Mid$and$Far$Infrared$Proper/es$of$a$Complete$Sample$of$Local$AGNs

1

Kohei$Ichikawa$(Kyoto$University)

The$Second$AKARI$ConferenceFeb$27I29,$2012$in$Jeju,$Korea

CollaboratorsYoshihiro$Ueda$(Kyoto$Univ.),$Yuichi$Terashima$(Ehime$Univ.),$Shinki$Oyabu$(Nagoya$Univ.),$Poshak$Gandhi,$Keiko$Matsuta,$

and$Takao$Nakagawa$(ISAS/JAXA)

Ichikawa/et/al./2012/submi7ed/to/ApJ

Ac/ve$Galac/c$Nuclei$(AGN)

The$AGN$unified$model

AGNs in ULIRGs are buried

AGNs obscured by torus-shaped dust

Detectable via optical spectroscopy

NLR

Sy2Classical$AGN

ⓒNASA

Op/cal$SpectroscopyMainly$type$1$

(+$small$number$of$type$2)

AGN$has$various$kind$of$torus$size.

NewIType$AGN

ⓒISAS/JAXA

XIray$SpectroscopyVery$small$torus$opening$angle,

buried$AGN(NewIType$AGN:$NH~1024$cmI2)$

Ueda+$’07,$Eguchi+$’09

3

faceIon(type$1)

edgeIon(type$2)

Mo/va/on:AGN$torus$structureTorus$structure$itself$is$not$well$studied...

We$can$observa/onally$constrain$the$torus$models$of$AGNs$with$various$kind$of$torus$size.

LMIR(typeI2)

AGN$sampleOur$Goal$No.1：Making$new$AGN$sample$including$NewIType$AGN

＝We$need$NH$unbiased$surveysOur$Goal$No.2：To$constrain$the$torus$models$observa/onally

Parent$Sample：Swij/BAT$Hard$XIray$(14$I195$keV)$catalog

5

Our$Sample:$Hard$XIray$&$Mid$Infrared$(MIR)$All$Sky$Survey$Catalog

(Hard$XIray$(E>10$keV):$strong$penetra/on$up$to$NH$~$1024.5$cmI2$)

MIR$catalog$I>$$AKARI$All$Sky$Survey$Catalog$(9,$18,$and$90$um)$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$IRAS$Point/Faint$Source$Catalog$(12,$25$um)

$$$$$$$WISE$preliminary$Catalog$(12,$22$um)

Note:$AKARI,$IRAS,$WISE:$Difference$of$Central$Wavelength

Rela/ons$between$AKARI$and$WISE,$IRAS

AKARI$9$um$v.s.$IRAS$12$um,$WISE$12$um

AKARI$18$um$v.s.$IRAS$25$um,$WISE$22$umWe$checked$luminosity$rela/ons

10 Ichikawa et al.

0

5

10

15

20

25

30

0 0.05 0.1 0.15 0.2

Num

ber o

f sou

rces

Distance[arcmin]

IRCFIS

Fig. 1.— The histograms of position difference between the optical counterparts of the Swift/BAT AGNs and their AKARI counterparts(red: IRC, blue: FIS).

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(IR

AS 1

2µm

) [er

g s-

1 ]

log!L!(AKARI 9µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(IR

AS 2

5µm

) [er

g s-

1 ]

log!L!(AKARI 18µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(W

ISE

12µm

) [er

g s-

1 ]

log!L!(AKARI 9µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(W

ISE

25µm

) [er

g s-

1 ]

log!L!(AKARI 18µm) [erg s-1]

Fig. 2.— The plot of infrared luminosities between AKARI and IRAS (top panels). Each panel shows luminosity relation betweenAKARI 9 µm v.s. IRAS 12 µm (Left: 48 sample) , AKARI 18 µm v.s. IRAS 25 µm (Right: 51 sample) respectively. Bottom panels showthe infrared luminosities between AKARI and WISE, AKARI 9 µm v.s. WISE 12 µm (Left: 31 sample) and AKARI 18 µm v.s. WISE 22µm (Right 32 sample) .

10 Ichikawa et al.

0

5

10

15

20

25

30

0 0.05 0.1 0.15 0.2

Num

ber o

f sou

rces

Distance[arcmin]

IRCFIS

Fig. 1.— The histograms of position difference between the optical counterparts of the Swift/BAT AGNs and their AKARI counterparts(red: IRC, blue: FIS).

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(IR

AS 1

2µm

) [er

g s-

1 ]

log!L!(AKARI 9µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(IR

AS 2

5µm

) [er

g s-

1 ]

log!L!(AKARI 18µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(W

ISE

12µm

) [er

g s-

1 ]

log!L!(AKARI 9µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5lo

g!L !

