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Supernova TaxonomySupernova TaxonomyFirst published 1996 October 17;last updated 2002 February 12 byM. Montes.A Supernovae Taxonomy Flow ChartDescription of the Flow ChartThe observational classes are in sharp-cornered boxes. Theoreticalinterpretations (i.e. possible progenitors) are listed in theboxes with rounded corners. Examples are listed underneath theobservational classes. It should be noted that SN 1987A had a fairly oddbehavior (for fairly well understood reasons) and is certainlynot a prototypical SN IIP. It was rather sub-luminous, andwhile it may represent a certain population of sub-luminous SN II, wewill probably not detect too many members of this population preciselybecause they are sub-luminous. SN 1987A may be better classified as anSN IIpec.A theoretical interpretation of observations has driven theorganization of this plot. At the left side, there is little or nohydrogen present in the ejecta; as one moves right, there is increasingevidence for hydrogen. SN IIP have a plateau in their post-maximumlight curve, while SN IIL do not (Barbon et al 1979). SN IIL and IIPmay differ in the amount of hydrogen present in their envelope(see Popov 1993); they may also differ spectroscopically (Schlegel1996). I am not familiar with the light curves (as opposed to spectra)of SN IIn in general. In particular, the light curve of SN 1988Z isseveral magnitudes brighter (slower decline) than either IIP or IILlight curves at very late times (Stathakis & Sadler 1991; Aretxaga etal. 1999).Current Classification SchemeThe current classification scheme has these broad divisions: SN I showno hydrogen lines in their early spectra; SN II do show hydrogen intheir early spectra. Subclasses determined by spectral evidence aredenoted by lower-case letters, Ia, Ib, Ic, IIb (Woosley et al. 1987;Filippenko 1988), and IIn (Schlegel 1990) . Subclassesdetermined by certain properties of the (usually) B orV light curves are denoted by upper-case letters, such asIIP and IIL (Barbon et al 1979; Doggett & Branch 1985). There is somesuggestion (Schlegel 1996) that there are particular spectroscopicdifferences between SNe IIL and IIP; currently these SNe are most easilyidentified by their light curves. Host GalaxiesSN Ia have been observed to occur in all types ofgalaxies. SNe Ib, Ic, and II have only been observed in variousspirals, barred spirals, and irregular galaxies. In a recentpaper, van den Bergh, Li, & Filippenko (2003) find that five SNeof types SNe Ib/c and II observed in their sample occurred inbright E or S0 galaxies, but please read their discussioncarefully. In any case, they find no more 3% of SNe Ib/c and IIoccur in S/E0. Relevant graphs by other researchers are presented attheInternational Supernova Network.Radio EmissionRadio emission has been observed for some supernovae in SN types Ib,Ic, IIb, IIn, IIL, and now IIP. Radio emission is an indicator of thepresence of circumstellar medium (CSM). The SN IIpec 1987A was observedin the radio, but it probably would not have been observed at thedistance of a few megaparsecs. Radio emission has not been observedfrom SNe Ia, but certain models of SN Ia propose radio emission at somelevel before maxima. The sole IIP observed near the time of itsexplosion in the radio is SN 1999em (Lacey et al. 1999); additionallythe SN IIP 1923A has recently been detected in the radio (Eck et al.1998). It is possible that SNe IIP are not usually observed in the radiosince their usually tenuous CSM imply much weaker radio emission thanwe are able to detect with typical observations.Distance estimates, observed B or V magnitudes, SN type,and age since optical maximum are used to help