysics Data System 0907-091 0704+351A 0658+330 0647+693 0905-098 0754+351B 0457+054 0431-134 1619+428 1257+282 1250-150 1244+699 1132+492 1055+570A 0335+096 0327+246B 0327+246A 0314+416 0309+411 0304-123B 0258+356 1615+425 1615+351 1556+274 1519+488B 1519+488A 1339+266B 1339+266A 1330+507 1256+280 1108+411 1055+570B 0304-123A 0256+132 0154+319 0123-016B 0123-016A 0053-016 0053-015 0039-097 0039-095B 0039-095A 0039+211 Source IntegratedFractionalCoreFluxJetMinimum Flux DensityContributionRadiusPressure b a a a >4.93 (Jy) (kpc)10”^-^dynescm"2 0.17 0.29 0.04 0.11 0.13 0.30 0.22 0.16 0.88 0.11 0.02 0.13 0.39 0.37 0.28 0.61 0.36 0.80 0.52 0.32 0.30 0.88 0.75 0.19 0.16 0.37 0.74 0.16 0.91 0.04 4.27 0.12 0.05 0.07 1.13 1.50 0.18 .08 .09 .06 .05 .20 C C C C C C 0.9 0.6 0.1 0.7 0.8 0.7 0.8 0.3 0.9 0.3 0.3 0.3 0.9 1.0 1.0 0.9 0.3 0.8 0.8 0.9 0.9C 1.0 0.9c 11 0.9 11 0.6 11 0.3 • Table II.Sourceparameters. 11 11 11 11 11 11 11 11 11 11 11 11 11 11 4 4 1 7 6 1 1 5 a <0.0006 <0.005 <0.007 <0.0007 <0.002 <0.002 <0.0004 a <0.0025 a <0.002 <0.065 0.0008 0.008 0.032 0.021 0.005 0.0063 0.034 0.0135 0.002 0.031 0.119 0.001 0.022 0.052 0.005 0.024 0.017 0.0032 0.0014 0.060 0.017 0.008 0.042 0.007 0.0156 0.0035 0.004 0.0074 0.012 0.294 0.0047 0.0067 0.034 0.006 a 016 009 006 024 123 026 025 018 024 023 021 021 226 • • • • • • • Twin JetNATParameters <0 <5 <1 <0 ~0 <2 <5 <1 <2 <0 <0 <1 <2 <1 0.6 0.3 2 5 947 1985AJ 90 . . 9270 948 C.P.O’DEAANDF.N.OWEN:RADIOSOURCESINCLUSTERSOFGALAXIES © American Astronomical Society • Provided by the NASA Astrophysics Data System 2322+143B 2322+143A 2316+184 1706+787 1706+786 4. JaffeandPerola(1974) 1918+439 1850+702 1753+580 1707+787 3. BijleveldandValentijn(1982) 2. Ekersetal.(1978) 1712+638 1621+380 1705+786 1709+397 1658+328 6. Millsetal.(1978) 5. Harrisetal.(1980b) 1. Bridleetal.(1972) c b 1624+406 0039-095A 003$f211 0039-097 0039-095B 0053-016 0053-015 0123-016A assuming thesamefractionalcontributionofbothsourcestototalfluxdensity. data fromPaperIII. flux densitymeasuredat4.9GHz. Source IntegratedFractionalCoreFluxJetMinimum Source RedshiftRightAscensionDeclinationRef.RankNotes a a Flux DensityContributionRadiusPressure 0.0556 28 0.0518 26 0.1017 25 0.0518 26 0.042 27 0.0386 29 0.0182 30 • • 0.15 0.08 0.19 0.01 0.04 0.18 0.78 0.29 0.14 0.16 0.06 0.24 0.27 0.04 (Jy) (kpc)10“HdynescnT^ 0.28 0.4 0.7 0.9 0.6 0.6 0.7 0.5 1.0 Table III.Theopticalidentifications. 