\—IU ; The Astrophysical Journal Supplement Series, 72:41-59,1990 January ^ © 1990. The American Astronomical Society. AU rights reserved. Printed in U.S.A. r" C/} ft 1 OPTICAL OBSERVATIONS OF GALAXIES CONTAINING RADIO JETS: A CATALOG OF " SOURCES WITH REDSHIFT SMALLER THAN 0.15 L. Colina1,2 Departmento de Física Teórica, Universidad Autónoma de Madrid, Spain; and Space Telescope Science Institute AND I. Pérez-Fournon1 Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain Received 1989 April 3; accepted 1989 July 13 ABSTRACT CCD imaging of 47 radio sources from the Bridle and Perley list of galaxies with radio jets is reported. All the observed galaxies are within the redshift range 0.01
I. INTRODUCTION nearby companions play in triggering the radio activity? (5) Over the past few years many authors have devoted their Which is the optical morphology of these radio jet galaxies? attention to survey radio galaxies with high angular resolution On the other hand, since most of the galaxies with radio using the VLA (Parma et al 1987 and their series of papers; jets are low-luminosity radio galaxies, this study can be also Machalski and Condon 1985; O’Dea and Owen 1985a, b; used as a complement to the optical investigations of high- Ulrich and Meier 1984; Bums and Gregory 1982; Bums, luminosity radio galaxies samples (Heckman et al 1986; Lilly White, and Hough, 1981). All these studies have permitted the and Prestage 1987; Hutchings 1987). detailed study of the radio properties of the different type of With the purpose of getting a new insight to all these radio galaxies. fundamental questions, we have started an optical survey of On the other hand, high angular resolution optical imaging galaxies with radio jets. Results on individual galaxies are of these galaxies and their surroundings is very scarce. Only given in separate papers (M87: Pérez-Foumon et al. 1988; 3C very recently some authors (Lilly and Prestage 1987; Heck- 120 and 3C 433: Colina and Pérez-Foumon 1989h). In the man et al 1986) have investigated different samples of high- present paper only the contour maps and general characteris- luminosity radio galaxies. These studies and some others tics of the galaxies are presented, while the physical implica- (Vettolani and Gregorini 1987; Heckman, Carty, and Bothun tions obtained from these data and the radio data from the 1985; Shaver et al 1982) suggest a relation between the mor- Bridle and Perley (1984) compilation will be discussed in a phology of the radio emission regions and the surrounding separate paper (Colina and Pérez-Foumon 1989a). intergalactic medium (companions, groups, or cluster of galaxies). Some of these galaxies show a similar elongated radio structure, the so-called radio jets (see Bridle and Perley 1984 II. THE DATA for a review). Radio jets are supposed to transfer mass, energy, and momentum from the core of the radio galaxy to a) The Sample the extended radio lobes. It is of fundamental importance to The observed sample consists of 47 galaxies within the investigate, by optical CCD imaging and spectroscopy, the redshift range 0.01
