Multi-frequency VLBA Observations of the Compact Double B2 2050+36: Constraints on Interstellar Scattering Revisited

Details Multi-frequency VLBA Observations of the Compact Double B2 2050+36: Constraints on Interstellar Scattering Revisited Multi-frequency VLBA Observations of the Compact Double B2 2050+36: Constraints on Interstellar Scattering Revisited

2001-06-23

arxiv.org/abs/astro-ph/0106434v1

Astronomy and Astrophysics

Astrophysics

19 pages LaTeX2e with AASTeX 5, 3 figures in 7 PostScript files; accepted for publication in the ApJ

Scientific paper

10.1086/322958

We present multi-frequency observations with the Very Long Baseline Array of the compact double radio source B2 2050+36. Our observations are at 0.33, 0.61, 1.67, 2.3, and 8.4 GHz, with the 0.61 GHz observations forming the third epoch of observation of this source at that frequency. At 0.61 GHz, the structure of B2 2050+36 is dominated by two components 56 mas apart. Within the uncertainties of the various measurements, this separation has remained unchanged for the past 16 years. Any differential image wander caused by refractive interstellar scattering is less than 4 mas. Both the lack of differential image wander and the frequency dependence of the angular diameter of B2 2050+36 below 1 GHz indicate that the electron density power spectrum along this line of sight has a spectral index near the Kolmogorov value, with a value of 4 being highly unlikely. We conclude that diffractive scattering dominates along this line of sight; results in the literature indicate that this conclusion also holds true for the line of sight to the pulsar PSR B2020+28 (8.7 deg. from B2 2050+36). Comparison of our 1.67 GHz observations with those obtained 21 years previously place a limit on the projected linear separation velocity of the two components of c.

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