We have performed intensity monitoring observations toward the Galactic center compact nonthermal radio source, Sagittarius A*, at λ = 3 and 2 mm (100 and 140 GHz) from 1996 to 2002 using the Nobeyama Millimeter Array (NMA). In 1996, 1997, 1998, and 2000, the observations were performed during a period of one to two months for each year in a single (intermediate resolution) array con.guration in order to exclude a systematic error caused by sampling different source structures with the different beam sizes. From November 2000 to May 2001, and from November 2001 to May 2002, the observations were carried out over several months in order to investigate the longer term variability. We have detected two .ares in March 2000 and April 2002 as well as a .are observed in March 1998 (Tsuboi et al. 1999). The peak .ux densities of the .ares were 2-3 Jy at 3 mm, while the mean quiescent .ux densities was ∼1 Jy. In particular for the March 2000 .are, the .ux densities of Sgr A* at 2 mm had also reached a peak, ∼4 Jy, on 8 March and increased ΔS/S ∼ 300%. The .ux density decreased by half in a day. We have detected the intra-day variability of Sgr A*. The upper limit for size of the variable component estimated from timescale of the .are is a few tens of AU. For spectra made from our observations at mm-wavelengths, the variability of .ux density increases with frequency. It appears that the variability in the .are propagates from higher to lower frequency. The folded lightcurve with 106 days cycle, which determined from the analysis of the VLA cm-wavelength data, shows distinct high and low activity states. These results provide evidence for quasiperiodic variability of the .ux density of Sgr A* at mm-wavelengths.
Read full abstract