3CRR Atlas:Alphanumeric Listing An Atlas of DRAGNs Alphanumeric Listing
Radio Name Radio Type Optical Type Spectrum Redshift Power Size 3C 16 R+HB Galaxy 0.405 26.55 336.4 3C 19 CD Galaxy 0.482 26.69 31.8 3C 20 CD Galaxy 0.174 26.34 135.1 3C 28 RD Galaxy 0.1971 26.06 127.0 3C 31 TTJ Galaxy 0.0173 23.92 878.4 3C 33.1 CD Galaxy 0.181 25.86 625.2 3C 33 CD Galaxy 0.0595 25.51 267.8 3C 35 CD Galaxy 0.0670 24.90 846.0 3C 42 CD Galaxy 0.395 26.52 132.1 3C 46 CD Galaxy 0.4373 26.61 733.6 3C 47 CD Quasar 0.425 26.97 342.1 3C 48 SB+? Quasar 0.367 27.10 3.8 3C 61.1 CD Galaxy 0.186 26.27 497.0 3C 66B TTJ Galaxy 0.0215 24.28 277.0 3C 67 CD Galaxy 0.3102 26.21 10.0 3C 76.1 BTJ Galaxy 0.0324 24.33 118.8 3C 79 CD N Galaxy 0.2559 26.56 294.7 3C 83.1B TTJ/NAT Galaxy 0.0179 24.15 408.9 3C 84 RD/SSC Galaxy 0.0179 24.52 454.0 3C 98 CD Galaxy 0.0306 24.87 174.3 3C 109 CD N Galaxy 0.3056 26.56 360.6 3C 123 PD Galaxy 0.2177 27.19 122.7 3C 132 CD Galaxy 0.214 26.03 65.8 3C 153 HP+HB Galaxy 0.2769 26.30 31.0 3C 171 PD N Galaxy 0.2384 26.17 109.2 3C 173.1 CD Galaxy 0.2920 26.38 220.0 3C 184.1 CD Galaxy 0.1182 25.49 342.7 3C 192 CD Galaxy 0.0598 25.10 204.1 3C 200 SB+HB Galaxy 0.458 26.65 116.9
http://www.jb.man.ac.uk/atlas/alpha.html (1 of 3) [5/26/1999 2:43:24 PM] 3CRR Atlas:Alphanumeric Listing 3C 215 R+SB Quasar 0.411 26.58 256.7 3C 219 CD Galaxy 0.1744 26.34 481.7 3C 223 CD Galaxy 0.1368 25.67 647.8 3C 234 CD N Galaxy 0.1848 26.28 300.5 3C 236 SB+HB Galaxy 0.0989 25.37 4025.6 3C 244.1 CD Galaxy 0.428 26.84 234.7 3C 249.1 HP+HB Quasar 0.311 26.27 165.1 3C 264 WP+HP Galaxy 0.0214 24.30 163.8 3C 268.3 R+HB Galaxy 0.371 26.39 7.6 3C 272.1 BTJ Galaxy 0.0040 22.71 13.9 3C 274 RD/SSC Galaxy 0.0040 24.45 64.4 3C 274.1 R?+HB Galaxy 0.422 26.74 695.1 3C 284 CD Galaxy 0.2394 26.07 566.4 3C 285 CD Galaxy 0.0794 25.09 247.2 3C 288 R+SP Galaxy 0.246 26.31 114.3 3C 293 CD/SSC Galaxy 0.04503 24.63 206.8 3C 295 CD Galaxy 0.4599 27.48 25.1 3C 296 BTJ Galaxy 0.0237 24.08 192.6 3C 299 CD Galaxy 0.367 26.44 48.8 3C 300 R?+HB Galaxy 0.270 26.36 350.6 3C 303 CD N Galaxy 0.141 25.58 101.9 3C 305 PD Galaxy 0.0410 24.65 10.1 3C 310 RD Galaxy 0.0540 25.44 291.1 3C 314.1 RD Galaxy 0.1197 25.42 382.4 3C 315 RD/SSC Galaxy 0.1083 25.55 340.0 3C 319 R+HB Galaxy 0.192 26.00 289.8 3C 321 CD Galaxy 0.096 25.32 486.4 3C 326 R+HB Galaxy 0.0885 25.44 1782.7 3C 341 CD Galaxy 0.448 26.61 361.8 3C 338 RDpec Galaxy 0.0299 24.85 64.4 3C 346 SB+HB Galaxy 0.161 25.67 40.8 3C 349 CD Galaxy 0.205 25.99 252.0 3C 351 CD Quasar 0.371 26.52 309.5 3C 381 CD Galaxy 0.1605 25.87 177.3 3C 382 CD Galaxy 0.0578 25.04 188.8
http://www.jb.man.ac.uk/atlas/alpha.html (2 of 3) [5/26/1999 2:43:24 PM] 3CRR Atlas:Alphanumeric Listing 3C 386 RD Galaxy 0.0170 24.06 93.4 3C 388 R+HB Galaxy 0.0908 25.53 77.7 3C 390.3 CD Galaxy 0.0569 25.41 229.2 3C 401 SB+HB Galaxy 0.201 26.16 67.5 3C 433 SB+HP Galaxy 0.1016 25.99 109.0 3C 436 CD Galaxy 0.2145 26.16 320.6 3C 438 RD Galaxy 0.290 26.84 83.3 3C 442A RDpec Galaxy 0.0263 24.27 290.8 3C 449 TTJ Galaxy 0.0171 23.75 482.5 3C 452 CD Galaxy 0.0811 25.78 372.9 3C 457 CD Galaxy 0.428 26.68 907.9 3C 465 PD Galaxy 0.0313 24.79 346.5 4C 11.71 HP+WP Galaxy 0.0250 24.05 417.6 4C 12.03 R+SP Galaxy 0.157 25.63 546.5 4C 14.11 CD Galaxy 0.206 25.92 330.4 4C 14.27 R+HB Galaxy 0.392 26.51 161.3 4C 35.40 WP+HP Galaxy 0.0301 24.21 492.9 4C 73.08 CD Galaxy 0.0581 24.91 965.8 A 1552 TTJ Galaxy 0.0843 25.15 238.2 DA 240 CD Galaxy 0.0350 24.64 1382.0 NGC 6251 WB+HP Galaxy 0.024 23.98 1758.0
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Last modified: 1997 March 20 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/alpha.html (3 of 3) [5/26/1999 2:43:24 PM] 3CRR Atlas:3C 16: Main Page 3C 16 B0035+130
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 12.2 0.94 II R+HB Gal 0.405 R(c) = 19.5* 78.00 26.55 336.4
Image:
Size: 76.8 × 76.8 arcsec² LUT: Logarithmic Beam: 1.25 arcsec Frequency: 1477 MHz Method: VTESS Telescope: VLA A+B Credits: Leahy & Perley (1991)
3C 16 is highly asymmetric in brightness: the northern component is only visible in this picture because of the logarithmic LUT. It qualifies as a fat double because it has no true hotspots; but the bright diffuse component at the end of the south lobe makes it unusual for this class (and it is also the most luminous fat double known). The identification does not sit, as expected, between the two lobes but is in the middle of the south lobe, between the two brighter patches (which are too diffuse to be called jets). There is no radio core, and because of the peculiar position of the identification, there is some doubt as to whether it is correct. A possible interpretation is that this is a DRAGN whose AGN has just died, and the southern hotspot has been caught in the act of expanding into the lobe, now that the jet has been cut off. Unfortunately, this explains neither the asymmetry of the lobes nor the position of the galaxy.
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Page created: 1998 Mar 12 22:27:05 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C16.html [5/26/1999 2:43:33 PM] 3CRR Atlas:3C 19: Main Page 3C 19 B0038+328
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 13.2 0.63 II CD Gal 0.482 R(c) = 19.41 6.80 26.69 31.8
Image:
Size: 11.5 × 11.5 arcsec² LUT: Logarithmic Beam: 0.15 arcsec Frequency: 1534 MHz Method: CLEAN Telescope: MERLIN/VLA Credits: Leahy (1997), G. Hill (priv comm)
Possible cluster. The cross marks the centre of the host galaxy; the size of the cross gives the uncertainty in the position. The radio core is the peak underneath the cross; close examination of this image suggests that it is extended towards the south. Probably this is caused by emission from the beginning of a jet. The radio structure is relatively small (similar in scale to the host galaxy); in other respects this is a typical classical double. This is a MERLIN MFS image including short-spacing VLA data contributed by Gary Hill.
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Page created: 1998 Mar 12 22:27:05 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C19.html [5/26/1999 2:43:35 PM] 3CRR Atlas:3C 20: Main Page 3C 20 B0040+517
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 46.8 0.66 II CD Gal 0.174 R(c) = 19* 53.10 26.34 135.1
Image:
Size: 76.8 × 76.8 arcsec² LUT: Logarithmic Beam: 1.5 arcsec Frequency: 1407 MHz Method: CLEAN Telescope: VLA A Credits: R. A. Laing (unpublished)
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Page created: 1998 Mar 12 22:27:06 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C20.html [5/26/1999 2:43:41 PM] 3CRR Atlas:3C 28: Main Page 3C 28 B0053+261
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 17.8 1.06 II RD Gal 0.1971 R(c) = 16.84 45.60 26.06 127.0
Image:
Size: 76.8 × 76.8 arcsec² LUT: Linear Beam: 1.1 arcsec Frequency: 1424 MHz Method: VTESS Telescope: VLA A+B Credits: This Atlas, Feretti et al. (1984)
3C 28 is identified with the brightest member of the double galaxy cluster Abell 115. The cluster's double structure is shown nicely in the X-ray image by Forman et al. (1981). The host galaxy is at the centre of the northern condensation. The radio structure is a prototypical "relaxed double", lacking bright compact structure in the lobes. Our image shows for the first time a very faint and narrow filament crossing the gap between the lobes, and passing (to within the uncertainties) through the position of the galaxy nucleus (marked here with a red cross). There is no sign of a break at the nucleus, nor is there a brightening that could be interpreted as a compact core. The structure could be either a pair of twin jets or a filament of the kind found between the lobes in 3C 338 and 3C 442A. 3C 28 is at the peak of the X-ray emission of its sub-cluster, and the high-resolution X-ray image of Feretti et al (1984) shows that the hot gas peaks between the two lobes and is elongated perpendicular to the radio axis. Feretti et al. show that the gas is probably a cooling flow core, with ample pressure to confine the radio lobes. It seems likely that the distorted tails of the lobes are bending to follow the pressure gradient away from the galaxy and cluster centre. The radio spectrum is very steep at high frequencies; the spectral index averages nearly 2 and reaches nearly 3 in the tails (Macklin 1983, Giovannini, Feretti & Gregorini 1987). This is not unusual for DRAGNs in cluster centres. The single-dish fluxes at 1.4 GHz and above listed on our Data Page appear to be substantially too high and may be affected by confusion with another cluster radio galaxy 4 arcmin to the NE. The depolarization wavelength of 31 cm recorded by Strom & Conway (1985) also appears to be in error. No polarization at all is detected at 21 cm, and the peak polarization of 9% at 6 cm (Giovannini et al.) is
http://www.jb.man.ac.uk/atlas/object/3C28.html (1 of 2) [5/26/1999 2:43:43 PM] 3CRR Atlas:3C 28: Main Page low enough to suggest that substantial depolarization has already set in. This would imply Rotation Measures > 200 rad/m², making the Faraday rotation of 3C 28 comperable to those of other DRAGNs in cluster centres (e.g. Taylor, Barton & Ge 1994). Our image is based on VLA A-configuration data obtained for the atlas, combined with the B-configuration data of Feretti et al (1984).
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Page created: 1998 Mar 12 22:27:06 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C28.html (2 of 2) [5/26/1999 2:43:43 PM] 3CRR Atlas:3C 31: Main Page 3C 31 B0104+321
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 18.3 0.57 I TTJ Gal 0.0173 R = 11.11 2700.00 23.92 878.4
Image:
Size: 2519.0 × 2519.0 arcsec² LUT: Logarithmic Beam: 29×52 arcsec Frequency: 608 MHz Method: CLEAN Telescope: WSRT Credits: This Atlas
NGC383; binary with NGC382 in Pisces group; First ranked member of cluster. Check out Alan Bridle's beautiful images of this object.
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Page created: 1998 Mar 12 22:27:06 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C31.html [5/26/1999 2:43:46 PM] 3CRR Atlas:3C 33.1: Main Page 3C 33.1 B0106+729
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 14.2 0.62 II CD Gal 0.181 r = 20* 238.70 25.86 625.2
Image:
Size: 127.8 × 291.6 arcsec² LUT: Logarithmic Beam: 3.0 arcsec Frequency: 1535 MHz Method: CLEAN Telescope: VLA A+B+C Credits: J. P. Leahy (unpublished)
Double galaxy. This image is rotated by 42°.
