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The Supernova Rate with WFXT
M. Della Valle INAF-Napoli
SN 1994D
P. Rosati, M. Paolillo D. De Martino, S. Campana, L. Stella
+
Bologna, 2009 2
Outline
• SN classification• X-ray from SNe
Ejecta vs- CSM InteractionShock Break-out/failed GRBGRBs
• Exotics objects (Dark SNe, LBV-SNe, Monsters…. Ia?)
• Conclusions
Bologna, 2009 3
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
Bologna, 2009 4
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 RSG
ISMH 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)
Bologna, 2009 13
14
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
15
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
16
17
The associated X- flare is a softer and fainter version of
a GRB
18
19
Supernova Shock Break-out
Soderberg et al. 2008
Wang et al. 2008
Modjaz et al. 2008
Chevalier & Fransson 2008
20
Failed GRB
Mazzali et al. 2008;
Tanaka et al. 2008, 2009
Li 2008;
Xu et al. 2008
SNe GRBs
21
+ 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)
22
+ Failed GRB
i) SN 2008D is not a “standard” CC event (EK)
23
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
24
+ Failed GRB
i) 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
25
X-Ray 080109 matches the Amati Relationship
Bologna, 2009
Bologna, 2009 26
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 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
II ? Ibc HNe
wide 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
Bologna, 2009 28
II ? Ibc HNe
wide 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)
Bologna, 2009 29
Bologna, 2009 30
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 ?
Bologna, 2009 31
courtesy of R. Margutti
Bologna, 2009 32
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
Bologna, 2009 35
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)
Bologna, 2009 36
Bologna, 2009
Gehrels et al. 2006
Mangano et al. 2007
Low redshift:z = 0.125
SN search?
E vai……!!!!
0s 50s 100s
37
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
>1
00
Bologna, 2009 38
Bologna, 2009
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
Bologna, 2009
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.
40
Bologna, 2009
The Monster
41
SN 2006gy
Bologna, 2009
Type IIn AV ~ 1.8+0.4
-0.3 mag
Smith et al. 2008Smith & McKray 2007
Ofek et al. 2007Agnoletto et al. 2009Kawabata et al. 2009
Woosley et al. 2007
42
Bologna, 2009
SN 2006gy is H-rich Type IIn !
43
• 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
Bologna, 2009 45
Bologna, Nov, 2009 46
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 ?
Bologna, 2009 47
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
Bologna, 2009 48
To Do List
• SN Thresholds• SFR• correction for absorption
Bologna, 2009 49