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1996ApJS..107...19McCarthy+
(OCR+proof by H.Andernach 1/97)
See also MRC 1Jy sample II.
and MRC 1Jy sample III.

The Molonglo Reference Catalog / 1-Jansky Radio Source Survey I. Radio Galaxy Identifications

P. J. MCCARTHY, V. K. KAPAHI, W. VAN BREUGEL, S. E. PERSSON, R. M. ATHREYA, & C. R. SUBRAHMANYA

Abstract

This is the first in a series of papers discussing the properties of a complete set of radio sources selected near S408 = 1 Jy. We present optical or infrared identifications for a sample of 452 radio galaxies. The sources were selected from the 408 MHz Molonglo Reference Catalog, restricted only by flux density and position on the sky, as follows: S408 > 0.95 Jy and -30d<DEC50<-20d, and 09h20m<RA(1950)<14h04m or 20h20m <RA1950<06h14m. This complete sample, the MRC/1 Jy survey, contains 558 radio galaxies or quasars, of which six are occulted by bright stars or galaxies and two are multiple confused sources. Of the remaining 550 sources, 527, or 96%, are identified to an r magnitude of 25, and eight additional sources are identified to K = 19. Of the 17 unocculted objects that remain unidentified, 15 are sources for which we have either poor radio maps or inadequate optical/IR images. This paper presents finding charts and astrometric positions for the 452 sources that are not identified as either quasars or BL Lacertae objects. Magnitudes in the r passband accurate to typically 0.1 mag are given for 353 of the radio galaxy identifications. Redshifts for 268 of the galaxies are also listed; those have been derived from 450 spectroscopic observations. The radio observations, quasar and BL Lac identifications, spectroscopy, and near-IR images will be presented in subsequent papers in this series.

Subject headings: galaxies: photometry-quasars: general-radio continuum: galaxies-surveys

1. INTRODUCTION

All studies of astronomical objects have their origins in surveys of one sort or another. Our understanding of radio galaxies and quasars in particular is strongly rooted in welldefined samples drawn from large surveys (e.g., the 3CRR; Laing, Riley, & Longair 1983). Radio surveys are also strongly motivated by their utility in identifying classes of objects that can be observed at other wavelengths, and thereby can be used for purposes beyond the study of radio source physics per se. The earliest radio surveys with sufficient resolution to allow the identification of the sources on optical photographs contained many sources below the limit of either the Palomar Observatory Sky Survey or the deepest prime focus plates taken at the Hale 5 m telescope (e.g., Wyndham 1966; Veron 1966). As radio observations with resolutions of several arcseconds or better became widely available (e.g., Jenkins, Pooley, & Riley 1977) it became clear that a significant fraction of strong sources could not be identified on any plate material (e.g., Kristian, Sandage, & Katem 1974; Windhorst, Koo, & Kron 1985). The use of CCDs and, more recently, near-IR arrays on large aperture telescopes allows one to identify all, or nearly all, strong and intermediate strength sources, as this paper and others demonstrate (e.g., Dunlop et al. 1989). There are, however, only a handful of radio surveys for which intensive optical follow-up observations have been made. The paucity of radio samples for which complete optical identifications and redshifts exist has hampered our ability to obtain a thorough census of the radio source population and has limited the degree to which radio sources can be used as probes of the distant universe.

This paper is the first in a series aimed at expanding our knowledge of the radio, optical, and infrared properties of a sample of sources selected solely by low-frequency flux density. This survey will be used to address a variety of astrophysical problems. Understanding the high-redshift radio galaxies and the relationship between radio galaxies and radio quasars are two examples of goals for which this program was initiated. Despite the existence of numerous radio surveys at a variety of frequencies, there are at present few complete and unbiased surveys of extragalactic sources for which corresponding optical observations are available. The 178 MHz 3CRR survey (Bennet 1962; Laing et al.1983) is the best-studied sample of strong low-frequency selected sources and is one of the few complete radio samples for which optical identifications and redshift measurements exist for all the sources (see Rawlings et al. 1996 for the last of the 3CRR sources; see Djorgovski et al. 1988 and Spinrad et al. 1985 for the 3CR identifications). At higher frequencies there are several samples that have been fully identified with optical counterparts (e.g., Wall & Peacock 1985). The Parkes Selected Regions (Downes et al. 1986; Dunlop et al. 1989) is a large and completely identified sample selected at 2700 MHz. The redshift content for this sample, however, is fairly meager. Other high-frequency surveys having a high fraction of optical identifications and/or redshifts are confined to strong sources and sample the radio source population with a selection function ...

