New Paths toward the Supernova Rate Measurements M. Della Valle + - - PowerPoint PPT Presentation

New Paths toward the Supernova Rate Measurements

• M. Della Valle

INAF-Napoli ICRANet-Pescara

+

• P. Rosati, M. Paolillo,
• D. De Martino

Wide-Field X-ray Telescope

(Murray et al. 2010)

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Why SN rates ?

• Explosive Death of Stars
• Metal Enrichment
• Energy Injection
• Distance Indicators
• Tracers of high-z Stellar Populations
• Bright Background Sources

ISM-IGM Studies

• Bright Echoes

3-D Structure of CSM

• Cosmic Rays
• NS & BHs
• Neutrinos
• GWs

Evolution of stellar population and galaxies; GRBs Cosmology GRBs Core-Collapse SNe

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Outline

• Classical SN searches
• X-ray from CC-SNe

Ejecta vs- CSM Interaction Shock Break-out/failed GRB GRB-SNe

• X-ray and SNe-Ia
• Exotics objects (Dark SNe, LBV-SNe, Monsters….)
• Conclusions

SN 1998dh

How to search

Compare images taken at different epochs

• few days < time interval < 1-2 month
• 14 < limiting magnitude < 24
• 0.01 < target redshift < 1
• 5 arcmin < field of view < 1 deg
• B-V < band < R-I

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JAN FEB MARAPR MAYJUN JUL AGO SEP DEC NOV

• bserving

log

1. The observing log: epoch, limiting magnitude 2. Target apparent light curve: SN type, target distance 3. Galaxy sample: distance, type, inclination …….

How to compute rates

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Compute SN rate

) ( ) ( ) ( ) (

, G V SN BV i SN B SN V i

A t K z t M t m + + + = µ

) 1 (

• +

=

N i SN i SN i SN

CT N z r

SN light curve in B absolute magnitude galaxy distance modulus B to V K-correction galactic extinction

t0 = t /(1+z)

d ) ( ) ( m m m L CT

SN i i i

• =

detection efficiency

galaxy luminosity time SN stays at m-m+dm

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5 5 historical historical SN searches SN searches

Asiago (Italy) Photographic Cappellaro et al. 1993 A&A 268, 472 Crimea (Russia) Photographic Tsvetkov 1983 SA 27, 22 O.C.A. (France) Photographic Pollas 1994 Calan/Tololo (Chile) Photographic Hamuy et al. 1993 AJ 106, 2392 Evans (Australia) Visual Evans 1997 PASA 14, 204

RC3 galaxies surveyed 9346 SNe discovered 137 Total control time ~ 25000 yr

Local SN Rate

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Local Supernova Rates

Mannucci et al. 2005

SNe per century per 1010 M SNe per century per 1010 K-band L

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Cappellaro et al. 1999

The robotic Lick Observatory Supernova Search (LOSS), conducted with the the 0.76-m Katzman Automatic Imaging Telescope (KAIT) equipped with a CCD imaging camera, has discovered over 400 supernovae in the past 7 years. This makes KAIT the world's most successful search engine for nearby supernovae. The LOSS sample has about 14,000 galaxies, roughly half of which are available at any given season, and these are imaged with temporal frequencies that typically range from 2 to 10 days.

The Lick Observatory Supernova Search

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CCD (local) SN Rates are similar to photographic (local) SN rates

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Surveys for Transients

• PANSTARRS
• The SDSS Supernova Survey
• The ESSENCE Supernova Survey
• SNLS SuperNova Legacy Survey
• GOODS/HST TRANSIENT SEARCH (2004)

SN search

target reference

• SN 2000fc

type Ia z = 0.42 V=22.4 IAUC7537

difference

=

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Panoramic Survey Telescope and Rapid Response System 1

• 1.8m telescope on Haleakala (Maui)
• 1.4 gigapixel camera (GPC1)
• 40x40 cm focal plane
• 7 sq. deg. FOV, 0”.26 pixels
• 8x8 chips, 8x8 cells per chip, 584x591 pixels

I.e., an “array of arrays”

SN Surveys

• PANSTARRS
• The SDSS Supernova Survey
• The ESSENCE Supernova Survey
• SNLS SuperNova Legacy Survey
• GOODS/HST TRANSIENT SEARCH (2004)

Della Valle et al. 2005

Extreme Large Telescope (160 nights) SNe (ground/HST) SNe Ia SNe II SNe Pop III

X-ray from SNe

X-ray from interaction between SN ejecta and CSM (Soderberg et al. 2010)

