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SN Rates vs. Environments : The Rate of type Ia SNe in Radio- Galaxies

SN Rates vs. Environments : The Rate of type Ia SNe in Radio- Galaxies. Seyfert ; Metallicity ; Cluster vs. field; Rates in Interacting galaxies; SN Properties vs. off-sets; SN vs X; . Botticella M.T. ( Naples ) Cappellaro E. (Padova) Della Valle M. ( Naples )

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SN Rates vs. Environments : The Rate of type Ia SNe in Radio- Galaxies

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  1. SN Rates vs. Environments: The Rate of typeIaSNe in Radio-Galaxies Seyfert; Metallicity; Cluster vs. field; Rates in Interacting galaxies; SN Properties vs. off-sets; SN vs X; Botticella M.T. (Naples) Cappellaro E. (Padova) Della Valle M. (Naples) Mannucci F. (Arcetri) Padovani P. (ESA/STScI) Panagia N. (ESA/STScI) Turatto, M. (Padova) ChornockR. (Berkeley) Filippenko A. (Berkeley) LeamanJ. (Berkeley) Maoz D. (Tel Aviv) Nayak I. (Berkeley) Li W. (Berkeley)

  2. SN Rates vs. Environments: The Rate of typeIaSNe in Radio-Galaxies Seyfert; Metallicity; Cluster vs. field; Rates in Interacting galaxies; SN Properties vs. off-sets; SN vs X; Botticella M.T. (Naples) Cappellaro E. (Padova) Della Valle M. (Naples) Mannucci F. (Arcetri) Padovani P. (ESA/STScI) Panagia N. (ESA/STScI) Turatto, M. (Padova) ChornockR. (Berkeley) Filippenko A. (Berkeley) LeamanJ. (Berkeley) Maoz D. (Tel Aviv) Nayak I. (Berkeley) Li W. (Berkeley)

  3. Madau, Della Valle & Panagia 1998 The DTD is the distribution of the lags between when the progenitor is formed and the time of the explosion as SN-Ia. • Knowledge of the DTD is useful for understanding the route along which cosmic metal enrichment and energy input by SNeproceed • For obtaining clues about the SN progenitor systems. Different progenitor stars, binary systems, and binary-evolution scenarios (e.g. SD and/or DD) predict different DTDs.

  4. Collection of galaxy models from Bruzual & Charlot (2003), different SF histories (single burst to a rate extended over a Hubble time) metallicities from 2%--250% solar. For each model: present day (B-K) colour and SN-Ia rate, obtained by convolving the SFH of each galaxy with a given DTD Deriving the DTD • evolution of the rate with redshift (Dahlen et al., 2004) • dependence of the rate on the colors (Mannucci et al., 2005) • dependence of the rate with radio-power (Della Valle et al., 2005) Is there a DTD satisfying all of them?

  5. Deriving the DTD Two populations: 30-50% prompt + 70-50% tardy “prompt” “tardy” Mannucci, Della Valle & Panagia 2006

  6. Asiago T<-1.5 X NRAOVLA SKY SURVEY It is a Survey at 1.4 GHz covering the whole sky north of –40o Parkes MIT NRAO Survey at 4.85 GHz f1.4=f5x(5/1.4) -0.75

  7. Sadler, Jenkins & Kotanyi 1989

  8. SNe-Ia in Radio-GalaxiesDella Valle & Panagia 2003; Della Valle et al. 2005 Galaxies C.T. (yr) x 1010 LB SNe Rate SNu(B)

  9. SNe-Ia in Radio-GalaxiesDella Valle & Panagia 2003; Della Valle et al. 2005 Galaxies C.T. (yr) x 1010 LB SNe Rate SNu(B)

  10. SNe-Ia in Radio-GalaxiesDella Valle & Panagia 2003; Della Valle et al. 2005 We concluded that the rate of SNeI-a in radio-loud galaxies is definitely higher than it is in radio-quiet by a factor ~ 2÷6. Significance level ~3σ (Della Valle & Panagia 2003; Della Valle et al. 2005) Galaxies C.T. (yr) x 1010 LB SNe Rate SNu(B)

