SN 2005gl: Difference between revisions
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'''SN 2005gl''' was a [[supernova]] in the [[barred-spiral galaxy]] [[NGC 266]]. It was discovered using CCD frames taken October 5, 2005, from the 60 cm automated telescope at the Puckett Observatory in Georgia, and reported by Tim Puckett in collaboration with Peter Ceravolo. It was independently identified by Yasuo Sano in Japan.<ref name="iauc8615">{{cite news |
'''SN 2005gl''' was a [[supernova]] in the [[barred-spiral galaxy]] [[NGC 266]]. It was discovered using CCD frames taken October 5, 2005, from the 60 cm automated telescope at the Puckett Observatory in Georgia, US, and reported by Tim Puckett in collaboration with Peter Ceravolo. It was independently identified by Yasuo Sano in Japan.<ref name="iauc8615">{{cite news |
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| title=Circular No. 8615 | date=2005-10-12 |
| title=Circular No. 8615 | date=2005-10-12 |
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| publisher=Central Bureau for Astronomical Telegrams, IAU |
| publisher=Central Bureau for Astronomical Telegrams, IAU |
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Revision as of 11:53, 12 September 2013
| Event type | Supernova  |
|---|---|
| Type IIn | |
| Date | 2005-10-05 |
| Constellation | Pisces |
| Right ascension | 03h 08m 16.05s[1] |
| Declination | +32° 16′ 56.8″[1] |
| Epoch | J2000.0 |
| Galactic coordinates | NGC 266 |
| Distance | 66 Mpc |
| Progenitor | NGC266 LBV 1 |
| Progenitor type | Luminous blue variable |
| Other designations | SN 2005gl |
SN 2005gl was a supernova in the barred-spiral galaxy NGC 266. It was discovered using CCD frames taken October 5, 2005, from the 60 cm automated telescope at the Puckett Observatory in Georgia, US, and reported by Tim Puckett in collaboration with Peter Ceravolo. It was independently identified by Yasuo Sano in Japan.[1] The supernova was located 29.8″ east and 16.7″ north of the galactic core.[2] Based upon its spectrum, this was classfied as a Type IIn core-collapse supernova. It has a redshift of z = 0.016, which is the same as the host galaxy.[3]
Using archived images from the Hubble Space Telescope, a candidate progenitor star was identified. This is believed to be a luminous blue variable (LBV), similar to Eta Carinae, with an absolute magnitude of −10.3 and a surface temperature of about 13,000 K. However, there is a small probability that the source was instead located in a compact cluster of stars.[4]
References
- ^ a b c d "Circular No. 8615". Central Bureau for Astronomical Telegrams, IAU. 2005-10-12. Retrieved 2011-07-05.
- ^ Puckett, T.; Ceravolo, P.; George, D. "Supernova 2005gl in NGC 266". Central Bureau Electronic Telegrams. Bibcode:2005CBET..250....1P.
{{cite news}}: CS1 maint: multiple names: authors list (link) - ^ "Classification of SNe 2005gl and 2005gm". The Astronomer's Telegram. 2005-10-14. Retrieved 2009-05-20.
- ^ Gal-Yam, Avishay; et al. (2007). "On the progenitor of SN 2005gl and the nature of Type IIn supernovae". The Astrophysical Journal. 656: 372–381. arXiv:astro-ph/0608029. Bibcode:2007ApJ...656..372G. doi:10.1086/510523.
{{cite journal}}: Explicit use of et al. in:|author=(help)
External links
- Bishop, David. "Supernova 2005gl in NGC 266". International Supernova Network & Rochester Academy of Sciences. Retrieved 2009-04-20.
- Villard, Ray; Gal-Yam, Avishay (2009-03-22). "Hubble Uncovers an Unusual Stellar Progenitor to a Supernova". Hubble News Center. Retrieved 2009-04-20.
{{cite news}}: CS1 maint: multiple names: authors list (link)