00 3916.38 00 3903.09 00 3918.55 00 3918.44 00 5352.49 00 5352.08 00 5351.23 00 5352.41 00 5329.31 00 5328.36 01 2311.53 (1950.0) h mso. t References toTableII Table II.(continued) 10 11 11 11 11 2 9 3 10. Birkinshaw(1978) 11. Owenetal.(1982) 9. GavazziandPerola(1980) 8. MileyandHarris(1977) 7. WilsonandVallee(1977) <0.007 <0.010 <0.008 0.021 0.0016 0.033 0.006 0.015 0.013 0.0016 0.015 0.002 0.006 0.0035 0.0083 -09 3329.7 -09 4216.7 -09 3437.6 -01 3231.6 -01 3157.1 -01 3242.0 -01 3616.9 -01 3256.0 -01 3649.1 -01 3824.5 21 0743.0 Twin JetNATParameters 14,15 2 3 1 3 3 3 2 3 3 3 4 • ID ID 948 1985AJ 90 . . 9270 949 © American Astronomical Society • Provided by the NASA Astrophysics Data System C. P.O’DEAANDF.N.OWEN:RADIOSOURCESINCLUSTERSOFGALAXIES ab 0907-091 0905-098 0658+330 0704+351 0647+693 0457+054 0431-134 1055+570A 1055+570B 0335+096 0304-123A 0.08940» 1108+411 0327+246B 0327+246A 0258+356 0256+132 0309+411 0154+319 0123-016B 0.018530 0304-123B Source a a a a a 0.1391 36 0.1362 36® 0.0790 25 0.0727 25 0.0585 35 0.0534 34 0.0737 25 0.0737 32 0.0127 40®>t> 0.0541 25 0.0316 26 0.1063 25 0.110 25 0.0472 26® 0.035 33 0.1063 25 0.0183 26 0.0776 4 0.0896 26® Redshift • • • • • • • Right Ascension 04 3152.03 06 5852.97 04 5722.07 04 3151.42 03 3530.70 04 5723.89 03 2731.05 09 0659.96 09 0536.4 07 0422.74 07 0421.95 07 0424.34 06 4754.58 04 5720.77 03 2744.72 03 0429.38 02 5844.08 10 5522.14 03 0944.93 03 0429.80 02 5846.68 02 5845.38 02 5845.08 02 5843.92 11 0853.49 10 5531.04 03 0946.00 03 0945.75 02 5843,72 03 0944.72 03 0439.10 03 0440.33 03 0432.25 02 5843.30 02 5844.56 02 5630.0 01 5423.07 01 5421.51 01 5423.35 01 5422.08 01 5423.46 01 5422.45 01 2326.07 01 5421.75 01 2327.55 (1950.0) Table III.(continued) -09 1032.0 -09 4731 -13 2806.3 -13 2824.6 -12 1659.3 -12 1718.2 -12 1753.7 -12 1825.1 -12 1752.4 -01 3559.9 -01 3618.9 Declination Ref. 41 0643.1 57 0403.3 57 0343.5 35 0814.0 35 0823.9 35 0822.8 05 2536.5 05 2525.7 05 2444.7 09 5519.2 33 0146.8 69 2331.5 24 3736.0 24 3736.3 41 0842.6 41 0847.9 41 0847.5 35 3832.5 41 0854.6 35 3830.8 35 3838.8 35 3824.6 35 3824.6 35 3835.7 35 3841.5 35 3841.8 13 1517 32 0017.8 31 5941.2 31 5942.8 32 0009.5 32 0002.0 32 0024.3 32 0034.8 (1950.0) 1 1 1 1 4,5 2 3 1 1 1 1 3 3 3 3 3 3 2 Ref. RankNotes 18 17 4,16 6 1 3 1 3 3 3 2 3 3 3 2 2 3 2(1?) 3 1 3 3 2 3 3 3 2 2 1 2 2 No ID ID ID ID ID? ID? ID ID 949 1985AJ 90 . . 