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X-ray from SN Shock Break-out (and/or failed GRB) (Rabinak & Waxman 2010) X-ray from GRB-SNe (Bufano et al. 2010)

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X-ray from accretion on massive WDs

(progenitors of SNe-Ia) (Gilfanov & Bogdan 2010)

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

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Luminosity from Interaction: ejecta vs. CSM

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SN 1941C SN 1959D SN 1968D SN 1980K SN 1992ad SN 1993J SN 1994I SN 2004et SN 2006bp

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Distance Distribution

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

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SN Time Machine

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z N

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300 Ibc deg-2 yr-1

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SNeIbc = 588 deg-2 yr-1

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SN rates from Cappellaro 1999 Correction for dust MDVP 2008

Cosmic SFR Hopkins & Beacom 2006

Ingredients

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¯ ¯

to check what we are doing……

Woosley & Bloom 2006

7.1 SNe per sec 3.3 SNe per sec

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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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X-ray from SNe

X-ray from interaction between SN ejecta and CSM (Soderberg et al. 2010)

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X-ray from SN Shock Break-out (and/or failed GRB) (Rabinak & Waxman 2010) X-ray from GRB-SNe (Bufano et al. 2010)

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X-ray from accretion on massive WDs

(progenitors of SNe-Ia) (Gilfanov & Bogdan 2010)

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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

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SNe GRBs

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+ Shock break-out

The presence of : i) a dim peak in the optical lightcurve ii) 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 GRB

i) SN 2008D is not a “standard” CC event (EK)

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The theoretical modelling of the lightcurve and spectra

• f 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 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

• bserved 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 < 0.04 Dlate < 102 Mpc  z < 0.025

Shock Break-out detections

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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)

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OUTPUT

• Clarify the conundrum Shock Break-
• ut/Failed GRB  physics of the SN

explosion

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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-
• ut/Failed GRB  physics of the SN

explosion

• Independent measurement of the CC-SN or

HN rates (alternative method to “boring”

• ptical/NIR SN surveys)

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X-ray from SNe

X-ray from interaction between SN ejecta and CSM (Soderberg et al. 2010)

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X-ray from SN Shock Break-out (and/or failed GRB) (Rabinak & Waxman 2010) X-ray from GRB-SNe (Bufano et al. 2010)

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X-ray from accretion on massive WDs

(progenitors of SNe-Ia) (Gilfanov & Bogdan 2010)

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Direct Detections of GRBs: 060218/SN 2006aj

(Campana et al. 2006)

z = 0.033 faint: Eγ ∼ 1049 erg MV (host) = -16 Host has brightness Similar to SMC

Z/Z ~ 0.3 2006aj = SN-Ic

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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 of LL-GRBs

How representative of GRB Pop is it ?

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courtesy of R. Margutti

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

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

OUTPUT

Conclusions

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A wide field X-ray telescope can offer an independent measurement of the local SN rate which is particular relevant for different areas of modern astrophysics (Neutrinos, GWs) May help to discriminate among genuine SN shock break-out event and different phenomena connected with the BH formation and GRB engine Open new windows of opportunity for observations of new kind

• f stellar explosions

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Peculiar Events (< 5% CC-SNe)

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X-ray from SNe-Ia (progenitors)

• Double degenerate: two C-O WDs in a

binary systems make coalescence as result

• f the lost of orbital energy for GWs
• Single Degenerate: Cataclysmic-like

systems (WD accreting from MS star)

RNe (WD+giant)

Symbiotic systems (WD+Mira or red giant) Supersoft X-ray Sources (WD+MS star)

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The X-ray Signatures of these two paths are significantly different

No strong X-ray emission is expected in the merger scenario until shortly before the SN explosion, whereas in the SD scenario the WD accreting material from the non-degenerate companion becomes a source of copious X-rays for ~ 107 yr before the explosion

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The X-ray Signatures of these two paths are significantly different

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The Monster

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SN 2006gy

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Gehrels et al. 2006 Mangano et al. 2007

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

0s 50s 100s

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

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

Dark SNe?

Factor >100

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LBV-SNe

Pastorello et 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

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The progenitor of SN2006jc was hydrogen deficient. An LBV-like

• utburst of a Wolf- Rayet star could be invoked, but this would be the

first observational evidence of such a phenomenon.

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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

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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

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X-ray from Ia ?