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Page created: 1998 Mar 12 22:27:06 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C33P1.html [5/26/1999 2:43:48 PM] 3CRR Atlas:3C 33: Main Page 3C 33 B0106+130
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 59.3 0.76 II CD Gal 0.0595 R = 14.80 257.00 25.51 267.8
Image:
Size: 307.2 × 307.2 arcsec² LUT: Logarithmic Beam: 4.0 arcsec Frequency: 1477 MHz Method: CLEAN Telescope: VLA B+C Credits: Leahy & Perley (1991)
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Page created: 1998 Mar 12 22:27:06 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C33.html [5/26/1999 2:43:50 PM] 3CRR Atlas:3C 35: Main Page 3C 35 B0109+492
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 11.4 0.77 II CD Gal 0.0670 V = 15.6* 750.00 24.90 869.2
Image:
Size: 2304.0 × 2304.0 arcsec² LUT: Logarithmic Beam: 13.5 arcsec Frequency: 1422 MHz Method: CLEAN Telescope: VLA CS Credits: Sandell & Leahy (1998)
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Page created: 1998 Mar 26 14:00:03 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C35.html [5/26/1999 2:43:53 PM] 3CRR Atlas:3C 42: Main Page 3C 42 B0125+287
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 13.1 0.73 II CD Gal 0.395 r = 20* 31.00 26.52 132.1
Image:
Size: 76.8 × 76.8 arcsec² LUT: Logarithmic Beam: 1.2 arcsec Frequency: 1477 MHz Method: CLEAN Telescope: VLA A Credits: Leahy & Perley (1991)
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Page created: 1998 Mar 12 22:27:06 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C42.html [5/26/1999 2:43:55 PM] 3CRR Atlas:3C 46: Main Page 3C 46 B0132+376
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 11.1 1.13 II CD Gal 0.4373 r = 19.5* 164.00 26.61 733.6
Image:
Size: 256.0 × 256.0 arcsec² LUT: Logarithmic Beam: 4.2 arcsec Frequency: 1477 MHz Method: CLEAN Telescope: VLA B+C Credits: This Atlas, P. P. Kronberg (unpublished)
The host is listed as a possible cluster member by Spinrad et al. (1985). This is one of the most distant and powerful giant radio galaxies in the LRL sample. The structure is a typical classical double. Higher resolution (but undersampled) observations by Neff, Roberts & Hutchings (1995) show that the south hotspot is double, with the more compact component leading. The core is coincident with the optical identification, marked on our image by a small red cross near the inner edge of the S lobe. Neff et al.'s near-simultaneous measurements at 6 and 20 cm show that the core has a steep spectrum. Our image was made using a combiniation of unpublished VLA data, observed in B-configuration by J. P. Leahy and in C-configuration by P. P. Kronberg.
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Page created: 1998 Mar 12 22:27:07 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C46.html [5/26/1999 2:43:57 PM] 3CRR Atlas:3C 47: Main Page 3C 47 B0133+207
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 28.8 0.98 II CD QSO 0.425 V = 18.1 77.50 26.97 342.1
Image:
Size: 76.8 × 76.8 arcsec² LUT: Logarithmic Beam: 1.0 arcsec Frequency: 1650 MHz Method: CLEAN/VTESS Telescope: VLA A+B Credits: Leahy (1996)
3C 47 was identified with a quasar by Schmidt & Matthews (1964), only a year after the first quasars were discovered. It was the first one known to have a conventional classical double radio structure; in fact the DRAGN is the brightest CD in the sky identified with a quasar. The axis defined by the jet and hotspots is significantly rotated relative to that defined by the main lobes, giving the structure an S symmetry which suggests that the jet is precessing. Because its high flux density makes observation easy, this is one of the best examples of the Laing-Garrington effect, which has been studied in detail in 3C 47 by Fernini et al. (1991); see also Leahy (1996). Superluminal motion with a speed of about 6 c has been detected in the compact core (Vermeulen et al. 1993). This is interesting in the context of unified schemes since it is one of the most lobe-dominated quasars, which suggests that it is pointed about as far off our line of sight as it is possible for a quasar to be. The observed superluminal motion nevertheless implies that it is aligned within about 20° of the line of sight, which is consistent with the very strong Laing-Garrington effect. This is an example of the sort of evidence which has led to the idea that quasars pointing at right angles from us must be seen as something else, namely radio galaxies. The faint compact peak on the south-east edge of the northern lobe has a flat spectrum, and is probably a background quasar.
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http://www.jb.man.ac.uk/atlas/object/3C47.html (1 of 2) [5/26/1999 2:43:59 PM] 3CRR Atlas:3C 47: Main Page Page created: 1998 Mar 12 22:27:07 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C47.html (2 of 2) [5/26/1999 2:43:59 PM] 3CRR Atlas:3C 48: Main Page 3C 48 B0134+329
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 60.0 0.59 I SB+? QSO 0.367 V = 16.2 0.92 27.10 3.8
Image:
Size: 0.6 × 0.5 arcsec² LUT: Linear Beam: 0.006 arcsec Frequency: 1662 MHz Method: VTESS Telescope: VLBI Credits: Wilkinson et al (1991)
3C 48 was one of the first two quasars to be discovered. It is sometimes classified as an N-galaxy because the host galaxy is relatively bright, just visible on the Palomar Sky Survey. The core is the faint compact peak at the southern end of the structure. This image does not show the full large-scale structure of 3C 48. The halo surrounding the jet is visible in our C20 image. R. C. Walker and D. Briggs have recently discovered an extremely faint component to the south of the region covered by this picture, i.e. on the "counter-jet" side, so this really is a double source.
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Page created: 1998 Mar 12 22:27:07 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C48.html [5/26/1999 2:44:01 PM] 3CRR Atlas:3C 61.1: Main Page 3C 61.1 B0210+860
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 34.0 0.77 II CD Gal 0.186 R = 18.43 186.00 26.27 497.0
Image:
Size: 256.0 × 256.0 arcsec² LUT: Logarithmic Beam: 3.7 arcsec Frequency: 1477 MHz Method: CLEAN Telescope: VLA B+C Credits: Leahy & Perley (1991)
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Page created: 1998 Mar 12 22:27:07 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C61P1.html [5/26/1999 2:44:04 PM] 3CRR Atlas:3C 66B: Main Page 3C 66B B0220+427
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 26.8 0.50 I TTJ Gal 0.0215 R(c) = 12.21 690.00 24.28 277.0
Image:
Size: 722.5 × 722.5 arcsec² LUT: Linear Beam: 12.5 arcsec Frequency: 1425 MHz Method: CLEAN Telescope: VLA C+D Credits: Hardcastle et al. (1996)
Identified with UGC 01841, the dominant member of a triple galaxy at the centre of a poor cluster. See the Other Images page for a high-resolution image of the jets in the centre.
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Page created: 1998 Mar 12 22:27:07 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C66B.html [5/26/1999 2:44:05 PM] 3CRR Atlas:3C 67: Main Page 3C 67 B0221+276
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 10.9 0.58 II CD Gal 0.3102 r = 18.5* 2.67 26.21 10.0
Image:
Size: 5.1 × 5.1 arcsec² LUT: Linear Beam: 0.065 arcsec Frequency: 4995 MHz Method: CLEAN Telescope: MERLIN Credits: Lüdke et al. (1997)
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Page created: 1998 Mar 12 22:27:07 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C67.html [5/26/1999 2:44:07 PM] 3CRR Atlas:3C 76.1: Main Page 3C 76.1 B0300+162
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 13.3 0.77 I BTJ Gal 0.0324 R(c) = 14.14 200.00 24.33 118.8
Image:
Size: 384.0 × 384.0 arcsec² LUT: Linear Beam: 4.9 arcsec Frequency: 1477 MHz Method: VTESS Telescope: VLA B+C Credits: Leahy & Perley (1991)
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Page created: 1998 Mar 12 22:27:07 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C76P1.html [5/26/1999 2:44:09 PM] 3CRR Atlas:3C 79: Main Page 3C 79 B0307+169
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 33.2 0.92 II CD N 0.2559 R(c) = 17.47 88.70 26.56 294.7
Image:
Size: 47.5 × 109.5 arcsec² LUT: Linear Beam: 1.5 arcsec Frequency: 1446 MHz Method: CLEAN Telescope: VLA A+B Credits: Spangler, Myers & Pogge (1984)
Possible cluster. This image is rotated by 10°.
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Page created: 1998 Mar 12 22:27:08 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C79.html [5/26/1999 2:44:12 PM] 3CRR Atlas:3C 83.1B: Main Page 3C 83.1B B0314+416
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 29.0 0.62 I TTJ/NAT Gal 0.0179 R(c) = 12.63 1216.00 24.15 408.9
Image:
Size: 768.0 × 768.0 arcsec² LUT: Logarithmic Beam: 12 arcsec Frequency: 1380 MHz Method: CLEAN Telescope: VLA C+D Credits: C. P. O'Dea (unpublished)
NGC1265 in the Perseus cluster. The radio tail extents much further than is visible in our main image; see the C20 image on the Icon List page, which is a detail from the 90 cm WSRT image of the Perseus cluster by G. de Bruyn (unpublished). To the SE of the head of 3C83.1B in the C20 image lies the bright compact source 3C83.1A, which is an unrelated background object.
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Page created: 1998 Mar 12 22:27:08 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C83P1B.html [5/26/1999 2:44:14 PM] 3CRR Atlas:3C 84: Main Page 3C 84 B0316+413
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 66.8 0.78 I RD/SSC Gal 0.0179 R(c) = 11.17 1350.00 24.52 454.0
Image:
Size: 1024.0 × 1024.0 arcsec² LUT: Logarithmic Beam: 21 arcsec Frequency: 1380 MHz Method: SDCLN Telescope: VLA C+D Credits: Pedlar et al. (1990)
3C 84 is is the famous radio galaxy Perseus A, identified with NGC 1275, the dominant giant elliptical galaxy in the Perseus cluster. NGC 1275 was one of the original group of six galaxies with strong nuclear emission lines studied by Seyfert (1943), which gave rise to the term Seyfert Galaxy. However NGC 1275 differs from the other five in that it is a radio-loud elliptical instead of a radio-quiet spiral, and hence it is now generally regarded as a radio galaxy rather than a Seyfert Galaxy. (Curiously, Seyfert thought that it was a spiral, partly because a spiral galaxy in the cluster is seen projected in front of NGC 1275, and makes its optical structure appear much more complicated than a normal elliptical). NGC 1275 is at the centre of a massive cooling flow visible in X-ray images of the Perseus cluster (see Richard White's Perseus Cluster page). The radio structure is complicated and particularly difficult to image well. At the very centre is an extremely bright flat-spectrum core, often imaged with VLBI (e.g. Romney et al. 1996). In our image this has been subtracted to make the extended structure more visible; its position is marked by the green cross at the centre of the red region. The latter is the steep-spectrum core (SSC) which at higher resolution is a pair of lobes with the southern one dominated by a knotty jet. On larger scales still lies the extended halo, which dominates our image. The small-scale ripples ringing the central peak are artifacts caused by the bright central core. The compact peaks at the left of the picture and to the NNW of the centre are background radio sources, while the compact feature at the western tip of the structure is the nucleus of another Persues cluster galaxy, NGC 1272. The lack of compact structure in the halo gives this object its Relaxed Double classification. In fact the halo is much larger than is visible here, essentially filling the region covered by this picture. The full extent is shown in the C20 image.
http://www.jb.man.ac.uk/atlas/object/3C84.html (1 of 2) [5/26/1999 2:44:18 PM] 3CRR Atlas:3C 84: Main Page Prev. Data Page Other images Next Search Alphanumeric List Icon List Atlas Index
Page created: 1998 Mar 12 22:27:08 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C84.html (2 of 2) [5/26/1999 2:44:18 PM] 3CRR Atlas:3C 98: Main Page 3C 98 B0356+102
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 51.4 0.78 II CD Gal 0.0306 R = 14.18 309.90 24.87 174.3
Image:
Size: 307.2 × 307.2 arcsec² LUT: Logarithmic Beam: 3.7 arcsec Frequency: 4860 MHz Method: VTESS Telescope: VLA C+D Credits: A. H. Bridle (unpublished)
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Page created: 1998 Mar 12 22:27:08 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C98.html [5/26/1999 2:44:20 PM] 3CRR Atlas:3C 109: Main Page 3C 109 B0410+110
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 23.5 0.85 II CD N 0.3056 R(c) = 16.91 97.32 26.56 360.6
Image:
Size: 45.5 × 130.5 arcsec² LUT: Logarithmic Beam: 1.5 arcsec Frequency: 1446 MHz Method: CLEAN Telescope: VLA A+B Credits: Giovaninni et al. (1994)
This image is rotated by 51°. The Other Images page has a high-resolution 5 GHz image.
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Page created: 1998 Mar 12 22:27:08 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C109.html [5/26/1999 2:44:22 PM] 3CRR Atlas:3C 123: Main Page 3C 123 B0433+295
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 206.0 0.70 II PD Gal 0.2177 R(c) = 18.94 42.70 27.19 127.5
Image:
Size: 72.6 × 57.0 arcsec² LUT: Logarithmic Beam: 1.15 arcsec Frequency: 1413 MHz Method: CLEAN Telescope: VLA A Credits: R. A. Laing (unpublished)
3C 123 lies at galactic latitude -12. It is either heavily obscured or unusually faint for a radio galaxy. It is listed as a cluster member by Spinrad et al (1985). The DRAGN has a plumed double structure, with compact hotspots well aligned across the nucleus on the inside of more diffuse plumes. The northern hotspot is relatively weak and in our image is not as bright as the diffuse maximum at the bend of the bright ridge which dominates the northern lobe. However higher resolution observations by R. A. Laing, (reproduced by Cox, Gull & Scheuer 1991), clearly show that this hotspot is the highest-brightness feature. Cox et al. interpret the Z-symmetry as clear evidence for the precession of the jet axis. For such a bright source, with such unusual structure, 3C 123 has been remarkably little studied, perhaps because of the optical obscuration. In our image one can just see some weak stripes across the radio emission at about PA 100°; these are artifacts.
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Page created: 1998 Mar 12 22:27:08 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C123.html [5/26/1999 2:44:24 PM] 3CRR Atlas:3C 132: Main Page 3C 132 B0453+227
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 14.9 0.68 II CD Gal 0.214 V = 19* 24.20 26.03 71.4
Image:
Size: 20.5 × 20.5 arcsec² LUT: Logarithmic Beam: 0.33 arcsec Frequency: 4860 MHz Method: CLEAN Telescope: VLA A+B Credits: J. P. Leahy (unpublished)
Listed as a cluster member by Spinrad et al. (1985) 3C 132 is a good example of a DRAGN with "bottleneck" lobes; that is, the hotspots and the high-brightness emission behind them projects out of much more diffuse bridges. There are several other examples of this sort of structure in the Atlas, for instance 3C 184.1. There is very faint emission to the east of the SE lobe, visible in the C20 image. An earlier VLA snapshot image was given by Neff, Roberts & Hutchings (1995).