9270 950 C.P.O’DEAANDF.N.OWEN:RADIOSOURCESINCLUSTERSOFGALAXIES © American Astronomical Society • Provided by the NASA Astrophysics Data System 1244+699 0.157 1132+492 0.0324 1256+282 0.0224 1615+351 0.0295 1330+507 0.280 1257+282 0.0237 1615+425 0.1375 1556+274 0.0904 1519+488B 0.1074 1339+266B 0.0693 1339+266A 0.0752 1619+428 0.1394 1519+488A 0.1078 1250-150 0.053 1709+397 0.0621 1658+328 0.1024 1624+406 0.0303 1621+380 0.0310 1850+702 0.079 1706+787 0.0581 1706+786 0.0570 Source RedshlftRightAscensionDeclinationRef.RankNotes 1753+580 0.160 1707+787 0.0601 1705+786 0.0561 1712+638 0.0829 • • • • • • • • • • • • • • b b b 40»» 124355.46 37 113203.95 26* 125018.19 38 125658.3 26* 133050.92 38 125710.7 41 161953.57 25 161459.05 25 151916.96 39 1330.84 39 1329.49 20 161549.0 26 155609.9 25 151909.63 26* 162408.86 20 162116.9 40*» 184947.24 10 165818.75 40*> 175312.18 20 170916.69 22 171255.67 26* 170738.81 23 170621.02 23 170619.34 23 170551.70 12 4401.15 12 4357.87 12 5020.08 12 5015.84 12 5020.28 13 3051.14 16 1952.02 16 1953.13 16 1953.42 16 1459.60 16 1949.20 (1950.0) 17 5310.74 17 5312.35 17 5314.01 Vi mao»«• Table III.(continued) -15 0411.8 -15 0356.3 -15 0349.3 -15 0414.6 49 1356.58 69 5547.2 69 5600.9 69 5550.4 28 1052.33 28 1345.53 50 4709.5 48 5008.4 26 3731.63 50 4658.8 48 5023.8 26 3719.73 42 3415.2 35 073213 27 24549 42 5226.8 42 3413.9 78 4153.411 78 3955.611 63 50595 32 3936.710 40 3556.9 42 5201.5 42 5211.0 78 4222.711 78 4352.611 39 4507.91 42 5241.4 42 5217.9 38 021713 58 0533.7 70 1733.6 58 0528.5 58 0540.7 58 0536.5 24 3 23,15 3 15,20 2 3 19 2 19 3 20 2 22 3 20 3 23 3 23 3 23 3 21 2 10 3 3 2 3 2 3 3 ID 3 2 ID 3 3 3 3 ID 3 3 3 1 3 ID 3 3 1 3 2 2 ID 3 ID 3 3 3 950 1985AJ 90 . . 9270 951 C.P.O’DEAANDF.N.OWEN:RADIOSOURCESINCLUSTERSOFGALAXIES © American Astronomical Society a b c a 2322+143B 2322+143A 0.044026* 2316+184 0.039526* 1918+439 0.052926 Source 21. GavazzlandPerola(1980) 20. Ulrich(1978) Probable backgroundsource,noID. Cluster redshlftisestimated, Galaxy redshlftIsunknown;clusterisgiven, 22. HintzenandScott(1980) 12. Birkinshaw(1978) 11. Bridleetal.(1979) 10. BijleveldandValentijn(1982) 15. RudnlckandOwen(1976) 13. Ekersetal.(1978) 19. Willson(1970) 16. BurnsandUlmer(1980) 14. Riley(1975) 18. MelnlckandQuintana(1981a) 17. Valentijn(1979b) 5. Harris,Kapahi,andEkers(1980) 4. Hintzen,Scott,andTarenghi(1977) 3. Owen,Rudnlck,andPeterson(1977) 2. Schilizzi(1975) 8. ValleeandWilson(1976) 6. RudnlckandOwen(1977) 1. Simon(1979) 9. Harrisetal.(1980a) 7. Harrisetal.(1980b) 0.0455 36 Redshlft Right Ascension 23 2206.25 19 1845.3 23 2204.79 23 1609.56 23 2204.92 23 2203.26 23 2201.13 (1950.0) h ms References toTableIII Table III.