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© American Astronomical Society • Provided by the NASA Astrophysics Data System 42 COLINA AND PEREZ-FOURNON Vol. 72 TABLEI Observed Radio Jet Galaxy Sample a Name a (1950) 0(1950) Redshift mv References (1) (2) (3) (4) (5) (6) NGC 315 OOh55n 05s.6 30o04'56'.'0 0.0167 12.50 NGC 326 00 55 40.8 26 35 45.0 0.0483 13.00 3C31 01 04 39.2 32 08 43.6 0.0163 12.14 NGC 541 01 23 11.2 -01 38 21.1 0.0181 13.00 NGC 708 01 49 50.0 35 54 20.0 0.0160 14.50 4C 35.03 02 06 39.2 35 33 41.0 0.0373 13.00 3C 66B 02 20 01.8 42 45 54.6 0.0215 12.90 NGC 1044 ... 02 38 25.0 08 31 24.0 0.0214 13.27 3C75 02 55 03.1 05 49 36.2 0.0241 13.16 4C 13.17B 02 56 30.0 13 1517.0 0.0748 16.80 3C78 03 05 49.1 03 55 13.1 0.0288 12.94 NGC 1265 ... 03 14 57.0 41 40 33.4 0.0255 12.50 NGC 1275 ... 03 16 29.6 41 19 52.1 0.0177 11.87 W 7.08.14 ... 03 26 06.5 39 37 12.0 0.0243 14.90 3C 111 04 15 00.6 37 5419.0 0.0485 18.05 3C120 04 30 31.5 05 15 01.0 0.0334 14.12 3C129 04 45 21.2 44 56 45.0 0.0208 19.40 B2 0658+ 33 . 06 58 53.0 33 01 46.8 0.1270 16.18 4C35.16A ... 07 04 20.0 35 08 39.0 0.0780 15.50 4C 53.16 07 12 42.1 53 28 31.5 0.0640 15.00 0908 + 37 09 08 45.4 37 36 33.0 0.1047 15.50 NGC 4789 ... 12 51 52.3 27 20 57.8 0.0270 13.30 NGC 4782/3. 12 52 00.1 -12 17 07.0 0.0138 13.50 NGC 4869 ... 12 56 58.7 28 10 51.0 0.0224 14.90 4C 29.47 13 16 43.8 29 54 27.0 0.0728 15.00 NGC 5127 ... 13 21 26.3 31 49 33.0 0.0161 13.90 NGC 5490 ... 14 07 37.0 17 46 48.0 0.0163 13.40 3C296 14 14 26.0 11 0215.1 0.0237 12.21 3C303 14 41 24.8 52 1418.7 0.1410 17.29 3C305 14 48 17.6 63 28 36.4 0.0410 13.74 B2 1450+ 28 . 14 50 23.8 28 1015.0 0.1265 16.50 A 2172 16 14 59.1 42 3415.2 0.1310 4C 53.37 16 38 24.0 53 5210.0 0.1098 16.50 3C371 18 07 18.5 69 48 59.0 0.0500 14.81 3C 388 18 42 35.4 45 30 21.7 0.0908 15.32 4C 47.51 19 19 49.8 48 00 35.2 0.1030 15.15 3C 402N 19 40 22.5 50 29 29.0 0.0247 14.00 3C405 19 57 44.4 40 35 45.2 0.0565 16.22 NGC 7052 ... 21 16 20.7 26 14 08.0 0.0164 14.00 3C433 21 21 30.5 24 51 33.0 0.1016 16.24 3C445 22 21 14.7 -02 2126.8 0.0562 15.77 3C449 22 29 07.7 39 06 04.6 0.0171 13.20 B2 2236+ 35 . 22 36 12.3 35 0411.0 0.0277 15.00 OZ 127 23 16 09.6 18 24 58.2 0.0395 NGC 7626 ... 23 18 04.0 07 5712.0 0.0112 12.80 3C465 23 35 59.0 26 45 18.0 0.0293 15.00 4C 47.63 23 54 57.4 47 09 39.0 0.0460 15.00
References.—(1) Burbidge and Crowne 1979; (2) van Breugel et ai 1985; (3) Parma et al. 1986; (4) O’Dea and Owen 1985a; (5) Bums and Owen 1979; (6) Jaffee etal. 1976; (7) Clarke et al 1976; (8) Colla et al. 1975; (9) Bums and Gregory 1982.