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Page created: 1998 Mar 12 22:27:08 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C132.html [5/26/1999 2:44:28 PM] 3CRR Atlas:3C 153: Main Page 3C 153 B0605+480
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 16.7 0.66 II HP+HB Gal 0.2769 V = 18.5* 9.09 26.30 31.7
Image:
Size: 11.5 × 11.5 arcsec² LUT: Logarithmic Beam: 0.15 arcsec Frequency: 1534 MHz Method: CLEAN/VTESS Telescope: MERLIN/VLA Credits: Leahy (1997), R. A. Laing (priv comm)
In a distant cluster. The northern hotspot is almost in the centre of its lobe, making it one of the most "recessed" hotspots in the Atlas sample. In the southern lobe, as well as the prominent hotspot at the tip, there is a low-contrast compact feature near the northeastern (inner) edge of the lobe, visible here as a yellowish peak. This feature is more prominent in a 6-cm image (R. A. Laing, priv. comm.), i.e. its spectrum is flatter than the surrounding lobe. The small red cross gives the position of the identification and its size gives the nominal uncertainty; but there may be a larger systematic uncertainty in aligning the radio and optical coordinate systems. The faint peak just north of the cross is the most likely candidate for a radio core. An alternative possibility is the very faint (0.5 mJy) peak in the centre of the "gap" between the two lobes, about 0.5 arcsec from the nominal optical position. Neither of these components has a particularly flat spectrum. The other compact features between the lobes suggest there is at least one jet. If the core is the component nearest the optical position, the jet is one-sided, consisting of three faint knots and directed towards the northern hotspot. The other interpretation would give a two-sided jet with the northern hotspot symmetric across the core from the compact feature in the southern lobe. McCarthy, Spinrad & van Breugel (1995) found extended H alpha +[N II] emission along the radio axis, suggesting that the peculiar structure of the northern lobe may be caused by a jet-cloud interaction.
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Page created: 1998 Mar 12 22:27:09 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C153.html [5/26/1999 2:44:30 PM] 3CRR Atlas:3C 171: Main Page 3C 171 B0651+542
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 16.7 0.66 I PD N 0.2384 R(c) = 17.94 34.40 26.17 109.2
Image:
Size: 49.2 × 40.4 arcsec² LUT: Logarithmic Beam: 1.3 arcsec Frequency: 1441 MHz Method: CLEAN Telescope: VLA A R. A. Laing (unpublished), Heckman, Credits: van Breugel and Miley (1984)
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Page created: 1998 Mar 12 22:27:09 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C171.html [5/26/1999 2:44:32 PM] 3CRR Atlas:3C 173.1: Main Page 3C 173.1 B0702+749
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 16.8 0.88 II CD Gal 0.2920 R(c) = 17.50 61.00 26.38 220.0
Image:
Size: 76.8 × 76.8 arcsec² LUT: Logarithmic Beam: 1.1 arcsec Frequency: 1477 MHz Method: CLEAN Telescope: VLA A+B Credits: Leahy & Perley (1991)
In cluster
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Page created: 1998 Mar 12 22:27:09 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C173P1.html [5/26/1999 2:44:34 PM] 3CRR Atlas:3C 184.1: Main Page 3C 184.1 B0734+805
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 14.2 0.68 II CD Gal 0.1182 R = 17.21 182.00 25.49 342.7
Image:
Size: 307.2 × 307.2 arcsec² LUT: Logarithmic Beam: 4.3 arcsec Frequency: 1477 MHz Method: CLEAN Telescope: VLA B+C Credits: Leahy & Perley (1991)
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Page created: 1998 Mar 12 22:27:09 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C184P1.html [5/26/1999 2:44:36 PM] 3CRR Atlas:3C 192: Main Page 3C 192 B0802+243
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 23.0 0.79 II CD Gal 0.0598 R = 15.20 200.50 25.10 209.9
Image:
Size: 230.0 × 256.0 arcsec² LUT: Logarithmic Beam: 3.9 arcsec Frequency: 1411 MHz Method: CLEAN Telescope: VLA B+C R. A. Laing, published in Baum et al Credits: (1988)
In cluster
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Page created: 1998 Mar 12 22:27:09 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C192.html [5/26/1999 2:44:38 PM] 3CRR Atlas:3C 200: Main Page 3C 200 B0824+294
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 12.3 0.84 II SB+HB Gal 0.458 R(c) = 19* 25.60 26.65 116.9
Image:
Size: 25.6 × 20.1 arcsec² LUT: Logarithmic Beam: 0.33 arcsec Frequency: 4860 MHz Method: CLEAN Telescope: VLA A Credits: D. A. Clarke and J. O. Burns, (unpublished)
The striping parallel to the jet is an artifact. There is more faint emission than is visible in this image, seen better in the C20 image. Yet more shows up in the very low resolution map by Garrington et al. (1991).
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Page created: 1998 Mar 12 22:27:09 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C200.html [5/26/1999 2:44:42 PM] 3CRR Atlas:3C 215: Main Page 3C 215 B0903+169
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 12.4 1.06 I R+SB QSO 0.411 V = 18.27 59.10 26.58 256.7
Image:
Size: 65.0 × 50.6 arcsec² LUT: Logarithmic Beam: 0.90 arcsec Frequency: 4860 MHz Method: CLEAN Telescope: VLA A+B Credits: Bridle et al. (1994)
Another version of this image is on Alan Bridle's 3C 215 Page.
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Page created: 1998 Mar 12 22:27:10 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C215.html [5/26/1999 2:44:44 PM] 3CRR Atlas:3C 219: Main Page 3C 219 B0917+458
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 44.9 0.81 II CD Gal 0.1744 R = 16.20 190.40 26.34 485.3
Image:
Size: 192.0 × 153.0 arcsec² LUT: Logarithmic Beam: 1.4 arcsec Frequency: 1519 MHz Method: CLEAN Telescope: VLA A+B Credits: Clarke et al. (1992)
In Zwicky cluster ZC 0917.9+4548. First ranked member. This image is a stack of the 22 and 18 cm images made by Clarke et al. Other images of this object (including high-resolution pictures of the jet) can be found on Alan Bridle's 3C219 page.
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Page created: 1998 Mar 12 22:27:10 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C219.html [5/26/1999 2:44:47 PM] 3CRR Atlas:3C 223: Main Page 3C 223 B0936+361
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 16.0 0.74 II CD Gal 0.1368 R(c) = 16.37 306.00 25.67 647.8
Image:
Size: 307.2 × 307.2 arcsec² LUT: Logarithmic Beam: 4.1 arcsec Frequency: 1477 MHz Method: CLEAN Telescope: VLA B+C Credits: Leahy & Perley (1991)
In cluster
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Page created: 1998 Mar 12 22:27:10 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C223.html [5/26/1999 2:44:49 PM] 3CRR Atlas:3C 234: Main Page 3C 234 B0958+290
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 34.2 0.86 II CD N 0.1848 R = 17.24 113.00 26.28 300.5
Image:
Size: 256.0 × 256.0 arcsec² LUT: Logarithmic Beam: 5.0 arcsec Frequency: 1411 MHz Method: CLEAN Telescope: VLA B+C Credits: Leahy, Pooley & Riley (1986)
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Page created: 1998 Mar 12 22:27:10 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C234.html [5/26/1999 2:44:54 PM] 3CRR Atlas:3C 236: Main Page 3C 236 B1003+351
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 15.7 0.51 II SB+HB Gal 0.0989 R = 15.36 2478.00 25.37 4025.6
Image:
Size: 2304.0 × 2304.0 arcsec² LUT: Logarithmic Beam: 28×48 arcsec Frequency: 608 MHz Method: CLEAN Telescope: WSRT Credits: Mack et al. (1996)
The Other Images pages shows an image of the steep-spectrum core.
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Page created: 1998 Mar 12 22:27:10 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C236.html [5/26/1999 2:44:57 PM] 3CRR Atlas:3C 244.1: Main Page 3C 244.1 B1030+585
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 22.1 0.82 II CD Gal 0.428 V = 19* 53.00 26.84 234.7
Image:
Size: 76.8 × 58.8 arcsec² LUT: Logarithmic Beam: 1.3 arcsec Frequency: 1452 MHz Method: CLEAN Telescope: VLA A Credits: R. A. Laing (unpublished)
In cluster
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Page created: 1998 Mar 12 22:27:10 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C244P1.html [5/26/1999 2:45:00 PM] 3CRR Atlas:3C 249.1: Main Page 3C 249.1 B1100+772
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 11.7 0.81 II HP+HB QSO 0.311 V = 15.72 46.30 26.27 173.3
Image:
Size: 48.9 × 72.6 arcsec² LUT: Logarithmic Beam: 1.15 arcsec Frequency: 1417 MHz Method: CLEAN Telescope: VLA A Credits: R. A. Laing (unpublished)
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Page created: 1998 Mar 12 22:27:10 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C249P1.html [5/26/1999 2:45:04 PM] 3CRR Atlas:3C 264: Main Page 3C 264 B1142+198
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 28.3 0.75 I WP+HP Gal 0.0214 R(c) = 12.16 410.00 24.30 163.8
Image:
Size: 1024.0 × 1024.0 arcsec² LUT: Logarithmic Beam: 12×36 arcsec Frequency: 1396 MHz Method: CLEAN Telescope: WSRT Credits: This Atlas
NGC 3862 in Abell 1367
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Page created: 1998 Mar 12 22:27:11 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C264.html [5/26/1999 2:45:06 PM] 3CRR Atlas:3C 268.3: Main Page 3C 268.3 B1203+645
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 11.7 0.50 II R+HB Gal 0.371 R(c) = 19.53 1.85 26.39 7.6
Image:
Size: 3.8 × 3.8 arcsec² LUT: Logarithmic Beam: 0.061 arcsec Frequency: 4995 MHz Method: CLEAN Telescope: MERLIN Credits: Lüdke et al. (1997)
In distant cluster.
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Page created: 1998 Mar 12 22:27:11 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C268P3.html [5/26/1999 2:45:08 PM] 3CRR Atlas:3C 272.1: Main Page 3C 272.1 B1222+131
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 21.1 0.60 I BTJ Gal 0.0040 R(c) = 8.11 188.50 22.71 14.5
Image:
Size: 256.0 × 256.0 arcsec² LUT: Logarithmic Beam: 3.86 arcsec Frequency: 1414 MHz Method: CLEAN Telescope: VLA A+B Credits: Laing & Bridle (1987)
Identified with the large elliptical galaxy M 84 in the core of the Virgo cluster, 3C 272.1 is the lowest-power DRAGN in our sample. Because of the malmquist bias it is much more representative of the "typical" DRAGNs than the other members of the sample. It is quite small, comperable in size with the observed optical and X-ray diameters of M 84, consistent with the general correlation between size and power in FR I DRAGNs (Fanti et al. 1987). Laing & Bridle mapped the Faraday Rotation across this object and showed that the rotation is due to gas in front of, but not mixed with, the radio lobes. This gas is visible in soft X-rays (Forman, Jones & Tucker 1984). The Other Images pages has higher resolution images of the central jets.
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Page created: 1998 Mar 12 22:27:11 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C272P1.html [5/26/1999 2:45:10 PM] 3CRR Atlas:3C 274: Main Page 3C 274 B1228+126
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 1144.5 0.79 I RD/SSC Gal 0.0040 R(c) = 8.08 836.00 24.45 64.4
Image:
Size: 2560.0 × 2560.0 arcsec² LUT: Logarithmic Beam: 45 arcsec Frequency: 1465 MHz Method: CLEAN Telescope: VLA D Credits: R. A. Perley (unpublished)
3C 274 is the famous radio source Virgo A, identified with M 87, the giant elliptical galaxy at the centre of the Virgo cluster. Virgo A is best known for its synchrotron-emitting jet. This was first noticed in an optical image by H. D. Curtis in 1918; in retrospect it was one of the first pieces of evidence for active galactic nuclei, although its significance was only gradually appreciated over the following sixty years. The jet has been observed from radio to X-ray wavelengths and imaged at high resolution with the HST and the VLA. An HST image can be accessed via the Messier Database link given above. The jet is too small to show up in our image of the large-scale structure of Virgo A. The DRAGN consists of a central Steep-Spectrum Core (SSC, in this case sometimes called the "core object" or "inner lobes") seen here in red, surrounded by a much fainter but larger halo, through which a sinuous ridge can be traced. Our classification of Virgo A as a relaxed double is based on the structure of the halo. The jet is embedded in the SSC, which has been imaged in detail by Biretta & Meisenheimer (1993). The optical and X-ray structure of the Virgo cluster are nicely shown on Richard White's Virgo Cluster page. Although in optical images M 87 is only one of several comparably bright galaxies in the cluster, it dominates the X-ray image, showing that it lies at the centre of mass of the cluster. The X-ray brightness peak is distorted on the scale of the radio halo, probably because of an interaction between radio- and X-ray emitting plasma.
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Page created: 1998 Mar 12 22:27:11 J. P. Leahy
http://www.jb.man.ac.uk/atlas/object/3C274.html (1 of 2) [5/26/1999 2:45:14 PM] 3CRR Atlas:3C 274: Main Page [email protected]
http://www.jb.man.ac.uk/atlas/object/3C274.html (2 of 2) [5/26/1999 2:45:14 PM] 3CRR Atlas:3C 274.1: Main Page 3C 274.1 B1232+216
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 18.0 0.87 II R?+HB Gal 0.422 R(c) = 19.5* 164.70 26.74 724.6
Image:
Size: 256.0 × 256.0 arcsec² LUT: Logarithmic Beam: 4.5 arcsec Frequency: 1652 MHz Method: CLEAN Telescope: VLA B+C Credits: Leahy, Pooley & Riley (1986)
The HST image of the host galaxy (de Koff et al. 1996) shows distorted isophotes, suggesting a possible dust lane. (The galaxy location is marked in our picture by a small red cross). Yates, Miller & Peacock (1989) give a larger-scale optical image which shows a number of companion galaxies, although, contrary to a note by de Koff et al, the local galaxy density is probably not high enough to qualify as a cluster. Consistent with this, there is no sign of Faraday rotation from any intra-cluster gas (Leahy et al. 1986). This giant radio galaxy has been classified as R?+HB because the peak at the end of the south-western lobe appears to be too large to count as a genuine hotspot, thus the SW lobe is apparently relaxed. However, it is possible that a higher-resolution image would reveal a marginal hotspot (hence the question mark).
