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I ; the Astrophysical Journal Supplement Series \—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 <z <> 0.15 and are constrained in position to Ä > -15°. We describe the observations and the reduction procedure. Contour maps of all the sources are presented. Comments on individual galaxies as well as morphological features are given. Subject headings: galaxies: jets — galaxies: structure — radio sources: galaxies 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 <z< 0.15 and 8 > —15° from the Bridle characteristics of the parent galaxy and the nearby intergalac- and Perley list of radio galaxies which contain well-defined tic environs as well as to detect the optical counterpart of the radio jets (see Table 1). Column (1) indicates the galaxy name radio jet in order to answer the following questions: (1) How from NGC, 3C, 4C or B2 catalogs; columns (2) and (3) are is the radio activity generated? (2) How is the energy/mass the coordinates obtained from the reference indicated in transfer made? (3) How does the radio jet interact with the column (6); column (4) is the redshift value from the Bridle interstellar/intergalactic medium? (4) Which role do the and Perley compilation (1984); and column (5) represents the optical apparent magnitude obtained mainly from the refer- ences indicated in column (6). The observed sample can not 1 Visiting Astronomer, German-Spanish Astronomical Center, Calar be considered in any sense as complete, but all these galaxies Alto Observatory, operated by the Max-Planck Institut für Astronomie present the same kind of radio morphology at the VLA scale. jointly with the Spanish National Comission for Astronomy. 2Affiliated to the Astrophysics Division, ESTEC, Nordwijk, The This can be considered as an indicator for the same physical Netherlands. processes to operate in these objects. 41 © 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.
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