Mid and Far Infrared Proper/es of a Complete Sample of Local AGNs 1 Kohei Ichikawa (Kyoto University) The Second AKARI Conference Feb 27I29, 2012 in Jeju, Korea Collaborators Yoshihiro 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
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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
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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
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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
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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$model
9
○□◇! :!WISE●■◆(small):!AKARI●■◆(Large):!IRAS
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Infrared$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
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