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Supernova and GRB observations

Jesper Sollerman DARK, NBI, Copenhagen Gamma-Ray Bursts; The first three hours Santorini August 30 2005. Supernova and GRB observations. A personal biased optical observational tutorial on SNe and GRBs. Supernova studies goes way back. SN 1054. Walter Baade (1893-1960).

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Supernova and GRB observations

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  1. Jesper Sollerman DARK, NBI, Copenhagen Gamma-Ray Bursts; The first three hours Santorini August 30 2005 Supernova and GRB observations A personal biased optical observational tutorial on SNe and GRBs..

  2. Supernova studies goes way back SN 1054

  3. Walter Baade (1893-1960) Fritz Zwicky (1898-1974) “With all reservation we advance the view that a supernova represents the transition of an ordinary star into a neutron star, consisting mainly of neutrons” (Baade & Zwicky 1934). Core-collapse SNe..

  4. Classification The Supernova zoo ...

  5. SupernovaSpectroscopy near maximum two weeks later Type Ia

  6. Supernova Spectroscopy Type II

  7. Supernova classification core collapse in massive stars SN II (H) SN Ib/c (no H/He) Hypernovae/GRBs SN Ia (no H) thermonuclear explosions Compare GRB Zoo? (GRB, XRF, XRGRB, short, long, dark, weak, hard, soft..) [obafgkm]

  8. Supernova types Thermonuclear SNe from low-mass stars (<8M) highly evolved stars (white dwarfs) explosive C and O burning binary systems required complete disruption Core-collapse SNe high mass stars (>8M) large envelopes burning due to compression single stars (binaries for SNe Ib/c) neutron star/(BH)

  9. Energy sources Gravity →Type II supernovae (and Ib/c) collapse of a solar mass or more to a neutron star release of 1053 erg mostly νe 1051 erg in kinetic energy (expansion of the ejecta) 1049 erg in radiation Nuclear (binding) energy → Type Ia • explosive C and O burning of about one solar mass • release of 1051 erg (again! most to kinetic energy)

  10. Type Ia SNe

  11.  ~ 0.13 mag SNe Ia Supernova Cosmology Project

  12. GRB cosmology Mörtsell & Sollerman 2005 Require z, tjet

  13. Classification For Ia = short GRB, see Dar & Rujula, Phys. Rep. 405, 203 (2004)

  14. SN 1987A

  15. SN 1987A Suntzeff (2003) Core-collapse supernovae < Days (linear scale)

  16. Core-Collapse Diversity Patat et al. 1996 – Type II SNe Richardsson et al. 2002 Type Ibc SNe

  17. Isotopes of Ni and other elements conversion of -rays and positrons into heat and optical photons Radioactivity Diehl and Timmes (1998) Lpeak ~ M(56Ni)

  18. Gamma-Ray Bursts Vela

  19. A Gamma-Ray Burst is a burst of gamma-rays... (J. Fynbo)

  20. Supernova- connection from the start

  21. Theories..... Nerimoff 1994

  22. Theories..... Nerimoff 1994 Several may be correct!

  23. Theories..... Nerimoff 1994 Most must be wrong!

  24. CGRO/BATSE 1991-2000 Cosmological? Beppo-Sax 1996-2002 Cosmological!

  25. The first hint .. GRB 980425 <--> SN 1998bw @ z=0.0085

  26. SN 1998bw Galama et al. 1998 3 1 1-3 2 Fynbo et al. 2000 Sollerman et al. 2002

  27. A peculiar supernova at the right place and time.. Unusally energetic! (The supernova!) Galama et al. 1998 Sollerman et al. 2000 Patat et al. 2001 Sollerman et al. 2002 Maximum Light Spectra But no afterglow.. Suggestive rather than conclusive.. Nando Patat - IAU Colloquium 192 – Supernovae(5 years of SN1998bw)

  28. GRB 980326 Red Bumps Castro-Tirado & Gorosabel 1999 Bloom et al. 1999

  29. GRB explosion sites. e.g., Bloom et al., Sokolov et al., Fruchter et al., and many others

  30. II Zw 40 GRB 990123, HST days 16, 59 och 380.

  31. GRB 011121: z = 0.36 Greiner et al. 2003 Garnavich et al. 2003

  32. GRB 030329 z=0.168526

  33. GRB 030329 optical afterglow Guziy et al. (200 ) Deng et al.

  34. SN 2003dh Stanek et al. 2003 (Matheson et al. )

  35. Hjorth, Sollerman, Moller, et al. 2003

  36. SN 2003dh Amazingly similar..

  37. SN 2003dh expansion velocity SN 1998bw @ 8 days Si II6355 SN 2003dh @ 10 days SN 1998bw @ 12 days v = 0.12c @ 10 days

  38. SN 2003dh lightcurve: faster rise & decay Larger expansion velocity than SN 1998bw (and any other SN) Indicates a short delay between SN and GRB (see recent Deng et al. 2005) SN 1998bw @ z = 0.1685 SN 1998bw – 7 days SN 1998bw stretched 0.7

  39. Santorini GRB summerschool – The first three hours.... Sokolov et al. 2003, Bull.Spec.Ast.Obs., 56, 5

  40. GRB 031203 = SN 2003lw Thomsen et al. 2004 (also Cobb et al, Gal-Yam et al.) Malesani et al. 2004 Another SN 1998bw look alike! And like GRB980425, also no afterglow..

  41. And now to something completely different? XRF 030723 Fynbo, Sollerman, Hjorth, et al. 2004

  42. July 26, FORS1, 3.8 hr, G300V 3800Å 8900Å

  43. 5300Å 8900Å Aug 7+8, FORS2, 3.8 hr, G600RI

  44. GRB021004, NOT, z=2.33 GRB000926, NOT, z=2.04 XRF030723, VLT

  45. Spectral Energy Distribution (SED)

  46. Interpretation: Supernova

  47. Supernova? • In qualitative agreement with the evidence (lightcurve + SED) • Peaks early and has a narrow peak • Incompatible with SN1998bw lightcurve at any redshift • Envelope-stripped progenitor, asymmetric explosion seen near a pole, high ionisation? • SN1994I at z=0.6 is the known SN that gives the best match • Abs. Mag: • z=0.4 => similar to SN1994I • z=1.0 => brighter than SN1998bw Tominaga et al. (2004).

  48. GRB 021211 Della Valle et al. 2003 XRF 020903 Soderberg et al. 2005 See also Zeh, Klose & Hartmann 2004

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