On the connection of the apparent proper motion and the VLBI structure of compact radio sources

A. Moór, S. Frey, S. B. Lambert, O. A. Titov, J. Bakos

Research output: Contribution to journalArticle

20 Citations (Scopus)

Abstract

Many of the compact extragalactic radio sources that are used as fiducial points to define the celestial reference frame are known to have proper motions detectable with long-term geodetic/astrometric very long baseline interferometry (VLBI) measurements. These changes can be as high as several hundred microarcseconds per year for certain objects. When imaged with VLBI at milliarcsecond (mas) angular resolution, these sources (radio-loud active galactic nuclei) typically show structures dominated by a compact, often unresolved "core" and a one-sided "jet." The positional instability of compact radio sources is believed to be connected with changes in their brightness distribution structure. For the first time, we test this assumption in a statistical sense on a large sample rather than on only individual objects. We investigate a sample of 62 radio sources for which reliable long-term time series of astrometric positions as well as detailed 8 GHz VLBI brightness distribution models are available. We compare the characteristic direction of their extended jet structure and the direction of their apparent proper motion. We present our data and analysis method, and conclude that there is indeed a correlation between the two characteristic directions. However, there are cases where the 1-10mas scale VLBI jet directions are significantly misaligned with respect to the apparent proper motion direction.

Original languageEnglish
Article number178
JournalAstronomical Journal
Volume141
Issue number6
DOIs
Publication statusPublished - Jun 1 2011

Keywords

  • BL Lacertae objects: individual (OJ 287)
  • galaxies: active
  • quasars: general
  • radio continuum: galaxies
  • reference systems
  • techniques: interferometric

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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