b) Observations cal exposure times were 20-30 minutes while the seeing, Observations of the present sample were conducted during measured from star profiles in the CCD frames, was typically three observing periods, 1985 November and 1986 June and between I'.'O and 1'.'5 (FWHM). November at the Calar Alto Observatory in southern Spain. All the observations were made with a RCA CCD camera c) Data Reduction attached to the Cassegrain focus (f/8) of the 2.2 m telescope. The reduction procedure consisted of many steps. The bias The CCD camera consisted of 320 by 512 pixels of 30 /¿m in correction was done using a set of exposures of zero seconds size giving a scale of O'.^Sl pixel-1 and a field of view of 112" exposure time without opening the camera shutter. A mean by 180". The Gunn-Thuan r filter (Thuan and Gunn 1976; r. bias frame was subtracted from all the others. The dark ^effect = 6550 À, FWHM = 900 Á) was used throughout. Typi- current was found to be negligible for the chip used. Correc-
© American Astronomical Society • Provided by the NASA Astrophysics Data System No. 1,1990 GALAXIES CONTAINING RADIO JETS 43 ^ tion for the pixel to pixel sensitivity variations, including a nucleus of the galaxy which become more elliptical, off- fixed pattern of bad columns at faint light levels, as well as centered and slightly distorted at larger radii. ^ the large scale sensitivity gradient along the CCD chip, was 0149 4- 35 (NGC 708).—This galaxy, which is the brightest < performed using a set of lamp-dome and twilight exposures. galaxy in the Abell cluster A 262, has a conspicuous central The sky background was obtained from the mode of the dust lane in P.A. 356° (clearly visible in our unpublished g ^ pixels’ value distribution around the edge of the frame. image). This dust lane is almost perpendicular to the S-shaped Atmospheric conditions were not always photometric dur- radio emission which appear elongated along P.A. 70° (Parma ing all observing nights. Therefore, the data reported here are etal. 1986). Also the isophotes show a twist which could be referred to the sky background. A Hubble constant H0 = 75 associated with some physical interaction with the nearby km s_1 Mpc-1 has been used to obtain the projected dis- edge-on spiral galaxy, NGC 705, located at 20.6 kpc south- tances from the CCD arcsec scale. All distances indicated in west (P.A. 245°) of NGC 708. Some other smaller elliptical the following comments must be considered as projected galaxies appear at distances shorter than 30 kpc. distances in the plane of the sky. 0206 + 35 (4C 35.03).—This radio galaxy consists of a core Contour maps of the reduced CCD images are presented as with a two-sided jet (P.A. 125° and P.A. 305°) embedded in a Figure 1 following the text. symmetric halo of diffuse emission (Parma etal. 1986) and presents a S-shaped morphology (de Ruiter and Parma 1984). At optical wavelengths, our CCD image reveals several pecu- III. COMMENTS ON INDIVIDUAL SOURCES liarities. The outer isophotes show a clear twist towards the 0055 + 30 (NGC 315).—This galaxy presents a radio jet in southeast (P.A. 108°) were a nearby elliptical galaxy sepa- position P.A. 310° with a possible counter jet (Bridle et al. rated by 30.8 kpc is located. This elliptical companion also 1979). Butcher, van Breugel, and Miley (1980) did not find presents an elongation in the direction of 4C 35.03. These any optical counterpart of the radio jet from their blue image. facts can be considered as an evidence of interaction between Our optical image shows an elliptical galaxy with its major these two galaxies. A third small galaxy, located at a distance optical axis in a direction perpendicular to the observed radio of 16.2 kpc to the southwest (P.A. 201°) of the radio source jet. As indicated by Ebneter and Balick (1985), from their nucleus, also presents an elongation toward 4C 35.03. B — R CCD color map, NGC 315 contains dust distributed in 0220 + 42 (3C 66B).—This galaxy, which has an optical jet irregular patches in the galaxy. as a counterpart of the radio one (Butcher et al. 1980), shares 0055 + 26 (NGC 326).—This galaxy appears as a dumbbell a projected halo with a smaller elliptical companion separated galaxy with two equally bright nuclei separated by 6.5 kpc in by a distance of 9.8 kpc in position P.A. 131°. The outer P.A. 152°. The outer isophotes show a clear twist changing isophotes are twisted as well as off-centered with respect to the position angle of the major axis toward a smaller compan- the inner ones. A detailed study of the optical jet and isophote ion galaxy located 40.2 kpc southwest (P.A. 201°) of NGC analysis will be given in Pérez-Foumon and Colina (1990). 