1. SN Rates vs. Environments: The Rate of type Ia SNe in Radio-Galaxies 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) Chornock R. (Berkeley) Filippenko A. (Berkeley) Leaman J. (Berkeley) Maoz D. (Tel Aviv) Nayak I. (Berkeley) Li W. (Berkeley) 1 Seyfert; Metallicity; Cluster vs. field; Rates in Interacting galaxies; SN Properties vs. off-sets; SN vs X;

2. SN Rates vs. Environments: The Rate of type Ia SNe in Radio-Galaxies 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) Chornock R. (Berkeley) Filippenko A. (Berkeley) Leaman J. (Berkeley) Maoz D. (Tel Aviv) Nayak I. (Berkeley) Li W. (Berkeley) 2 Seyfert; Metallicity; Cluster vs. field; Rates in Interacting galaxies; SN Properties vs. off-sets; SN vs X;

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4. 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 SNe proceed 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 Madau, Della Valle & Panagia 1998

5. 5 Deriving the DTD 1. 1.evolution of the rate with redshift (Dahlen et al., 2004) 2. 2.dependence of the rate on the colors (Mannucci et al., 2005) 3. 3.dependence of the rate with radio-power (Della Valle et al., 2005) Is there a DTD satisfying all of them? Timescale few Gyrs evolution of the cosmic SFR 0.5-1 Gyr evolution of the colors 0.1 Gyr lifetime of radio activity 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

6. 6 Two populations: 30-50% prompt + 70-50% tardy Deriving the DTD “ prompt ” “ tardy ” Mannucci, Della Valle & Panagia 2006

7. NVSS N RAO V LA S KY S URVEY It is a Survey at 1.4 GHz covering the whole sky north of –40 o PMN P arkes M IT N RAO Survey at 4.85 GHz f1.4=f5x(5/1.4) -0.75 X Asiago T<-1.5 7

8. Sadler, Jenkins & Kotanyi 1989 Radio-loud 10 29 erg s -1 Hz -1 Radio-faint >10 27 & <10 29 erg s -1 Hz -1 Radio-quiet < 10 27 erg s -1 Hz -1 8

9. 9 Radio-Quiet 1729 7127 +0.06 0.11 -0.03 Radio-Faint 212 1770 +0.18 0.23 -0.11 Radio-Loud 267 2199 +0.19 0.43 -0.14 SNe Galaxies C.T. (yr) x 10 10 L B  Rate SNu(B) SNe-Ia in Radio-Galaxies Della Valle & Panagia 2003; Della Valle et al. 2005

10. 10 Radio-Quiet 1729 71277 +0.06 0.11 -0.03 Radio-Faint 212 17704 +0.18 0.23 -0.11 Radio-Loud 267 219910 +0.19 0.43 -0.14 SNe Galaxies C.T. (yr) x 10 10 L B  Rate SNu(B) SNe-Ia in Radio-Galaxies Della Valle & Panagia 2003; Della Valle et al. 2005

11. 11 Radio-Quiet 1729 71277 +0.06 0.11 -0.03 Radio-Faint 212 17704 +0.18 0.23 -0.11 Radio-Loud 267 219910 +0.19 0.43 -0.14 SNe Galaxies C.T. (yr) x 10 10 L B  Rate SNu(B) SNe-Ia in Radio-Galaxies Della 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 ~3 σ (Della Valle & Panagia 2003; Della Valle et al. 2005)

12. 12 … is expected to be spatially confined to the regions close to jets and/or the bulk of radio activity 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

13. 13 There is no convincing spatial correlation between SN sites and radio- jets (no statistically supported) The Bondi accretion becomes relevant for v<1 km/s. For typical star velocities of ~ 100km/s, the amount of accreted material onto the WD (for a crossing-time of 100Myr) is ~ 10 -5 / -6 M  (good for nova stars)

14. 14 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

15. 15 there is not 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. Therefore…. 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)

16. 16 Deriving the DTD 1. 1.evolution of the rate with redshift (Dahlen et al., 2004) 2. 2.dependence of the rate on the colors (Mannucci et al., 2005) 3. 3.dependence of the rate with radio-power (Della Valle et al., 2005) Is there a DTD satisfying all of them? Timescale few Gyrs evolution of the cosmic SFR 0.5-1 Gyr evolution of the colors 0.1 Gyr lifetime of radio activity

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18. SN Rates vs. Environments: The Rate of type Ia SNe in Radio-Galaxies Cappellaro et al. (1999) 2208 E/S0 (T<-1.5) 11096 yr (x L B  ) 21 SNe Weidong  3178 E/S0 1024 E/S0 (T<-1.5) 15305 yr (x L B  ) 37 SNe 18

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21. 21 W. vs E. 25 vs 10 in rl 10 vs 4 in rf 2 vs 7 in rq

22. NVSS N RAO V LA S KY S URVEY It is a Survey at 1.4 GHz covering the whole sky north of –40 o PMN P arkes M IT N RAO Survey at 4.85 GHz f1.4=f5x(5/1.4) -0.75 X Li et al. 2011 T<-1.5 22

23. 23 The SN rate per unit mass B the only available band for a large number of local galaxies until… Jarrett et al., (2003) Log(M/L K ) = 0.212(B-K) – 0.959 Mass from NIR data Mannucci et al. (2005)

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27. 27 Two populations: 30-50% prompt + 70-50% tardy Deriving the DTD “ prompt ” “ tardy ” Mannucci, Della Valle & Panagia 2006

28. 28 Mannucci, DV & Panagia 2006 single population: gaussian, 3.4 Gyr Deriving the DTD

29. 29 single population: exponential decay, 3 Gyr Deriving the DTD 8 5 3 M☉M☉ Mannucci, Della Valle & Panagia 2006

30. 30 Deriving the DTD Theoretical model: Matteucci & Recchi (2001) - SD

31. 31 Deriving the DTD Theoretical model: Greggio (2005) – DD (Similar to Yungelson & Livio 2000)

32. 32 Theoretical model: Belczinsky et al. (2004) - SD Deriving the DTD Prompt 50%  30%

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34. 34 Conclusions

35. 35 + SN 2006X

36. 36 “…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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