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Weird and Wild Supernovae Mem. S.A.It. Vol. 81, 367 c SAIt 2010 Memorie della Weird and wild supernovae M. Della Valle1;2 1 Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, I-80131 Napoli, Italy 2 International Center for Relativistic Astrophysics, Piazzale della Repubblica 2, I-65122, Pescara, Italy, e-mail: [email protected] Abstract. I review the observational status of Supernovae originating from the explosion of massive stars. Key words. Stars: Supenovae High Energy: Gamma-ray Bursts 1. Introduction spect to the past and to detect SNe up to very faint luminosity levels (Rmax ∼ 24 − 25) The beginning of the modern study of and up to distance of cosmological interest Supernovae (SNe) started about ∼ 70 years ago (z = 0:83 (Perlmutter et al. 1998)). In the with the pioneristic works of Zwicky (1942) last ten years (“Modern Times”) SN observa- and Minkowski (1942) on SN rates and SN tions have been characterized by fully exploit- classification. As a consequence of the evo- ing new observational opportunities, such as: lution of astronomical instrumentations during i) 10m class telescopes, which accomplished the years (larger telescopes and detectors sen- the the spectroscopic follow-up of SNe dis- sitivity, better spatial and temporal resolution covered with HST (Riess et al. 2004); ii) gath- observations, multiwavelnghts approach due ering multi-wavelengths observations in radio to observations from space) the “Supernova (Weiler et al. 2002); X-ray (Campana et al. story” can be crudely summarized in three 2006) and UV (Panagia 2003; Immler et al. different chronological stages. I identify as 2007); iii) robotic telescopes for SN searches “Heroic Times” the epoch from early 40’s to in the local universe aimed at improving the the end of 70’s, in which observations were local SN rate measurements (Weidong et al. carried out with ground-based telescopes and 2010); iv) moderately deep surveys (z < 1) data were collected on photographic plates. aimed at measuring the SN rates at different The occurence of SN 1987A in the LMC redshifts (Botticella et al. 2008). boosted enormously the interest for SNe, start- ing a real SN “Golden Age”. In those years The increasing number of SN detections entirely new classes of SNe have been dis- (from about 30/year at the end of 80’s to covered and the SN taxonomy has been ac- current 600/year) and their systematic spectro- cordingly revised (Filippenko 1997). The use scopic and photometric foolow-up has made of CCD arrays coupled with 4m class tele- possible to discover new classes of rare SNe, scopes allowed to increase the rate of SN dis- such as broad-lined SNe-Ibc, a fraction of coveries by an order of magnitude with re- which is connected with Gamma-ray Bursts 368 Della Valle: Supernovae (Guetta & Della Valle 2007), Luminous ence of H-Balmer lines (Filippenko 1997). Blue Variable-SNe (Pastorello et al. 2007a); SNe of type II (SNe-II) have been always ultra-faint (Pastorello et al. 2007b) and ultra- discovered in Spirals and never in Ellipticals luminous (Quimby et al. 2009) SNe, very which are essentially formed by an old stel- fast evolving objects such as SN 2002bj lar populations. Both these facts have consol- (Poznaski et al. 2009) and objects like SN idated the general consensus that SNe-II orig- 2005E (Perets et al. 2009) or SN 2005cz inate from the collapse of the core of massive (Kawabata et al. 2009) which occur in “un- stars > 8 − 10M (Iben & Renzini 2000). The usual” environments, characterized by the lack photometric behaviour shows a broad range of of trace of recent star formation, although both luminosity at maximum, spanning more than a SNe exhibit properties of core-collapse events. factor 1000 in luminosity (see paragraphs on In this paper, I’ll go through each “SN age” in ultra-faint and ultra-bright SNe) and complex some details. lightcurve morphology (e.g. Patat et al. 1994). The idea is that much of this variety in the luminosity at maximum and in the lightcurve 2. The heroic times morphologies is due to the mass of the H enve- The SN classification as proposed by lope of the progenitors at the time of the col- Minkowski (1942) in his seminal paper lapse of the core and the properties of the cir- was spectroscopically based and very simple. cumburst medium. Minkowski reported about “...two types of The first hint that the Minkowski’s classi- supernovae. Nine objects form an extremely fication was an over-simplified version of SN homogeneous group provisionally called taxonomy came from Bertola’s observations type I. The remaining ve objects are distinctly (1962) of SN 1961V. The lack of H in the spec- dierent; they are provisionally designed as type tra hinted for a type I SN, but the simultaneous II. The individual dierences in this group are absence of the absorption feature at 6150Å was large...” SNe of type I are defined by the lack clueing Bertola to conclude that “....supernova of hydrogen in the spectra. Nowadays we des- in NGC 1058...must be considered of a new ignated as type-Ia (SNe-Ia) those type-I SNe type...’