326. This small companion also presents a light bridge toward 0238 + 08 (NGC 1044).—This galaxy forms a system with a NGC 326. These two features can indicate a physical interac- smaller elliptical companion located in position P.A. 122° and tion between both galaxies. The radio emission, which has a at a projected distance of only 7.8 kpc. The outer isophotes well-developed S shape (Fomalont 1983), shows twin jets are off-centered with respect to the nuclear ones and stretched along directions P.A. 135° and P.A. 315°, i.e., in a similar toward the southwest. These two galaxies are almost aligned direction to that joining the nuclei of the two galaxies. This with a third companion which is located to the NW radio morphology has been interpreted as being due to pre- (P.A. 305°) and separated by 23.5 kpc. The three galaxies are cessional motions (Ekers et al. 1981). altogether almost aligned with the observed radio jet emission 0104-\- 32 (3C 37).—This radio galaxy, NGC 383, shows (P.A. 135° and P.A. 315° from Fomalont, Palimaka, and up in our image as an elliptical galaxy with a close smaller Bridle 1980 radio map). elliptical companion (NGC 382) located at 10.6 kpc and in 0255 3-05 (3C 75).—This galaxy is a well-known peculiar direction P.A. 202°. The parent radio galaxy shows a central radio galaxy having a multiple system of radio jets (Owen dust lane parallel to the optical major axis (clearly visible in et al. 1985). It is the central galaxy of the Abell cluster A400 our g- r color map, Colina 1987 and also indicated by and has a dumbbell morphology with the two equally bright Ebneter and Balick 1985), and with the minor axis almost nuclei separated by 7.5 kpc in the north-south direction. perpendicular to the inner part of the S-shaped radio emis- Morphologically, these galaxies (3C 75A, B) appear as two sion (Fomalont et al. 1980; de Ruiter and Parma 1984). This ellipticals in projection and without optical peculiarities. A radio morphology has been interpreted (Blanford and Icke resolved faint object, superposed to the northeast radio jet 1978) as due to dynamical interaction between NGC 382 and (P.A. 110°), is probably a fainter galaxy of the same cluster NGC 383. An optical counterpart of the norther radio jet (Pérez-Foumon etal. 1986; Colina 1987). (P.A. 341°) was detected by Butcher and collaborators 0256 + 13 (4C 13.17B).—This galaxy located in the Abell (Butcher, van Breugel, and Miley 1980). cluster A401, has a narrow angle tail radio morphology (O’Dea 0123 - 01 (NGC 541).—This is a well-known radio galaxy, and Owen 1985a). At optical wavelengths it appears as an located in the Abell cluster A 194, which has recently been elliptical galaxy without morphological peculiarities and with considered as an example of star formation, the Minkowski a nearby edge-on spiral galaxy located in position P.A. 44° object, triggered by a radio jet (van Breugel et al. 1985; and separated by 31 kpc. A light bridge between both galaxies Brodie, Bowyer, and McCarthy 1985). Our deep CCD image could be present, but ghost effects due to a bright foreground shows an elliptical galaxy with rounder isophotes at the star do not permit a firm conclusion.
© American Astronomical Society • Provided by the NASA Astrophysics Data System 44 COLINA AND PEREZ-FOURNON Vol. 72 0305 + 03 (3C 78).—This radio source appears, in our CCD belonging the same cluster, appear within our CCD field of image, as an elliptical galaxy isolated and without morpholog- view. ^ ical peculiarities. At radio frequencies, a northeast (P.A. 53°) 0712 + 53 (4C 53.16).—This galaxy, located in the Zwicky § radio jet perpendicular to the major optical axis is observed cluster 0712.9 + 5334 (Bums and Owen 1979), appears in our S (Unger, Pooler, and Pedlar 1984). CCD image as a system of two galaxies separated by 27 kpc 2 0314 + 41 (NGC1265).—This radio galaxy is located in the in position angle P.A. 127°. The companion of the radio Perseus cluster (A426). It has a narrow angle tail morphology galaxy has a size of 0.36 times that of 4C 53.16. The observed observed at radio frequencies (Owen, Bums, and Rudnrick radio lobes (Bums and Gregory 1982) appear elongated along 1978). Our CCD image indicates the presence of an object P.A. 118°, i.e., almost identical to the one connecting the near the nucleus which is most probably a foreground star. galaxy centers, and within the optical extend of the galaxy. Also a smaller elliptical galaxy is detected at a distance of 20 Some other galaxies are also visible within the CCD image. kpc to the southeast (P.A. 97°) of NGC 1265. 