SN Ia Rate Dependence on Host Galaxy Properties in Subaru ...okumura/up/okumura_KyotoBinary.pdf · Type Ia Supernova • thermonuclear explosions of carbon-oxgen white dwarf (WD)

SN Ia Rate Dependence on Host Galaxy Properties in Subaru SXDS and Implications for Delay Time Distribution

Jun Okumura (Kyoto Univ.)

Tomonori Totani (Kyoto Univ), Yutaka Ihara (Tokyo Univ.), Tomoki Morkuma (NAOJ), Mamoru Doi (Tokyo Univ.),

Naoki Yasuda (IPMU)

2010年7月26日月曜日

Type Ia Supernova• thermonuclear explosions of carbon-oxgen white dwarf

(WD) in binary systems

• The progenitor binary system leading to SNe Ia is still unknown

- single degenerate scenario (SD)

the accretion is from a non-degenerate companion star

- double degenerate scenario (DD)

a merger of two WDs results in a SNe Ia


Delay Time Distribution (DTD)

• SNe Ia are expected to have a wide range of delay times from star formation to supernova explosions, and the DTD can be used to discriminate the the proposed progenitor models



• SNe Ia are expected to have a wide range of delay times form star formation to supernova explosions, and the DTD can be used to discriminate the the proposed progenitor models

- DD : the delay times is mainly determined by the from the formation of a DD binary to a merger after angular momentum loss by gravitational wave radiation

- power-law like DTD

tGW




- DD : the delay times is mainly determined by the from the formation of a DD binary to a merger after angular momentum loss by gravitational wave radiation

- power-law like DTD

tGW

tIa ∼ tGW ∝ a4 a : separation

fsep(a) ∝ aβ

fD ∝ fsep(a)da

dtIa∝ t−(3−β)/4

Ia




- SD : the delay time is essentially determined by the main-sequence lifetime of the secondary star in a binary

- some characteristic secondary mass scales preferred for successful SN Ia events


Totani+08• measured the SN Ia DTD in a delay time range of

0.1-8.0 Gyr by using faint variable objects detected in Subaru/XMM-Newton Deep Survey (SXDS)

• passive galaxy sample (already formed 90% of stars)

> delay time can be approximated by stellar age

• 65 SN candidates showing significant spatial offset fromthe nuclei of the host galaxies

• Power-law DTD at ~0.1-10Gyr

DTD ∝ t−1


Totani+08• measured the SN Ia DTD in a delay time range of

0.1-8.0 Gyr by using faint variable objects detected in Subaru/XMM-Newton Deep Survey (SXDS)

• passive galaxy sample (already formed 90% of stars)

> delay time can be approximated by stellar age

• 65 SN candidates showing significant spatial offset fromthe nuclei of the host galaxies

• Power-law DTD at ~0.1-10Gyr

DTD ∝ t−1

< tIa >=� tga0 tIaψ(tga − tIa)fD(tia)dtIa� tga

0 ψ(tga − tIa)fD(tIa)dtIa


DTD and Ia progenitor

- consistent with generic DTD features of DD models

- in SD case, observed DTD strongly constrain the parameter space of SD models


This Work• In Totani+08, only passive galaxies were selected and SN

Ia candidate were picked up as transient having significant offset so that DTD can be measured safely

> Motivation: would like to examine the DTD including all types of galaxies using SN Ia sample identified by LC fitting

• the correlation between SN Ia rate and host properties

• Investigate the correlation between SN Ia rate and host galaxy properties (SSFR, stellar mass, SFR) and test various DTD models/functions


This Work• In Totani+08, only passive galaxies were selected and SN

Ia candidate were picked up as transient having significant offset so that DTD can be measured safely

> Motivation: would like to examine the DTD including all types of galaxies using SN Ia sample identified by LC fitting

• the correlation between SN Ia rate and host properties

• Investigate the correlation between SN Ia rate and host galaxy properties (SSFR, stellar mass, SFR) and test various DTD models/functions

Mannucci+05Nearby (~100Mpc)

Sullivan+060.2 < z < 0.75


SXDS Data - Galaxy- wide (~1deg^2)

- multi-wavelength surveyoptical: B,V,Rc,i’,z(Subaru/Suprime-Cam)NIR: J, K (UKIDSS survey)IR: 3.6μm, 4.5μm (Spitzer/IRAC)X-ray: 0.5-2.0, 2.0-100keV (XMM-Newton)

• ~10 epochs during 2002/09-2005/09

• hyperz code

> SFH, stellar mass, Av

• > 69159 galaxieswave length

flu

x

Rc, i�, 3.6µm detection (mlim = 27.7, 27.7, 23.1)


SNe sample (Ihara+10, in prep)

• photometrically confirmed 46 SNe Ia (0.2 < z < 1.3)

- Light curve fitting with Hsiao+08 template

- in our galaxy sample > 39 SNe Ia Free parameter:• maximum brightness• stretch• redshift


testing DTD models• Power-law DTD

- Totani+08 DTD

- Pritchet+08 DTD

- index -1.5 DTD

• A+B model (Scannapieco & Bildsten 05)

