AFGL 2591
AFGL 2591 is a star forming region in the constellation Cygnus. Its dense cloud of gas and dust make its interior invisible to optical telescopes. Images in the infrared show a bright young stellar object, with an associated reflection nebula seen as a glowing cone projecting from the young star. A cluster of stars is forming within the molecular cloud, but most of the infrared radiation is coming from this star, AFGL 2591-VLA3.[3]
| Reflection nebula | |
|---|---|
| molecular cloud | |
| Observation data: J2000 epoch | |
| Right ascension | 20h 29m 24.867s[1] |
| Declination | +40° 11′ 19.41″[1] |
| Distance | 3330±110[2] pc |
| Apparent diameter | 0.51' [1] |
| Constellation | Cygnus |
| Physical characteristics | |
| Radius | est. 0.87–2.0[2] pc |
| Notable features | high-mass star-forming region[3] |
| Designations | AFGL 2591 IRAS 20275+4001 RAFGL 2591[1] |
Initially AFGL 2591 was thought to be a single young, massive star expelling clouds of gas and dust in multiple events. It was estimated to be about 10 times the mass of the sun and at a distance of only 1,000 parsecs (3,300 light-years).[4]
References
- "Basic data: RAFGL 2591 — Young Stellar Object". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 28 April 2014.
- Johnston, K. G.; Shepherd, D. S.; Robitaille, T. P.; Wood, K. (2013). "The standard model of low-mass star formation applied to massive stars: a multi-wavelength picture of AFGL 2591". Astronomy & Astrophysics. 551: A43, 1–23. arXiv:1212.1719. Bibcode:2013A&A...551A..43J. doi:10.1051/0004-6361/201219657.
- Sanna, A.; Reid, M. J.; Carrasco-González, C.; et al. (2012). "Clustered star formation and outflows in AFGL 2591". The Astrophysical Journal. 745 (2): 191–200. arXiv:1111.0843. Bibcode:2012ApJ...745..191S. doi:10.1088/0004-637X/745/2/191.
- "Gemini Spies Strong Stellar Gusts in Nearby Massive Star". Gemini Observatory. 23 July 2001. Retrieved 28 April 2014.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.