0908 + 37.—From our CCD image, this galaxy appears as 0316 3-41 (NGC 1275).—This is a giant elliptical galaxy an elliptical with a very distorted morphology presenting a with a Seyfert nucleus and located at the center of the Perseus second, and less compact, emission peak at a distance of 6.4 cluster (A426). Pedlar, Booler, and Davis (1983) detected an kpc in position P.A. 335°. The radio structure presents two unresolved radio core with two knots which are interpreted as lobes at positions P.A. 13° and P.A. 189° respectively (Parma a radio jet along position angle P.A. 160°. Our CCD image etal. 1986; Machalski and Condon 1983) with a jet connect- shows the well-known systems of filaments which can be ing the compact nucleus with the northern radio lobe. associated with cooling flows (Cowie etal. 1983; Hu etal. 1251 3-27 (NGC 4789).—This source appears as an isolated 1983; Johnstone and Fabian 1988). Most of this emission and elliptical galaxy with no traces of peculiar morphology. corresponds to Ha flux included in the r filter. The object to the north is a bright star producing saturation 0326 3- 39 (W 7.08.14).—This radio galaxy shows a two- effects on the CCD. sided radio jet along the east-west direction (Ekers etal. 1981) 1252 — 12 (NGC 4782/3).—This radio source with a sys- and has, as indicated in our CCD image, a nearby galaxy tem of twisted radio jets (Baum et al 1988) is associated with separated by 11 kpc at P.A. 23° and enclosed by a projected the southern nucleus (NGC 4782; Sandage 1972), of a dumb- halo. The inner isophotes are rounder than the outer ones. bell galaxy. The two equally bright components are separated 04153-37 (3C 111).—This radio galaxy shows a knotty by 11.4 kpc in position P.A. 18°. Isophote distortion is clearly radio jet along P.A. 63° (Linfield and Perley 1984). In our visible in both components which are surrounded by a large optical image, 3C 111 appears as a very faint source slightly halo, indicating an ongoing physical interaction between the resolved. No structural or morphological features are detected two galaxies (this effect has recently been confirmed by Borne, at the present detection level. Balcells, and Hoessel 1988). 0430 + 05 (3C 120).—This is a well-known high luminosity 1256 + 28 (NGC 4869).—This galaxy is located in the Abell radio galaxy with a Seyfert 1 nucleus, a nuclear superluminal cluster A1656 and presents a narrow angle tail radio morphol- jet, two extended lobes to the NW and SE and one elongated ogy (O’Dea and Owen 1985a). Our CCD image shows NGC radio emission connecting the core with the NW lobe (Walker 4869 as an elliptical galaxy with twisted isophotes and optical et al. 1987). A detailed study of the optical counterpart of the filaments in position P.A. 150°. Although the seeing is poor, observed western radio jet is under progress (Colina and these filaments could be similar, at least in morphology, to Pérez-Foumon 1989h). those observed in 3C 120 (Colina 1987; Colina and Pérez- 0445 3- 44 (3C 129).—This galaxy with a WAT radio struc- Foumon 1989&). ture (Downes 1984) appears in our CCD image as a faint 1316 3-29 (4C 29.47).—This radio source shows an S- elliptical galaxy without peculiarities in its morphology. shaped morphology which has been explained due to preces- B2 0658 + 33.—This radio source is associated with one of sional motions by Condon and Mitchell (1984). At optical the dominant galaxies of the A567 cluster and has twin jets wavelengths, 4C 29.47 appears as an elliptical galaxy with no which bend gradually producing a wide angle tail morphology morphological pecuharities and with a nearby edge-on spiral (O’Dea and Owen 1985û). Our CCD image shows distorted galaxy in direction P.A. 278°. isophotes and the presence of faint companions along P.A. 1321 + 31 (NGC 5127).—Our CCD image shows NGC 121° and P. A. 258° and located within the outer envelope. 5127 as an elliptical galaxy with no peculiar morphology at 0704 3-35 (4C 35.16A).—Located in the Abell cluster the present detection level. The radio extended emission shows A568, this source presents a rather complex structure at the a two-sided jet along P.A. 120° (Fanti et al 1982), i.e., in- VLA resolution. O’Dea and Owen (1985æ) suggest that this clined by about 30° with respect to the optical minor axis. could be an unique example of physically interacting radio 1407 3-17 NGC 5490).