SNR = AMtot(t) + Bψ(t)delayed prompt

DTD ∝ t−0.5(Pritchet + 08)

DTD ∝ t−1.08(Totani + 08)

Maoz+10

SNR =� t

0ψ(t�)DTD(t− t�) dt�

A = 11.7 [10−14yr−1 M−1⊙ ]

B = 12.1 [10−4M−1⊙ ]


Rate Calculation

• control time (CT) : detectable time of SN Ia

• SNR: Suprenova rate

- SN rate can be affected by dust extinction- photo-z Av (might be an overcorrection)- tried to see how extinction can affect the SN rate for

two extreme case (w/o extinction, photo-z Av)

0

10

20

30

40

50

60

70

0.2 0.4 0.6 0.8 1 1.2 1.4

cont

rol t

ime

[day

]

redshift

Av 0.0Av 0.2Av 0.4Av 0.6Av 0.8Av 1.0Av 1.2Av 1.4Av 1.6Av 1.8Av 2.0

con

trol

tim

eredshift

SNR =Nobs

Σ CTi(z,AV )

Observation

Why extinction ?


result - stellar massSN

Ia R

ate

stellar mass

A+B Power-law DTD

-4

-3.5

-3

-2.5

-2

-1.5

-1

-0.5

8 8.5 9 9.5 10 10.5 11 11.5 12

LOG

SN

Ia ra

te p

er g

alax

y [y

r-1]

stellar mass [Msun]

w/ extinctionw/o extinction

This WorkSullivan+06

Neil+06Scannappieco ildsten 05

-4

-3.5

-3

-2.5

-2

-1.5

-1

-0.5

8 8.5 9 9.5 10 10.5 11 11.5 12LO

G S

N Ia

rate

per

gal

axy

[yr-1

]

stellar mass [Msun]


Totani+08 DTDPritchet+08 DTD

index -1.5 DTD


result - SFRSN

Ia R

ate

SFR

A+B Power-law DTD

-4

-3.5

-3

-2.5

-2

-1.5

-1

-0.5

-1.5 -1 -0.5 0 0.5 1 1.5 2 2.5

LOG

SN

Ia ra

te p

er g

alax

y [y

r-1]

LOG SFR [Msun yr-1]



Neil+06Scannappieco ildsten 05 -4

-3.5

-3

-2.5

-2

-1.5

-1

-0.5

-1.5 -1 -0.5 0 0.5 1 1.5 2 2.5LO

G S

N Ia

rate

per

gal

axy

[yr-1

]

LOG SFR [Msun yr-1]



index -1.5 DTD


result - SSFRSN

uM

SSFR

A+B Power-law DTD

-14

-13.5

-13

-12.5

-12

-11.5

-11

-10.5

-13 -12 -11 -10 -9 -8LO

G S

NuM

[yr-1

Msu

n-1]

LOG SSFR[yr-1]



index -1.5 DTD-14

-13.5

-13

-12.5

-12

-11.5

-11

-10.5

-13 -12 -11 -10 -9 -8

LOG

SNu

M [y

r-1M

sun-1

]

LOG SSFR[yr-1]



Neil+06Scannapieco ildsten 05


A+B model• the values of A and B

- A+B model can reproduce the observation well, however, these value can be changed which field or populations we are looking on

- need a careful treatment when applied as universal DTD

Sullivan+06 Neil+06 Scannapieco&Bildsten05

A = 5.3+1.2−1.2

B = 3.9+0.7−0.7

A = 1.4+1.0−1.0

B = 8.0+2.6−2.6

A = 4.4+1.6−1.4

B = 26+11−11

A = 11.7 [10−14yr−1 M−1⊙ ]

B = 12.1 [10−4M−1⊙ ]


conclusion• the correlation between SN Ia rate and host galaxy

properties is confirmed at z=0.2-1.3

• extinction correction could affect the SN rate estimates significantly and must be carefully taken into account

• Totani+08 DTD is consistent with the data within the uncertainty of extinction, but Pritchet DTD seems to be shallow in SSFR-SNuM plot

• A+B model is also consistent with the data, but the AB values are significantly different among different samples/papers



SN Ia rate study in SXDS

• Ihara+10, in prep in collaboration with Supernova Cosmology Project

- SN Ia rates at 0.2 < z < 1.3

- Ia rate increases up to z~1.2

rV (z) = r0(1 + z)α

r0 = 0.20+0.08−0.05(stat.)+0.03

−0.04(syst.)× 10−4yr−1Mpc−3

α = 2.55+0.56−0.40(stat.)+0.22

−0.32(syst.)


sullivan+06stellar mass SFR


DTD

DTD models

Del

ay T

ime

Dis

trib

utio

n

0.01

0.1

1

10

0.1 1 10

SN Ia

DTD

[cen

tury

-1 (1

010L K

,0)-1

)]

