LORD OF THE RINGS: A KINEMATIC DISTANCE TO CIRCINUS X-1 FROM A GIANT X-RAY LIGHT ECHO
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Heinz-2015-LORD OF THE RINGS_ A.pdf
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Author(s)
Heinz, S.
Burton, M.
Braiding, C.
Brandt, W. N.
Jonker, P. G.
Sell, P.
Fender, R. P.
Nowak, Michael A.
Schulz, Norbert S.
Date Issued
June 2015
Journal
The Astrophysical Journal
Publisher
IOP Publishing
Citation
Heinz, S., M. Burton, C. Braiding, W. N. Brandt, P. G. Jonker, P. Sell, R. P. Fender, M. A. Nowak, and N. S. Schulz. “LORD OF THE RINGS: A KINEMATIC DISTANCE TO CIRCINUS X-1 FROM A GIANT X-RAY LIGHT ECHO.” The Astrophysical Journal 806, no. 2 (June 20, 2015): 265. © 2015 The American Astronomical Society
Version
Final published version
Abstract
Circinus X-1 exhibited a bright X-ray flare in late 2013. Follow-up observations with Chandra and XMM-Newton from 40 to 80 days after the flare reveal a bright X-ray light echo in the form of four well-defined rings with radii from 5 to 13 arcmin, growing in radius with time. The large fluence of the flare and the large column density of interstellar dust toward Circinus X-1 make this the largest and brightest set of rings from an X-ray light echo observed to date. By deconvolving the radial intensity profile of the echo with the MAXI X-ray light curve of the flare we reconstruct the dust distribution toward Circinus X-1 into four distinct dust concentrations. By comparing the peak in scattering intensity with the peak intensity in CO maps of molecular clouds from the Mopra Southern Galactic Plane CO Survey we identify the two innermost rings with clouds at radial velocity ~ -74 and ~ -81 km s[superscript -1], respectively. We identify a prominent band of foreground photoelectric absorption with a lane of CO gas at ~ -32 km s[superscript -1]. From the association of the rings with individual CO clouds we determine the kinematic distance to Circinus X-1 to be D[subscript CirX-1 = 9.4[+0.8 over -1.0] kpc. This distance rules out earlier claims of a distance around 4 kpc, implies that Circinus X-1 is a frequent super-Eddington source, and places a lower limit of Γ [> over ~] 22 on the Lorentz factor and an upper limit of θ[subscript jet] [< over ~] 3° on the jet viewing angle.
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1088/0004-637x/806/2/265