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The r magnitude of each source identification was measured in a series of apertures ranging from 0.5" to 10", and a growth curve was determined. Local sky was determined by computing the median within a 3" wide concentric annulus with an inner radius 4" to 8", the exact location of which was chosen to avoid contamination from nearby stars or galaxies. When nearby objects could not be avoided, they were edited out of the image before the photometry was performed. There are several objects that are too close to foreground stars or galaxies for this procedure to succeed, and their magnitudes are consequently highly uncertain, i.e., +-0.5 mag, and these are noted below. The r magnitudes listed in Table 2 refer to a 4" diameter aperture. For the brightest galaxies the 4" aperture magnitude grossly underestimates the total magnitude.

4. RESULTS

Table 2 lists each radio galaxy or empty field by its IAU name based on the 1950 source position in the MRC, its 1950 position, the provisional redshift when available, the r magnitude within a 4" diameter aperture, the telescope and observing run for which the identification image was obtained, a code number for the size of the image in Figure 1, and a brief comment. The positions refer to the optical or infrared identifications as derived above, except for those sources noted as unidentified. For the latter the VLA radio positions are listed. There are 452 entries in Table 2, several more than the difference between the original catalog of 558 sources and the 110 quasar and BL Lac identifications. This occurs because a few of the sources listed in the MRC were found to be multiple in our VLA images. The identification for these sources are included here, and those which are not part of the complete radio sample are also identified as such in the notes. The redshifts listed in Table 2 are provisional only. Final precise redshifts and detailed notes concerning the spectra will be presented in Paper IV. The redshift presented here should be accurate to delta_z~0.05.

Figure 1 (Plates 6-28) presents finding charts for nearly all of the radio galaxies. Each image is a 200 x 200 pixel subsection of a larger CCD or infrared camera image with north at the top and east to the left. The radio source identification is positioned at the central pixel in nearly all cases, but for a few objects this was either not possible or desirable. In all cases two vertical and two horizontal ticks mark the identification. For the few sources that remain unidentified, we have indicated the positions of the radio components with circles 5" in diameter. For small doubles we have marked only the midpoint position.

The size of the field displayed depends on the telescope and detector used. Column (12) in Table 2 contains a code number for the field size, which is given in the notes to the table. The vast majority of the images were taken with the 2.5 m/TI CCD combination and so have a field of 66.4"x 66.4" (code 1). Many of the brighter objects were imaged with the 1.0 m and TI CCD and have a field of 87" x 87" (code 2). The infrared images are 70" x 70" (code 3), nearly the same as the 2.5 m/TI CCD images. Several of the bright galaxies were not observed with the 1.0 m telescope, and for these we reproduce 100 x 100 pixel images from the digitized SERC J sky survey films that have been rebinned to 200 x 200 pixel images with a field size of 170" x 170" (code 4). A few images were taken with the 2.5 m plus Tektronix CCD and have a field of 59" x 59" (code 5).

Here we make a few remarks on some objects that have interesting characteristics or for which the finding chart alone may not provide enough information to make the identification clear to the reader. All of the 5 GHz and 1400 MHz data referred to below are presented in Paper II.

