Fifteen years of XMM-Newton and Chandra monitoring of Sgr A* : evidence for a recent increase in the bright flaring rate
Skip to main content
Open Access Publications from the University of California


UCLA Previously Published Works bannerUCLA

Fifteen years of XMM-Newton and Chandra monitoring of Sgr A* : evidence for a recent increase in the bright flaring rate

  • Author(s): Ponti, G;
  • De Marco, B;
  • Morris, MR;
  • Merloni, A;
  • Munoz-Darias, T;
  • Clavel, M;
  • Haggard, D;
  • Zhang, S;
  • Nandra, K;
  • Gillessen, S;
  • Mori, K;
  • Neilsen, J;
  • Rea, N;
  • Degenaar, N;
  • Terrier, R;
  • Goldwurm, A
  • et al.

We present a study of the X-ray flaring activity of Sgr A* during all the 150 XMM-Newton and Chandra observations pointed at the Milky Way center over the last 15 years. This includes the latest XMM-Newton and Chandra campaigns devoted to monitoring the closest approach of the very red Br-Gamma emitting object called G2. The entire dataset analysed extends from September 1999 through November 2014. We employed a Bayesian block analysis to investigate any possible variations in the characteristics (frequency, energetics, peak intensity, duration) of the flaring events that Sgr A* has exhibited since their discovery in 2001. We observe that the total bright-or-very bright flare luminosity of Sgr A* increased between 2013-2014 by a factor of 2-3 (~3.5 sigma significance). We also observe an increase (~99.9% significance) from 0.27+-0.04 to 2.5+-1.0 day^-1 of the bright-or-very bright flaring rate of Sgr A*, starting in late summer 2014, which happens to be about six months after G2's peri-center passage. This might indicate that clustering is a general property of bright flares and that it is associated with a stationary noise process producing flares not uniformly distributed in time (similar to what is observed in other quiescent black holes). If so, the variation in flaring properties would be revealed only now because of the increased monitoring frequency. Alternatively, this may be the first sign of an excess accretion activity induced by the close passage of G2. More observations are necessary to distinguish between these two hypotheses.

Many UC-authored scholarly publications are freely available on this site because of the UC's open access policies. Let us know how this access is important for you.

Main Content
For improved accessibility of PDF content, download the file to your device.
Current View