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A Dramatic (and Invisible!) Flare in NRAO 530

3 mm λ VLBI Observations
  • Geoffrey C. Bower
  • Don Backer
  • Rick Forster
  • Melvin Wright
Conference paper
Part of the International Astronomical Union book series (IAUS, volume 175)

Abstract

3 mm λ VLBI observations of the extremely flat spectrum QSO NRAO 530 at the peak of its brightest recorded flare show a resolved core only slightly changed from its pre-outburst state. Observations with Haystack, Kitt Peak and Owens Valley observatories in April 1994, prior to the onset of the flare found a single component with T b = 8 × 1010 K. One year later, within one week of the peak of flare at 3 mm λ, observations with Haystack, Kitt Peak and Hat Creek observatories revealed a component comparable in size and flux density with T b = 7 × 1010 K. Table 1 details the source models for the two experiments.

Keywords

Flux Density Source Model Radio Source Apparent Velocity Closure Phase 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

Copyright information

© International Astronomical Union 1996

Authors and Affiliations

  • Geoffrey C. Bower
    • 1
  • Don Backer
    • 1
  • Rick Forster
    • 1
  • Melvin Wright
    • 1
  1. 1.UC Berkeley Radio Astronomy LabBerkeleyUSA

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