0007-287 The central component of this radio source lies within 2" of a V~15 mag star, as confirmed spectroscopically by R. Hunstead and V. Kapahi with the Anglo-Australia Telescope (AAT). No other plausible identification can be seen on our CCD images.
0022-209 There are two sources in our map, both are identified with bright galaxies in the cluster Abell 27. Only the westernmost of the two sources is strong enough to remain in the complete sample.
0023-203 This source is 23" south of a bright star. The identification is confirmed by our K image where the contrast against the scattered light from the star is better.
0029-232 This is a large source, and the identification is slightly uncertain. The galaxy marked is ~2" from the symmetry axis of the source. No other potential identification is visible.
0029-243 The identification consists of two components. The SW component is close to the midpoint of the radio source and is the correct identification.
0041-224 The 5 GHz VLA map reveals a compact component that is well off center and slightly north of the symmetry axis of the double source. Our (poor seeing) CCD images fail to reveal an object at the location of this component or anywhere else along the source axis. Our K image, however, does reveal a very red galaxy along the source axis but not coincident with the compact radio component. We believe that this red galaxy is the correct identification and that the compact radio component is most likely to be unrelated. We present both the r and K images for this source to help the reader identify the field.
0045-255 This source is identified with the starburst galaxy NGC 253; no chart is included.
0048-233 This source is identified with a bright galaxy that lies only ~10" north of a bright star. The CCD image was taken through clouds.
0052-241 The identification is quite faint and does not appear clearly in the chart shown in Figure 1. Strong Ly_alpha emission (see Paper IV) confirms that this is the correct identification.
0102-256 The identification of this source is uncertain. The radio source is unresolved, and its position is 2" east of the galaxy marked. The positional disagreement is larger than the +-1.5" that we used as the nominal acceptance criterion.
0112-219 This source was not observed with the VLA, and we are unable to identify it on the basis of the MRC position. We have not included a finding chart.
0113-245 We are unable to identify the central component of the source in our 5 GHz maps. CCD images taken with the 2.5 and 1.0 m telescopes fail to reveal any object at the location of the most plausible candidate for the central component. The structure of the 5 GHz map suggests a larger source, and this is reinforced by a 1400 MHz map (see Paper II). It is unclear if the larger component is related, as no optical counterpart appears near its midpoint. In Figure 1 we show a sky survey image with the four components marked. The field of view of this image is 340" x 340"
0115-261 This source is identified with a moderately faint galaxy located 15.5"E and 10.5"N of a much brighter galaxy. This source was incorrectly identified with the brighter galaxy by Ekers et al. (1989), and thus the source should not be part of their optical magnitude limited sample.
0122-255 The central component of this triple source is coincident with the stellar object at the center of the chart in Figure 1. Spectra obtained by us with the CTIO 4 m shows this object to be a star. We detect no other potential identifications for this source.
0127-276 Our 6 cm map reveals a single resolved component located 6"E and 2"S of the marked identification. Long-slit spectra obtained with the CTIO 4 m (Paper IV) reveals strong spatially extended [O III] lambda 5007,4959 emission at the location of the identification and the radio source. We are confident that we have the correct identification and suspect that we are missing the western lobe of the source in our map.
0149-260 The identification of this source is uncertain. The 5 GHz map reveals two sources, the eastern one of which is identified with the galaxy marked A in Figure 1. The other source could be identified with either of the two objects marked as B1 and B2, although we believe that B1 is the most likely identification.
0203-209 There are three faint galaxies near the center of the field shown in Figure 1. The central galaxy is the identification for the triple source (see McCarthy et al. 1990).
0211-258 There is a compact group of galaxies near the center of this double source. We believe that the brightest galaxy in the group is the correct identification.
0221-285 The identification for this double source is uncertain. The presence of a star 4"W and 4"S of the midpoint interferes with the imaging. The faint object marked in Figure 1 lies along the radio axis but is 3.5" from the midpoint. No other potential identifications are visible in our deep CCD images.
0226-284 Our 5 GHz maps reveal this to be two sources, both of which are identified with bright cluster galaxies. The identifications, noted as 0226-284A and 0226-284B, are both shown in Figure 1. Source 0226-284B may fall below our 408 MHz flux density limit of 950 mJy.
0242-221 This source is not identified on our CCD images, but our deep K image shows a faint galaxy within 2" of the position of the compact radio source. The position given in Table 2 is derived from the K image.
0251-273 This narrow-lined galaxy has the highest redshift in our sample (z=3.16). Our r and narrowband Lye images reveal no significant structure, and our K images also show the object to be compact.
0255-247 The structure of this source as revealed by our 6 cm map suggests that we may be seeing only one component of a larger double source. Our CCD images reveal no potential identification at the location of the radio component seen in our map.
0256-236 The source is a low surface brightness 46" double, and it was resolved out in our 5 GHz observations. We do not have a CCD image of this field, and we are unable to identify the source on the digitized sky survey.
0259-252A,B We are unable to identify this source or even decide for certain if it is one or two sources. Our 5 GHz map is quite poor and suggests either a very large source (size>360") or two sources. Our 1400 MHz map reveals both components but is ambiguous as to whether it is one or two sources. We have obtained images at the positions of both components and near the midpoint with the 1.0 m telescope and fail to find any plausible candidate identifications for either the one or two source scenarios. We reproduce a 340" x 340" chart from the digitized sky survey with the two components marked.
