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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
Others: J. Maund (Texas), J. Danziger (Trieste), P. Meikle (Imperial),
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Overview
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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
Hydrogen lines
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Type I
Type II

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
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Si
He
———
He
or Si
Photometry/spectra properties
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Ia
Ib
Ic
II-P, II-L, IIn, IIb, II-p
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M101
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NGC3621
NGC3949
Example:
 HST Key project – H0 with
Cepheids
 Blue supergiants at 2-7Mpc from
8m telescopes - Bresolin et al.
(2001)
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M81 zoom in
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First red supergiant
progenitor
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SN2003gd discovered
2003 June 12
Normal type II-P
M74 - distance 9.3 1.8
Mpc
3100s WFPC2 preexplosion image F606W
Gemini gri (480-960s),
0.56” images
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Detection of
progenitor
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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
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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 +4-2 M
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
Maund et al. (2005), Li et al. (2006)
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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
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Other examples: no
detection
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SN1999gi in NGC3184,
HST U+V pre-explosion
D=11Mpc (Leonard et al. 2002)
M  12 M
Smartt et al. 2001
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Smartt et al. 2002
SN2001du in NGC1365
HST UVI pre-explosion
D=17Mpc (Cepheid Key P.)
M  15 M
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Summary of II-P
progenitors
SN
Type
Mass
Z
2006bc
II-P
<15
~Z
2005cs
II-P
9 +3/-2
~Z
2004et
II-P
15  2
~1-0.5Z
2004dj
II-P
15  5
~Z
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
Ref
Li et al. 2005
Maiz-Apellaniz et al. 2004,
Wang et al. 2005,2006
Rest from Crockett
et al. 2006, Maund &
Smartt 2005, Maund
et al. 2005, Hendry
et al. 2006, Smartt et
al. 2004, 2003,
2002, 2001
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93J
Observed
Ib/c
Observed
II-P
80K
87A
Heger et al. (2000) - now can place observational constraints
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STARS stellar evolutionary tracks (Eldridge & Tout 2004)
 Eldridge, Smartt (in prep) - probability without mass cut ~5%
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UVOIR Light Curves and 56Ni
Mass
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56
Ni  56Co  e   e  
( 1/2  6 days)
56
Co  56 Fe  e   e  
( 1/2  77.1 days)
Late time tail powered by
radioactive 56Ni
56Ni explosively created
from Si burning after corecollapse
Direct probe of the
explosion
How Is it related to
progenitor mass ?
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Black-hole forming SNe ?
Zampieri et al., Nomoto et al - low luminosity SNe form black-holes
 No evidence so far of the branching at high luminosity
 Detailed comparison with models now possible
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Constraints on a Type Ic
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SN2004gt - type Ic
Gamma-ray bursts
coincident with Ic
supernovae
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Restricted region in the
HRD
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Maund, Smartt, Schwiezer (2005)
Gal-Yam et al. (2005)
We would have detected
massive evolved stars
Either a star of 120-150M
or
More likely a lower mass
object in a binary
Four other Ib/c SNe, all
with similar luminosity
limits
Type Ia SNe - 7 events,
no object/cluster.
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Conclusions
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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
H0= 75 kms-1Mpc-1
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10
No. of
SN per
year in
galaxies
less than
Vrad km/s
8
<1000 km/s
<1500 km/s
6
4
2
0
1999
2000
2001
2002
2003
2004
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Nsn (Vrad <1500) = 8.7 yr-1
2005
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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
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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
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Magnitude
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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 Ktype and it would be
detected in V and R.
Wavelength
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Dust enshrouded red
supergiants ?
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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
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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
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Maund, Smartt, Kudritzki, Podsiadlowski, Gilmore 2004, Nat.
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) ?
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