1 / 27

The progenitor stars of core-collapse supernovae

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

triage
Télécharger la présentation

The progenitor stars of core-collapse supernovae

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. 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),

  2. 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 ?

  3. Credit: LOSS and T. Debosz

  4. 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 ———

  5. M101 NGC3621 Example: • HST Key project – H0withCepheids • Blue supergiants at 2-7Mpc from 8m telescopes - Bresolin et al. (2001) NGC3949

  6. M81 zoom in

  7. 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 gri (480-960s), 0.56” images

  8. 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

  9. 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 -2M +4 Magnitudes and colours of progenitor Smartt et al. 2004, Science

  10. SN2005cs in M51 • 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

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

  12. 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 • SN2001du in NGC1365 • HST UVI pre-explosion • D=17Mpc (Cepheid Key P.) • M  15 M Smartt et al. 2002

  13. Summary of II-P progenitors Rest from Crockett et al. 2006, Maund & Smartt 2005, Maund et al. 2005, Hendry et al. 2006, Smartt et al. 2004, 2003, 2002, 2001

  14. 93J Observed Ib/c Observed II-P 80K 87A Heger et al. (2000) - now can place observational constraints

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

  16. 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

  17. 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

  18. Constraints on a Type Ic • SN2004gt - type Ic • Gamma-ray bursts coincident with Ic supernovae

  19. 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 • Four other Ib/c SNe, all with similar luminosity limits • Type Ia SNe - 7 events, no object/cluster. Maund, Smartt, Schwiezer (2005) Gal-Yam et al. (2005)

  20. 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

  21. Nsn (Vrad <1500) = 8.7 yr-1 Nearby core-collapse SNe: discovery rates H0= 75 kms-1Mpc-1 No. of SN per year in galaxies less than Vrad km/s

  22. Radio and X-ray luminosity of II-P Chevalier et al. (2005) Radio and X-ray LPconsistent with direct mass estimates

  23. 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

  24. 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. Magnitudes and colours of progenitor Magnitude Wavelength

  25. 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

  26. 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

  27. 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.

More Related