decide whether or not (andwhen) to observe SN in the radio. A few supernovae (SNe 1978K, 1981K,1986J) have been serendipitously discovered in the radio before they weresubsequently observed at other wavelengths. A list of supernovae that have been observed (both detections andnon-detections) in the radio may be found here.X-Ray EmissionX-Ray emission is another indicator of the presence of reasonably densecircumstellar medium, and has been observed for a small number ofsupernovae at different ages. Many SN IIn (SNe 1988Z, 1995N, 1994W, ...),some IIL (1980K, 1979C), all the recent nearby objects ( 1987A, 1993J, and1994I), and a IIP (1999em) have been at least detected in x-rays. To myknowledge, no SNe Ia have been detected in x-rays. Frequently (but not always) radio detection is used to determine whether ornot to observe at x-ray wavelengths.A list of supernovae detected in X-Rays may be found here. PhotometryPoznanski et al. (2002) have proposed a classification method based onphotometry when spectroscopy is not available. The capabilities andlimitations of this method are described in their article (see thereferences section below).Supernova ProgenitorsSupernova Types II, Ib, & IcAll observations taken together imply that SNe II, Ib, and Ic arise fromstars that are young, and were initially very massive. These supernovaeare believed to form when their core collapses, that is, when nuclearburning cannot produce any more energy. Spectra and numerical models ofSNe Ib & SNe Ic imply they have have lost much or all of their hydrogenenvelopes; SNe Ic may also have lost much of their helium envelopes (see,for example, Nomoto et al. 1995; Nomoto et al. 1996; Filippenko 1997). Models and spectra of SNe IIn seem to imply the shock and ejecta of thesupernova are interacting with a very dense circumstellar medium (see, forexample, Cumming & Lundqvist 1997; Filippenko 1997).Type Ia Supernovae SNe Ia are believed to arise from accretiononto a white dwarf (a very old, dense, relatively low mass star that is notundergoing thermonuclear reactions in its core), although the exactpopulation has yet to be identified. In this case, a detonation(supersonic burning front) or a deflagration (subsonic burning front) [Idon't think the models are clear on this point yet] of the star occurswhen it has accreted enough matter (the exact amount depends on theparticular situation). Links to more detailed explanations may befound in the tutorialsection of my Supernova andSupernova Remnants pages.What is NOT Included in the Taxonomy ChartI have not included SN IIn or SN IIpec (peculiar) supernovae. I madethis chart awhile back, and cannot remember why I did not include them.Perhaps they will be included in a later version of this chart.SN IIpec was proposed by Doggett & Branch (1985) to be a catch-all for all of Zwicky's SN III, SN IV, and SN V. I believe that the current class SNIIpec contains those SN II that are not SN IIL, IIP, IIb, or IIn.SN IIn were introduced in Schlegel (1990). Members of the classtypically have absent (or weak) H-alpha absorption, and narrow H-alphaemission on a broad base. Several members of this class have beenobserved in radio and X-Ray. Some recent ideas on the diversity of SNIIn are presented in Cumming & Lundqvist (1997). Some supernovaclassified as Zwicky's SN III, IV, and V were probably IIn. Some IIn(SN 1986J, SN 1978K) have been called SN V in the past.For the curious, SN 1961I was listed as an SN III; SN 1961F is theprototype of Zwicky's SN IV; and SN 1961V was for quite some time thesole member of Zwicky's SN V (Zwicky 1964). (For a more recentdiscussion SN V, see Ball 1993.) SN V are a weird case, and manybelieve that SN 1961V was actually the outburst