The Supernova/Gamma-Ray Burst Connection. Jens Hjorth Dark Cosmology Centre Niels Bohr Institute University of Copenhagen

Transcription

1 The Supernova/Gamma-Ray Burst Connection Jens Hjorth Dark Cosmology Centre Niels Bohr Institute University of Copenhagen

2 Galama et al. 1998; Fynbo et al. 2000

3 SN 1998bw/GRB Galama et al. 1998

4 Collapsar model We predict that all GRBs produced by the MacFadyen & Woosley 1999 collapsar model will also make supernovae like SN 1998bw

5 GRB : light curve bump Castro-Tirado & Gorosabel 1999; Bloom et al. 1999

6 SN 2003dh/GRB GRB was an unusual GRB: Low luminosity and no afterglow Planned discovery: a SN in a high luminosity, higher redshift, afterglow dominated GRB? Spectral evolution from afterglow power law to broad-lined Ic supernova like SN 1998bw Hjorth et al. 2003; Stanek et al. 2003

7 Hjorth et al. 2003; Patat et al. 2001

8 VLT: a UV-VIS-NIR transient explorer

9 GRB A / SN 2012?? FeII* [OII] MnII FeII MnII FeII MnII MgII MgII MgI Normalised flux TiII CaII TiII CaII TiII [OII] [OII] [NeIII] CaII CaII [NeIII] H CaI H [OIII] Observed wavelength (Å)

10 Low-luminosity GRBs

11 Low-luminosity GRBs GRB D SN 1998bw 2003lw 2006aj 2010bh Redshift T 90 (s) E peak (kev) E γ,iso (erg) GRB /SN 1998bw prototype E γ,iso ~ erg Smooth high-energy lightcurves, sometimes long durations Low peak energy (often XRFs) Diverse SN lightcurves Bromberg et al. 2011

12 -18 GRB /SN 1998bw GRB /SN 2003lw GRB /SN 2006aj GRB D/SN 2010bh Absolute magnitude (mag) Time since GRB (days)

13 Low-luminosity GRBs ~100 times more common than long GRBs Rate similar to broad-lined Ic à No major beaming Pian et al. 2006; Soderberg et al. 2006; Bromberg et al. 2011

14 Jet-driven shock-breakout GRBs ~100 times more common than long GRBs Rate similar to broad-lined Ic à No major beaming Relativistic ejecta Interaction with circumburst stellar wind Thermal component SN 2006aj/GRB Colgate 1974; Kulkarni et al. 1998; Campana et al. 2006; Nakar & Sari 2012

15 Collapsar GRBs

16 M V (mag) Afterglow Supernova Host galaxy Time since explosion (days)

17 Total lighcurve Supernova Afterglow Host galaxy M V (mag) Time since explosion (days)

18 Total lighcurve Supernova Afterglow Host galaxy M V (mag) Time since explosion (days)

19 Total lighcurve Supernova Afterglow Host galaxy M V (mag) Time since explosion (days)

20 SN 2003dh/GRB Lipkin et al. 2004

21 Hjorth et al. 2003

22 -18 GRB /SN 2003dh GRB /SN 1998bw GRB /SN 2003lw GRB /SN 2006aj GRB D/SN 2010bh Absolute magnitude (mag) Time since GRB (days) Hjorth et al. 2003

23 Cano et al. 2011

24 Cano et al. 2011

25 SN 2010ma/GRB B Sparre et al. 2011

26

27 Quantifying the strength of evidence Grade A B C D E Description Strong spectroscopic evidence A clear light curve bump as well as some spectroscopic evidence A clear bump consistent with other GRB-SNe at the spectroscopic redshift of the GRB A bump, but the inferred SN properties are not fully consistent with other GRB-SNe or the bump was not well sampled or there is no spectroscopic redshift of the GRB A bump, either of low significance or inconsistent with other GRB-SNe Hjorth & Bloom 2012

28 SAX IPN HETE-II Integral Swift Hjorth & Bloom 2012

29 SNe from different classes of GRBs -20 Low-luminosity GRBs Collapsar GRBs -19 GRB GRB M V (mag) log E,iso (erg)

30 SN Ic brightness distributions 1.0 Fraction (> M V ) GRB SNe Ic-BL SNe Ic SNe M V (mag) Hjorth & Bloom 2012; Drout et al. 2011; various sources

31 Rates of cosmic explosions Type Rate Ibc supernovae ~10000 Gpc -1 yr -1 Broad-lined Ic supernovae ~500 Gpc -1 yr -1 Low-luminosity GRBs ~ Gpc -1 yr -1 Collapsar GRBs ~1 Gpc -1 yr -1 Podsiadlowski et al. 2004; Pian et al. 2006; Soderberg et al. 2006

32 Supernovae with no GRB

33 SN 2009bb: relativistic Ic-BL, no GRB Collapsar GRBs Low-luminosity GRBs Soderberg et al. 2010; Pignata et al. 2011

34 Lazzati et al. 2012

35 Lazzati et al. 2012; Bromberg et al. 2011

36 Jet-driven Type IIn SNe? 2010jp Prediction of collapsar model Jet/engine SN with massive H envelope will not lead to GRB Smith et al. 2012; Nomoto et al. 2003; Papish & Soker 2011; Chevalier 2012

37 GRBs with no supernove

38 Short GRBs BATSE: T 90 < 2 s Swift: T 90 < 0.7 s? Extended emission Redshift effect (1+z) Kouveliotou et al. 1993; Bromberg et al. 2011

39 -18 GRB /SN 2003dh GRB /SN 1998bw GRB /SN 2003lw GRB /SN 2006aj GRB D/SN 2010bh Absolute magnitude (mag) GRB B GRB Time since GRB (days) Hjorth et al. 2005a,b

40 Short GRBs No supernova detected Defining characteristic? Mergers of compact objects

41 -18 GRB /SN 2003dh GRB /SN 1998bw GRB /SN 2003lw GRB /SN 2006aj GRB D/SN 2010bh Absolute magnitude (mag) GRB GRB Time since GRB (days) Fynbo et al. 2006

42 Long GRBs with no (bright) SN Compact object merger progenitor with longer duration? 56 Ni fallback? Fynbo et al.; Della Valle; Gal-Yam et al.; Gehrels et al. 2006; Ofek et al. 2007

43 CC SNe SN-GRBs GRBs Relativistic Ic-BL (SN 2009bb) Low luminosity GRBs (SN 1998bw/GRB ) Fall-back SNe? (GRB ) Type IIn? (SN 2010jp) Collapsars (SN 2003dh/GRB ) Mergers (GRB B)