(continued) Provided bythe NASA Astrophysics Data System 30. ChlncarlniandRood(1977) 27. Grandi(1983) 24. Webber(1974) 23. BridleandFomalont(1976) 31. ChincariniandRood(1971) 29. MelnickandQuintana(1981b) 28. Hoessel,Gunn,andThuan(1980) 26. Sarazin,Rood,andStruble(1982) 25. OwenandWhite(1984) 34. Harris,Costain,andDewdney(1984) 33. Schwartz,Schwarz,andTucker(1980) 32. Ulrich(1976) 41. Ciardulloetal.(1983) 40. Owenetal.(1982) 38. Roodetal.(1972) 37. Colemanetal.(1976) 35. FaberandDressier(1977) 39. Hintzen(1979) 36. Humason,Mayall,andSandage(1956) Declination 43 5703.7 14 2154.9 18 2458.2 14 2205.1 14 2203.9 14 2135.3 14 2156.8 (1950.0) Ref. 12 Ref. RankNotes ÏD ID 951 1985AJ 90 . . 9270 Harris, D.E.,Costain,C.H.,Strom,R. G.,Pineda,F.J.,Delvaille,J.P., Harris, D.E.(1982).InExtragalacticRadioSources,ProceedingsofIAU Hardee, P.E.,Eilek,J.A,andOwen,F.N.(1980).Astrophys.242,502. Gavazzi, G.,andPerola,G.C.(1980).Astron.Astrophys.84,228. Harris, D.E.,Costain,C.H.,andDewdney, P.E.(1984).Astrophys.J.280, Harris, D.E.,Bahcall,N.A.,andStrom, R.G.(1977).Astron.Astrophys. Grandi, S.A.(1983).Mon.Not.R.Astron.Soc.204,691. Gisler, G.R.,andMiley,K.(1979).Astron.Astrophys.76,109. Forman, W.,andJones,C.(1982).Annu.Rev.Astron.Astrophys.20,547. Fanti, C,R.,Feretti,L.,Gioia,I.M.,Giovannini,G.,Gregorini, Fanti, R.,Lari,C,Parma,P.,Bridle,A.H.,Ekers,R.D.,andFomalont,E. Fanti, R.,Lari,C.,Parma,P.,andEkers,R.D.(1981).Astron.Astrophys. Faber, S.M.,andDressier,A.(1977).Astron.J.82,187. Ekers, R.D.,Fanti,R.,Lari,C,andUlrich,M.-H.(1978).Astron.As- Ekers, R.D.,Fanti,R.,Lari,C,andParma,P.(1981).Astron.Astrophys. Eilek, J.A.,Bums,O.,O’Dea,C.P.,andOwen,F.N.(1984).Astrophys. De Young,D.S.(1976).Annu.Rev.Astron.Astrophys.14,447. Cornwell, T.J.(1983).Astron.Astrophys.121,281. Coleman, G.D.,Hintzen,P.,Scott,J.S.,andTarenghi,M.(1976).Nature Cowie, L.L.,andMcKee,C.F.(1975).Astron.Astrophys.43,337. Ciardullo, R.,Ford,H.,Bartko,F.,andHarms,R.(1983).Astrophys.J. Christiansen, W.A.,Pacholczyk,A.G.,andScott,J.S.(1981).Astrophys. Chincarini, G.,Rood,H.J.,Sastry,G.N.,andWelch,A.(1977).As- Chincarini, G.,Rood,H.J.,Sastry,G.N.,andWelch,A.(1971).As- Chincarini, G.,andRood,H.J.(1971).Astrophys.168,321. Bums, J.O.,andUlmer,M.P.(1980).Astron.85,773. Bums, J.O.,Owen,F.N.,andRudnickL.(1979).Astron.84,1683. Bums, J.O.,andGregory,S.A.(1982).Astron.87,1245. Bums, J.O.(1979).Ph.D.thesis,IndianaUniversity. Bridle, A.H.,Fomalont,E.B.,Miley,G.K.,andValentijn,(1979). Bridle, A.H.,andFomalont,E.B.