—Our CCD image shows an ellipti- sources. Our deep CCD image shows a rather complex mor- cal galaxy with no peculiar morphology. At radio frequencies phology also at optical wavelengths. The main system consists (5 GHz), a linear radio emission along directions P.A. 80° of two galaxies almost identical in size. These two galaxies and P.A. 260° have been detected (Jenkins 1982). separated by 22 kpc along P.A. 337° show a distorted ellipti- 1414 3-11 (3C 296).—This radio source is located in the cal morphology with the outer isophotes off-centered with Abell cluster A1890. The radio emission has a Fanaroff-Riley respect to the inner ones. The system is completed by other type I morphology and shows a jet along P.A. 35° (Birkinshaw, three smaller galaxies located at distances of 36-34 kpc and Laing, and Peacock 1981), i.e., perpendicular to the optical positions P.A. 69°, P.A. 9°, and P.A. 125° with respect to the major axis, together with a fainter counteijet along P.A. 215°. nucleus of the main galaxy. Many other galaxies, probably At optical wavelengths, the radio galaxy has a small compan-
© American Astronomical Society • Provided by the NASA Astrophysics Data System No. 1,1990 GALAXIES CONTAINING RADIO JETS 45 CM ^ ion, relative size 0.36, located at a distance of 15.4 kpc in faint objects located within the halo of 3C 388 (identified as position P.A. 168°. galaxies by Bums and Christiansen 1980). The smaller com- ^ 1441 + 52 (3C 303).—This galaxy appears as elliptical in ponents have a mean relative size of 0.15 that of the main < morphology with no trace of peculiarities and with a rather body of 3C 388. They are located at a distance of 12.4 kpc at S compact nucleus. There is no clear indication of optical a P.A. 254° and of 24 kpc at P.A. 112° and P.A. 225°, ^ emission associated with the knotty radio jet oriented towards respectively. The outer envelopes of this system are elongated the northwest (P.A. 278°; Lonsdale, Hartley-Davies, and in direction southwest toward a region where two other nearby Morison 1983), although object “u” could be the optical galaxies are located. counterpart of the radio hot spot (see Lonsdale, Hartley- 1919 + 48 (4C 47.51).—This source is the central and largest Davies, and Morison 1983 and Keel 1988 for detailed discus- of a group of galaxies within a radius of 85 kpc. The galaxy sions). itself shows a knot at P.A. 326° well inside the galaxy and a 1448 + 63 (3C 305).—This is a well-known radio galaxy diffuse elongation at P.A. 110° which could agree, at least in previously studied in detail, at both optical and radio frequen- position, with the inner part of the radio jet (knot D^ cies, by Heckman and collaborators (Heckman etal 1982; observed in P.A. 111° (Robertson 1984). Heckman et al. 1986). Although the image trailed, we confirm 1940+ 50 (3C 402N).—The radio source presents a two- the main morphological results of the previous authors. sided jet structure, with total extent of 34" at a position angle B2 1450 + 28.—This source located in the cluster A1984 of about 175° (Riley and Pooley 1975), near the position shows a dumbbell morphology with the two components angle of the companions with respect to the main galaxy. The separated by 24 kpc along the north-south direction. The optical galaxy shows an elliptical morphology with a nuclear outer isophotes are stretched toward P.A. 215° where a com- optical peak (star?) in position P.A. 260°. Also a light bridge panion galaxy is located. The radio emission, associated with connects the outer envelope of 3C 402N with a northwest the southernmost component of the pair of galaxies, is elon- smaller disk galaxy located at a distance of 18 kpc in position gated along P.A. 117° (Parma et al. 1986). P.A. 341°, whilé another companion is located along P.A. 1615+ 42.—This radio galaxy, located in the Abell cluster 151° at 23 kpc from the radio galaxy nucleus. Both of these A2172 shows two-sided nuclear jets and was classified as wide companions appear to be late-type galaxies seen edge-on. angle tail radio structure by O’Dea and Owen (1985a). Our 1957 + 40 (3C 405).