 | |
| Event type | Supernova remnant |
|---|---|
| Type II (?) | |
| Constellation | Aquila |
| Right ascension | 18h 56m 11s |
| Epoch | J2000 |
| Galactic coordinates | G034.6-00.5 |
| Distance | ~3,000 parsecs |
| Remnant | PSR B1853+01 |
| Notable features | Interaction with a molecular cloud |
3C 392 (also known as SNR G034.6-00.5, W44 and CTB 60) [1] is a supernova remnant located in the constellation Aquila. It was discovered by Gart Westerhout in 1958 as part of a study of continuous radiation in the Milky Way at a frequency of 1390 MHz. [2]
3C 392 is a supernova remnant of mixed morphology characterized by a bright radio-band shell and concentrated thermal X-ray emission from its center. In the radio band, 3C 392 has the appearance of a quasi-elliptic asymmetric bright shell, its emission being most intense along the eastern boundary; in the western region a bright arc can be seen. [3] In the X-ray spectrum it presents continuums of radiant recombination of highly ionized atoms, a common characteristic of other remnants with mixed morphology. The emission is predominantly thermal, which is based on the presence of magnesium, silicon and sulfur emission lines. [4] Likewise, the emission in hard X-rays has an arc-shaped structure that is correlated in space with the filament seen in the radio band. [5] 3C 392 has also been detected in gamma rays, probably originating from the decay of neutral pions. [6]
3C 392 is one of the few demonstrated cases of interaction between a supernova remnant and a molecular cloud, as corroborated by observations of OH masers at 1720 MHz. [4] Two stellar objects have been discovered at the interface between 3C 392 and an H II region massive youth. [5]
3C 392 is associated with the pulsar PSR B1853+01, located to the south of the rest of the supernova, indicating that 3C 392 comes from a core collapse (CC) supernova. The wind from the pulsar has created a small synchrotron nebula (PWN) observed in both radio frequencies and X-rays. [7]
The age of 3C 392, evaluated by the characteristic age of the associated pulsar, is approximately 20,000 years. [8] Another different estimate, calculated by the age of the thermal plasma, 16,700 ± 2,500 years, is comparable to the previous value; however, its dynamic age—based on the speed and size of the shock wave—is considerably higher, although it is subject to a wide margin of error (55,000 ± 20,000 years). [9]
3C 392 is located at a distance between 2200 [10] and 3000 [11] parsecs, and is located in a complex region of the inner galactic plane. It is immersed in the W48 molecular cloud complex, a rich region of star formation.
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