.’ Today we know that these SNe belong that are characterized by a strong absorption to the SN-Ibc class, related with core-collapse observed at ∼ 6150Å (attributed to the P-Cyg events rather than exploding WDs. prole of Si II, λλ 6347, 6371) and lack of H. The absence of H, and the fact that these SNe 3. The golden age are discovered also in elliptical galaxies, hint that they may arise from the thermonuclear The criteria to classify the members of this sub- disruption of a white dwarf approaching the class of type-I SNe just as “peculiar” objects Chandrasekhar limit, after accreting material were adopted in the literature for the follow- from a binary companion or coalescing with it ing 20 years. Only in the mid-1980s (Panagia on time scales of 0.1-10 Gyrs (Mannucci et al. 1985; Elias et al. 1985; Uomoto & Kirshner 2006). Their spectroscopic (Filippenko 1987) 1985; Wheeler & Levreault 1985)) it was re- and photometric homogeneity (Barbon et al. alized that sufficient observational differences 1973) have justified “sic et simpliciter” for did exist to justify having two separate classes about three decades the use of these SNe as of objects. Type-Ib SNe are characterized by standard candles. Only in the early 90’s (e.g. spectra with no presence of H or very weak Della Valle & Panagia (1992), Phillips (1993), lines (Branch et al. 2002) and strong He I Hamuy et al. (1996)) was realized that the use lines at 4471, 5876, 6678 and 7065 Å. When of SN-Ia as cosmic yardsticks was much more even He lines are no prominent (if not to- complicated that previously thought. tally absent) a new class, Ic, has been advo- Type II SNe display a completely different cated (Wheeler & Harkness 1986). Spectra of behaviour: the spectra are definitely different Ic SNe show Ca II H & K, NIR Ca II triplet from each other and characterized by the pres- and O I lines with P-Cyg proles. Type-Ib/c Della Valle: Supernovae 369 SNe have been so far observed only in late (GRB) 980425, (Galama et al. 1998). GRB- type galaxies and their most outstanding spec- SNe are characterized by: i) lack of H and He troscopic feature is the lack of H in the spec- in the ejecta; ii) very broad features, which tra. Both facts suggest that their progenitors implies large expansion velocity of the or- are massive stars, possibly in binary systems der of 0:1c; iii) the non-relativistic ejecta (Maund et al. 2004) which undergo the col- are characterized by a very high kinetic en- lapse of their cores after they have lost the re- ergy content of ∼ 1052 erg, that is about 10 spective H or He envelopes, via strong stel- larger than observed in “standard” CC-SNe; lar wind or transfer to a binary companion iv) the explosions are strongly aspherical as via Roche overflow. This scenario is fully con- derived from profile of nebular lines O vs. sistent with observations at radio wavelengths Fe (Maeda et al. 2008) and from polarization that reveal the existence of a strong radio emis- measurements (Gorosabel et al. 2008); v) they sion due to the interaction of the ejecta with a are very luminous at maximum light, which 5÷6 1 56 dense pre-explosion stellar wind (10 M yr ) implies that a large amount of Ni mass (∼ /established circumstellar medium, produced 0:5M ) has been produced. GRB-SNe are very by the progenitor (Weiler et al. 2002). In the rare phenomena compared to SN explosions same years the discovery of SN 1987K showed without GRBs. Only << 1% of all CC-SNe that some SN could undergo a “trasgender” produce GRBs (Guetta & Della Valle 2007), behaviour. Initially classified as SN-II for the which implies that very special conditions are presence of H in its spectrum, SN 1987K requested to stars to become GRB progenitors: evolved into type Ib/c (lack of H) during the i) to be massive > 30 − 40M (Raskin et al. nebular stages. The neat interpretation of this 2008); ii) H envelopes to be (mostly) lost be- behaviour was that the massive progenitors still fore the collapse of the core; iii) low metal- retained a “thin” H envelope prior to explod- licity star forming environments seem also ing. The H layer was still detectable at early necessary (Fruchter et al. 2006; Modjaz et al. stages but it becomes optically thin at later 2008); iv) high rotation of progenitor stars stages as soon as the ejecta expanded.
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