(1967).Astron.Astrophys.52,107. Bridle, A.H.,Davis,M.M.,Fomalont,E.B.,andLequeux,J.(1972).As- Birkinshaw, M.(1978).Mon.Not.R.Astron.Soc.184,387. Bijleveld, W.,andValentijn,E.A.(1982).Astron.Astrophys.Ill,50. Begelman, M.C,Rees,J.,andBlandford,R.D.(1979).Nature279,770. Baars, J.W.M.,Genzel,R.,Pauliny-Toth,1.1.K.,andWitzel,A.(1977). Andernach, H.,Waldthausen,andWielebinski,R.(1980).Astron.As- Anderaach, H.(1982).InExtragalacticRadioSources,ProceedingsoflAU Abell, G.O.(1958).Astrophys.J.Suppl.3,211. tremely distortedjetsanddiffuselobes.Finally,0704+351 appears tobetwophysicallyinteractingtwin-jetsources. sources, respectively.0123—016Bisa“double”withex- 952 C.P.O’DEAANDF.N.OWEN:RADIOSOURCESINCLUSTERSOFGALAXIES and Shnopper,H.W.(1980b).Astron. Astrophys. 90,283. 60, 27. Dordrecht), p.77. Symposium No.97,editedbyD.S.HeeschenandC.M.Wade(Reidel, Astron. Astrophys.Suppl.51,179. Padrielli, L.,Parma,P.,Tomasi,Maraño,B.,andZitelli,V.(1983). J. 278,37. 262, 476. 273, 24. J. 251,518. 94, 61. trophys. 69,253. B. (1982).Astron.Astrophys.110,169. trophys. J.214,351. trophys. J.168,11. 532. Astron. Astrophys.80,201. 101, 194. tron. J.77,405. Astron. Astrophys.61,99. trophys. Suppl.41339. Dordrecht), p.41. Symposium No.97,editedbyD.S.HeeschenandC.M.Wade(Reidel, © American Astronomical Society • Provided by the NASA Astrophysics Data System REFERENCES A. BridleandS.Baumforcommentsonthemanuscript. some ofthedata,P.Smileyforherworkonfigures,and Rudnick, L.,andOwen,F.N.(1976).Astrophys. J.Lett.20,L107. Rudnick, L.,andOwen,F.N.(1977).Astron. J.82,1. Rudnick, L.,andEdgar,B.K.(1984).Astrophys. J.279,74. Rudnick, L.(1982).InExtragalacticRadio Sources,ProceedingsofIAU Perley, R.A.,Bridle,A.H.,Willis,G.,andFomalont,E.B.(1980). Pacholczyk, A.G.,andScott,J.S.(1976).Astrophys.203.313. Pacholczyk, A.G.(1970).RadioAstrophysics(Freeman,SanFrancisco). Owen, F.N.,White,R.A.,andBums,J.O.(1984).Inpreparation. Owen, F.N.,andWhite,R.A.(1984).Inpreparation. O’Dea, C.P.,andOwen,F.N.(1985a).Astron.J.90,954(paperII). Rood, H.J.,Page,T.L.,Kintner,E.C,andKing,I.R.(1972).Astrophys. Roland, J.(1982).Astron.Astrophys.107,267. Riley, J.M.(1975).Mon.Not.R.Astron.Soc.170,53. Reynolds, J.E.(1980).Proc.Astron.Soc.Aust.4,74. Owen, F.N.,Burns,J.O.,andRudnick,L.(1978).Astrophys.Lett.226, O’Dea, C.P.,andOwen,F.N.(1985b).Inpreparation(paperIII). O’Dea, C.P.(1984).Ph.D.thesis,UniversityofMassachusetts,Amherst. Jones, T.W.,andOwen,F.N.(1979).Astrophys.J.234,818. JafFe, W.J.,Perola,G.C.,andValentijn,E.A.