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The Supernova Rate with WFXT

The Supernova Rate with WFXT. M. Della Valle INAF -Napoli. SN 1994D. P. Rosati , M. Paolillo D. De Martino, S. Campana , L. Stella. +. Outline. SN classification X-ray from SNe Ejecta vs - CSM Interaction Shock Break-out/failed GRB GRBs

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The Supernova Rate with WFXT

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  1. The Supernova Rate with WFXT M. Della Valle INAF-Napoli SN 1994D P. Rosati, M. Paolillo D. De Martino, S. Campana, L. Stella +

  2. Outline • SN classification • X-ray from SNe • Ejectavs- CSM Interaction • Shock Break-out/failed GRB • GRBs • Exotics objects (Dark SNe, LBV-SNe, Monsters…. Ia?) • Conclusions Bologna, 2009

  3. Supernova Classification IIp (P-Cygni), IIb Core collapse of massive single stars II II l, IIn(Balmer emission) H Core collapse of massive stars (likely) in binary systems SNe Ic (weak He) Ib (strong He) No H Thermonuclear explosion of white dwarfs I Ia (strong Si) Bologna, 2009

  4. Supernova Classification IIp (P-Cygni), IIb Core collapse of massive single stars II II l, IIn(Balmer emission) H Core collapse of massive stars (likely) in binary systems SNe Ic (weak He) High KE=GRB-SNe Ib (strong He) No H Thermonuclear explosion of white dwarfs I Ia (strong Si) Bologna, 2009

  5. X-ray from SNe X-ray from interaction between SN ejecta and CSM X-ray from SN Shock Break-out (or failed GRB) X-ray from GRBs

  6. H II ISM CSM ~10 km/s RSG Reverse shock ~103 km/s; 107 K Forward shock ~ 104 km/s; 109 K

  7. Luminosity from Interaction: ejecta vs. CSM SN 1941C SN 1959D SN 1968D SN 1980K SN 1992ad SN 1993J SN 1994I SN 2004et SN 2006bp

  8. Distance Distribution

  9. D ~ 10 Mpc & L ~ 5x1038 erg/s; Δt ~ 107 s >> 4ks and 13ks and > 400 ks wide < 35 Mpc medium < 100 Mpc deep < 370 Mpc

  10. OUTPUT • Indirect measurements of the SN rate • The X-ray luminosity is a function of the density of the CSM and ejecta velocities  properties of the CSM (ρ, v)  mass loss of the progenitor stars of SNe (N.B. one of the most poorly constrained astrophysical quantity) Bologna, 2009

  11. In the Shock Break-out Arena The X-ray transient 080109/SN 2008D was serendipitously discovered by XRT (Berger & Soderberg 2008) while Swift was observing SN 2007uy

  12. Soderberg et al. 2008 Modjaz et al. 2008 Malesani et al. 2008 Chevalier & Fransson 2008 Xu et al. 2008 Li et al. 2008 Mazzali et al. 2008 Tanaka et al. 2008 Wang et al. 2008 Tanaka et al. 2009

  13. The associated X- flare is a softer and fainter version of a GRB

  14. SupernovaShock Break-out Soderberg et al. 2008 Wang et al. 2008 Modjaz et al. 2008 Chevalier & Fransson 2008

  15. Failed GRB SNe GRBs Mazzali et al. 2008; Tanaka et al. 2008, 2009 Li 2008; Xu et al. 2008

  16. + Shock break-out The presence of : • a dim peak in the optical lightcurve • the softness of the X-ray emission • the Energy budget ~ 1046 erg is close to the predicted shock breakout radiation energy of “standard” SNe-Ibc (Matzner and McKee 1999)

  17. + Failed GRB • SN 2008D is not a “standard” CC event (EK)

  18. The theoretical modelling of the lightcurve and spectra of SN 2008D (Tanaka et al. 2008) finds a progenitor mass on the main sequence of about 25 M and a kinetic energy of 6 x 1051 erg.  SN 2008D has a significantly higher energy than “standard” CC-SNe (~1051 erg) although less than GRB-HNe (~1052 erg)  it is unlikely that all CC-SNe can produce a X-ray flash like 080109

  19. + Failed GRB • SN 2008D is not a “standard” CC event (EK) • The similarities between 060218 and 080109 (lightcurves and both match the Amati relationship) suggest that this X-ray transient is a weaker version of a GRB event • the shock break-out theory predicts that the radiation spectrum is thermal-dominated. The observed one is a power-law (though see Wang et al. 2008 ) iv) Polarization

  20. X-Ray 080109 matches the Amati Relationship Bologna, 2009

  21. Lpeak~ 3 x 1043 erg/s i) Learly~3 x 1041 erg/s Δt ~ 103s ii) Llate~ 1040 erg/s, Δt ~ 104s D=31 Mpc fearly ~ 2.6 x 10-12 erg cm-2s-1 flate~ 8.6 x 10-14 erg cm-2s-1 treshearly ~ 10-13 erg cm-2s-1 treshlate ~ 8x10-15erg cm-2s-1 Dearly < 160 Mpcz < 0.04 Dlate < 102 Mpcz < 0.025 Bologna, 2009

