The youngest lobe-dominated radio sources

Abstract

We present an analysis of multi-epoch global VLBI observations of the Compact Symmetric Objects: 2352+495 and 0710+439 at 5 GHz. Analysis of data spread over almost two decades shows strong evidence for an increase in separation of the outer components of both sources at a rate of ∼ 0.2h −1 c (for q • =0.5 and H • = 100h kms −1 Mpc −1 ). Dividing the overall sizes of the sources by their separation rates implies that these Compact Symmetric Objects have a kinematic age ≪ 10 4 years. These results (and those for other CSOs) strongly argue that CSOs are indeed very young sources and that they are probably evolve into the much larger classical doubles.

Soon After the Birth of Radio Sources

“…The first results from this analysis of the 5 GHz VLBI data were published in , and Owsianik et al (1999). In June 2000 we have performed new VLBA+Effelsberg 5 GHz observations of these sources, thereby extending the time baseline to more than twenty years.…”

Multifrequency VLBA observations of two compact symmetric objects

“…consistent with those derived by multiple epoch presented here and elsewhere conclude the census of observations at 6 cm by Owsianik & Conway CSOs in the complete PR and CJ1 sample. There are (1998), Owsianik et al (1998) and Owsianik et al 15 confirmed CSOs in this 200 source sample, (these proceedings) and will not be discussed further.…”

“…Light blu symbols represent the data taken in U band, the red symbols are observation taken in C band. Square and circles are relative to the observations used in this work, the diamonds are relative to the work by Owsianik et al (1998) and the triangles represent the observations from the paper by Taylor et al, (2000). The 5 GHz observations were compared with the work by Owsianik et al, (1998).…”

“…Square and circles are relative to the observations used in this work, the diamonds are relative to the work by Owsianik et al (1998) and the triangles represent the observations from the paper by Taylor et al, (2000). The 5 GHz observations were compared with the work by Owsianik et al, (1998). Owsianik et al, (1998), found that the hot spots in J0111+3906 have a separation velocity of about v C sep = (0.25 ± 0.04) c. The di↵erence in this case are probably due to the di↵erent instrument used.…”

“…Multi-epoch observations of the MOJAVE project, measurements obtained by Owsianik et al, (1998) and the data used by Taylor et al, (2000), were taken in to account for the multi-epoch study of J0111+3906. All the data used for multi epoch analysis of the source J0111+3906 are presented in Table 5.4.…”