Astronomy:3C 392
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| Event type | Supernova remnant |
|---|---|
| Spectral class | 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]
Morphology
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]
Remnant
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]
Age and distance
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.
See also
References
- ↑ "W44". http://simbad.u-strasbg.fr/simbad/sim-id.
- ↑ Westerhout, Gart (December 31, 1958). "A Survey Of the Continuous Radiation From The Galactic System At Frequency of 1390 Mc/S". http://articles.adsabs.harvard.edu/pdf/1958BAN....14..215W.
- ↑ Loru, S.; Pellizzoni, A.; Egron, E.; Righini, S.; Iacolina, M. N.; Mulas, S.; Cardillo, M.; Marongiu, M. et al. (2019-01-01). "Investigating the high-frequency spectral features of SNRs Tycho, W44, and IC443 with the Sardinia Radio Telescope". Monthly Notices of the Royal Astronomical Society 482 (3): 3857–3867. doi:10.1093/mnras/sty1194. ISSN 0035-8711. Bibcode: 2019MNRAS.482.3857L.
- ↑ 4.0 4.1 Okon, Hiromichi; Tanaka, Takaaki; Uchida, Hiroyuki; Yamaguchi, Hiroya; Tsuru, Takeshi Go; Seta, Masumichi; Smith, Randall K.; Yoshiike, Satoshi et al. (2020-02-01). "Deep XMM-Newton Observations Reveal the Origin of Recombining Plasma in the Supernova Remnant W44". The Astrophysical Journal 890 (1): 62. doi:10.3847/1538-4357/ab6987. ISSN 0004-637X. Bibcode: 2020ApJ...890...62O. https://ui.adsabs.harvard.edu/abs/2020ApJ...890...62O.
- ↑ 5.0 5.1 Onić, D. (2015-12-01). "On the Integrated Continuum Radio Spectrum of Supernova Remnant W44 (G34.7-0.4): New Insights From Planck". Serbian Astronomical Journal 191 (191): 29–37. doi:10.2298/SAJ150715004O. Bibcode: 2015SerAJ.191...29O. https://ui.adsabs.harvard.edu/abs/2015SerAJ.191...29O.
- ↑ Cardillo, M.; Tavani, M.; Giuliani, A.; Yoshiike, S.; Sano, H.; Fukuda, T.; Fukui, Y.; Castelletti, G. et al. (2014-05-01). "The supernova remnant W44: Confirmations and challenges for cosmic-ray acceleration". Astronomy and Astrophysics 565: A74. doi:10.1051/0004-6361/201322685. ISSN 0004-6361. Bibcode: 2014A&A...565A..74C. https://ui.adsabs.harvard.edu/abs/2014A&A...565A..74C.
- ↑ Onić, D. (2015-12-01). "On the Integrated Continuum Radio Spectrum of Supernova Remnant W44 (G34.7-0.4): New Insights From Planck". Serbian Astronomical Journal 191 (191): 29–37. doi:10.2298/SAJ150715004O. Bibcode: 2015SerAJ.191...29O. https://ui.adsabs.harvard.edu/abs/2015SerAJ.191...29O.
- ↑ Harrus, Ilana M.; Hughes, John P.; Singh, K. P.; Koyama, K.; Asaoka, I. (1997-10-01). "Interpretation of the Center-filled Emission from the Supernova Remnant W44". The Astrophysical Journal 488 (2): 781–791. doi:10.1086/304717. ISSN 0004-637X. Bibcode: 1997ApJ...488..781H. https://ui.adsabs.harvard.edu/abs/1997ApJ...488..781H.
- ↑ Suzuki, Hiromasa; Bamba, Aya; Shibata, Shinpei (2021-06-01). "Quantitative Age Estimation of Supernova Remnants and Associated Pulsars". The Astrophysical Journal 914 (2): 103. doi:10.3847/1538-4357/abfb02. ISSN 0004-637X. Bibcode: 2021ApJ...914..103S. https://ui.adsabs.harvard.edu/abs/2021ApJ...914..103S.
- ↑ Peron, Giada; Aharonian, Felix; Casanova, Sabrina; Zanin, Roberta; Romoli, Carlo (2020-06-01). "On the Gamma-Ray Emission of W44 and Its Surroundings". The Astrophysical Journal 896 (2): L23. doi:10.3847/2041-8213/ab93d1. ISSN 0004-637X. Bibcode: 2020ApJ...896L..23P. https://ui.adsabs.harvard.edu/abs/2020ApJ...896L..23P.
- ↑ Ranasinghe, S.; Leahy, D. A. (2018-05-01). "Revised Distances to 21 Supernova Remnants". The Astronomical Journal 155 (5): 204. doi:10.3847/1538-3881/aab9be. ISSN 0004-6256. Bibcode: 2018AJ....155..204R. https://ui.adsabs.harvard.edu/abs/2018AJ....155..204R.
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