SN 2005hk
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 Host galaxy UGC 272 imaged by Legacy Surveys | |
| Event type | Supernova |
|---|---|
| Type Iax[1] | |
| Date | October 30, 2005[2][3] |
| Instrument | SDSS[2] |
| Constellation | Cetus |
| Right ascension | 00h 27m 50.89s[4] |
| Declination | −01° 11′ 53.3″[4] |
| Epoch | J2000 |
| Distance | 185.1 Mly (56.75 Mpc)[5] |
| Redshift | 0.012993±0.000041[1] |
| Host | UGC 272[1] |
SN 2005hk was a peculiar Type Iax supernova event in UGC 272 [d], which is a barred spiral galaxy[6] in the equatorial constellation of Cetus. This galaxy is located at a distance of approximately 185.1 million light-years (56.75 Mpc) from the Milky Way.[5] The supernova was discovered October 30, 2005.[7]
This event was discovered by J. Burket and W. Li on October 30, 2005. At magnitude 17.5, it was located 17.2″ east and 6.9″ north of the UGC 272 nucleus.[7] This supernova was independently discovered on images taken with the SDSS telescope dated October 28. The event was not observed on images taken two days earlier.[2]
The early spectra of SN 2005hk appeared peculiar, with prominent lines of double-ionized iron and only weak lines of intermediate mass elements. It was similar to SN 2002cx, with an unusually slow photospheric velocity of 6,000 km/s. These peculiarities could not be readily explained as the result of a large asymmetry in the explosion.[8] It was under-luminous for a Type Ia supernova, reaching peak light on November 9 with a near-normal spectrum for a supernova of this type. The later spectrum then continued to resemble SN 2002cx as it evolved.[3][9]
At later stages, this supernova did not show the nebular emission lines of a normal Type Ia supernova, instead showing iron and calcium lines.[10] It was suggested that the peculiarity of this event was due to a deflagration explosion.[11] However, observations with the Hubble Space Telescope showed no evidence of unburnt material at late stages, ruling out a "complete deflagration" model.[10] Type Iax supernovae such as SN 2005hk are now widely interpreted as a pure deflagration of a Chandrasekhar mass carbon-oxygen white dwarf. This explosion may have been insufficient to completely unbind the progenitor. Instead, it could have left behind a stellar remnant that is coated in the nuclear products of the explosion, including 56Ni.[12]
References
- 1 2 3 Friedman, Andrew S.; et al. (October 2004), "CfAIR2: Near-infrared Light Curves of 94 Type Ia Supernovae", The Astrophysical Journal, 613 (2): 1120–1132, arXiv:astro-ph/0105490, Bibcode:2004ApJ...613.1120G, doi:10.1086/422986.
- 1 2 3 Barentine, J.; et al. (November 2005), Green, D. W. E. (ed.), "Supernovae 2005hk-2005ik", Central Bureau Electronic Telegrams, 268: 1, Bibcode:2005CBET..268....1B.
- 1 2 Stanishev, V.; et al. (August 2007), "The Peculiar Type Ia Supernova 2005hk", The Multicolored Landscape of Compact Objects and their Explosive Origins, AIP Conference Proceedings, vol. 924, pp. 336–341, arXiv:astro-ph/0611354, Bibcode:2007AIPC..924..336S, doi:10.1063/1.2774878.
- 1 2 Zheng, Chen; et al. (May 2008), "First-Year Spectroscopy for the Sloan Digital Sky Survey-II Supernova Survey", The Astronomical Journal, 135 (5): 1766–1784, arXiv:0802.3220, Bibcode:2008AJ....135.1766Z, doi:10.1088/0004-6256/135/5/1766.
- 1 2 Tully, R. Brent; et al. (October 2013), "Cosmicflows-2: The Data", The Astronomical Journal, 146 (4): 25, arXiv:1307.7213, Bibcode:2013AJ....146...86T, doi:10.1088/0004-6256/146/4/86, S2CID 118494842, 86.
- ↑ Phillips, M. M.; et al. (April 2007), "The Peculiar SN 2005hk: Do Some Type Ia Supernovae Explode as Deflagrations?", The Publications of the Astronomical Society of the Pacific, 119 (854): 360–387, arXiv:astro-ph/0611295, Bibcode:2007PASP..119..360P, doi:10.1086/518372.
- 1 2 Quimby, R.; et al. (October 31, 2005), Green, D. W. E. (ed.), "S/2005 P 1, S/2005 P 2; 2005hh, 2005hi, 2005hj, 2005hk", International Astronomical Union Circular, 8625: 1, retrieved 2026-03-23.
- ↑ Chornock, Ryan; et al. (May 2006), "Spectropolarimetry of the Peculiar Type Ia Supernova 2005hk", The Publications of the Astronomical Society of the Pacific, 118 (843): 722–732, arXiv:astro-ph/0603083, Bibcode:2006PASP..118..722C, doi:10.1086/504117.
- ↑ Sahu, D. K.; et al. (June 2008), "The Evolution of the Peculiar Type Ia Supernova SN 2005hk over 400 Days", The Astrophysical Journal, 680 (1): 580–592, arXiv:0710.3636, Bibcode:2008ApJ...680..580S, doi:10.1086/587772.
- 1 2 McCully, Curtis; et al. (May 2014), "Hubble Space Telescope and Ground-based Observations of the Type Iax Supernovae SN 2005hk and SN 2008A", The Astrophysical Journal, 786 (2), id. 134, arXiv:1309.4457, Bibcode:2014ApJ...786..134M, doi:10.1088/0004-637X/786/2/134.
- ↑ Maund, Justyn R.; et al. (October 2010), "A Spectropolarimetric View on the Nature of the Peculiar Type I SN 2005hk", The Astrophysical Journal, 722 (2): 1162–1174, arXiv:1008.3985, Bibcode:2010ApJ...722.1162M, doi:10.1088/0004-637X/722/2/1162.
- ↑ Callan, F. P.; et al. (May 2024), "Including a luminous central remnant in radiative transfer simulations for Type Iax supernovae", Monthly Notices of the Royal Astronomical Society, 530 (2): 1457–1473, arXiv:2403.15084, Bibcode:2024MNRAS.530.1457C, doi:10.1093/mnras/stae847.