—This radio galaxy is often considered CCD image shows an elliptical galaxy forming a system with as the archetypal classic double radio galaxy showing a weak a smaller companion. The size of the companion is 0.40 that radio jet along P.A. 285° (Perley, Dreher, and Cohen 1984). of the radio galaxy and is located at 16.5 kpc in position P.A. Our CCD image shows Cyg A as an elliptical galaxy with 109°. This companion, which could be confused with a star, distorted nuclear isophotes. This morphological feature seems appears as very compact but extended. In fact asymmetry in to be due to the presence of two nuclei (Pierce and Stockton the isophotes distribution is observed towards the east. A 1986): the continuum featureless southeastern peak and the third component appears in P.A. 137° and slightly separated emission line northwestern peak. with respect to the radio jet direction (P.A. 146°; O’Dea and 2116 + 26 (NGC 7052).—This galaxy presents at radio fre- Owen 1985 a). Also the outer envelopes of the main galaxy are quencies a twin radio jet in positions P.A. 21° and P.A. 201° elongated toward the SW (P.A. 235°) where a companion (Parma et al. 1986). Our CCD image shows NGC 7052 with elliptical galaxy is located at a distance of 110 kpc. an elliptical morphology in the inner isophotes while the outer 1638 + 53 (4C 53.37).—This radio galaxy is a giant dis- ones appear boxy. torted elliptical, located in the Abell cluster A2220, showing a 2121 + 24 (3C 433).—This is a very peculiar high-luminos- small companion, relative size 0.22 that of 4C 53.37, at a ity radio galaxy (van Breugel etal. 1983) which forms a distance of 40 kpc to the southwest (P.A. 207°). The outer dumbbell system with its more compact NE companion. A isophotes present a distorted morphology with a well-defined detailed account of the features and detection of the optical optical emission peak at P.A. 191° and a broad emission counterpart of the southern radio lobe is in progress (Colina feature at P.A. 162°. None of these features are related to the and Pérez-Foumon 19896). detected radio jet elongated along the P.A. 137° direction 2221 - 02 (3C 445).—This radio source shows an elongated (Bums and Owen 1980). Although the seeing conditions in radio structure extended over 10' and almost aligned along our CCD image are poor, these emission peaks agree with the the NS direction (Kronberg, Wielebinski, and Graham 1986). faint and diffuse objects observed in Palomar plates (Bums This radio emission ends in a complex and single hot spot to and Owen 1980). the north and south, respectively. At optical wavelengths, this 1807 + 69 (3C 371).—This radio galaxy has a compact core radio galaxy has an elliptical morphology with a very compact with a small jet (1" long) in direction P.A. 235° (Browne and nucleus (N galaxy). Our r CCD image does not show as clear Orr 1981). At optical wavelengths, our CCD image shows an as the V image of Heckman and collaborators (Heckman elliptical morphology with no peculiarities but with a rather et al. 1986), the bright tail extending up to 10" at P.A. 230°. compact nucleus. This could be therefore associated with [O m] emission lines 1842 + 45 (3C 388).—This classical double edge-bright- rather than continuum emission. ened radio galaxy (Bums and Christiansen 1980; Bums, 2229 + 39 (3C 449).—This galaxy shows the presence of Christiansen, and Hough 1982) has a complex jet embedded two highly collimated symmetric jets on each side of an in the southwest lobe. 3C 388 is associated with a cD galaxy unresolved core and elongated along directions P.A. 13° and at the center of a poor cluster (Mathews, Morgan, and Schmidt P.A. 186° (Perley, Willis, and Scott 1979). The most striking 1964) and appears in our CCD image as a galaxy with three aspect of this source is the nearly perfect mirror symmetry of
© American Astronomical Society • Provided by the NASA Astrophysics Data System 0055+30 N 0055+26 © American Astronomical Society • Provided by theNASA Astrophysics Data System 46
Fig. 1.—All the figures represent the contour maps of the different galaxies in the Gunn-Thuan r filter obtained from our CCD images. The first contour is at the 5% level above the background value except for 055 + 26, 0149 + 35, 0206 + 35, 0220 + 42, 0238 + 08, 0305 + 03, 0326 + 39, 1807 + 69, and 2318 + 07, where the first contour is at the 10% level and for 0908 + 37, 1414 + 11, 1450 + 28, 1615 + 42, and 2121 + 24 where the first contour is at the 2.5% level. The spacing between the contours corresponds to 0.5 mag. The images were smoothed with a 3 by 3 median filter. U
