Angular broadening measurements of the sources 1849+005 and 2013+370 Available to Purchase

Angular broadening measurements, with different instruments and for different purposes, are reported for the radio sources 1849+005 and 2013+370. The former source lies in a part of the sky characterized by heavy scattering. Observations with the Very Large Array at Frequencies of 1.46 and 0.33 GHz were made of this object and 45 others in its vicinity. We were particularly interested in investigating the possibility that the supernova remnant G33.6+0.1 might be responsible for the enhanced scattering. Preliminary inspection of the data reveals at least one other source which is approximately as heavily scattered as 1849+005. An intriguing preliminary result is a possible increase of scattering in the galactic plane with decreasing galactic longitude. Our observations indicate that between 20 and 30 degrees of longitude, the 1.46 GHz scattering size is of the order of 1 to 2 arcseconds. The second source, 2013+370, is much less heavily scattered than 1849+005, and VLBI is needed to resolve the scattering disk. The line of sight to this object transfixes the Cygnus OB1 association. Our observations of this source were primarily motivated to measure the spectral index of interstellar density irregularities. The observations are consistent with a value of α=3.79±0.05, which supports a quasi‐Kolmogoroff spectrum in the interstellar medium.