(WIS

E 25

µm) [

erg

s-1 ]

log!L!(AKARI 18µm) [erg s-1]

Fig. 2.— The plot of infrared luminosities between AKARI and IRAS (top panels). Each panel shows luminosity relation betweenAKARI 9 µm v.s. IRAS 12 µm (Left: 48 sample) , AKARI 18 µm v.s. IRAS 25 µm (Right: 51 sample) respectively. Bottom panels showthe infrared luminosities between AKARI and WISE, AKARI 9 µm v.s. WISE 12 µm (Left: 31 sample) and AKARI 18 µm v.s. WISE 22µm (Right 32 sample) .

AKARI$18um AKARI$18um

IRAS$25um

AKARI$18um$v.s.$IRAS$25um AKARI$18um$v.s.$WISE$22$um

WISE$22um

AKARIとWISE,)IRASの相関AKARI)9)um)v.s.)IRAS)12)um,)WISE)12)um

AKARI)18)um)v.s.)IRAS)25)um,)WISE)22)umバンド間のずれは?

10 Ichikawa et al.

0

5

10

15

20

25

30

0 0.05 0.1 0.15 0.2

Num

ber o

f sou

rces

Distance[arcmin]

IRCFIS

Fig. 1.— The histograms of position difference between the optical counterparts of the Swift/BAT AGNs and their AKARI counterparts(red: IRC, blue: FIS).

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(IR

AS 1

2µm

) [er

g s-

1 ]

log!L!(AKARI 9µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(IR

AS 2

5µm

) [er

g s-

1 ]

log!L!(AKARI 18µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(W

ISE

12µm

) [er

g s-

1 ]

log!L!(AKARI 9µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(W

ISE

25µm

) [er

g s-

1 ]

log!L!(AKARI 18µm) [erg s-1]

Fig. 2.— The plot of infrared luminosities between AKARI and IRAS (top panels). Each panel shows luminosity relation betweenAKARI 9 µm v.s. IRAS 12 µm (Left: 48 sample) , AKARI 18 µm v.s. IRAS 25 µm (Right: 51 sample) respectively. Bottom panels showthe infrared luminosities between AKARI and WISE, AKARI 9 µm v.s. WISE 12 µm (Left: 31 sample) and AKARI 18 µm v.s. WISE 22µm (Right 32 sample) .

10 Ichikawa et al.

0

5

10

15

20

25

30

0 0.05 0.1 0.15 0.2

Num

ber o

f sou

rces

Distance[arcmin]

IRCFIS

Fig. 1.— The histograms of position difference between the optical counterparts of the Swift/BAT AGNs and their AKARI counterparts(red: IRC, blue: FIS).

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(IR

AS 1

2µm

) [er

g s-

1 ]

log!L!(AKARI 9µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(IR

AS 2

5µm

) [er

g s-

1 ]

log!L!(AKARI 18µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(W

ISE

12µm

) [er

g s-

1 ]

log!L!(AKARI 9µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5lo

g!L !

(WIS

E 25

µm) [

erg

s-1 ]

log!L!(AKARI 18µm) [erg s-1]

Fig. 2.— The plot of infrared luminosities between AKARI and IRAS (top panels). Each panel shows luminosity relation betweenAKARI 9 µm v.s. IRAS 12 µm (Left: 48 sample) , AKARI 18 µm v.s. IRAS 25 µm (Right: 51 sample) respectively. Bottom panels showthe infrared luminosities between AKARI and WISE, AKARI 9 µm v.s. WISE 12 µm (Left: 31 sample) and AKARI 18 µm v.s. WISE 22µm (Right 32 sample) .

AKARI)18um AKARI)18um

IRAS)25um

AKARI)18um)v.s.)IRAS)25um AKARI)18um)v.s.)WISE)22)um

WISE)22um

113$are$selected$from$137$sources$(~82%$completeness)(type$1:$47,$type$2:$52,$New$type:$14)

AKARIとWISE,)IRASの相関AKARI)9)um)v.s.)IRAS)12)um,)WISE)12)um

AKARI)18)um)v.s.)IRAS)25)um,)WISE)22)umバンド間のずれは?

10 Ichikawa et al.

0

5

10

15

20

25

30

0 0.05 0.1 0.15 0.2

Num

ber o

f sou

rces

Distance[arcmin]

IRCFIS

Fig. 1.— The histograms of position difference between the optical counterparts of the Swift/BAT AGNs and their AKARI counterparts(red: IRC, blue: FIS).

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(IR

AS 1

2µm

) [er

g s-

1 ]

log!L!(AKARI 9µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(IR

AS 2

5µm

) [er

g s-

1 ]

log!L!(AKARI 18µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(W

ISE

12µm

) [er

g s-

1 ]

log!L!(AKARI 9µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(W

ISE

25µm

) [er

g s-

1 ]

log!L!(AKARI 18µm) [erg s-1]

Fig. 2.— The plot of infrared luminosities between AKARI and IRAS (top panels). Each panel shows luminosity relation betweenAKARI 9 µm v.s. IRAS 12 µm (Left: 48 sample) , AKARI 18 µm v.s. IRAS 25 µm (Right: 51 sample) respectively. Bottom panels showthe infrared luminosities between AKARI and WISE, AKARI 9 µm v.s. WISE 12 µm (Left: 31 sample) and AKARI 18 µm v.s. WISE 22µm (Right 32 sample) .

