Image Details
Caption: Figure 9.
Measured correlated flux densities of Sgr A* on April 6 and 7 of the HOPS (top) and CASA (bottom) data overplotted with a thin (unresolved) ring model with a ∼50 μas diameter, which has been blurred with a 23 μas FWHM circular Gaussian source (Papers III and IV). Flux densities have been calibrated based on estimated station SEFDs, measured light curves (Section 3.2.1), and calibrator gain transfers (Section 3.2.2). The data are averaged in 120 s bins, which causes phase coherence losses in a few scans. Error bars denote ±1σ uncertainty from thermal noise. Detections are color-coded by baselines, as in Figure 8. Redundant baselines are shown with different symbols: circles for baselines to ALMA and SMA; diamonds for baselines to APEX and JCMT.
© 2022. The Author(s). Published by the American Astronomical Society.