Journal
SCIENCE
Volume 341, Issue 6149, Pages 981-983Publisher
AMER ASSOC ADVANCEMENT SCIENCE
DOI: 10.1126/science.1240755
Keywords
-
Categories
Funding
- Smithsonian Astrophysical Observatory (SAO) [GO2-13110, NAS8-03060]
- Chandra Mission Planning
- Raymond and Beverley Sackler Distinguished Visitor fellowship
- Netherlands Organization for Scientific Research Vidi Fellowship [639.042.711]
- NASA through the Einstein Postdoctoral Fellowship [PF2-130097]
- SAO for NASA [SV3-73016]
- Hubble Fellowship [HST-HF-51298.01]
- CONICYT-Chile through FONDECYT [11100240]
- Basal [PFB0609]
- Anillo [ACT1101]
- National Natural Science Foundation of China
- 973 Project of China [2009CB824800]
- STFC [ST/K000985/1, ST/J001538/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/K000985/1, ST/J001538/1] Funding Source: researchfish
Ask authors/readers for more resources
Most supermassive black holes (SMBHs) are accreting at very low levels and are difficult to distinguish from the galaxy centers where they reside. Our own Galaxy's SMBH provides an instructive exception, and we present a close-up view of its quiescent x-ray emission based on 3 megaseconds of Chandra observations. Although the x-ray emission is elongated and aligns well with a surrounding disk of massive stars, we can rule out a concentration of low-mass coronally active stars as the origin of the emission on the basis of the lack of predicted iron (Fe) K alpha emission. The extremely weak hydrogen (H)-like Fe K alpha line further suggests the presence of an outflow from the accretion flow onto the SMBH. These results provide important constraints for models of the prevalent radiatively inefficient accretion state.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available