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Page created: 1998 Mar 12 22:27:11 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C274P1.html [5/26/1999 2:45:17 PM] 3CRR Atlas:3C 284: Main Page 3C 284 B1308+277
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 12.3 0.95 II CD Gal 0.2394 R(c) = 17.41 178.50 26.07 568.0
Image:
Size: 256.0 × 256.0 arcsec² LUT: Logarithmic Beam: 5.0 arcsec Frequency: 1527 MHz Method: CLEAN Telescope: VLA B+C Credits: Leahy, Pooley & Riley (1986)
The host galaxy is in a moderately rich cluster (McCarthy, Spinrad & van Breugel 1995). The HST image (de Koff et al 1996) suggests a dust lane, and there are tails to the NE and SW (all within the central 3 arcsec). McCarthy et al. found a region of emission-line gas, unassociated with any galaxy, about 40 arcsec (130 kpc) from the nucleus, on the southern edge of the SE lobe. This is a candidate case of jet-induced star formation. Although not very clear with our logarithmic LUT, there is a weak but compact hotspot at the tip of the NW lobe.
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Page created: 1998 Mar 12 22:27:11 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C284.html [5/26/1999 2:45:20 PM] 3CRR Atlas:3C 285: Main Page 3C 285 B1319+428
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 12.3 0.95 II CD Gal 0.0794 R(c) = 15.47 183.70 25.09 247.2
Image:
Size: 256.0 × 256.0 arcsec² LUT: Linear Beam: 5.5 arcsec Frequency: 1530 MHz Method: CLEAN Telescope: VLA B+C Credits: Leahy, Pooley & Riley (1986)
The host galaxy of 3C 285 is a distorted elliptical, the brightest member of a group (e.g. Baum et al. 1988). The centre of the galaxy is marked by a red cross in our picture. Its outer structure is S-shaped, suggestive of tidal tails caused by interaction with a companion about 40 arcsec to the north. It contains a large amount of emission-line gas (Baum et al.) which is apparently rotating about an axis in PA 81° (Baum, Heckman & van Breugel 1990). The rather irregular inner structure of the the galaxy also suggests that there is a fair amount of dust (c.f. the R- and U-band images presented by van Breugel & Dey 1993). There is no sign of Faraday rotation from any intra-group medium (Leahy et al. 1986). Tyson, Crane & Saslaw(1977) discovered very faint (B=23.6) optical emission coincident with the compact eastern hotspot, studied in more detail in Saslaw, Crane & Tyson (1978). This may be one of only a handful of hotspots still visible in the optical; unfortunately it is so faint that it has not been possible to test that the optical emission really is synchrotron radiation by looking for polarization or getting a spectrum. An alternative explanation is that this is a chance alignment with a faint galaxy. Tyson et al. also drew attention to a brighter object (B=20.9) in the middle of the eastern lobe, which they christened 3C 285/09.6. They found it to be probably polarized (9±5%) and speculated that it might be a background quasar. However, when Baum et al (1988) took a narrow-band image to isolate H-alpha at the redshift of 3C 285, /09.6 showed up as well, showing that it is at the same distance. In their detailed study, van Breugel & Dey argue convincingly that 3C 285/09.6 is a starburst, and speculate that it is a case of jet-induced star formation. The radio structure of 3C 285 is just on the "classical" side of the divide between classical and relaxed doubles. In particular the peak in the western lobe barely counts as a hotspot, while even the eastern
http://www.jb.man.ac.uk/atlas/object/3C285.html (1 of 2) [5/26/1999 2:45:22 PM] 3CRR Atlas:3C 285: Main Page hotspot is very weak compared to most hotspots in classical doubles. The lobes are very "fat" (best seen on the C20 image), and tail off to the south, away from the companion galaxy to the north. There is a jet in the eastern lobe, which in van Breugel & Dey's high-resolution image (on our Other Images page) breaks up into a series of four knots, the last and brightest of which marks a sharp bent towards the hotspot. A single very faint knot on the counterjet side (invisible on some browsers) is probably part of a counter-jet. Our image is a combination of the 1.4 and 1.6 GHz images of Leahy et al (1986).
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Page created: 1998 Mar 12 22:27:12 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C285.html (2 of 2) [5/26/1999 2:45:22 PM] 3CRR Atlas:3C 288: Main Page 3C 288 B1336+391
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 20.6 0.85 I R+SP Gal 0.246 V = 18.3* 36.20 26.31 117.3
Image:
Size: 38.4 × 38.4 arcsec² LUT: Linear Beam: 0.60 arcsec Frequency: 4885 MHz Method: CLEAN Telescope: VLA A Credits: Bridle et al. (1989)
Possibly dominant galaxy in cluster. 3C 288 has faint extensions to the north and south, invisible in this image but shown clearly in our C20 image. See also the higher-resolution 8-GHz image on Alan Bridle's 3C 288 page.
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Page created: 1998 Mar 12 22:27:12 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C288.html [5/26/1999 2:45:25 PM] 3CRR Atlas:3C 293: Main Page 3C 293 B1350+316
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 13.8 0.45 II CD/SSC Gal 0.04503 R = 13.72 256.00 24.63 206.8
Image:
Size: 256.0 × 256.0 arcsec² LUT: Logarithmic Beam: 7.6 arcsec Frequency: 1524 MHz Method: CLEAN Telescope: VLA B+C Credits: Leahy, Pooley & Riley (1986)
Identified with the disturbed galaxy UGC 08782. Very unusually for a radio galaxy, this has a well defined gaseous disk, detected as a prominent dust lane, via neutral hydrogen absorption (Baan & Haschick 1981), and in optical emission lines (van Breugel et al. 1984). Like 3C 305, this is an excellent candidate for a recent merger between a spiral and an elliptical. The galaxy is apparently interacting with a faint companion, but is otherwise relatively isolated. A radio image with higher resolution and sensitivity than ours is given by Bridle, Fomalont & Cornwall (1981), but unfortunately is no longer available in digital form. Although the outer structure is formally a classical double, the luminosity of 3C 293 is well below the FR break, and it differs from typical CDs in several respects. Most obviously, the central component is a kpc-sized steep-spectrum core, with a curious "double double structure"; see our image of the SSC on the Other Images page. In early radio maps (e.g. Argue, Riley & Pooley 1978) the large-scale structure appeared to be one-sided, with only the large NW hotspot detected. While the ratio of flux density between the two lobes is unusually high (about 4.4), the apparent one-sidedness was mainly due to the difficulty of detecting any extended emission in the presence of the bright SSC. The 'bridge' emission is brighter close to the nucleus and connects directly with it, rather than distorting or fading near the nucleus as in other classical doubles. Our "bridge" emission is superimposed on a fainter bridge visible in Bridle et al.'s map, and they suggest that the brighter component actually comes from a disrupted jet. The steep-spectrum core has attracted a lot of attention, partly because it is interacting directly with the gas disk. Henriksen, Vallée & Bridle (1981) have suggested that the Z-shaped distortion of the SSC is due to the response of twin jets to the pressure gradient in the disk. Since the pressure is a maximum in the disk plane, the pressure gradient is perpendicular to the disk. The projected disk major axis is at PA
http://www.jb.man.ac.uk/atlas/object/3C293.html (1 of 2) [5/26/1999 2:45:29 PM] 3CRR Atlas:3C 293: Main Page 65° so the inner axis of the SSC (PA 90°), presumably that of the jets, is misaligned with the pressure gradient. As a result, buoyancy forces bend the jets towards the disk axis, or "refract" them, as Henriksen et al. put it. The irregular structure of the SSC, with a pair of compact edge-brightened inner lobes, then larger and fainter intermediate lobes, means that the smooth bending envisaged by Henriksen et al. was too simple, but the idea that buoyancy forces are responsible for the symmetry is very plausible. There is a compact flat-spectrum core at the inner edge of the western lobe of the SSC (van Breugel et al 1984, Akujor et al. 1996). The depolarization asymmetry in the SSC (Akujor et al.) suggests that the eastern component is on the near side, but it is possible that the asymmetry arises because the western lobe is much closer to the nucleus, rather than through orientation effects. In their 5 GHz MERLIN map of the SSC, Akujor et al. detect a jet running from the core to the "hotspot" in the eastern lobe, which again suggests that that is the near side; although there is also a possible counter-jet.
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Page created: 1998 Mar 12 22:27:12 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C293.html (2 of 2) [5/26/1999 2:45:29 PM] 3CRR Atlas:3C 295: Main Page 3C 295 B1409+524
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 91.0 0.63 II CD Gal 0.4599 R(c) = 18.92 5.80 27.48 26.5
Image:
Size: 15.4 × 15.4 arcsec² LUT: Logarithmic Beam: 0.20 arcsec Frequency: 8711 MHz Method: CLEAN Telescope: VLA A Credits: Perley & Taylor (1991)
3C 295 is the most powerful DRAGN in our sample, only slightly less luminous than Cygnus A. It is identified with the central cD galaxy in the rich cluster 1410+5226, usually known as the 3C 295 cluster. Henry & Henriksen (1986) show an X-ray image from the Einstein HRI, and argue that there is a cooling flow in the cluster. The DRAGN is quite small, about the size of the optical image of the host galaxy. It is embedded in the X-ray core of the cluster. Perley & Taylor find that the cluster gas causes extreme Faraday Rotation. The relatively "fat" SE lobe resembles that in Cyg A, in that it is marked by a bright ridge around the eastern boundary. The SE hotspot forms a resolved ridge parallel to the main axis, while the NW hotspot is very compact. There is a curious protrusion of intermediate brightness to the east of this hotspot, seen more clearly in the our supplementary high-resolution 15 GHz image on the Other Images page.
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Page created: 1998 Mar 12 22:27:12 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C295.html [5/26/1999 2:45:32 PM] 3CRR Atlas:3C 296: Main Page 3C 296 B1414+110
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 14.2 0.67 I BTJ Gal 0.0237 R = 11.43 437.00 24.08 192.6
Image:
Size: 382.5 × 384.0 arcsec² LUT: Logarithmic Beam: 4.9 arcsec Frequency: 1477 MHz Method: CLEAN/VTESS Telescope: VLA B+C Credits: Leahy & Perley (1991)
NGC 5532
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Page created: 1998 Mar 12 22:27:12 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C296.html [5/26/1999 2:45:36 PM] 3CRR Atlas:3C 299: Main Page 3C 299 B1419+419
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 12.9 0.65 II CD Gal 0.367 R(c) = 18.51 11.90 26.44 48.8
Image:
Size: 13.2 × 13.2 arcsec² LUT: Logarithmic Beam: 0.15 arcsec Frequency: 1534 MHz Method: CLEAN Telescope: MERLIN Credits: Leahy (1997)
Although listed as a cluster member by Spinrad et al. (1985), galaxy counts by Hill & Lilly (1991) show there is no significant galaxy cluster around 3C 299. 3C 299 is the most asymmetric classical DRAGN in the Atlas sample, in terms of both lobe length and lobe flux. The reason for this is apparent from the optical emission-line image of McCarthy, Spinrad & van Breugel (1995): the eastern jet has run into a high-density cloud which is visible through strong line emission. The filamentary structure of this obstructing cloud is clearly visible in the HST R-band image of de Koff et al. (1996). (Most of the emission in the hotspot region of their image is probably from H-beta+[OIII], which are redshifted into their passband for 3C 299). In the HST image, the host galaxy proper is double-peaked, either due to a dust lane across the nucleus or because this is a double galaxy. Accurate optical astrometry would locate these peaks relative to the nucleus as defined by the radio core, and so resolve this ambiguity. 3C 299 is also the most hotspot-dominated object in our sample, with both lobes containing well over 50 % of their flux density in very compact structure. It is particularly interesting that this is true for the faint southwestern lobe (whose partial bridge is so faint that it is only visible on our C20 image), since it is unaffected by the cloud collision. It may be significant that the second-most hotspot-dominated object in our sample, 3C 321 is also highly asymmetric in total flux density (but not in lobe length). Because of the large asymmetry and poor astrometry, the bright eastern hotspot of 3C 299 was originally believed to be a compact steep-spectrum source (CSS), coincident with the host galaxy. Many images of this DRAGN therefore only show the hotspot, which has sometimes been mistaken for a jet pointing towards the south. The western hotspot was discovered by Laing (1981a), but the true nature of 3C 299
http://www.jb.man.ac.uk/atlas/object/3C299.html (1 of 2) [5/26/1999 2:45:42 PM] 3CRR Atlas:3C 299: Main Page did not become clear until the discovery of the central component by Liu & Pooley (1991b) and van Breugel et al. (1992).