10 Ichikawa et al.

0

5

10

15

20

25

30

0 0.05 0.1 0.15 0.2

Num

ber o

f sou

rces

Distance[arcmin]

IRCFIS

Fig. 1.— The histograms of position difference between the optical counterparts of the Swift/BAT AGNs and their AKARI counterparts(red: IRC, blue: FIS).

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(IR

AS 1

2µm

) [er

g s-

1 ]

log!L!(AKARI 9µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(IR

AS 2

5µm

) [er

g s-

1 ]

log!L!(AKARI 18µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(W

ISE

12µm

) [er

g s-

1 ]

log!L!(AKARI 9µm) [erg s-1]

42

42.5

43

43.5

44

44.5

45

45.5

42 42.5 43 43.5 44 44.5 45 45.5

log!

L !(W

ISE

25µm

) [er

g s-

1 ]

log!L!(AKARI 18µm) [erg s-1]

Fig. 2.— The plot of infrared luminosities between AKARI and IRAS (top panels). Each panel shows luminosity relation betweenAKARI 9 µm v.s. IRAS 12 µm (Left: 48 sample) , AKARI 18 µm v.s. IRAS 25 µm (Right: 51 sample) respectively. Bottom panels showthe infrared luminosities between AKARI and WISE, AKARI 9 µm v.s. WISE 12 µm (Left: 31 sample) and AKARI 18 µm v.s. WISE 22µm (Right 32 sample) .

AKARI)18um AKARI)18um

IRAS)25um

AKARI)18um)v.s.)IRAS)25um AKARI)18um)v.s.)WISE)22)um

WISE)22um

Rela/ons$between$AKARI$and$WISE,$IRASInfrared Properties of Local AGNs 3

FIS sources, respectively, which correspond to typical 3σpositional errors at faintest fluxes (Ishihara et al. (2010);Yamamura et al. (2010)). We find 71, 80, and 63 AKARIcounterparts in the 9 µm, 18µm, and 90 µm bands outof the total 137 non-blazar BAT AGN sample. Figure 2shows the distribution of the angular separation betweenAKARI and optical positions for the Swift/BAT AGNswith IRC counterparts (red) and those with FIS counter-parts (blue). The IRC sources are more concentrated ina small distance range (with an average of 〈∆r〉 = 0.02′)than the FIS sources (〈∆r〉 = 0.08′), as expected fromthe positional accuracy in these catalogs.Further, for AGNs whose MIR fluxes are not reliably

measured (FQUAL < 3) or not detected with AKARI(66 and 57 sources in the 9 µm and 18 µm), we search fortheir counterparts at 12 µm or 25 µm in the IRAS-FSCand IRAS-PSC. Here we adopt the 50 arcsec radius, cor-responding to the

Results

8

LIR(9,$18$um)$∝L(14I195keV)

All$type(TypeI1,$TypeI2,$NewIType)follow$same$correla/ons

$$$$$$$$At$the$same$Lx$,LMIR(typeI2)$~$LMIR(typeI1)

midIIR/XIray$luminosity$rela/on

41.5

42

42.5

43

43.5

44

44.5

45

45.5

41.5 42 42.5 43 43.5 44 44.5 45 45.5

log

L(14

-195

keV)

[erg

s-1

]log L (18!m) [erg s-1]

1041

1042

1043

1044

1045

1046

1041 1042 1043 1044 1045 1046

L(1

4-19

5keV

)[erg

s-1

]

L (90µm) [erg s-1]

New-TypeType-2Type-1

NewITypeTypeI2TypeI1

Our$results$supportClumpy$dust$torus$model

9

○□◇!　:!WISE●■◆(small):!AKARI●■◆(Large):!IRAS

Infrared$average$SEDHao+$(2007)

The$excess$comes$from$7.7$um$PAH$emission?$

NewIType$AGN$host$galaxies$have$

ac/ve$starburst?

0.1

1

10

1 10 100

Nor

mal

ized

Lum

inos

ity

Wavelength[µm]

9um$excess?

1041

1042

1043

1044

1045

1046

1041 1042 1043 1044 1045 1046

L(1

4-19

5keV

)[erg

s-1

]

L (90µm) [erg s-1]

New-TypeType-2Type-1

NewIType

TypeI2

TypeI1

NewIType$AGN$9um$excess$sign

10

Summary

All$type$(TypeI1,$TypeI2,$NewIType)$follow$the$same$correla/ons

Our$results$does$not$support$smooth$dust$model

but$clumpy$dust$torus$model.

11

MidIIR$luminosity$is$a$good$tracer$of$AGN$ac/vity.

LMIR(9,$18$um)$∝L(14I195keV)

NewIType$9$um$excessIf$we$believe$this$excess$comes$from$7.7$um$PAH$emission,NewIType$AGN$host$galaxies$have$strong$starburst?

Future$workInves/ga/ng$the$origin$of$the$9$um$excess$sign$by$spectroscopy