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The progenitor stars of core-collapse supernovae

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Stephen J. SmarttAstrophysics Research CentreQueen’s University Belfast

Queen’s SNe & Massive star group: J. Eldridge, S. Mattila, A. Pastorello, M. Crockett, D. Young, M. Hendry, P. Dufton, C. Trundle, I. Hunter

Others: J. Maund (Texas), J. Danziger (Trieste), P. Meikle (Imperial),

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Overview

Core-collapse SNe drive the chemical evolution of galaxies, and formation through feedback

Test stellar evolution theory and NS/BH formation scenarios

Linked to the formation of long duration GRBs

Are the ideas of SNe progenitor stars correct ? Are SNe explosion and lightcurve models

consistent ?

3Credit: LOSS and T. Debosz

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Summary of SNe types

Supernovae are classified by their optical spectra

No hydrogen

Type I

Si He He or Si Ia Ib Ic

———

Hydrogen lines

Type II

Photometry/spectra properties II-P, II-L, IIn, IIb, II-p

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Example: HST Key project – H0 with

Cepheids Blue supergiants at 2-7Mpc from

8m telescopes - Bresolin et al. (2001)

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M101

NGC3621

NGC3949

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M81 zoom in

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First red supergiant progenitor

SN2003gd discovered 2003 June 12

Normal type II-P M74 - distance 9.3 1.8

Mpc 3100s WFPC2 pre-

explosion image F606W Gemini gri (480-960s),

0.56” images

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Detection of progenitor

HST ACS - ToO (Cycles 10-15) Smartt et al. (2003), Van Dyk et al. (2003): possible progenitors

from ground based astrometry calibration Star A: Differential astrometry: r = 13 ± 33 mas

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Magnitudes and colours of progenitor

V=25.8 ± 0.15 V–I=2.5 ± 0.2

d=9.1 ± 1.9 kpc ; E(B–V)=0.14 ± 0.13

K5-M3Ib supergiant (Elias et al. 1985)

STARS stellar evolutionary tracks:M = 8 -2 M

+4 Smartt et al. 2004, Science

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SN2005cs in M51

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• SN2005cs – discovered 20050628

• Hubble Heritage Team - deep mosaic BVI+H with ACS (Jan. 2005)

• F814W/F555W 1360s•WFPC2 U+R band (Jul.

1999)

Also deep NIR images:NICMOS (F110W+F160W; see Li et al. 2006) Gemini NIRI (JHK) 500-600s deep UBVRIJHK images

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Detection of progenitor

HST ToO : ACS post-explosion (F555W) Star detected in I-band only (J. Maund PhD thesis) I=23.3±0.05, and limiting V-band mag is V5 > 25 Not detected in any of the NIR bands; K>20.7

Maund et al. (2005), Li et al. (2006)

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Other examples: no detection

SN1999gi in NGC3184, HST U+V pre-explosion D=11Mpc (Leonard et al. 2002) M 12 M

SN2001du in NGC1365 HST UVI pre-explosion D=17Mpc (Cepheid Key P.) M 15 M

Smartt et al. 2001

Smartt et al. 2002

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Summary of II-P progenitors

SN Type Mass Z Ref2006bc II-P <15 ~Z

2005cs II-P 9 +3/-2 ~Z

2004et II-P 15 2 ~1-0.5Z Li et al. 2005

2004dj II-P 15 5 ~ZMaiz-Apellaniz et al. 2004, Wang et al. 2005,2006

2004am II-P 8-10 ~Z

2004dg II-P <12 ~Z

2004A II-P 10 2 ~0.5Z

2003gd II-P 8 +4/-2 ~Z

2002hh II-P <15 ~Z

2001du II-P <15 ~Z

1999ev II-P 16 2 1-2 Z

1999em II-P <15 1-2 Z

1999gi II-P <12 1-2 Z

1999br II-P <12 ~Z

1999an II-P <20 ~2 Z

Rest from Crockett et al. 2006, Maund & Smartt 2005, Maund et al. 2005, Hendry et al. 2006, Smartt et al. 2004, 2003, 2002, 2001

14Heger et al. (2000) - now can place observational constraints

Observed II-P

93J

87A80K

Observed Ib/c

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STARS stellar evolutionary tracks (Eldridge & Tout 2004) Eldridge, Smartt (in prep) - probability without mass cut ~5%

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Late time tail powered by radioactive 56Ni

56Ni explosively created from Si burning after core-collapse

Direct probe of the explosion

How Is it related to progenitor mass ?