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v

Immler et al. 2006

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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Rate: ~ 1 GRB Gpc-3yr-1 (Schmidt 2001, Guetta et al. 2004) volz=1.4 = 312 Gpc3  312 GRBs Medium = 312 x 0.073 x 2 x 0.9 ~ 41 Deep = 312 x 0.0024 x 1 x 0.9 x 40 ~ 27

<fb-1> ~500 (Frail et al. 2001) (~ 4°) <fb-1> ~75 (Guetta, Piran & Waxman 2004) (~ 10°)

HL- GRBs

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Rate: ~ 10 HL-GRB (Guetta & DV 2007) <fb-1> < 10 (Guetta & DV 2007 for low lum GRBs) (> 25°) Medium = 312 x 0.073 x 2 x 0.9 ~ 120-410 Deep = 312 x 0.0024 x 1 x 0.9 x 40 ~ 60-270

<fb-1> ~500 (Frail et al. 2001) (~ 4°) <fb-1> ~75 (Guetta, Piran & Waxman 2004) (~ 10°)

LL- GRBs

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Rate: 0.5-1 GRB Gpc-3yr-1 (Schmidt 2001, Guetta et al. 2004) volz=1.4 = 312 Gpc3  150 ÷ 300 GRBs

<fb-1> ~500 (Frail et al. 2001) (~ 4°) <fb-1> ~75 (Guetta, Piran & Waxman 2004) (~ 10°)

<fb-1> < 10 (Guetta & DV 2007 for low lum GRBs) (> 25°)

<fb-1> ~ 1 (Ruffini et al. 2006, GRB 050315)

2x104 SNe-I(b)c Gpc-3 yr-1 (Guetta & DV 2007)

GRB/SNe-I(b)c: 2.5%-0.4%-0.05%-0.005%

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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

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SNe GRBs

Cappellaro, Evans, Turatto 1999 A&A 351, 459

Local SN Rate

• Ia rate (per unit LB) constant through galaxy type
• Core-Collapse rate peaks in late spirals
• Ib/c are 15% of core collapses
• SN rate in the Galaxy are 2.2 ±1.2 per century,

4/5 core-collapse

Pulsar birthrate from Parkes Multi-beam survey  4.50 ±1.16 (Vranasevic et al. 2003 astro-ph/0310201)

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The Pan-STARRS project

Panoramic Survey Telescope and Rapid Response System

PS1: 1x1.8m telescope on Haleakala PS1 surveys started May 2009 PS4: 4 x1.8m telescope on Mauna-Kea Final goal of project

Pan-STARRS is run by the University of Hawaii partially funded by the US Air Force

SDSS vs PS1

SDSS = Sloan Digital Sky Survey (~800 refereed papers so far, 2002+)

Param SDSS PS1 Telescope 2.5m 1.8m Camera 120 Mpix 1.4 Gpix Sky coverage 8,000 sq deg 30,000 sq deg (0.75 entire sky) Limiting mag (r’) ~22 ~24 Spatial resolution 0.4’’ 0.24’’

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Campana et al. 2006

GRB 060218

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… a shock is generated which propagates through the progenitor star and ejects the envelope. Accompanying the emergence of the shock wave through the surface of the star is a very bright UV/X burst of radiation…

Merate, Nov 2006

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56 Ni

Shock Break-out

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Campana et al. 2006

3 x104 km/s s

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Red Supergiant R~4x1013 cm Blue Supergiant R~4x1012 cm R~4x1011 cm



SNe-CC size progenitors

The radius of the progenitor  W-R Star

The near simultaneity of non thermal (GRB) and thermal (SN) X-ray emissions indicates that the SN and GRB are coeval events within ~ a few x 102s

GRB SN +Δt(d)

• Δt(d)

Ref.

980425 1998bw 0.7 2

Iwamoto et al.

000911 Bump 1.5 7

Lazzati et al.

021211 2002lt 1.5 3

Della Valle et al.

030329 2003dh 2 8 2

Kawabata et al Matheson et al

031203 2003lw 2

Malesani et al.

041006 Bump 2

Stanek et al.

050525A 2005nc 2

Della Valle et al.

060218 2006aj ~0.004

• Campana et al.

z v b i SN Ia SN II

Color Selection: An example

b v i z

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Supernova Classification

Thermonuclear explosion of white 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 N

• H

Ic (weak He)

Core collapse of massive stars (likely) in binary systems

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Supernova Classification

Thermonuclear explosion of white 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 N

• H

Ic (weak He)

Core collapse of massive stars (likely) in binary systems

High KE=GRB-SNe