0309-260 The source is a very low surface brightness double, and the identification is also of very low surface brightness and is not easily visible in the chart shown in Figure 1.
0312-271 The source is complex and is composed of two or more double sources. No plausible identifications for various assignments of the components to two or more sources are seen in our CCD images obtained with the 1.0 m telescope.
0315-205 The identification for this source is diffuse and barely visible in the r-band, although it is easily seen at H. We reproduce the r image here but give the position based on astrometry from the H image.
0316-257 This is the second highest redshift in our sample and the galaxy has a complex morphology. The western component is the correct identification for the small double source (see McCarthy et al. 1990).
0327-261 The source is complex and is composed of two or more sources.
0349-278 This is a well-known identification and optical spectra reveal strong emission lines extended over many arcseconds (e.g., Danziger et al. 1984).
0353-207 We are unable to identify this unresolved steep spectrum source on our CCD images obtained with the 2.5 m telescope. We do not have a K-band image.
0357-264 We have not succeeded in identifying this source. The only image that we have of this field is a 600 s exposure with the 1.0 m telescope. Deeper imaging is required.
0422-249 The identification for this source is faint and diffuse in the optical and we do not convincingly detect it in our r image. The identification is well detected at K, and we reproduce both our r and K images in Figure 1.
0428-236 This source is not identified on our CCD images obtained with the 1.0 m telescope.
0428-281 The correct identification is the northwesternmost object of the three at the center of the field.
0431-250 We are unable to identify this triple source on our r-band CCD images obtained with the 2.5 m telescope.
0436-203 We have no CCD images of this source. For completeness we include the sky survey chart with the VLA position marked.
0442-289 We have no CCD images of this source, but for completeness we include the sky survey chart with the VLA position marked.
0457-235 The identification is 4"W and 5"S of the bright star near the field center. The identification consists of two components, one of which is coincident with the central component of the radio source, the other with the NE radio lobe. The NE component is seen more clearly in the g image than in the r image shown in Figure 1.
0541-288 There are two possible identifications for this source, the object marked and the object located 4"W and 3"N of the center. Our K images show the SE object to be redder and is thus more likely the correct identification.
0543-265 The correct identification is the easternmost object of the pair at field center.
0551-226 The correct identification is 1.5"E and 0.5"N of a star and is seen more clearly at K.
0552-249 The correct identification is 1.9"W and 3.3"N of the star near the field center.
0557-235 The midpoint of this double source is only 4" from a bright star. We are able to identify it only at K due to the scattered light from the star at r.
0614-295 We do not have an r image of this source but have identified it on the basis of a K-band image, shown in Figure 1.
0946-237 Our 5 GHz map reveals two sources, only one of which is strong enough to remain in the sample. It is identified with the southernmost of the two objects at the center of the field.
0946-262 The identification for this double source is 1.5"W and 2"N of the southernmost of the pair of stars near the center of the K image shown in Figure 1.
0947-217 We are unable to identify this source. Our 5 GHz map is quite poor and reveals three components, one of which may or may not be part of the source. Our 1400 MHz map shows the source to be a double. The positions of these two components are shown on the chart in Figure 1. Neither our r- nor our K-band images show plausible candidates for the identification.
0947-249 Our 5 GHz map reveals two sources, one of which is strong enough to remain in the sample; it is identified with a faint galaxy. The counterpart of the other source is not detected in our CCD image.
0955-283 The correct identification is the northwest component of the double object at the center of the field.
0958-227 There are two possible identifications for this compact source. The southeastern of the two objects near the field center is the more likely one (and is marked) but the northwestern one cannot be ruled out.
1006-286 The northeastern of the two objects at the field center is the correct identification for this small double source.
1014-278 We are unable to identify this unresolved source in either our deep r- or K-band images, setting upper limits of r > 24 and K > 19.
1021-217 There is a z=2.4 field galaxy 14" east of the radio source, marked on the chart with an F.
1023-226 Our 5 GHz map reveals both a double and a compact source. The double source is identified with the galaxy at the field center. The compact source is too weak for inclusion in our sample and lies close to a bright star.
1023-243 This small double source is not identified in our deep r and i images obtained with the 2.5 m telescope. The identification is, however, clearly seen in our J. H. and K images. We show the H-band image in Figure 1.
1027-225 There are two plausible identifications for this 16" double source. Both of the potential identifications are marked with ticks in Figure 1.
1034-265 This source lies 2.4"E and 0.7"S of the apparently stellar object shown at the center of the chart in Figure 1. Spectroscopy of this object by Hunstead & Kapahi with the AAT confirms that it is a star. We are unable to identify the source.
1040-285 The identification is northeast of the star near the center of the field. We present our J image in Figure 1 since the contrast against the nearby star is best in this image.
1048-211 We are unable to identify this unresolved source in either our deep r- or K-band images, setting upper limits of r > 24 and K > 19.
1051-274 There are two possible identifications along the source axis. The r image shows a faint object along the radio axis, while the K image reveals a very red object also along the axis, but further from the midpoint. We show both images in Figure 1 and give the positions for both the r- and K-based candidate identifications in Table 2. The candidate K-band identification is marked with a pair of small tick marks in the center of the chart.