of a Luminous BlueVariable. For the latest on SN 1961V, see Stockdale et al (2001) andFilippenko et al (1995). SN III and SN IV have been reclassified asvarious SN IIpec (Doggett & Branch, 1985; Patat et al, 1993).The ChartThis chart is also available as an EPS file at taxonomy.sne.ps. This chart is also available as an EPS file at taxonomy.sne.ps.Published ReferencesThese are more or less recent references. I hope I am not slightinganyone by leaving out even other references. Please consult thereferences of these references for more information.I.Aretxaga, S. Benetti, R.J. Terlevich, A.C. Fabian, E. Cappellaro,M. Turatto, and M. Della Valle 1999, Monthly Notices ofthe Royal Astronomical Society, 309, 343 [SN IIn]L. Ball 1993, Proceedings of the Astronomical Society ofAustralia, 10, 357 (Workshop Proceedings with abstracts by:A.J. Turtle; E.M. Sadler; D. Allen; S.D. Ryder; L. Staveley-Smith; A.Achterburg; M.A. Dopita; and L. Ball.) [SN V]R. Barbon, F. Ciatti, and L. Rosino 1979, Astronomy andAstrophysics, 72, 287 [SN IIP, SN IIL]R.J.Cumming and P. Lundqvist 1997, in Advances in Stellar Evolution, ed. R.T. Rood (Cambridge: Cambridge University Press), p. 297e-print atxxx.lanl.gov [SN IIn]J.B. Doggett and D. Branch 1985, AstronomicalJournal, 90, 230 [SNI, SNIIP, SNIIL, SNIII, SNIV, SNV, SNIIpec]C.R.Eck, D.A. Roberts, J.J. Cowan, and D. Branch 1998, AstrophysicalJournal, 508, 664 [SN IIP]A.V.Filippenko 1997, in Annual Reviews of Astronomy andAstrophysics, 35, 309 [SN Ia,Ib,Ic,IIP,IIL,IIn]A.V. Filippenko 1996, in Thermonuclear Supernovae, ed. R.Canal, P. Ruiz-Lapuente, and J. Isern (Dordrecht: Kluwer) [SNIa,Ib,Ic] A.V.Filippenko, A.J. Barth, G.C. Bower, L.C. Ho, G.S. Stringfellow,R.W. Goodrich and A.C. Porter 1995,Astronomical Journal, 110, 2261 [SN1961V, SNV]A.V. Filippenko 1991, in Supernovae, ed. S.E. Woosley(New York:Springer-Verlag), p. 467 [SN Ib/IIb]A.V. Filippenko 1988, Astronomical Journal,96, 1941R.P. Harkness and J.C. Wheeler 1990, in Supernovae,ed. A. Petschek, page 1C.K.Lacey, R.A. Sramek, S.D. Van Dyk, and K.W. Weiler 1999,International Astronomical Union Circular, 7318, 2 [SNIIP] K. Nomoto, K. Iwamoto, T. Suzuki, O.R. Pols, H. Yamaoka,M. Hashimoto, P. Hoflich, and E.P.J. Van Den Heuvel 1996, inCompact Stars in Binaries, J. van Paradijs et al., (eds),p. 119 [SN Ib,Ic,IIb,IIL]K. Nomoto, K. Iwamoto, and T. Suzuki 1995 PhysicsReports, 256, 173 [SN Ib,Ic,IIb,IIL]F.Patat, R. Barbon, E. Capellaro, and M. Turatto 1993, Astronomy and Astrophysics Supplement Series, 98, 443[SN IIP,IIL]D.V.Popov 1993, Astrophysical Journal, 414, 712 [SNIIP,IIL] D. Poznanski,A. Gal-Yam, D. Maoz, A.V. Filippenko, D.C. Leonard, and T. Matheson2002, e-print at LANL [Photometric Classification of SNe]E.M.Schlegel 1990, Monthly Notices of the Royal Astronomical Society, 244, 269 [SN IIn]E.M.Schlegel 1996, Astronomical Journal, 111, 1660.[SNIIL] R.A. Stathakis and E.M. Sadler 1991, Monthly Notices of theRoyal Astronomical Society, 250, 786C.J. Stockdale, M.P. Rupen, J.J. Cowan, Y.-H. Chu, and S.S. Jones2001, Astronomical Journal, 122, 283.[SN 1961V,SNV]S. van den Bergh,W. Li, and A. V. Filippenko 2003 [SN types and host galaxymorphology] S.E. Woosley, P.A. Pinto, P.G. Martin, and T.A. Weaver 1987,Astrophysical Journal, 318, 664F.Zwicky 1964, Astrophysical Journal, 139, 514. [SN1961V, SNV] F. Zwicky 1965, in Stars and Stellar Systems, Vol. 8,ed. by L.H. Aller and D.B. McLaughlin (Chicago: Univ. of ChicagoPress), p. 367Other Online ResourcesDr. M.Richmond's CurrentSupernovae Taxonomy.An online compendium of Supernova andSupernova Remnant Resources by M. MontesLast updated 2002 February 12.M. Montesmontes@rsd.nrl.navy.mil |
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