Henize 70 (N70) is a faint emission nebula and superbubble located in the Large Magellanic Cloud in the constellation of Dorado.
Henize 70 was first observed in 1950 in a survey of bright planetary nebulae. Based on appearance it was proposed that it might be a supernova remnant. In 1956, it was added to a catalogue of Hñ emission stars and nebulae by Karl Gordon Henize, where it was described as an emission nebula rather than a planetary nebula.
A paper published in 1978 proposed that the formations of Henize 70 and other emission nebulae could be due to stellar winds. Later in 1981, a scientific article mentioned a higher likeliness of a supernova explosion forming the nebula instead of stellar winds. A 2014 study measured that Henize 70 featured high S<sub>II</sub> and Hñ ratios, indicating that it is not a supernova remnant.
Henize 70 has spectral line ratios relatively similar to that of supernova remnants due to having similar S<sub>II</sub>/Hñ line ratios although most supernova remnants have higher N<sub>II</sub>/Hñ line ratios.