1107-272 We are unable to identify this source in large part because of the presence of strong scattered light from a bright star south of the radio position.
1108-212 The identification for this triple source appears to be a galaxy ~15" from a bright star.
1117-217 This double source is identified with a galaxy in our K-band images. It is not seen in our (low quality) r-band image. Our K image is shown in the chart in Figure 1.
1132-258 This source was identified with a stellar object. Spectroscopy with the AAT showed this object to be a star. The positional coincidence between the radio position and the star is such that we have not attempted to image this source to seek a fainter identification.
1136-211 The correct identification is the northwesternmost of the three objects at the center of the field.
1137-257 The identification for this source is uncertain. The object marked in Figure 1 lies 4" east of the compact radio source.
1138-262 The identification for this bent triple source is highly complex. The image shown is the sum of several r images for a total of more than 6000 s of integration.
1145-248 There are two possible identifications for this small triple source. The northern object is closer to the midpoint (and possible core) of the source, while the southern object is brighter. We suspect that the northern component is the correct identification, and it is marked on the chart in Figure 1.
1210-290 Our deep r and i images fail to reveal an identification for this 5" double source. Our K-band images, however, clearly reveal the identification and a very red companion object. We show both our r and K images to help the reader recognize the field.
1219-264 The identification of this large triple source is a very diffuse and low surface brightness galaxy.
1239-256 The identification for this source is faint and diffuse. Figure 1 shows an I-band image; the identification has I = 23.
1245-292 The identification for this source lies 2.5"E and 4"S of the star near the field center.
1255-282 The identification for this source appears stellar on our images obtained with the 1.0 m telescope. The source is a 45" double with bright bridge emission. This source may be a quasar.
1258-211 The potential identifications for this small double consist of two components aligned east to west and just to the southeast of the star near field center. Our astrometry places the radio midpoint closer to the westernmost object, and its redder color also suggests that it is the correct identification. It is possible, however, that the two optical components are extranuclear light associated with the alignment effect and that the nucleus lies between them.
1302-206 This small double source is obscured by a bright foreground galaxy.
1307-217 There are two plausible identifications for this source. The northern source is brighter and closer to the radio midpoint and possible central component and is more likely to be the correct identification.
1334-296 This source is identified with NGC 5236; no chart is included.
1343-253 The identification is the bright elliptical south of the field center.
1351-235 We have not been able to convincingly detect an identification for this double source, despite repeated efforts in both the visible and near-infrared. The identification appears to be fainter than r >24, K >19.
2028-223 This source was not observed with the VLA, and we are not able to identify it on the basis of the MRC (Large et al. 1981) position.
2036-254 The correct identification is a faint galaxy 4" east of a brighter foreground galaxy seen near the center of the chart in Figure 1.
2039-291 The identification for this double source is uncertain. There is a faint galaxy detected at both r and K lying 4" north and west of the midpoint, nominally too far to be considered a secure identification. There is some low surface brightness radio emission near the faint galaxy so we consider it as a possible, but unlikely, identification.
2044-272 There is a very faint galaxy at the position of this unresolved source, and we consider it a tentative identification.
2045-256 This source is identified with a faint galaxy that lies just south of a bright star. It is too close to the star to allow spectroscopy.
2048-272 The identification for this small double source is not visible in either our deep r- or I-band images. It is clearly seen in our deep K image, and optical spectroscopy has confirmed it to be the correct identification.
2057-286 The correct identification is the southernmost of the two objects near the field center.
2058-237 The identification is only marginally detected in our r-band CCD images, but it is well detected at K.
2104-290 This large double source is identified only in our deep K images.
2111-275 Our r image was taken in very poor seeing and the identification is only marginally visible. We have included a K image which shows the identification more clearly.
2116-294 We have not been able to identify this large double source. There are no galaxies brighter than r~22 within 10" of the midpoint.
2123-292 The identification of this double source lies only 35" from a very bright star and is not easily seen in the chart in Figure 1.
2131-241 The identification is a galaxy 1" northwest of a star visible at the center of the chart in Figure 1.
2247-232 The identification for this source is quite faint and is not easily seen in the reproduction of our r image in Figure 1. For clarity we have also included a K-band image. The radio galaxy is southeastern of the two galaxies appearing at the meeting of the tick marks in the K image.
2303-253 The identification of this source consists of a chain of galaxies, the southwesternmost lying closest to the radio core. A 6cm map and larger optical image of this source is given in McCarthy et al. (1991).
2304-257 We are able to identify this galaxy only at K, even though our r images are fairly deep. Both the r and K images are shown in Figure 1 to aid in the recognition of the field.
2314-211 Our 6 cm VLA map shows this to be three sources. which we designate A,B, and C. We show separate finding charts with the identifications marked for each source. Sources 2314-211A and 2314-211B do not belong in the complete sample as their 1410 MHz flux densities imply that they fall below our 408 MHz flux density limit.
2355-214 The identification for this small double source is the southwesternmost of the two objects at the center of the field.

