Emission nebula | |
---|---|
Superbubble | |
![]() Amateur photograph of Henize 70 | |
Observation data: J2000 epoch | |
Right ascension | 05h 43m 17.5s[1] |
Declination | −67° 50′ 48″[1] |
Distance | ~50,000[2] pc |
Apparent dimensions (V) | 7′ × 8′[3] |
Constellation | Dorado |
Physical characteristics | |
Dimensions | 346 × 396 ly[4][a] |
Notable features | Superbubble |
Designations | Henize 70,[5] N70,[3] LHA 120-N 70,[3][6] DEM L 301, MCELS L-373[6] |
Henize 70 (N70) is a faint[7] emission nebula[8] and superbubble[5][4][9][10] located in the Large Magellanic Cloud. It is located 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.[7] 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 instead of a planetary nebula.[8]
In a paper published in 1978, it was proposed that stellar winds could be a major part of the formation of Henize 70 and other emission nebulae.[11] Later, in a scientific article 1981 it was mentioned that it was more likely from a supernova explosion rather than stellar winds.[12] Another study in 2014 measured high SII and Hα ratios, indicating that it is not a supernova remnant.[13]
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.[14]