The Supernova Rate with WFXT

M. Della Valle INAF-Napoli

SN 1994D

P. Rosati, M. Paolillo D. De Martino, S. Campana, L. Stella

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Outline

• SN classification• X-ray from SNe

Ejecta vs- CSM InteractionShock Break-out/failed GRBGRBs

• Exotics objects (Dark SNe, LBV-SNe, Monsters…. Ia?)

• Conclusions

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Supernova Classification

Thermonuclearexplosion ofwhite dwarfs

SNe

Core collapse of massive single stars

II

Ib (strong He)I

II l, IIn (Balmer emission)

IIp (P-Cygni), IIb

Ia (strong Si)

H

No H

Ic (weak He)

Core collapse of massive stars (likely) in binary systems

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Supernova Classification

Thermonuclearexplosion ofwhite dwarfs

SNe

Core collapse of massive single stars

II

Ib (strong He)I

II l, IIn (Balmer emission)

IIp (P-Cygni), IIb

Ia (strong Si)

H

No H

Ic (weak He)

Core collapse of massive stars (likely) in binary systems High KE=GRB-SNe

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

CSM ~10 km/s RSGISM

H II

Forward shock ~ 104 km/s; 109 K

Reverse shock ~103 km/s; 107 K

Luminosity from Interaction: ejecta vs. CSM

SN 1941CSN 1959DSN 1968DSN 1980KSN 1992ad SN 1993J SN 1994I SN 2004et SN 2006bp

Distance Distribution

D ~ 10 Mpc & L ~ 5x1038 erg/s; Δt ~ 107 s >> 4ks and 13ks and >

400 ks

wide < 35 Mpcmedium < 100 Mpcdeep < 370 Mpc

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)

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The X-ray transient 080109/SN 2008D was serendipitously discovered by XRT (Berger & Soderberg 2008) while Swift was observing SN 2007uy

In the Shock Break-out Arena

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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

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

a GRB

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Supernova Shock Break-out

Soderberg et al. 2008

Wang et al. 2008

Modjaz et al. 2008

Chevalier & Fransson 2008

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Failed GRB

Mazzali et al. 2008;

Tanaka et al. 2008, 2009

Li 2008;

Xu et al. 2008

SNe GRBs

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+ Shock break-out

The presence of :

i) a dim peak in the optical lightcurve

ii) the softness of the X-ray emission

iii) the Energy budget ~ 1046 erg is close to the predicted shock breakout radiation energy of “standard” SNe-Ibc (Matzner and McKee 1999)

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+ Failed GRBi) SN 2008D is not a “standard” CC event (EK)

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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

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+ Failed GRBi) SN 2008D is not a “standard” CC event (EK)ii) 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

iii) 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

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X-Ray 080109 matches the Amati Relationship

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Lpeak ~ 3 x 1043 erg/s

i) Learly ~3 x 1041 erg/s Δt ~ 103 s

ii) Llate ~ 1040 erg/s, Δt ~ 104 s

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 ~ 8x10-15 erg cm-2s-1

Dearly < 160 Mpc z < 0.04Dlate < 102 Mpc z < 0.025

Shock Break-out detections

Cappellaro et al. 1999; Mannucci et al. 2005, Guetta & DV 2007 early lateII = 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

II ? Ibc HNewide 4268 (267) 1422 (90) 71 (5)

medium 2464 (47) 821 (16) 41 (1)

deep 1263 (32) 421 (11) 21 (0.5)

OUTPUT

• Clarify the conundrum Shock Break-out/Failed GRB physics of the SN explosion

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II ? Ibc HNewide 4268 (267) 1422 (90) 71 (5)

medium 2464 (47) 821 (16) 41 (1)

deep 1263 (32) 421 (11) 21 (0.5)

+ optical follow-up

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)

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Lpeak ~ 5 x 1046 erg

Llate ~ 5 x1043 erg, Δt ~ 104 s

D=130 Mpc

flate ~ 5 x 10-11 erg cm-2s-1

treshlate ~ 10-14 erg cm-2s-1

Dlate (L) < 104 Mpc z < 1.4

Direct detections GRBs

How representative of GRB Pop is it ?

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courtesy of R. Margutti

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GRBs/SNe-I(b)c: 0.4%-0.7% (Guetta & DV 2007, Soderberg et al.

2009)

(<3 % and <4.5% at 99% c.l.)

SN Time Machine

z

N

300 Ibc deg-2 yr-1

SNeIbc = 588 deg-2 yr-1

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GRB/SNe-I(b)c: 0.4%-0.7% (Guetta & DV 2007, Soderberg et al. 2009)

(<3 % and <4.5% at 99% c.l.)

300 Ibc deg-2 yr-1

GRBs θ=4° (500) θ=10°(75) θ=25° (10)Frail et al.2001 Guetta et al. 2004 Guetta & DV 2007

medium 6.1-11.0x103 12-22 80-145 < 600

deep 4.3-7.4x103 9-15 55-100 < 425

HL-GRBs LL-GRBs

Peculiar Events (< 5% CC-SNe)

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Gehrels et al. 2006Mangano et al. 2007

Low redshift:z = 0.125SN search?E vai……!!!!

0s 50s 100s

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Late time:host galaxy contribution(no variation)Upper limit:MV > -13.5 (3)

Della Valle et al. 2006; Gal-Yam et al. 2006; Fynbo et al. 2006

Dark SNe?

Fact

or

>100

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LBV-SNe

Pastorello et al. 2006SN 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 39

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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.

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The Monster

41SN 2006gy

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Type IIn AV ~ 1.8+0.4

-0.3 mag

Smith et al. 2008Smith & McKray 2007Ofek et al. 2007Agnoletto et al. 2009Kawabata et al. 2009Woosley et al. 2007

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SN 2006gy is H-rich Type IIn !

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• 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 44Bologna, 2009

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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)

X-ray from Ia ?

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v

Immler et al. 2006

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 Ibc detections (w+m+d) and ~ 120

well 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

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To Do List • SN Thresholds• SFR• correction for absorption

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