0149+35 N 0206+35 © American Astronomical Society • Provided by theNASA Astrophysics Data System 47 i 1 ..se 0255*05 N 0256*13 © American Astronomical Society • Provided by theNASA Astrophysics Data System 0316+41 N 0326+39 © American Astronomical Society • Provided by theNASA Astrophysics Data System 49 0445+44 N 0658+33 © American Astronomical Society • Provided by theNASA Astrophysics Data System 50 19 90ApJS. . .72. . .41C © American Astronomical Society • Provided by theNASA Astrophysics Data System 51 1316+29 N 1321+31 © American Astronomical Society • Provided by theNASA Astrophysics Data System 52 19 90ApJS. . .72. . .41C © American Astronomical Society • Provided by theNASA Astrophysics Data System 1638+53 N 1807+69 © American Astronomical Society • Provided by theNASA Astrophysics Data System 19 90ApJS. . .72. . .41C © American Astronomical Society • Provided by theNASA Astrophysics Data System 2221-02 N 2229*39 © American Astronomical Society • Provided by theNASA Astrophysics Data System ..çe 56 se se 19 90ApJS. . .72. . .41C © American Astronomical Society • Provided by theNASA Astrophysics Data System 1 „se Ul 57 U COLINA AND PÈREZ-FOURNON Vol. 72 ™ the jets and outer lobes about an axis through the central minor axis along P.A. 92°. The radio structure of the source is ; nucleus. At optical wavlengths, it seems to form a system with that of a well-defined jet along P.A. 35° ±5° with a total ^ its nearby companion, relative size 0.44 that of the radio length of about 80" (Birkinshaw and Davies 1985). g source, located at 12.4 kpc in position P.A. 13°. 3C 449 has a 2335 3-26 (3C 465).—This galaxy, located in the Abell nuclear dust lane almost parallel to the optical major axis, cluster A2634, presents a wide angle tail morphology at radio ^ clearly visible in our unpublished image in the g filter (see frequencies (Leahy 1984). The optical image shows a system also Ebneter and Balick 1985), and twisted isophotes. The of two nuclei, the northern component with a size 0.30 that of companion galaxy shows a very compact nucleus and a warp the southern component, separated by 6.7 kpc in direction of the outer isophotes toward 3C 449. Also the common P.A. 10°. These two nuclei are well inside the outer isophotes envelope shows elongations toward the NE and SW direc- show warped elongations to the southwest. To the east, two tions. This system could be a good candidate for a detailed other galaxies appear, elliptical and lenticular respectively, study of the relation between the S-shaped radio morphology located in position P.A. 77° and P.A. 94° and separated by and orbital motions. 30.4 kpc and 52 kpc apart from the 3C 465 nucleus, respec- B2 2236 + 35.—This galaxy has a S radio morphology with tively. the inner radio jet elongated along P.A. 46° (Parma et al. 2354 + 47 (4C 47.63).—This radio source shows a two-sided 1986). At optical wavelengths, it shows an elliptical morphol- radio jet toward P.A. 58° and P.A. 218° within the first 30" ogy with twisted isotopes. An elliptical, with a relative size (Bums and Gregory 1985). The galaxy itself shows an ellipti- 0.50 that of the radio source, is located at a distance of 42 kpc cal morphology. A smaller galaxy is located along P.A. 18° at in position P.A. 55°. The wide optical filaments which appear a distance of 35.8 kpc from the radio galaxy nucleus. No trace in the outer isophotes in positions P.A. 85° and P.A. 255° are of light bridge between these two galaxies, which can indicate ghosts due to reflections and do not appear in other images physical interaction rather than projection effect, is detected obtained with the 3.5 m telescope. at the present detection limit. 2316 3-18 (OZ 127).—This radio source located in the cluster A 2572 shows a twin tail radio structure and exhibits a sudden transition from jet to diffuse tail (O’Dea and Owen 1985¿z). From our CCD image, this galaxy is elliptical in morphology with a small companion, of size 0.36 that of OZ We wish to thank the Panel for Allocation of Telescope 127, at a distance of 13.2 kpc in southeast direction (P.A. Time for generous allocation of observing time, and the Calar 133°). Many other galaxies, probably belonging to the same Alto staff for help during the observations. L. Colina ac- cluster, appear at different distances and positions surround- knowledge the support of the European Space Agency through ing the radio galaxy. an ESA postdoctoral fellowship. I. Pérez-Foumon would like 2318 3-07 (NGC 7626).—This galaxy is a bright elliptical to thank J. I. Gonzalez-Serrano for discussions and help in with no clear peculiarities in its morphology and with the developing the reduction software.
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Luis Colina: Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218
Ismael Pérez-Fournon: Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain
© American Astronomical Society • Provided by the NASA Astrophysics Data System