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Quic k Ti me™ and a T IFF (Unc om pres s ed) dec om pres s or are needed to s ee t his pic t ure. QuickTi me™ and a T IFF (Uncom pressed) decom pressor are needed to see t his pict ure. QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. 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), 1 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 ? 2 Credit: LOSS and T. Debosz 3 Summary of SNe types Supernovae are classified by their optical spectra No hydrogen Hydrogen lines Type I Type II Si He ——— He or Si Photometry/spectra properties Ia Ib Ic II-P, II-L, IIn, IIb, II-p 4 M101 QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. NGC3621 NGC3949 Example: HST Key project – H0 with Cepheids Blue supergiants at 2-7Mpc from 8m telescopes - Bresolin et al. (2001) 5 M81 zoom in QuickTime™ and a YUV420 codec decompressor are needed to see this picture. 6 First red supergiant progenitor SN2003gd discovered 2003 June 12 Normal type II-P M74 - distance 9.3 1.8 Mpc 3100s WFPC2 preexplosion image F606W Gemini gri (480-960s), 0.56” images 7 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 8 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 +4-2 M Smartt et al. 2004, Science 9 SN2005cs in M51 • • QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. • • 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 10 Detection of progenitor Maund et al. (2005), Li et al. (2006) 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 11 Other examples: no detection SN1999gi in NGC3184, HST U+V pre-explosion D=11Mpc (Leonard et al. 2002) M 12 M Smartt et al. 2001 Smartt et al. 2002 SN2001du in NGC1365 HST UVI pre-explosion D=17Mpc (Cepheid Key P.) M 15 M 12 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 13 93J Observed Ib/c Observed II-P 80K 87A Heger et al. (2000) - now can place observational constraints 14 STARS stellar evolutionary tracks (Eldridge & Tout 2004) Eldridge, Smartt (in prep) - probability without mass cut ~5% 15 UVOIR Light Curves and 56Ni Mass 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 ? 16 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 17 Constraints on a Type Ic SN2004gt - type Ic Gamma-ray bursts coincident with Ic supernovae 18 Restricted region in the HRD 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. 19 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 20 Nearby core-collapse SNe: discovery rates H0= 75 kms-1Mpc-1 12 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 Nsn (Vrad <1500) = 8.7 yr-1 2005 21 Radio and X-ray luminosity of II-P QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. Chevalier et al. (2005) Radio and X-ray LP consistent with direct mass estimates 22 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 23 Magnitudes and colours of progenitor Magnitude 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 24 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 25 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 26 Evolutionary model 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) ? 27