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Page created: 1998 Mar 12 22:27:12 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C299.html (2 of 2) [5/26/1999 2:45:42 PM] 3CRR Atlas:3C 300: Main Page 3C 300 B1420+198
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 19.5 0.78 II R?+HB Gal 0.270 R(c) = 18.26 104.70 26.36 359.9
Image:
Size: 256.0 × 256.0 arcsec² LUT: Logarithmic Beam: 4.4 arcsec Frequency: 1646 MHz Method: CLEAN Telescope: VLA B Credits: Leahy, Pooley & Riley (1986)
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Page created: 1998 Mar 12 22:27:12 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C300.html [5/26/1999 2:45:48 PM] 3CRR Atlas:3C 303: Main Page 3C 303 B1441+522
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 12.2 0.76 II CD N 0.141 R = 16.29 47.00 25.58 101.9
Image:
Size: 76.8 × 76.8 arcsec² LUT: Logarithmic Beam: 1.2 arcsec Frequency: 1477 MHz Method: CLEAN Telescope: VLA A+B Credits: Leahy & Perley (1991)
In cluster
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Page created: 1998 Mar 12 22:27:12 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C303.html [5/26/1999 2:45:52 PM] 3CRR Atlas:3C 305: Main Page 3C 305 B1448+634
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 17.1 0.85 I PD Gal 0.0410 V = 13.75 13.60 24.65 10.1
Image:
Size: 16.2 × 16.2 arcsec² LUT: Logarithmic Beam: 0.15 arcsec Frequency: 1534 MHz Method: CLEAN/VTESS Telescope: MERLIN/VLA Leahy (1997), Condon, Machalski & Credits: Wrobel (1997)
Identified with the peculiar galaxy IC 1065. 3C 305 is very small for an intermediate-luminosity DRAGN, being entirely confined within its host galaxy. It has a "plumed double" structure, i.e. it is dominated by compact hotspots, with the lobes forming plumes extending outwards, instead of the usual bridge stretching back towards the centre. The hotspots are sited at the ends of a pair of narrow jets, moderately asymmetric in brightness. The jets are slightly curved in an S-shape, suggesting that the ejection axis is slowly precessing anticlockwise. IC 1065 has been called both a spiral and an elliptical galaxy, but neither description is accurate. The definitive study is by Heckman et al. (1985a). Although the central regions look like a normal elliptical, apart from extensive patches of dust and line-emitting gas, there are clear spiral features in the outer parts. However long-slit spectra of the stellar absorption lines show that the stars lack the coherent motions of a true spiral disk, yet have a much larger systematic rotation than in a normal large elliptical. The galaxy appears to be an oblate spheroid, rotating around a roughly north-south axis in the sense that the eastern side is approaching, and tilted so that the northern side is furthest away. Heckman et al. argue strongly that IC 1065 is the result of a recent merger between two galaxies, at least one of which was a gas-rich spiral. Heckman et al. (1982) showed that the DRAGN is intimately connected with the emission-line nebula at the centre of IC 1065. The nebula forms a Z-shaped structure centred on the nucleus, with the bar of the Z nearly parallel to the radio jets, and the corners of the Z at about the position of the hotspots; these are also the sites of the strongest line emission. The outer arms of the Z lie just beyound the radio lobes. Spectroscopy shows that the gas is moving much faster than the stars in the galaxy, with the North-Eastern gas approaching and the South-Western gas receding from us. Almost certainly the gas
http://www.jb.man.ac.uk/atlas/object/3C305.html (1 of 2) [5/26/1999 2:45:57 PM] 3CRR Atlas:3C 305: Main Page motion has been disturbed by the impact of the radio jets. In fact, the actual line emission is thought to come from tiny condensations inside dense gas clouds which are otherwise invisible. These clouds take the impact of the jets, and are therefore responsible for confining the DRAGN to such a small size. From the gas velocities, we can tell that the NE jet is approaching and the SW jet is receding. The difference in brightness between the two jets might therefore be due to relativistic beaming. The unusual structure of 3C 305 may be related to the clumpyness of the gas in IC 1065. Although the gas clouds prevent expansion along the jet axis, the jet material can escape around the sides of the clouds to form the plumes. The anticlockwise rotation of the galaxy may stretch out the plumes to contribute to the rough rotational symmetry of the DRAGN.
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Page created: 1998 Mar 12 22:27:13 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C305.html (2 of 2) [5/26/1999 2:45:57 PM] 3CRR Atlas:3C 310: Main Page 3C 310 B1502+262
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 60.1 0.92 II RD Gal 0.0540 R = 13.92 305.00 25.44 291.1
Image:
Size: 380.0 × 380.0 arcsec² LUT: Linear Beam: 4.0 arcsec Frequency: 1446 MHz Method: CLEAN Telescope: VLA B+C Credits: van Breugel & Fomalont (1984)
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Page created: 1998 Mar 12 22:27:13 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C310.html [5/26/1999 2:45:59 PM] 3CRR Atlas:3C 314.1: Main Page 3C 314.1 B1510+709
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 11.6 0.95 I RD Gal 0.1197 V = 17* 201.00 25.42 382.4
Image:
Size: 201.6 × 174.0 arcsec² LUT: Linear Beam: 4.2 arcsec Frequency: 1477 MHz Method: VTESS Telescope: VLA B+C Credits: Leahy & Perley (1991)
In cluster
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Page created: 1998 Mar 12 22:27:13 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C314P1.html [5/26/1999 2:46:02 PM] 3CRR Atlas:3C 315: Main Page 3C 315 B1511+263
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 19.4 0.72 I RD/SSC Gal 0.1083 R = 16.16 201.40 25.55 353.0
Image:
Size: 256.0 × 256.0 arcsec² LUT: Logarithmic Beam: 5.5 arcsec Frequency: 1417 MHz Method: CLEAN Telescope: VLA B+C Credits: Leahy, Pooley & Riley (1986)
Double galaxy in cluster. There is an image of the steep-spectrum core on the Other Images page.
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Page created: 1998 Mar 12 22:27:13 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C315.html [5/26/1999 2:46:04 PM] 3CRR Atlas:3C 319: Main Page 3C 319 B1522+546
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 16.7 0.90 II R+HB Gal 0.192 R = 18.07 109.30 26.00 298.8
Image:
Size: 256.0 × 256.0 arcsec² LUT: Linear Beam: 4.0 arcsec Frequency: 1646 MHz Method: CLEAN Telescope: VLA B+C Credits: Leahy, Pooley & Riley (1986)
3C 319 is identified with the brightest galaxy of a cluster or group: a dozen or so other members are visible in the deep optical images of Crane, Tyson & Saslaw (1983) and Keel & Martini (1995). No quantitative measures of clustering are available but this is unlikely to be a rich cluster as there is no evidence for Faraday rotation caused by an intra-cluster medium: Leahy et al. (1986) found that the Rotation Measure was constant to better than ±4 rad m-2, around two orders of magnitude below the typical RM fluctuations found in central radio sources in Abell clusters; there is also negligible depolarization at wavelengths shorter than 21 cm (Leahy, unpublished, and compare the polarization maps at 18 cm in Leahy et al. and at 3.6 cm in Hardcastle et al 1997a). The depolarization wavelength of 20 cm listed by Tabara & Inoue (1980) is therefore in error. Apart from the host, three other galaxies are projected within the radio lobes, but there is no sign that either the total intensity or polarization structure of the DRAGN is affected by them, so they are probably behind the lobes. The radio structure is unusual in that although the north-east lobe has a normal hotspot at its end (seen at high resolution in the maps of Hardcastle et al), there is no sign of a hotspot or even "warmspot" at the end of the south-west lobe (which we therefore classify as relaxed). There is also no sign of a radio core. Since one of the other galaxies is projected close to the northern hotspot, it has been suggested that that is the true identification, making this a head-tail DRAGN. However, the identification with the central galaxy seems secure, based on the clear division into two lobes with a central brightness minimum (first shown by Bridle & Fomalont 1979)), and the spectral index maps (Macklin 1983, Alexander & Leahy 1987) which show that both ends of the DRAGN have relatively flat spectra, with the spectrum steepening towards the centre as in typical classical doubles.
http://www.jb.man.ac.uk/atlas/object/3C319.html (1 of 2) [5/26/1999 2:46:07 PM] 3CRR Atlas:3C 319: Main Page It has also been suggested (e.g. by Crane et al. 1983) that the northern optical object is not a galaxy, but synchrotron emission from the hotspot; however it is not exactly coincident with the hotspot and in any case a spectrum by Keel & Martini shows that almost certainly it is a galaxy.
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Page created: 1998 Mar 12 22:27:13 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C319.html (2 of 2) [5/26/1999 2:46:07 PM] 3CRR Atlas:3C 321: Main Page 3C 321 B1529+242
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 14.7 0.60 II CD Gal 0.096 R(c) = 14.16 307.00 25.32 486.4
Image:
Size: 235.2 × 244.2 arcsec² LUT: Logarithmic Beam: 1.37 arcsec Frequency: 1507 MHz Method: CLEAN Telescope: VLA A+B Credits: Baum et al (1988)
There is some very faint bridge emission, visible only on the C20 image.
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Page created: 1998 Mar 12 22:27:13 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C321.html [5/26/1999 2:46:09 PM] 3CRR Atlas:3C 326: Main Page 3C 326 B1549+202
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 22.2 0.88 II R+HB Gal 0.0885 R = 15.72 1206.00 25.44 1782.7
Image:
Size: 2048.0 × 2048.0 arcsec² LUT: Linear Beam: 14×39 arcsec Frequency: 1415 MHz Method: CLEAN Telescope: WSRT Credits: This Atlas
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Page created: 1998 Mar 12 22:27:13 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C326.html [5/26/1999 2:46:11 PM] 3CRR Atlas:3C 341: Main Page 3C 341 B1626+278
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 11.8 0.85 II CD Gal 0.448 R(c) = 19* 80.00 26.61 361.8
Image:
Size: 76.8 × 76.8 arcsec² LUT: Logarithmic Beam: 1.3 arcsec Frequency: 1477 MHz Method: CLEAN/VTESS Telescope: VLA A+B Credits: Leahy & Perley (1991)
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Page created: 1998 Mar 12 22:27:14 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C341.html [5/26/1999 2:46:12 PM] 3CRR Atlas:3C 338: Main Page 3C 338 B1626+396
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 51.1 1.19 I RDpec Gal 0.0299 R(c) = 12.00 117.00 24.85 64.4
Image:
Size: 66.0 × 127.8 arcsec² LUT: Logarithmic Beam: 1.0 arcsec Frequency: 4860? MHz Method: VTESS Telescope: VLA B+C Credits: Ge & Owen (1994)
NGC 6166 in Abell 2199 First ranked member
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Page created: 1998 Mar 12 22:27:14 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C338.html [5/26/1999 2:46:14 PM] 3CRR Atlas:3C 346: Main Page 3C 346 B1641+173
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 11.9 0.52 I SB+HB Gal 0.161 R(c) = 16.48 17.00 25.67 40.8
Image:
Size: 25.6 × 25.6 arcsec² LUT: Logarithmic Beam: 0.35 arcsec Frequency: 1534 MHz Method: CLEAN/VTESS Telescope: MERLIN/VLA Leahy (1997), Akujor & Garrington Credits: (1995).
3C 346 is dominated by the bright strong-flavour jet, and the compact core. There is a weak but definite hotspot at the edge of the western lobe. These features are seen most clearly on the high-resolution image on the "other images" page. The very "fat" lobes are only visible here thanks to the logarithmic LUT. In the C20 image, very faint extensions are visible almost at right angles to the main jet-hotspot axis, and the largest dimension is actually across this faint extension. Based on its size measured along the main axis, 3C 346 would be FR class II. Optical/UV emission from the jet was discovered by Dey & van Breugel (1994), and the HST image by de Koff et al. (1996) shows that the jet appears very similar in the optical and radio bands. About two arcsec from the core the jet appears to bend suddenly by about 65°. The point is marked by a knot about sixty times brighter than anywhere else on the jet, presumably produced by the shocks which must occur when a supersonic flow is suddenly bent. In fact, the shocks needed for a 65° bend ought to make the flow subsonic (Williams 1991) and would probably disrupt the jet; so the bend angle is probably exaggerated by forshortening. Radio polarimetry by Akujor & Garrington (1995) shows that the magnetic field in the jet is generally parallel to the axis, except for a short section just downstream from the knot where the field is transverse. The lobes show a strong Laing-Garrington effect. VLBI observations by Cotton et al. (1995) resolved the core-jet structure of the compact core, and detected the bright jet knot. The bright and sharply-curved jet, strong Laing-Garrington effect, small projected size, fat lobes, and
http://www.jb.man.ac.uk/atlas/object/3C346.html (1 of 2) [5/26/1999 2:46:17 PM] 3CRR Atlas:3C 346: Main Page unexpected faint extensions, are all consistent with this being a DRAGN seen rather close to the jet axis, so that the jet is enhanced by relativistic beaming, the lobes and jet are seen extremely forshortened, and typical faint central distortions appear in projection outside the main axis. A fly in the ointment is that there is no sign of the broad lines in the optical spectrum (e.g. Dey & van Breugel 1994) that we would expect according to unified schemes if we are looking down the throat of an AGN. It is also unlikely that a combination of beaming and projection could hide a strong hotspot on the jet side; in other suspected cases of "end-on" DRAGNs the jet-side hotspot is extremely bright (e.g. 3C 303). More likely, from a larger angle 3C 346 would resemble 3C 401. Because at high-resolution 3C 346 is dominated by the core and the nearby jet knot, it has been included in the sample of compact steep-spectrum sources studied in van Breugel et al. (1992) and earlier papers by the same team. In fact the existence of emission on scales larger than the few arcsec characteristic of true CSS objects has been known at least since Pooley & Henbest (1974), and 3C 346 cannot be considered a CSS in any meaningful sense. The faint fine-scale detail in the diffuse lobes of our high-resolution image is mainly due to a mixture of noise and artifacts produced by the core and bright jet knot. In particular, the apparent brightness minima in the lobes surrounding each of these features are probably artifacts; the dip in brightness is only about 0.5% of the peaks.
