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SN 1988Z was a prototypical type IIn supernova event in the equatorialconstellation of Leo. The apparent host is an irregular galaxy with the designation MCG +03-28-22. It has a redshift of z equal to 0.0225. This was a very luminous supernova that faded unusually slowly and has remained detectable three decades after the event. It is one of the most radio and X-ray luminous supernova ever detected, and it has been extensively studied.
This supernova displayed a number of unusual characteristics. It was unusually bright at maximum and showed very slow fading. There were strong, narrow emission lines caused by thick circumstellar material. Unlike a typical type II supernova, no P Cygni profiles or absorption lines were observed. Emission lines of neutral helium were also visible. The spectral lines displayed a complex structure that evolved over time. Decline in the Hydrogen-alpha line strength was unusually slow and lacked an explanation in terms of radioactive decay. The overall picture suggested interaction between the supernova ejecta and a dense circumstellar medium.
A year after the event, radio emission from the supernova was detected using the Very Large Array. The host galaxy shows a redshift of z equal to 0.022, making this the most distant radio supernova detected at that time. It was also one of the most luminous radio supernova discovered. The radio properties indicated a very massive progenitor star in the range of 20–30 M☉. In the late evolutionary stages of the star, it underwent a high rate of mass loss on the order of 10 M☉·yr, which created a dense circumstellar cocoon. In 1996, X-ray emission from the supernova was detected by ROSAT, making it the most distant supernova to be detected in this band. The estimated X-ray luminosity was 10 erg·s, which is consistent with a supernova event within dense circumstellar material.
Most studies now favor a model of a very massive progenitor that ejected up to 10 M☉ at a rate of around 10 M☉·yr for a period of about 10,000 years prior to the explosion. The mass loss rate apparently ramped up during the final millennium prior to core collapse.
References
^ Barbon, R.; Buondi, V.; Cappellaro, E.; Turatto, M. (2008), "VizieR Online Data Catalog: Asiago Supernova Catalogue (Version 2008-Mar)", VizieR On-line Data Catalog, Bibcode:2008yCat.2283....0B.
^ Smith, Nathan; et al. (April 2017), "Endurance of SN 2005ip after a decade: X-rays, radio and Hα like SN 1988Z require long-lived pre-supernova mass-loss", Monthly Notices of the Royal Astronomical Society, 466 (3): 3021–3034, arXiv:1612.02011, Bibcode:2017MNRAS.466.3021S, doi:10.1093/mnras/stw3204.
Pollas, C.; et al. (December 15, 1988), Marsden, Brian G. (ed.), "Supernova 1988Z in MCG +03-28-022", IAU Circulars, 4691, Central Bureau for Astronomical Telegrams, retrieved 2024-01-08.
Heathcote, S.; et al. (December 1988), Marsden, B. G. (ed.), "Supernova 1988Z in MCG +03-28-022", IAU Circular, 4693: 1, Bibcode:1988IAUC.4693....1H.
Turatto, M.; et al. (May 1993), "The type II supernova 1988Z in MCG +03-28-022 : increasing evidence of interaction of supernova ejecta with a circumstellar wind", Monthly Notices of the Royal Astronomical Society, 262: 128–140, Bibcode:1993MNRAS.262..128T, doi:10.1093/mnras/262.1.128.
van Dyk, Schuyler D.; et al. (December 1993), "SN 1988Z: The Most Distant Radio Supernova", The Astrophysical Journal, 419: L69 – L72, Bibcode:1993ApJ...419L..69V, doi:10.1086/187139.
Fabian, A. C.; Terlevich, R. (May 1996), "X-ray detection of Supernova 1988Z with the ROSAT High Resolution Imager", Monthly Notices of the Royal Astronomical Society, 280 (1): L5 – L8, Bibcode:1996MNRAS.280L...5F, doi:10.1093/mnras/280.1.L5.
Aretxaga, I. (May 2000), Arthur, Jane; et al. (eds.), "The Hyper-Energetic SN 1988Z", Astrophysical Plasmas: Codes, Models, and Observations, Proceedings of the conference held in Mexico City, October 25-29, 1999, Revista Mexicana de Astronomía y Astrofísica (Serie de Conferencias), vol. 9, pp. 286–287, Bibcode:2000RMxAC...9..286A.
Chugai, N. N.; Danziger, I. J. (May 1994), "SN 1988Z: low-mass ejecta colliding with the clumpy wind?", Monthly Notices of the Royal Astronomical Society, 268: 173–180, Bibcode:1994MNRAS.268..173C, doi:10.1093/mnras/268.1.173.
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