  22. Shock Break-out detections Cappellaro et al. 1999; Mannucci et al. 2005, Guetta & DV 2007 early late II = 3.51 x 10-2 deg2 yr-1 8.78 x 10-3 deg-2 s-1 Ibc = 1.17 x 10-2 deg2 yr-1 2.93 x 10-3 deg-2 s-1 Ia = 1.40 x 10-2 deg2 yr-1 3.51 x 10-3 deg-2 s-1 HNe = 5.85 x 10-4 deg2 yr-1 1.47 x 10-4 deg-2 s-1

  23. OUTPUT • Clarify the conundrum Shock Break-out/Failed GRB  physics of the SN explosion + optical follow-up Bologna, 2009

  24. OUTPUT • Clarify the conundrum Shock Break-out/Failed GRB  physics of the SN explosion • Independent measurement of the CC-SN rate (alternative method to “boring” optical/NIR SN surveys) Bologna, 2009

  25. Direct detections GRBs Lpeak~ 5 x 1046 erg Llate~ 5 x1043 erg, Δt ~ 104s D=130 Mpc flate~ 5 x 10-11 erg cm-2s-1 treshlate ~ 10-14erg cm-2s-1 Dlate (L) < 104Mpcz < 1.4 Bologna, 2009

  26. How representative of GRB Pop is it ? courtesy of R. Margutti Bologna, 2009

  27. GRBs/SNe-I(b)c:0.4%-0.7% (Guetta & DV 2007,Soderberg et al. 2009) (<3 % and <4.5% at 99% c.l.) Bologna, 2009

  28. SN Time Machine N z

  29. 300 Ibc deg-2 yr-1 SNeIbc = 588 deg-2 yr-1

  30. GRB/SNe-I(b)c:0.4%-0.7% (Guetta & DV 2007,Soderberg et al. 2009) (<3 % and <4.5% at 99% c.l.) 300Ibc deg-2 yr-1 HL-GRBs LL-GRBs Bologna, 2009

  31. Peculiar Events (< 5% CC-SNe) Bologna, 2009

  32. Low redshift:z = 0.125 SN search? E vai……!!!! Gehrels et al. 2006 Mangano et al. 2007 Bologna, 2009 0s 50s100s

  33. Factor >100 Dark SNe? Late time: host galaxy contribution(no variation) Upper limit: MV > -13.5 (3) Bologna, 2009 Della Valle et al. 2006; Gal-Yamet al. 2006; Fynboet al. 2006

  34. LBV-SNe Pastorelloet al. 2006 SN 2006jc Dec 2001 Oct 2004 21 Sept 2006 29 Oct 2006 The pre-explosion transient appears similar to the giant outbursts of Luminous Blue Variables (LBV) of 60-100 M. The massive star has exploded “prematurely” during the LBV phase preventing the progenitor to explode as a W-R Bologna, 2009

  35. The progenitor of SN2006jc was hydrogen deficient. An LBV-like outburst of a Wolf- Rayet star could be invoked, but this would be the first observational evidence of such a phenomenon. Bologna, 2009

  36. The Monster SN 2006gy Bologna, 2009

  37. Type IIn AV ~ 1.8+0.4-0.3 mag Smith et al. 2008 Smith & McKray 2007 Ofek et al. 2007 Agnoletto et al. 2009 Kawabata et al. 2009 Woosley et al. 2007 Bologna, 2009

  38. SN 2006gy is H-rich Type IIn ! Bologna, 2009

  39. Pair-instability Supernova (Smith et al. 2008) • Collision between high velocity shells originated in • subsequent outbursts of a very massive star undergoing • structural instabilities caused by pair production • (pulsational pair-instability, Woosley et al. 2007). • Thermonuclear or massive star (Ofek et al. 2008) • Strong interaction of the SN ejecta with “very dense” and • “clumpy” LBV environment (~ 10M) + 3M of 56Ni • (Agnoletto et al. 2009; Kawabata et al. 2008) • Progenitor Mass  60-100 M. LBV progenitor? • Canonical stellar evolution “predicts” that the progenitors of CC-SNe should experience the collapse of the core (i.e. the SN explosion) during the red Supergiant or W-R phases Bologna, 2009

  40. Bologna, 2009

  41. X-ray from SNe-Ia • Double degenarate: where two C-O WDs in a binary systems make coalescence as result of the lost of orbital energy for GWs (Webbink 1984; Iben & Tutukov 1984) • Single Degenerate: Cataclysmic-like systems: RNe(WD+giant, WD+He) Symbiotic systems(WD+Mira or red giant) Supersoft X-ray Sources(WD+MS star) Bologna, Nov, 2009

  42. X-ray from Ia ? Immler et al. 2006 v Bologna, 2009

  43. Conclusions • X-ray from Ejecta – CSM Interaction: ~ 100 detections (II+Ibc) • Ia detections ? If 2005ke is representative of Ia population, yes • Shock break-out: ~ 2500 Ibcdetections (w+m+d) and ~ 120well observed events. Possibility to resolve the break-out/failed GRB ambiguity. • ~ 8000 (350) detections if also type II display such a behaviour • GRBs: ~ 25-250 HL-events (m+ d), < 600 LL-GRBs • Output:Independent measurements of SN rates. GRB beaming factors • Chances to enter into unknown “territories” (Dark SNe, LBV-SNe, Super-Bright SNe (pair instability?), unusual transients) < 100 events. • Need for Optical/NIR Follow-up Bologna, 2009

  44. To Do List • SN Thresholds • SFR • correction for absorption Bologna, 2009

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