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Page created: 1998 Mar 12 22:27:14 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C346.html (2 of 2) [5/26/1999 2:46:17 PM] 3CRR Atlas:3C 349: Main Page 3C 349 B1658+471
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 14.5 0.74 II CD Gal 0.205 R(c) = 17.84 85.30 25.99 244.3
Image:
Size: 76.8 × 76.8 arcsec² LUT: Logarithmic Beam: 1.2 arcsec Frequency: 1477 MHz Method: CLEAN/VTESS Telescope: VLA A+B Credits: Leahy & Perley (1991)
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Page created: 1998 Mar 12 22:27:14 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C349.html [5/26/1999 2:46:19 PM] 3CRR Atlas:3C 351: Main Page 3C 351 B1704+608
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 14.9 0.73 II CD QSO 0.371 V = 15.28 75.00 26.52 309.5
Image:
Size: 76.8 × 76.8 arcsec² LUT: Logarithmic Beam: 1.85 arcsec Frequency: 1417 MHz Method: CLEAN Telescope: VLA A+B Leahy & Perley (1991), R. A. Laing Credits: (priv comm)
The mottling in the fainter regions is an artifact of the imaging process, caused by the very bright northern hotspots. See also the high-resolution image on Alan Bridle's 3C 351 Page.
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Page created: 1998 Mar 12 22:27:14 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C351.html [5/26/1999 2:46:21 PM] 3CRR Atlas:3C 381: Main Page 3C 381 B1832+474
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 18.1 0.81 II CD Gal 0.1605 R(c) = 16.86 74.00 25.87 177.3
Image:
Size: 80.0 × 80.0 arcsec² LUT: Logarithmic Beam: 1.25 arcsec Frequency: 1477 MHz Method: CLEAN Telescope: VLA A+B Credits: Leahy & Perley (1991)
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Page created: 1998 Mar 12 22:27:15 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C381.html [5/26/1999 2:46:23 PM] 3CRR Atlas:3C 382: Main Page 3C 382 B1833+326
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 21.7 0.59 II CD Gal 0.0578 R = 13.58 186.00 25.04 188.8
Image:
Size: 212.4 × 204.0 arcsec² LUT: Logarithmic Beam: 4.5 arcsec Frequency: 1477 MHz Method: CLEAN/VTESS Telescope: VLA B+C Credits: Leahy & Perley (1991)
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Page created: 1998 Mar 12 22:27:15 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C382.html [5/26/1999 2:46:26 PM] 3CRR Atlas:3C 386: Main Page 3C 386 B1836+171
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 26.1 0.59 I RD Gal 0.0170 V = 12.93 292.00 24.06 93.4
Image:
Size: 384.0 × 384.0 arcsec² LUT: Linear Beam: 5.8 arcsec Frequency: 1477 MHz Method: VTESS Telescope: VLA B+C Credits: Leahy & Perley (1991)
Early studies of 3C 386 were considerably confused by its apparently zero redshift (Schmidt 1965), which, combined with the relaxed structure led to the suggestion that this might be an object in our Galaxy such as a supernova remnant (Mackay 1969); it is relatively close to the galactic plane (latitude 11°). The mystery was solved when Lynds (1971) showed that there is an F7 star on the line of sight to the galaxy; the zero redshift belonged to the star. Lynds also pointed to the similarity between the diffuse structure of 3C 386 and other objects such as 3C 315. These objects are now known as relaxed doubles. 3C 386 is a typical example: its lobes contain considerable fine structure including curved filaments near the edges that may be parts of loops or shells. The compact source to the west, and a fainter one just visible to the north west, are unrelated background objects.
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Page created: 1998 Mar 12 22:27:15 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C386.html [5/26/1999 2:46:28 PM] 3CRR Atlas:3C 388: Main Page 3C 388 B1842+455
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 26.8 0.70 II R+HB Gal 0.0908 R = 14.12 51.40 25.53 77.7
Image:
Size: 76.8 × 76.8 arcsec² LUT: Logarithmic Beam: 1.32 arcsec Frequency: 1385 MHz Method: CLEAN Telescope: VLA B+C Credits: Roettiger et al. (1994)
3C 388 is identified with a cluster-dominating cD galaxy. Prestage & Peacock's (1988) correlation analysis found that the surrounding cluster was comperable in richness to an Abell cluster, although it does not appear in either the Abell or Zwicky catalogues. The cluster has been detected in X-rays (Feigelson & Berg 1983). The Faraday rotations of around 100 rad m-2 (Burns, Christiansen & Hough 1982, Roettiger et al. 1994) are comperable to those found in groups and non-cooling flow Abell clusters. The radio structure of 3C388 initially appeared to be a typical classical double (e.g. Burns, Owen & Rudnick 1978). On closer examination this description has become increasingly innappropriate. On our system the eastern lobe is classified as relaxed: there is a moderately compact "warmspot" near the centre of the lobe but its surface brightness is too low to qualify as a true hotspot. Unlike typical classical doubles, the eastern lobe is not edge-brightened. Instead, there is a diffuse "relic" lobe outside the main lobe (the latter appears orange in our image). The boundary between these two is marked by a sharp drop in brightness and increase in spectral index (Roettiger et al.); as our image shows, the outer edge of the relic lobe itself is also very sharp. The western lobe contains a curved, well-collimated jet linking the core with the bright hotspot. A tail or flare of emission extends south from the hotspot, and Roettiger et al's spectral index map shows that this region has a relatively flat spectrum; presumably this is the current outflow from the hotspot. In contrast the wing of emission to the north seems to be analogous to the eastern relic, with a steep spectrum and a much lower brightness than the main lobe emission surrounding the jet. Roettiger et al.'s high resolution 4.8 GHz image also shows a probably counter-jet (their "finger") in the eastern lobe. Roettiger et al. note that there is little depolarization asymmetry between the two lobes. Since the X-ray
http://www.jb.man.ac.uk/atlas/object/3C388.html (1 of 2) [5/26/1999 2:46:30 PM] 3CRR Atlas:3C 388: Main Page core radius is comparable to the radio size, a significant asymmetry would be expected unless the source axis is rather close to the plane of the sky. This would be consistent with the clear gap between the lobes and with the detectability of the counterjet.
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Page created: 1998 Mar 12 22:27:15 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C388.html (2 of 2) [5/26/1999 2:46:30 PM] 3CRR Atlas:3C 390.3: Main Page 3C 390.3 B1845+797
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 51.8 0.75 II CD Gal 0.0569 R = 14.64 229.00 25.41 229.2
Image:
Size: 262.5 × 262.5 arcsec² LUT: Logarithmic Beam: 2.8 arcsec Frequency: 1565 MHz Method: CLEAN/VTESS Telescope: VLA A+B+C Credits: Leahy & Perley (1995)
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Page created: 1998 Mar 12 22:27:15 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C390P3.html [5/26/1999 2:46:32 PM] 3CRR Atlas:3C 401: Main Page 3C 401 B1939+605
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 22.8 0.71 II SB+HB Gal 0.201 V = 19.1* 23.90 26.16 67.5
Image:
Size: 25.6 × 25.6 arcsec² LUT: Logarithmic Beam: 0.35 arcsec Frequency: 1534 MHz Method: CLEAN/VTESS Telescope: MERLIN/VLA Credits: J. P. Leahy (unpublished)
In cluster. A higher-resolution image is shown on the Other Images page, which shows the detailed structure of the jet. The stippling of the extended structure in that image is a mixture of noise and deconvolution artifacts.
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Page created: 1998 Mar 12 22:27:15 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C401.html [5/26/1999 2:46:34 PM] 3CRR Atlas:3C 433: Main Page 3C 433 B2121+248
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 61.3 0.75 I SB+HP Gal 0.1016 V = 15.98 68.60 25.99 114.0
Image:
Size: 80.2 × 80.2 arcsec² LUT: Linear Beam: 0.75 arcsec Frequency: 8350 MHz Method: VTESS Telescope: VLA A+B+C Credits: Black et al. (1992)
Christened `the flagpole' by Hans de Ruiter, 3C 433 is the most bizarre DRAGN in our sample, and it is identified with one of the most unusual galaxies. The host galaxy is a member of a close pair, often classified as a dumbell galaxy (e.g. Colina & Perez-Fournon 1990). The locations of both galaxies are shown by green crosses in the picture. The HST image of de Koff et al. (1996) shows complex central structure which they attribute to dust and possible star formation. HI absorption against the radio source was detected by Mirabel (1989); although the integrated optical depth is low (0.005), only a small fraction of the radio emission is close enough to the galaxy to act as a background source, implying that substantial absorption must take place near the centre. The HI shows a narrow feature with broad (700 km/s) wings. Baum et al. (1988) detected an extended emission-line nebula in the host, and a long-slit spectrum (Baum et al. 1990) showed complex kinematics, with a total velocity range similar to that seen in HI. Although the nuclear spectrum is typical of narrow-line galaxies, the near- and far-infrared colours are non-stellar (Lilly, Longair & Miller 1985, Yates & Longair 1989); the SED peaks at around 25 microns. 3C 433 also has a relatively high X-ray luminosity (Fabbiano et al. 1984); all these suggest that there is a powerful AGN in the galaxy that is obscured in the optical. The environment is sometimes described as a cluster, but it would be more accurate to say that the dumbell and a few much smaller galaxies make up a small group; consistent with this there is little Faraday depolarization. The high resolution images of Black et al. (1992) show that there are two compact components at the base of the jet, separated by about 0.5 arcsec. The optical astrometry is not good enough to determine
http://www.jb.man.ac.uk/atlas/object/3C433.html (1 of 2) [5/26/1999 2:46:40 PM] 3CRR Atlas:3C 433: Main Page which is coincident with the galaxy centre, but most likely it is the slightly brighter southern component, so that the jet is fully one-sided. Neither of the very asymmetric lobes closely resembles any other in our sample. The good collimation and knotty structure of the jet in the northern lobe are typical strong-flavour, but the magnetic field is often diagonal to the jet axis. The jet's second quarter is invisible. Diffuse emission surrounds its path, and near the end trails off to the east to form the northern lobe. Distinct ridges emanate from the jet's brightest knot and from the very end of the jet. There is a fairly compact hotspot near the centre of the northern lobe, slightly fainter than the peak of the jet. There is no obvious connection between jet and hotspot and it is not clear what is keeping the hotspot compact. The southern lobe is much brighter, although faint emission trails off to the west at about the same brightness level as the northern lobe, suggesting an X-type structure. The main part of the southern lobe is a plateau of roughly constant brightness, albeit with a lot of low-contrast structure; this suggests that in 3-D the structure must be significantly edge-brightened. The lobe has two bright peaks, close to the outer and inner edges respectively. At low resolution the outer peak is brighter, putting 3C 433 in the FR II class, consistent with its luminosity. On the other hand the inner peak contains a compact peak well aligned across the core with the jet; this is the brightest point at high resolution, and gives this lobe its "plume" classification. Just as with the tip of the northern jet, there are ridges in the lobe surrounding this peak which give the impression that the compact structure is rotating clockwise, leaving a sort of wake behind.
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Page created: 1998 Mar 12 22:27:15 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C433.html (2 of 2) [5/26/1999 2:46:40 PM] 3CRR Atlas:3C 436: Main Page 3C 436 B2141+279
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 19.4 0.86 II CD Gal 0.2145 R(c) = 17.32 108.50 26.16 320.6
Image:
Size: 138.0 × 76.8 arcsec² LUT: Logarithmic Beam: 1.1 arcsec Frequency: 1502 MHz Method: CLEAN Telescope: VLA A+B Credits: W. A. Christiansen (unpublished)
The Other Images page has a higher-resolution 5 GHz image, which shows the detailed structure of the hotspots and jet.
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Page created: 1998 Mar 12 22:27:16 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C436.html [5/26/1999 2:46:44 PM] 3CRR Atlas:3C 438: Main Page 3C 438 B2153+377
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 48.7 0.88 II RD Gal 0.290 R(c) = 17.90 23.20 26.84 83.3
Image:
Size: 23.0 × 23.0 arcsec² LUT: Linear Beam: 0.29 arcsec Frequency: 1534 MHz Method: CLEAN/VTESS Telescope: MERLIN/VLA Credits: Leahy (1997)
3C 438 is the best example known of a DRAGN with well-defined strong-flavour jets in both lobes. The prominence of these jets is perhaps related to the surprising absence of hotspots; instead, the outer regions of the lobes on both sides show a high surface brightness with small-scale fluctuations at the level of tens of percent (notice that our image is displayed with a linear LUT). The jets are very well collimated (they are best seen on our high-resolution supplementary image). The northern jet has three prominent knots, whose peaks are noticably off the jet axis. The southern jet brightens significantly from the bend about six arcsec from the core, and the jet seems to be brighter on the outside edge of the bend (this weak effect is at the limit of believability). If real, this suggests that the jet material is flowing around the bend in response to a pressure gradient, as opposed to ballistic models in which each part of the jet moves at constant velocity away from the core, so that bends indicate changes in the direction of ejection. Because of the strong depolarization, the magnetic field orientation is unknown. The faint extension to the south from the north-west lobe is best seen in our C20 image. The AGN powering 3C 438 is remarkably weak in the optical, with even narrow emission lines only just detected (Rawlings et al. 1989a). Surprisingly, 3C 438 is a relatively strong X-ray source (Feigelson & Berg 1983, Prieto 1996), but since the the host galaxy is in a cluster (Burbidge & Crowne 1979, de Koff et al. 1996) the X-rays may be from the ICM rather than the AGN. If so, this would be a massive cluster atmosphere, comperable to a rich Abell cluster. A very dense surrounding medium is also consistent with the strong depolarization. It may also explain why such a high-power DRAGN should have a relaxed double structure, which is normally found in objects with powers around the FR break. A very high
http://www.jb.man.ac.uk/atlas/object/3C438.html (1 of 2) [5/26/1999 2:46:47 PM] 3CRR Atlas:3C 438: Main Page pressure in the ambient medium will raise the lobe pressure, which in turn may lead to increased dissipation in the jets, reducing the energy flux available to power hotspots. At the same time the hotspot prominence is reduced anyway because high-pressure lobes will be relatively bright in the radio. Weak fine-scale structure is undersampled in our supplementary full-resolution image and should not be relied on. The weak striping parallel to the jets is an artifacts, but there are features in the southern lobe that are not exactly parallel to the jet and are probably real.
