the progenitor stars of core-collapse supernovae
DESCRIPTION
The progenitor stars of core-collapse supernovae. Stephen J. Smartt Astrophysics Research Centre Queen’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 - PowerPoint PPT PresentationTRANSCRIPT
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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 ?
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Credit: 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
87A
80K
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 =6days)56Co→ 56Fe+ e+ +νe +γ(τ1/2 =77.1days)
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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.