sn rates vs. environments : the rate of type ia sne in radio- galaxies

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

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Seyfert; Metallicity; Cluster vs. field; Rates Seyfert; Metallicity; Cluster vs. field; Rates in Interacting galaxies; SN Properties vs. in Interacting galaxies; SN Properties vs. off-sets; SN vs X; off-sets; SN vs X;

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

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Seyfert; Metallicity; Cluster vs. field; Rates Seyfert; Metallicity; Cluster vs. field; Rates in Interacting galaxies; SN Properties vs. in Interacting galaxies; SN Properties vs. off-sets; SN vs X; off-sets; SN vs X;

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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.

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Madau, Della Valle & Panagia 1998

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Deriving the DTD

1. evolution of the rate with redshift (Dahlen et al., 2004)

2. dependence of the rate on the colors (Mannucci et al., 2005)

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 Gyrevolution of the

colors

0.1 Gyrlifetime 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

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Two populations: 30-50% prompt + 70-50% tardy

Deriving the DTD

“prompt” “tardy ”

Mannucci, Della Valle & Panagia 2006

NNRAOVVLA SSKY SSURVEY

It is a Survey at 1.4 GHz covering the whole sky north of –40o

PParkes MMIT NNRAO Survey at 4.85 GHz f1.4=f5x(5/1.4) -0.75

XX

Asiago T<-1.5 Asiago T<-1.5

7

Sadler, Jenkins & Kotanyi Sadler, Jenkins & Kotanyi 19891989

Radio-loud1029

erg s-1 Hz-1

Radio-faint>1027 & <1029

erg s-1 Hz-1

Radio-quiet < 1027

erg s-1 Hz-1

8

99

Radio-Quiet1729

7127 +0.06

0.11

-0.03

Radio-Faint212

1770 +0.18

0.23 -0.11

Radio-Loud267

2199 +0.19

0.43 -0.14

SNeSNeGalaxies C.T. (yr) x 1010 LB Rate SNu(B)Rate SNu(B)

SNe-Ia in Radio-Galaxies Della Valle & Panagia

2003;

Della Valle et al. 2005

1010

Radio-Quiet1729

7127 7 +0.06

0.11

-0.03

Radio-Faint212

1770 4 +0.18

0.23 -0.11

Radio-Loud267

2199 10 +0.19

0.43 -0.14

SNeSNeGalaxies C.T. (yr) x 1010 LB Rate SNu(B)Rate SNu(B)

SNe-Ia in Radio-Galaxies Della Valle & Panagia

2003;

Della Valle et al. 2005

1111

Radio-Quiet1729

7127 7 +0.06

0.11

-0.03

Radio-Faint212

1770 4 +0.18

0.23 -0.11

Radio-Loud267

2199 10 +0.19

0.43 -0.14

SNeSNeGalaxies C.T. (yr) x 1010 LB Rate SNu(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 ~3σ

(Della Valle & Panagia 2003; Della Valle et al. 2005)

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… 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

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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)

32 v WDacc MM

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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

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The strong enhancement of SNI-a rate in radiogalaxies has the same common origine as the radio activity but there is there is notnot 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)

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Deriving the DTD

1. evolution of the rate with redshift (Dahlen et al., 2004)

2. dependence of the rate on the colors (Mannucci et al., 2005)

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 Gyrevolution of the

colors

0.1 Gyrlifetime of radio

activity

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

Cappellaro et al. (1999)Cappellaro et al. (1999)

2208 E/S0 (T<-1.5)

11096 yr (x LB) 21 SNe

Weidong Weidong 3178 E/S0 3178 E/S0

1024 E/S0 (T<-1.5)

15305 yr (x LB) 37 SNe

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19

20

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W. vs E.W. vs E.

25 vs 10 in rl25 vs 10 in rl

10 vs 4 in rf10 vs 4 in rf

2 vs 7 in rq2 vs 7 in rq

NNRAOVVLA SSKY SSURVEY

It is a Survey at 1.4 GHz covering the whole sky north of –40o

PParkes MMIT NNRAO Survey at 4.85 GHz f1.4=f5x(5/1.4) -0.75

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Li et al. 2011 T<-1.5 Li et al. 2011 T<-1.5

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2323

The SN rate per unit massB the only available band for a large number of local galaxies until…

Jarrett et al., (2003)

Log(M/LK) = 0.212(B-K) – 0.959

Mass from NIR data

Mannucci et al. (2005)

2424

2525

26

2727

Two populations: 30-50% prompt + 70-50% tardy

Deriving the DTD

“prompt” “tardy ”

Mannucci, Della Valle & Panagia 2006

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Mannucci, DV & Panagia 2006

single population: gaussian, 3.4 Gyr

Deriving the DTD

2929

single population: exponential decay, 3 Gyr

Deriving the DTD

8

53

M☉

Mannucci, Della Valle & Panagia 2006

3030

Deriving the DTDTheoretical model: Matteucci & Recchi (2001) - SD

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Deriving the DTDTheoretical model: Greggio (2005) – DD (Similar to Yungelson & Livio 2000)

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Theoretical model: Belczinsky et al. (2004) - SD

Deriving the DTD

Prompt 50% Prompt 50% 30% 30%

3333

3434

Conclusions

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Conclusions

++

SN 2006XSN 2006X

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

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