  11. The ‘jet-induced’ accretion scenario Capetti (2002) and Livio et al. (2002) suggest that jets may lead to an increase of the accretion onto the WDs from ISM up to drive the WD to approach the Chandra limit and trigger an Ia explosion. In the ‘jet-induced’ accretion scenario the enhancement of the rate of SNeI-a … is expected to be spatially confined to the regions close to jets and/or the bulk of radio activity

  12. Thereis no convincingspatialcorrelationbetween SN sites and radio-jets(no statisticallysupported) The Bondi accretionbecomesrelevant for v<1 km/s. For typical star velocities of ~ 100km/s, the amount of accretedmaterialonto the WD (for a crossing-time of 100Myr) is~ 10-5/-6 M (good for nova stars)

  13. The common origin of SNeI-and radio-jets Repeated episodes of interactions or mergers between E’s and dwarf companions are responsible for: a) Strong radio activity in early-types galaxies, which is mostly triggered by interaction or/and mergers (Baade & Minkowski 1954, Heckman et al. 1986). b) the fresh supply of relatively young stellar population in which SNeI-a are best produced

  14. Therefore…. The strong enhancement of SNI-a rate in radiogalaxies has the same common origine as the radio activity but there is not causality link between the two phenomena. By assuming that the radio activity and an episode of star formation are coeval the observed excess of type Ia SNe in radio-loud galaxies implies evolutionary times (main sequence+time to accrete up to explosion) of the same order of magnitude than the duration of radio-activity, i.e. ~ 100 Myr (Srinand & Gopal-Krishna; Wan et al. 2000)

  15. Deriving the DTD • evolution of the rate with redshift (Dahlen et al., 2004) • dependence of the rate on the colors (Mannucci et al., 2005) • dependence of the rate with radio-power (Della Valle et al., 2005) Is there a DTD satisfying all of them?

  16. SN Rates vs. Environments: The Rate of typeIaSNe in Radio-Galaxies Weidong 3178 E/S0 1024 E/S0 (T<-1.5) 15305 yr (x LB) 37 SNe Cappellaro et al. (1999) 2208 E/S0 (T<-1.5) 11096 yr (x LB) 21 SNe

  17. W. vs E. 25 vs 10 in rl 10 vs 4 in rf 2 vs 7 in rq

  18. Li et al. 2011 T<-1.5 X NRAOVLA SKY SURVEY It is a Survey at 1.4 GHz covering the whole sky north of –40o Parkes MIT NRAO Survey at 4.85 GHz f1.4=f5x(5/1.4) -0.75

  19. The SN rate per unit mass B the only available band for a large number of local galaxies until… Jarrett et al., (2003) Mass from NIR data Log(M/LK) = 0.212(B-K) – 0.959 Mannucci et al. (2005)

  20. Deriving the DTD Two populations: 30-50% prompt + 70-50% tardy “prompt” “tardy” Mannucci, Della Valle & Panagia 2006

  21. Deriving the DTD single population: gaussian, 3.4 Gyr Mannucci, DV & Panagia 2006

  22. 3 5 M☉ 8 Deriving the DTD single population: exponential decay, 3 Gyr Mannucci, Della Valle & Panagia 2006

  23. Deriving the DTD Theoretical model: Matteucci & Recchi (2001) - SD

  24. Deriving the DTD Theoretical model: Greggio (2005) – DD (Similar to Yungelson & Livio 2000)

  25. Deriving the DTD Theoretical model: Belczinsky et al. (2004) - SD Prompt 50%  30%

  26. Conclusions

  27. Conclusions SN 2006X +

  28. “…the progenitor to be 10–100 times fainter than previous limits on other SN Ia progenitors. This directly rules out luminous red giants and the vast majority of helium stars as the mass donating companion ….These observations favour a scenario where the exploding WD of SN 2011fe accreted matter either from another WD, or by Roche-lobe overflow from a subgiant or main-sequence companion star….”

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