Delay Time [Gyr]

index -1.0index -0.5index -1.5

0.01

0.1

1

10

0.1 1 10

SN Ia

DTD

[cen

tury

-1 (1

010L K

,0)-1

)]

Delay Time [Gyr]

index -1.0index -0.5index -1.5

w/o extinction w/extinction


SSFR

prompt & delayed components

late typeearly type

SNuM

-14

-13.5

-13

-12.5

-12

-11.5

-11

-10.5

-13 -12 -11 -10 -9 -8

LOG

SNu

M [y

r-1M

sun-1

]

LOG SSFR[yr-1]


Totani+08 DTDprompt

delayed


SSFR

A & B components

late typeearly type

SNuM

-14

-13.5

-13

-12.5

-12

-11.5

-11

-10.5

-13 -12 -11 -10 -9 -8

LOG

SNu

M [y

r-1M

sun-1

]

LOG SSFR[yr-1]


A+B modelA-componentB-component


SSFR

SSFR histogram

SSFR大late type

SSFR小early type

SNuM

0

2

4

6

8

10

12

14

16

18

20

-13 -12 -11 -10 -9 -8

Num

ber

LOG sSFR [yr-1]

SNe Iagalaxies / 1000


stellar massSN

Ia R

ate


-4

-3.5

-3

-2.5

-2

-1.5

-1

-0.5

8 8.5 9 9.5 10 10.5 11 11.5 12

LOG

SN

Ia ra

te p

er g

alax

y [y

r-1]

stellar mass [Msun]


Totani+08 DTDprompt

delayed


stellar massSN

Ia R

ate

A & B components

-4

-3.5

-3

-2.5

-2

-1.5

-1

-0.5

8 8.5 9 9.5 10 10.5 11 11.5 12

LOG

SN

Ia ra

te p

er g

alax

y [y

r-1]

stellar mass [Msun]




stellar massSN

Ia R

ate

stellar mass histogram

0

2

4

6

8

10

12

14

16

6 7 8 9 10 11 12

Num

ber

LOG stellar mass [Msun]



SFRSN

Ia R

ate


-4

-3.5

-3

-2.5

-2

-1.5

-1

-0.5

-1.5 -1 -0.5 0 0.5 1 1.5 2 2.5

LOG

SN

Ia ra

te p

er g

alax

y [y

r-1]

LOG SFR [Msun yr-1]


Totani+08 DTDprompt

delayed


SFRSN

Ia R

ate

A & B components

-4

-3.5

-3

-2.5

-2

-1.5

-1

-0.5

-1.5 -1 -0.5 0 0.5 1 1.5 2 2.5

LOG

SN

Ia ra

te p

er g

alax

y [y

r-1]

LOG SFR [Msun yr-1]




SFRSN

Ia R

ate

SFR histogram

0

2

4

6

8

10

12

14

16

-3 -2 -1 0 1 2

Num

ber

LOG SFR [Msun yr-1]



Mannucci+06


Mannucci+06


sed-sfr vs uv-sfrSE

D-S

FR

10-4

10-2

100

102

104

10-4 10-2 100 102 104

SED

-SFR

[Msu

n yr

-1]

UV-SFR [Msun yr-1]

z>0.466z<0.466SN host

UV-SFR


SFR vs stellar massSF

R

stellar mass

10-4

10-3

10-2

10-1

100

101

102

103

104

104 105 106 107 108 109 1010 1011 1012 1013

UV-

SFR

[Msu

n yr

-1]

stellar mass [Msun]

galaxiesSN host


star extractionR

- 3

.6μm

R - i’

-4

-2

0

2

4

6

8

-0.5 0 0.5 1 1.5 2

mR

-m3.

6 [m

ag]

mR-mi’ [mag]

extra-galacticgalactic


MB vs stretch-1

-22

-21.5

-21

-20.5

-20

-19.5

-19

-18.5

-18

-17.5 0.8 0.9 1 1.1 1.2 1.3

MB

[mag

]

stretch-1


Rate Calculation

• control time (CT) : detectable time of SN Ia

• SNR: Suprenova rate

- Nexp = 37.61（Nobs = 39）- w/o extinction : Nexp = 71.87

0

10

20

30

40

50

60

70

0.2 0.4 0.6 0.8 1 1.2 1.4

cont

rol t

ime

[day

]

redshift

Av 0.0Av 0.2Av 0.4Av 0.6Av 0.8Av 1.0Av 1.2Av 1.4Av 1.6Av 1.8Av 2.0

con

trol

tim

eredshift

SNR =Nobs

Σ CTi(z,AV )

SNR =� t

0ψ(t�)DTD(t− t�) dt�

Observation

Model

Nexp = Σ SNRi · CTi


Documents

SN Ia Rate Dependence on Host Galaxy Properties in Subaru ...okumura/up/okumura_KyotoBinary.pdf · Type Ia Supernova • thermonuclear explosions of carbon-oxgen white dwarf (WD)