Markarian 3 - A double radio source in a Seyfert galaxy

1980 ◽  
Vol 237 ◽  
pp. L61 ◽  
Author(s):  
A. S. Wilson ◽  
G. G. Pooley ◽  
E. D. Clements ◽  
A. G. Willis
Keyword(s):  
Radio Source ◽  
Seyfert Galaxy ◽  
Double Radio Source

Anomalous component motion in the mas double radio source, 0646+600

1994 ◽  
pp. 367-368
Author(s):  
Chidi E. Akujor ◽  
Richard W. Porcas
Keyword(s):  
Radio Source ◽  
Anomalous Component ◽  
Double Radio Source ◽  
Component Motion

scholarly journals The Radio Core of Markarian 348

1984 ◽  
Vol 110 ◽  
pp. 263-264
Author(s):  
S. G. Neff ◽  
A. G. de Bruyn
Keyword(s):  
Radio Source ◽  
Seyfert Galaxy ◽  
Small Scale ◽  
Early Type ◽  
Disc Galaxy ◽  
Relative Proximity ◽  
The Galaxy ◽  
Continuum Radio ◽  
The Continuum

The type 2 Seyfert galaxy Markarian 348 (NGC 262) is a normal early-type disc galaxy (SO/a or Sa) surrounded by a very large HI envelope. The continuum radio source in the galaxy is unresolved by conventional interferometers on scales as small as an arcsecond, is variable on time scales of a few months, and is quite strong by Seyfert standards (300 mJy). Mkn 348 is relatively nearby, allowing one to study very small-scale structure in the galaxy (at the assumed distance of 60 Mpc (Ho = 75 km/sec/Mpc), one light year subtends an angle of about one mas). Both the relative proximity and the radio source strength make it a good candidate for VLBI studies.

scholarly journals Radio Emission from the Seyfert Galaxy NGC 5548

1982 ◽  
Vol 97 ◽  
pp. 191-192
Author(s):  
J. S. Ulvestad ◽  
A. S. Wilson ◽  
D. G. Wentzel
Keyword(s):  
High Resolution ◽  
Radio Emission ◽  
Radio Source ◽  
Seyfert Galaxy ◽  
Central Component ◽  
The Galaxy ◽  
Ngc 5548

Weak radio emission from the type 1.5 Seyfert galaxy NGC 5548 has been mapped with high resolution at the VLA at both 1465 and 4885 MHz. The galaxy contains the largest (5.9 kpc) triple radio source known in a Seyfert galaxy. The central component of that triple is unresolved (<0.39×0.15 kpc) and has a flatter spectrum than the well-resolved outer lobes. In addition, the field surrounding NGC 5548 and two of the sources in that field have been mapped at 1465 MHz; the field sources are unlikely to be physically associated with NGC 5548.

Anomalous component motion in the mas double radio source, 0646+600

1994 ◽  
Vol 216 (1-2) ◽  
pp. 367-368
Author(s):  
Chidi E. Akujor ◽  
Richard W. Porcas
Keyword(s):  
Radio Source ◽  
Anomalous Component ◽  
Double Radio Source ◽  
Component Motion

C 343, a Double Radio Source with Very Wide Component Separation.

1965 ◽  
Vol 141 ◽  
pp. 1580 ◽  
Author(s):  
Alan T. Moffet
Keyword(s):  
Radio Source ◽  
Component Separation ◽  
Double Radio Source

Scorpius X-1 - an evolving double radio source

1986 ◽  
Vol 311 ◽  
pp. 805 ◽  
Author(s):  
B. J. Geldzahler ◽  
E. B. Fomalont
Keyword(s):  
Radio Source ◽  
Double Radio Source

Formation of double radio source structures and superluminal expansion

1977 ◽  
Vol 216 ◽  
pp. L1 ◽  
Author(s):  
W. A. Christiansen ◽  
J. S. Scott
Keyword(s):  
Radio Source ◽  
Double Radio Source ◽  
Superluminal Expansion

scholarly journals The H I emission and absorption spectra towards the double radio source 1830-211

1992 ◽  
Vol 259 (1) ◽  
pp. 63-66 ◽  
Author(s):  
R. Subrahmanyan ◽  
M. J. Kesteven ◽  
P. t. L. Hekkert
Keyword(s):  
Radio Source ◽  
Absorption Spectra ◽  
Emission And Absorption Spectra ◽  
Double Radio Source

scholarly journals The Two-Sided VLBI Source in the Seyfert Galaxy Mrk 231

1998 ◽  
Vol 164 ◽  
pp. 199-200 ◽  
Author(s):  
J. S. Ulvestad ◽  
J. M. Wrobel ◽  
C. L. Carilli
Keyword(s):  
Radio Source ◽  
Seyfert Galaxy ◽  
Central Component ◽  
Linear Scale ◽  
Radio Image ◽  
Total Size ◽  
The Core

AbstractThe Seyfert 1/starburst/IR galaxy Mrk 231 (UGC 08058), at z = 0.0422, has been imaged with the VLBA at frequencies ranging from 1.4 GHz to 22 GHz. The radio image shows a triple source of total size 50 mas (30h−1 pc), with a self-absorbed central component and two detached lobes. The northern lobe, located 12h−1 pc from the core, is free-free absorbed at the lowest frequencies; there also seems to be free-free absorption in the southern component. The linear scale over which this absorption takes place is several times larger than that seen in NGC1275/3C84.The axis of the 50-mas radio source is approximately 60° from the elongation of the central component on the 1-mas scale. The spectrum of this central component becomes optically thin between 5 and 8.4 GHz, and resolves into a small triple source of size ~ 1.0h−1 pc at 15 GHz. There is no hint of a jet or other structure directly connecting this central component to the outer VLBI lobes.

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