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Page created: 1998 Mar 12 22:27:16 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C438.html (2 of 2) [5/26/1999 2:46:47 PM] 3CRR Atlas:3C 442A: Main Page 3C 442A B2212+135
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 17.5 0.96 II RDpec Gal 0.0263 R(c) = 13.08 597.00 24.27 290.8
Image:
Size: 488.8 × 665.6 arcsec² LUT: Linear Beam: 7.5 arcsec Frequency: 1375 MHz Method: VTESS Telescope: VLA A+B+C Credits: Comins & Owen (1991)
Identified with the E galaxy NGC 7237, which is strongly interacting with its neighbour, NGC 7236. There are several compact background sources projected in and around this large DRAGN; the true core is the point source near the centre of the image, between the two filaments that cross the central gap. Apart from the core, there are no high-brightness compact features in the DRAGN, hence the classification as a relaxed double (RD). We have added the suffix "pec" for peculiar, because of the filaments. These cannot be jets, as they do not emanate from the core; at present we do not understand how such filaments are formed. This main Atlas image is a smoothed version of the original VTESS image, which is available on the "other images" page. The original shows more details but also some weak artifacts in the form of low-level stripes.
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Page created: 1998 Mar 12 22:27:16 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C442A.html [5/26/1999 2:46:49 PM] 3CRR Atlas:3C 449: Main Page 3C 449 B2229+390
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 12.5 0.58 I TTJ Gal 0.0171 R = 12.35 1500.00 23.75 482.5
Image:
Size: 2304.0 × 2304.0 arcsec² LUT: Logarithmic Beam: 30×48 arcsec Frequency: 608 MHz Method: CLEAN Telescope: WSRT Credits: This Atlas
Identified with the E galaxy UGC 12064 in the poor cluster Zw 2231.2+3732. HST images of UGC 12064 show a prominent dust lane perpendicular to the jets. At high resolution, the central region of 3C 449 is one of the classic examples of weak-flavour twin jets (Perley, Willis & Scott 1979, Corwall & Perley 1984). These jets make up the slightly fainter region between the two bright peaks in our image; at higher resolution the peaks are resolved into extended components with surface-brightness substantially less than the jets. 3C 449 is projected behind the faint HII region S 126 in our own galaxy. When displayed at high contrast, our C20 image shows faint radio emission from S 126 crosses the lower half of the DRAGN (Andernach et al. 1992).
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Page created: 1998 Mar 12 22:27:16 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C449.html [5/26/1999 2:46:51 PM] 3CRR Atlas:3C 452: Main Page 3C 452 B2243+394
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 59.3 0.78 II CD Gal 0.0811 R(c) = 15.43 278.00 25.78 381.1
Image:
Size: 317.2 × 345.8 arcsec² LUT: Logarithmic Beam: 6.0 arcsec Frequency: 1413 MHz Method: CLEAN Telescope: VLA A+C Credits: R. A. Laing (unpublished)
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Page created: 1998 Mar 12 22:27:16 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C452.html [5/26/1999 2:46:53 PM] 3CRR Atlas:3C 457: Main Page 3C 457 B2309+184
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 14.3 1.01 II CD Gal 0.428 V = 19.5* 205.00 26.68 907.9
Image:
Size: 384.0 × 384.0 arcsec² LUT: Logarithmic Beam: 5.1 arcsec Frequency: 1477 MHz Method: CLEAN Telescope: VLA B+C Credits: Leahy & Perley (1991)
This giant radio galaxy is one of the objects listed in 3C but not in 3CR, probably because it was slightly resolved in that survey. The accurate 4CT flux density is clearly above the sample limit. A faint jet is visible, entering the northern lobe. The compact source just south of the southern hotspot complex is almost certainly an unrelated background object.
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Page created: 1998 Mar 12 22:27:16 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C457.html [5/26/1999 2:46:55 PM] 3CRR Atlas:3C 465: Main Page 3C 465 B2335+267
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 41.2 0.75 I PD Gal 0.0313 R(c) = 12.52 603.00 24.79 346.5
Image:
Size: 716.8 × 716.8 arcsec² LUT: Logarithmic Beam: 5.4 arcsec Frequency: 1414 MHz Method: CLEAN Telescope: VLA A+C Credits: F. N. Owen (unpublished)
Identified with NGC 7720, the dominating D galaxy in the cluster Abell 2634. 3C 465 is the prototypical "wide-angle tail" (WAT). There are two features which distinguish it from typical twin-jet FR I's like 3C 449. The more obvious is the bending of the tails which gave the WAT class its name. A lot of work has been done to try to understand how the tails became bent. The simplest idea, that this is a less extreme version of the "wind-of-passage" bending found in twin-tails like 3C 83.1B, does not work for 3C 465, for several reasons (Leahy 1984, Eilek et al. 1984). For instance, this mechanism cannot explain why the bending is so irregular; in addition, WATs tend to be associated with central galaxies which are nearly stationary in the centres of clusters, (although in this case NGC 7720 has a line-of-sight velocity of 200 km/s relative to the cluster average). It is now believed that the tails of 3C 465 are bent by large-scale gas flows associated with the accretion of sub-clusters into the main cluster; but similar amounts of bending in other DRAGNs appear to have quite different causes. The second distinguishing feature is the structure of the jets. The jets in WATs never show the bright, smooth, "weak-flavour" structure typical of twin-jets. Instead they go straight from the initial inconspicuous and highly collimated "strong-flavour" structure into a pair of "hot spots", where they suddenly brighten, bend, and broaden into a pair of meandering tails. These bending sites are analogous to the hotspots of classical doubles in at least one sense, that they seem to mark the transition from jet to lobe and from supersonic to subsonic flow, as inferred from the much smoother brightness distribution downstream. At least for 3C 465, it is tempting to associate the hotspots with the points at which the jets emerge from a protecting interstellar medium into the flowing intra-cluster medium. This jet-hotspot-tail transition is now seen as the really important difference between 3C 465 and twin-jet DRAGNs, since the bending does not tell us much about the underlying physics. Because nobody wanted to invent a new name, "wide-angle tail" now, perversely, means a DRAGN showing this kind of
http://www.jb.man.ac.uk/atlas/object/3C465.html (1 of 2) [5/26/1999 2:46:57 PM] 3CRR Atlas:3C 465: Main Page transition, irrespective of whether it also shows "wide-angle" bending.
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Page created: 1998 Mar 12 22:27:17 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/3C465.html (2 of 2) [5/26/1999 2:46:57 PM] 3CRR Atlas:4C 11.71: Main Page 4C 11.71 B2247+113
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 11.7 0.75 I HP+WP Gal 0.0250 R(c) = 12.20 892.00 24.05 413.9
Image:
Size: 1280.0 × 1280.0 arcsec² LUT: Logarithmic Beam: 22×106 arcsec Frequency: 1415 MHz Method: CLEAN Telescope: WSRT Credits: Robertson (1981)
Identified with NGC 7385, an elliptical galaxy in the group of galaxies Zw 2247.3+1107. The centre of NGC 7385 is marked with a green cross. The unresolved source just north of 4C 11.71 is identified with NGC 7386, another galaxy in the same group. This is a prototypical head-tail galaxy. The bright head region is unresolved in the north-south direction with our very elongated beam. High-resolution observations by Hardee, Eilek & Owen (1980) show that the initial ejection axis is projected parallel to the tail. Most of the tail appears to be the extension of the south-west jet. To the north-east, there is a stubby lobe which could be interpreted as a "stalled" jet. A VLA map at intermediate resolution (Condon & Broderick 1988) shows faint emission to the north-west of the head (not resolved from the head at all in our image). This may be the tail associated with the north-east "jet". Simkin & Ekers (1979) discovered a massive H II region at the edge of the NE lobe. This may be an example of jet-induced star formation. The extensions to the east and north from the bright head are calibration artifacts.
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Page created: 1998 Mar 12 22:27:16 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/4C11P71.html [5/26/1999 2:47:00 PM] 3CRR Atlas:4C 12.03: Main Page 4C 12.03 B0007+124
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 10.9 0.87 II R+SP Gal 0.157 V = 16.5* 232.00 25.63 546.5
Image:
Size: 384.0 × 384.0 arcsec² LUT: Linear Beam: 5.0 arcsec Frequency: 1477 MHz Method: VTESS Telescope: VLA B+C Credits: Leahy & Perley (1991)
4C12.03 is on the borderline between relaxed doubles and classical doubles. There are low-contrast "warmspots" at the end of each lobe, but in the south the the lobe centre is about four times brighter than the warmspot (presumably there is a longer pathlength, so the emissivity in the two regions is similar). The host galaxy is at the centre of the structure, (marked by a tiny red dot in the picture). A slight peak in the brightness at this position is probably the core (not clearly visible here). Straddling the core to north and south are elongated structures, unresolved in width, that are probably segments of jets. It would be useful to check this interpretation with a higher-resolution image. The most remarkable feature is the pair of faint secondary lobes or wings at an angle of about 60° to the main axis. Another example of this kind of structure is 3C 315, the prototype winged DRAGN.
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Page created: 1998 Mar 12 22:27:05 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/4C12P03.html [5/26/1999 2:47:02 PM] 3CRR Atlas:4C 14.11: Main Page 4C 14.11 B0411+141
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 12.1 0.84 II CD Gal 0.206 r = 19.1* 115.00 25.92 330.4
Image:
Size: 105.9 × 105.9 arcsec² LUT: Linear Beam: 1.4 arcsec Frequency: 1477 MHz Method: CLEAN/VTESS Telescope: VLA A+B Credits: Leahy & Perley (1991)
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Page created: 1998 Mar 12 22:27:08 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/4C14P11.html [5/26/1999 2:47:06 PM] 3CRR Atlas:4C 14.27: Main Page 4C 14.27 B0832+143
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 11.2 1.15 II R+HB Gal 0.392 V = 19.5* 38.90 26.51 165.1
Image:
Size: 76.8 × 76.8 arcsec² LUT: Linear Beam: 1.25 arcsec Frequency: 1477 MHz Method: CLEAN Telescope: VLA A Credits: Leahy & Perley (1991)
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Page created: 1998 Mar 12 22:27:10 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/4C14P27.html [5/26/1999 2:47:09 PM] 3CRR Atlas:4C 35.40: Main Page 4C 35.40 B1615+351
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 11.7 0.76 I WP+HP Gal 0.0301 B = 14.9* 890.00 24.21 492.9
Image:
Size: 2304.0 × 2304.0 arcsec² LUT: Logarithmic Beam: 28×48 arcsec Frequency: 608 MHz Method: CLEAN Telescope: WSRT Credits: This Atlas
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Page created: 1998 Mar 12 22:27:14 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/4C35P40.html [5/26/1999 2:47:10 PM] 3CRR Atlas:4C 73.08: Main Page 4C 73.08 B0945+734
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 15.6 0.85 II CD Gal 0.0581 R = 14.74 1004.00 24.91 1024.0
Image:
Size: 2520.1 × 2520.1 arcsec² LUT: Logarithmic Beam: 30.0 arcsec Frequency: 608 MHz Method: CLEAN Telescope: WSRT Credits: This Atlas
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Page created: 1998 Mar 12 22:27:10 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/4C73P08.html [5/26/1999 2:47:15 PM] 3CRR Atlas:A 1552: Main Page A 1552 B1227+119
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 12.5 0.94 I TTJ Gal 0.0843 V = 16* 168.00 25.15 238.2
Image:
Size: 256.0 × 256.0 arcsec² LUT: Linear Beam: 5.6 arcsec Frequency: 1490 MHz Method: CLEAN Telescope: VLA A+B Credits: Owen, White & Burns (1992)
This twin-tail DRAGN is associated with one of the two bright dumbell galaxies that dominate the distant galaxy cluster Abell 1552. It was not detected in early radio surveys as it is less than one degree from the very bright object Virgo A (3C 274). As a result this object is usually known by its IAU name. The host nucleus is located at the eastern end of the western bright patch, which is the base of a poorly-resolved jet. The other bright galaxy in A 1552, 1227+120, is also a DRAGN, but is several times weaker.