(1976).Astron.Astrophys. Jaffe, W.J.,andPerola,G.C.(1974).Astron.Astrophys.31,223. Jaffe, W.J.,andPerola,G.C.(1973).Astron.Astrophys.26,423. Owen, F.N.,White,R.A.,Hilldrup,K.C,andHanisch,J.(1982). Owen, F.N.,Rudnick,L.,andPeterson,B.M.(1977).Astron.J.82,677. Owen, F.N.,andRudnick,L.(1976).Astrophys.J.Lett.205,LI. Owen, F.N.,Bums,J.O.,andWhite,R.A.(1984).InGroupsClusters Owen, F.N.,Burns,J.O.,Rudnick,L.,andGreisen,E.W.(1979).As- Mills, B.Y.,Hunstead,R.W.,andSkellem,D.J.(1978).Mon.Not. Miley, G.K.,andHarrisD.E.(1977).Astron.Astrophys.61,L23. Miley, G.K.(1980).Annu.Rev.Astron.Astrophys.18,165. Miley, G.K.(1973).Astron.Astrophys.26,413. Miley, G.K.,Perola,C,vanderKruit,P.andLaan,H. Menon, T.K.(1980).Astron.J.85,1577. Melnick J.,andQuintana,H.(1981b).Astron.J.86,1567. Melnick, J.,andQuintana,H.(1981a).Astron.Astrophys.Suppl.44,87. McHardy, I.M.(1978).Mon.Not.R.Astron.Soc.185,927. Humason, M.L.,Mayall,N.U.,andSandage,A.R.(1956).Astron.J.61, Hoglund, B.(1967).Astrophys.J.Suppl.15,61. Hoessel, J.G.,Gunn,E.,andThuan,T.X.(1980).Astrophys.241,486. Hintzen, P.,andScott,J.S.(1980).Astrophys.239,765. Kapahi, V.K.,Joshi,M.N.Subrahmanya,C.R.andKrishna,G.(1973). Hintzen, P.,Scott,J.S.,andTarenghi,M.(1977).Astrophys.212,8. Hintzen, P.(1979).Publ.Astron.Soc.Pac.91,426. Hill, J.M.,andLongair,M.S.(1971).Mon.Not.R.Astron.Soc.154,125. Harris, D.E.,andMiley,G.K.(1978).Astron.Astrophys.34,117. Harris, D.E.,Lari,C,Vallee,J.P.,andWilson,A.S.(1980a).Astron. Harris, D.E.,Kapahi,V.K.,andEkers,R.(1980).Astron.Astrophys. Dordrecht), p.47. Symposium No.97,editedbyD.S.Heeschen andC.M.Wade(Reidel, J. 175,627. Astron. J.85,499. Astron. J.871083. Astron. Soc.185,5IP. 49, 179. of Galaxies,editedbyM.Mardirossian,G.Giuricin,andMezetti trophys J.Lett.229,L59. L119. (1972). Nature,237,269. Astron. J.78,673. 97. Astrophys. Suppl.42,319. (Reidel, Dordrecht),p.295. Suppl. 39,215. We wouldliketothankB.KevenEdgarforcalibrating 952 1985AJ 90 . . 9270 Ulrich, M.-H.(1978).Astrophys.J.221,422. Ulrich, M.-H.(1976).Astrophys.J.206,364. Thompson, A.R.,Clark,B.G.,Wade,C.M.,andNapier,P.J.(1980). Schilizzi, R.T.,Lockhart,I.A.,andWall,J.V.(1972).Austr.Phys.25, Schilizzi, R.T.(1975).Mem.Astron.Soc.79,75. Sarazin, C.L.,Rood,H.J.,andStruble,M.F.(1982).Astron.Astrophys. Valentijn, E.A.(1979a).Astron.Astrophys.78,367. Schwartz, D.A.,Schwarz,J.,andTucker,W.(1980).Astrophys.J.Lett. Schneider, D.P.,andGunn,J.E.(1982).Astrophys.263,14. Schilizzi, R.T.,andMcAdam,W.B.(1975).Mem.Astron.Soc.79,1. Sandage, A.,Kristian,J.,andWestphal,J.A.