UVOIR Light Curves and 56Ni Mass

56Ni→ 56Co+ e+ +νe +γ(τ1/2 =6y)56Co→ 56Fe + e+ +νe +γ(τ1/2 =77.1y)

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Black-hole forming SNe ?

Zampieri et al., Nomoto et al - low luminosity SNe form black-holesNo evidence so far of the branching at high luminosityDetailed comparison with models now possible

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Constraints on a Type Ic

SN2004gt - type Ic Gamma-ray bursts

coincident with Ic supernovae

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Restricted region in the HRD

We would have detected massive evolved stars

Either a star of 120-150M or

More likely a lower mass object in a binary

Maund, Smartt, Schwiezer (2005)Gal-Yam et al. (2005)

Four other Ib/c SNe, all with similar luminosity limits

Type Ia SNe - 7 events, no object/cluster.

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Conclusions

SN II-P: most common type, red supergiant progenitors (~M0Ib 8-12M)

Detections and limits on 15 II-P SNe imply they only come from RSG stars with MZAMS<15M

No evidence for BH forming Sne Within 3 years project ~30 progenitors (HST SNAP +

VLT/Gemini NIR purpose built archive) Optical/NIR monitoring of SNe gives 56Ni - probe of explosion

Direct constraints on all core-collapse SNe types

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Nearby core-collapse SNe: discovery rates

0

2

4

6

8

10

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1999 2000 2001 2002 2003 2004 2005

<1000 km/s<1500 km/s

No. of SN per year in galaxies less thanVrad km/s

Nsn (Vrad <1500) = 8.7 yr-1

H0= 75 kms-1Mpc-1

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Radio and X-ray luminosity of II-P

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Chevalier et al. (2005)Radio and X-ray LP consistent with direct mass estimates

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M31 RSG variable

Young, Smartt et al. in prep.

4 years monitoring of M31 (microlensing)

Largest variation ±0.5m

±0.2 dex in logL/L M-type

supergiant, M~20M, logL~5.2 dex

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Magnitudes and colours of progenitor

d=8.4 ± 1 kpc; E(B – V)=0.14 ± 0.02 Colours of K5-M4Ib

supergiant scaled to I=23.3

Bluer than early K-type and it would be detected in V and R.

WavelengthM

agnitude

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Dust enshrouded red supergiants ?

Could progenitors be dusty red supergiants, some of higher luminosity ?

SNe are clearly not reddened But could be destroyed in

explosion (e.g. Meikle & Graham 1986)?

Our deep K-band image rules this out (K>20.7)

If visual extinction AV~5 K-band limit implies MK>-9.5 or

log L/L < 4.6 Hence M < 12M

Gemini NIRI K-band 0.5”

50 Galaxies (<10Mpc) surveyed with VLT/Gemini/UKIRT. Deep JHK images for future SNe

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ACS images SN1993J: U330=20.8 3 Faint companions within 0.35” Contribution to SN of <20% Why is SN1993J so bright in

UV ? Deep, near-UV Keck spectrum

with LRIS-B

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Evolutionary model

ZAMS = 15 and 14M stars

5.8 year period High mass loss from

progenitor to companion ~1000 yrs pre-explosion (4x10-2 M /yr)

SN1987A like event (in 10 000 years time) ?

Maund, Smartt, Kudritzki, Podsiadlowski, Gilmore 2004, Nat.