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Page created: 1998 Mar 12 22:27:11 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/A1552.html [5/26/1999 2:47:19 PM] 3CRR Atlas:DA 240: Main Page DA 240 B0745+560
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 23.2 0.77 II CD Gal 0.0350 R = 13.71 2109.00 24.64 1346.8
Image:
Size: 2520.1 × 2520.1 arcsec² LUT: Logarithmic Beam: 34 arcsec Frequency: 608 MHz Method: CLEAN Telescope: WSRT Credits: Atlas
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Page created: 1998 Mar 12 22:27:09 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/DA240.html [5/26/1999 2:47:21 PM] 3CRR Atlas:NGC 6251: Main Page NGC 6251 B1637+826
Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D 10.9 0.72 I WB+HP Gal 0.024 R = 11.66 3940.00 23.98 1758.0
Image:
Size: 5100.0 × 5100.0 arcsec² LUT: Logarithmic Beam: 55 arcsec Frequency: 327 MHz Method: CLEAN Telescope: WSRT Credits: Mack et al. (1996)
At just over one degree across, NGC 6251 is the largest known DRAGN in the northern sky. It was missed in 3CR and other early radio surveys because its radio emission was too spread out to be identified as a single object. Our Westerbork image shows dozens of background radio sources within and around the twin lobes of NGC 6251 itself. Most of these are distant DRAGNs at much higher redshift. The brightest part of NGC 6251 is its one-sided jet, which has been studied in detail at much higher resolution by Perley, Bridle & Willis (1984). The host galaxy, NGC 6251 proper, is located at the eastern end of the jet. A very faint counterjet is also just visible. This relatively nearby and very bright example provides a useful test of our understanding of how radio jets work. Perley et al. concluded that the jet is confined into its narrow channel by the pressure of the hot interstellar gas of the galaxy. Recently a deep X-ray observation by Birkinshaw & Worrall (1993) showed that there is much less gas present than is needed, so we still have work to do on this point! The structure is intermediate between tailed and bridged twin-jets, which the western lobe surrounding the jet (i.e. a bridge) but the eastern lobe apparently beginning at the "warmspot" which marks the end of the eastern jet. The northern lobe also contains a relatively compact "warmspot" so this object also seems to be an "almost" classical double. The apparent faint emission in the top left and bottom right corner of this image is an artifact due to imperfect deconvolution. A higher-resolution 608 MHz image is on the Other Images page; it suffers from the same artifacts as the main image, as well as striping paralled to the jet.
http://www.jb.man.ac.uk/atlas/object/NGC6251.html (1 of 2) [5/26/1999 2:47:24 PM] 3CRR Atlas:NGC 6251: Main Page Prev. Data Page Other images Next Search Alphanumeric List Icon List Atlas Index
Page created: 1998 Mar 12 22:27:14 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/object/NGC6251.html (2 of 2) [5/26/1999 2:47:24 PM] 3CRR Atlas:Contributors An Atlas of DRAGNs Credits
Contributors
This Atlas would not have been possible without the kindness of the observers who have sent us images and calibrated data. They are listed here. (Addresses are current addresses, except for people who have since left astronomy). Chidi Akujor, Imo State University, Nigeria. Paul Alexander, Mullard Radio Astronomy Observatory, University of Cambridge, England. Peter Barthel, Kapteyn Astronomical Institute, Groningen, the Netherlands. Adam Black, Cambridge University Press, England. (formally at Mullard Radio Astronomy Observatory, University of Cambridge). Wil van Breugel, Institute of Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, California, USA. Alan Bridle, National Radio Astronomy Observatory, Charlottesville, Virginia, USA. Ger de Bruyn, Netherlands Foundation for Research in Astronomy, Dwingeloo, the Netherlands. Jack Burns, New Mexico State University, Las Cruces, NM, USA. Wayne Christiansen, Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC, USA. David Clarke, Dept. of Astronomy & Physics, St. Mary's University, Halifax, Nova Scotia, Canada. Neil Comins, University of Maine, Orono, MA, USA. Jim Condon, National Radio Astronomy Observatory, Charlottesville, Virginia, USA. Pat Crane, formerly at National Radio Astronomy Observatory, Socorro, New Mexico, USA. Luigina Feretti, Istituto di Radioastronomia, Bologna, Italy. Ed Fomalont, National Radio Astronomy Observatory, Charlottesville, Virginia, USA. Simon Garrington, Nuffield Radio Astronomy Laboratories, University of Manchester, England. JingPing Ge, Steward Observatory, University of Arizona, Tuscon, AZ, USA. Harbinder Ghataure, Astronomy Group, University of Southampton, England. Gabriele Giovannini, Istituto di Radioastronomia, Bologna, Italy. Martin Hardcastle, Mullard Radio Astronomy Observatory, University of Cambridge, England. Ronald Hes, formerly at Kapteyn Astronomical Institute, Groningen, the Netherlands. Gary Hill, McDonald Observatory, University of Texas at Austin, USA. Phil Kronberg, Department of Astronomy, University of Toronto, Toronto, Ontario, Canada. Wim Jägers, formerly at Sterrewacht Leiden, the Netherlands. Robert Laing, Royal Greenwich Observatory, Cambridge, England. Paddy Leahy, Nuffield Radio Astronomy Laboratories, University of Manchester, England. Roger Linfield, Jet Propulsion Laboratory, Pasadena, California, USA.
http://www.jb.man.ac.uk/atlas/contributors.html (1 of 3) [5/26/1999 2:47:29 PM] 3CRR Atlas:Contributors Everton Lüdke, Departamento de Fisica, Universidade Federal de Santa Maria, Brazil. Tom Muxlow, Nuffield Radio Astronomy Laboratories, University of Manchester, England. Chris O'Dea, Space Telescope Science Institute, Baltimore, Maryland, USA. Frazer Owen, National Radio Astronomy Observatory, Socorro, New Mexico, USA. Alan Pedlar, Nuffield Radio Astronomy Laboratories, University of Manchester, England. Rick Perley, National Radio Astronomy Observatory, Socorro, New Mexico, USA. Guy Pooley, Mullard Radio Astronomy Observatory, University of Cambridge, England. Julia Riley, Mullard Radio Astronomy Observatory, University of Cambridge, England. Kurt Roettiger, NASA Goddard Space Flight Center, Greenbelt, Maryland, USA. Hardip Sanghera, Joint Institute for VLBI in Europe, Dwingeloo, the Netherlands. Steve Spangler, University of Iowa, Iowa City, IA, USA. Richard Strom, Netherlands Foundation for Research in Astronomy, Dwingeloo, the Netherlands. Greg Taylor, National Radio Astronomy Observatory, Socorro, New Mexico, USA. Tasso Tzioumis, Australia Telescope National Facility, Sydney, New South Wales, Australia. Peter Wilkinson, Nuffield Radio Astronomy Laboratories, University of Manchester, England. Tony Willis, Dominion Radio Astrophysical Observatory, Penticton, British Colombia, Canada. Joan Wrobel, National Radio Astronomy Observatory, Socorro, New Mexico, USA. We are also grateful to the following, who sent us data that for one reason or another we did not use: Ski Antonucci, Wil van Breugel, Roberto and Carla Fanti, Peppo Gavazzi, Robert Laing, Hans de Ruiter, and Paola Parma. Telescopes
MERLIN The Multi-Element Radio Linked Interferometer Network. Operated by the University of Manchester on behalf of the Particle Physics and Astrophysics Research Council (PPARC). VLA The Very Large Array, operated by the National Radio Astronomy Observatory (NRAO), which is a facility of the National Science Foundation (NSF), operated under cooperative agreement by Associated Universities, Inc. (AUI). N.B. in the "telescope" field of the main pages we list the VLA configurations used; e.g. VLA A+B means a combination of data from the A and B configurations. WSRT The Westerbork Synthesis Radio Telescope, of the Netherlands Foundation for Research in Astronomy (NFRA), a national facility supported by the Netherlands Organization for Scientific Research (NWO).
http://www.jb.man.ac.uk/atlas/contributors.html (2 of 3) [5/26/1999 2:47:29 PM] 3CRR Atlas:Contributors Other Acknowledgements
We thank Mike Evans, who, as a summer student in 1991, made many of the C20 images and took a lot of the morphological measurements. He also compiled most of the data from the literature, and created the prototype of this Atlas, as a hypercard stack. The web version of the Atlas was inspired by the SEDS Messier Database, (well worth checking out), created by Guy McArthur and Hartmut Frommert. For their M.Sc. technical projects, Jolene Horlock and Paul Rayner produced the prototype search page and frames/Java navigation bar, respectively.
<<<< Atlas Index >>>> Alphanumeric List Icon List Jodrell Bank home page
Last modified: 1997 June 20 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/contributors.html (3 of 3) [5/26/1999 2:47:29 PM] 3CRR Atlas: Home Page
An Atlas of DRAGNs
Edited by J. P. Leahy, A . H. Bridle, and R. G. Strom
We present radio images and other data for the nearest 85 DRAGNs (radio galaxies and related objects) in the so-called "3CRR" sample of Laing, Riley & Longair (1983).
JAVA-enhanced Frames Version about frames Index
Beginners: try the Introductory Pages. For full details, see the Description Pages. To see the images, check the Listings, or type a source name here: ● Introductory Material ❍ The Radio Sky See the Universe in a different light... ❍ What are DRAGNs? ❍ Some cosmological complications ❍ Notes on radio images ❍ Glossary Technical terms for non-specialists. ● Description of the Atlas ❍ The Atlas project A brief introduction and summary of the data available. ❍ The Atlas Web pages How to use this site. ❍ FTP instructions How to download the original radio images. ❍ The Atlas sample What's in, what's out, and why. ❍ The Anatomy of DRAGNs ❍ The classification system
http://www.jb.man.ac.uk/atlas/index.html (1 of 2) [5/26/1999 2:47:37 PM] 3CRR Atlas: Home Page ❍ Description of the data. ❍ Table of radio data from the literature. ❍ Table of positions from the literature. ❍ Table of optical data from the literature. ❍ Table of structural data from the Atlas. (Real soon now!). ❍ Alternative names Messier, NGC, UGC, Abell... (with links) ❍ Famous radio sources omitted from the Atlas with a few links. ❍ Credits People, telescopes, and organizations which have contributed to the Atlas. ❍ References ● Links to Pages on individual DRAGNs ❍ Alphanumeric Listing ❍ Listing by icons A bit slow (170 kbytes of images!). ❍ Search for a specific DRAGN.
What's New! Current Status Please let us know if you find a mistake!
Intro Description Alphanumeric List Icon List Search Jodrell Bank home page
Last modified: 1998 March 12 J. P. Leahy [email protected]
View these pages with a browser that recognises HTML Tables and in-line JPEG images.
http://www.jb.man.ac.uk/atlas/index.html (2 of 2) [5/26/1999 2:47:37 PM] 3CRR Atlas:Icon list An Atlas of DRAGNs Listing by Icons
These thumbnail images are arranged in order of increasing radio power. Each image has been blurred so the beamwidth is 1/20 of the angular size; this allows the structures of objects with very different angular sizes to be easily compared. Click on a thumbnail to go to the individual Atlas page.
[No C20 image] 3C 31
3C 272.1 3C 449 NGC 6251 4C 11.71 3C 386
3C 296 3C 83.1B 4C 35.40 3C 442A 3C 66B 3C 264
[No C20 image] DA 240
3C 76.1 3C 274 3C 84 3C 293 3C 305
[No C20 image] 4C 73.08
3C 465 3C 338 3C 98 3C 35 3C 382
3C 285 3C 192 A 1552 3C 321 3C 236 3C 390.3
3C 314.1 3C 310 3C 326 3C 184.1 3C 33 3C 388
http://www.jb.man.ac.uk/atlas/icon.html (1 of 3) [5/26/1999 2:48:09 PM] 3CRR Atlas:Icon list
3C 315 3C 303 4C 12.03 3C 223 3C 346 3C 452
3C 33.1 3C 381 4C 14.11 3C 349 3C 433 3C 319
3C 132 3C 28 3C 284 3C 401 3C 436 3C 171
3C 67 3C 249.1 3C 61.1 3C 234 3C 153 3C 288
3C 20 3C 219 3C 300 3C 173.1 3C 268.3 3C 299
4C 14.27 3C 351 3C 42 3C 16 3C 109 3C 79
3C 215 3C 341 3C 46 3C 200 3C 457 3C 19
http://www.jb.man.ac.uk/atlas/icon.html (2 of 3) [5/26/1999 2:48:09 PM] 3CRR Atlas:Icon list
3C 274.1 3C 244.1 3C 438 3C 47 3C 48 3C 123
3C 295
<<<< Atlas Index >>>> Alphanumeric List Icon List Jodrell Bank home page
Last modified: 1996 November 20 J. P. Leahy [email protected]
http://www.jb.man.ac.uk/atlas/icon.html (3 of 3) [5/26/1999 2:48:09 PM] NRAL - Jodrell Bank Home Page
The Nuffield Radio Astronomy Laboratories (NRAL) at Jodrell Bank are a part of the University of Manchester's Department of Physics and Astronomy. The Laboratories are home to the Lovell Telescope and the MERLIN & VLBI National Facility which is operated by the University on behalf of PPARC.
NEW 13-May-99 Jodrell Bank Gets Grant to Observe the Big Bang
Find out what goes on at Public Information Jodrell Bank, including an on-line guided tour, telescope activities and our Science Centre & Arboretum (which is open to the public). Technical details about NRAL Telescopes & Technology telescopes and instrumentation. Includes details of MERLIN and VLBI systems for prospective observers. Research at Jodrell Bank Research including studies of stars, pulsars, galaxies, quasars, gravitational lenses, CMB and SETI. How to get in touch with Contact Information NRAL and the Science Centre, and how to find us. Latest results or News & Opportunities developments at Jodrell Bank including press releases, observing proposal details, postgraduate study and employment opportunities.
http://www.jb.man.ac.uk/ (1 of 2) [5/26/1999 2:48:19 PM] NRAL - Jodrell Bank Home Page Local computing and Resources scientific resources, and links to other useful sites.
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http://www.jb.man.ac.uk/ (2 of 2) [5/26/1999 2:48:19 PM] J. P. Leahy J. P. Leahy
I'm a lecturer in Radio Astronomy in the University of Manchester's Department of Physics and Astronomy. I'm based at Jodrell Bank.
Research Interests
● DRAGNs ● Numerical modelling of jets. ● Magnetic fields in the interstellar, intracluster, and intergalactic media. ● Techniques of synthesis imaging, especially using MERLIN. Current projects
● The Atlas of DRAGNs (with Alan Bridle & Richard Strom). ● Hercules A (with my student Nectaria Gizani, Simon Garrington, Rick Perley and John Dreher). ● Inverse-Compton emission from Giant Radio Galaxies (with my former M.Sc. student Dimitrios Tsakiris, and Colin Barber). ● The Distant DRAGNs project (imaging a sample of DRAGNs at redshift > 1.5), with my former Ph.D. student Duncan Law-Green, and my current M.Sc. student David Tansley. ● The Laing-Garrington Effect (with Simon Garrington, Robert Laing, Nectaria Gizani, and others). ● Spectral mapping of DRAGNs (with Tom Muxlow and Robert Laing). ● Modelling emission from relativistic jets (with my former research student Mark Bowman). ● The nearby hotspots project (with a cast of thousands).
Is the Universe Screwy?
(No it isn't, as a matter of fact). Back to Jodrell Bank home page Last modified: 1997 August 12 J. P. Leahy University of Manchester Nuffield Radio Astronomy Laboratories Jodrell Bank, Macclesfield Cheshire SK11 9DL Phone: 01477 571321 ext 207 Fax: 01477 571618
http://www.jb.man.ac.uk/~jpl/ (1 of 2) [5/26/1999 2:48:21 PM] J. P. Leahy [email protected]
http://www.jb.man.ac.uk/~jpl/ (2 of 2) [5/26/1999 2:48:21 PM]