Radiation transfer of cmbr into the CO parts of the nebula wind indicated those parts only must have a kelvin temperature state which is uniquely the least of any observed location in nature.

The kinetic energy (KE) of the CO outflow is theorized as the product of common-envelope evolution, which was a change in the outer environment (an envelope) of the dual orbital system of the binary system.

A succession of periodic observations from November 2011 (Atacama Large Millimeter Array) ending June 2012 (Australia Telescope Compact Array) with archived observations from Hubble (HST) (1998 & 2005) The nebula's visible double lobe was observed to be surrounded by a larger spherical region of cold gas seen only in sub-millimeter radio wavelengths. The nebula's outer fringes appear to be gradually warming.

As of mid-2017, it is believed that the star at the center of the nebula is a dying red giant.

ALMA (2017)

<gallery>

File:True shape of the Boomerang.jpg|

File:Boomerang nebula - ALMA-HST-- Potw1724a.tif|

</gallery>

HST

<gallery>

File:Boomerang HST big.jpg|Imaged using polarizing filters (analogous to polarized sunglasses) and color-coded by the angle associated with the polarized light.

File:Boomerang Nebula.png|Red filter applied to monochromatic data

</gallery>

Notes

References

  • NRAO Boomerang Nebula
  • The Boomerang Nebula - The Coolest Place in the Universe?, ESA, 20 February 2003
  • Hubble's View of the Boomerang Nebula, 13 September 2005; see also Scattered Light from the Boomerang Nebula
  • ESA/Hubble-Boomerang Nebula
  • SIMBAD, Coordinates and Scientific data. January 4, 2007.