2000A&A...362..426V

Query : 2000A&A...362..426V

2000A&A...362..426V - Astronomy and Astrophysics, volume 362426-434 (2000/10-2)

The nature of powerful compact radio galaxies.

VERON-CETTY M.-P., WOLTJER L., STAVELEY-SMITH L. and EKERS R.D.

Abstract (from CDS):

Three compact powerful radio galaxies, PKS 1353- 341, PKS 1814-637 and PKS 1934-638, have been imaged. The three galaxies seem to be giant ellipticals, the last two being bluer than normal gEs by 0.2-0.3mag in B-I, which is expected if they are the result of recent merging. HI absorption has been detected in all three objects with very different characteristics. The broad absorption in PKS 1353-341 probably takes place in a torus or a disk with a radius of at least a few tens of pc. For PKS 1814-637 the principal absorption is less broad and the disk radius more likely a few hundreds of pc. The absorption in PKS 1934-638 is very narrow and is probably due to gas not directly connected to the central engine. Data for a dozen of powerful radio galaxies with H I absorption are reviewed. Such absorption seems to be particularly common at high radio power.

Abstract Copyright: ∼

Journal keyword(s): galaxies: individual: PKS 1353-341, PKS 1814-637, PKS 1934-638 - radio lines: galaxies

Nomenclature: Fig.1, text: [VWS2000] PKS 1352-341 N (Nos 1-2).

Simbad objects: 32

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Number of rows : 32
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 2C 94 Sy2 01 08 52.8701830824 +13 20 14.262799812   15.19       ~ 494 2
2 Z 502-27 rG 01 19 35.00087601 +32 10 50.0619670   16 14.5     ~ 249 1
3 LEDA 13982 Sy2 03 51 35.7643720392 -27 44 34.896912468   16.0       ~ 157 1
4 3C 105.0 Sy2 04 07 16.4671273272 +03 42 25.813809432   18.5       ~ 241 0
5 3C 111 Sy1 04 18 21.2772425736 +38 01 35.801359968   19.75 18.05     ~ 1002 2
6 ESO 252-18A Sy1 05 19 49.7229323856 -45 46 43.852662732   15.73 15.77 14.85   ~ 714 0
7 QSO B0625-354 BLL 06 27 06.7286533392 -35 29 15.363665088   14.93       ~ 206 1
8 CD-32 5613 WD* 08 41 32.4290850497 -32 56 32.915823461   12.07 11.85 12.3   DA5.5 325 0
9 MCG-02-24-007 LIN 09 18 05.66848602 -12 05 43.8060823   14.38 14.8     ~ 1077 1
10 ATO J146.9381+07.4223 Sy1 09 47 45.1433922288 +07 25 20.595729756   17.37 16.95     ~ 389 1
11 3C 236.0 BLL 10 06 01.75023017 +34 54 10.4016113   15.97       ~ 473 2
12 PKS 1345+12 Sy2 13 47 33.36161873 +12 17 24.2398927   19.28 18.44 15.718   ~ 652 2
13 QSO B1353-341 Bla 13 56 05.38656310 -34 21 10.8588959   19.4   18.50   ~ 49 1
14 [VWS2000] PKS 1353-341 2 G 13 56 10.700 -34 20 48.00           ~ 1 0
15 3C 321 Sy1 15 31 43.46520 +24 04 18.9948   16.0   15.40   ~ 341 1
16 CD-28 11464 Pe* 15 38 59.6479538952 -28 35 36.973634856   12.310 11.797 11.794   A 121 0
17 2MASX J15520920+2005237 SyG 15 52 09.1938375312 +20 05 23.180614152   17.87 17.08     ~ 129 2
18 4C -00.67 Sy2 17 20 28.1680537512 -00 58 46.582453920   15.36       ~ 345 1
19 NGC 6328 QSO 17 23 41.02933859 -65 00 36.6106377   13.17 13.2 11.45 12.2 ~ 270 1
20 ICRF J173735.7-563403 Sy2 17 37 35.7711421992 -56 34 03.153321552   17.0       ~ 96 0
21 QSO B1814-637 Bla 18 19 35.00241 -63 45 48.1926   16.80 14.40 13.4   ~ 154 1
22 3C 388.0 SyG 18 44 02.3840387736 +45 33 29.628672300   16.91 15.56     ~ 338 1
23 [FBN87] G2 GiP 19 39 24.6 -63 42 45     19.59 18.92   ~ 4 0
24 ICRF J193925.0-634245 Sy2 19 39 25.0245304992 -63 42 45.640373400   18.87 18.37 17.64   ~ 1332 2
25 QSO B1946+708 BLL 19 45 53.51966298 +70 55 48.7285673   18.726 16.70 17.199   ~ 147 2
26 MCG+07-41-003 Bla 19 59 28.35656837 +40 44 02.0972325   16.22 15.10     ~ 2537 2
27 IC 5063 Bla 20 52 02.15 -57 04 06.7   12.92 13.60 11.30   ~ 710 1
28 3C 433.0 Sy2 21 23 44.5778423928 +25 04 27.670672416   17.660 16.350     ~ 338 1
29 2dFGRS TGS005Z206 Sy2 22 09 20.1637016208 -23 31 53.883877692   17.0   15.983   ~ 48 1
30 3C 452 Sy2 22 45 48.7616172744 +39 41 15.906782184   17.60 16.56     ~ 391 1
31 LEDA 71390 Sy1 23 25 19.72968960 -12 07 27.0814800   15.45 15.46     ~ 185 2
32 LEDA 73132 Sy2 23 59 04.31090 -60 54 59.2180   16.61       ~ 155 1

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