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The '''Cotton candy nebula''' (IRAS 17150−3224) is a [[protoplanetary nebula]] in the [[constellation]] of [[Ara]], The Altar. The nebula has a bipolar structure (meaning it consists of two large lobes), with a central [[star]].<ref name=arxiv>Lagadec, E. et Al. (2011). A mid-infrared imaging catalogue of post-asymptotic giant branch stars. ''Monthly Notices of the Royal Astronomical Society'', 417(1), pp.32-92. [https://arxiv.org/abs/1102.4561 arXiv:1102.4561 <nowiki>[astro-ph.SR]</nowiki>]</ref> This central star is not visible in optical image of the nebula due to a dark lane that obscures it. However is can be observed in the [[infrared]] portion of the [[electromagnetic spectrum]], where the obscuring effects of dust are greatly reduced. The two lobes are spearated by this dark lane.<ref name=arxiv/> It is thought there is a [[torus|toriodal]] (doughnut-shaped) structure at the very core of the nebula that is expanding.<ref>Weintraub, D., Huard, T., Kastner, J. and Gatley, I. (1998). The Onset of Molecular Hydrogen Emission from Proto–planetary Nebulae. ''The Astrophysical Journal'', 509(2), pp.728-732. [http://adsabs.harvard.edu/abs/1998ApJ...509..728W Bibcode:1998ApJ...509..728W]</ref>

The '''Cotton candy nebula''' (IRAS 17150−3224) is a [[protoplanetary nebula]] in the [[constellation]] of [[Ara]], The Altar. The nebula has a bipolar structure (meaning it consists of two large lobes), with a central [[star]].<ref name=arxiv>Lagadec, E. et Al. (2011). A mid-infrared imaging catalogue of post-asymptotic giant branch stars. ''Monthly Notices of the Royal Astronomical Society'', 417(1), pp.32-92. [https://arxiv.org/abs/1102.4561 arXiv:1102.4561 <nowiki>[astro-ph.SR]</nowiki>]</ref> This central star is not visible in optical image of the nebula due to a dark lane that obscures it. However is can be observed in the [[infrared]] portion of the [[electromagnetic spectrum]], where the obscuring effects of dust are greatly reduced. The two lobes are spearated by this dark lane.<ref name=arxiv/> It is thought there is a [[torus|toroidal]] (doughnut-shaped) structure at the very core of the nebula that is expanding.<ref>Weintraub, D., Huard, T., Kastner, J. and Gatley, I. (1998). The Onset of Molecular Hydrogen Emission from Proto–planetary Nebulae. ''The Astrophysical Journal'', 509(2), pp.728-732. [http://adsabs.harvard.edu/abs/1998ApJ...509..728W Bibcode:1998ApJ...509..728W]</ref>

The nebula lies approximately 9,650 [[light year]]s from [[Earth]] and have a temperature between 168-409 kelvin.<ref name=dist/> The total [[luminosity]] of the nebula has been estimated to be 12,000 times that of the [[Sun]].<ref name=dist/> Intense [[ultraviolet]] radiation emanating from the central star [[ionization|ionizes]] the enveloping [[gas]], causing it to glow.

The nebula lies approximately 9,650 [[light year]]s from [[Earth]] and have a temperature between 168-409 kelvin.<ref name=dist/> The total [[luminosity]] of the nebula has been estimated to be 12,000 times that of the [[Sun]].<ref name=dist/> Intense [[ultraviolet]] radiation emanating from the central star [[ionization|ionizes]] the enveloping [[gas]], causing it to glow.