SGR 1806-20 distance and dust properties in molecular clouds by analysis of a flare x-ray echoes

TL;DR

This study uses x-ray echoes from SGR 1806-20's 2006 burst to constrain its distance and analyze dust properties in molecular clouds, improving understanding of the source's energy output and interstellar dust characteristics.

Contribution

It provides the first use of x-ray echoes to simultaneously estimate the SGR's distance and study dust properties in molecular clouds.

Findings

Distance to SGR 1806-20 is constrained between 9.4 and 18.6 kpc.

Dust grain size distribution follows a power-law with index -3.3.

Dust grain size lower limit is 0.1 micron, consistent with interstellar medium measurements.

Abstract

The soft gamma repeater SGR 1806-20 is most famous for its giant flare from 2004, which yielded the highest gamma-ray flux ever observed on Earth. The flare emphasized the importance of determining the distance to the SGR, thus revealing the flare's energy output, with implications on SGRs energy budget and giant flare rates. We analyze x-ray scattering echoes observed by Swift/XRT following the 2006 August 6 intermediate burst of SGR 1806-20. Assuming positions and opacities of the molecular clouds along the line-of-sight from previous works, we derive direct constrains on the distance to SGR 1806-20, setting a lower limit of 9.4 kpc and an upper limit of 18.6 kpc (90% confidence), compared with a 6-15 kpc distance range by previous works. This distance range matches an energy output of ~10^46 erg/s for the 2004 giant flare. We further use, for the first time, the x-ray echoes in order to study the dust properties in molecular clouds. Analyzing the temporal evolution of the observed flux using a dust scattering model, which assumes a power-law size distribution of the dust grains, we find a power-law index of -3.3_{-0.7}^{+0.6} (1 sigma) and a lower limit of 0.1 micron (2 sigma) on the dust maximal grain size, both conforming to measured dust properties in the diffused interstellar medium (ISM). We advocate future burst follow-up observations with Swift, Chandra and the planned NuSTAR telescopes, as means of obtaining much superior results from such an analysis.