(1976).Astrophys.205,688. Slingo, A.(1974b).Mon.Not.R.Astron.Soc.168,307. Slingo, A.(1974a).Mon.Not.R.Astron.Soc.166,101. Simon, A.J.B.(1979).Mon.Not.Astron.Soc.188,637. Simon, A.J.B.(1978).Mon.Not.Astron.Soc.184,537. Ryle, M.,andWindram,M.D.(1968).Mon.Not.R.Astron.Soc.138,1. 953 C.P.O’DEAANDF.N.OWEN:RADIOSOURCESINCLUSTERSOFGALAXIES 238, L59. Astrophys. J.Suppl.44,151. 545. 108, L7. © American Astronomical Society Provided bythe NASA Astrophysics Data System Zwicky, F.,Karpowicz,M.,andKowal,C.T.(1965).CatalogofGalaxies Zwicky, F.,HerzogE.,andWild,R.(1961).CatalogofGalaxiesClus- Wirth, A.,Smarr,L.,andGallagher,J.S.,(1982).Astron.87,602. Wilson, A.S.,andVallee,J.,P.(1977).Astron.Astrophys.58,79. Willson, M.A.G.(1970).Mon.Not.R.Astron.Soc.151,1. Wellington, K.J.,Miley,G.K.,andvanderLaan,H.(1973).Nature244, Webber, J.C.(1974).Publ.Astron.Soc.Pac.86,223. Van Breugel,W.,Filippenko,A.V.,Heckman,T.,andMiley,G.(1985). Vallee, J.P.,Wilson,A.S.,andvanderLaan,H.(1979).Astron.Astrophys. Vallee, J.P.,andWilson,A.S.(1976).Nature259,451. Vallee, J.P.,Bridle,A.H.,andWilson,S.(1981).Astrophys.250,66. Valentijn, E.A.(1981).Astron.Astrophys.102,53. Valentijn, E.A.(1979b).Astron.Astrophys.Suppl.38,319. and ClustersofGalaxies(CaliforniaInstituteTechnology,Pasadena), Vol. 5. 77, 183. ters ofGalaxies(CaliforniaInstituteTechnology,Pasadena). Preprint. 502. 953 1985AJ 90 . . 9270 PLATE 74 1148 0704+351 0123-016A.B 1452MHz tary contourplotinFig.1. Fig. 2(a).B/Wradiophotographsof0123—016A,B,0431134,0457 + 054,and0704351.Thescaleisthesameasthatofcomplemen- C. O’DeaandF.Owen(seepage929) © American Astronomical Society •Provided bythe NASAAstrophysics Data System 1413 MHz0457+054 0431-134 4885MHz 1985AJ 90 . . 9270 tary contourplotinFig.1. C. O’DeaandF.Owen(seepage929) Fig. 2(b).B/Wradiophotographsof0907-091,1108+411,1330507, and1619+428.Thescaleisthesameasthatofcomplemen- 1108+411 1452MHz 0907-091 © American Astronomical Society •Provided bythe NASAAstrophysics Data System 1452 MHz1330+507 1619+428 1452MHz PLATE 75 1149 1985AJ 90 . . 9270 1150 PLATE 76 © American Astronomical Society •Provided bythe NASAAstrophysics Data System C. O’DeaandF.Owen (seepage930) orientation ofthechartsareshown in thetopleft-handcomer. Technology). Thepositionsoftheobjects denotedbythebarsaregiveninTableIII.Thescalearcminutes andthe Fig. 3(a).Opticalfieldsofclusterradio sources,reproducedfromtheEprintsofPalomarSkySurvey(Copyright 1960 NationalGeographicSociety—Palomar SkySurvey.ReproducedbypermissionoftheCaliforniaInstitute of # 0039- 097 0053-016 0123-016A.B (Cluster) A0085 A0119 A0194 Source 0039-095 0053-015 A0085 A0119 « 1985AJ 90 . . 