A Deep Chandra View of a Candidate Parsec-scale Jet from the Galactic Center Supermassive Black Hole

• Published in: The Astrophysical journal Vol. 875; no. 1; pp. 44 - 55
• Main Authors: Zhu, Zhenlin, Li, Zhiyuan, Morris, Mark R., Zhang, Shuo, Liu, Siming
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 10-04-2019; IOP Publishing
• Subjects: Astrophysics; black hole physics; Cooling; Deposition; Electrons; Fluctuations; Flux; Galaxy: center; ISM: jets and outflows; radiation mechanisms: non-thermal; Radiative cooling; Spectra; Supermassive black holes; X-rays: individual (G359.944−0.052)
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ab0e05

We have investigated the linear X-ray filament, G359.944−0.052, previously identified as a likely X-ray counterpart of a parsec-scale jet from the Galactic Center supermassive black hole (SMBH) Sagittarius A* (Sgr A*), using a total of ∼5.6 Ms ultra-deep Chandra observations taken from 1999 September to 2017 July. This unprecedented data set enables us to examine flux and spectral variations that might be related to intrinsic properties of the weakly accreting SMBH. We find no flux or spectral variation in G359.944−0.052 after the G2 periapsis passage around early 2014; however, a moderate flux increase of ∼2 significance might be associated with the periapsis passage of G1 in early 2001. The filament exhibits an unusually hard spectrum (photon index 1) in its portion closest to Sgr A* (i.e., near side) and a significant spectral softening in the more distant portion, which can be interpreted as synchrotron cooling of the relativistic electrons moving along the jet path. In particular, the hard spectrum of the near side suggests a piling up of quasi-monoenergetic electrons caused by rapid radiative cooling. The spectral and temporal properties of G359.944−0.052 strengthen the case for it being the X-ray counterpart of a jet launched by Sgr A*.