A 149 minute periodicity underlies the X-ray flaring of Sgr A*
  In a recent paper (Leibowitz 2017) I have shown that the 39 large X-ray
flares of Sgr A* that were recorded by Chandra observatory in the year 2012,
are concentrated preferably around tick marks of an equi-distance grid on the
time axis. The period of this grid as found in L1 is 0.1033 days. In this work
I show that the effect can be found among all the large X-ray flares recoded by
Chandra and XMM-Newton along 15 years. The midpoints of all the 71 large flares
recorded between the years 2000 and 2014 are also tightly grouped around tick
marks of a grid with this period, or more likely, 0.1032 day. This result is
obtained with a confidence level of at least 3.27{\sigma} and very likely of
4.62{\sigma}. I find also a possible hint that a similar grid is underlying IR
flares of the object. I suggest that the pacemaker in the occurrences of the
large X-ray flares of Sgr A* is a mass of the order of a low mass star or a
small planet, in a slightly eccentric Keplerian orbit around the SMBH at the
centre of the Galaxy. The radius of this orbit is about 6.6 Schwarzschild radii
of the BH.