9270 © American Astronomical Society •Provided bythe NASAAstrophysics Data System Technology). Thepositionsoftheobjects denotedbythebarsaregiveninTableIII.Thescalearcminutes andthe orientation ofthechartsareshown in thetopleft-handcorner. Fig. 3(b).Opticalfieldsofclusterradio sources,reproducedfromtheEprintsofPalomarSkySurvey(Copyright C. O’DeaandF.Owen (seepage930) 1960 NationalGeographicSociety—Palomar SkySurvey.ReproducedbypermissionoftheCaliforniaInstitute of 0309+411 0431-134 (Cluster) A0426 Source A0496 0304-123A,B 0335+096 0457+054 A0526 A0415 // PLATE 77 1151 1985AJ 90 . . 9270 nsi © AmericanAstronomical Society• Provided bytheNASA Astrophysics DataSystem PLATE 78 orientation ofthechartsareshown in thetopleft-handcomer. Technology). Thepositionsoftheobjects denotedbythebarsaregiveninTableIII.Thescalearcminutes andthe C. O’DeaandF.Owen (seepage930) Fig. 3(c).Opticalfieldsofclusterradio sources,reproducedfromtheEprintsofPalomarSkySurvey(Copyright 1960 NationalGeographicSociety—Palomar SkySurvey.ReproducedbypermissionoftheCaliforniaInstitute of 0907-091 1244+699 (Cluster) A0754 A1614 1055+570A.B 0647+693 1250-150 A0562 A1631 Al 132 W i 1985AJ 90 . . 9270 © American Astronomical Society •Provided bythe NASAAstrophysics Data System C. O’DeaandF.Owen (seepage930) Technology). Thepositionsoftheobjects denotedbythebarsaregiveninTableIII.Thescalearcminutes andthe orientation ofthechartsareshown in thetopleft-handcorner. Fig. 3(d).Opticalfieldsofclusterradio sources,reproducedfromtheEprintsofPalomarSkySurvey(Copyright 1960 NationalGeographicSociety—Palomar SkySurvey.ReproducedbypermissionoftheCaliforniaInstitute of 1519+488A.B 1615+425 (Cluster) A2172 A2064 1330+507 1556+274 1619+428 A2142 A1758 A2183 PLATE 79 1153 1985AJ 90 . . 9270 PLATE 80 1154 © AmericanAstronomical Society• Providedby theNASA Astrophysics DataSystem orientation ofthechartsareshown in thetopleft-handcomer. Technology). Thepositionsoftheobjects denotedbythebarsaregiveninTableIII.Thescalearcminutes andthe C. O’DeaandF.Owen (seepage930) Fig. 3(e).Opticalfieldsofclusterradio sources,reproducedfromtheEprintsofPalomarSkySurvey(Copyright 1960 NationalGeographicSociety—Palomar SkySurvey.ReproducedbypermisisonoftheCaliforniaInstitute of m m 1850+702 2316+184 # • (Cluster) A2572 Source * A2311 ♦ ♦ * -- ♦ * #♦ t # 2322+143A.B 1918+439 1753+580 A2319 A2593 A2289 ♦ -V *