Editing Mz 3 (section)

==Characteristics==
Mz 3 is radially expanding at a rate of about 50&nbsp;km/s and has its polar axis oriented at an angle of around 30° from the plane of the sky (Lopez & Meaburn 1983; Meaburn & Walsh 1985).  It is sometimes compared to the more extensively studied [[Planetary Nebula M2-9|Butterfly Nebula]] (M 2-9), and it is quite likely that both have a similar evolutionary history.  They both have point-like bright nuclei, are narrow-waisted bipolar nebulae, and share surprisingly similar spatially dependent spectra. Because of their similarity, their differences are noteworthy.  Their greatest difference is probably in their [[near infrared]] emissions.  Mz 3 has no trace of molecular hydrogen emission, whereas the M 2-9 has prominent H<sub>2</sub> emission lines in the near-IR.  The lack of H<sub>2</sub> emissions from Mz 3 is unusual given the strong correlation between such emissions and bipolar structures of PN.  Additionally, the polar lobes of Mz 3 are more mottled and rounded as compared to M 2-9. Finally, Mz 3 is not known to evidence temporal variability in its polar lobes as is found in M 2-9 (Doyle et al. 2000). {{Harv|Smith|2003}}

The [[Herschel Space Observatory]] has detected [[laser]] light emissions from the nebula -- specifically, hydrogen recombination line laser emissions.  This confirms the presence of a [[white dwarf]] with a binary companion at the heart of the nebula.<ref>{{cite web|url=http://www.esa.int/Our_Activities/Space_Science/Herschel/A_space_ant_fires_its_lasers|title=A space ant fires its lasers|last=esa|website=European Space Agency}}</ref>

===Chakram===
Of the morphological features of Mz 3, one of the most unusual and odd is the chakram (first noticed in 2004), a faint, large, limb brightened ellipse that appears to have its center on the PN's nucleus.  While the plane of the ellipse is near the other feature's shared reflection symmetry plane, it is definitely offset.  This structure's kinematics are the only such ones known among studied PN.  Unlike all the other Mz 3 structures, there is no increase of velocity as the radial offset from the nucleus increases.  Consequently, this must not be a simple equatorial flow despite the fact that its motion appears to be strictly radial (that is, there is no indication of rotation which would suggest that this feature is dynamically stable).  All the kinematic properties of the ellipse are symmetric and very ordered relative to the nucleus, consistent with all the other Mz 3 features.  Therefore, the ellipse must be historically linked to the evolution of the central star. {{Harv|Santander-García|Corradi|Balick|Mampaso|2004}}

The Ant Nebula is 8,000 light years away from Earth and it has a magnitude of 13.8.