 | |
| 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]
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 remains 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, whose emission probably comes 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". simbad.u-strasbg.fr. Retrieved 2024-07-18.
- ^ Westerhout, Gart (December 31, 1958). "A Survey Of the Continuous Radiation From The Galactic System At Frequency of 1390 Mc/S". ADSABS at HARVARD. Retrieved July 17, 2024.
- ^ Loru, S.; Pellizzoni, A.; Egron, E.; Righini, S.; Iacolina, M. N.; Mulas, S.; Cardillo, M.; Marongiu, M.; Ricci, R.; Bachetti, M.; Pilia, M.; Trois, A.; Ingallinera, A.; Petruk, O.; Murtas, G. (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: 3857–3867. doi: 10.1093/mnras/sty1194. ISSN 0035-8711.
- ^ a b Okon, Hiromichi; Tanaka, Takaaki; Uchida, Hiroyuki; Yamaguchi, Hiroya; Tsuru, Takeshi Go; Seta, Masumichi; Smith, Randall K.; Yoshiike, Satoshi; Orlando, Salvatore; Bocchino, Fabrizio; Miceli, Marco (2020-02-01). "Deep XMM-Newton Observations Reveal the Origin of Recombining Plasma in the Supernova Remnant W44". The Astrophysical Journal. 890: 62. ISSN 0004-637X.
- ^ a b 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: 29–37. doi: 10.2298/SAJ150715004O.
- ^ Cardillo, M.; Tavani, M.; Giuliani, A.; Yoshiike, S.; Sano, H.; Fukuda, T.; Fukui, Y.; Castelletti, G.; Dubner, G. (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.
- ^ 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: 29–37. doi: 10.2298/SAJ150715004O.
- ^ 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: 781–791. doi: 10.1086/304717. ISSN 0004-637X.
- ^ Suzuki, Hiromasa; Bamba, Aya; Shibata, Shinpei (2021-06-01). "Quantitative Age Estimation of Supernova Remnants and Associated Pulsars". The Astrophysical Journal. 914: 103. ISSN 0004-637X.
- ^ 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: L23. ISSN 0004-637X.
- ^ Ranasinghe, S.; Leahy, D. A. (2018-05-01). "Revised Distances to 21 Supernova Remnants". The Astronomical Journal. 155: 204. ISSN 0004-6256.
|
| |
| 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]
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 remains 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, whose emission probably comes 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". simbad.u-strasbg.fr. Retrieved 2024-07-18.
- ^ Westerhout, Gart (December 31, 1958). "A Survey Of the Continuous Radiation From The Galactic System At Frequency of 1390 Mc/S". ADSABS at HARVARD. Retrieved July 17, 2024.
- ^ Loru, S.; Pellizzoni, A.; Egron, E.; Righini, S.; Iacolina, M. N.; Mulas, S.; Cardillo, M.; Marongiu, M.; Ricci, R.; Bachetti, M.; Pilia, M.; Trois, A.; Ingallinera, A.; Petruk, O.; Murtas, G. (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: 3857–3867. doi: 10.1093/mnras/sty1194. ISSN 0035-8711.
- ^ a b Okon, Hiromichi; Tanaka, Takaaki; Uchida, Hiroyuki; Yamaguchi, Hiroya; Tsuru, Takeshi Go; Seta, Masumichi; Smith, Randall K.; Yoshiike, Satoshi; Orlando, Salvatore; Bocchino, Fabrizio; Miceli, Marco (2020-02-01). "Deep XMM-Newton Observations Reveal the Origin of Recombining Plasma in the Supernova Remnant W44". The Astrophysical Journal. 890: 62. ISSN 0004-637X.
- ^ a b 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: 29–37. doi: 10.2298/SAJ150715004O.
- ^ Cardillo, M.; Tavani, M.; Giuliani, A.; Yoshiike, S.; Sano, H.; Fukuda, T.; Fukui, Y.; Castelletti, G.; Dubner, G. (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.
- ^ 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: 29–37. doi: 10.2298/SAJ150715004O.
- ^ 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: 781–791. doi: 10.1086/304717. ISSN 0004-637X.
- ^ Suzuki, Hiromasa; Bamba, Aya; Shibata, Shinpei (2021-06-01). "Quantitative Age Estimation of Supernova Remnants and Associated Pulsars". The Astrophysical Journal. 914: 103. ISSN 0004-637X.
- ^ 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: L23. ISSN 0004-637X.
- ^ Ranasinghe, S.; Leahy, D. A. (2018-05-01). "Revised Distances to 21 Supernova Remnants". The Astronomical Journal. 155: 204. ISSN 0004-6256.