5. SUMMARY

We have presented optical/near-IR identifications and finding charts for a large and complete sample of low-frequency selected radio galaxies. This sample is well suited to a wide range of statistical studies as well as to detailed investigation of selected subsamples. In subsequent papers in this series we will provide all of the remaining basic data that is needed to fully utilize the survey data.
We gratefully acknowledge the assistance of the support staffs of the Las Campanas and Cerro Tololo Obscrvatorics as well as that of the National Radio Astronomy Observatory. In particular, we thank M. Hernandez, P. Ugarte, and H. Terrado at CTIO, and F. Perralta, H. Olivares, and O. Duhalde at LCO. We also thank I. Thompson, D. Murphy, and A. Sivaramakrishnan for their work in the development of the CCD and near-IR cameras used in this program. P. M. was supported by a Hubble Fellowship during part of the time that this investigation took place. The research of W. v. B. was performed at IGPP/LLNL under the auspices of the US Department of Energy under contract W-7405-ENG-48. P. M. C. and V. K. gratefully acknowledge the support of the American Astronomical Society through a Chretien grant. We thank Liz Doubleday for her expert assistance in the preparation of the manuscrint.

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Table 2. Optical Positions of MRC / 1 Jy Radio Galaxies
IAUname     RA_DEC_B1950    pos z    rmag  Filt FOV Run# rmag2 F2 FOV2 Notes  Remarks
----+----1----+----2----+----3----+----4----+----5----+----6----+----7----+----8----+----9
0001-233   000129.13-232339.7  0.097   16.3   r  2    11
0001-237   000114.45-234624.5  0.315   18.7   r  2    11