1. Observed properties of SN From Woosley Lecture 16 See also Filippenko (1997; ARAA 35, 309) See also http://rsd-www.nrl.navy.mil/7212/montes/sne.html http://www.supernovae.net/snimages/ http://www.supernovae.net/snimages/snlinks.html#Catalogs

2. SN 1994D

3. SN 1987A in the LMC

4. SN2007gr, observed by students at NOT Magnitude ~ 13.5

5. SN2007gr, observed by students at NOT

6. Supernovae - Observed Characteristics See also http://rsd-www.nrl.navy.mil/7212/montes/sne.html http://www.supernovae.net/snimages/ http://www.supernovae.net/snimages/snlinks.html#Catalogs

7. Summary

8. Filippenko (1997; ARAA 35, 309)

9. Ia II Ic Ib Filippenko (1997; ARAA 35, 309) Ia II Ic Ib

10. Properties: Type Ia supernovae Classical SN Ia; no hydrogen; strong Si II ll 6347, 6371 line Maximum light spectrum dominated by P-Cygni features of Si II, S II, Ca II, O I, Fe II and Fe III Nebular spectrum at late times dominated by Fe II, III, Co II, III Found in all kinds of galaxies, elliptical to spiral, some (controversial) evidence for a mild association with spiral arms Prototypes 1972E (Kirshner and Kwan 1974) and SN 1981B (Branch et al 1981) Brighest kind of supernova, though briefer. Higher average velocities. M bol ~ -19.3 Assumed due to an old stellar population. Favored theoretical model is an accreting CO white dwarf that ignites at the Chandrasekhar mass.

11. Spectra of three Type Ia supernovae near peak light Filippenko (1997; ARAA 35, 309) Spectra are very similar from event to event

12. Type Ia Filippenko (1997; ARAA 35, 309 )

14. The B-band (blue) light curves of 22 Type Ia supernovae (Cadonau 1987). Roughly speaking they are quite similar.

15. Suntzeff (1996; in McCray & Wang, eds: Supernovae and supernova remnants, CUP, p. 41)

16. Goldhaber et al. (2001; ApJ 558, 359) (b) etc: 1-day averages (c – d): 1 + z correction (e – f): additional stretch factor z = 0.5 – 1 z = 0.03 – 0.1

17. Phillips (1993; ApJ 413, L105)

18. The Phillips Relation (post 1993) Broader = Brighter Can be used to compensate for the variation in observed SN Ia light curves to give a “calibrated standard candle”. Note that this makes the supernova luminosity at peak a function of a single parameter – e.g., the width.

19. Possible Type Ia Supernovae in Our Galaxy SN D(kpc) m V 185 1.2+-0.2 -8+-2 1006 1.4+-0.3 -9+-1 1572 2.5+-0.5 -4.0+-0.3 1604 4.2+-0.8 -4.3+-0.3 Expected rate in the Milky Way Galaxy about 1 every 200 years, but dozens are found in other galaxies every year. About one SN Ia occurs per decade closer than 5 Mpc. Tycho’s SN

20. Properties: Type Ib/c supernovae Lack hydrogen, but also lack the Si II ll 6355 feature that typifies SN Ia. SN Ib have strong features due to He I at 5876, 6678, 7065 and 10830 A. SN Ic lack these helium features, at least the 5876 A line. Some people think there is a continuum of properties between SN Ib and Sn Ic Found in spiral and irregular galaxies. Found in spiral arms and star forming regions. Not found in ellipticals. Often strong radio sources Fainter at peak than SN Ia by about 1.5 magnitudes. Otherwise similar light curve. Only supernovae definitely associated with gamma-ray bursts so far are Type Ic

21. Properties: Type II supernovae Have strong Balmer lines – H a, H b, H g - in peak light and late time spectra. Also show lines of Fe II, Na I, Ca II, and, if the supernova is discovered early enough, He I. Clearly come from massive stars. Found in star forming regions of spiral and irregular galaxies. Not found in ellipticals. Two presupernova stars identified: SN 1987A = B3 supergiant; SN 1993J = G8 supergiant (Aldering et al 1994) Fainter than Type I and highly variable in brightness (presumably depending on hydrogen envelope mass and radius and the explosion energy). Typically lower speed than Type Ia. Last longer. Come in at least two varieties (in addition to 87A) – Type II-p or “plateau” and Type II-L or “linear”. There may also be Type II-b supernovae which have only a trace amount of hydrogen left on what would otherwise have been a Type Ib/c (e.g., SN 1993J) Strong radio sources and at least occasionally emit neutrino bursts

22. Type II-p

23. SN 1988A (Type II-p) Ruiz-Lapuente et al. (1990; AJ 100, 782)

24. Filippenko (1990) Typical Type II-p on the Plateau

25. SN 1987A Philipps (1987) CTIO 2 days after SN)

26. Neutrinos from SN 1987A Hirata et al. (1987; PRL 58, 1490)

27. Summary

28. Ia II Ic Ib Filippenko (1997; ARAA 35, 309) Ia II Ic Ib

30. Supernovae remnants

31. Crab Nebula, X rays and optical

32. Centre of Crab Nebula in X rays (Chandra)

34. SN 1006 in X rays (Chandra)

35. Supernova Frequencies Van den Bergh and Tammann, ARAA, 29, 363 (1991) Based upon 75 supernovae. 1 SNu == one supernova per century per 10 10 solar luminosities for the host galaxy in the blue band. h ~ 0.7. The Milky Way is an Sb or Sbc galaxy.

36. Lupus 1006 Crab 1054 3C 58 1151? Kepler 1604 Tycho 1572 Cas A 1658?