| Henize 70 | |
| Credit: | Dylan O’Donnell |
| Epoch: | J2000 |
| Type: | emission |
| Type2: | Superbubble |
| Dist Pc: | ~50,000 |
| Size V: | 7′ × 8′ |
| Constellation: | Dorado |
| Dimensions: | 346 × 396 ly |
| Notes: | Superbubble |
| Names: | Henize 70, N70, LHA 120-N 70, DEM L 301, MCELS L-373 |
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 Hα 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 SII and Hα 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 SII/Hα line ratios although most supernova remnants have higher NII/Hα line ratios.